# GCN_circulars

GRB_name: GRB090618A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9528
SUBJECT: GRB090618: Swift-XRT team refined analysis
DATE:    09/06/18 19:06:26 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore (U. Leicester) and P. Schady (MSSL-UCL) report on
behalf of the Swift-XRT team:

We have analysed 12.3 ks of Swift-XRT data for GRB 090618 (Schady et
al. GCN Circ. 9512), from 124 s to 25.7 ks after the BAT trigger. The
data span five orbits and comprise 2.3 ks in Windowed Timing (WT) mode
and 10.0 ks in Photon Counting (PC) mode. The UVOT-enhanced XRT
position for this burst was reported by Evans et al. (GCN 9521).

The burst was initially very bright in X-rays, observed at a rate 
of ~8000 count s^-1, and decayed rapidly with a slope of ~6, before
breaking at T+310 s to a shallower decay slope of 0.71 +/- 0.02.
A further break is seen at T+4700 s with the decay steepening to 
1.22 +/- 0.05.

The WT spectrum from T+250 s to T+1065 s can be fit by an absorbed
powerlaw with a photon index of 2.11 +/- 0.03 and intrinsic absorption
of (1.78 +/- 0.14) x 10^21 cm^-2 (at z=0.54, Cenko et al., GCN 9518),
in addition to the Galactic column of 5.8 x 10^20 cm^-2 in the
direction of the source (Kalberla et al. 2005). The observed 0.3-10
keV flux for this model is (8.2 +0.2 -0.1) x 10^-10 erg cm^-2
s^-1. The corresponding unabsorbed flux is (1.16 +/- 0.02) x 10^-9 
erg cm^-2 s^-1.

If the light curve continues to decay at the same rate we predict a
count rate of 0.13 count s^-1 at T+24 hours, which corresponds to an
observed (unabsorbed) 0.3-10 keV flux of 4.9 x 10^-12 (7.2 x 10^-12)
erg cm^-2 s^-1.

The results of the XRT team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00355083.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9529
SUBJECT: GRB 090618: SARA observations
DATE:    09/06/18 23:00:02 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria Updike, Sean Brittain, Dieter Hartmann (Clemson University), Andrew
Colson, Renata Cumbee, Brianne Hackett, Josiah Lewis, and Marten Kronberg
(SARA REU) report:

We observed the field of GRB 090618 (Schady et al., GCN 9512) using the
0.9m SARA telescope at Kitt Peak National Observatory beginning 1.5 hours
after the trigger and continuing for 2 hours.  Our observations consisted
of 45 sec exposures in the I and R bands.  The afterglow was detected in
every image.  Magnitudes are given below as compared to the USNOB.1
catalog.  Time is given in seconds after the trigger; exposure time in
seconds.

Time   Filter   Exp      Mag
------------------------------------
5400     I      45     16.2 +/- 0.05
6300     R      45     16.8 +/- 0.05

Further observations are planned.

http://www.saraobservatory.org/


GRB_name: GRB090618A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9530
SUBJECT: GRB 090618: Swift-BAT refined analysis
DATE:    09/06/19 00:43:00 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings
(GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm
(GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), P. Schady (MSSL-UCL),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-5 to T+320 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 090618 (trigger #355083)
(Schady, et al., GCN Circ. 9512).  The BAT ground-calculated position is
RA, Dec = 294.008, 78.352 deg, which is
   RA(J2000)  =  19h 36m 01.8s
   Dec(J2000) = +78d 21' 07.1"
with an uncertainty of 0.46 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 62.5%.

The mask-weighted light curve shows two episodes with four prominent
peaks. The first episode is a smooth 50 sec peak starting at T-5 sec,
and ends at T+45 sec. The second episode is about 275 second long
and consists of three overlapping peaks. The second episode starts
at ~T+45 sec, the first peak is around T+62 sec, the second peak is
around T+80, and the third is around T+112 and finally ends at
T+320 sec.  Our T90 (15-350 keV) is 113.2 +/- 0.6 sec (estimated
error including systematics).

The time-averaged spectrum from T-5 to T+109 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.712 +/- 0.018. The fluence in the 15-150 keV band is
1.06 +/- 0.01 x 10^-4 erg/cm2. The 1-sec peak photon flux measured
from T+65.12 sec in the 15-150 keV band is 38.9 +/- 0.8 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/355083/BA/


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9531
SUBJECT: GRB090618 - Continued optical monitoring and light curve  break
DATE:    09/06/19 08:56:19 GMT
FROM:    Zach Cano at ARI/John Moores Liverpool  <zec@astro.livjm.ac.uk>

Z. Cano (Liverpool JMU), C. Guidorzi (U. Ferrara), D. Bersier,
A. Melandri, I.A. Steele, R.J. Smith, C. Mundell (Liverpool JMU)
report, on behalf of a large collaboration:

Following our report of observations (GCN 9520) we continued monitoring
the field of GRB090618 (Swift trigger 355083) on the Liverpool Telescope
(La Palma) from 13.6 hours to 17.9 hours post burst in R and i bands.
Below is a summary of a few R-band images:

t_exp  t-T0          R-mag

300s   13.6 hours    18.9  0.1
300s   15.6 hours    19.1  0.1
300s   17.9 hours    19.3  0.1

The calibration is still preliminary and determined against stars in
the USNO catalog.

We note a break in the R-band light curve, and find a decay index of
alpha~1.4 by 17.9 hours post burst, as compared to alpha~0.7 previously
reported (GCNs 9517, 9520).


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9532
SUBJECT: GRB 090618 15GHz radio detection
DATE:    09/06/19 09:50:32 GMT
FROM:    Guy Pooley at MRAO, Cambridge, UK  <ggp1@cam.ac.uk>

Guy Pooley (Cavendish Astrophysics, U. Cambridge) reports on behalf 
of the AMI collaboration:

The AMI Large Array (the rebuilt Ryle Telescope) was used to observe 
the field of GRB 090618 (Schady et al, GCN9512) on 2009 June 19 
from 02h45m to 05h45m UT (18.25 to 21.25h after the burst) 
using the position from Cenko et al (GCN9213). 
The observing band was 14.6 to 17.5 GHz and the rms noise 85 microJy. 
The angular resolution is approx. 50" x 20".

We make a clear detection of a source at the position of the GRB
with a flux density 550 microJy. A split of the data suggests that 
the flux density increased from 425 to 640 microJy between the
first and second halves of the observation, but this is barely 
statistically significant. 

There is no radio source visible at that position in the NVSS (1.4GHz).

This report may be quoted in publications.


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9533
SUBJECT: VLA radio detection of GRB 090618
DATE:    09/06/19 14:04:59 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on
behalf of a larger collaboration:

"We used the Very Large Array to observe the field of view toward the
GRB 090618 (GCN 9512) at a frequency of 8.46 GHz on 2009 June 19.33 UT.
We observed the radio afterglow of the GRB at P60 optical afterglow
position reported by Cenko et al. (GCN 9513). The GRB radio afterglow
flux density is 383+/-47 uJy. Further observations are planned.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB090618A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9534
SUBJECT: GRB 090618, Swift-BAT refined spectral analysis
DATE:    09/06/19 18:13:00 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

T. Sakamoto (GSFC/UMBC), T. N. Ukwatta (GWU/GSFC),
S. D. Barthelmy (GSFC), (i.e. the Swift-BAT team):

Using the data set from T-373 to T+962 sec from the
recent telemetry downlink, we report further spectral
analysis of BAT GRB 090618 (trigger #355083)
(Schady, et al., GCN Circ. 9512).

The time-averaged spectrum from T-4.4 to T+213.6 sec
is best fit by a power law with an exponential cutoff.
This fit gives a photon index 1.42 +/- 0.08,
and Epeak of 134 +/- 19 keV (chi squared 14.6
for 56 d.o.f.).  For this model the total fluence in
the 15-150 keV band is 1.05 +/- 0.01 x 10^-04 erg/cm2
and the 1-sec peak flux measured from T+65.38 sec in
the 15-150 keV band is 38.8 +/- 0.8 ph/cm2/sec.
A fit to a simple power law gives a photon index
of 1.72 +/- 0.02 (chi squared 55.8 for 57 d.o.f.).
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/355083/BA/


GRB_name: GRB090618A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9535
SUBJECT: GRB 090618: Fermi GBM observation
DATE:    09/06/19 22:55:39 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

Sheila McBreen (UCD/MPE)
reports on behalf of the Fermi GBM Team:

"At 08:28:26.66 UT on 18 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090618 (trigger 267006508 / 090618353)
which was also detected by Swift/BAT (Schady et al. 2009, GCN 9512)
and AGILE (Longo et al. 2009, GCN 9524).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 133 degrees.

The GBM light curve consists of 4 pulses
with a duration of about 155 s (8-1000 keV).
The time-averaged spectrum from T0 to T0+140 s is
adequately fit by a Band function with Epeak = 155.5 (+11.1/-10.5) keV,
alpha = -1.26 (+0.06/-0.02), and beta = -2.50 (+0.15/-0.33).
We observe significant spectral evolution within the fitted
time interval.

The event fluence (8-1000 keV) in this time interval is
(2.70 +/- 0.06)E-4 erg/cm^2.  Using standard cosmology
(Omega_matter = 0.27, Omega_lambda = 0.73, H0=71)
and the reported redshift of 0.54 (Cenko et al. 2009, GCN 9518)
the isotropic equivalent energy in the 8-1000 keV band is
E_iso = 2.0E+53 erg.

The 1-sec peak photon flux measured starting from T0+63 s
in the 8-1000 keV band is  73.4 +/- 2.0 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9536
SUBJECT: GRB090618: OAA-OAUV Optical observations
DATE:    09/06/19 23:05:06 GMT
FROM:    Alberto Fernandez-Soto at IFCA (CSIC/UC,Santander)  <fsoto@ifca.unican.es>

A. Fernandez-Soto (IFCA-Santander), V. Peris (OAUV-Valencia), and
J. Alonso-Lorite (OAUV-Valencia) report:

We have observed the field of GRB090618 (Schady et al., GCN 9512) with
the OAUV-0.4m telescope at the Observatorio Astronomico de Aras (OAA)
in Aras de Alpuente (Valencia, Spain). Observations began after local
sunset on June 18 (UT 19:32, (t-t0)~11.1 hours).

We took 23 four-minute exposures using a Johnson R filter. The
individual frames have been combined in five groups. The afterglow
reported in GCN9512 and confirmed by Cenko et al. (GCN 9513) is
clearly detected in all five images, with magnitudes and times:

UT(middle)   Exposure    R    Error
----------   --------  -----  -----
  21:30:03     5x4min   18.67   0.14
  21:50:51     5x4min   18.57   0.09
  22:42:14     4x4min   18.62   0.09
  23:21:44     5x4min   18.92   0.13
  23:45:19     2x4min   18.96   0.13

All magnitudes have been calibrated using stars in the field and the
USNO-B1 catalog (R1 mags).

Our results agree with those reported by Cano et al. (GCN 9531), and
support the presence of a break in the R-band decay, which happened at
(t-t0) ~ 14.6 hours.

A lightcurve combining our data and previous GCNs is posted at
http://ayalga.uv.es/~fsoto/grb090618

OAA is operated by the Observatori Astronomic de la Universitat de
Valencia (OAUV).


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9537
SUBJECT: GRB090618, underlying supernova search
DATE:    09/06/20 09:08:39 GMT
FROM:    Arnon Dar at Technion-Israel Inst. of Tech  <arnon@physics.technion.ac.il>

S. Dado and A. Dar report:

The inferred photon spectral index Gamma=2.01+/-0.05 of the early time 
X-ray afterglow of the relatively nearby bright GRB090618 (z=1.54, GCN 
9518) from the Swift XRT observations (Evans et al. 
http://www.swift.ac.uk/xrt_spectra/00355083/) implies, in the CB model 
(e.g. ApJ 696 (2009), 994), an asymptotic achromatic power-law decline of 
the afterglow with a spectral index beta=1.01+/-0.05 and a temporal index 
alpha=beta+1/2=1.51+/-0.05. The R-band light curve of the anticipated 
underlying supernova akin to SN1998bw is expected to reach maximum 
brightness magnitude R=23.9 (Galactic extinction included) around July 10, 
2009 (approximately 22 days after GRB090618). Using the latest optical 
measurements reported in GCN 9531 and GCN 9536, the GRB afterglow is 
expected to decay by July 10, 2009 to a magnitude R=24.6+/-0.20 yielding 
R=23.4+/-0.3 for the optical transient superposed on a bright host galaxy 
with r=22.7 +/- 0.3 (GCN 9526). Like in the case of GRB 030319 (ApJ 594 
(2003), L89), the search for an underlying supernova (GCN 9526) in 
GRB060618 may be more successful using large telescopes with high 
resolution for photometric and/or spectroscopic follow up measurements of 
its optical afterglow.


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9538
SUBJECT: GRB 090618 : WSRT radio detection
DATE:    09/06/20 19:59:19 GMT
FROM:    Atish Kamble at U. of Amsterdam  <A.P.Kamble@uva.nl>

Atish Kamble (University of Amsterdam), A.J. van der Horst (NASA/ORAU) 
and Ralph Wijiers (University of Amsterdam) reports on behalf of 
a larger collaboration :

"We observed the position of GRB 090618 afterglow at 4.9 GHz 
using the Westerbork Synthesis Radio Telescope between
June 19.78 to 20.30 UT i.e. 1.7 days after the burst (GCN 9512, 
GCN 9532, GCN 9533). The radio afterglow was clearly detected 
and its measured flux density is about 501 +/- 47 microJy.

We would like to thank the WSRT staff for scheduling and carrying out 
these observations."


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9539
SUBJECT: GRB 090618: ZTSh optical observations
DATE:    09/06/21 01:01:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO), A. Pozanenko (IKI)  report on behalf of larger GRB 
follow-up collaboration:

We observed the afterglow (Schady  et al., GCN 9512; Cenko et al., GCN 9513; 
Perley, GCN 9514; Rujopakarn et al., GCN 9515) of  the Swift GRB 090618 
between  (UT) Jun. 18  19:51 -  Jun. 19 00:51 with Shajn telescope of  CrAO. 
We detect afterglow in every  BVRI of 60 s exposure images of the series. 
Coordinates of the afterglow are RA(J2000):  19 35 58.77 Dec(J2000): +78 21 
24.2 with uncertainties of  0.3 arcsec.

Preliminary photometry of selected images based on USNO-B1.0 star 
1683-0077955  (RA=19 36 36.34   Dec=+78 21 07.00) assuming R=16.57  is 
following:

T0+     Filter, Exposure, mag.,     err.
(d)             (s)

0.4763   R       60     18.60 +/-0.05
0.5680   R       60     18.87 +/-0.03
0.6496   R       60     19.17 +/-0.04
0.6796   R       60     19.19 +/-0.10

The power low index of light curve approximation between 0.48 - 0.65 days 
is ~ -1.6, while after  0.65 days after burst onset we observe flattening of 
the light curve. A finding chart can be found at 
http://grb.rssi.ru/GRB090618/GRB090618_090618_R_ZTSh.gif 


GRB_name: GRB090621A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9540
SUBJECT: GRB 090621: Swift detection of a burst
DATE:    09/06/21 04:53:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P.A. Curran (MSSL-UCL), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. Stamatikos (NASA/ORAU), M. C. Stroh (PSU),
T. N. Ukwatta (GSFC/GWU) and H. Ziaeepour (UCL-MSSL) report on behalf
of the Swift Team:

At 04:22:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090621 (trigger=355303).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 10.986, +61.968 which is 
   RA(J2000) = 00h 43m 57s
   Dec(J2000) = +61d 58' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed weak emission during
the 8 seconds of the trigger interval.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~4 sec after the trigger. 

There was a second BAT trigger (trigger=355304) at 04:27:05, about 
4 minutes after the initial trigger from the same location.  This 
portion of the BAT light curve is not immediately available from 
TDRSS, but the retrigger could indicate an extended prompt phase. 

The XRT began observing the field at 04:24:40.46 UT, 117.3 seconds after
the BAT trigger. XRT found an uncatalogued, variable X-ray source located
at RA, Dec 11.0191, 61.9417 which is equivalent to:
   RA(J2000)  = 00h 44m 04.58s
   Dec(J2000) = +61d 56' 30.2"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 110 arcseconds from the BAT onboard position, within the BAT
error circle.  There is a bright peak at about 250s after the initial trigger
which could be X-ray emission during prolonged prompt emission. 


UVOT took a finding chart exposure of 150 seconds with the White filter
starting 122 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain extinction expected. 




Burst Advocate for this burst is P.A. Curran (pac AT mssl.ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090618A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9541
SUBJECT: GRB 090618: BOAO V-band Observation
DATE:    09/06/21 06:09:55 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

  M. Im (CEOU/Seoul National Univ), Y.-B. Jeon (KASI), and
  Y. Urata (NCU)

   We observed GRB090618 (Schady et al. GCN 9512) in V using
  a 15.5cm refractor at Bohyunsan Optical Astronomical Observatory
  in Korea, operarted by the Korea Astronomy Space Science Institute.
   A series of exposures were taken starting at 2009 June 18, 11:54:19.
   The afterglow, identified earlier by many groups
  (GCN 9513, 9514, 9515, 9520, 9522), was clearly detected
  at V=17.9 +- 0.1 magnitude at mid-time of 2009 12:55:07
  (about 4hr 26.6min after the BAT trigger).
   The photometry was calibrated against nearby SDSS stars
  where the transformation of SDSS magnitude to V-band magnitude
  was carried out using the recipe of Chonis & Gaskell (2008).


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9542
SUBJECT: GRB090618: Spectrum and photometry from 6.0m BTA
DATE:    09/06/21 09:05:13 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

T. Fatkhullin, A. Moskvitin (SAO-RAS Niznijh Arkhyz, Russia),
A.J. Castro-Tirado (IAA-CSIC Granada), A. de Ugarte Postigo
(ESO, INAF/OAB), on behalf of a larger collaboration, report:

We have observed the field of GRB090618 (Schady et al.,
GCN 9512) with the 6-m telescope of the SAO RAS in
Caucasus. We obtained B, Rc and Ic images as well as a
low-resolution spectrum under non favorable weather conditions.
The range and resolution of the spectrum were 3900-9200AA
and FWHM=15-17A, respectively. A preliminary processing of
the spectrum showed a faint emission line at 5748.55A which we
interpret as [OII] 3727A. A corresponding redshift of 0.54 is in
full agreement with one obtained by Cenko et al. (GCN 9518).
Because of strong night sky OH bands and low resolution of the
spectrum we could not clearly detect expected Hbeta and
[OIII]4959,5007A lines. The photometry was calibrated using a
number of SDSS stars in the field. Below we present a summary
of some of our observations:

               middle date, UT         results
   -------------------------------------------------------
   spectrum   19.977 June 2009      [OII]3727A detection
          Rc     19.941 June 2009      20.51 +/- 0.06

This message can be cited.


GRB_name: GRB090621A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9543
SUBJECT: GRB 090621: Swift-XRT Team refined analysis
DATE:    09/06/21 12:18:05 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) & P.A. Curran (UCL-MSSL) report on behalf of the 
Swift-XRT team:

We have analysed the first four orbits of XRT data obtained for GRB 
090621 (Curran et al., GCN Circ. 9540), comprising 192 s of Windowed 
Timing (WT) mode and 6.4 ks of Photon Counting (PC) mode. The refined XRT 
position is RA, Dec = 11.01982, 61.94115, which is equivalent to

RA (J2000) =  00 44 04.76 
Dec(J2000) = +61 56 28.1

with an uncertainty of 3.6 arcsec (radius, 90% containment).

The X-ray light-curve shows a large increase in emission peaking at 264 s 
after the initial trigger, corresponding to the time of the second BAT 
trigger (Curran et al., GCN Circ. 9540). The underlying decay, however, 
can be parameterised as a single power-law with alpha = 0.81 +/- 0.04.

As is common, there is clear spectral evolution during the flare. A 
spectrum extracted from the PC mode data after the flare subsides (500 s 
after the trigger) can be modelled with a power-law of Gamma = 2.07 
+0.37/-0.35 and a total absorbing column of (1.5 +/- 0.4)x10^22 cm^-2; the 
Galactic column in this direction is 5.6x10^21 cm^-2 (Kalberla et al. 
2005). Using this spectrum, the counts to observed (unabsorbed) flux 
conversion factor is 6.3x10^-11 (1.5x10^-10) erg cm^-2 count^-1.

If the light-curve continues to decay with alpha ~ 0.81, the predicted 
count rate at 24 hours is 0.015 count s^-1, corresponding to an observed 
(unabsorbed) flux of 9.5x10^-13 (2.2x10^-12) erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090621A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9544
SUBJECT: GRB 090621: Swift/UVOT Upper Limits
DATE:    09/06/21 12:29:18 GMT
FROM:    Peter Curran at MSSL  <pac@mssl.ucl.ac.uk>

P.A. Curran (UCL-MSSL) reports on behalf of the Swift/UVOT team:


The Swift/UVOT began settled observations of the field of GRB 090621
123 s after the BAT trigger (Curran et al., GCN 9540). No optical
afterglow consistent with the refined XRT position (Page et al., GCN 
9543) is detected in the initial UVOT exposures. Preliminary 3-sigma 
upper limits using the UVOT photometric system (Poole et al. 2008, 
MNRAS, 383, 627) for the first exposures are:


Filter         T_start(s)  T_stop(s)  Exp(s)     Mag

wh             123         7115       805        >21.5
v              613         6089       333        >19.4
b              538         6910       310        >20.5
u              282         6705       736        >20.5
uw1            662         6500       320        >19.8
um2            637         6295       333        >19.7
uw2            588         5884       333        >19.9


The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090621B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9545
SUBJECT: GRB 090621B: Swift detection of a short hard burst
DATE:    09/06/21 22:38:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

P.A. Curran (MSSL-UCL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), A. Rowlinson (U Leicester),
T. Sakamoto (NASA/UMBC), P. Schady (MSSL-UCL), M. C. Stroh (PSU) and
H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team:

At 22:07:25 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090621B (trigger=355359).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 313.432, +69.013 which is 
   RA(J2000)  =  20h 53m 44s
   Dec(J2000) = +69d 00' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration less than 128 millisec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at  22:08:36UT, 70.7 s after the BAT trigger. 
In promptly downlinked data, XRT found a faint uncatalogued source at RA, Dec 
(J2000) = 313.4700,   69.0282, which is
RA = 20h 53m 52.8s
Dec = +69d 01' 41.5"
with an uncertainty of 8.0 arcseconds (radius, 90% containment). This
location is 73 arcseconds from the BAT onboard position, within the BAT
error circle. 

UVOT took a finding chart exposure of nominal 150 seconds with the
White filter  starting 76 seconds after the BAT trigger. No credible
afterglow candidate has  been found in the initial data products at
the XRT position. Data from the 2.7'x2.7' sub-image are not available
at this time. The 8'x8' region for the list of sources generated
on-board covers 100% of the BAT error circle. The list of sources is
typically complete to about 18 mag. No correction has been made for
the expected extinction corresponding to E(B-V) of 0.43 (Schlegel et
al. 1998). 

Burst Advocate for this burst is P.A. Curran (pac AT mssl.ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090621A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9546
SUBJECT: GRB 090621A: Swift-BAT refined analysis
DATE:    09/06/22 01:14:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
P.A. Curran (MSSL-UCL), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090621A (trigger #355303)
(Curran, et al., GCN Circ. 9540).  The BAT ground-calculated position is
RA, Dec = 10.987, 61.938 deg, which is 
   RA(J2000)  =  00h 43m 56.8s 
   Dec(J2000) = +61d 56' 17.6" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
 
The mask-weighted light curve shows two small precursor peaks starting
at ~T-30 sec, peaking at ~T-20 and T+10 sec, and returning to background
at ~T+100 sec.  Then the mmain emission starts at ~T+210 sec, peaks at ~T+240
and T+265 sec, and returns to background around T+350 sec.
T90 is not possible because of a lack of the complete set of event by event
data set for this burst.   This also prevents giving spectral results.


GRB_name: GRB090621B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9547
SUBJECT: GRB 090621B: Optical Observations
DATE:    09/06/22 01:41:48 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), P. Curran (MSSL), K. Wiersema (U. Leicester)
and P. Groot (Nijmegen) report:

"We observed the location of the short GRB 090621B (Curran et al. GCN
9545) with the WHT, beginning at 23:48:33 UT. Observations were
obtained in the i-band, with a total exposure time of 1800s. Inside
the XRT error box we find a faint object at

RA = 20 53 53.07 
Dec = +69 01 40.8

with errors of approximately 0.5" in each axis. The object is
significantly fainter than the DSSII limit, and shows no obvious
variability between the first and last exposures (taken ~1.7 and
~2.3 hours post burst). Given the relatively high foreground
extinction the probability of a chance alignment within the XRT
error box is non-trivial. Hence we are unable to make strong
statements about the association of this source with GRB 090621B 
at this stage."


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9548
SUBJECT: GRB 090618: RTT150 optical observations
DATE:    09/06/22 09:50:24 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

A. Galeev, I. Bikmaev, N. Sakhibullin (KSU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

We observed the OT (Schady et al., GCN 9512; Cenko et al., GCN 9513; Perley,
GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 with
Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey), in BRc bands, starting at 22 Jun, 00:03 UT,
i.e. approximately 3.65 days after the burst, using TFOSC.
  
We made 3x900s exposures in Rc band and 2x900 in B band. The OT is detected
in all images. Using the same USNO-B1 star as it was used by Rumyantsev and
Pozanenko (GCN 9539) we estimate Rc magnitude as m_Rc=21.60+/-0.04 (3.68
days after the burst).

The finding chart can be found at:

http://hea.iki.rssi.ru/grb/090618/indexeng.html


GRB_name: GRB090621B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9549
SUBJECT: GRB 090621B: RTT150 optical observations
DATE:    09/06/22 09:55:15 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

A. Galeev, I. Bikmaev, N. Sakhibullin (KSU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU),  E. Gogus (Sabanci Uni.)

report:

We observed the field of the Swift-BAT GRB 090621B (Curran et al., GCN9545)
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey), starting at 21 Jun, 22:52:55 UT, i.e. approximately 45
minutes after the burst, using TFOSC. 

We made 3x300s exposures in Rc band. On combined image we do not detect any
new source inside the XRT error circle (Curran et al., GCN 9545) besides the
source reported by Levan et. al. (GCN 9547), which is detected only
marginally. There is also one more brighter point-like source
(RA=20:53:51.25, DEC=+69:01:37.4, J2000) outside but close to the edge of
XRT error circle. Using USNO-B1 stars we estimate its magnitude as
m_Rc=21.8+/-0.06. The limiting magnitude of combined image is m_Rc ~23.6.

The finding chart can be found at:

http://hea.iki.rssi.ru/grb/090621b/indexeng.html


GRB_name: GRB090621B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9550
SUBJECT: GRB 090621B: Swift-XRT refined analysis
DATE:    09/06/22 10:16:55 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore, K.L. Page (U. Leicester) and P.A. Curran (UCL-MSSL)
report on behalf of the Swift-XRT team:

We have analysed five orbits of Swift-XRT photon counting (PC) mode data 
from GRB 090621B (Curran et al., GCN Circ. 9545), spanning the interval 
T+80 s to T+19.5 ks after the trigger.  In 10.0 ks we find a refined XRT 
position of RA, Dec = 313.47049, 69.02845, which is equivalent to

RA (J2000) =  20:53:52.92
Dec(J2000) = +69:01:42.4

with an uncertainty of 4.0 arcsec (90% containment). This position
is 1.2 arcsec from the XRT position quoted in GCN Circ. 9545.

The X-ray light-curve shows a faint, fading source with a decay index
of 0.61  +/- 0.19. If the source continues to decay at the same rate 
we predict an XRT count rate of 8.6e-4 count s^-1 at T+24 hours.

The PC mode spectrum from T+80 s to T+17.1 ks can be fit by an absorbed 
powerlaw with a photon index of 1.47+/-0.66, assuming a Galactic column 
density of 1.9e21cm^-2 in the direction of the burst.  The observed 
(unabsorbed) 0.3-10keV flux for this model is 3.8e-13 (4.5e-13)
erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090621B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9551
SUBJECT: GRB 090621B: Swift-BAT refined analysis
DATE:    09/06/22 13:08:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P.A. Curran (MSSL-UCL), E. E. Fenimore (LANL),
N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT short hard burst GRB 090621B (trigger #355359)
(Curran, et al., GCN Circ. 9545).  The BAT ground-calculated position is
RA, Dec = 313.455, 69.034 deg, which is 
   RA(J2000)  =  20h 53m 49.3s 
   Dec(J2000) = +69d 02' 02.9" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 69%.
 
The mask-weighted light curve shows a single peak starting a ~T+0 sec
and ending at ~T+0.2 sec.  There is a 2.5-sigma hint of extended emission
from ~T+150 to ~T+240 sec.  T90 (15-350 keV) is 0.14 +- 0.04 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.028 to T+0.148 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.82 +- 0.23.  The fluence in the 15-150 keV band is 7.0 +- 1.0 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.44 sec in the 15-150 keV band
is 3.9 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/355359/BA/


GRB_name: GRB090621B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9552
SUBJECT: GRB 090621B: Swift/UVOT Upper Limits
DATE:    09/06/22 13:45:39 GMT
FROM:    Peter Curran at MSSL  <pac@mssl.ucl.ac.uk>

P.A. Curran (MSSL-UCL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090621B
76s after the BAT trigger (Curran et al., GCN 9545). No optical
afterglow consistent with the refined XRT position (Beardmore et al.,
GCN 9550) or the optical source observed by Levan et al. (GCN  9547) is
detected in the UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first exposures are:

Filter T_start(s) T_stop(s)  Exp(s)  Mag
wh      76         18173      1221    >22.29
v       618        10774      1142    >20.67
b       544        23952      1986    >21.88
u       289        29731      2675    >21.77
uw1     668        29017      2882    >21.63
um2     643        28110      2006    >21.32
uw2     594        6589       432     >20.50

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.44 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090618A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9553
SUBJECT: Konus-Wind and Konus-RF observations of GRB 090618
DATE:    09/06/22 14:41:45 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long GRB 090618 (Schady et al. 2009, GCN 9512)
triggered Konus-Wind
at T0=30504.974 s UT (08:28:24.974),
and Konus-RF instrument onboard CORONAS-PHOTON s/c
at T0=30507.060 s UT (08:28:27.060).

The burst light curve shows a smooth multi-peaked structure
with a duration of ~160 s. Significant spectral evolution
was observed during the burst.

-- 
As observed by Konus-Wind the burst had
a fluence of (2.5  0.06)x10-4 erg/cm2,
and a 64-ms peak flux measured from T0+63.616 s
of (1.6  0.2)x10-5 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+142 s) can be fitted
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -1.28  0.02,
the high energy photon index beta = -2.66(-0.2, +0.14),
the peak energy Ep = 186  8 keV (chi2 = 103/60 dof).

The spectrum at the maximum count rate,
measured from T0+62.720 to T0+64.0 s, is well fitted
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.99 (-0.06, +0.07),
the high energy photon index beta = -2.29(-0.5, +0.23),
the peak energy Ep = 440  70 keV (chi2 = 52/55 dof).

-- 
As observed by Konus-RF the burst
had a fluence of (2.82  0.06)x10-4 erg/cm2
(both in the 20 keV - 2 MeV energy range),
and a 500-ms peak flux measured from T0+63.0 s
of (1.6  0.1)x10-5 erg/cm2/s
(in the 20 keV - 1.5 MeV energy range).

The time-integrated spectrum of the burst
(from T0-1.4 to T0+113.0 s) can be fitted
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -1.28  0.03,
the high energy photon index beta = -3.06(-0.5, +0.3),
the peak energy Ep = 220  8 keV (chi2 = 240/132 dof).

The spectrum at the maximum count rate,
measured from T0+63.0 to T0+63.5 s, is well fitted
(in the 20 keV - 1.5 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.89 (-0.1, +0.3),
the high energy photon index beta = -2.56(-1.0, +0.6),
the peak energy Ep = 385 (-136, +64) keV (chi2 = 78/74 dof).

-- 
All the quoted values are preliminary.
The quoted errors are at the 90% confidence level.

The light curves of this GRB is available
at http://www.ioffe.ru/LEA/GRBs/GRB090618_T30504/


GRB_name: GRB090620A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9554
SUBJECT: GRB 090620: Fermi GBM detecion
DATE:    09/06/22 15:11:42 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 09:36:23.47 UT on 20 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090620 (trigger 267183385 / 090620400).

The on-ground calculated location, using the GBM trigger
data, is RA = 237.4 deg, DEC = 61.2 deg (J2000 degrees,
equivalent to 15 h 50 m, 61 d 12 '), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 60 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve shows a single peak
with a duration (T90) of about 16.5 s (8-1000 keV).
The time-averaged spectrum from T0-0.003 s to T0+16.640 s is
best fit by a Band function with Epeak = 156 +/- 6 keV,
alpha = -0.40 +/- 0.04, and beta = -2.44 +/- 0.10
(chi squared 576 for 532 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(6.6 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+4.352 s in the 8-1000 keV band
is 7.0 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090621B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9555
SUBJECT: GRB 090621B: VLA observations
DATE:    09/06/22 16:03:04 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger and W.-f. Fong (Harvard) report:

"We observed the field centered on the XRT error circle of the short GRB 
090621B (GCNs #9545,9550) with the VLA at a frequency of 8.46 GHz 
starting on 2009 June 22.53 UT (14.6 hours post burst).  We do not 
detect any sources within the refined XRT error circle to a 3-sigma 
limit of 54 microJy."

[GCN OPS NOTE(22jun09): Per author's request, the missing "B"
was added to the GCN name.]


GRB_name: GRB090621A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9556
SUBJECT: GRB 090621: Fermi GBM observation
DATE:    09/06/22 17:28:10 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 04:26:34.49  UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090621 (trigger 267251196  / 090621185) which was
also detected by the Swift/BAT (Curan et al. 2009, GCN 9540). The GBM
triggered on the second BAT trigger (355304) and at approx. 4 min after the
initial BAT trigger (355303) for this event. The GBM on-ground location is
consistent with the Swift position.
 
The angle from the Fermi LAT boresight is 12 degrees.

The GBM light curve shows a faint peak coinciding with the initial Swift
trigger (355303) and two brighter peaks starting at the GBM trigger time.
The burst duration (T90) including the first faint peak is about 294 s
(8-1000 keV).

The time-averaged spectrum of the two brighter peaks starting from the GBM
trigger time T0-6.10 s to T0+45.06 s is best fit by a Band function with
Epeak = 56.0 +/- 10.7 keV, alpha = -1.1 +/- 0.2, and beta = -2.12 +/- 0.09
(chi squared 377 for 366 d.o.f.).

The event fluence (8-1000 keV) in the above time interval is
(4.4 +/- 1.0)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+35.840 s in the 8-1000 keV band is  1.92 +/- 0.06 
ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090621B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9557
SUBJECT: GRB 090621B: P60 Observations
DATE:    09/06/22 17:40:24 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), A. J. Levan (U. Warwick), M. M. Kasliwal, S. R.
Kulkarni (Caltech) report on behalf of a larger collaboration:

We have imaged the field of the short GRB090621B (Curran et al., GCN 9545)
with the automated Palomar 60-inch telescope.  Observations consisted of
20 x 180 s images in the i' filter at a mean epoch of 5:37 UT on 22 June
2009 (~ 7.5 hours after the burst).

We detect the candidate afterglow reported by Levan et al. (GCN 9547) and
Galeev et al. (GCN 9549) at low significance.  Using several USNO-B
sources in the field for reference, we measure a magnitude of I ~ 22.9.
No other sources are detected inside the revised XRT error circle
(Beardmore et al., GCN 9550).

Directly comparing our P60 image with the WHT image from ~ 2 hours after
the burst (GCN 9547), we find the candidate has faded marginally by 0.5 +-
0.3 mag.  Further late-time observations will be needed to confirm if this
is the optical afterglow of GRB090621B.


GRB_name: GRB090621C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9558
SUBJECT: GRB 090621C: Fermi GBM detection
DATE:    09/06/22 19:42:15 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 10:00:52.10 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090621C (trigger 267271254 / 090621417).

The on-ground calculated location, using the GBM trigger
data, is RA = 257.5 deg, DEC = -28.5 deg (J2000 degrees,
equivalent to 17 h 10 m, -28 d 28 '), with an uncertainty
of 3.3 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 52 degrees.

The GBM light curve consists of multiple short peaks
with a duration (T90) of about 59.9 s (8-1000 keV).
The time-averaged spectrum from T0-3.072 s to T0+28.672 s is
well fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.4 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 148 +/- 34 keV
(chi squared 444 for 461 d.o.f.).

The event fluence (8-1000 keV) in the above mentioned time interval is
(1.8 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+4.096 s in the 8-1000 keV band
is 2.29 +/- 0.06 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090621B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9559
SUBJECT: GRB 090621B: Gemini spectrum of afterglow candidate
DATE:    09/06/22 19:42:32 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger (Harvard), A. Cucchiara, D.B. Fox (Penn State), and A.J. Levan 
(U. Warwick) report:

"On 2009 June 22.41 UT we used the GMOS instrument mounted on the 
Gemini-North 8-m telescope to obtain spectroscopic observations of the 
candidate optical afterglow (GCN #9547) of the short GRB 090621B (GCN 
#9545).  A pair of 1800 sec exposures were obtained with a wavelength 
coverage of 4500-7500A.  The combined spectrum of the source reveals 
broad features typical of an early M dwarf star.  We therefore conclude 
that this object is unrelated to the GRB."


GRB_name: GRB090621D
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9560
SUBJECT: GRB 090621D: Fermi GBM detection
DATE:    09/06/22 19:47:45 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 10:43:45.14  UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090621D (267273827 / 090621447).

The on-ground calculated location, using the GBM trigger
data, is RA = 12.3, DEC = -22.6 (J2000 degrees,
equivalent to 00 h 49 m, -22 d 36 '), with an uncertainty
of 4.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 79 degrees.

The GBM light curve consists of two peaks
with a duration (T90) of about 39.9 s (8-1000 keV).
The time-averaged spectrum from T0-1.024  s to T0+20.480 s is
adequately fit by a simple power law function with index -1.66 +/- 0.05
(chi squared 752 for 694 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(1.34 +/- 0.03)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-1.024 s in the 8-1000 keV band
is 1.74 +/- 0.05 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090621B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9561
SUBJECT: GRB 090621B: I-band observations from 1.23m CAHA
DATE:    09/06/22 20:05:29 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), P. Kubanek (GACE and IAA-CSIC), S. Mottola  
(DLR), U. Carsenty (DLR), A. Levan (U. Warwick), M. Jelinek (IAA- 
CSIC), A.J. Castro-Tirado (IAA-CSIC), A. de Ugarte Postigo (ESO, INAF/ 
OAB), report on behalf of a larger collaboration:

"Following the detection of the short-hard GRB 090621B by SWIFT  
(Curran et al. GCNC 9545) we carried out I-band observations with the  
1.23m telescope at Observatory of Calar Alto. The observations were  
done on June 22.094-22.161 UT (4.14-5.75 hours post burst) with a  
total exposure time of 22x240s. The candidates reported by Levan et  
al. (GCNC 9547) and Galeev (GCNC 9549) are preliminarily detected at  
I~22.5 and I~20.6, respectively, against USNO-B field stars."


GRB_name: GRB090621B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9562
SUBJECT: GRB 090621B: Fermi GBM detection
DATE:    09/06/23 00:03:11 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

A. Goldstein (UAH) and J.M. Burgess (UAH) 
report on behalf of the Fermi GBM Team: 

"At 22:07:25.70 UT on 21 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090621B (trigger 267314847 / 090621922)
which was also detected by the Swift BAT (P.A. Curran et al. 2009, 
GCN 9545). The GBM on-ground location is consistent with the 
Swift position.  The angle from the Fermi LAT boresight 
is 108 degrees.

The GBM light curve consists of one short spike
with a duration (T90) of about 0.128 s (8-1000 keV). 
The time-averaged spectrum from T0-0.064 s to T0+0.064 s is 
best fit by a Band function with Epeak = 321.60 +/- 129.00 keV, 
alpha = -0.13 +/- 0.38, and beta = -1.57 +/- 0.08
(chi squared 401 for 481 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(3.71 +/- 0.58)E-07 erg/cm^2. The 0.128-sec peak photon flux measured 
starting from T0-0.064 s in the 8-1000 keV band 
is 6.4 +/- 1.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090618A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9563
SUBJECT: PAIRITEL observations of GRB 090618
DATE:    09/06/23 01:00:35 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan,  C. R. Klein,  J. S. Bloom,  (UC Berkeley), report:

We observed the location of the optical afterglow of GRB 090618
(Schady et al., GCN 9512) with the 1.3m PAIRITEL located at Mt.
Hopkins, Arizona. Observations began at 2009-06-18 08:29:40 UT, 71
seconds after the Swift Trigger, under non-ideal sky conditions. In
the initial images, we detect a variable infrared source (identified
as the IR afterglow) in individual frames of 7.8 second simultaneous
exposures in the J, H, and Ks bands.

The preliminary photometry on selected stacks of images yield the
following photometry:

time
post burst exp.   filt  mag   m_err
[s]        [s]

210        93.6   J     12.7  0.1
210        93.6   H     12.1  0.1
210        93.6   Ks    11.4  0.2

2818       327    J     15.1  0.1
2818       327    H     14.6  0.1
2818       327    Ks    13.7  0.1

10636      585    J     16.2  0.2
10636      585    H     15.7  0.2
10636      585    Ks    >14.8 3-sigma

Intermittent clouds led to highly variable transmission and sky
brightnesses during the PAIRITEL observations. All magnitudes are
given in the Vega system, calibrated to 2MASS. No correction for
Galactic extinction has been made to the above reported values.
Further analysis is ongoing.


GRB_name: GRB090621A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9564
SUBJECT: GRB 090621A: GRT Optical Observation
DATE:    09/06/23 02:08:36 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),  
T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU),  
C.A. Wallace (FGCU) 

We observed the field of GRB 090621A detected by Swift 
(trigger #355303; Curran et al., GCN #9540) with the 14-inch 
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical 
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).   
 
100 set of 30 sec exposures were taken in the R filter starting 
from June 21 05:00:15 (UT) about 37.3 min after the trigger and 
stopped on June 21 05:56:22 (UT).  We do not detect the optical 
afterglow both in the individual images and the combined image 
inside the XRT position (Page et al., GCN #9543).  The estimated 
three sigma upper limit of the combined image (total exposure 
of 2850 sec; excluding five bad quality images) is ~17.9 mag using 
the USNO-B1 catalog. 


GRB_name: GRB090621B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9565
SUBJECT: GRB 090621B: GRT Optical Observation
DATE:    09/06/23 02:18:16 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),  
T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU),  
C.A. Wallace (FGCU) 
  
We observed the field of GRB 090621B detected by Swift 
(trigger #355359; Curran et al., GCN #9545) with the 14-inch 
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical 
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).   

100 set of 30 sec exposures were taken in the R filter starting 
from June 22 01:51:44 (UT) about 3.7 hours after the trigger and 
stopped on June 22 02:47:51 (UT).  We do not detect the optical 
afterglow both in the individual images and the combined image 
inside the XRT position (Beardmore et al., GCN #9550).  The 
estimated three sigma upper limit of the combined image (total 
exposure of 2880 sec; excluding four bad quality images) is 
~17.8 mag using the USNO-B1 catalog. 


GRB_name: GRB090623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9566
SUBJECT: GRB 090623: Fermi GBM detection
DATE:    09/06/23 14:52:32 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 02:34:17.56 UT on 23 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090623 (trigger 267417259 / 090623107).

The on-ground calculated location, using the GBM trigger
data, is RA = 309.0deg, DEC = -43.2 deg (J2000 degrees,
equivalent to 20 h 36 m, -43 d 12 '), with an uncertainty
of 2.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 73 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of at least five peaks
with a duration (T90) of about 72.2 s (8-1000 keV).
The time-averaged spectrum from T0-1.920 s to T0+40.064 s is
best fit by a power law function with an exponential
high energy cutoff.  The power law index is -0.73 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 476 +/- 39 keV
(chi squared 738 for 655 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(9.60 +/- 0.02)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.003 s in the 8-1000 keV band
is 3.30 +/- 0.04 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 737 for 654 
d.o.f.)
with Epeak= 428 +/- 51 keV, alpha = -0.69 +/- 0.05 and beta = -2.3 +/- 0.4.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090621A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9567
SUBJECT: GRB 090621A: Enhanced Swift-XRT position
DATE:    09/06/24 09:24:00 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page, P.A. Evans and M.R. Goad (U. Leicester) report
on behalf of the Swift-XRT team:

Using 5877 s of XRT Photon Counting mode data and 11 UVOT
images, we find an astrometrically corrected X-ray position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 11.02150, 61.94110 which is equivalent to:

RA (J2000):  00 44 5.16
Dec (J2000): +61 56 28.0

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

This position may be improved as more data are received.  The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090618A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9568
SUBJECT: GRB 090618: Suzaku WAM observation of the prompt emission
DATE:    09/06/24 13:05:44 GMT
FROM:    Kenta Kono at Miyazaki U  <kenta0514@astro.miyazaki-u.ac.jp>

K. Kono, A. Daikyuji, E. Sonoda, N. Ohmori, H. Hayashi, K. Noda,
Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa,
T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda,
T. Sugasahara (Saitama U.), Y. Urata (NCU),
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The bright, long GRB 090618 was detected by the Suzaku Wide-band All-sky
Monitor (WAM) which covers an energy range of 50 keV - 5 MeV
at 08:28:25.592 UT (=T0).
The observed light curve shows a multi-peaked structure
starting at T0-5 s and ending at T0+149 s,
with a duration (T90) of about 105 seconds.
The fluence in 100 - 1000 keV was (1.58 $B!^(B 0.07) x10-4 erg/cm2.
The 1-s peak flux measured from T0+65 s was 20.7 (-0.9, +0.8) photons/cm2/s
and 9.83(-0.36, +0.26) x10-5 erg/cm2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-5 s
to T0+149 s is well fitted by a single power-law with a photon index
of 2.32 $B!^(B 0.04 (chi2/d.o.f = 51/51).
The 1-s peak spectrum is well fitted by a power-law with exponential
cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha: 1.21 $B!^(B 0.13, and
Epeak: 623 (-39, +44) keV (chi2/d.o.f. = 41/50).

Due to the brightness of this burst, a 3% systematic error
was added for low energy channels.
All the quoted errors are at 90% confidence level,

The light curves for this burst are now available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB090617A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9569
SUBJECT: GRB 090617: Suzaku WAM observation of the prompt emission
DATE:    09/06/24 15:14:32 GMT
FROM:    Norisuke Ohmori at Miyazaki U  <ohmori@astro.miyazaki-u.ac.jp>

N. Ohmori, A. Daikyuji, E. Sonoda, K. Kono, H. Hayashi, K. Noda,  
Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa,
T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda,
T. Sugasahara (Saitama U.), Y. Urata (NCU),
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The short GRB 090617 (Fermi-GBM trigger 266907600 / 090617208;
Bissaldi et al., GCN 9523) triggered the Suzaku Wide-band All-sky 
Monitor (WAM) which covers an energy range of 50 keV - 5 MeV
at 04:59:58.105 UT (=T0).

The observed light curve shows a bright multi-peaked structure
starting at T0+0.45 s, ending at T0+0.6 s. 
The total T90 duration is about 0.14 seconds.

The fluence in 100 - 1000 keV was 8.8 (-5.9, +2.8)x10-7 erg/cm2.
The 1-s peak flux measured from T0 s was 1.7 (-1.0, +0.5) photons/cm2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0 s to T0+1 s is well fitted by a power-law with exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha       -0.02(-1.21, +1.07), and
  Epeak        698(+859, -171) keV (chi2/d.o.f. = 13.7/13).
 
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
 
The light curves for this burst is available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9570
SUBJECT: GRB 090618: Correction to GCN 9568
DATE:    09/06/24 15:47:37 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

K. Kono (Univ. of Miyazaki),
on behalf of the Suzaku WAM team, report:

There are some garbled characters and a wrong value reported
 in Kono et al. (GCN 9568).

The correct values are as follows:

1-s peak flux                :  9.83 (-0.36, +0.26) x 10^-6 erg/cm^2/s
The fluence in 100 - 1000 keV: (1.58 +/- 0.07) x 10^-4 erg/cm^2
The photon index
for time-averaged spectrum :    2.32 +/- 0.04
alpha for 1-s peak spsctrum:    1.21 +/- 0.13

We apologize for any inconvenience.


GRB_name: GRB090625A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9571
SUBJECT: GRB 090625: Fermi GBM detection
DATE:    09/06/25 14:15:33 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 05:37:00.21 UT on 25 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090625 (trigger 267601022  / 090625234).

The on-ground calculated location, using the GBM trigger
data, is RA = 20.3, DEC = -6.4 (J2000 degrees,
equivalent to 01 h 21 m, -06 d 24'), with an uncertainty
of 3.1 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 13 degrees.

The GBM light curve shows multiple weak pulses
with a duration (T90) of about 51 s (8-1000 keV).
The time-averaged spectrum from T0-6.144 s to T0+12.288 s is
well fit by a power law function with an exponential
high energy cutoff.  The power law index is -0.6 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 198 +/- 36 keV
(chi squared 551 for 579 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(8.8 +/- 1.2)E-07 erg/cm^2. The 4.096-sec peak photon flux measured
starting from T0+4.096 s in the 8-1000 keV band
is 0.50 +/- 0.02 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090625B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9572
SUBJECT: GRB 090625B: a long GRB localized by INTEGRAL
DATE:    09/06/25 14:18:54 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

D.Gotz (CEA-Saclay), S.Mereghetti, A.Paizis (IASF-Milano), A. Neronov, 
V.Beckmann, M. Beck (ISDC, Versoix), and J. Borkowski (CAMK, Torun) on 
behalf of the IBAS Localization Team report:

A long GRB with duration of about 11 s has been detected by IBAS in 
IBIS/ISGRI data at 13:26:21 UT on June 25th.

The refined coordinates (J2000)  are:

 RA:    2.2626 [degrees]
 DEC: -65.7816 [degrees]

with an uncertainty of 1.7 arcmin (90% c.l.).

A preliminary analysis gives a peak flux in the 20-200 keV range of  
about 2 ph/cmq/s (1 s integration time) and a fluence over the same energy
range of about  1.5e-6 erg/cmq.

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB090625B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9573
SUBJECT: GRB 090625B: Swift observation of the INTEGRAL GRB 090625B
DATE:    09/06/25 14:50:41 GMT
FROM:    David Burrows at PSU/Swift  <dxb15@psu.edu>

J. Mao (INAF-OAB), D. N. Burrows (PSU), E. A. Hoversten (PSU),
J. A. Kennea (PSU), K. L. Page (U Leicester), M. A. Stark (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

Swift executed a Target of Opportunity observation 
of the INTEGRAL GRB 090625B, slewing to the 
burst at 14:24 UT. 

XRT observations began at 14:30:13.  The observation begins too late 
after the burst for us to determine whether any sources in the field 
of view are fading.  However, we find a faint X-ray source located at
RA,Dec = 2.2618, -65.7803 which is equivalent to:

RA  (J2000) =  00 09 2.83
DEC (J2000) =  -65 46 49.2

with an uncertainty of 4.1 arcsec (radius, 90% containment). 

UVOT observations are being made, but data will not be available until
a ground downlink. 

Burst Advocate for this burst is J. Mao (jirong.mao AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090625B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9574
SUBJECT: GRB 090625B: Faulkes Telescope South observations
DATE:    09/06/25 17:20:34 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), D. Bersier (Liverpool JMU), P. O'Brien,
N. Tanvir (U. Leicester) on behalf of a large collaboration report:

On 2009 June 25 at 13:28:21 UT the 2-m Faulkes Telescope South
automatically began observing the INTEGRAL GRB 090625B
(Gotz et al., GCN Circ. 9572).

Observations started 120 seconds after the IBAS trigger time and
were performed using the B, V, R and i' filters. We could not find any
uncatalogued object inside the XRT error circle (Mao et al., GCN Circ.
9573) down to the following limiting magnitudes:

For single frames:

Mid Time   Exposure  Filter   Limit
  (s)       (s)              (mag)
-------------------------------------
141         3x10      R       > 19.3
526           10      i'      > 18.5
-------------------------------------

For coadded frames:

Time Range Exposure  Filter   Limit
  (min)     (s)               (mag)
-------------------------------------
22.5-45.2    420      R       > 21.0
25.4-48.2    420      i'      > 20.3
-------------------------------------

Calibration was performed using a few USNOB1 nearby stars, adopting
R2 and I values.


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9575
SUBJECT: GRB 090618: SARA Second Epoch Observations
DATE:    09/06/25 21:08:25 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria Updike, Sean Brittain, Dieter Hartmann (Clemson University), Andrew
Colson, Renata Cumbee, Brianne Hackett, Josiah Lewis, and Marten Kronberg
(SARA REU) report:

We re-observed the field of GRB 090618 (Schady et al., GCN 9512) using the
0.9m SARA telescope at Kitt Peak National Observatory beginning 20 hours
after the trigger and continuing for 3 hours.  Our observations consisted
of 45 sec exposures in the R and I bands under good conditions.  The
afterglow is detected in stacked images.  Magnitudes are given below as
compared to the USNOB.1 catalog.  Time is given in days after the trigger;
exposure time in seconds.

Time   Filter   Exp      Mag
------------------------------------
0.84     R      1215     19.4 +/- 0.1
0.86     I      1215     18.8 +/- 0.1


http://www.saraobservatory.org/


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9576
SUBJECT: GRB090618: HCT optical observations 
DATE:    09/06/25 21:41:30 GMT
FROM:    D.K. Sahu at Indian Inst of Astrophysics,Bangalore  <dks@iiap.res.in>

G.C. Anupama, U.K. Gurugubelli, D.K. Sahu  report

Optical afterglow of GRB090618 (Schady et al., GCN 9512) was observed
with the 2m.  Himalayan Chandra Telescope of the Indian Astronomical
Observatory, Hanle, India. The optical afterglow was observed in
Bessell R filter and it was detected in all the frames.

The preliminary magnitude of the optical afterglow, calibrated
using the USNO B1 (R1 magnitude) of the nearby  stars in the
GRB field is as under:
 Date         Mid UT    Exposure       R Mag     Error
 18-06-2009   19:29     300sec         18.70     0.07
 18-06-2009   19:36     300sec         18.75     0.06
 19-06-2009   22:08     2x300+450      20.30     0.09


GRB_name: GRB090623A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9577
SUBJECT: GRB 090623: Suzaku WAM observation of the prompt emission
DATE:    09/06/26 03:41:48 GMT
FROM:    Yujin E. Nakagawa at RIKEN  <yujin@crab.riken.jp>

Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, E. Sonoda,
K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka,
S. Sugita (Aoyama Gakuin U.), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.),
Y. Urata (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team,
report:

The long GRB 090623 (Fermi/GBM trigger 267417259 / 090623107, Rau et al.,
GCN 9566) was detected by the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 02:34:17.04 UT (=T0). The observed
light curve shows a multi-peaked structure lasting from T0-2 s, ending at
T0+48 s, with a duration (T90) of about 38 seconds. 

The fluence in 100 - 1000 keV was 2.7 (-0.9, +0.2) * 10^-5 ergs/cm^2.
The 1-s peak flux measured from T0+0.5 s was 5.3 (-1.2, +0.3) photons/cm^2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s to T0+48 s
is well fitted by a power-law with an exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha        1.0(-0.3, +0.3), and
  Epeak        601(-100, +147) keV (chi2^/d.o.f. = 15/18).
 
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
 
The light curves for this burst is available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090625B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9578
SUBJECT: GRB 090625B: GROND upper limits
DATE:    09/06/26 09:29:18 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler, F. Olivares, and J. Greiner (all MPE Garching) report on behalf
of the GROND team:

We observed the field of GRB 090625B (Gotz et al., GCN #9572)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPI/ESO telescope at La Silla Observatory
(Chile).

Observations started on 26 June 2009 at 03:58 UT, 14.5 hours after the
burst, continued until 05:58 UT and were performed under variable sky
conditions. In stacked images of 75 min total integration time in griz and
60 min in JHK, we do not detect any object within the XRT error circle
(Mao et al., GCN #9573), down to the following limiting magnitudes (all in
the AB system):

g' > 23.6
r' > 23.8
i' > 23.1
z' > 22.7
J  > 21.5
H  > 21.0
K  > 20.5

These upper limits were derived using USNO-B1 and 2MASS field stars as
reference. No correction has been made for the Galactic foreground
extinction corresponding to E(B-V) of 0.02 mag (Schlegel et al., 1998).


GRB_name: GRB090626A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9579
SUBJECT: GRB 090626: Fermi GBM detection
DATE:    09/06/26 11:26:22 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 04:32:08.88  UT on 26 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090626 (trigger 267683530  / 090626189).
The on-ground calculated location, using the GBM trigger data,
is RA = 169.3, DEC = -36.1 (J2000 degrees, equivalent to 11h 17m, -36d 06'),

with a statistical uncertainty of less than 1 degree 
(radius, 1-sigma containment) and an additional systematic error which 
is currently estimated to be 2 to 3 degrees. 
The angle from the Fermi LAT boresight is 15 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of four main peaks with a duration (T90) 
of about 70 s (8-1000 keV). The time-averaged spectrum from 
T0-0.256 s to T0+69.377 s is best fit by a Band function with 
Epeak = 175 +/- 12 keV, alpha = -1.29 +/- 0.02, and 
beta = -1.98 +/- 0.02 (chi squared 578 for 477 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(3.5 +/- 0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+1.024 s in the 8-1000 keV band 
is 17.9 +/- 1.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090625B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9580
SUBJECT: GRB 090625B: Swift-XRT refined analysis
DATE:    09/06/26 11:44:10 GMT
FROM:    Jirong Mao at INAF-OAB  <jirong.mao@brera.inaf.it>

J. Mao, R. Margutti (INAF-OAB) and C. Guidorzi (U. Ferrara) report
on behalf of the Swift-XRT team:

We have analyzed the first three orbit data (6.9 ks exposure) of the
Swift ToO observation of the INTEGRAL burst GRB 090625B (Gotz, GCN
Circ. 9572).

Swift-XRT observations started at 14:30:13 UT (Mao et al. GCN Circ. 9573),
4ks from trigger.

The source is fading with a best fit simple power law model index
of alpha= 0.6+/- 0.3, confirming its nature of X-ray afterglow.

A spectrum extracted from PC mode data can be modelled with an
absorbed power-law, with Gamma = 3.3 +1.1/-0.8 and NH = (3.7
+2.2/-1.7)x1021 cm^-2. The Galactic column in this direction is
2.1 x 1020 cm-2 (Kalberla et al. 2005).

The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 2.8 x 10-11 (1.8 x 10-10) erg cm-2 count-1.

If the light curve continues to decay with a power-law decay index of 0.6,
the count rate at T+24 hours will be 6.3x10-3 count s-1, corresponding to
an observed (unabsorbed) 0.3-10 keV flux of 1.8x10-13 (1.1x10-12) erg 
cm-2 s-1.

This circular is an official product of the Swift-XRT team.

[GCN OPS NOTE(26jun09): Per author's request, "Cristiano" was replaced
with "Guidorzi".]


GRB_name: GRB090625B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9581
SUBJECT: GRB 090625B: Swift/UVOT Upper Limits
DATE:    09/06/26 16:56:21 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/GSFC/USRA) and J. Mao (INAF-OAB)
report on the behalf of the Swift UVOT team:

       The Swift/UVOT observed the field of GRB 090625B starting 3679 s
after the INTEGRAL/IBAS detection (Gotz, et al., 2009, GCN
Circ. 9572).  We do not find any new source, relative to the DSS,
USNO-B1.0, or 2MASS at the position of the XRT afterglow (Mao, et
al. 2009, GCN Circ. 9573).  Preliminary 3-sigma upper limits for
detecting a source in the co-added images are

Filter   T_start    T_stop   Exp(s)      Mag
--------------------------------------------
v           3679      5007       318   >20.0
b           4192    11,398       413   >20.8
u           3987    67,218      6439   >21.7
uvw1        5218    17,045      1781   >21.5
uvm2        5012    16,139      1082   >21.0
uvw2        4602      4802       197   >20.1
white       3828      4596       344   >21.8
--------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.02 mag (Schlegel, et al., 1998, ApJS, 500,
525).  All photometry is on the UVOT photometry system described in
Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB090423A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9582
SUBJECT: GRB 090423:  Spitzer observations of the z~8.3 burst
DATE:    09/06/26 21:12:05 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

R. Chary, J. Surace, S. Carey (SSC/Caltech), E. Berger (Harvard), and G. 
Fazio (SAO/Harvard) report on behalf of a larger collaboration:

"As part of the IRAC Warm Instrument Characterization Campaign (IWIC), 
we observed the field of the z=8.3 GRB090423 (GCN 9198) for 72 hours 
using Spitzer/IRAC at 3.6 microns.  The observations took place between 
2009 June 5.01 and 10.81 UT, corresponding to about 46 days after the 
burst in the observer frame, or about 5 days in the rest-frame.  We 
detect a weak source at the location of the near-IR afterglow (Tanvir et 
al. 2009 arXiv:0906.1577), confirmed through an astrometric tie to the 
Gemini-North near-IR images.  Aperture-corrected photometry of the 
source results in a 3.6 micron flux density of 46+/-17 nJy (or 
27.2+/-0.3 AB mag).  The spectral energy distribution and power-law 
decay of the afterglow presented in Tanvir et al. 2009 predicts a 3.6 
micron flux density of ~27.3 AB mag at the time of our observations.  
The detected source is thus consistent with being the afterglow.

An image of the region can be found at:    
http://www.its.caltech.edu/~rchary/grb090423/

Light colors designate bright flux, dark colors are faint.  The pixel 
scale in the IRAC image (left) is 0.4"/pixel.  The right-hand image is 
the Gemini J-band image from Cucchiara et al. (GCN 9209).  The red 
circles are 1" radius and show the position of the afterglow.

Further analysis is ongoing, and a second epoch of observations is 
planned for February 2010 to assess the contribution of an
underlying host galaxy to the measured flux."


GRB_name: GRB090625B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9583
SUBJECT: GRB 090625B: Fermi GBM observation
DATE:    09/06/26 21:49:03 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 13:26:22.51  UT on 25 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090625B (trigger 267629184 / 090625560)
which was also detected by the INTEGRAL (Goetz et al. 2009, GCN 9572).
The GBM on-ground location is consistent with the INTEGRAL position.
 
The angle from the Fermi LAT boresight is 125 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 13.6 s (8-1000 keV).
The time-averaged spectrum from T0-2.048 s to T0+6.144 s is
well fit  by a power law function with an exponential
high energy cutoff.  The power law index is -0.9 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 165 +/- 28 keV
(chi squared 429 for 453 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(1.04 +/- 0.13)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+3.072 s in the 8-1000 keV band
is 1.87 +/- 0.09 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 424 for 454 
d.o.f.)
with Epeak= 100 +/- 32 keV, alpha = -0.4 +/- 0.5, and beta -2.0 +/- 0.2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090626A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9584
SUBJECT: Fermi LAT observations of GRB 090626
DATE:    09/06/28 19:08:13 GMT
FROM:    Valerie Connaughton at MSFC  <valerie@nasa.gov>

Fred Piron (LPTA), Francesco Longo (INFN/Trieste), 
Giulia Iafrate (INAF/OA Trieste), Teddy Cheung (NASA/GSFC), 
Hiro Tajima (SLAC) and Valerie Connaughton (UAH) report on 
behalf of the Fermi LAT collaboration:

Ground processing of data from the Fermi Large Area Telescope (LAT) 
reveals that the LAT significantly detects emission from GRB 090626, 
reported as a bright Fermi Gamma-ray Burst Monitor (GBM) burst (von 
Kienlin GCN 9579).

The LAT localization of this burst is RA, Dec = 170.01, -33.50  
0.32 deg (statistical, 95% CL), with an additional systematic error 
estimated at 0.1 deg.   There appears to be significant emission 
above 100 MeV until about 250 s after the GBM trigger time.  
Further information will be available following more detailed 
analysis.

The point of contact for this burst is Fred Piron 
(frederic.piron@lpta.in2p3.fr).

The Fermi LAT is a pair conversion telescope designed to cover the 
energy band from 20 MeV to greater than 300 GeV. It is the product of 
an international collaboration between NASA and DOE in the U.S. and 
many scientific institutions across France, Italy, Japan and Sweden.

This message can be cited.


GRB_name: GRB090628A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9585
SUBJECT: GRB 090628: Swift detection of a burst
DATE:    09/06/28 21:42:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU),
D. M. Palmer (LANL), B. Sbarufatti (INAF-IASFPA),
M. Stamatikos (NASA/ORAU) and M. A. Stark (PSU) report on behalf of
the Swift Team:

At 21:20:12 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090628 (trigger=355942).  Swift could not immediately 
slew to the burst.  The BAT on-board calculated location is 
RA, Dec 237.050, -15.977 which is 
   RA(J2000)  =  15h 48m 12s
   Dec(J2000) = -15d 58' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an Earth limb constraint, a prompt slew was not possible.  
Swift will execute a delayed slew after 2656 s.  No XRT or UVOT 
data will be available until the slew occurs. 

The series GCN Notices for this burst are corrupted 
with many (but not all) bogus values.  For the moment,
please disregard the original series of notices.  We may
issue Updated position notices when the information becomes available. 

Burst Advocate for this burst is V. Mangano (vanessa AT ifc.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090628A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9586
SUBJECT: GRB 090628: Swift XRT position
DATE:    09/06/28 23:04:34 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

B. Sbarufatti, V. Mangano (INAF-IASF PA)
report on behalf the Swift XRT team:

Analysis of preliminary data from the BAT trigger 355942 (GRB090628, 
Mangano, et al., GCN Circ 9585)
reveals an uncatalogued point source at RA, Dec = 237.05355, -15.98577 
which is equivalent to:

RA(J2000) = 15h48m12.85s
Dec(J2000) = -15:59:08.79

with an estimated uncertainty of 6.5 arcseconds radius (90% confidence).
Analysis is ongoing and an improved analysis will be reported as soon as
more data will be available.

This is an official product of the Swift XRT team.


GRB_name: GRB090628A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9587
SUBJECT: GRB 090628: Swift/UVOT Finding Chart Observation
DATE:    09/06/28 23:55:02 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten and V. Mangano (INAF-IASFPA) report on behalf of the Swift UVOT
team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 2790 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. The 2.7'x2.7' sub-image covers
100% of the XRT error circle. The typical 3-sigma upper limit has been about
19.6 mag. The 8'x8' region for the list of sources generated on-board covers
100% of the XRT error circle. The list of sources is typically complete to
about 18 mag. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.18.


GRB_name: GRB090626A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9588
SUBJECT: GRB 090626:  IPN localization
DATE:    09/06/29 03:20:25 GMT
FROM:    Valerie Connaughton at MSFC  <valerie@nasa.gov>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, and D. Svinkin on behalf of the 
Konus-Wind and Konus-RF teams, and T. Cline on behalf of the Konus-Wind
team,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, K. Makishima, and Y. Hanabata on behalf of the Suzaku-WAM 
team,

A. von Kienlin, G. Lichti, and A. Rau on behalf of the
INTEGRAL SPI-ACS GRB team,

K. Hurley, on behalf of the INTEGRAL and Odyssey teams,

J. Cummings, D. Palmer, H. Krimm, S. Barthelmy, and N. Gehrels on behalf 
of the Swift-BAT team,  and

V. Connaughton, M.S. Briggs and C.A. Meegan on behalf of the Fermi 
GBM team


report: 

Suzaku-WAM, Konus-Wind, Konus-RF, Swift-BAT, Odyssey-HEND,
and INTEGRAL-SPI-ACS observed the long GRB 
090626 at about 04:32:08 UT (corresponding to the Fermi/GBM
trigger 267683530/ 090626: von Kienlin, GCN 9579; also detected by 
Fermi/LAT: Piron et al., GCN 9584).  The burst was outside the 
coded field-of-view of the Swift BAT.

Triangulation gives various annuli which are shown in the 
figure at:

ftp://ftp.nsstc.org/outgoing/mbriggs/ipn_090626/GRB090626_IPN_v2.png.

The Konus-Wind-GBM annulus is centered at 
RA(2000)=257.678 (17h 10m 43s)  Dec(2000)=-27.309 (-27d 18' 34"), with a
radius of 73.391  0.246 deg (3 sigma).  The Konus-Wind-Odyssey
annulus is centered at RA(2000)=226.080 (15h 04m 19s) 
Dec(2000)=-16.554 (-16d 33' 13"), with a radius of 52.513  0.163 deg 
(3 sigma).

These annuli intersect to form the following 
3-sigma error box:

-----------------------------------------------
   RA(2000), deg               Dec(2000), deg
-----------------------------------------------
Center:
  170.419 (11h 21m 41s)   -33.051 (-33d 03' 04")
Corners:
  170.543 (11h 22m 10s)   -32.147 (-32d 08' 48")
  170.207 (11h 20m 50s)   -32.836 (-32d 50' 11")
  170.305 (11h 21m 13s)   -33.942 (-33d 56' 31")
  170.633 (11h 22m 32s)   -33.264 (-33d 15' 51")

-----------------------------------------------

The error box area is 0.363 sq. deg (1307.6 sq. arcmin).
This error box may be improved.


The box contains the LAT location (Piron et al., GCN 9584),
so that the IPN localization confirms the LAT location 
and narrows it to a much smaller region.

The Konus-Wind-GBM and Konus-Wind-Odyssey IPN triangulation 
map superimposed with the LAT location (95% CL 
error, statistical only) is available at 

ftp://ftp.nsstc.org/outgoing/mbriggs/ipn_090626/loc_090626_ipn_teeny.gif.

We encourage follow-up observations of the overlapping region 
between the IPN box and the LAT error circle.


GRB_name: GRB090628A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9589
SUBJECT: GRB 090628: 1.23m CAHA optical observations
DATE:    09/06/29 03:56:33 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

P. Kubanek (IAA-CSIC & GACE), N. Morales (IAA-CSIC), J.L. Ortiz
(IAA-CSIC), A. de Ugarte Postigo (ESO, INAF/OAB), J. Gorosabel (IAA-CSIC),
A.J. Castro-Tirado (IAA-CSIC), M. Jelinek (IAA-CSIC), report on behalf of
a larger collaboration:

We carried out R-band observations of the GRB 090628 XRT position
(Sbarufatti et al., GCN 9586) with the 1.23m Calar Alto telescope. The
observations were done on June 28.9486-29.0225 UT (1.43-3.20 hours post
GRB) with an exposure time of 3120s. A quick inspection of the XRT error
box reveals no object brighter than R ~ 22.


GRB_name: GRB090628A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9590
SUBJECT: GRB 090628: Enhanced Swift-XRT position
DATE:    09/06/29 08:00:55 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3973 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 090628, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 237.05272, -15.98489 which is equivalent
to:

RA (J2000): 15h 48m 12.65s
Dec (J2000): -15d 59' 05.6"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090628A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9591
SUBJECT: GRB 090628: GROND upper limits
DATE:    09/06/29 09:05:28 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler (MPE Garching), S. Klose (Tautenburg) and J. Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 090628 (Swift trigger #355942; Mangano et
al., GCN #9585) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla
Observatory (Chile).

Observations started at 02:06 UT on June 29th, 2009, 4.8 hr after the
burst and were performed under poor seeing conditions. In stacked images
of 75 min total integration time in griz and 60 min in JHK, we do not
detect any object within the enhanced XRT error circle (Goad et al., GCN
#9590), down to the following limiting magnitudes (all in the AB system):

g' > 23.7
r' > 24.0
i' > 23.0
z' > 22.8
J > 21.8
H > 21.1
K > 20.5

These upper limits were derived using the GROND zeropoints and 2MASS field
stars as reference and are not corrected for the Galactic foreground
extinction corresponding to a reddening of E(B-V)=0.18 mag (Schlegel et
al., 1998).

We note the presence of a r'~23.5 mag source ~5 arcsec north east of the
center of the enhanced XRT error circle, which given the large offset is
very unlikely to be related to the GRB.


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9592
SUBJECT: GRB090618: 15GHz radio emission faded
DATE:    09/06/29 11:26:44 GMT
FROM:    Guy Pooley at MRAO, Cambridge, UK  <ggp1@cam.ac.uk>

Further to GCN 9532, Guy Pooley (Cavendish Astrophysics, U. Cambridge)
reports on behalf of the AMI consortium that the radio emission 
at 15 GHz from GRB090618 has faded. 
Data from the AMI Large Array are given below, including data
taken on 090619 reported in GCN 9532:


yymmdd.ddd      hhmm-hhmm       S       rms
                   UT         microJy microJy 
090619.073      0245-0415       425     120
090619.208      0415-0545       640     120

090620.182      0340-0505       415      87
090621.275      0536-0736       139      91
090622.175      0328-0457        63      96

090627.021      0013-0048      -127     190

These results may be quoted in publications.


GRB_name: GRB090628A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9593
SUBJECT: GRB 090628: Swift-BAT refined analysis
DATE:    09/06/29 12:43:06 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+649 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090628 (trigger #355942)
(Mangano, et al., GCN Circ. 9585).  The BAT ground-calculated position is
RA, Dec = 237.038, -15.969 deg, which is 
   RA(J2000)  =  15h 48m 09.0s 
   Dec(J2000) = -15d 58' 09.0" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 63%.
 
The mask-weighted light curve shows a weak 1-sec wide precursor peak
at ~T-7.5 sec that then returns almost to background levels, and the
main peak starting at ~T-0.3 sec, peaking at ~T+1 sec, and ending 
at ~T+6 sec.  T90 (15-350 keV) is 20.1 +- 4.6 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-25.0 to T+4.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.20.  The fluence in the 15-150 keV band is 7.0 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.05 sec in the 15-150 keV band
is 1.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/355942/BA/


GRB_name: GRB080628A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9594
SUBJECT: GRB080628: SAO RAS optical observations
DATE:    09/06/29 13:24:31 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. Moskvitin, O. Spiridonova, A. Valeev, T. Fatkhullin (SAO RAS, Niznijh
Arkhyz, Russia), on behalf of a larger collaboration, report:

We observed the field of GRB 090628 (Mangano et al., GCN #9585) in Rc
band (14 x 60 seconds) with the Zeiss-1000 telescope of SAO RAS
(Russia). The observations were carried out at high air mass. We did
not detect any object within the enhanced XRT error circle (Goad et al.,
GCN #9590) down to the limiting magnitude 19.3 (according to nearby
USNO-B1 stars). The average time of observations is 22:23:16 UT,
1.05 hours after the trigger.

This message can be cited.


GRB_name: GRB090626A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9595
SUBJECT: Konus-Wind observation of GRB 090626
DATE:    09/06/29 14:12:22 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long bright GRB 090626 localized by IPN and Fermi/LAT (Golenetskii 
et al., GCN 9588; Piron et al., GCN 9584; corresponding to the Fermi/GBM
trigger 267683530: von Kienlin, GCN 9579) triggered Konus-Wind at 
T0(KW)=16330.962 s UT (04:32:10.962) and Konus-RF at T0(KRF)=16332.013 s 
UT (04:32:12.013).

The burst light curve shows a multipeaked structure with a duration of
~60 s

As observed by Konus-Wind the burst
had a fluence of 7.78(-1.01, +0.91)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0+21.056 s
of 1.41(-0.25, +0.24)x10^-5 erg/cm2/s
(both in the 20 keV - 7 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+61.696 s) can be fitted (in the 20 keV - 7 MeV
range) by GRB (Band) model for which:
the low-energy photon index alpha = -1.26(-0.08, +0.09),
the high energy photon index beta = -2.43(-0.54, +0.20),
the peak energy Ep = 202(-24, +29) keV (chi2 = 98.7/78 dof).

All the quoted errors are at the 90% confidence level.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.ru/LEA/GRBs/GRB090626_T16332/


GRB_name: GRB090628A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9596
SUBJECT: GRB 090628: Swift/UVOT Upper Limits
DATE:    09/06/29 22:59:56 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU) and V. Mangano (INAF-IASFPA) report on behalf
of the Swift/UVOT team.

The Swift/UVOT began observing the field of GRB 090628 2790s after
the BAT trigger (Mangano et al., GCN Circ. 9585).  Data summed
from the first orbit does not reveal a source at the refined
position of the X-ray afterglow (Goad et al., GCN Circ.
9590).

The 3-sigma upper limits for the finding chart (fc) and
summed exposures are reported below:

FILTER     T_start(s)  T_stop    Exposure     Mag/3UL
=============================================================
white fc     2791       2941        147       > 20.26
white        3361       3560        196       > 20.72

v            3771       3971        196       > 19.23

b            3155       3355        196       > 20.16
b            4591       4672         79       > 19.64

u            2950       3149        196       > 19.63
u            4386       4586        196       > 19.82

uvw1         4181       4381        196       > 19.65

uvm2         3976       4176        196       > 19.33

uvw2         3566       3766        196       > 19.62
=================================================================

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.05 (Schlegel et al.,
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9597
SUBJECT: GRB 090618: RTT150 optical observations
DATE:    09/06/30 14:12:04 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

I. Khamitov, M. Parmaksizoglu, T. Ak, Z. Eker (TUG),
Z. Aslan (Kultur Uni.), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Bikmaev, N. Sakhibullin (KSU/AST),

report:

We observed the OT (Schady et al., GCN 9512; Cenko et al., GCN 9513; 
Perley, GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK 
National Observatory, Turkey), in Rc band during three nights 25,26 and 27 
June 2009 and in B band in 26 June.

Every night we made 3x900s exposures in Rc band and in 26 June we made 
additionally 3x900 in B band. The OT is detected in all stacked images in 
Rc. The brightness of OT is not changed inside of photometric error.
Our preliminary estimate of its magnitude during these observations is
m_Rc=22.3+/-0.1 (7.68, 8.64, 9.58 days after the burst).

We found no OT on stacked B-image. The limiting magnitude of the frame is 
mlim_B=23.4 (8.68 days after the burst).


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GRB_name: GRB090630A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9598
SUBJECT: GRB 090630: Fermi GBM detection
DATE:    09/06/30 15:11:20 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 07:27:21.17 UT on 30 June 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090630 (trigger 268039643 / 090630311).

The on-ground calculated location, using the GBM trigger
data, is RA = 146.6, DEC = -46.6 (J2000 degrees,
equivalent to 09 h 24 m, -46 d 36 '), with an uncertainty
of 5.8 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 75 degrees.

This burst was also detected (although not triggered) by INTEGRAL SPI-ACS.

The GBM light curve consists of a single peak
with a duration (T90) of about 5.1 s (8-1000 keV).
The time-averaged spectrum from T0-1.024 s to T0+4.096 s is
best fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.5 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 79 +/- 13 keV
(chi squared 537 for 475 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(5.1 +/- 0.7)E-07 erg/cm^2. The 2.048-sec peak photon flux measured
starting from T0+0.003 s in the 8-1000 keV band
is 2.78 +/- 0.05 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 535 for 474 
d.o.f.)
with Epeak= 71 +/- 24 keV, alpha = -1.5 +/- 0.2 and beta = -2.3 +/- 0.4.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090628A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9599
SUBJECT: GRB 090628: Swift XRT refined analysis
DATE:    09/06/30 15:35:22 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano, B. Sbarufatti (INAF-IASF PA) report on behalf
the Swift XRT Team:

We have analyzed 19 ks of PC data of the candidate X-ray
afterglow of GRB 090628 (Mangano et al, GCN Circ. 9585)
spanning the time interval from T+2796 s to T+101.7 ks.

The best position available for the source is the
enhanced Swift-XRT position from Goad et al. (GCN Circ. 9590):
RA, Dec = 237.05272, -15.98489 which is equivalent to

RA (J2000): 15h 48m 12.65s
Dec (J2000): -15d 59' 05.6"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

The 0.3-10 keV XRT light curve shows an initial flat or rising
phase followed by a steep decay. The best fit with a broken
power-law model is insensitive to the initial rise slope,
of the order of 0.4, possibly consistent with zero,
and provides a break at 14+/-4 ks after the trigger
and a post-break decay slope of -1.3+/-0.3.
The source is rather faint, and at this rate it will
reach a level of 8.0e-4 counts/s at T+48 hours.
All quoted errors are at the 90% confidence level.

The average spectrum can be fitted by an absorbed
power-law model with Cash statistics. Best fit spectral
parameters are NH < 2.0e21 cm^-2 (consistent with Galactic
absorption of 8.7e20 cm^-2, Kalberla et al. 2005)
and photon index = 1.4 +/- 0.3 (Cstat(dof): 87.6(113)).
The 0.3-10 keV observed(unabsorbed) average flux is
5.0e-13(5.5e-13) erg cm^-2 s^-1.

The rate to flux conversion factor is 8.0e-11.

The results of the XRT team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00355942

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090701A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9600
SUBJECT: GRB 090701: Fermi GBM detection
DATE:    09/07/01 15:43:49 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

Sheila McBreen (UCD/MPE)
reports on behalf of the Fermi GBM Team:

"At 05:23:55.84 UT on 01 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090701 (trigger 268118637 / 090701225).

The on-ground calculated location, using the GBM trigger
data, is RA = 114.7, DEC = -42.1 (J2000 degrees,
equivalent to 07 h 39 m, -42 d 06 '), with an uncertainty
of 4.2 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 13 degrees.

The GBM light curve comprises one pulse
with a duration (T90) of about 12 s (8-1000 keV).
The time-averaged spectrum from T0-10 s to T0+2 s is
adequately fit by  a simple power law function
with index 1.84 +/- 0.09 (chi squared 440 for 485 d.o.f.).

The event fluence (8-1000 keV) in this time interval is about
4.5E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.024 s in the 8-1000 keV band
is 2.1 +/- 0.1 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9601
SUBJECT: GRB 090404: Deep optical imaging and possible host association
DATE:    09/07/02 06:33:36 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, S. B. Cenko, and J. S. Bloom (UC Berkeley) report:

We imaged the field of dark gamma-ray burst GRB 090404 (Ziaeepour et 
al., GCN 9086) using the Keck I telescope (+LRIS) on the night of 
2009-06-25 (UT) for 1670 seconds in g-band and 1560 seconds in I-band 
under excellent (0.5 arcsecond) seeing and photometric conditions.

The object outside the XRT error circle mentioned by Malesani et al. 
(GCN 9093, GCN 9095) is clearly detected as an extended source, likely a 
moderate-redshift galaxy (hereafter "G1").  A second, slightly fainter 
extended source ("G2") is also detected 3.5 arcseconds to its northeast, 
and the two sources appear to be connected by faint emission, perhaps a 
tidal bridge.  Both sources are marginally detected in Sloan Digital Sky 
Survey archival images (see also GCN 9096).

Additional faint, extended emission is detected just west of the 
brighter galaxy G1.  The emission appears to be spread over several 
arcminutes in the g-band image, with an obvious "knot" located 1 
arcsecond northeast of the millimeter afterglow position reported by 
Catro-Tirado et al. (GCN 9100).  The extended region itself passes 
directly through the millimeter position.  A false-color image of the 
field, with the millimeter and enhanced XRT positions 
(http://www.swift.ac.uk/xrt_positions/00348428/image.php) superimposed, 
is posted to: http://lyra.berkeley.edu/~dperley/090404/090404_gI.png

We hypothesize that the extended emission may be a tidal tail extending 
from G1 as a result of interaction with its northeastern neighbor. 
Alternatively, the extended region may represent a very faint background 
host galaxy.  Aperture photometry at the location of the millimeter 
afterglow gives a magnitude of g = 27.3 +/- 0.2.

We encourage spectroscopy of the two bright galaxies G1 and G2 to 
determine their redshifts.


GRB_name: GRB090404A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9602
SUBJECT: GRB 090404: Deep optical imaging and possible host association (correction)
DATE:    09/07/02 07:38:53 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley (UC Berkeley) reports:

In the third paragraph of the previous circular (GCN 9601), the 
reference to the extended emission possibly associated with G1 being 
spread over several "arcminutes" should instead read that the emission 
is spread over several arcseconds.

A g-band thumbnail image showing this emission (and the nearby "knot") 
more clearly is posted to: 
http://lyra.berkeley.edu/~dperley/090404/090404_g.png


GRB_name: GRB090313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9606
SUBJECT: GRB 090313: optical observations
DATE:    09/07/03 10:53:29 GMT
FROM:    Graziella Pizzichini at IASF/CNR,Bologna  <pizzichini@iasfbo.inaf.it>

   E. Maiorano, G. Pizzichini (INAF/IASF Bologna), C. Bartolini, G. Greco,
   A. Guarnieri, A. Mantegna, A. Piccioni (Bologna University),
   D. Nanni (INAF/OAR and Second University of Rome "Tor Vergata"),
   F. Terra (Second University of Roma "Tor Vergata"), R. Gualandi
   (Bologna Observatory) report:

    During the night between 09/03/13 and 09/03/14 we observed the OT of
    GRB090313 (Chornock et al., GCN 8979, Mao et al., GCN 8980) with the
    1.52 cm telescope of the Bologna Observatory in Loiano. Airmass 1.24
    and seeing less than 2" .
    Observations were disturbed by the moon. The images were calibrated
    using the star quoted by Guidorzi et al.,  GCN 8989.
    By summing 9 images in filter R, with a total duration of 2280s
    obtained on March 14 between 00:41:11 and 01:27:59 UT, (mid exposure
    time 15.97 hr after the burst) we find R mag = 19.26 +/- 0.15

    Our  image has been posted in our public directory
    from where it can be retrieved by sftp using
    sftp publicGRB@137.204.66.221
    password: GRB_bo
    cd GRB090313


GRB_name: GRB090702A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9607
SUBJECT: GRB 090702: UVOT upper limits
DATE:    09/07/03 11:13:55 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and D. M. Palmer (LANL) report on behalf of the  
Swift/UVOT team:

The Swift/UVOT began observing the field of INTEGRAL GRB 090702,  
3.5hrs after the
INTEGRAL trigger (Paizis et al., GCN 9603). We do not detect any  
source at the
Swift XRT position (Sbarufatti et al. GCN 9604).

The 3-sigma upper limits for the finding chart exposure is:

Filter   T_start(s)   T_stop(s)   Exp(s)  Mag (3-sigma upper limit)
-------------------------------------------------------------
white      14080       20350        971     > 22.72
v          14646       20964       1126     > 21.20
b          13516       25451       1753     > 22.37
u          12951       24855       1796     > 21.89
-------------------------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.039 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).


GRB_name: GRB090703A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9608
SUBJECT: GRB 090703: Fermi GBM detection
DATE:    09/07/03 17:04:48 GMT
FROM:    Elisabetta Bissaldi at MPE  <ebs@mpe.mpg.de>

Elisabetta Bissaldi (MPE) reports on behalf of the Fermi GBM Team:


"At 07:54:02.48 UT on 03 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090703 (trigger 268300444 / 090703329).
The on-ground calculated location, using the GBM trigger data, 
is RA =  0.8, DEC = 9.7 (J2000 degrees, equivalent to 
00h 03m, 09d 42'), with an uncertainty of 5.3 degrees 
(radius, 1-sigma containment, statistical only; there is 
additionally a systematic error which is currently 
estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 25 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 9 s (8-1000 keV).
The time-averaged spectrum from T0-2.6 s to T0+6.7 s is
adequately fit by a simple power law function with
index -1.72 +/- 0.06 (Castor C-stat 232 for 240 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(6.8 +/- 0.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0 in the 8-1000 keV band is 1.00 +/- 0.10 ph/s/cm^2.


The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090529A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9610
SUBJECT: GRB 090529: Mt.Terskol optical observations
DATE:    09/07/03 22:10:53 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy),  A.
Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:

We report a photometry of  the optical afterglow (Xin et al. GCN 9431) of 
the Swift GRB 090529 (Sakamoto et al. GCN 9430) observed with the Z-600 
telescope of Mt.Terskol observatory in R-filter (Andreev et al, GCN 9437). 
The photometry is based on reference star USNO-B1.0  1144-0210607 (J2000) 
14 09 58.32 +24 27 35.6), assuming R=16.46:

T0+     Filter, Exposure, mag.,
(d)             (s)

0.2420 R 20x120  21.13 +/- 0.2 


GRB_name: GRB090529A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9611
SUBJECT: GRB 090529: MTM-500 optical observations 
DATE:    09/07/03 22:16:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU), K. Naumov, V. Kouprianov, A. Devyatkin (Pulkovo 
Observatory), A. Pozanenko (IKI)  report on behalf of larger GRB follow-up 
collaboration:

We observed   the field of the Swift GRB 090529  (Sakamoto et al. GCN 9430) 
with MTM-500 (0.5m) telescope of  Kislovodsk solar station (43d 44.77' N, 
42d 31.42' W) of the Pulkovo observatory  in two series in R-filter starting 
May 29 (UT) 19:58. We do not detect optical afterglow
(Xin et al. GCN 9431). The upper limits  of combined images based on 
USNO-B1.0 are following:

T0+     Filter, Exposure, mag.,
(d)             (s)

0.2817   R       60x60     > 19.3
0.3324   R       55x60     > 19.4


GRB_name: GRB090529A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9612
SUBJECT: GRB 090529: CrAO optical upper limit
DATE:    09/07/03 22:27:56 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

D. Shakhovkoy, V. Rumyantsev (CrAO), A. Pozanenko (IKI)  report on behalf of 
larger GRB  follow-up collaboration:

We observed the field of the Swift GRB 090529 (Sakamoto et al. GCN 9430) 
with AZT-11 telescope of CrAO between (UT) May 29  18:41 -- 19:42 under poor 
weather conditions. We do not detect optical afterglow (Xin et al. GCN 
9431). Upper limit of a stacked image based on USNO-B1.0 star  (RA=14 09 
47.65 Dec=+24 27 44.30) assuming I=17.54  is following:

T0+      Filter, Exposure, mag.
(d)              (s)

0.2075   I       20x180    > 20.3 


GRB_name: GRB090618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9613
SUBJECT: GRB 090618: Mondy optical observations
DATE:    09/07/04 00:32:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Klunko (ISTP), A. Volnova (SAI MSU), A. Pozanenko (IKI) on behalf of 
larger GRB follow up collaboration  report:

We observed the afterglow (Schady  et al., GCN 9512; Cenko et al., GCN 9513; 
Perley, GCN 9514; Rujopakarn et al., GCN 9515) of  the Swift GRB 090618 
between  (UT) Jun. 18  18:14 -- 18:43  with 1.5m telescope of Sayan 
observatory (Mondy).   The afterglow is  detected in stacked images. 
Preliminary photometry of the stacked images based on USNO-B1.0 star
1683-0077955 (RA=19 36 36.34   Dec=+78 21 07.00) assuming R=16.57  is 
following:

T0+     Filter, Exposure, mag.,     err.
(d)             (s)

0.4083   R       10x30     18.60 +/-0.10


GRB_name: GRB090705A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9615
SUBJECT: GRB 090705: Swift detection of a possible burst
DATE:    09/07/05 05:36:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (GSFC/GWU), S. D. Barthelmy (GSFC), V. D'Elia (ASDC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), C. Pagani (PSU),
D. M. Palmer (LANL), M. Perri (ASDC), T. Sakamoto (NASA/UMBC),
M. H. Siegel (PSU), M. A. Stark (PSU) and G. Stratta (ASDC) report on
behalf of the Swift Team:

At 05:11:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located possible GRB 090705 (trigger=356516).  Swift slewed almost 
immediately to the location.  The BAT on-board calculated location is 
RA, Dec 318.484, +62.578 which is 
   RA(J2000) = 21h 13m 56s
   Dec(J2000) = +62d 34' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for an image trigger, there is
no obvious variation in the immediately available light curve. 

The XRT began observing the field at 05:17:25.8 UT, 354.7 seconds after
the BAT trigger. No source was detected in the promptly available XRT
data. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 357 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.83. 

Due to the marginal detection (7.02 sigma) in the BAT image, and
the non-detection by XRT, we cannot confirm that this is a real burst. 
Further analysis will require the full downlink of data through
the Malindi ground station. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090705A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9616
SUBJECT: GRB 090705: PAIRITEL NIR Observations
DATE:    09/07/05 07:54:54 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, B. E. Cobb, S. B. Cenko,  J. S. Bloom, (UC Berkeley), report:

We observed the field of the possible GRB 090705 (Ukwatta et al., GCN
9615) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona.
Observations began at 2009-07-05 05:44:53 UT, ~33 minutes after the
Swift trigger.  In preliminary mosaics (effective exposure time of
~450 seconds) taken simultaneously in the J, H, and Ks filters, we
detect no new sources inside the BAT error circle down to the 2MASS
limits.


GRB_name: GRB090705A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9617
SUBJECT: Possible GRB090705: Swift-XRT observations
DATE:    09/07/05 13:25:13 GMT
FROM:    Valerio D'Elia at INAF-OAR  <delia@oa-roma.inaf.it>

V. D'Elia, M. Perri (ASDC), T.N. Ukwatta (GSFC/GWU) report on behalf
of the Swift-XRT team:

We analyzed the first 2.9 ks of the XRT data for the possible GRB 090705
(Ukwatta et al., GCN Circ. 9615). Data are in Photon Counting (PC) mode
and start ~6 minutes after the BAT trigger.
No source is detected within or near to the BAT error circle. The 3-sigma
upper limit on the count rate is 0.005 count s-1, corresponding to an
approximate observed 0.3-10 keV flux of 2.5x10-13 erg cm-2 s-1 (using a
standard counts to flux conversion factor).

This circular is an official product of the Swift-XRT team.

-------------------------------------------------
This mail sent through IMP: http://horde.org/imp/


GRB_name: GRB090706A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9619
SUBJECT: GRB 090706: Fermi GBM detection
DATE:    09/07/06 15:06:24 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 06:47:40.43  UT on 06 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090706 (trigger 268555662 / 090706283).

The on-ground calculated location, using the GBM trigger
data, is RA = 205.1, DEC = -47.1 (J2000 degrees,
equivalent to 13 h 40 m, -47 d 06 '), with an uncertainty
of 3.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 20 degrees.

The GBM light curve consists of two peaks
with a duration (T90) of about 100 s (8-1000 keV).
The time-averaged spectrum from T0-34.8s to T0+7.2 s is
adequately fit by a simple power law function with index -2.16 +/- 0.09
(chi squared 410 for 339 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(1.5 +/- 0.1)E-06 erg/cm^2. The 4-sec peak photon flux measured
starting from T0-30.7 s in the 8-1000 keV band
is 1.24 +/- 0.05  ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090704A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9620
SUBJECT: GRB 090704: a long GRB found in INTEGRAL off-line analysis
DATE:    09/07/07 16:23:44 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

S.Mereghetti, A.Paizis (IASF-Milano), D.Gotz (CEA-Saclay), C. Ferrigno, M. 
Beck (ISDC, Versoix), and J. Borkowski (CAMK, Torun) on behalf of the IBAS 
Localization Team report:

During an off-line analysis of low significance IBAS triggers we found a 
long GRB detected in IBIS/ISGRI data at 05:47:43 UT on July 4th.  The 
burst had a duration of about 60 s.

The burst coordinates (J2000)  are:

 RA:    208.205 [degrees]
 DEC:    22.790 [degrees]

with an uncertainty of 1.7 arcmin (1 sigma c.l.).

The peak flux in the 20-200 keV range was about 2 ph/cmq/s (1 s 
integration time) and the fluence over the same energy range about 6e-6 
erg/cmq.

The low significance of the IBAS trigger, below the threshold for 
automatic alert delivery, was due to the very large off-axis angle of 
about 14 degrees.

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB090708A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9621
SUBJECT: GRB 090708: Swift detection of a burst
DATE:    09/07/08 03:48:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. Rowlinson (U Leicester),
T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), M. A. Stark (PSU),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:

At 03:38:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090708 (trigger=356776).  Swift did not slew because of 
Sun constraint.  The BAT on-board calculated location is 
RA, Dec 154.629, +26.637 which is 
   RA(J2000)  =  10h 18m 31s
   Dec(J2000) = +26d 38' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows single peak
with a duration of about 20 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to an observing constraint, Swift cannot slew to the BAT position,
and it will not be observable until early October. 
There will thus be no XRT or UVOT data for this trigger. 

Burst Advocate for this burst is H. A. Krimm (krimm AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090708A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9622
SUBJECT: GRB 090708: ROTSE-III Optical Limits
DATE:    09/07/08 03:58:49 GMT
FROM:    Fang Yuan at ROTSE  <yuanfang@umich.edu>

F. Yuan (U Mich), E.S. Rykoff (UCSB), H. Flewelling (IfA/Hawaii), T.  
Guver (U Arizona), S. B. Pandey (U Mich), W. Rujopakarn (Steward),  
report on behalf of the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB  
090708 (Swift trigger 356776; Krimm et al., GCN 9621), producing  
images beginning 7.4 s after the GCN notice time. An automated  
response took the first image at 03:39:04.5 UT, 49.2 s after the  
burst, under fair conditions. We took 10 5-sec, 10 20-sec and 10 60- 
sec exposures. These unfiltered images are calibrated relative to USNO  
A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the  
3-sigma Swift/BAT error circle, for both single images and coadding  
into sets of 10. Individual images have limiting magnitudes ranging  
from 14.8-16.1; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
03:39:04.5   03:39:09.5         5     15.0           49.2       N
03:39:04.5   03:40:11.6        67     16.6           49.2       Y
03:40:27.8   03:45:35.8       308     17.4          132.5       Y


GRB_name: GRB090708A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9623
SUBJECT: GRB 090708, Swift-BAT refined analysis
DATE:    09/07/08 14:26:44 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC/UMD), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
T. N. Ukwatta (GWU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 090708 (trigger #356776)
(Krimm, et al., GCN Circ. 9621).  The BAT ground-calculated position is
RA, Dec = 154.632, 26.616 deg which is
   RA(J2000)  =  10h 18m 31.7s
   Dec(J2000) = +26d 36' 58.7"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 27%.

The main pulse began at T-2 sec, peaked at ~T+4 sec and decayed by
~T+16 sec. There is a hint of some low-level emission out to ~T+100 sec.
At T+160 sec, a pre-planned slew took the burst out of the BAT field of
view. T90 (15-350 keV) is 15.0 +- 3.9 sec (estimated error including 
systematics).

The time-averaged spectrum from T-1.3 to T+17.7 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.78 +- 0.22.  The fluence in the 15-150 keV band is
6.9 +- 1.0 x 10-7 erg/cm2. The 1-sec peak photon flux measured from
T+3.37 sec in the 15-150 keV band is 1.3 +- 0.3 ph/cm2/sec.  All the
quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/356776/BA/


GRB_name: GRB090708A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9624
SUBJECT: GRB 090708: Early RAPTOR Optical Limits
DATE:    09/07/08 20:31:21 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis, B. Norman
of Los Alamos National Laboratory report:

The RAPTOR telescope system responded to Swift trigger
356776 (Krimm et al., GCN 9621) under good observing conditions.
A nearly full moon was above the horizon at the time of the
observations, limiting sensitivity.  Our narrow-field instruments
began observing the location at 03:39:05.87 UTC, 50.62 s after
the Swift trigger (6.9 s after receipt of GCN message).  The data
from our R-band filtered system was calibrated to the USNO-B1
catalog.  These data show no new source within the BAT error
circle (Palmer et al., GCN 9623) when compared to the DSS.  We
can put the following R-band (Cousins) limits on the emission:

t-mid(s)          exp(s)   mag    mag-err
[since trigger]
----------------------------------------------------
61.59             5.0      16.2   3 sigma limit
101.85           30.0      17.3   3 sigma limit


GRB_name: GRB090709A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9625
SUBJECT: GRB 090709: Swift detection of a bright burst
DATE:    09/07/09 08:07:08 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. C. Morris (PSU), A. P. Beardmore (U Leicester),
P. A. Evans (U Leicester), H. A. Krimm (CRESST/GSFC/USRA),
V. Mangano (INAF-IASFPA), J. Mao (INAF-OAB),
C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. Rowlinson (U Leicester), M. H. Siegel (PSU),
M. A. Stark (PSU), G. Tagliaferri (INAF-OAB),
T. N. Ukwatta (GSFC/GWU) and H. Ziaeepour (UCL-MSSL) report on behalf
of the Swift Team:

At 07:38:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090709 (trigger=356890).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 289.933, +60.731 which is 
   RA(J2000) = 19h 19m 44s
   Dec(J2000) = +60d 43' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed about four major
peaks starting at T-20 and continuing to T+100 seconds. The peak 
count rate was ~15000 counts/sec (15-350 keV), at ~25 sec after the trigger. 

The XRT began observing the field at 07:39:42 UT, 67.8 seconds after the BAT
trigger. In the 2.5-s image-mode data we find a fading, uncatalogued X-ray
source with a position: RA, Dec 289.9291, +60.7271 which is equivalent to:
   RA(J2000)  = 19h 19m 42.99s
   Dec(J2000) = +60d 43' 37.5"
with an uncertainty of 4 arcseconds (radius, 90% containment). This
location is 16 arcseconds from the BAT onboard position, within the BAT
error circle. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 76 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The overlap of the sub-image and the
XRT error circle is 100%. The overlap of the 8'x8' region for the list of
sources generated on-board and the XRT error circle is 100%. No correction
has been made for the expected extinction corresponding to E(B-V) of 0.09. 

Burst Advocate for this burst is D. C. Morris (morris AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9626
SUBJECT: GRB 090709: ROTSE-III Optical Limits
DATE:    09/07/09 08:32:56 GMT
FROM:    Fang Yuan at ROTSE  <yuanfang@umich.edu>

S. B. Pandey (U Mich), W. Rujopakarn (Steward), H. Flewelling (IfA/ 
Hawaii), F. Yuan (U Mich), B. E. Schaefer (Louisiana State), report on  
behalf of the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB  
090709 (Swift trigger 356890; Morris D. C., GCN 9625), producing  
images beginning 5.6 s after the GCN notice time. An automated  
response took the first image at 07:39:00.6 UT, 26.0 s after the  
burst, and during the gamma-ray emission, under good conditions. We  
took 10 5-sec and 50 20-sec exposures. These unfiltered images are  
calibrated relative to USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the  
3-sigma Swift/BAT error circle or the XRT error circle, for both  
single images and coadding into sets of 10. Individual images have  
limiting magnitudes ranging from 16.4-17.2; we set the following  
specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
07:39:00.6   07:39:05.6         5     16.5           26.0       N
07:39:00.6   07:40:07.7        67     17.8           26.0       Y
07:40:20.2   07:45:02.4       282     18.2          105.6       Y


GRB_name: GRB090704A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9627
SUBJECT: GRB 090704: Fermi GBM observation
DATE:    09/07/09 08:46:35 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

S. McBreen (UCD/MPE)
reports on behalf of the Fermi GBM Team:

"At 05:47:48.18 UT on 04 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090704 (trigger 268379270 / 090704242)
which was also detected by IBIS/ISGRI
(Mereghetti et al. 2009, GCN 9620).
The GBM on-ground location is consistent with the ISGRI position.
The angle from the Fermi LAT boresight is 77 degrees.

The GBM light curve consists of one main pulse
with a duration (T90) of about 70 s (8-1000 keV).
The time-averaged spectrum from T0-0 s to T0+70 s is
well fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.13 (+0.07)
and the cutoff energy, parameterized as Epeak,
is 233.7 (+37.6/-28.5) keV (chi squared 358 for 365 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(5.8 +/- 0.3)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+14.3 s in the 8-1000 keV band
is  1.2 +/- 0.1 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090709A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9628
SUBJECT: GRB 090709: PAIRITEL NIR Upper Limits
DATE:    09/07/09 08:58:46 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, C. R. Klein, D. A. Perley, J. S. Bloom, (UC Berkeley), report:

We observed the field of GRB 090709 (Morris et al., GCN 9625) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2009-07-09 07:40:22 UT, ~108 seconds after the Swift trigger.  In
preliminary mosaics (effective exposure time of ~374 seconds) taken
simultaneously in the J, H, and Ks filters, we detect no source at the
XRT position.

The preliminary photometry yields:

post_burst
t_mid(s) exp(s)  filt  U. Limit (3 sig)
438       374     J     > 17.7
438       374     H     > 16.9
438       374     Ks    > 15.3

All magnitudes given in the Vega system, calibrated to 2MASS.  No
correction for Galactic extinction has been made to the above reported
values.  Observations are ongoing.

[GCN OPS NOTE(09jul09): Per author's request, in the Subject line
the "090609" was changed to "090709".]


GRB_name: GRB090626A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9629
SUBJECT: GRB 090626: Suzaku WAM observation of the prompt emission
DATE:    09/07/09 09:00:05 GMT
FROM:    Kazuhiro Noda at Miyazaki U  <kaz1206@astro.miyazaki-u.ac.jp>

K. Noda, E. Sonoda, M. Yamauchi, N. Ohmori, H. Hayashi,
K. Kono, A. Daikyuji, Y. Nishioka (Univ. of Miyazaki),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda,
T. Sugasahara (Saitama U.), Y. Urata (NCU),
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa,
T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.),
on behalf of the Suzaku WAM team, report:


The long GRB 090626 (Fermi/GBM trigger 267683530 / 090626189 ; A. von Kienlin et al.,
GCN 9579) triggered the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 04:32:09 UT (=T0). The observed
light curve shows a multi-peaked structure lasting from T0-2 s, ending at
T0+65 s, with a duration (T90) of about 45 seconds.

The fluence in 100 - 1000 keV was 3.60 (-0.07, +0.22) x10-5 erg/cm2.
The 1-s peak flux measured from T0+2 s was 10.51 (-0.76, +0.67)
photons/cm2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-2s to T0+65s is well fitted by a power-law with exponential cutoff model:
  dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha 1.76(-0.18, +0.17), and
  Epeak 270(-79, +63) keV (chi2/d.o.f. = 26/22).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst will be available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090709A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9630
SUBJECT: GRB 090709: Faulkes Telescope North Upper Limits
DATE:    09/07/09 09:35:32 GMT
FROM:    Zach Cano at ARI/John Moores Liverpool  <zec@astro.livjm.ac.uk>

GRB 090709: Faulkes Telescope North Upper Limits

Z. Cano (Liverpool JMU), A. Melandri, C. Guidorzi (U. Ferrara), D. Bersier,
I.A. Steele, R.J. Smith, C. Mundell (Liverpool JMU)
report, on behalf of a large collaboration:

Following Swift detection of burst (Morris et al. GCN Circ. 9625), Faulkes
Telescope North (Hawaii) reacted robotically and began observing the field
of GRB 090709 in BVRi bands starting at 07:41:27 UT.

We detect no new source within the XRT error circle:

t_exp     t-T0(mid exposure)    mag

30s      207 s    R2 > 19.3
180s    457 s    I  > 18.3

The upper limits are determined against stars in the USNO B1 catalog.


GRB_name: GRB090708A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9631
SUBJECT: GRB 090708 :  Fermi GBM detection
DATE:    09/07/09 11:38:49 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

S. McBreen (UCD/MPE)
reports on behalf of the Fermi GBM Team:

"At 03:38:18.46 UT on 08 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090708 (trigger 268717100 / 090708152)
which was also detected by the Swift-BAT (Krimm et al. 2009, GCN 9621).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 55 degrees.

The GBM light curve consists of one pulse
with a duration of about 18 s (8-1000 keV).
The time-averaged spectrum from T0-2.0 s to T0+16.2 s is
adequately fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.29 (+0.41/-0.34)
and the cutoff energy, parameterized as Epeak, is
47.5 (+12.0/-9.5) keV (chi squared 359 for 361 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
about 4E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.1 s in the 8-1000 keV band
is 1.0 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9632
SUBJECT: GRB 090709 : planned Suzaku-ToO observation
DATE:    09/07/09 13:01:58 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

Kazuhisa Mitsuda on behalf of the Suzaku GRB-ToO team:

We will carry out a Suzaku-ToO observation of GRB 090709 
(Morris et al., GCN 9625) at location (RA=289.9291, DEC=+60.7271, 
J2000) with the narrow field instruments (the XIS and HXD).
It will start 13:00 UT on July 9, 2009, and
 will continue until 21:32 UT on July 10, 2009.


GRB_name: GRB090709B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9633
SUBJECT: GRB 090709B: Swift detection of a burst
DATE:    09/07/09 15:19:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), V. D'Elia (ASDC), P. A. Evans (U Leicester),
O. Godet (U Leicester), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. Rowlinson (U Leicester),
B. Sbarufatti (INAF-IASFPA), M. H. Siegel (PSU), M. A. Stark (PSU),
R. L. C. Starling (U Leicester) and T. N. Ukwatta (GSFC/GWU) report
on behalf of the Swift Team:

At 15:07:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090709B (trigger=356912).  Swift did not slew because
of Sun constraint.  The BAT on-board calculated location is 
RA, Dec 93.593, +64.085, which is 
   RA(J2000)  =  06h 14m 22s
   Dec(J2000) = +64d 05' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of at least 10 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun constraint, Swift cannot slew to the BAT position until 
18th July 2009. There will thus be no immediate XRT or UVOT data for 
this trigger. 

Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9634
SUBJECT: GRB 090709A: Subaru NIR observation 
DATE:    09/07/09 18:47:52 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

K. Aoki, M. Ishii (Subaru Telescope), M. Kuzuhara (Univ. of Tokyo), 
Y. Takahashi (Univ. of Advanced Study) and N. Kawai (Tokyo Tech) 
report on behalf of the Subaru GRB team:

We observed the field of GRB 090709A (Morris et al. GCN 9625)
with MOIRCS on Subaru Telescope in J and K bands under a
cirrus condition, starting at ~9:30 UT on July 9, approximately
2 hours after the burst.
We detected following two objects near the XRT error circle.
Their preliminary magnitudes based on a nearby 2MASS star are following.

object A:  J(Vega)=19.0, K(Vega)=18.2
object B:  J undetected, K(Vega)=18.6

We placed the K band finding chart at

http://www.hp.phys.titech.ac.jp/nkawai/grb/090709/GRB090709.jpg

We further performed spectroscopy for them with the following results:

Object A: zJH spectroscopy, a flat spectrum with no break detected.

Object B: HK and zJH spectroscopy, a continuum detected in K-band,
   no continuum detected in J band, 
   possibly no continuum in H-band but with high background.

Lack of H band continuum could suggest that the object B is at high 
redshift (z~10), though its poor SNR does not allow us to confirm it.
Fading is not confirmed for either of them.

Further NIR/optical observations are strongly encouraged.


GRB_name: GRB090709A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9635
SUBJECT: GRB 090709A - PAIRITEL Discovery of a Red Afterglow
DATE:    09/07/09 19:03:47 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, J. S. Bloom, C. R. Klein (UC Berkeley), report:

Using a re-reduction of the early PAIRITEL data for GRB 090709A
(Morgan et al. GCN 9628) we report a probable detection of a red
source in the H and Ks bands within the XRT circle (Morris et al. GCN
9625).  The source is located at the following J2000 position (3.15
arcsec away from the center of the current XRT position):

RA = 19:19:42.64
Dec = +60:43:39.3

The uncertainty in this position relative to the ICRS is 0.4" in each direction.

The preliminary photometry yields:

post_burst
t_mid(s) exp(s)  filt  mag
438       374     J     > 17.7 (3 sig)
438       374     H     16.7 +/- 0.2
438       374     Ks    15.3 +/- 0.2

Deeper mosaics obtained later in the night do not contain this source,
indicating that it has faded.  We thus conclude that this is the
afterglow of GRB 090709A.  Note that this is the same source 'B' as
that was just reported in Aoki et al. (GCN 9634).  Our detection in
the H band places a less stringent redshift limit on the afterglow
(although this limit is still high; z > 8.5), if indeed our
non-detection in J is due to a Lyman break and not extinction.  We
also note that source 'A' of GCN 9634, which is of comparable
brightness to 'B' 2 hours after the burst, is not detected in our
shallower image, confirming our conclusion that source 'B' has faded
and is the afterglow.

All magnitudes given in the Vega system, calibrated to 2MASS.  No
correction for Galactic extinction has been made to the above reported
values.


GRB_name: GRB090709A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9636
SUBJECT: GRB 090709A: Enhanced Swift-XRT position
DATE:    09/07/09 20:21:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2188 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 090709A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 289.92664, +60.72764 which is equivalent
to:

RA (J2000): 19h 19m 42.39s
Dec (J2000): +60d 43' 39.5"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9637
SUBJECT: GRB 090709A, RIMOTS optical upper limits
DATE:    09/07/09 21:16:12 GMT
FROM:    Kenta Kono at Miyazaki U  <kenta0514@astro.miyazaki-u.ac.jp>

K.Kono, E.Sonoda, N.Ohmori, H.hayasi,
A.Daikyuji, Y.Nisioka, K.Noda, M.Yamauchi
(University of Miyazaki)

We have observed the field covering the error circle of
GRB090709A (Swift trigger 356890, GCN 9625, D.C.Morriset al.)
with the unfiltered CCD camera on the 30-cm telescope
at University of Miyazaki.
The observation was started 11:42:32 UT (4.1 hr after the Swift trigger),
under cloudy condition.
First analyzable image was obtained at 16:18:26 UT (8.8 hr after the
Swift trigger).

We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position.
(GCN 9634, K.Aoki et al. GCN 9636, J.P.Osborne et al.)

the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames Limit (mag.)
--------------------------------------------------------------
16:18:26 16:18:56 1 13.6
16:18:26 18:39:38 38 16.4
---------------------------------------------------------------


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9638
SUBJECT: GRB 090709A: Wyoming Infrared Observatory NIR upper limits
DATE:    09/07/09 21:57:07 GMT
FROM:    Jerry Bonnell at NASA-GSFC/LHEA  <jerry.t.bonnell@nasa.gov>

GRB 090709A: Wyoming Infrared Observatory NIR upper limits

Jay Norris (U. Denver),
Jerry Bonnell (CRESST/UMCP/GSFC),
Tzitlaly Barajas (Los Angeles City College),
Amanda McAuley (Cal State U. Los Angeles)
report on behalf of the Goddard/Univ. Wyoming NIR camera collaboration.

We observed the Swift XRT position reported by Morris et al. (GCN
Circ. 9625) for GRB 090709A with the 2.3-meter WIRO telescope and
the Goddard IR camera starting 52 minutes after the Swift trigger.

Using stacked J- and K- band exposures begining at 08:30 UT, we
derive the following 2 sigma upper limits for the afterglow source
reported by Morgan et al. (GCN Circ. 9635) from PAIRITEL observations.

       Tmid (UT)    Mag

        09:30      J-band > 21.5
        09:55      K-band > 18.5

The source is designated source B in the Subaru K-band finder chart
from Aoki et al. (GCN Circ. 9634).

Our K-band observations were compromised by cirrus. Our upper limits
are derived based on a comparison with two field stars with J-band
magnitudes 14.5 and 15.7 in the 2MASS catalog.

Further analysis of J- and K-band images is ongoing.


GRB_name: GRB090709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9639
SUBJECT: GRB090709A: High Energy BAT/XRT Analysis Suggests Low to Moderate Redshift
DATE:    09/07/09 22:39:12 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

Nat Butler (UC Berkeley) Reports:

We reduce the Swift XRT and BAT data using our automated pipeline (see,
http://astro.berkeley.edu/~nat/swift for more details of the fits and
summary plots for this and other Swift GRBs).

The intermediate time PC mode XRT data (t=4-10 ksec post trigger) are
well-fit (chi^2/nu=80.48/59) by an absorbed powerlaw with photon index
Gamma=1.9+/-0.1 and column density 1.7+/-0.5 x 10^21 cm^-2 in excess of
the anticipated Galactic contribution (6.6 x 10^20 cm^-2) at the 6.7-sigma
level.  This detection of an excess column is suggestive of a low to
moderate redshift (i.e., z<~2) for the GRB (e.g,. Grupe et al. 2007, ApJ,
133, 2216).

The time-integrated BAT spectrum is well-modeled by a powerlaw times
exponential function (chi^2/nu=29.67/55).  We derive Epeak,obs = 200
(176,298) keV and a rest-frame isotropic equivalent energy release Eiso ~
1.4 x 10^53 erg (z=1).  If the GRB were at very high z~8, Eiso ~ 4.5 x
10^54 erg, comparable to the intrinsically brightest few GRBs ever detected,
further suggestive of a low to moderate redshift for this event.


GRB_name: GRB090709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9640
SUBJECT: GRB 090709A: Swift-BAT refined analysis
DATE:    09/07/09 22:52:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. C. Morris (PSU),
D. M. Palmer (LANL), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+505 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090709A (trigger #356890)
(Morris, et al., GCN Circ. 9625).  The BAT ground-calculated position is
RA, Dec = 289.944, 60.728 deg, which is 
   RA(J2000)  =  19h 19m 46.7s 
   Dec(J2000) = +60d 43' 40.8" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows a complex structure.  It starts
at ~T-80 sec, peaks at T-70 sec, and returns to almost background
at ~T-20 sec.  Then a series of overlapping peaks starts with the
brightest centered at ~T+22 sec.  Then begins an exponential decay
with a series of decreases eventually returning to background level
at ~T+270 sec.  There two more peaks at ~T+330 and ~T+400 sec.  A third peak
is chopped off while still rising when the source went out of the BAT FOV
at ~T+490 sec due to the spacecraft slewing because of an observing constraint.
T90 (15-350 keV) is 89 +- 3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-66.7 to T+101.5 sec is well fit by 
simple power law.  The power law index of the time-averaged spectrum is
1.22 +- 0.03.  The fluence in the 15-150 keV band is 2.57 +- 0.03 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+21.80 sec in the 15-150 keV band
is 7.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/356890/BA/


GRB_name: GRB090709B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9641
SUBJECT: GRB 090709B, Swift-BAT refined analysis
DATE:    09/07/09 23:02:32 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. N. Ukwatta (GWU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), F. E. Marshall 
(NASA/GSFC),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
(i.e. the Swift-BAT team):

Using the data set from T-61 to T+242 sec from the recent telemetry 
downlink,
we report further analysis of BAT GRB 090709B (trigger #356912)
(Marshall et al., GCN Circ. 9633).  The BAT ground-calculated position is
RA, Dec = 93.522, 64.081 deg which is
   RA(J2000)  =  06h 14m 05.4s
   Dec(J2000) = +64d 04' 51.9"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 15%.

The mask-weighted light curve shows a main peak beginning at T-5 seconds 
and
continuing until T+10 sec.  There are then two much weaker peaks at 
approximately
T+25 and T+35 sec. At T+240 sec, a pre-planned spacecraft slew took the 
source
out of the BAT FOV. T90 (15-350 keV) is 27.2 +- 6.6 sec (estimated error 
including systematics).

The time-averaged spectrum from T-5.4 to T+35.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.51 +- 0.18.  The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10-6 
erg/cm2.
The 1-sec peak photon flux measured from T+1.47 sec in the 15-150 keV band
is 2.1 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/356912/BA/


GRB_name: GRB090709A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9642
SUBJECT: GRB 090709A: Swift XRT Refined Analysis
DATE:    09/07/09 23:06:12 GMT
FROM:    Antonia Rowlinson at U.of Leicester  <bar7@star.le.ac.uk>

A. Rowlinson (U Leicester) and D. C. Morris (PSU) report on behalf of
the Swift-XRT team:

We have analysed 9.4 ks of XRT data for GRB 090709A (Morris et al. GCN
Circ. 9625), from 74 s to 27.3 ks after the BAT trigger. The data
comprise 445 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Osborne et al. (GCN. Circ 9636).

The light curve can be modelled with a broken power-law decay. The
initial decay index is alpha=0.77(+/-0.1), at T+7918 s the light curve
breaks to a decay with alpha=1.51(+/-0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+/-0.04). The
best-fitting absorption column is 2.14 (+0.13, -0.12) x 10^21 cm^-2, in
excess of the Galactic value of 6.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.05 (+/-0.08) and a
best-fitting absorption column of 2.68 (+0.26, -0.25) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.2 x 10^-11 (6.7 x 10^-11) erg cm^-2
count^-1.

If the light curve continues to decay with a power-law decay index of
1.51, the count rate at T+24 hours will be 0.043 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of  1.8 x
10^-12 (2.9 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00356890.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9643
SUBJECT: GRB 090709A: RAPTOR Limits During Gamma-Ray Emission
DATE:    09/07/09 23:41:47 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis, B. Norman
of Los Alamos National Laboratory report:

The RAPTOR telescope system responded to Swift trigger
356890 (Morris et al., GCN 9625) under good observing conditions.
Our narrow-field instruments began observing the location at
07:39:03.4 UTC, 28.8 s after the Swift trigger (7.1 s after
receipt of GCN message).  We obtained simultaneous observations
during the gamma-ray emitting interval in Cousins V, R, and I
bands as well as unfiltered data.  We do not detect the counterpart
observed by the Subaru Telescope (Aoki et al., GCN 9634) and
PARITEL (Morgan et al., GCN 9635).  The data from our unfiltered
and filtered systems was calibrated to the USNO-B1 catalog.  We
can put the following limits on the prompt emission:

t-mid(s)          exp(s)   filter  mag    mag-err
[since trigger]
----------------------------------------------------
31.34             5        clear  17.1   5 sigma limit
52.35             5        V      14.8   5 sigma limit
52.35             5        R      15.1   5 sigma limit
52.35             5        I      15.5   5 sigma limit
89.95             40       V      16.9   5 sigma limit      


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9644
SUBJECT: GRB 090709A: NOT optical observations
DATE:    09/07/10 00:10:54 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@astro.ku.dk>

D. Malesani (DARK/NBI), J. Telting (NOT), P. Wilson (NOT and Univ. 
Oslo), P. Jakobsson (Univ. Iceland), J.P.U. Fynbo, G. Leloudas 
(DARK/NBI), A.J. Levan (Univ. Warwick), and K. Wiersema (Univ. 
Leicester), report on behalf of a larger collaboration:

We observed the field of GRB 090709A (Morris et al., GCN 9625) with the 
NOT equipped with ALFOSC. Observations were carried out in the R band, 
starting on 2009 Jul 9.943 (14.97 hr after the trigger), for a total 
exposure time of 30 min.

At the position of the NIR transient (Aoki et al., GCN 9634; Morgan et 
al., GCN 9635) we do not detect any source, down to a limiting magnitude 
R >~ 24. The calibration is based on a number of closeby USNO-B1 stars 
(R2 magnitudes).


GRB_name: GRB090709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9645
SUBJECT: GRB 090709A: Quasiperiodic variations in the BAT light curve
DATE:    09/07/10 01:00:23 GMT
FROM:    Craig Markwardt at NASA/GSFC/UMD  <craigm@milkyway.gsfc.nasa.gov>

C. B. Markwardt (GSFC/UMD), F. P. Gavriil (GSFC/UMBC), D. M. Palmer
(LANL), W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC)

We performed a timing analysis of GRB 090709A.  Visually, there
appears to be a quasiperiodic signal at period near 8 seconds.
More formally, a power spectrum of the full burst shows an
apparent strong excess at 8.06 seconds.

This analysis is based on a de-trended 64 msec BAT light
curve (15-350 keV), T-50 s to T+150 s, where the trend was based
on a smoothed version of the light curve (smoothing scale 10
sec).  After normalizing the power spectrum by the local noise
level (0.2 to 0.6 Hz), we find a peak power of ~52, which has a
probability of occurring by random chance of ~1e-6 after
adjusting for the number of trials.  The results are relatively
insensitive to trend smoothing timescale, to within a factor of
~2.

The number of trials is based on the number of independent
Fourier frequencies examined (~2000) and an estimated 100 BAT
bursts long enough in duration to perform such an analysis.  We
consider this to be a conservative estimate: we are likely to
have overestimated the number bursts for which we could do this
analysis; and the 0.2 to 0.6 Hz range used to compute the noise
level has the most noise, which decreases the overall peak
significance.

The amplitude of the modulations is as high as ~70% of the
smoothed light curve, and as small as 10%.

The signal is not strictly coherent.  The "Q factor", the ratio
of peak centroid frequency to FWHM, is ~11 (whereas a coherent
signal with a duration of ~200 seconds could be as sharp as Q=24).

We believe such a detection is the first time strong near-periodic
oscillations have been seen at this significance for classical
gamma-ray bursts.  Periodic variations at 8 seconds would be
typical for galactic magnetars.  If this source is at a redshift
of 8.5-10 (Aoki et al. GCN 9634, Morgan et al. GCN 9635), then
the intrinsic period would be ~800 milliseconds, which falls
outside of the magnetar range.  If on the other hand the source
is at low redshift (Butler, GCN 9639), the observed period would
be typical of magnetars.


Figures

GRB 090709A BAT light curve
   http://gcn.gsfc.nasa.gov/gcn/other/grb090709a_bat_lc.gif

GRB 090709A BAT light curve after removing trend
   http://gcn.gsfc.nasa.gov/gcn/other/grb090709a_bat_detrended.gif

GRB 090709A BAT light curve (black) and trend (red)
   http://gcn.gsfc.nasa.gov/gcn/other/grb090709a_bat_trend.png

GRB 090709A power spectrum of detrended BAT light curve, normalized by
local noise level
   http://gcn.gsfc.nasa.gov/gcn/other/grb090709a_powspec.png


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9646
SUBJECT: GRB 090709A: P60 Observations
DATE:    09/07/10 06:31:02 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko, J. S. Bloom, A. N. Morgan, and D. A. Perley (UC
Berkeley) report on behalf of a larger collaboration:

We have imaged the field of GRB090709A (Morris et al., GCN 9625) with the
automated Palomar 60-inch telescope.  Observations began at 7:40:26 UT on
9 July 2009 (~ 2 minutes after the burst trigger) and were taken in the
r', i', and z' filters.

We marginally detect a faint source at the location of the NIR afterglow
(Aoki et al., GCN 9634, Morgan et al., GCN 9635) in our first r' and z'
images.  However, nothing is detected at this location in subsequent
images or deeper coadditions at later times.  We therefore cannot
entirely rule out that these represent chance statistical fluctuations.

We report the following photometry and upper limits (referenced with
respected to the USNO-B1 catalog):

UT Midpoint     Exposure (s)    Filter          AB Mag
----------------------------------------------------------------------
7:40:56         60              r'              21.7 +- 0.4
7:45:12         60              r'              > 21.4
8:08:57         600             r'              > 22.9
7:46:38         60              i'              > 21.0
8:11:59         480             i'              > 22.8
7:45:55         120             z'              20.5 +- 0.5
8:13:59         480             z'              > 21.5

The r' and z' detections, if real, would argue strongly in favor of a low
or moderate redshift origin with a large extinction column in the GRB host
galaxy (Butler, GCN 9639).  A combined fit of approximately co-eval
PAIRITEL (GCN 9635, Morgan et al.) and P60 photometry assuming moderate
redshift (z < 4) is consistent with a highly dust-extinguished (A_V > 2
mag) power-law spectral energy distribution.

A smoothed version of our first r' image can be found at:

   http://astro.berkeley.edu/~cenko/public/grb/grb090709/p60r.jpg

The blue circle is the refined XRT localization (Osborne et al., GCN
9639), while the red circle is the location of the PAIRITEL NIR afterglow
(Morgan et al., GCN 9635).


GRB_name: GRB090709A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9647
SUBJECT: Konus-Wind and Konus-RF observations of GRB 090709A
DATE:    09/07/10 10:43:10 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long GRB 090709A (Morris et al., GCN 9625)
triggered Konus-Wind
at T0=27514.965 s UT (07:38:34.965),
and Konus-RF instrument onboard CORONAS-PHOTON s/c
at T0(KRF)=27513.934 s UT (07:38:33.934).

The burst light curve shows a multi-peaked structure
with a duration of ~100 s. We confirm presence of
quasi-period in the light curve (Markwardt et al., GCN 9645).
The corresponding peaks in the FFT power spectrum
of 128 ms light curve are clearly seen around
P=8.28s (0.1208 Hz) and P=16.56s (0.0604 Hz).

The Konus-Wind light curves of this GRB are vailable
at http://www.ioffe.ru/LEA/GRBs/GRB090709_T27514/

The normalized power spectrum of the detrended
Konus-Wind light curve (128 ms, in 20-1150 keV range)
is available at
http://www.ioffe.ru/LEA/GRBs/GRB090709_T27514/GRB090709_T27514_KW_power.png

As observed by Konus-Wind the burst had
a fluence of (9.1  0.07)x10-5 erg/cm2,
and a 256-ms peak flux measured from T0+23.308 s
of (3.9  0.6)x10-6 erg/cm2/s
(both in the 20 keV - 3 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+102.912 s) is well fitted
(in the 20 keV - 3 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.85  0.08,
the high-energy photon index beta = -2.7(-0.3, +0.2),
the peak energy Ep = 298  27 keV (chi2 = 71/67 dof).

The spectrum at the maximum count rate,
measured from T0+16.640 to T0+24.320 s, is well fitted
(in the 20 keV - 3 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.86 (-0.07, +0.10),
the high-energy photon index beta = -2.6(-2.6, +0.53),
the peak energy Ep = 416(-100, +95) keV (chi2 = 63/67 dof).

All the quoted values are preliminary.
The quoted errors are at the 90% confidence level.


GRB_name: GRB090709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9648
SUBJECT: GRB 090709A: evidence for a very red afterglow at low z
DATE:    09/07/10 12:02:42 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri, C.G. Mundell, D. Bersier,
Z. Cano, S. Kobayashi, I.A. Steele, R.J. Smith (Liverpool JMU),
and A. Gomboc (U. Ljubljana) report, on behalf of a large collaboration:

We re-analysed the data promptly acquired with the 2-m Faulkes
Telescope North in the R and i' filters (Cano et al. GCN 9630)
of the Swift GRB 090709A (Morris et al. GCN 9625).
 From the stacked images, we marginally detect a source in the
r' frame at the position of the NIR afterglow found by PAIRITEL
(Morgan et al. GCN 9635), identified as source 'B' by Subaru
(Aoki et al. GCN 9634) and possibly detected in the r' and z' bands
(Cenko et al. GCN 9646). The same object is not detected in the
i' band frame (although with a shorter total exposure).

Start time        End time        Exposure      Filter    mag
(min)             (min)           (s)
-------------------------------------------------------------------
2.88             55.02           720            R        22.7 +/- 0.5
7.55             47.05           520            i'       > 20.6
-------------------------------------------------------------------

Calibration was performed against the I and R2 values of the USNOB1
nearby star at 19:19:44.575, +60:43:27.44 assuming I=14.68 and R2=15.70.

We built a tentative SED at the PAIRITEL observation mid time of 438 s
(Morgan et al. GCN 9635), combining the P60 values in the z' filter
(Cenko et al. GCN 9646) and the assuming for the r' filter an
intermediate value comprising both the P60 and our own value.
This value as well as our i' band upper limits were backextrapolated
to the chosen time assuming a range of power-law decay indices, from
0.3 to 1. The SED was finally corrected for the Galactic reddening
of E(B-V)=0.09. We found that the SED can be fitted with a simple
power-law with spectral index beta=3.4 +/- 0.8 (90%cl) and no
evidence for a Lyman drop.
We therefore support the nature of a very red afterglow at low z
(Butler et al. GCN 9639) and possibly associated with a non-GRB
progenitor as suggested by the quasi-periodic oscillations found
in the gamma-ray profile (Markwardt et al. GCN 9645; Golenetskii
et al. GCN 9647).

Our stacked R band frame is available at the following link (red
and green circles show the Swift-XRT and PAIRITEL circles, respectively):

http://www.fe.infn.it/u/guidorzi/GRB090709A/090709A_R.jpg


GRB_name: GRB090709A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9649
SUBJECT: GRB 090709A: confirmation of the periodicity in the SPI-ACS data
DATE:    09/07/10 12:15:28 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D. Gotz (CEA-Saclay), S. Mereghetti (IASF-Milano), A. von Kienlin (MPE  
Garching), M. Beck (ISDC Versoix)  report:

The Swift GRB 090709A (Morris at al., GCN 9625) is clearly detected  
also in the data of Anticoincidence System (ACS) of the spectrometer  
SPI on board INTEGRAL. SPI-ACS consists on 91 BGO detectors that are  
sensitive to photons above 100 keV, and their light curves are  
continuously stored in 50 ms bins. No directional or spectral  
information is available. The light curve of GRB 090709A  can be found  
here

http://ibas.iasf-milano.inaf.it/090709Alc.jpg

The ~8 s periodicity reported by Markwardt et al. (GCN 9645) in the  
Siwft/BAT data and by Golenetskii et al. (GCN 9647) in Konus-Wind data  
is clearly detected also in the SPI-ACS data. A periodogram over the  
entire burst duration can be found here

http://ibas.iasf-milano.inaf.it/090709A.jpg

By fitting the peak of the periodogram using a gaussian function one  
obtains a best period of 8.11 s. A light curve folded to the best  
period can be fond here

http://ibas.iasf-milano.inaf.it/090709A_folded.jpg


This message can be cited.


GRB_name: GRB090709B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9650
SUBJECT: GRB 090709B: Fermi GBM detection
DATE:    09/07/10 15:53:17 GMT
FROM:    Charles Meegan at NASA/MSFC  <charles.a.meegan@nasa.gov>

C. Meegan (USRA) and A. J. van der Horst (NASA/MSFC/ORAU) 
report on behalf of the Fermi GBM Team: 

"At 15:07:41.14 UT on 09 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090709B (trigger 268844863 / 090709630), 
which was also detected by the SWIFT-BAT (GCN 9633).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 35 degrees.

The GBM light curve consists of two pulses
with a duration (T90) of about 32 s (8-1000 keV). 
The time-averaged spectrum from T0-2.0 s to T0+27.6 s is 
best fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.01 +/- 0.16 and
the cutoff energy, parameterized as Epeak, is 130 +/- 24 keV
(chi squared 354 for 365 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(1.3 +/- 0.2)E-6 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+2.0 s in the 8-1000 keV band 
is 2.0 +/- 0.3 ph/s/cm^2.

The temporal and spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9651
SUBJECT: GRB 090709A: WHT LIRIS observations 
DATE:    09/07/10 19:51:09 GMT
FROM:    Klaas Wiersema at U of Leicester  <kw113@star.le.ac.uk>

K. Wiersema, D. Malesani and A. Levan report on behalf of a larger 
collaboration:

We observed the field of GRB 090709A (Morris et al., GCN 9625) with the
William Herschel Telescope, using the LIRIS instrument.
We obtained a total of 1890 secs of exposure time in J band, under reasonable 
conditions, starting at 04:48 UT July 10th (20.8 hrs after burst).

We do not detect the afterglow (Aoki et al. GCN 9634; Morgan et
al. GCN 9635), with limiting magnitude J>~20. Source A of Aoki et al is 
clearly detected.

We are grateful to Don Pollaco and Ian Skillen for performing these 
observations.


GRB_name: GRB090709A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9652
SUBJECT: GRB 090709A:  Swift UVOT upper limits
DATE:    09/07/10 20:34:40 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

T. A. Pritchard (PSU), E. A. Hoversten (PSU) and D. C. Morris (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began observing the field of GRB 090709A, 77 seconds
after the BAT trigger (Morris et al., GCN 9625). We do not detect any
source at the Swift enhanced XRT position (Osborne et al., GCN 9636).

The 3-sigma upper limits in each filter are:

Filter   T_start(s)   T_stop(s)   Exp(s)  Mag (3-sigma upper limit)
-------------------------------------------------------------
white(FC)    77          227       150       > 21.03
v          4697         4897       200       > 19.59
b          4081         4281       200       > 20.01
u           290          471       181       > 20.09
uvw1       5107         5307       200      > 19.83
uvm2       4902         5102       200       > 19.63
uvw2       4492         4692       200       > 19.85
-------------------------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.09 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).


GRB_name: GRB090709A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9653
SUBJECT: GRB 090709A: Suzaku WAM observation of the prompt emission
DATE:    09/07/11 11:34:36 GMT
FROM:    Masanori Ohno at ISAS/JAXA  <ohno@astro.isas.jaxa.jp>

M. Ohno (ISAS/JAXA), W. Iwakiri (Saitama U.),
M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, E. Sonoda,
K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, S. Sugita (Aoyama Gakuin U.), S. Hong (Nihon U.),
N. Vasquez (Tokyo Tech.), Y. Urata (NCU),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
on behalf of the Suzaku WAM team, report:


The bright, long GRB 090709A (Swift/BAT trigger #356890 ; Morris et
al., GCN 9625) triggered the Suzaku Wide-band  All-sky Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at 07:38:33 UT (=T0).

The observed light curve shows a multi-peaked structure with a duration
(T90) of about 81 seconds. The corresponding peaks in the FFT power
spectrum of 1 s light curve are clearly seen around P=8.06(-0.20,+0.20) s,
which is consistent with the previous reports (Markwardt et al., GCN 9645;
Golenetskii et al., GCN 9647; Gotz et al., GCN 9649).
The fluence in 100 - 1000 keV was 6.06(-0.36, +0.48) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+70s was 4.83(-0.69, +0.27) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-10s to T0+110s is well fitted by a power-law with exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha       0.97(-0.43, +0.52), and
  Epeak       439(-58, -48) keV (chi^2/d.o.f. = 62.9/48).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst are available at:
 http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9654
SUBJECT: GRB090709A : WSRT Radio observation
DATE:    09/07/11 12:15:37 GMT
FROM:    Atish Kamble at U. of Amsterdam  <A.P.Kamble@uva.nl>

"Atish Kamble (U of Amsterdam), A.J. van der Horst (NASA/MSFC/ORAU),
C. Kouveliotou (NASA/MSFC), R.A.M.J. Wijers and E. Rol (U of Amsterdam)
report on behalf of a large collaboration"

The Westerbork Synthesis Radio Telescope observed the position of the GRB090709A 
afterglow (Morris et al. GCN 9625) at 4.9 GHz between July 10.71 and 11.26, 2009 
(i.e. about 1.67 days after the burst). No radio counterpart to the afterglow was detected
up to three sigma rms limit of 141 microJy. The formal flux measured at the position 
of the NIR counterpart (Morgan et al. GCN 9635) is 104 +/- 47 microJy.

We would like to thank the WSRT staff for rapidly scheduling and obtaining
these observations."


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9655
SUBJECT: GRB 090709A: deep optical observation with the 10.4m GTC
DATE:    09/07/11 12:18:38 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC Granada), A. de Ugarte Postigo (OAB-INAF),
J. Gorosabel, S. Guziy, M. Jelnek (IAA-CSIC), P. Kubnek (IAA-CSIC and
GACE Valencia), D. Prez-Ramrez (Univ. de Jan), N. Mirabal (UCM Madrid),
A. Llorente, J. M. Castro Cern (ESAC Villafranca del Castillo), C.
Alvarez (IAC/GTC La Palma) and J. Cepa (IAC Tenerife),

report:

Following the detection of GRB 090709A by Swift (Morris et al. GCNC
9625), we have conducted follow-up observations with the 10.4-m Gran
Telescopio Canarias (GTC) at the Observatorio del Roque de los Muchachos
of the Instituto de Astrofsica de Canarias, in the island of La Palma.
Images in the i-band filter (7 x 300-s) under 1.0 seeing were gathered
with the OSIRIS instrument (Cepa et al. 2009, in prep.) on 11 July 2009,
00:45 UT (i.e. 41 hr after the event).

At the position of the reported nIR/optical afterglow (Aoki et al. GCNC
9634, Morgan et al. GCNC 9635, Cenko et al. GCNC 9646) we detect no single
object down to i ~ 25.5 (preliminary 3-sigma limit), or i ~ 25.2 when
taking into account the foreground Galactic extinction. We note two nearby
faint objects, which lie 3.3 south-east and 4 north of the afterglow.

The stacked GTC .jpg image is available at the following link:
http://www.iaa.es/~gss/GRB090709A

Although we cannot exclude that GRB 090709A occurred in a low redshift
galaxy (Butler et al. GCNC 9639, Guidorzi et al. GCNC 9648), our
non-detection of a host galaxy, together with the reported 8-s
quasi-periodic oscillations (Markwardt et al. GCN 9645, Golenetskii et al.
9647, Gotz et al. GCNC 9649, Ohno et al. GCNC 9653) and the fact that the
event is at galactic coordinates of about (l = 91, b = 20) cannot rule out
that the initial observed gamma-ray emission arose from a nearby magnetar
candidate in the Milky Way, much closer than GRB 070610 / SWIFT
J195509+261406 (Castro-Tirado et al. 2008, Nature 455, 506).
Multiwavelength observations are encouraged.

We acknowledge the excellent support from the GRANTECAN staff.


This Circular can be quoted.


GRB_name: GRB090621B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9656
SUBJECT: GRB 090621B: MTM-500 optical observations 
DATE:    09/07/11 20:19:43 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (SAI MSU), V. Kouprianov, Ya. Naiden, V. 
Slesarenko, A. Devyatkin (Pulkovo Observatory),   report on behalf of larger 
GRB follow-up collaboration:

We observed   the field of the Swift GRB 090621B (Curran et al, GCN  9545) 
with MTM-500 telescope of  Kislovodsk solar station of the Pulkovo 
observatory  in two series in R-filter between (UT) 2009-06-21 22:31 - 
2009-06-22 00:01, i.e. starting ~24 minutes after burst onset.  The upper 
limit of a stacked image of first 15 frames based on USNO B1.0 stars is 
following

T0+         Filter   Exp.      mag.
(mid, d)                 s
0.02147  R        15x60  >18.5 (3 sigma)

While we do not detect  objects reported in GCN 9547 (Levan  et al.) and GCN 
9549 (Galeev et al.) in  the stacked image above, we may suggest a possible 
object near the edge of  the refined XRT error box (Beardmore et al., GCN 
9550) in coordinates (J2000) RA  =  20:53:53.24 Dec = +69:01:45.5. This 
possible object appears more intense in the stacked image of the first five 
frames, and does not appear in the second epoch of our observations started 
on Jun.21 (UT) 23:37. Due to low S/N ratio we cannot confirm the object is 
real. We encourage re-analysis of  later deep observations to clarify the 
nature of the object.

The finding chart can be found at 
http://grb.rssi.ru/GRB090621B/grb090621B_MTM.png , where source labeled #5 
is the USNO B1.0 star 1590-0172172  (RA(J2000)=20:53:57.28, 
Dec(J2000)=+69:01:47.8, R2=19.41)


GRB_name: GRB090709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9657
SUBJECT: VLA radio observations of GRB 090709A
DATE:    09/07/12 01:40:32 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of a
larger collaboration:

"We used the Very Large Array to observe the field of view towards the
GRB 090709A (GCN 9625) at a frequency of 8.46 GHz on 2009 Jul. 10.46
UT and Jul. 11.42 UT, and at a frequency of 1.43 GHz on 2009 Jul. 11.39
UT. The GRB radio afterglow is undetected at the PAIRITEL NIR afterglow
position (GCN 9635). The peak flux at the GRB afterglow position on 11th
July observations is 62+/-35 uJy in 8.46 GHz band and 79+/-144 uJy at
1.43 GHz band.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9658
SUBJECT: GRB 090709A: Xinglong TNT optical upper limit
DATE:    09/07/12 03:16:43 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, W.K. Zheng, Y.L. Qiu, J.Y. Wei, J. Wang, 
J.S. Deng and J.Y. Hu on behalf of EAFON report:

We have observed GRB 090709A (Morris et al.GCN 9625)
with Xinglong TNT telescope from July 9, 13:41:18 (UT),
6.04 hour after the burst. After combined 10*600s R
band images, no new source or afterglow counterpart (Morgan et al.GCN
9635;Guidorzi et al. GCN 9648) was 
found in our combined image within the XRT errorbox (Morris et al. GCN
9625). 
The uplimit is estimated to be about 20.6 mag at the mean time 
of 6.816 hours since the trigger. 

This message may be cited.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org/grb/


GRB_name: GRB090712A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9659
SUBJECT: GRB 090712: Swift detection of a burst
DATE:    09/07/12 04:00:29 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. T. Holland (CRESST/USRA/GSFC), N. Gehrels (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
A. Rowlinson (U Leicester), M. H. Siegel (PSU) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 03:51:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090712 (trigger=357072).  Swift could not slew due to 
the Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 70.103, +22.557 which is 
   RA(J2000) = 04h 40m 25s
   Dec(J2000) = +22d 33' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single broad
triangular peak structure with a duration of about 100 sec.  
The peak count rate was ~1000 counts/sec (15-350 keV), 
at ~0 sec after the trigger. 

Because of the constraint, the BAT position is unobservable 
by Swift until 21st July 2009. There will thus be no prompt XRT or UVOT 
data for this trigger. 

Burst Advocate for this burst is S. T. Holland (sholland AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090712A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9660
SUBJECT: GRB 090712: Swift-BAT refined analysis
DATE:    09/07/12 16:08:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), S. T. Holland (CRESST/USRA/GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+355 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090712 (trigger #357072)
(Holland, et al., GCN Circ. 9659).  The BAT ground-calculated position is
RA, Dec = 70.097, 22.525 deg, which is 
   RA(J2000)  =  04h 40m 23.2s 
   Dec(J2000) = +22d 31' 29.4" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.
 
The mask-weighted light curve shows a mostly smooth peak starting
at ~T-160 sec, peaking at ~T_zero, and ending at ~T+170 sec.
T90 (15-350 keV) is 145 +- 52 sec (estimated error including systematics).
 
The time-averaged spectrum from T-99.1 to T+157.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.33 +- 0.11.  The fluence in the 15-150 keV band is 4.0 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-6.10 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/357072/BA/


GRB_name: GRB090713A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9661
SUBJECT: GRB 090713: Fermi GBM detection
DATE:    09/07/13 15:20:47 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM Team:

"At 00:29:28.06 UT on 13 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090713 (trigger 269137770 / 090713020).
The on-ground calculated location, using the GBM trigger data, is
RA = 284.8, Dec = -3.3 (J2000 degrees, equivalent to 18h59m, -3d20'),
with an uncertainty of 2.4 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which is
currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 63 degrees.

The GBM light curve consists of multiple peaks with a duration (T90)
of about 113 s (8-1000 keV).
The time-averaged spectrum from T0-4.1 s to T0+55.3 s is well fit by
a power law function with an exponential high energy cutoff. The
power-law index is -0.34 +/- 0.12 and the cutoff energy, parameterized
as Epeak, is 99 +/- 5 keV (chi squared 339 for 359 d.o.f.).

The event fluence (8-1000 keV) in this time interval is (3.7 +/- 0.4)E-6
erg/cm^2. The 1-sec peak photon flux measured starting from T0+24.6 s
in the 8-1000 keV band is 1.6 +/- 0.2 ph/s/cm^2.

The temporal and spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090712A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9662
SUBJECT: GRB 090712: Fermi GBM observation
DATE:    09/07/13 15:26:01 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 03:51:00.34 UT on 12 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090712 (trigger 269063462 / 090712160), 
which was also detected by the SWIFT-BAT (Holland et al. 2008, GCN 9659,
Barthelmy et al., GCN 9660). The GBM on-ground location is consistent 
with the Swift position. 

The angle from the Fermi LAT boresight is 33 degrees.

The GBM light curve shows one single pulse with a duration (T90) 
of about 72 s (8-1000 keV). The time-averaged spectrum from 
T0-22.528 s to T0+49.153 s is best fit by a power law function 
with an exponential high energy cutoff.  The power law index 
is -0.68 +/- 0.13 and the cutoff energy, parameterized as Epeak, 
is 505 +/- 101 keV (chi squared 511 for 486 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(4.2 +/- 0.3)E-06 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+7.168 s in the 8-1000 keV band 
is 0.63 +/- 0.04 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090713A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9663
SUBJECT: GRB090713 optical limit by "Pi of the Sky"
DATE:    09/07/14 14:00:29 GMT
FROM:    Marcin Sokolowski at Soltan Inst. Nuc Studies,Warsaw  <msok@fuw.edu.pl>

T.Batsch, M.Cwiok, W.Dominik, G.Kasprowicz, A.Majcher, A.Majczyna,
K.Malek, L.Mankiewicz, K.Nawrocki, L.W.Piotrowski,
M.Siudek, M.Sokolowski, J.Uzycki, G.Wrochna, M.Zaremba, A.F.Zarnecki
on behalf of "Pi of the Sky" collaboration http://grb.fuw.edu.pl

The "Pi of the Sky" apparatus observed error box of Fermi GRB090713
before, during and after the burst, starting 20 minutes before the
Fermi trigger. No new source brighter than 11 mag has been identified
on 10s exposures.
IPN triangulation for this burst is strongly encouraged.


GRB_name: GRB090618A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9665
SUBJECT: Detection of GRB 090618 by RT-2 Experiment onboard the CORONAS-PHOTON Satellite
DATE:    09/07/15 08:23:22 GMT
FROM:    Sandip K. Chakrabarti at S.N. Bose Nat. Centre for Basic Sci.  <chakraba@bose.res.in>

Detection of GRB 090618 by RT-2 Experiment onboard the CORONAS-PHOTON Satellite


A. R. Rao, J. P. Malkar, M. K. Hingar, V. K. Agrawal (TIFR, Mumbai, India), S. K. 
Chakrabarti, A. Nandi, D. Debnath, T. C. Kotoch (ICSP, Kolkata, India), T. R.
Chidambaram, P. Vinod, S. Sreekumar (VSSC, Thiruvananthapuram, India), Y. D.
Kotov, A. S. Buslov, V. N. Yurov, V. G. Tyshkevich, A. I. Arkhangelskij, R. A.
Zyatkov (MephI, Moscow, Russia) report:

The RT-2 Experiment onboard the CORONAS-PHOTON satellite has clearly detected
GRB 090618 (Schady et al., 2009, GCN 9512) which triggered at T0 = 30507.00
sec (UT) (08h 28m 27s). The satellite was in the SHADOW mode (away from the
SUN) with GOOD time (away from the polar and SAA regions) observation of 700
sec starting at 08h 23m 27sec (UT) and ending at 08h 36m 46.99sec (UT).

The GRB light curve shows a complex profile (Golenetskii et al., 2009, GCN 
9553) of time duration of around 150 sec. The burst profile has three main 
pulses with the brightest pulse (~700 cts/sec) started at T0+65 sec, the second 
one at T0+85 sec and the last one at T0+115 sec.

Both RT-2/S and RT-2/G detectors have registered this multi-structured burst 
profile of the light curve in the energy band of 60 - 215 keV. In high-energy 
band of 330 - 1000 keV, the profile becomes simple with a single bright peak at 
T0+65 sec. It is also noted that the burst width decreases with the increase in 
the energy band, a quiet natural phenomena of GRB burst profile. The burst was 
incident at an angle of 77 degrees to the detector axis. It showed the typical 
Band spectrum with peak energy at about 180 keV and integrated 20 keV - 1MeV
flux of 2.8 X 10^-4 ergs/ cm^2.
 
The light curve is available at the web-site:
http://csp.res.in/rt2_files/grb090618-lc.html


GRB_name: GRB090715A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9666
SUBJECT: GRB 090715: Swift detection of a short hard burst
DATE:    09/07/15 17:44:43 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (PSU), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), D. Grupe (PSU),
S. T. Holland (CRESST/USRA/GSFC), R. Margutti (Univ Bicocca&OAB),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), M. H. Siegel (PSU),
M. Stamatikos (NASA/ORAU) and L. Vetere (PSU) report on behalf of the
Swift Team:

At 17:25:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090715 (trigger=357498). 
The BAT on-board calculated location is 
RA, Dec 152.122, +9.997 which is 
   RA(J2000) = 10h 08m 29s
   Dec(J2000) = +09d 59' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 0.4 sec.  The peak count rate
was ~11,000 counts/sec (15-350 keV), at ~0.3 sec after the trigger. 

Due to current problems with the Solid State Recorder (GCN 9664),
automatic slewing to sources is disabled.  However, this burst
location is also in Sun constraint and will not come out of 
constraint until October 9, 2009.  There will thus be no XRT or 
UVOT data for this trigger. 

We note the existence of an S0/A galaxy NGC 3130 (z=0.027) near
the edge of the BAT error circle (nominal position of
the galaxy is 4.33 arcminutes from the center of the
error circle, with NED reporting a radius of 1.0 arcmin
for the galaxy). 

Burst Advocate for this burst is J. L. Racusin (racusin AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090715A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9667
SUBJECT: GRB 090715A: ROTSE-III Optical Limits
DATE:    09/07/15 17:47:35 GMT
FROM:    Shashi Bhushan Pandey at ARIES, INDIA  <shashi@aries.ernet.in>

S. B. Pandey (U Mich), S.A. Yost (College of St. Benedict), W. Zheng,
F. Yuan (U Mich), report on behalf of the ROTSE collaboration:

ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia,
responded to the short-hard GRB 090715A (Swift trigger 357498,  Racusin J. L., GCN 9666), producing images
beginning 7.1 s after the GCN notice time. An automated response took
the first image at 17:26:05.1 UT, 25.9 s after the burst, under fair
conditions.
We took 10 5-sec and 10 20-sec exposures and imaging is ongoing.
These unfiltered images are calibrated relative to USNO A2.0 (R). 

Comparison to the DSS (second epoch) reveals no new sources
within the 3-sigma Swift/BAT error circle, for both single images and
coadding into sets of 10.
Individual images have limiting magnitudes ranging from 15.4-16.6; we
set the following specific limits.
start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
17:26:05.1   17:27:21.5        76     16.8           25.9       Y
17:27:36.4   17:32:18.5       282     17.4          117.2       Y


GRB_name: GRB090715B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9668
SUBJECT: GRB 090715B: Swift detection of a burst with a possible optical counterpart
DATE:    09/07/15 21:34:31 GMT
FROM:    Loredana Vetere at PSU  <vetere@astro.psu.edu>

L. Vetere (PSU), A. P. Beardmore (U Leicester),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU),
S. T. Holland (CRESST/USRA/GSFC), F. E. Marshall (NASA/GSFC),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (PSU), J. L. Racusin (PSU), B. Sbarufatti (INAF-IASFPA),
M. H. Siegel (PSU), M. Stamatikos (NASA/ORAU) and M. A. Stark (PSU)
report on behalf of the Swift Team:

At 21:03:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090715B (trigger=357512).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 251.344, +44.827 which is 
   RA(J2000) = 16h 45m 23s
   Dec(J2000) = +44d 49' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked 
structure with a duration of about 100 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 21:04:00.9 UT, 46.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 251.3405, +44.8377 which is equivalent to:
   RA(J2000)  = 16h 45m 21.71s
   Dec(J2000) = +44d 50' 15.7"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 39 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 53 seconds after the BAT trigger. There is a weak source in
2.7'x2.7' sub-image near the edge of the XRT error circle at the position of
  RA(J2000) = 16:45:21.62
  Dec(J2000) = +44:50:21.3
The estimated white magnitude 20.5 with an estimated error of 0.5 mag. 
No correction has been made for the expected extinction corresponding 
to E(B-V) of 0.01. 

Swift autonomous slewing to new GRBs was enabled just prior to this
burst.  It was disabled previously due to an anomaly with the
on-board solid state recorder.  That problem is now resolved. 

Burst Advocate for this burst is L. Vetere (vetere AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9670
SUBJECT: GRB 090715B - Liverpool Telescope Optical Afterglow Candidate
DATE:    09/07/16 00:25:24 GMT
FROM:    Carole Mundell at ARI, JMU,Liverpool  <cgm@astro.livjm.ac.uk>

R.J. Smith, C.G. Mundell, A. Melandri, I.A. Steele, S. Kobayashi, C.J. 
Mottram, D.F. Bersier, Z. Cano (Liverpool JMU), A. Gomboc (Ljubljana), C. 
Guidorzi (INAF-OAB) report:

"The 2-m Liverpool Telescope robotically followed up GRB090715
(SWIFT trigger 357512; Vetere et al. GCN 9668) beginning 11.07 min after 
the GRB trigger time.

An uncatalogued course is detected at:

  16 45 21.67 +44 50 21 (J2000) (positional uncertainty +/-1")

         with magnitude r' = 19.6 +/- 0.2 mag (wrt SDSS) at T=11.53 min.

Observations and analysis are ongoing.

This message may be cited"


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9671
SUBJECT: GRB 090715B: NOT optical observations
DATE:    09/07/16 01:42:48 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@astro.ku.dk>

D. Malesani (DARK/NBI), T. Augusteijn (NOT), C. Mackay, D. King, T. 
Staley (IoA Cambridge), A. De Cia and P. Jakobsson (Univ. Iceland) 
report on behalf of a larger collaboration:

We observed the field of GRB 090715B (Vetere et al., GCN 9668) with the 
NOT equipped with StanCam, in the V, R, and I filters.

In a single 180 s exposure starting on 2009 July 16.040 UT (3.91 hr 
after the GRB), we clearly detect the object reported by Vetere et al. 
(GCN 9668) and Smith et al. (GCN 9670) with a magnitude R = 19.92 +- 
0.03 (assuming R = 17.16 for the USNO star at 16:45:24.24, +44:50:57.3). 
Although our measurement indicates only moderate fading when compared to 
the value by Smith et al. (GCN 9670), the object is missing from the 
SDSS frames of this field, and is thus very likely the afterglow of GRB 
090715B.


GRB_name: GRB090715B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9672
SUBJECT: GRB 090715B: Swift-BAT refined analysis
DATE:    09/07/16 03:12:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU), L. Vetere (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090715B (trigger #357512)
(Vetere, et al., GCN Circ. 9668).  The BAT ground-calculated position is
RA, Dec = 251.337, 44.837 deg, which is 
   RA(J2000)  =  16h 45m 20.9s 
   Dec(J2000) = +44d 50' 12.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a series of peaks.  The first starts
at ~T-10 sec, peaks at ~T+7 sec, and returns almost to background at T+35 sec.
The second peak start at ~T+45 sec and ends at ~T+100 sec.  The third peak
starts at ~T+230 sec and ends at ~T+290 sec.
T90 (15-350 keV) is 266 +- 11 sec (estimated error including systematics).
 
The time-averaged spectrum from T-11.6 to T+292.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.57 +- 0.07.  The fluence in the 15-150 keV band is 5.7 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.46 sec in the 15-150 keV band
is 3.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/357512/BA/


GRB_name: GRB090715B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9673
SUBJECT: GRB090715B: WHT redshift
DATE:    09/07/16 05:19:03 GMT
FROM:    Klaas Wiersema at U of Leicester  <kw113@star.le.ac.uk>

K. Wiersema (Leicester), A. Levan (Warwick), A. Kamble (Amsterdam), N. 
Tanvir (Leicester) and D. Malesani (DARK/NBI) report on behalf of a larger 
collaboration:

We observed the afterglow of GRB090715B (Vetere et al, GCN 9668; Smith et 
al GCN9 670) with the William Herschel Telescope, using the ISIS 
spectrograph. Exposure times were 3 x 900 seconds with the R300B and R316R 
grisms in the blue and red arm respectively, starting at 23:46 UT. We 
detect a multitude of lines, including Lyman alpha, Lyman beta, SiII and 
SII at redshift z=3.00.

We thank T. Ottosen for acquiring this dataset.


GRB_name: GRB090715B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9674
SUBJECT: GRB 090715B: Swift XRT Refined Analysis
DATE:    09/07/16 05:45:40 GMT
FROM:    Loredana Vetere at PSU  <vetere@astro.psu.edu>

L. Vetere (PSU) reports on behalf of the Swift-XRT team:

We have analysed ~2 ks of XRT data for GRB 090715B (Vetere et al. GCN
Circ. 9668), from 52 s to 10.2 ks after the BAT trigger. The data
comprise 471 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The refined XRT position for this burst is
Ra, Dec 251.340   44.838 which is:

    RA(J2000) = 16h 45m 21.7s
    Dec(J2000) = +44d 50' 18.1"

The light curve shows multiple peaks in WT and a power-law decay in PC  
with a
decay index of alpha=1.1(+/-0.2).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.84 (+/-0.02). The
best-fitting absorption column is 1.09 (+/-0.02) x 10^21 cm^-2, in
excess of the Galactic value of 1.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.3 (+/-0.3) and a
best-fitting absorption column of 1.4 (+/-0.1) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.8 x 10^-11 (5.8 x 10^-11) erg cm^-2
count^-1.

If the light curve continues to decay with a power-law decay index of
1.1, the count rate at T+24 hours will be 0.02 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.6 x
10^-13 (1.2 x 10^-12) erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9675
SUBJECT: GRB 090715B: Observation of the optical afterglow
DATE:    09/07/16 08:27:41 GMT
FROM:    Angelo Antonelli at Obs. Astro. di Roma  <a.antonelli@oa-roma.inaf.it>

L. A. Antonelli (INAF-OAR), S. Marinoni (INAF-TNG), F. Montalvo (UNAM- 
OAN), A. Vazquez (UNAM-IA) report:

We observed the field of GRB 090715B (Vetere et al., GCN 9668) with  
the 1.5 m Telescope in San Pedro Martir (BCN-Mexico) equipped with  
LaRuca, in the B, V, and R filters.

We started observations on 2009 July 16.1729 UT (7.07 hrs after the  
burst) and we detect the object reported by Malesani et al., (GCN  
9671), Smith et al. (GCN 9670) and Vetere et al. (GCN 9668) in all  
filters. The object has a magnitude R = 20.4 +- 0.1 (calibrated  
against USNO B1). The object has faded with respect of the value  
reported by Malesani et al., (GCN 9671) with a decay index of 0.77 
+-0.39. Due to its fading behavior we can confirm that it is the  
optical afterglow of GRB 090715B.

This message can be cited.


GRB_name: GRB090715B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9676
SUBJECT: GRB 090715B: Enhanced Swift-XRT position
DATE:    09/07/16 11:11:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2329 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 090715B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 251.33969, +44.83889 which is equivalent
to:

RA (J2000): 16h 45m 21.53s
Dec (J2000): +44d 50' 20.0"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9677
SUBJECT: GRB 090715B: break in the optical afterglow decay
DATE:    09/07/16 11:49:28 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), Z. Cano, A. Melandri, C.G. Mundell,
R.J. Smith, I.A. Steele,  D. Bersier, S. Kobayashi (Liverpool JMU),
A. Gomboc (U. Ljubljana) on behalf of a large collaboration report:

We began observing the Swift GRB 090715B (Vetere et al. GCN Circ. 9668)
with the Liverpool Telescope (LT) on July 15, 21:14:19 UT
(11.0 min post BAT trigger) with the SDSS riz filters,
confirming the detection of the optical afterglow seen by
Swift-UVOT (Smith et al. GCN Circ. 9670; Malesani et al GCN
Circ. 9671; Antonelli et al. GCN Circ. 9675).
Observations with the LT carried on until 5.6 hours post burst.
Our measurements are in agreement with the value reported by
Malesani et al. (GCN Circ. 9671) after correcting for the
different calibration.

We also observed the OT with the Faulkes Telescope North (FTN)
from July 16, 09:45:46 UT (i.e., at 12.71 hours) with the R filter.

The light curve in the r filter from 0.18 to 12.7 hours can be
fitted with a broken power-law with alpha1=0.25 +/- 0.02,
t_break =18 (-3, +12) ks, alpha2~0.7.


Telescope   Mid Time   Exposure  Filter   Mag
            (hours)     (s)
------------------------------------------------------
FTN         12.90      1200        R     20.98 +- 0.05
------------------------------------------------------

Calibration was performed against the SDSS star mentioned
by Malesani et al. (GCN 9671), assuming r'=17.74 and R=17.54.


GRB_name: GRB090715B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9678
SUBJECT: GRB 090715B: Swift/UVOT followup observations
DATE:    09/07/16 12:32:09 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. Breeveld (MSSL/UCL) and L. Vetere (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090715B
53 s after the BAT trigger (Vetere et al., GCN Circ. 9668).
The optical afterglow reported in Vetere et al., GCN 9668 and  
confirmed by Smith et al., GCN 9670, Malesani et al., GCN 9671,  
Wiersema et al., GCN 9673 and Antonelli et al., GCN 9675 is detected  
by the UVOT only in the initial white exposure. The detected magnitude  
and preliminary 3-sigma upper limits obtained using a 3" aperture and  
the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent summed exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC         53            203          147         20.37 +/- 0.15
white            4052         4252          196         >21.3
v                    5989       22687          795         >21.0
b                    3848         4047          197         >20.3
u                      266       16495          428         >21.2
w1              12053       16278          894         >21.2
m2                6195       10367          826         >21.0
w2                4258       22065          995         >21.4

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090715B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9679
SUBJECT: Konus-Wind and Konus-RF observations of GRB 090715B
DATE:    09/07/16 12:52:47 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long GRB 090715B (Vetere et al., GCN 9668)
triggered Konus-Wind at T0=75799.008 s UT (21:03:19.008),
and Konus-RF instrument onboard CORONAS-PHOTON s/c
at T0(KRF)=75798.895 s UT (21:03:18.895).

The burst had a multi-peaked structure with a duration of ~100 s.
The Konus-Wind light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090715_T75799/

As observed by Konus-Wind, the burst had a fluence
of 9.3(-1.1,+1.5)x10-6 erg/cm2,
and a 256-ms peak flux, measured from T0+4.912 s,
of 9.0(-2.5,+2.5)x10-7 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+82.176 s) is well fitted
(in the 20 keV - 2 MeV range) by a power-law with
exponential cutoff (CPL) model:
dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak), for which:
the photon index alpha = -1.1(-0.34,+0.4), and
the peak energy Ep = 134(-30,+56) keV (chi2 = 57/61 dof).

The spectrum at the maximum count rate,
measured from T0 to T0+8.448 s, is also well fitted
(in the 20 keV - 2 MeV range) by CPL model, for which:
the photon index alpha = -0.86(-0.20,+0.22), and
the peak energy Ep = 178(-23,+33) keV (chi2 = 49/61 dof).

All the quoted values are preliminary.
The quoted errors are at the 90% confidence level.


GRB_name: GRB090715A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9680
SUBJECT: GRB 090715A: Swift-BAT refined analysis
DATE:    09/07/16 13:24:23 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC),
J. L. Racusin (PSU), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090715A (trigger #357498)
(Racusin, et al., GCN Circ. 9666).  The BAT ground-calculated position is
RA, Dec = 152.102, 10.006 deg, which is 
   RA(J2000)  =  10h 08m 24.5s 
   Dec(J2000) = +10d 00' 22.4" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.
 
The mask-weighted light curve shows a single spike starting at ~T-0.1 sec,
peaking at ~T+0.1 sec, and ending at ~T+0.7 sec.  Following the intial spike,
there is extended emission from ~T+20 to ~T+55 sec at a flux level ~50 times
lower than the peak flux of the spike.  T90 (15-350 keV) is 63 +- 18 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.1 to T+67.8 sec is best fit by a simple
power-law model.  We note that this spectral analysis includes both
the spike and the extended emission.  Qualitatively, the spike is harder
than the extended emission. The power law index of the time-averaged spectrum is
1.28 +- 0.42.  The fluence in the 15-150 keV band is 9.8 +- 2.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.11 sec in the 15-150 keV band
is 3.9 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/357498/BA/


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9681
SUBJECT: GRB 090715B: MASTER optical limit
DATE:    09/07/16 13:32:17 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

D.Kuvshinov, V. Lipunov, V.Kornilov,  E. Gorbovskoy,
A.Belinski,  A. Krylov, N.Shatskiy, N.Tyurina, P.Balanutsa, V.V.Chazov, 
P.V.Kortunov
Sternberg Astronomical Institute, Moscow State University

A. Tlatov, A.V. Parkhomenko,
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinski, I.Zalognikh, T.Kopytova, Alexander Popov
Ural State University, Kourovka

S.Yazev, K.Ivanov
Irkutsk State University



MASTER  robotic telescope (MASTER-Net: http://observ.pereplet.ru, 
355 mm, 6 square degrees, 16Mpx Apogee CCD) located
at Vostrykovo (Moscow) responded to the  GRB 090715B (Swift 
trigger 357512,  L. Vetere , GCN 9668), producing images
beginning 19 s after the GCN notice time. An automated response took
the first image at 21:11:18 UT, 8m 04s after the  burst, under summer 
Moscow sky.
We have 160 images with 30 sec exposition each.
These unfiltered images are calibrated relative to USNO 08.R+0.2B (Usno 
A2.0).

Individual images have limiting magnitudes ranging from 17.8-17.0; we
set the following specific limits.

GRB_time     start UT       end UT      t_exp(s)   mlim     Coadd?
-------------------------------------------------------------------

484 - 514s    21:11:18      21:41:18        30      17.8       no
484 - 699s    21:11:18      21:14:57        90      18.5        3 
484 - 6699S   21:11:18      22:54:27      3330      20.0       111



Robot do not detect OT with limit 20.0 .

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB090715A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9682
SUBJECT: Konus-Wind observations of short/hard GRB 090715A
DATE:    09/07/16 17:34:07 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline
on behalf of the Konus-Wind team, report:

The short hard GRB 090715A (Swift trigger=357498:
Racusin et al., GCN 9666; Baumgartner et al., 9680)
triggered Konus-Wind at T0=62736.657 s UT (17:25:36.657).

The burst had a duration of ~0.32 s.
The Konus-Wind light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090715_T62736/

As observed by Konus-Wind the burst had
a fluence of 3.5(-1.5,+2.1)x10-6 erg/cm2, and
a 16-ms peak flux measured from T0+0.016 s
of 2.0(-0.8,+1.2)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+0.128 s) is well fitted (in the 20 keV - 10 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.13(-0.25,+0.42),
and Ep = 1658(-1010,+3957)keV (chi2 = 8.9/13 dof).

Fitting by GRB (Band) model yields:
the low-energy photon index alpha = -0.90(-0.45,+1.2),
the high energy photon index beta < -1.5,
the peak energy Ep = 738(-614,+3775) keV (chi2 = 8.2/12 dof).

The emission is clearly seen up to 7 MeV.

All the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB090715A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9683
SUBJECT: GRB 090715A:  VLA observations
DATE:    09/07/17 03:04:11 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger and W.-f. Fong (Harvard) report:

"We observed the field centered on the BAT error circle of the short GRB 
090715A (GCNs #9666,9680) with the VLA at a frequency of 8.46 GHz 
starting on 2009 July 16.98 UT (30.1 hours post burst).  We detect a
single bright source within the BAT error circle which is cataloged in
the VLA FIRST survey and is moreover extended.  No other sources are
detected within the BAT error circle above a 4-sigma level of 85
microJy.  In addition, we do not detect any point source in coincidence
with the nearby galaxy NGC3130."


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9684
SUBJECT: GRB 090715B: Lick observations
DATE:    09/07/17 17:28:04 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, J. Choi, A. Morton and M. Ganeshalingam (UC Berkeley) report:

We obtained a series of R-band exposures of the optical transient
associated with GRB 090715B  (GCN 9668, Vetere et al.; GCN 9670, Smith et
al.) at the 1-meter Nickel telescope at Lick Observatory under clear skies
and good seeing.  The transient is detected in individual frames.  We
report the following magnitudes relative to the calibration star of
Malesani et al. (GCN 9671):

t_start(UT)  exp(s)        mag                  t-t0(hr)
06:17:06.10   120    R = 20.23 +/- 0.21           9.23
06:27:36.17   200    R = 20.27 +/- 0.16           9.41
06:31:53.21   200    R = 20.06 +/- 0.14           9.48
06:42:53.80   300    R = 20.48 +/- 0.17           9.66
06:54:57.78   300    R = 20.40 +/- 0.16           9.86
07:01:01.97   300    R = 20.39 +/- 0.20           9.96
07:07:07.30   300    R = 20.24 +/- 0.14           10.07
07:19:01.36   300    R = 20.47 +/- 0.18           10.26
07:32:15.82   300    R = 20.71 +/- 0.23           10.44

A stack of all images gives an average magnitude of R = 20.23 +/- 0.07.


GRB_name: GRB090709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9685
SUBJECT: GRB 090709A - CARMA mm Observations
DATE:    09/07/17 22:01:56 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan,  G. C. Bower (UC Berkeley), report:

We observed the field of GRB 090709A (Morris et al., GCN 9625) with
the Combined Array for Research in Millimeter-Wave Astronomy (CARMA)
at an average frequency of 88.5 GHz beginning at 2009-07-15 04:41:33
UT, ~5.88 days after the Swift trigger.  No source was detected at the
position of the NIR/optical afterglow (Aoki et al., GCN 9634; Morgan
et al., GCN 9635; Cenko et al., GCN 9646; Guidorzi et al., GCN 9648)
down to the following limits:

post_burst
t_mid(d)  exp(h)  freq_mid(GHz)  bandwidth(MHz)  flux (mJy)
5.98      3.79    88.5           3000            < 1.1 (3 sig)

The quasar 1849+670 was used as a phase calibrator, and fluxes were
calibrated to an observation of Neptune taken at the end of the track.

We thank the staff and observers at CARMA and instructors of the CARMA
Summer School for excellent support during the observations and
analysis.


GRB_name: GRB090715A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9686
SUBJECT: GRB 090715A: Suzaku WAM observation of the prompt emission
DATE:    09/07/18 10:53:24 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

S. Sugita, K. Yamaoka (Aoyama Gakuin U.), M. Ohno, M. Suzuki, 
M. Kokubun, T. Takahashi (ISAS/JAXA), M. Tashiro, Y. Terada, 
A. Endo, K. Onda, W. Iwakiri, T. Sugasahara (Saitama U.), 
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, 
E. Sonoda, K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi 
(Univ. of Miyazaki), N. Vasquez (Tokyo Tech.), Y. Urata (NCU), 
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), 
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong 
(Nihon U.), on behalf of the Suzaku WAM team, report:

The short hard GRB 090715A (Swift/BAT trigger #357498; 
Racusin et al., GCN 9666; Baumgartner et al., GCN 9680) 
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an 
energy range of 50 keV - 5 MeV at 2009-07-15 17:25:39.033 UT (=T0). 

The observed light curve shows a multi-peaked structure, starting at 
T0+0.05 s and ending at T0+0.70 s, with a total duration (T90) of about 0.5 s. 
The fluence in 100 - 1000 keV was 1.13(-0.20, +0.08) x10^-6 erg/cm^2.  
The 1-s peak flux measured from T0 s was 2.25(-0.29, +0.12) photons/cm^2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0 s to T0+1 s is well fitted by a power-law with exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha:     0.76(-0.46, +0.37), and
  Epeak:     588(-118, +216) keV (chi^2/d.o.f. = 18.1/30).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst will be available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9687
SUBJECT: GRB 090715B: further NOT optical observations
DATE:    09/07/18 15:31:46 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@astro.ku.dk>

D. Malesani (DARK/NBI), G. C. Cox (NOT), C. Mackay, D. King, T. Staley 
(IoA Cambridge), and P. Jakobsson (Univ. Iceland) report on behalf of a 
larger collaboration:

We observed again the field of GRB 090715B (Vetere et al., GCN 9668) 
using the NOT telescope equipped with the StanCam instrument. The 
optical afterglow (Vetere et al., GCN 9668; Smith et al., GCN 9670) is 
well detected in the V and R filters, and is still bright. Using the 
same reference star as in GCN 9671, we measure R ~ 21.3 on mean time 
July 17.94 UT (2.06 days after the GRB).

Assuming an unbroken power-law fading (Fnu propto t^-alpha), the 
corresponding decay index is alpha ~ 0.44, which is unusually flat at 
such late epoch (although not unprecedented). Our measurement is also 
consistent within the uncertainties with the broken power-law fit 
reported by Guidorzi et al. (GCN 9677).

DM thanks Carole G. Mundell and Cristiano Guidorzi for discussion.


GRB_name: GRB090720A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9688
SUBJECT: GRB 090720: Fermi GBM detection
DATE:    09/07/20 14:44:23 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 06:38:08.28 UT on 20 July 20009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090720 (trigger 269764690 / 090720276).

The on-ground calculated location, using the GBM trigger
data, is RA = 199.5, DEC = -16.4 (J2000 degrees,
equivalent to 13 h 18 m, -16 d 24 '), with an uncertainty
of 5.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 113 degrees.

This burst was also independently detected (but not triggered) by 
INTEGRAL SPI-ACS.

The GBM light curve shows a single peak
with a duration (T90) of about 7.0 s (8-1000 keV).
The time-averaged spectrum from T0-1.856 s to T0+5.312 s is
best fit by a power law function with an exponential
high energy cutoff.  The power law index is -0.75 +/- 0.10 and
the cutoff energy, parameterized as Epeak, is 117.50 +/- 7.12 keV
(chi squared 507 for 507 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(2.9 +/- 0.1)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.002 s in the 8-1000 keV band
is 10.9 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090718A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9689
SUBJECT: GRB 090718: Fermi GBM detection
DATE:    09/07/20 14:45:43 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"At 17:16:42.93 UT on 18 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090718 (trigger 269630204 / 090718720).
The on-ground calculated location, using the GBM trigger data, is
RA = 242.5, DEC = -6.6 (J2000 degrees, equivalent to 16h10m, -6d35'),
with an uncertainty of 7.4 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error
which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 51 degrees.
Since the source is weak, the time-averaged spectrum is poorly constrained."


GRB_name: GRB090718B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9690
SUBJECT: GRB 090718B: Fermi GBM detection
DATE:    09/07/20 14:49:19 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"At 18:17:42.84 UT on 18 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090718B (trigger 269633864 / 090718762).
The on-ground calculated location, using the GBM trigger data, is
RA = 274.1, DEC = -36.4 (J2000 degrees, equivalent to 18h16m, -36d23'),
with an uncertainty of 1.2 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which
is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 76 degrees.

The GBM light curve consists of several peaks with
a duration (T90) of about 28 s (8-1000 keV).
The time-averaged spectrum from T0 to T0+29.7 s is well fit by
a power law function with an exponential high energy cutoff.  The
power law index is -1.21 +/- 0.02 and the cutoff energy, parameterized
as Epeak, is 198 +/- 9 keV (chi squared 507 for 480 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(2.52 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+21.5 s in the 8-1000 keV band
is 32.0 +/- 0.5 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 504 for
479 d.o.f.) with Epeak = 184 +/- 9 keV, alpha = -1.18 +/- 0.03 and
beta = -2.59 +/- 0.26.

The temporal and spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090719A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9691
SUBJECT: GRB 090719: Fermi GBM detection
DATE:    09/07/20 14:53:16 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"At 01:31:26.61 UT on 19 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090719 (trigger 269659888 / 090719063).
The on-ground calculated location, using the GBM trigger data, is
RA = 341.3, DEC = -67.9 (J2000 degrees, equivalent to 22h45m, -67d52'),
with an statistical uncertainty of less than 1 degree (radius, 1-sigma
containment), and an additional systematic error which is currently
estimated to be 2 to 3 degrees.
The angle from the Fermi LAT boresight is 88 degrees.

The GBM light curve consists of a bright pulse with some substructure,
with a duration (T90) of about 16 s (8-1000 keV).
The time-averaged spectrum from T0 to T0+16.6 s is best fit by
a Band function with Epeak = 254 +/- 6 keV, alpha = -0.68 +/- 0.02,
and beta = -2.92 +/- 0.16 (chi squared 652 for 483 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(4.83 +/- 0.04)E-5 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+4.4 s in the 8-1000 keV band
is 37.8 +/- 0.5 ph/s/cm^2.

The temporal and spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090717A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9692
SUBJECT: GRB 090717: Fermi GBM detection
DATE:    09/07/20 14:54:27 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

E. Kara (NASA MSFC/Barnard College), S. Guiriec (UAH) and V. Chaplin (UAH)
report on behalf of the Fermi GBM Team:

"At 00:49:32.11 UT on 17 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090717 (trigger 269484574 / 090717034).

The on-ground calculated location, using the GBM trigger
data, is RA = 86.8, DEC = -64.2 (J2000 degrees,
equivalent to 05 h 47 m, -64 d 12 '), with an uncertainty
of 1.0 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 70 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.


The GBM light curve shows two peaks
with a duration (T90) of about 70 s (8-1000 keV).
The time-averaged spectrum of the two peaks fit
together from T0+2.8 s to T0+12.0 s and T0+44.8 to T0+52.0 is
adequately fit by a Band function with Epeak = 120 +/- 5 keV,
alpha = -0.88 +/- 0.04, and beta = -2.33 +/- 0.06

(chi squared 967 for 845 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(4.5 +/- 0.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.8 s in the 8-1000 keV band
is 7.8 +/- 0.7 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090717B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9693
SUBJECT: GRB 090717B: Fermi GBM detection
DATE:    09/07/20 14:56:58 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 02:40:31.79 UT on 17 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090717B (trigger 269491233 / 090717111).

The on-ground calculated location, using the GBM trigger
data, is RA = 247.0, DEC = 23.0 (J2000 degrees,
equivalent to 16 h 28m m, 23 d 00 '), with an uncertainty
of 3.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 35 degrees.

This burst was also independently detected (although not triggered) by 
INTEGRAL SPI-ACS.

The GBM light curve consists of a single peak
with a duration (T90) of about 0.9 s (8-1000 keV).
The time-averaged spectrum from T0-0.256s to T0+0.128 s is
adequately fit by a simple power law function with index -1.02 +/- 0.04
(chi squared 604 for 732 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(4.83 +/- 0.03)E-07 erg/cm^2. The 0.384-sec peak photon flux measured
starting from T0-0.256 s in the 8-1000 keV band
is 3.91 +/- 0.42 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090720A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9694
SUBJECT: GRB 090720 Source found in ground processing of Swift-BAT data
DATE:    09/07/20 17:35:54 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (NASA/GSFC/CRESST), S. Holland (NASA/GSFC/CRESST),
M. Stamatikos (NASA/ORAU) on behalf of the Swift Team

At 06:38:08 on July 20, 2009 Swift-BAT rate-triggered on GRB 090720
(BAT trigger #357811). The burst was also detected by the Fermi
GBM (trigger #269764690, Rau, GCN #9688). No source was found
onboard in automated processing. A significant source on the edge
of the BAT field of view was found in ground processing. The
position was RA, Dec 203.694, -10.335, which is equivalent to:

RA (J2000) 13h 34m 46.6s
Dec (J2000) -10d 20m 06s

with an error radius of 3 arcmin (estimated 90% containment). This
was 6 degrees from the Fermi GBM ground position, just outside the
GBM 1-sigma radius.

As seen in BAT, the burst was a single weak pulse about 3 seconds
long.

A Swift TOO has been requested and approved.

The Swift Burst Advocate for this burst is Erik Hoversten (hoversten
at astro dot psu dot edu). Please contact the BA by email if you
require additional information regarding Swift followup of this
burst. In extremely urgent cases, after trying the Burst Advocate,
you can contact the Swift PI by phone (see Swift TOO web site for
information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090715B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9695
SUBJECT: GRB 090715B: VLA radio detection
DATE:    09/07/20 19:54:32 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of a
larger collaboration:

"We used the Very Large Array (VLA) to observe the field of view towards
 the GRB 090715B (GCN 9668) at a frequency of 8.46 GHz on 2009 Jul. 20.14
UT. We clearly detect the GRB afterglow at the Swift UVOT afterglow
position (GCN 9668). The peak flux at the GRB afterglow position is
231+/-47 uJy.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB090709A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9696
SUBJECT: GRB 090709A: Swift XRT Timing Analysis
DATE:    09/07/21 12:18:24 GMT
FROM:    Nestor Mirabal at U.Complutense de Madrid  <mirabal@gae.ucm.es>

N. Mirabal (U. Complutense de Madrid) and E. V. Gotthelf (Columbia U.)
report:

In light of recent reports of quasi-periodic variations in the
gamma-ray light curve of GRB 090709A (Markwardt et al., GCN 9645;
Golenetskii et al., GCN 9647, Gotz et al., GCN 9649; Ohno et al.,
GCN 9653), we have analyzed Swift XRT observations of GRB 090709A
obtained between 2009 July 9.319 UT and 2009 July 11.862 UT
(79s - 61 hr after the trigger assuming T at 2009 July 9, 07:38:34 UT).
This period overlaps the BAT light curve from T+79 s to T+150 s
(Markward et al., GCN 9645). The first set of observations (390 s) was
taken in WT mode (1.77 ms timing resolution),  followed by three
pointings in PC mode (2.5 s timing resolution). Fast Fourier
Transform (FFT) analysis applied to the light curves
in each interval shows no significant power down to the Nyquist
limit of f < 283 Hz and f < 2 Hz, for the WT and PC mode data,
respectively. Furthermore, the power spectrum of the first 120 s
of WT mode data (79-469 s after the trigger) does not reveal
any significant signal. The FFTs show typical characteristics of both
white and red noise during the interval. The absence of oscillations in
the X-ray band appears to rule out coherent quasi-periodic variations
extending beyond T+150 s. We note that the 8-second cycle derived from
the gamma-ray light curve seems at odds with the spin period P ~ 1 ms
required to produce an energy release Egamma ~ 10^50 erg from a magnetar
engine (Thompson et al. 2004, ApJ, 611, 380), unless the neutron star 
was born
a millisecond pulsar and spun down to a 1-8 s period (depending on the
actual GRB redshift) on a ~10 s timescale.

The power spectrum of the GRB 090709A light curve (WT mode, 79-469 s
after the trigger) can be found at:

http://www.gae.ucm.es/~mirabal/grbs/grb090709a/grb090709a_fft.gif


GRB_name: GRB090720A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9697
SUBJECT: Swift XRT and UVOT refned analysis of GRB 090720
DATE:    09/07/22 13:34:27 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe (PSU), S. R Oates (MSSL-UCL), E. A. Hoversten (PSU), P.A.  
Evans and M.R. Goad (U. Leicester) report on behalf of the Swift team:


Swift XRT and UVOT started observing the field of GRB 090720 11 hours  
after the Fermi GBM  and Swift/BAT triggers (Rau et al. GCN circ 9688,  
Cummings et al. GCN circ 9694).

Using 1233 s of XRT Photon Counting mode data and one UVOT image, we  
find an astrometrically corrected X-ray position (using the XRT-UVOT  
alignment and matching UVOT field sources to the USNO-B1 catalogue):  
RA, Dec = 203.68020, -10.33480 which is equivalent to:

RA (J2000):  13 34 43.25
Dec (J2000): -10 20 05.3

with an uncertainty of 3.0 arcsec (radius, 90% confidence).

This position may be improved as more data are received.  The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

Swift has continued observing the field of GRB 090720 and the source  
is clearly fading. Currently it is at a level of less than 1.6e-3  
counts/s (or 5.0 e-14 ergs/s/cm2). Due to the low number of counts, no  
spectral analysis can be performed.

With the Swift/UVOT,  we do not detect any source at the Swift XRT  
position. The 3-sigma upper limits for the summed exposures is:

Filter   T_start(s)   T_stop(s)   Exp(s)  Mag (3-sigma upper limit)
-------------------------------------------------------------
white      41,776      63,952      579          > 21.28
u          39,573      63,855      3513         > 21.10
-------------------------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.05 mag.
All photometry is on the UVOT photometric system described in Poole et
al. (2008, MNRAS, 383, 627).

This circular is an official product of the Swift team.

[GCN OPS NOTE(22jul09): Per author's request, in the 5th paragraph
the "finding chart exposure" was changed to "summed exposures".]


GRB_name: GRB090720B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9698
SUBJECT: GRB 090720B: Fermi GBM detection
DATE:    09/07/22 13:57:40 GMT
FROM:    Michael Burgess at UAH  <james.burgess@uah.edu>

J. M. Burgess (UAH), A. Goldstein (UAH) and A. J. van der Horst
(NASA/MSFC/ORAU) report on behalf of the Fermi GBM Team:

"At 17:02:56.91 UT on 20 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090720B (trigger 269802178 / 090720710).
The on-ground calculated location, using the GBM trigger
data, is RA = 203.0, DEC = -54.8 (J2000 degrees,
equivalent to 13h 32m, -54d 48'), with an uncertainty
of 2.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 56 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of two bright peaks with a
duration (T90) of about 20 s (8-1000 keV).
The time-averaged spectrum from T0+0.0 s to T0+20.1 s is well
fit by a power law function with an exponential high energy cutoff.
The power law index is -1.01 +/- 0.05 and the cutoff energy,  
parameterized
as Epeak, is 982 +/- 186 keV (chi squared 484 for 483 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(1.06 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.8 s in the 8-1000 keV band
is 10.9 +/- 0.4 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 482 for
482 d.o.f.) with Epeak= 924 +/- 201 keV, alpha = -1.00 +/- 0.05
and beta = -2.43 +/- 0.47.

The temporal and spectral analysis results presented above are  
preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090720A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9699
SUBJECT: GRB 090720:  Gemini-North Imaging and Optical Afterglow
DATE:    09/07/22 16:00:14 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara (PSU), S. B. Cenko (UC Berkeley), D. B. Fox (PSU),
E. Ofek (Caltech), N. Tanvir (U. Leicester) report:

"On April 21.26 UT and 22.24 UT we obtained two R-band images
of the Fermi/Swift GRB 090720 (GCN 9688,  9694) with GMOS on
the Gemini-North telescope for a total exposure time, at each
epoch, of 15 minutes.

In the coadded images we identify a possible R counterpart inside
the XRT error circle (Grupe et al., GCN 9697) at the coordinates:

RA (J2000): 13:34:43.33
Dec (J2000): -10:20:04.9

with an uncertainty of 0.5".

The estimated magnitude at the two epochs are:

R = 21.50 +- 0.03 mag
R = 22.34 +- 0.04 mag

The implied fading, by 0.84 +- 0.05 mag between our two epochs,
is consistent with a power-law decay of index alpha=1.12 +- 0.11
referenced to the burst trigger time.
We conclude from this fading behavior that the source is the optical
afterglow of GRB 090720.

Magnitude values are calibrated using the USNO B1 star at

RA= 13:34:39.9
Dec= -10:20:17.06

which has tabulated magnitude R = 19.79.
We thank the Gemini-N staff for the support in performing this
observations, in particular Tom Geballe and Paul Hirst."


GRB_name: GRB090720B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9700
SUBJECT: IPN Triangulation of bright GRB 090720B 
DATE:    09/07/22 16:08:03 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T.
Cline on behalf of the Konus-Wind team,

A. von Kienlin, A. Rau, and K. Hurley on behalf of the
INTEGRAL SPI-ACS GRB team,

M. Marisaldi, F. Fuschino, C. Labanti, M. Galli, G. Di Cocco
on behalf of the AGILE team,

K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, K. Makishima, and Y. Hanabata on behalf of the Suzaku-WAM 
team, and

V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi GBM
team, report:

Suzaku-WAM, Konus-Wind, AGILE-MCAL, and INTEGRAL (SPI-ACS) observed the 
bright GRB 090720B at about 17:02:57 UT (the Fermi/GBM trigger 
269802178/090720710: Burgess et al. GCN 9698).
We have triangulated this burst to a Konus-GBM annulus centered at 
RA(2000)=274.434 (18h 17m 44s)  Dec(2000)=-23.965 (-23d 57' 54"), whose 
radius is  60.824 +/- 0.031 (3 sigma).
Triangulation of the Konus-SPI-ACS gives an annulus centered
at RA(2000)=274.426 (18h 17m 42s)  Dec(2000)=-18.772 (-18d 46' 19"), 
whose radius is  64.910 +/- 0.252 (3 sigma).

Together, these 2 annuli yield a 3-sigma error box whose center and 
corners are:
-----------------------------------------------
      RA(2000), deg              Dec(2000), deg
-----------------------------------------------
Center:
   201.609 (13h 26m 26s)   -55.000 (-55d 00' 01")
Corners:
   201.763 (13h 27m 03s)   -59.798 (-59d 47' 54")
   201.580 (13h 26m 19s)   -58.693 (-58d 41' 36")
   201.793 (13h 27m 10s)   -50.725 (-50d 43' 29")
   201.823 (13h 27m 17s)   -51.627 (-51d 37' 36")
-----------------------------------------------

The error box area is 0.500 sq. deg and may be refined.

The GBM on-ground location (Burgess et al. GCN 9698) is consistent with 
the IPN box.

A map is posted at http://www.ioffe.ru/LEA/GRBs/GRB090720_T61379/IPN/
showing GBM contours (statistical) and best-fit position (star),
and the IPN annuli (solid lines with centers dot-dashed).

This map will also be posted at http://ssl.berkeley.edu/ipn3/090720B .

The IPN localization may be improved.


GRB_name: GRB090720B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9701
SUBJECT: Konus-Wind observations of bright hard GRB 090720B
DATE:    09/07/23 10:06:08 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline
on behalf of the Konus-Wind team, report:


GRB 090720B (Fermi/GBM trigger 269802178/090720710: Burgess et al., GCN 9698;
IPN localization box: Golenetskii et al., GCN 9700)
triggered Konus-Wind at T0=61379.486 s UT (17:02:59.486).

This bright hard GRB started with a series of several short spikes,
followed by a smoother structure. The emission is seen above 10 MeV
for the whole duration of the event (~16 s).
The Konus-Wind light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090720_T61379/

As observed by Konus-Wind the burst had a fluence
of 1.8(-0.5,+0.7)x10-5 erg/cm2, and
a 2-ms peak flux, measured from T0+0.186 s,
of 8.3(-2.8,+4.1)x10-5 erg/cm2/s
(both in the 20 keV - 15 MeV energy range).

The time-integrated spectrum of the burst, measured from T0 to T0+16.640 s,
is well fit (in the 20 keV - 15 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), with
alpha = -1.16(-0.13,+0.17), and
Ep = 1370(-580,+1190)keV (chi2 = 99/98 dof).

The spectrum at the maximum count rate, measured from T0+0.128 to T0+0.192 s,
is also well fit (in the 20 keV - 15 MeV range) by a power law with
exponential cutoff model, for which:
alpha = -0.47(-0.42,+0.71), and
Ep = 710(-280,+590)keV (chi2 = 7.3/8 dof).

All the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB090718B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9703
SUBJECT: Konus-RF and Konus-Wind observations of GRB 090718B
DATE:    09/07/24 11:08:04 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long GRB 090718B (Fermi/GMM trigger 269633864/09071876;
A.J. van der Horst, GCN 9690)
triggered Konus-RF instrument onboard CORONAS-PHOTON s/c
at T0=65863.878 s UT (18:17:43.878),
and Konus-Wind
at T0=65882.144 s UT (18:18:02.144),

The burst light curve shows a smooth structure
with a duration of ~35 s. The Konus-RF and Konus-Wind
light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090718_T65882/

As observed by Konus-RF the burst
had a fluence of 2.6(-0.13, +0.13)x10-5 erg/cm2,
and a 64-ms peak flux measured from T0+20.904 s
of 5.0(-0.24, +0.24)x10-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst
(from T0-2.0 to T0+34.0 s) is well fit
(in the 20 keV - 1 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -1.3  0.1,
the high energy photon index beta = -4.6( < -2.2),
the peak energy Ep = 250(-50, +35) keV (chi2 = 126/106 dof).

The spectrum of the burst at the maximum count rate
(from T0+20.5 to T0+21.0 s) is well fit
(in the 20 keV - 1 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.83  0.13,
the high energy photon index beta = -3.0( < -2.3),
the peak energy Ep = 245(-40, +45) keV (chi2 = 51/60 dof).

Due to uncertainties in the burst incident angle
the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.
--


GRB_name: GRB090719A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9704
SUBJECT: Konus-Wind and Konus-RF observations of GRB 090719
DATE:    09/07/24 12:11:25 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, and D. Svinkin on behalf of
the Konus-Wind and Konus-RF teams, and
T. Cline on behalf of the Konus-Wind team, report:

The long GRB 090719 (Fermi/GBM trigger 269659888/090719063;
A.J. van der Horst, GCN 9691)
triggered Konus-Wind at T0=05489.199 s UT (01:31:29.199),
and Konus-RF instrument onboard CORONAS-PHOTON s/c
at T0=05487.876 s UT (01:31:27.876),

The burst light curve shows a smooth structure
with a duration of ~20 s. The Konus-RF and Konus-Wind
light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090719_T05489/
===========================================================

As observed by Konus-Wind the burst
had a fluence of (4.6  0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.992 s,
of 9.4(-0.5, +0.6)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+16.128 s) is well fit
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.76  0.05,
the high energy photon index beta = -4.7( < -3.3),
the peak energy Ep = 260(-11, +10) keV (chi2 = 50/48 dof).

The spectrum at the maximum count rate
(from T0+4.096 to T0+5.120 s) is well fit
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.44(-0.56,+0.31),
the high energy photon index beta = -3.7( < -2.8),
the peak energy Ep = 328(-31, +32) keV (chi2 = 50/48 dof).
===========================================================

As observed by Konus-RF the burst
had a fluence of 5.2(-0.15, +0.15)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.368s,
of 1.1(-0.1, +0.1)x10-5 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0-2.0 to T0+20.0 s) is well fit
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.85  0.5,
the high energy photon index beta = -3.7( < -3.0),
the peak energy Ep = 286(-15, +15) keV (chi2 = 141/130 dof).

The spectrum at the maximum count rate
(from T0+3.0 to T0+3.5 s) is well fit
(in the 20 keV - 2 MeV range) by GRB (Band) model
for which:
the low-energy photon index alpha = -0.26(-0.19,+0.28),
the high energy photon index beta = -2.9( < -2.3),
the peak energy Ep = 327(-60, +60) keV (chi2 = 73/70 dof).
===========================================================

Due to uncertainties in the burst incident angles
the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.
-- 


GRB_name: GRB090726A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9706
SUBJECT: GRB 090726: Swift detection of a burst
DATE:    09/07/26 22:56:51 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), D. M. Palmer (LANL),
A. Rowlinson (U Leicester), M. H. Siegel (PSU), M. A. Stark (PSU) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 22:42:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090726 (trigger=358422).  Swift did not slew immediately
to the burst due to an Earth constraint. 
The BAT on-board calculated location is 
RA, Dec 248.819, +72.871 which is 
   RA(J2000) = 16h 35m 16s
   Dec(J2000) = +72d 52' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a small precursor
at T-20 followed by a single FRED structure overlaid with rapid
variability with a duration of about 50 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~10 sec after the trigger. 

Swift will not slew until T0+48.9 minutes. There will be no 
XRT or UVOT data until this time. 

Burst Advocate for this burst is K. L. Page (kpa AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090726A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9707
SUBJECT: GRB 090726: Swift-XRT position of probable counterpart
DATE:    09/07/27 00:18:24 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Following a delay caused by an Earth-limb constraint, the Swift-XRT 
started observing GRB 090726 about 49 minutes after the trigger, at 
23:36:32 UT. The XRT initially centroided on a cosmic ray; however, using 
promptly downlinked data we find an uncatalogued X-ray source with an 
enhanced position: RA, Dec = 248.6788, 72.8843 (degrees) which is 
equivalent to:

RA  (J2000) = 16 34 42.90
DEC (J2000) = +72 53 03.3

with an uncertainty of 2.2 arcsec (radius, 90% containment). This location 
is 156.1 arcseconds from the BAT onboard position, inside the BAT error 
circle.

It is not possible to determine whether the source is fading at this time.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090726A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9708
SUBJECT: GRB 090726: Swift/UVOT Finding Chart Observation
DATE:    09/07/27 01:06:32 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU), M. A. Stark (PSU) and K.L. Page (U. Leicester)  
report
on behalf of the Swift UVOT team:

UVOT observed GRB 090726 (Page et al., GCN Circ 9706) with a finding
chart exposure of 150 seconds with the White filter starting 3610
seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 8'x8' region for the list of
sources generated on-board covers 100% of the XRT error circle reported
by Page et al. (GCN Cic 9707). The list of sources is typically complete
to about 18 mag.  No correction has been made for the expected  
extinction
corresponding to E(B-V) of 0.04.


GRB_name: GRB090726A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9709
SUBJECT: GRB 090726: optical transient candidate
DATE:    09/07/27 03:50:30 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. Moskvitin, T. Fatkhullin & A. Valeev
(SAO-RAS Niznijh Arkhyz, Russia),
on behalf of a larger colaboration, report:

We have observed the field of GRB090618
(Page et al., GCN 9706) with the 1-m telesecope
of the SAO RAS in Caucasus. Within the XRT error
circle (Page et al., GCN 9707) we detected one
object which not present in the DSS. The object's
coordinates are:
    R.A. (J2000) = 16:34:43.044
    DEC. (J2000) = +72:53:04.82
with uncertainty about 0.5 arcsec. Using
the USNO A2.0 star 1628-0121951 (R2=14.51)
as a calibration we estimated the object's
brightness as following:

   R_mag         exp.(sec)       mid.time
                             (sec after the trigger)
18.26 +/- 0.05     60              2126
18.39 +/- 0.05     60              2252
18.33 +/- 0.05     60              2344
18.71 +/- 0.05    120              3183
18.97 +/- 0.05    180              4296
19.17 +/- 0.06    180              5492
19.28 +/- 0.07    240              6089
19.55 +/- 0.12    300              6824

According to its variability we concluded that
the detected object is the OT of the GRB090726.

Further analysis are ongoing.

This message may be cited.


GRB_name: GRB090726A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9710
SUBJECT: GRB 090726: Enhanced Swift-XRT position
DATE:    09/07/27 11:53:24 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 4286 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 090726, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 248.67985, +72.88426 which is equivalent
to:

RA (J2000): 16h 34m 43.16s
Dec (J2000): +72d 53' 03.4"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090726A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9711
SUBJECT: GRB 090726: Swift-XRT Team refined analysis 
DATE:    09/07/27 13:30:11 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

We have analysed the first five orbits of data collected for GRB 090726, 
comprising 9.4 ks between 3.6 and 28 ks after the trigger, all in Photon 
Counting mode. The enhanced XRT position for this burst was given by Evans 
et al. in GCN Circ. 9710.

The X-ray light-curve can be modelled with a single power-law with a decay 
index of alpha = 1.29 +/- 0.12.

A spectrum formed from these PC data can be fitted with an absorbed 
power-law of Gamma = 2.50 +0.26/-0.24 and a total absorbing column of NH = 
(1.2 +/- 0.5) x 10^21 cm^-2, which is in excess of the Galactic value 
(3.83 x 10^20 cm^-2; Kalberla et al. 2005). The counts to observed 
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum 
is 3.1 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1.

If the light-curve continues to decay with alpha ~ 1.29, the predicted 
count rate at 24 hours is 3.4 x 10^-3 count s^-1, corresponding to an 
observed (unabsorbed) flux of 1.1 x 10^-13 (1.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at 
http://www.swift.ac.uk/xrt_products/00358422.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090726A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9712
SUBJECT: GRB090726: 6-meter telescope redshift
DATE:    09/07/27 14:06:50 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

T. Fatkhullin (SAO RAS, Russia), J. Gorosabel  (IAA-CSIC, Spain),
A. de Ugarte Postigo (OAB-INAF, Italy), A. Moskvitin, A. Valeev,
S. Fabrika, O. Sholukhova (SAO RAS, Russia), A. Castro-Tirado
(IAA-CSIC, Spain) & V. Sokolov (SAO RAS, Russia) on behalf of a
larger colaboration, report:

Following the detection of the GRB090726 optical
transient (Moskvitin et al., GCN 9709) we observed
the afterglow with the SAO RAS 6-m telescope in
Caucasus using SCORPIO in the spectroscopic mode.
The wavelength coverage and resolution were
3700-7800AA and FWHM=10A, respectively.
One 10-min long exposure was obtained starting at
00:15 27 July 2009 UT (T-T0 = 1.545 hours after the
trigger). A number of absoption lines were detected
in the spectrum. These are  SiI 1526.7, CIV 1548.2,1550.8,
AlII 1670.8, SiII 1304.4,1309.3, SiIV 1393.7,1402.7,
FeII  1608.4 as well as Ly alpha at common z = 2.71
which we interpret as the GRB090726 redshift.

This message may be cited.

P.S. We made a typo in GCN 9709.
In the first line one should read "GRB090726"
instead of "GRB090618". We apologize for our carelessness.


GRB_name: GRB090711A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9713
SUBJECT: GRB 090711: Fermi GBM detection
DATE:    09/07/27 14:10:00 GMT
FROM:    Bill Paciesas at UAH  <bill.paciesas@nasa.gov>

Colleen A. Wilson-Hodge (NASA/MSFC)
reports on behalf of the Fermi GBM Team:

"At 20:23:22.92 UT on 11 July 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090711 (trigger 269036604 / 090711850).

The on-ground calculated location, using the GBM trigger
data, is RA = 139.6, DEC = -64.7 (J2000 degrees,
equivalent to 09 h 18 m, -64 d 42 '), with an uncertainty
of 1 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 13 degrees.

The GBM light curve consists of multiple peaks
with a duration of at least 100 s (8-1000 keV). The GBM detectors
were turned off for SAA entry about 83 seconds after the
trigger. The time-averaged spectrum from T0-20.992 s to T0+82.433 s is
adequately fit by a power law function with an exponential
high energy cutoff.  The power law index is 1.3 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 210 +/- 70  keV

The event fluence (8-1000 keV) in this time interval is
(1.17 +/- 0.16 )E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.536 s in the 8-1000 keV band
is 4.2 +/- 0.6 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090726A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9714
SUBJECT: GRB 090726: D50 optical observations
DATE:    09/07/27 14:27:51 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@asu.cas.cz>

Cyril Polasek (1), Jan Strobl (1), Martin Jelinek (2), Petr
Kubanek (3), Matus Kocka (1), Martin Nekola (1), Martin Blazek
(1) and Rene Hudec (1) (1. ASU Ondrejov, 2. IAA Granada, 3.
GACE Valencia)

We observed the localization of the Swift GRB090726 (Page et
al., GCN 9706) with the 50 cm telescope in Ondrejov (Czech
Republic), starting at 22:45:41 UT, i.e. 194s after the GRB
trigger.

We clearly detect the afterglow reported by Moskvitin et al.
(GCN 9709) in its rising phase on the first image with
magnitude ~ 18.3 (same calibration as GCN 9709). 

This message can be cited.


GRB_name: GRB090726A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9715
SUBJECT: GRB 090726: Afterglow candidate photometryfrom Crni Vrh
DATE:    09/07/27 15:43:32 GMT
FROM:    Jure Skvarc at OCV  <jure@ing.iac.es>

S. Maticic and J. Skvarc on behalf of PIKA observing program at Crni Vrh
Observatory.

We present photometry of the source reported by Moskvitin, Fatkhullin
and Valeev (GCN 9709). The object was observed from Crni Vrh
Observatory with a 60 cm telescope using R filter and a CCD.  First
exposure started at 2009-07-26 22:44:31 UT.  All twenty exposures were
of 60 s.  The table contains the time since the Swift GRB detection to
the middle of exposure in seconds, R magnitude and formal 1-sigma
magnitude error estimate.  Comparison stars were 1629-0117020,
1628-0121875 and 1628-0121948 using R2 magnitudes from the USNO B1.0
catalogue.

Time     Mag     Err.
  [s]     [R]    [1-sigma]
----------------------------------
  153.8   18.44   0.04
  224.9   18.35   0.04
  296.0   17.86   0.04
  367.2   17.69   0.04
  438.0   17.68   0.04
  508.8   17.75   0.04
  579.6   17.82   0.04
  650.3   17.76   0.04
  721.0   17.76   0.04
  791.8   17.83   0.04
  862.5   17.71   0.04
  933.3   17.83   0.04
1004.0   17.89   0.04
1074.7   18.05   0.04
1146.1   18.17   0.04
1218.2   18.11   0.04
1288.9   18.00   0.04
1359.6   18.02   0.04
1430.5   18.16   0.04
1501.5   17.96   0.04

This message can be cited.


GRB_name: GRB090726A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9716
SUBJECT: GRB 090726, Swift-BAT refined analysis
DATE:    09/07/27 15:57:17 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC),
C. B. Markwardt (GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. M. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the
recent telemetry downlink, we report further analysis
of BAT GRB 090726 (trigger #358422) (Page, et al.,
GCN Circ. 9706).  The BAT ground-calculated position is
RA, Dec = 248.681, 72.866 deg which is
   RA(J2000)  =  16h 34m 43.5s
   Dec(J2000) = +72d 51' 56.5"
with an uncertainty of 1.7 arcmin, (radius, sys+stat,
90% containment). The partial coding was 85%.

The mask-weighted light curve shows a weak single peak
starting at ~T-40 sec, peaking at ~T+5 aec,
and ending at ~T+70 sec. T90 (15-350 keV) is
67.0 +/- 15.2 sec (estimated error including systematics).

The time-averaged spectrum from T-34.7 to T+47.3 sec is
best fit by a simple power-law model.  The power law
index of the time-averaged spectrum is 2.25 +/- 0.19.
The fluence in the 15-150 keV band is
8.6 +/- 1.0 x 10^-07 erg/cm2. The 1-sec peak photon
flux measured from T+7.30 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are
at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/358422/BA/


GRB_name: GRB090726A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9717
SUBJECT: GRB090726: Swift/UVOT observations
DATE:    09/07/27 16:01:04 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.B. Landsman (NASA/GSFC) and K.Page (U. Leicester)report on behalf of 
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090726, 
3610s after the BAT trigger (Page et al., GCN Circ. 9706),  and the 
afterglow first reported by Moskvitin et al., (GCN Circ. 9709) is 
detected in the UVOT white, v, and b filters.

The initial magnitudes and upper limits are as follows:

Filter   T_start(s)  Exp(s)    Mag
white     3610       147   20.62  0.18
white     4179       197   21.36  0.29
v         4589       197   19.98  0.36
b         3974       197   20.80  0.44
u         3769       197   >20.9 (3 sigma)
uvw1      5000       197   >20.6 (3 sigma)
uvm2      4794       197   >20.6 (3 sigma)
uvw2      4385       197   >21.0 (3 sigma)

The nondetections in the u and UV filters are consistent with the 
redshift of z= 2.71 reported by Fatkhullin et al (GCN 9712)

The values quoted above are not corrected for the Galactic extinction 
due to the reddening of E(B-V) = 0.045 in the direction of the burst.
The photometry is on the UVOT photometric system described in Poole et 
al. (2008, MNRAS, 383, 627).


GRB_name: GRB090727A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9718
SUBJECT: GRB 090727: Swift detection of a burst
DATE:    09/07/27 22:59:22 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

P. A. Evans (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
M. M. Chester (PSU), S. T. Holland (CRESST/USRA/GSFC),
N. P. M. Kuin (MSSL), C. B. Markwardt (CRESST/GSFC/UMD),
K. L. Page (U Leicester), A. Rowlinson (U Leicester),
M. H. Siegel (PSU), M. A. Stark (PSU) and T. N. Ukwatta (GSFC/GWU)
report on behalf of the Swift Team:

At 22:42:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090727 (trigger=358520).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 315.972, +64.916 which is 
   RA(J2000) = 21h 03m 53s
   Dec(J2000) = +64d 54' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 25 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 22:43:46.0 UT, 87.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 315.96139, 64.92438 which is equivalent
to:
   RA(J2000)  = 21h 03m 50.73s
   Dec(J2000) = +64d 55' 27.8"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 34 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
2.48e+21 cm^-2 (Kalberla et al. 2005). 


UVOT took a finding chart exposure of nominal 150 seconds with the White filter
starting 91 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. Data from the 2.7'x2.7' sub-image are
not available at this time. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.54. 




Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9719
SUBJECT: GRB 090727: Liverpool Telescope possible OT candidate
DATE:    09/07/28 02:19:38 GMT
FROM:    James Smith at ARI,Liverpool John Moors U  <rjs@astro.livjm.ac.uk>

R.J. Smith, C.G. Mundell (Liverpool JMU) on behalf of a large 
collaboration report:

The 2-m Liverpool Telescope robotically reacted to GRB 090727 (SWIFT 
trigger 358520, Evans et al, GCN Circ. 9718), starting observing at 
22:44:59UTC. A source which is not visible in the digitized sky survey is 
detected in both SDSS r' and i' filters at position 21:03:50.6 +64:55:30 
J2000. This lies within the XRT error circle reported by Evans et al, GCN 
Circ. 9718. The approximate magnitude, calibrated with respect to nearby 
USNOB stars is R=21.3 +/- 0.2 and I = 20.2 +/- 0.2. The target is slightly 
crowded by brighter stellar sources and analysis is ongoing to determine 
if the OT candidate is fading.


GRB_name: GRB090715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9720
SUBJECT: GRB 090715B: Late-time Lick 3m observations
DATE:    09/07/28 06:13:01 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, N. R. Butler, and S. B. Cenko (UC Berkeley) report:

We obtained additional, late-time imaging of the field of GRB 090715B 
(GCN 9668, Vetere et al.; GCN 9670, Smith et al.) with the Lick 3m 
telescope (+PFCam) in the R-band filter under dark skies, good seeing 
conditions and thin cloud cover.   Observations were conducted on the 
night of 2009-07-24 (UT) between 04:46 and 06:15 UT, and consisted of 
seven 300-second exposures followed by four 600-second exposures.

The afterglow is faintly detected in the combined image.  Photometry 
relative to the reference star of Malesani et al. (GCN 9671) gives a 
magnitude of R = 23.6 +/- 0.3 mag at this time (t = 8.35 days after the 
GRB).

Relative to the NOT observation at 2.06 days (Malesani et al., GCN 
9687), this corresponds to a decay index of alpha ~ 1.5, indicating that 
the unusually long period of slow fading has ended and the optical 
afterglow has resumed a "normal" power-law decay.


GRB_name: GRB090727A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9721
SUBJECT: GRB 090727: Enhanced Swift-XRT position
DATE:    09/07/28 09:53:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 5314 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 090727, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 315.96078, +64.92481 which is equivalent
to:

RA (J2000): 21h 03m 50.59s
Dec (J2000): +64d 55' 29.3"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9722
SUBJECT: GRB 090727: Liverpool Telescope Afterglow Confirmation and Optical Flare
DATE:    09/07/28 10:35:59 GMT
FROM:    Carole Mundell at ARI, JMU,Liverpool  <cgm@astro.livjm.ac.uk>

R.J. Smith, C.G. Mundell, I.A. Steele,  A. Melandri, S. Kobayashi, C.J.
Mottram, D.F. Bersier, Z. Cano (Liverpool JMU), A. Gomboc (Ljubljana), C.
Guidorzi (INAF-OAB) report:

"Further analysis of the optical light curves of the uncatalogued optical 
source, at RA(J2000)=21:03:50.6, Dec(J2000)= +64:55:30, reported by Smith 
& Mundell (GCN Circ. 9719) show significant variability and confirm this 
object as the optical afterglow of GRB 090727 (SWIFT trigger 358520, 
Evans et al, GCN Circ. 9718; Goad et al. GCN Circ. 9721).

Within the first 100 mins, the optical light curve shows an early-time 
flare, peaking at r'=19.4 mag, followed by a plateau and break - features 
that are the same as suggested by the partially sampled XRT light curve.

Observations are ongoing."


GRB_name: GRB090727A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9723
SUBJECT: GRB 090727: Swift-XRT refined analysis
DATE:    09/07/28 11:30:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. A. Evans (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 11 ks of XRT data for GRB 090727 (Evans et al. GCN
Circ. 9718), from 91 s to 29.2 ks after the BAT trigger. The data
comprise 40 s in Windowed Timing (WT) mode from T+260 s to T+300 s,
with  the remainder in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN. Circ 9721).

The XRT initially observed the GRB for only 210 s before slewing away,
and the data in this interval are dominated by a flare, making it
impossible to determine the underlying decay rate. Fitting only the data
from the second snapshot onwards (beginning at T+3.9 ks) we find a
power-law decay with an index of alpha=0.73 (+/-0.19).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.60 (+0.20, -0.14). The
best-fitting absorption column is consistent with the Galactic value of
2.5 x 10^21 cm^-2  (Kalberla et al. 2005).

If the light curve continues to decay with a power-law decay index of
0.73, the count rate at T+24 hours will be 0.0043 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-13 (2.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00358520.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090727A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9724
SUBJECT: GRB 090727: Swift-BAT refined analysis
DATE:    09/07/28 12:00:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P. A. Evans (U Leicester), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090727 (trigger #358520)
(Evans, et al., GCN Circ. 9718).  The BAT ground-calculated position is
RA, Dec = 315.917, 64.937 deg, which is 
   RA(J2000)  =  21h 03m 40.0s 
   Dec(J2000) = +64d 56' 12.7" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
 
The mask-weighted light curve shows an initial FRED-like peak starting at
~T-5 sec, peaking at ~T_zero, and ending at ~T+20 sec.  The second, weaker,
peak starts at ~T+130 to ~T+150 sec.  The third peak starts at ~T+180 sec,
peaks at ~T+270 sec, and ends at ~T+320 sec.  This third peak corresponds
to the flare mentioned in Circ 9723 (Evans).  T90 (15-350 keV) is 302 +- 23 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-1.3 to T+318.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.24 +- 0.24.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.12 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/358520/BA/


GRB_name: GRB090728A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9725
SUBJECT: GRB 090728: Swift detection of a burst
DATE:    09/07/28 15:00:04 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
P.A. Curran (MSSL-UCL), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU), N. P. M. Kuin (MSSL),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-IASFPA), M. H. Siegel (PSU),
M. Stamatikos (NASA/ORAU) and M. A. Stark (PSU) report on behalf of
the Swift Team:

At 14:45:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090728 (trigger=358574).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 29.660, +41.647 which is 
   RA(J2000) = 01h 58m 38s
   Dec(J2000) = +41d 38' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 20 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 14:47:36.5 UT, 110.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 29.65234, 41.63270 which
is equivalent to:
   RA(J2000)  = 01h 58m 36.56s
   Dec(J2000) = +41d 37' 57.7"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 55 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
7.35e+20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 3.90e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
116 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The 3-sigma upper limit is about 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The list of sources is typically complete to about 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.07. The XRT position is near a bright (< 6.5 mag) star. 

Burst Advocate for this burst is V. Mangano (vanessa AT ifc.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090728A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9726
SUBJECT: GRB 090728A: Faulkes Telescope North Optical Afterglow Candidate
DATE:    09/07/28 15:41:48 GMT
FROM:    Andrea Melandri at Liverpool John Moores U  <axm@astro.livjm.ac.uk>

A. Melandri, C.G. Mundell, Z. Cano, R.J. Smith, I.A. Steele,
S. Kobayashi, C.J. Mottram, D.F. Bersier (Liverpool JMU),A.
Gomboc (Ljubljana), C. Guidorzi (INAF-OAB) report:

"The 2-m Faulkes Telescope North robotically followed up GRB090728
(SWIFT trigger 358574; Mangano et al. GCN 9725) beginning about 9.6
min after the GRB trigger time.

We identify a rapidly fading optical counterpart at:

RA (J2000)=01:58:36.6
Dec(J2000)=+41:37:59.6

This source is not detected in our R-band images, but is detected
in SDSS-I band images with i'=19.55+/-0.3 mag (at a mean time of
13.2 min after the burst) wrt USNO-B1 I-mag.

Spectroscopic followup is encouraged."


GRB_name: GRB090728A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9727
SUBJECT: GRB 090728, RIMOTS optical upper limits
DATE:    09/07/28 17:32:46 GMT
FROM:    Hidenori Hayasi at Miyazaki U  <hayasi@astro.miyazaki-u.ac.jp>

Sub:GRB 090728, RIMOTS optical upper limits  

K.Noda, H.Hayasi, E.Sonoda, N.Ohmori, K.Kono  
A.Daikyuji, Y.Nisioka, M.Yamauchi
(University of Miyazaki)

 We have observed the field covering the error circle of
GRB 090728 (Swift trigger 358574, GCN 9725, V. Mangano et al.) 
with the unfiltered CCD camera on the 30-cm telescope 
at University of Miyazaki.
The observation was started 14:46:53 UT, about 23 sec
after the Swift trigger time. 
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position. 
(Swift trigger 358574, GCN 9725, V. Mangano et al.) 

the upper limits are as follows:
--------------------------------------------------------------
Start(UT)   End(UT)    Num. of frames    Limit (mag.)
--------------------------------------------------------------
14:59:59 15:00:29          1            13.8
14:46:53 15:00:29         11            15.4
---------------------------------------------------------------


GRB_name: GRB090727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9728
SUBJECT: GRB 090727: I-band observations from 1.23m CAHA
DATE:    09/07/28 17:56:59 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC, Spain), N. Huelamo (LAEFF-CAB/INTA-CSIC, Spain),
M. Fernandez (IAA-CSIC, Spain), M. Jelinek (IAA-CSIC, Spain), P. Kubanek
(IAA-CSIC, Spain), A. de Ugarte Postigo (OAB-INAF, Italy), A.J.
Castro-Tirado (IAA-CSIC, Spain), R.J. Smith (JMU, Liverpool, UK), C.G.
Mundell (JMU, Liverpool, UK), on behalf of a larger collaboration, report:

"We carried out I-band observations of the GRB 090727 XRT optical
afterglow (Smith et al. GCN Circ. 9719; GCN Circ. 9722) with the 1.23m
Calar Alto telescope. The observations were carried out on July
27.9646-28.0063 UT (0.45-1.45 hours post GRB) with an exposure time of
3600s. Very preliminary photometry yields I ~ 19.4 (Vega system) for the
afterglow, against USNO B1.0 star with I=18.72 placed at (RA_J2000,
DEC_J2000) = (21:03:49.099, +64:55:58.23)."


GRB_name: GRB090728A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9729
SUBJECT: GRB 090728: Enhanced Swift-XRT position
DATE:    09/07/28 19:59:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2365 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 090728, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 29.65290, +41.63313 which is equivalent
to:

RA (J2000): 01h 58m 36.70s
Dec (J2000): +41d 37' 59.3"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090728A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9730
SUBJECT: GRB 090728: Swift/UVOT Upper Limits
DATE:    09/07/28 22:58:42 GMT
FROM:    Patricia Schady at MSSL/Swift  <msslba@googlemail.com>

GRB 090728: Swift/UVOT Upper Limits

P.A. Curran (MSSL-UCL), V. Mangano (INAF-IASFPA), report on behalf of
the Swift/UVOT team:


The Swift/UVOT began settled observations of the field of GRB 090728
117s after the BAT trigger (Mangano et al., GCN 9725). No optical
afterglow consistent with the refined XRT position (Osborne et al., GCN
9729)  or the optical counterpart (Melandri et al. , GCN 9726) is
detected in the UVOT exposures.  This is consistent with the R-band
non-detection of Melandri et al.


Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the initial finding chart (FC)
and subsequent exposures are:

Filter   T_start(s)    T_stop(s)    Exp(s)    Mag

v       422             6883           479        > 20.70
b       372             6643           491        > 21.45
u       117             366            150        > 20.00 (FC)
u       117             6437           842        > 21.34
uw1     472             6233           452        > 21.05
um2     447             6026           452        > 20.75
uw2     398             6849           490        > 20.89

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090727A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9731
SUBJECT: GRB 090727: Swift/UVOT Upper Limits
DATE:    09/07/29 02:00:58 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M.M. Chester (PSU) and P. A. Evans (U Leicester) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090727
92 s after the BAT trigger (Evans et al., GCN Circ. 9718).  We do not find 
any new source at the position of the XRT afterglow (Goad et al., GCN Circ. 
9721). Preliminary 3-sigma upper limits for the white finding chart and the 
co-added images, using the UVOT photometric system (Poole et al. 2008, 
MNRAS, 383, 627), are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            92          241          147         >20.6
white               92         5987          541         >21.5
v                 4760        57429         3737         >21.1
b                 4145        46543         1752         >21.3
u                 3939        52323         4261         >21.8
w1                5171        51651         4625         >22.1
m2                4965        57845         4989         >22.3
w2                4556        56519         3825         >21.7

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.54 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090726A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9732
SUBJECT: GRB 090726: GRT Optical Observation
DATE:    09/07/29 10:22:47 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU),
C.A. Wallace (FGCU)

We observed the field of GRB 090726 detected by Swift
(trigger #358422; Page et al., GCN Circ. 9706) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

89 set of 30 sec exposures were taken in the R filter starting
from July 27 02:31:44 (UT) about 3.75 hours after the trigger and
stopped on July 27 03:22:10 (UT).  We do not detect the optical
afterglow (Moskvitin et al., GCN Circ. 9709; Fatkhullin et al.,
GCN Circ. 9712; Polasek et al., GCN Circ. 9714; Maticic et al.,
GCN Circ. 9715; Landsman et al., GCN Circ. 9717) both in the
individual images and the combined image.  The estimated three
sigma upper limit of the combined image (total exposure of 2670.0 sec)
is ~18.9 mag using the USNO-B1 catalog.


GRB_name: GRB090727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9733
SUBJECT: GRB 090727: optical observations
DATE:    09/07/29 12:31:34 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. Moskvitin, A. Valeev, T. Fatkhullin,
O. Sholukhova & S. Fabrika (SAO-RAS Niznijh Arkhyz, Russia),
on behalf of a larger colaboration, report:

We observed the GRB090727 optical afterglow (Smith et al. GCN Circ. 9719,
GCN Circ. 9722; J. Gorosabel et al. GCN Circ 9728 ) with the SAO RAS 6-m
telescope in Caucasus. The observations were carried out in the R band 
with a total exposure of 158 sec. The weather was cloudy with a sufficient
atmospheric extinction. We estimated the brightness of the object as
R = 21.53 +/- 0.17 at the middle epoch of 23:21:12 27 July 2009 UT
(2334 sec after the trigger). Calibration was done aganist 10 USNO B1.0 
stars.

This message may be cited.


GRB_name: GRB090728A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9734
SUBJECT: GRB 090728: Swift XRT refined analysis 
DATE:    09/07/29 15:26:40 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano, B. Sbarufatti (INAF IASF Pa)
report on beahalf the Swift XRT Team:


We have analysed 9.8 ks of XRT data for GRB 090728 (Mangano et al. GCN
Circ. 9725), from 116.9 s to 53.1 ks after the BAT trigger. The data
comprise 55.3 s in Windowed Timing (WT) mode from T+116.9 s to T+172.2
s, with  the remainder in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN. Circ 9729).

The 0.3-10 keV XRT light curve is well modeled by a doubly broken
power law with initial decay slope -5.5  0.5, first break at
T+204  10 s, plateau phase slope -0.11  0.14, second break
at T+1.8  1.2 ks and final slope -1.7  0.1.
Decaying at the present rate the source will reach a level of
2e-4 counts/s on July 30 at 14:45 UT (48 h after the trigger).

We extracted the average WT spectrum of the early decay phase (55.3 s
exposure), and the average PC spectra of the plateau phase (866 s
exposure, from T+174 s to T+1071 s) and the final decay phase (7.4 ks
exposure, from T+4383 s to T+18.4 ks). The three spectra are well fitted
by an absorbed power law model with NH consistent with the Galactic
value of 7.35e20 cm-2 (Kalberla et al. 2005) and photon indices of
2.4  0.4, 1.8  0.2, and 2.0  0.3, respectively.
The average 0.3-10 keV observed [unabsorbed] fluxes are
1.6e-10 [2.9e-10] erg cm-2 s-1, 2.7e-11 [3.0e-11] erg cm-2 s-1,
and 1.5e-12 [2.3e-12] erg cm-2 s-1, respectively.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00358574.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9735
SUBJECT: GRB 090727: GRT Optical Observation
DATE:    09/07/29 19:19:45 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (JHU/GSFC), T.N. Ukwatta (GWU/GSFC), Y. Urata (NCU),
C.A. Wallace (FGCU)

We observed the field of GRB 090727 detected by Swift
(trigger #358520; Evans et al., GCN Circ. 9718) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

77 set of 30 sec exposures (excluding the bad quality images) were 
taken in the R filter starting from July 28 01:57:45 (UT) about 
3.2 hours after the trigger and stopped on July 28 02:40:50 (UT).  
We do not detect the optical afterglow (Smith et al., GCN Circ. 
9719; Gorosabel et al., GCN Circ. 9728; Moskvitin et al., GCN Circ. 
9733) both in the individual images and the combined image.  The 
estimated three sigma upper limit of the combined image (total 
exposure of 2310 sec) is ~16.6 mag using the USNO-B1 catalog.


GRB_name: GRB090728A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9736
SUBJECT: GRB 090728: Swift-BAT refined analysis
DATE:    09/07/29 20:08:49 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), C. B. Markwardt (GSFC/UMD),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090728 (trigger #358574)
(Mangano, et al., GCN Circ. 9725).  The BAT ground-calculated position is
RA, Dec = 29.644, 41.632 deg which is 
   RA(J2000)  =  01h 58m 34.5s 
   Dec(J2000) = +41d 37' 53.7" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.
 
The mask-weighted light curve shows a single pulse starting at ~T-10 sec,
peaking at ~T+2 sec, and ending at ~T+70 sec.  T90 (15-350 keV) is
59 +- 18 sec (estimated error including systematics).
 
The time-averaged spectrum from T-5.0 to T+63.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.05 +- 0.26.  The fluence in the 15-150 keV band is 1.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.25 sec in the 15-150 keV band
is 1.0 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/358574/BA/


GRB_name: GRB090709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9737
SUBJECT: GRB 090709A : Quick look analysis of the Suzaku observation
DATE:    09/07/30 16:07:34 GMT
FROM:    Yujin E. Nakagawa at RIKEN  <yujin@crab.riken.jp>

Y. E. Nakagawa, T. Tamagawa (RIKEN), K. Yamaoka, S. Sugita, A. Yoshida
(Aoyama Gakuin University), R. Sato, M. Ohno (ISAS/JAXA), K. Nakazawa
(University of Tokyo), M. Tashiro, T. Sugasahara, W. Iwakiri, K. Onda
(Saitama University), Y. Urata (National Central University), D. Yonetoku,
T. Murakami (Kanazawa University), N. Kawai, R. Usui, H. Nakajima, A. Endo
(Tokyo Institute of Technology), M. Yamauchi, E. Sonoda, N. Ohmori,
K. Kohno, H. Hayashi, A. Daikyuji, K. Noda, Y. Nishioka (University of Miyazaki),
M. Suzuki (TKSC/JAXA), F. Tazaki, S. Eguchi, K. Kubota, Y. Ishino, K. Hiroi,
Y. Ueda (Kyoto University), on behalf of the Suzaku GRB ToO team, report:

We report on a Suzaku ToO observation of the GRB 090709A X-ray afterglow
(Morris et al. 2009, GCN 9625), started on 2009-07-09 13:16:17 UT,
for a net exposure time of about 62 ksec (Mitsuda et al. 2009, GCN 9632).
The observation covers time ranging from 23 ksec to 135 ksec after the
Swift/BAT trigger time (2009-07-09 07:38:34 UT). The X-ray afterglow was
clearly detected in the XIS CCDs at a position consistent with that of
the Swift/XRT observations (Morris et al. 2009, 9625). The 0.2-12 keV
light curve is well fit by a power law with a decay index of 1.53+/-0.02.

A preliminary analysis of the XIS data shows that a time average spectrum
in 0.2-12 keV band is well fit by a power law with a photon index of
2.02+/-0.03, absorbed by a hydrogen column density of (2.2+/-0.2)*10^21 cm^-2.
The unabsorbed 0.2-12 keV flux is (5.2+/-0.2)*10^-12 ergs cm^-2 s^-1.
The XIS data confirm the hydrogen column density in excess of the
Galactic value of 6.6*10^20 cm^-2, consistent with the Swift/XRT result
(Rowlinson et al. 2009, GCN 9642).

We would like to thank the Suzaku managers and the operation team
for approving and carrying out the ToO observation.


GRB_name: GRB090717A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9738
SUBJECT: GRB 090717A: Suzaku WAM observation of the prompt emission
DATE:    09/07/31 12:42:00 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

N. Vasquez (Tokyo Tech.), K. Yamaoka, S. Sugita (Aoyama Gakuin U.),
K. Noda, E. Sonoda, M. Yamauchi, N. Ohmori, H. Hayashi,
K. Kono, A. Daikyuji, Y. Nishioka (Univ. of Miyazaki),
Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda,
T. Sugasahara (Saitama U.), Y. Urata (NCU),
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo),
Y. E. Nakagawa, T. Tamagawa (RIKEN), S. Hong (Nihon U.),
on behalf of the Suzaku WAM team, report:

The long GRB 090717A (Fermi-GBM trigger #269484574; Kara et al., GCN 9692),
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 00:49:32.019 UT.

The light curve shows a double pulse structure with a duration
 (T90) of 56 seconds. The fluence in 100 - 1000 keV was
 1.10(-0.15, +0.12) x10^-5 erg/cm^2. The 1-s peak flux measured
from T0+6 s was 3.14(-0.53, +0.36) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum
from T0 to T0+60 s is well fitted by a single power-law model with a
photon index of 2.13(-0.22, +0.33)  (chi^2/d.o.f. = 15.1/17).
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst are now available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB090726A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9741
SUBJECT: GRB 090726: optical observation
DATE:    09/07/31 20:36:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU),  E. Pavlenko, A. Sklyanov, O. Antoniuk (CrAO), A. 
Pozanenko (IKI)  report on behalf of larger GRB follow-up collaboration:

We observed the field of  the Swift GRB 090726 (Page et al., GCN 9706)    in 
R-filter on Jul. 27 between  (UT) 18:19:22 - 20:28:58  with Shajn telescope 
of  CrAO. We  detect afterglow (Moskvitin et al., GCN  9709)  in a stacked 
image. The photometry against nearby USNO-B1.0 stars is following:

T0+     Filter, Exposure, mag.,     err.
(d)                (s)

0.8626  R     114x60     23.60 +/- 0.25

While the index of power law approximation  of  the light curve during early 
observation  (Moskvitin et al., GCN  9709) is ~ -1.0, the power law index 
between observation  presented by Moskvitin et al. (GCN  9709) and our 
observation is -1.6, clearly suggesting a break between 0.079 and 0.863 
days. 


GRB_name: GRB090802A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9742
SUBJECT: GRB 090802: Fermi GBM detection
DATE:    09/08/02 21:19:06 GMT
FROM:    Elisabetta Bissaldi at MPE  <ebs@mpe.mpg.de>

Elisabetta Bissaldi (MPE) reports on behalf of the Fermi GBM Team:


"At 05:39:03.08 UT on 02 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090802 (trigger 270884345 / 090802235).
The on-ground calculated location, using the GBM trigger
data, is RA = 51.0, DEC = +37.9 (J2000 degrees,
equivalent to 03h 24m, 37d 54'), with an uncertainty
of 4.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 123 degrees.

The GBM light curve consists of a single FRED-like pulse
with a duration (T90) of about 128 ms (8-1000 keV).
The time-averaged spectrum from T0-0.016 s to T0+0.056 s is
best fit by a Band function with Epeak = 283 (-53 +58) keV,
alpha = -0.42 (-0.17 +0.21), and beta = -2.4 (-0.7 +0.3)
(Castor C-stat 325 for 361 d.o.f.).

The event fluence (8-1000 keV) in this time interval is
(6.5 +/- 0.3)E-07 erg/cm^2. The 32-ms peak photon flux measured
starting from T0-0.008 s in the 8-1000 keV band
is 61.2 +/- 2.8 ph/s/cm^2.


The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090727B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9743
SUBJECT: IPN Triangulation and Konus-Wind observaions of GRB090727B
DATE:    09/08/03 11:35:38 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R. Aptekar, D. Frederiks, E. Mazets, and V. Pal'shin,
on behalf of the Konus-Wind team,

K. Hurley and T. Cline, on behalf of the Mars Odyssey
and Konus GRB teams,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team, and

J. Goldsten, on behalf of the MESSENGER NS GRB team,
report:


The long GRB 090727B triggered Konus-Wind at T0=84749.412 s UT
(23:32:29.412). The burst had a smooth temporal structure with
a duration of ~25 s. The Konus-Wind light curves are available at
http://www.ioffe.ru/LEA/GRBs/GRB090727_T84749/

This GRB was observed by Odyssey (HEND and GRS) and MESSENGER (GRNS).
Wind-Odyssey-MESSENGER triangulation, together with Konus-Wind
ecliptic latitude constrains, lead to the following preliminary,
3 sigma error box, which area is 1.00 sq. deg.

-----------------------------------------------
        RA(2000), deg            Dec(2000), deg
-----------------------------------------------
Center:
   343.358 (22h 53m 26s)   -46.700 (-46d 42' 00")
Corners:
   343.427 (22h 53m 42s)   -45.867 (-45d 52' 01")
   342.516 (22h 50m 03s)   -45.873 (-45d 52' 22")
   343.285 (22h 53m 08s)   -47.527 (-47d 31' 37")
   344.214 (22h 56m 51s)   -47.507 (-47d 30' 25")
-----------------------------------------------
IPN triangulation map can be found at
http://www.ioffe.ru/LEA/GRBs/GRB090727_T84749/GRB20090727_84749_IPN.png

As observed by Konus-Wind, the burst had a fluence
of (1.15  0.15)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+14.336 s,
of (8.5  3.2)x10-7 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+24.832 s) is well fit, in the 20 keV - 2 MeV range,
by GRB (Band) model, for which:
the low-energy photon index alpha = -0.18(-0.27,+0.34),
the high energy photon index beta = -2.97( < -2.50),
the peak energy Ep = 152(-16, +17) keV (chi2 = 54/57 dof).

All the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.

--


GRB_name: GRB090802B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9744
SUBJECT: GRB 090802B: Fermi GBM detection
DATE:    09/08/03 22:04:39 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"At 15:58:23.44 UT on 2 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090208B (trigger 270921505 / 090802666).
The on-ground calculated location, using the GBM trigger data, is
RA = 267.0, DEC = -71.8 (J2000 degrees, equivalent to 17h48m, -71d46'),
with an uncertainty of 10.7 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which
is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 104 degrees.
Since the source is weak, the time-averaged spectrum is poorly constrained."


GRB_name: GRB090807A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9746
SUBJECT: GRB 090807: Swift detection of a burst
DATE:    09/08/07 15:18:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
P.A. Curran (MSSL-UCL), A. de Ugarte Postigo (INAF-OAB),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (MSSL),
J. Mao (INAF-OAB), R. Margutti (Univ Bicocca&OAB),
K. L. Page (U Leicester), T. Sakamoto (NASA/UMBC),
M. H. Siegel (PSU), M. Stamatikos (NASA/ORAU),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:

At 15:00:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090807 (trigger=359378).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 273.744, +10.281 which is 
   RA(J2000)  =  18h 14m 59s
   Dec(J2000) = +10d 16' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT TDRSS light curve does not show anything
as is typical for image triggers. 

The XRT began observing the field at 15:03:00.5 UT, 153.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright, fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 273.7438,
10.2665 which is equivalent to:
   RA(J2000)  = 18h 14m 58.51s
   Dec(J2000) = +10d 15' 59.3"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (8.6e+20
cm^-2, Kalberla et al. 2005), with an excess column of 2 (+1.68/-1.50)
x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 8.55e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of nominal 150 seconds with the 
White filter  starting 163 seconds after the BAT trigger. No credible
 afterglow candidate has  been found in the initial data products. 
The  2.7'x2.7' sub-image covers 100% of the XRT error circle. The
3-sigma  upper limit is about 19.2 mag. The 8'x8' region for the list
of  sources generated on-board covers 100% of the XRT error circle. 
The  list of sources is typically complete to about 18.0 mag. No
correction  has been made for the expected extinction corresponding
to E(B-V) of  0.18. 

Burst Advocate for this burst is J. K. Cannizzo (cannizzo AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090807A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9747
SUBJECT: GRB 090807, RIMOTS optical upper limits
DATE:    09/08/07 16:43:17 GMT
FROM:    Kenta Kono at Miyazaki U  <kenta0514@astro.miyazaki-u.ac.jp>

K.Kono, K.Noda, E.Sonoda, N.Ohmori, H.hayasi,
A.Daikyuji, Y.Nisioka, M.Yamauchi
(University of Miyazaki)

We have observed the field covering the error circle of
GRB 090807 (Swift trigger 359378, GCN 9746, J. K. Cannizzo et al.)
with the unfiltered CCD camera on the 30-cm telescope
at University of Miyazaki.
The observation was started 15:04:25 UT, about 2.2 min
after the Swift trigger time.
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position.
(GCN 9746, J. K. Cannizzo et al.)

the upper limits are as follows:
--------------------------------------------------------------
Start(UT)  End(UT) $B!!!!(BNum. of frames $B!!(BLimit (mag.)
--------------------------------------------------------------
15:04:25  15:04:55  1  12.6
15:04:25  15:30:26  19  18.5
---------------------------------------------------------------


GRB_name: GRB090807A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9748
SUBJECT: GRB 090807: Enhanced Swift-XRT position
DATE:    09/08/07 19:10:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1531 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 090807, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 273.74377, +10.26583 which is equivalent
to:

RA (J2000): 18h 14m 58.50s
Dec (J2000): +10d 15' 57.0"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090807A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9749
SUBJECT: GRB 090807, Swift-BAT refined analysis
DATE:    09/08/07 20:06:11 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

T. N. Ukwatta (GWU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. K. Cannizzo (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+423 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 090807 (trigger #359378)
(Cannizzo, et al., GCN Circ. 9746).  The BAT ground-calculated position is
RA, Dec = 273.741, 10.279 deg which is
   RA(J2000)  =  18h 14m 57.8s
   Dec(J2000) = +10d 16' 45.9"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.

The mask-weighted light curve shows a complex structure lasting from
T-5 to T+150 seconds with at least five peaks superimposed on a broad,
soft and slowly varying background.  There is an additional peak at
T+185 sec which corresponds to a large flare seen in the Swift/XRT.
There is also possible precursor activity from T-200 to T-80 sec.
T90 (15-350 keV) is 140.8 +- 13.1 sec (estimated error including
systematics).

The time-averaged spectrum from T-9.5 to T+151.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.25 +- 0.14.  The fluence in the 15-150 keV band is 2.2 +- 0.2 x 10-6 erg/cm2.
The 1-sec peak photon flux measured from T+41.96 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/359378/BA/


GRB_name: GRB090807A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9750
SUBJECT: GRB 090807: Swift-XRT refined analysis
DATE:    09/08/07 22:37:04 GMT
FROM:    Raffaella Margutti at U. di Milano Bicocca  <raffaella.margutti@brera.inaf.it>

R. Margutti (Univ. Bicocca & INAF-OAB), J. Mao (INAF-OAB),
A. de Ugarte Postigo (INAF-OAB)  and J. K. Cannizzo (NASA/UMBC)
report on behalf of the Swift-XRT team:

We have analysed the first orbit of Swift-XRT data obtained for
GRB 090807 (Cannizzo et al. GCN Circ. 9746), covering 149 s of
Windowed Timing (WT) and 1.5 ks of Photon Counting (PC) mode data,
respectively, between 154 s and 1.9 ks after the trigger.
The UVOT-enhanced XRT position was given by Beardmore et al. in
GCN Circ. 9748.

The light curve shows a large flare peaking around 185 s which was
also detected in the 15-150 keV energy range by Swift/BAT (Ukwatta et
al. GCN Circ. 9749). The underlying light curve decays
with a power-law index of 5.0 +/- 0.5. Around T+580 s the decay flattens,
to a slope of 0.87 +/- 0.42.

The spectrum extracted from WT data can be modelled with an absorbed simple
power-law, with Gamma = 2.2 +/- 0.1 and NH = (3.0+/-0.2)x10^21 cm^-2 in
excess of the Galactic column in this direction which is 8.6x10^20 cm^-2
(Kalberla et al. 2005).
A spectrum extracted from PC data in the time interval T+310 s - T+1840 s
has a best-fitting photon index of 2.6 +/- 0.4 and a best-fitting 
absorption
column of NH = (3.3+/-0.1)x10^21 cm^-2 in excess of the Galactic value.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.1 x 10^-11 (8.4 x 10^-11) erg cm^-2 
count^-1.

If the light curve continues to decay with a power-law decay index
of 0.9, the count rate at T+24 hours will be 0.002 count s^-1, 
corresponding
to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x 10^-14 (1.7 x 10^-13)
erg cm^-2 s^-1. However, the light-curve is possible to break before 
this time,
making this prediction unreliable.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00359378.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090807A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9751
SUBJECT: GRB 090807: Swift/UVOT Upper Limits
DATE:    09/08/07 23:57:25 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and Cannizzo (NASA/UMBC)report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090807
164 s after the BAT trigger (Cannizzo et al., GCN Circ. 9746).
No optical afterglow consistent with the XRT position (Beardmore et al.,
GCN Circ. 9748) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           164          313          147         >21.2
u_FC               322          571          246         >20.1
white              164         1026          295         >21.1
u                  322          571          246         >20.1

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.18 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090807A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9752
SUBJECT: GRB 090807: MITSuME optical upper limit
DATE:    09/08/08 07:58:00 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, D. Kuroda, K. Yanagisawa, Y. Shimizu, S. Nagayama,
H. Toda (OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf
of the MITSuME collaboration:

We observed the field of GRB 090807 (Cannizzo et al. GCN 9746)
with optical three color (g', Rc and Ic) CCD camera attached to
the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2009-08-07 15:03:35 UT (3m 8s after
the burst). We did not find any point source in the error circle
of the XRT position reported by Beardmore et al. (GCN 9748) in
all the three bands.

Three sigma upper limits of the OT are listed below. We used USNO
B1 catalog for flux calibration.

PDAY        MID-UT   T-EXP     g'     Rc     Ic
---------------------------------------------------
0.00589   15:08:56   540.0   >18.3  >18.5  >18.2
0.04169   16:00:30  4860.0   >18.9  >19.1  >18.7
---------------------------------------------------


GRB_name: GRB090807A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9753
SUBJECT: GRB 090807: Liverpool Telescope observations
DATE:    09/08/08 11:31:45 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana), R.J. Smith, C.G. 
Mundell,
I.A. Steele, A. Melandri, S. Kobayashi, C.J. Mottram, D.F. Bersier, Z. 
Cano (Liverpool JMU),
N.R. Tanvir, P. O'Brien (U. Leicester) report on behalf of a large 
collaboration:

On 2009 August 07 at 23:45:24 UT we observed the Swift GRB 090807
(Cannizzo et al., GCN Circ. 9746) with the 2-m Liverpool Telescope.

Observations started 8.75 hours after the BAT trigger time and were
performed using the r' and i' filters. We could not find any
uncatalogued object inside the UVOT-enhanced XRT error circle (Beardmore 
et al.
GCN Circ. 9748) down to the following limiting magnitudes:

Time Interval     Total Exp  Filter     Limit
(hours from GRB)   (s)                  (mag)
----------------------------------------------
8.75-9.27          6x300      R > 22.1
9.29-9.90          6x300      I > 22.0
----------------------------------------------

Magnitudes have been calibrated against the nearby USNOB-1 star
RA=18:15:00.349, Dec=+10:15:45.21, using R2=16.19, I=15.82.

We note the presence of an uncatalogued source lying outside the XRT error
circle at 4.2" from the XRT centroid, at RA=18:14:58.24, Dec=+10:15:58.4 
with
estimated magnitudes R=22.4 +/- 0.2, I=21.6 +/- 0.2:

http://www.fe.infn.it/u/guidorzi/090807_LT_ri.png

At the moment we cannot assess whether this source is fading.


GRB_name: GRB090809A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9754
SUBJECT: GRB 090809: Swift detection of a burst with a possible optical counterpart
DATE:    09/08/09 17:51:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (CRESST/GSFC/UMD), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), A. de Ugarte Postigo (INAF-OAB),
N. Gehrels (NASA/GSFC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (MSSL), W.B Landsman (GSFC), J. Mao (INAF-OAB),
R. Margutti (Univ Bicocca&OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), P. Romano (INAF-IASFPA) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 17:31:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090809 (trigger=359530).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 328.645, -0.083 which is 
   RA(J2000)  =  21h 54m 35s
   Dec(J2000) = -00d 04' 59"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a weak peak
with a duration of about 10 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 17:32:58.5 UT, 104.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 328.67772, -0.08465 which is equivalent
to:
   RA(J2000)  = 21h 54m 42.65s
   Dec(J2000) = -00d 05' 04.7"
with an uncertainty of 4.5 arcseconds (radius, 90% containment). This
location is 117 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.08e+20
cm^-2, Kalberla et al. 2005), with an excess column of 2.5
(+2.71/-2.28) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of  86 seconds with the White 
filter  starting 107 seconds after the BAT trigger. A possible 
afterglow candidate has  been found in the list of sources generated 
on-board, located at RA=328.68008  (21:54:43.22), dec=-0.08385 
(-00:05:01.9), with an estimated White magnitude = 19.9 +/-0.4.  The 
2.7'x2.7' sub-image does not include the XRT position. No  correction 
has been made for the expected extinction corresponding to E(B-V) of  
0.10. 

Burst Advocate for this burst is C. B. Markwardt (Craig.Markwardt AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090809A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9755
SUBJECT: GRB 090809: afterglow confirmation at the NOT
DATE:    09/08/10 00:27:57 GMT
FROM:    Dong Xu at DARK,NBI  <dong@astro.ku.dk>

D. Xu, G. Leloudas, D. Malesani, J.P.U. Fynbo (DARK/NBI), P. Jakobsson 
(Univ. of Iceland), and G. Furesz (CfA/Harvard) report on a larger 
collaboration:

We observed the field of GRB 090809 (Markwardt et al., GCN 9754) with 
the Nordic Optical Telescope equipped with ALFOSC. We obtained 3x300 s 
I-band frames, starting on August 9th, 21:49:10 UT, 4.29889 hr after the 
burst; and 1x300 s R-band frame,  starting 5.29861 hr after the burst.

We confirm the presence of the UVOT source (Markwardt et al., GCN 9754) 
at coordinates:

RA(J2000) = 21:54:43.17
Dec(J2000) = -00:05:01.9

which are consistent with the UVOT position. We note that the source is 
not visible in the archival SDSS frames of this field, thereby proving 
that it is the optical afterglow of GRB 090809.

The afterglow is detected in each I-band and R-band frame. The 
preliminary magnitudes are I~19.9 and R~20.3 respectively, against the 
same reference star, 0899-0602834 in the USNO B1 catalog.

Further photometric observations are underway. We encourage 
spectroscopic follow-up.


GRB_name: GRB090809A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9756
SUBJECT: GRB 090809: Swift-BAT refined analysis
DATE:    09/08/10 02:07:52 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090809 (trigger #359530)
(Markwardt, et al., GCN Circ. 9754).  The BAT ground-calculated position is
RA, Dec = 328.665, -0.083 deg which is 
   RA(J2000)  =  21h 54m 39.5s 
   Dec(J2000) = -00d 04' 58.0" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.
 
The mask-weighted light curve shows a single, roughly triangularly shaped
peak starting at ~T-1 sec, peaking at ~T+3 sec, and ending at ~T+9 sec.
T90 (15-350 keV) is 5.4 +- 1.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.0 to T+6.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.24.  The fluence in the 15-150 keV band is 3.4 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+2.26 sec in the 15-150 keV band
is 1.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/359530/BA/


GRB_name: GRB090809A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9757
SUBJECT: GRB 090809: Enhanced Swift-XRT position
DATE:    09/08/10 02:38:47 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 5518 s of XRT Photon Counting mode data and 13 UVOT
images for GRB 090809, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 328.68012, -0.08366 which is equivalent
to:

RA (J2000): 21h 54m 43.23s
Dec (J2000): -00d 05' 01.2"

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090809A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9758
SUBJECT: GRB090809: Swift/UVOT observations
DATE:    09/08/10 05:37:54 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.B. Landsman (NASA/GSFC) and C. Markwardt (CRESST/GSFC/UMD) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090809 
108s after the BAT trigger (Markwardt et al., GCN Circ. 9754),      The 
tentative UVOT detection reported by Markwardt et al. is confirmed 
following the downlink of additional data.   The UVOT position 
determined from the white finding chart exposure is

RA (J2000)  21:54:43.19   =  328.679938 (deg)
Dec (J2000) -00:05:1.83   =  -0.083842 (deg)

with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence,  
statistical + systematic), consistent with the NOT afterglow position 
(Xu et al., GCN Circ. 9755).

The initial magnitudes and upper limits are as follows:

Filter   T_start(s) Tstop(s) Exp(s)      Mag
white        108    194      84     19.53 +/- 0.14
white       3396   3545     147     21.03 +/- 0.33

v           3552   5181     393     19.87 +/- 0.30
b           4365   5976     367    >21.1  (3 sigma)
u           4162   5796     391    >20.8  (3 sigma)
uvw1        3962   5592     393    >20.7  (3 sigma)
uvm2        3757   5386     393    >20.5  (3 sigma)
uvw2        4776  10964    1082    >21.6  (3 sigma)

The values quoted above are not corrected for the Galactic extinction 
due to the reddening of E(B-V) = 0.10 in the direction of the burst 
(Schlegel  et al. 1998). The photometry is on the UVOT photometric 
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB090809A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9759
SUBJECT: GRB 090809: Swift-XRT refined analysis
DATE:    09/08/10 08:01:42 GMT
FROM:    Jirong Mao at INAF-OAB  <jirong.mao@brera.inaf.it>

J. Mao, R. Margutti, A. de Ugarte Postigo (INAF-OAB) and C. B. Markwardt 
(CRESST/GSFC/UMD) report on behalf of the Swift-XRT team:

We have analysed 8.6 ks of XRT data for GRB 090809 (Markwardt et al. GCN 
Circ. 9754), from 107 s to 23.3 ks after the BAT trigger. The data 
comprise 59 s in Windowed Timing (WT) mode with the remainder in Photon 
Counting (PC) mode. The enhanced XRT position for this burst was given 
by Evans et al. (GCN. Circ 9757).

The light curve shows a first flare evidence peaking around 189s, then, 
it shows a second flare peaking around 4.6ks, these flares make an order 
of magnitude increase in count-rate, after that, the light curve decays 
continuously.  In general, the underlying light curve can be modelled 
with a power-law decay with a decay index of alpha=1.02+/-0.02.

A spectrum extracted from the WT mode data can be fitted with an 
absorbed power-law with a photon spectral index of 1.75 (+/-0.09). The 
best-fitting absorption column is 2.4 (+/-0.3) x 1021 cm^-2, in excess 
of the Galactic value of 6.1 x 1020 cm^-2 (Kalberla et al. 2005). The PC 
mode spectrum has a photon index of 1.84 (+0.14, -0.13) and a 
best-fitting absorption column of 1.18 (+0.19, -0.18) x 1021 cm^-2. The 
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor 
deduced from this spectrum is 1.08 x 10^-11 (1.24
x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of 
1.0, the count rate at T+24 hours will be 0.007 count s^-1, 
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.9 x 
10^-13 (3.4 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at 
http://www.swift.ac.uk/xrt_products/00359530.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090809B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9760
SUBJECT: GRB 090809B: Fermi GBM detection
DATE:    09/08/10 15:22:19 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"At 23:28:14.61 UT on 9 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090809B (trigger 271553296 / 090809978).
The on-ground calculated location, using the GBM trigger data, is
RA = 95.3, DEC = 0.1 (J2000 degrees, equivalent to 6h21m, +0d08'),
with an uncertainty of 1.2 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which is
currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 81 degrees.

The GBM light curve consists of a single pulse with a duration (T90)
of about 15 s (8-1000 keV).
The time-averaged spectrum from T0 to T0+14.3 s is best fit by a Band
function with Epeak = 198 +/- 13 keV, alpha = -0.85 +/- 0.04, and
beta = -2.02 +/- 0.06 (chi squared 552 for 484 d.o.f.).
The event fluence (8-1000 keV) in this time interval is
(2.26 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.1 s in the 8-1000 keV band is 23.6 +/- 0.5 ph/s/cm^2.

The temporal and spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090809A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9761
SUBJECT: GRB 090809 X-shooter redshift
DATE:    09/08/10 15:54:48 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

D. Malesani, J.P.U. Fynbo (DARK/NBI), L. Christensen (ESO),
A. de Ugarte Postigo (OAB-INAF), B. Milvang-Jensen (DARK/NBI),
S. Covino (OAB-INAF) report on behalf of a larger collaboration

We have observed the afterglow of GRB 090809 (Markwardt
et al. GCNC 9754) using the X-shooter spectrograph mounted
at the Kueyen telescope of ESO's VLT (Paranal Observatory,
Chile) during its science verification phase. The spectrum,
consisting of a combined exposure of 4x1800s, was started
at 03:40 UT on August 09 (10.15 hrs after the burst). It was
obtained with an initial seeing of 0.9" and an airmass of
1.2, when the afterglow had a magnitude of R~21. The
spectrum covers the complete range from 3000 to 25000
Angstroms. In a preliminary analysis we identify the
Lyman break, Lyman-alpha, SiII, OI, SiI*, SiIV, CIV, FeII, AlII,
AlIII and MgII at a common redshift of 2.737 +/- 0.002 (pending
final wavelength calibration), which we identify as the redshift
of the GRB.

We thank the Paranal staff for excellent support, in particular
Elena Mason and Claudia Cid.


GRB_name: GRB090809A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9762
SUBJECT: GRB 090809: WHT observations
DATE:    09/08/10 17:50:15 GMT
FROM:    Klaas Wiersema at U of Leicester  <kw113@star.le.ac.uk>

K. Wiersema (Leicester), D. Malesani (DARK/NBI), A. Levan, D. Steeghs, L. van 
Spaandonk (Warwick) report on behalf of a larger collaboration:

We observed the field of GRB 090809 (Markwardt et al. GCN 9754) with the 
William Herschel Telescope using the ACAM instrument. Observations 
consisted of 4 x 300 second exposures with a sloan i filter, starting on 
August 9, 23:41 UT (6.16 hrs after burst). We clearly detect the afterglow 
(Markwardt et al. GCN 9754, Xu et al. GCN 9755) with i = 20.48 +/- 0.03 
(calibrated using SDSS stars).


GRB_name: GRB090621A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9763
SUBJECT: GRB 090621A: MAGIC telescope GeV observation
DATE:    09/08/11 07:00:09 GMT
FROM:    Markus Garczarczyk at MPI/MAGIC  <garcz@mppmu.mpg.de>

Carosi A. (INAF Rome), Gaug M. (IAC Tenerife),
Antonelli L.A. (INAF Rome), Bastieri D. (Univ. Padova),
Becerra Gonzalez J. (IAC Tenerife), Covino S. (INAF Rome),
Galante N. (MPI Munich), Garczarczyk M. (IFAE Barcelona),
La Barbera A. (INAF Palermo), Longo F. (INFN Trieste),
Scapin V. (Univ. Udine) and Spiro S. (INAF Rome)
for the MAGIC collaboration

The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up
observation of the BAT burst GRB090621A (Curran et al., GCN Circ. 9540).
The burst was also triggered by Fermi-GBM (Arne Rau, GCN Circ. 9556)
We received the GCN alert at 04:23:38 UT (T0+55s). Data taking with MAGIC 
started at 04:36:18 UT (T0+815s), when the GRB zenith angle reached
46 degrees. The observation continued for 1833 s.

No evidence for VHE gamma-ray emission above the analysis threshold
of 196 GeV was found. The observation was carried out in twilight 
condition.

A preliminary analysis, for the hypothesis of steady emission and 
assumption of a differential photon spectral index of -2.5, yields the 
following 95% CL differential flux upper limits, including a 30% 
systematic uncertainty on the telescope efficiency:

E(175 - 300  GeV): 0.25 * 10^-10 erg cm^-2 s^-1
E(300 - 1000 GeV): 0.10 * 10^-10 erg cm^-2 s^-1
for the whole time of observation (from 04:36:18 UT to 05:06:51 UT).

We can also exclude emission of a constant flux in any 100s time bin 
smaller than:

E(175 - 300  GeV):  2.74 * 10^-10 erg cm^-2 s^-1
E(300 - 1000 GeV):  1.01 * 10^-10 erg cm^-2 s^-1
for a time window from 04:36:18 UT to 05:06:51 UT

This message can be cited.


GRB_name: GRB090621B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9764
SUBJECT: GRB 090621B: MAGIC telescope GeV observation
DATE:    09/08/11 07:10:46 GMT
FROM:    Markus Garczarczyk at MPI/MAGIC  <garcz@mppmu.mpg.de>

Carosi A. (INAF Rome), Gaug M. (IAC Tenerife),
Antonelli L.A. (INAF Rome), Bastieri D. (Univ. Padova),
Becerra Gonzalez J. (IAC Tenerife), Covino S. (INAF Rome),
Galante N. (MPI Munich), Garczarczyk M. (IFAE Barcelona),
La Barbera A. (INAF Palermo), Longo F. (INFN Trieste),
Scapin V. (Univ. Udine) and Spiro S. (INAF Rome)
for the MAGIC collaboration

The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up
observation of the BAT short burst GRB090621B (Curran et al., GCN Circ. 
9545). The burst was also triggered by Fermi-GBM (Goldstein et al., GCN 
Circ. 9562). We received the GCN alert at 22:07:38 UT (T0+13s). Data
taking with MAGIC started at 22:43:33 UT (T0+2169s), when the GRB zenith
angle went below 60 degrees. The observation continued for 12570 s.

No evidence for VHE gamma-ray emission above the analysis threshold was 
found.

A preliminary analysis, for the hypothesis of steady emission and
assumption of a differential photon spectral index of -2.5, yields the
following 95% CL differential flux upper limits, including a 30%
systematic uncertainty on the telescope efficiency.

Because of improving sensitivities and analysis threshold due to 
decreasing zenith angle during the observation, the data sample
was split into 4 parts:

E ( 300-1000 GeV): 0.42 * 10^-10 erg cm^-2 s^-1
for a time window from 22:43:33 UT to 23:38:37 UT
Analysis threshold: 407 GeV

E ( 175- 300 GeV): 5.61 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 0.19 * 10^-10 erg cm^-2 s^-1
for a time window from 23:38:37 UT to 00:32:31 UT
Analysis threshold: 291 GeV

E ( 175- 300 GeV): 4.97 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV): 0.24 * 10^-10 erg cm^-2 s^-1
for a time window from 00:32:31 UT to 01:23:06 UT
Analysis threshold: 224 GeV

E ( 125- 175 GeV): 15.27 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV):  1.25 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV):  0.22 * 10^-10 erg cm^-2 s^-1
for a time window from 01:23:06 UT to 02:13:04 UT
Analysis threshold: 186 GeV

We can also exclude emission of a constant flux in any 100s time bin
smaller than:

E ( 300-1000 GeV): 4.02 * 10^-10 erg cm^-2 s^-1
for a time window from 22:43:33 UT to 23:38:37 UT
Analysis threshold: 407 GeV

E ( 175- 300 GeV): 23.60 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV):  1.52 * 10^-10 erg cm^-2 s^-1
for a time window from 23:38:37 UT to 00:32:31 UT
Analysis threshold: 291 GeV

E ( 175- 300 GeV): 15.33 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV):  1.41 * 10^-10 erg cm^-2 s^-1
for a time window from 00:32:31 UT to 01:23:06 UT
Analysis threshold: 224 GeV

E ( 125- 175 GeV): 22.23 * 10^-10 erg cm^-2 s^-1
E ( 175- 300 GeV):  7.87 * 10^-10 erg cm^-2 s^-1
E ( 300-1000 GeV):  1.15 * 10^-10 erg cm^-2 s^-1
for a time window from 01:23:06 UT to 02:13:04 UT
Analysis threshold: 186 GeV

This message can be cited.


GRB_name: GRB090809A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9765
SUBJECT: VLA radio upper limit on GRB 090809
DATE:    09/08/11 14:53:03 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of a
larger collaboration:

"We used the Very Large Array to observe the field of view toward
GRB 090809 (GCN 9754) at a frequency of 8.46 GHz on 2009 Aug. 11.37
UT. The GRB radio afterglow is undetected. The peak flux at the NOT
optical afterglow position (GCN 9755) is 8+/-39 uJy.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB090809A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9766
SUBJECT: Title: GRB 090809: Further NOT optical observations
DATE:    09/08/11 17:31:56 GMT
FROM:    Dong Xu at DARK,NBI  <dong@astro.ku.dk>

D. Xu, G. Leloudas, J. P. U. Fynbo, D. Malesani (DARK/NBI), P. Jakobsson 
(Univ. Iceland), and and G. Furesz (CfA/Harvard) report on behalf of a 
larger collaboration:

We continued to observe the field of GRB 090809 (Markwardt et al., GCN 
9754; Xu et al., GCN 9755; Landsman et al., GCN 9758) with the Nordic 
Optical Telescope equipped with ALFOSC.  We obtained 4x300 s i-band 
frames staring on August 10th,  22:25:35 UT, 28.9 hr after the burst.

The optical afterglow is still detected in the stacked frame. The 
magnitude is i=22.3+/-0.1 against several reference stars of the USNO B1 
catalog in the field. The improved magnitude in our previous observation 
is i=20.20+/-0.04, being consistent with the measurement in Wiersema et 
al. (GCN 9762).  Therefore, the optical afterglow is decaying with a 
power-law slope of \alpha=1.0, similar to the general decaying of the 
X-ray afterglow (Mao et al., GCN 9759).

We note that the rest-frame T90 (Barthelmy et al., GCN 9756) is less 
than 2 s for this burst at z=2.737 (Malesani et al., GCN9761). But the 
early energetic X-ray flares tend to make this burst more consistent 
with the class of the conventional long bursts.


GRB_name: GRB090807B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9767
SUBJECT: GRB 090807B: Fermi GBM detection
DATE:    09/08/11 22:36:36 GMT
FROM:    Bill Paciesas at UAH  <bill.paciesas@nasa.gov>

W. Paciesas (UAHuntsville) reporta on behalf of the Fermi GBM Team:

"At 19:57:59.02 UT on 7 August 2009, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 090807B (trigger 271367881 / 090807.832).
The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 326.9, Dec = +7.2 (J2000 degrees, equivalent to
J2000 21h 48m, +7d 12'), with a statistical uncertainty of 2.6 degrees
(radius, 1-sigma containment, statistical only; there is additionally
a systematic error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 45 degrees.

The GBM light curve consists of a single structured pulse with a duration
of about 3 s (8-1000 keV). The time-averaged spectrum from T0-0.640 to T0+1.408 s
is best fit by a Band function with Epeak = 37 +/- 5 keV,
alpha = -0.6 +/- 0.4, and beta = -2.4 +/- 0.1 (chi^2 387 for 357 d.o.f.).
The fluence (8-1000 keV) in this time interval is (1.02 +/- 0.07)E-06 erg/cm^2.
The 1-sec peak photon flux measured starting from T0-0.512 s in the 8-1000 keV band
is 10.9 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090812A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9768
SUBJECT: GRB 090812: Swift detection of a burst with an optical counterpart
DATE:    09/08/12 06:20:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. Stamatikos (NASA/ORAU), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), C. Gronwall (PSU),
C. Guidorzi (U Ferrara), C. B. Markwardt (CRESST/GSFC/UMD),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL) and R. L. C. Starling (U Leicester) report on
behalf of the Swift Team:

At 06:02:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090812 (trigger=359711).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 353.194, -10.595 which is 
   RA(J2000) = 23h 32m 47s
   Dec(J2000) = -10d 35' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a triple-peaked
structure with a duration of about 70 sec.  The peak count rate
was ~6500 counts/sec (15-350 keV), at ~25 sec after the trigger. 

The XRT began observing the field at 06:03:25.7 UT, 76.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 353.20133, -10.60457 which
is equivalent to:
   RA(J2000)  = 23h 32m 48.32s
   Dec(J2000) = -10d 36' 16.5"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 43 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
2.26e+20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 4.95e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
298 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 23:32:48.53 = 353.20222
  DEC(J2000) = -10:36:17.3  = -10.60481
with a 90%-confidence error radius of about 0.78 arc sec. This position is 5.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.62 with a 1-sigma error of about 0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.02. 

Burst Advocate for this burst is M. Stamatikos (michael AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090812A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9769
SUBJECT: GRB 090812: P60 Confirmation of Optical Afterglow
DATE:    09/08/12 06:53:20 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration:

We have imaged the field of GRB090812 (Stamatikos et al., GCN 9768) with
the automated Palomar 60 inch telescope.  Observations were obtained in
the Sloan r', i', and z' filters beginning at 6:34 UT (~ 2.5 minutes after
the burst).

Near the XRT afterglow we detect a point source at coordinates (J2000):

   RA: 23:32:48.55
   Dec: -10:36:17.0

with an estimated uncertainty of ~ 0.3" in each coordinate.  This is
consistent with the position reported by the UVOT.

We measure the following magnitudes for the source, calculated with
respect to the SDSS DR7:

Time (UT mid-point)  Exposure (s)   Filter       Magnitude
-----------------------------------------------------------------------
06:05:02             60             r'           16.18
06:06:27             60             i'           16.39
06:09:28             60             r'           17.30
06:10:43             60             i'           17.34

The fading nature confirms this is the afterglow of GRB090812.

Further observations are planned.


GRB_name: GRB090812A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9770
SUBJECT: GRB 090812: Liverpool Telescope afterglow confirmation
DATE:    09/08/12 07:19:41 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

R.J. Smith (Liverpool JMU), A. Gomboc (U. Ljubljana), C. Guidorzi (U. 
Ferrara),
C.G. Mundell, I.A. Steele, A. Melandri, S. Kobayashi, C.J. Mottram, D.F. 
Bersier,
Z. Cano (Liverpool JMU) report on behalf of a large collaboration:

On 2009 August 12 at 06:03:54 UT the 2-m Liverpool Telescope automatically
began observing the Swift GRB 090812 (Stamatikos et al., GCN Circ. 9768)
using the r' and i' filters.

We clearly detected the fading optical afterglow reported by Swift-UVOT
and P60 (Cenko et al. GCN Circ. 9769) with the following values:

Mid Time   Delay from BAT   Total Exp  Filter     Mag
(UT)       trigger (s)      (s)
----------------------------------------------------------
06:03:59    111             10         r'    15.51 +- 0.04
06:06:26    258             10         r'    16.60 +- 0.10
----------------------------------------------------------

Magnitudes have been calibrated from nearby SDSS stars.


GRB_name: GRB090812A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9771
SUBJECT: GRB 090812 VLT redshift
DATE:    09/08/12 09:02:26 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (INAF-OAB), J. Gorosabel (IAA-CSIC),
J.P.U. Fynbo (DARK/NBI), K. Wiersema and N. Tanvir (Leicester)
report on behalf of a larger collaboration

We have observed the afterglow of GRB 090812 (Stamatikos et al.
GCNC 9768) using FORS2 at the VLT (Paranal observatory) starting
at 06:54 UT (52min after the burst). In the spectrum we detect strong
absorption lines, including Ly-alpha, SiII, SiII*, CII, SiIV, CIV,  
SiII, AlII,
AlIII, FeII, ZnII, MnII and TiII at a common redshift of 2.452 which we
identify as the redshift of the GRB. We also detect absorption lines  
from an
unidentified intervening system. Further analysis is ongoing.

We acknowledge the excellent support from Paranal staff, in particular
Jonathan Smoker, Cedric Ledoux and Karla Aubel.


GRB_name: GRB090812A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9772
SUBJECT: GRB 090812: Enhanced Swift-XRT position
DATE:    09/08/12 10:25:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 456 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 090812, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 353.20225, -10.60489 which is equivalent
to:

RA (J2000): 23h 32m 48.54s
Dec (J2000): -10d 36' 17.6"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090812A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9773
SUBJECT: GRB 090812: GROND Observations of the Optical/NIR Afterglow
DATE:    09/08/12 11:54:31 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

Adria Updike (Clemson University), Arne Rau, Thomas Kruehler, Felipe 
Olivares, and Jochen Greiner (all MPE Garching) report on behalf of the 
GROND team:

We observed the field of GRB 090812 (Swift trigger 359711; Stamatikos et 
al., GCN #9768) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla 
Observatory (Chile).

Due to cloud coverage, observations started only at 08:13 UT on August 12, 
2 hours and 11 minutes after the GRB trigger. They were performed at an 
average seeing of 1.1" and at an average airmass of 1.2 with light cirrus, 
and continued until twilight.

We clearly detect the afterglow in stacked images (Stamatikos et al. GCN 
#9768, Cenko GCN #9769). Based on the first 4 min of total exposures, we 
estimate preliminary magnitudes and upper limits (all in AB system) of

g' = 22.15 +- 0.15 mag,
r' = 21.50 +- 0.08 mag,
i' = 21.30 +- 0.13 mag,
z' = 21.02 +- 0.12 mag,
J = 20.57 +- 0.15 mag,
H > 19.8 mag,
K > 18.9 mag

The given magnitudes are calibrated against SDSS as well as 2MASS field 
stars and are not corrected for the expected Galactic foreground extinction 
corresponding to a reddening of E_(B-V)=0.02 mag in the direction of the 
burst (Schlegel et al. 1998).

The foreground extinction corrected spectral energy distribution is well 
fit with a pure power law and a spectral index of beta = 1.1+/-0.2 and no 
strong evidence of excess extinction.

The flux difference between the g' band magnitude and the extrapolation of 
the power law as defined by r'i'z'J is consistent with Lyman-alpha 
absorption at a redshift of 2.45 as reported by de Ugarte Postigo et al. 
(GCN #9771).


GRB_name: GRB090812A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9774
SUBJECT: GRB090812: Swift/UVOT observations
DATE:    09/08/12 13:52:31 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL) and M. Stamatikos (NASA/ORAU) report on behalf of the 
Swift UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090812 86s 
after the BAT trigger (Stamatikos et al., GCN Circ. 9768). An 
uncatalogued, fading source is detected in the UVOT white, v, b and u band 
filters at the position reported in Stamatikos et al. (GCN Circ. 9768), 
consistent with the refined XRT error circle (Goad et al., GCN Circ. 
9772). The detection of the afterglow in the white, v, b and u filters is 
consistent with the spectroscopic redshift of z=2.452 reported by Ugarte 
Postigo et al. (GCN Circ. 9771). Early time UVOT obserations indicate a 
decay rate of alpha~1.5.

The magnitudes and 3-sigma upper limits for the UVOT observations of GRB 
090812 in each filter are as follows:

Filter  T_start(s)  T_stop(s)  Exp(s)  Mag/3-sig UL
white      86         235       146    17.35+/-0.03
v          628        647       19     18.17+/-0.41
b          554        573       19     18.62+/-0.28
u          299        548       246    18.65+/-0.11
uvw1       677        1124      58     > 19.20
uvm2       652        1099      58     > 18.72
uvw2       603        1050      58     > 19.13

The values quoted above are not corrected for the Galactic extinction due 
to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel 
et al. 1998). The photometry is on the UVOT photometric system described 
in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB090812A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9775
SUBJECT: GRB 090812 Swift-BAT Refined Analysis
DATE:    09/08/12 15:09:27 GMT
FROM:    Michael Stamatikos at OSU/GSFC  <michael.stamatikos-1@nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), 
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU/NASA/GSFC),
J. Tueller (GSFC), T. N. Ukwatta (GWU) on behalf of the Swift-BAT team:
  
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 090812 (trigger #359711)
(Stamatikos, et al., GCN Circ. 9768).  The BAT ground-calculated position is
RA, Dec = 353.200, -10.609 deg which is 
   RA(J2000)  =  23h 32m 47.9s 
   Dec(J2000) = -10d 36' 34.1" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
 
The burst starts at ~T-4 sec and ends at ~T+120 sec, with 3 peaks at ~T+5 sec,
 ~T+27 sec and ~T+55 sec, respectively. T90 (15-350 keV) is 66.7 +- 14.7 sec 
(estimated error including systematics).
 
The time-averaged spectrum from T-5.4 to T+113.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.24 +- 0.05.  The fluence in the 15-150 keV band is 5.8 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+26.82 sec in the 15-150 keV band
is 3.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/359711/BA/.

[GCN OPS NOTE(13aug09):  Per author's request, the "080912" was changed
to "090812" in the Subject line.]


GRB_name: GRB090812A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9776
SUBJECT: GRB 090812, RIMOTS optical upper limits
DATE:    09/08/12 15:14:43 GMT
FROM:    Kazuhiro Noda at Miyazaki U  <kaz1206@astro.miyazaki-u.ac.jp>

K.Noda, A.Daikyuji, K.Kono, E.Sonoda,
N.Ohmori, H.hayasi, M.Yamauchi
(University of Miyazaki)

We have observed the field covering the error circle of
GRB 090812 (Swift trigger 359711, GCN 9768, M. Stamatikos et al.)
with the unfiltered CCD camera on the 30-cm telescope 
at University of Miyazaki.
The observation was started 12:30:59 UT, about 6.5 hr
after the Swift trigger time.
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position.
((GCN 9768(M. Stamatikos et al.), GCN 9769(S. B. Cenko et al.)
 GCN 9770(R.J. Smith et al.), GCN 9772(M.R. Goad et al.)
 GCN 9773(Adria Updike et al.), GCN 9774(P. Schady et al.))

the upper limits are as follows:
--------------------------------------------------------------
Start(UT)   End(UT)    Num. of frames    Limit (mag.)
--------------------------------------------------------------
12:30:59    12:31:29          1            12.1
12:30:59    13:45:22         62            17.3
---------------------------------------------------------------


GRB_name: GRB090812A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9777
SUBJECT: GRB 090812: Swift XRT refined analysis
DATE:    09/08/12 15:19:27 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R. Starling (U. Leicester) and M. Stamatikos (NASA/ORAU) report on behalf 
of the Swift-XRT team:

We have analysed the first two orbits of Swift XRT data for GRB 090812 
(trigger=359711, Stamatikos et al. GCN Circ. 9768) spanning T0+78 s to 
T0+12.4 ks. The UVOT-enhanced XRT position was given by Goad et al. in GCN 
Circ. 9748.

The light curve shows initial flaring, with two large flares overlaid on a 
power law of decay slope alpha1=1.5+/-0.5. The power law then breaks at 
approximately 960 s to a shallower slope of alpha=1.05+/-0.10.

A power law is an acceptable fit to a spectrum formed from the first orbit 
windowed timing (WT) mode data centred at T0+230 s, with a photon index, 
Gamma, of 1.97+/-0.03. The resulting column density at the source 
(z=2.452, de Ugarte Postigo et al. GCN Circ. 9771) is (1.00+/-0.09)e22 
cm^-2 in addition to the Galactic column of 2.26e20 cm^-2 (Kalberla et al. 
2005). 
The 0.3-10 keV observed (unabsorbed) count to flux conversion is 1 ct = 
3.4e-11 (4.2e-11) erg/cm2/s.
A fit to the spectrum formed from the first and second orbit photon 
counting (PC) mode data centred at T0+2760 s is consistent with the WT 
spectral results.

Interestingly, the X-ray spectral slope we derive is consistent with slope 
reported for the optical data from GROND, centred at T0+7860 s (Updike et 
al. GCN Circ. 9773.), which may imply a single spectral slope between
the X-ray and optical bands several thousand seconds after the trigger. 

While we only have two orbits of data, if we assume the light curve 
continues to decay with a power law of index alpha=1.05, the 
predicted count rate at T+24 hours will be 0.023 count s^-1, 
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.7e-13 
(9.5e-13) erg cm^-2 s^-1. 

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00359711.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090812A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9778
SUBJECT: GRB 090812: RAPTOR detections during the burst
DATE:    09/08/12 17:15:03 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis, B. Norman
of Los Alamos National Laboratory report:

The RAPTOR telescope system responded to Swift trigger
359711 (Stamatikos et al., GCN 9768) under good observing conditions.
Our narrow-field instruments began observing the location at
06:02:32.9 UTC, 24.0 s after the Swift trigger (7.0 s after
receipt of GCN message).  We obtained simultaneous observations
during the gamma-ray emitting interval in Cousins V, R, and I
bands as well as unfiltered data.  We detect the optical
counterpart in all color bands.  Initial analysis of our unfiltered
data calibrated to the USNO-B1 R-band revals the counterpart
brightening until ~T=70s after the trigger and then beginning a
steady decline.  The following table gives selected observations,
not corrected for extinction, from this event.  Further analysis
of the multi-color data is underway.

t-mid(s)    exp(s)     mag     mag-err
--------------------------------------------
26.48        5.0      15.98    0.18
46.08        5.0      15.39    0.11
73.55        5.0      14.84    0.07
91.71        5.0      15.13    0.09
101.21       5.0      15.25    0.10
141.62      10.0      15.63    0.10


GRB_name: GRB090812A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9779
SUBJECT: GRB 090812: Faulkes Telescope South Continued Optical Monitoring
DATE:    09/08/12 18:02:44 GMT
FROM:    Zach Cano at ARI/John Moores Liverpool  <zec@astro.livjm.ac.uk>

Z. Cano (Liverpool JMU), C. Guidorzi (U. Ferrara), C. Mundell, R.J. Smith,
D. Bersier, A. Melandri, I.A. Steele, S. Kobayashi, C.J. Mottram,
(Liverpool JMU), A. Gomboc (U. Ljubljana) report, on behalf of a large
collaboration:

Following our report of observations on the Liverpool Telescope (Smith et
al. GCN 9520) we continued monitoring the field of GRB090812 (Swift
trigger 359711, Stamatikos et al. GCN 9768) on the Faulkes Telescope South
(Australia) from 5.88 hours to 8.40 hours post burst in r' and i' bands.

We find from 6 x 300s stacked images:

t_exp          filter    t-T0          R-mag
----------------------------------------------------------
30min          i'        5.88 hours    22.43 +/- 0.25
30min          i'        8.40 hours    22.85 +/- 0.25
30min          r'        6.60 hours    22.31 +/- 0.09
----------------------------------------------------------

The calibration is still preliminary and determined against stars in
the sdss field.

Finally, we find the decay rate in i' from 111s to 2.35ks post burst is
consistent with alpha ~ 1.25 +/- 0.1


GRB_name: GRB090812A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9780
SUBJECT: GRB 090812: WIRO NIR upper limit
DATE:    09/08/12 20:06:03 GMT
FROM:    Jay Norris at U. of Denver  <jaypnorris@gmail.com>

Alexander Kutyrev (CRESST/UMCP/GSFC), Jay Norris (U. Denver),
report on behalf of the Goddard/U. Wyoming NIR camera collaboration.

We observed the afterglow position of GRB 090812 as reported by Cenko
(GCN Circ. 9769) with the 2.3-meter WIRO telescope and the Goddard
NIR camera, commencing 10:28 UT, 4.4 hrs after the Swift trigger
(Stamatikos et al., GCN Circ. 9768).

Using stacked J-band images with a total exposure time of 1360 s,
via comparison with two adjacent 2-MASS stars, we derive the following
3 sigma upper limit for the afterglow:

 Tmid (UT) Mag

 10:46 J-band > 21.2


GRB_name: GRB090813A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9781
SUBJECT: GRB 090813: Swift detection of a burst
DATE:    09/08/13 04:26:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
C. Gronwall (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
M. Stamatikos (OSU/NASA/GSFC) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:

At 04:10:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090813 (trigger=359884).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 227.017, +88.573 which is 
   RA(J2000) = 15h 08m 04s
   Dec(J2000) = +88d 34' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peaks
with a duration of about 8 sec.  The peak count rate
was ~9000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:12:01.7 UT, 78.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 225.8016, +88.5687 which is equivalent to:
   RA(J2000)  = 15h 03m 12.38s
   Dec(J2000) = +88d 34' 07.3"
with an uncertainty of 6.1 arcseconds (radius, 90% containment). This
location is 110 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 6.26e-10 erg cm^-2 s^-1 (0.2-10
keV). 


UVOT took a finding chart exposure of 150 seconds with the White filter
starting 87 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.17. 




Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090813A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9782
SUBJECT: GRB 090813: optical candidate from 1.23m CAHA telescope
DATE:    09/08/13 05:01:48 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel, V. Terron, M. Fernandez, P. Kubanek, M. Jelinek, A.J.
Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration, report;

We have  carried out  I-band observations of  the XRT position  of GRB
090813  (GCN  9781) with  the  1.23m  telescope  of Calar  Alto.   The 
observations started  at 04:18  UT (437 s  after the GRB  trigger). We
detect an object  with a rough magnitude of I~17 coincident with the XRT
position  no present  on the  DSS. We propose  that object  as the optical
afterglow of GRB 090813.


GRB_name: GRB090813A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9783
SUBJECT: GRB 090813: P60 Optical Afterglow Confirmation
DATE:    09/08/13 05:25:55 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (Caltech) reports on behalf of a larger collaboration:

We have imaged the field of GRB090813 (Cummings et al., GCN 9781) with the
automated Palomar 60 inch telescope.  Observations were taken in the Sloan
r', i', and z' filters beginning at approximately 4:12 UT (~ 2 minutes
after the burst).

Inside the XRT error circle we find a fading point source with coordinates
(J2000):

   RA: 15:03:08.48
   Dec: +88:34:05.5

with an estimated error of ~ 0.3" in each coordinate.  Presumably this is
the same source identified by Gorosabel et al. (GCN 9782).

With reference to several USNO-B1 sources in the field, we measure the
following I-band magnitudes for the afterglow:

UT (mid-point)     Exposure (s)       Magnitude
----------------------------------------------------------------
04:15:47           60                 17.8
04:20:33           60                 18.2

Further observations are planned.


GRB_name: GRB090813A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9784
SUBJECT: GRB 090813: Liverpool Telescope afterglow confirmation
DATE:    09/08/13 06:17:10 GMT
FROM:    James Smith at ARI,Liverpool John Moors U  <rjs@astro.livjm.ac.uk>

R.J. Smith, I.A. Steele, Z. Cano (Liverpool JMU), C. Guidorzi (U.
Ferrara),  C.G. Mundell, A. Melandri, S. Kobayashi, C.J. Mottram,
D.F. Bersier,  (Liverpool JMU), A. Gomboc (U. Ljubljana), report on behalf 
of a large collaboration:

On 2009 August 13 at 04:13:40.8 UT the 2-m Liverpool Telescope
automatically began observing the Swift GRB 090813 (Cummings et al.,
GCN Circ. 9781) using the r' and i' filters. We confirm the detection by 
Gorosabel et al (GCN 9782) and Cenko et al (GCN 9783) of an optical 
counterpart to the XRT source. We measure a position of 15:03:05.9 
88:34:05.5 J2000 with an uncertainty of 1arcsec and further, confirm the 
OT is fading. Ths position is 1 arcsec from and therefore conssitent from 
that reported by Cenko et al (GCN 9783).


Mid Time     Delay from BAT   Total Exp  Filter     Mag
(UT)      trigger (min)      (s)
----------------------------------------------------------
04:13:45.8      3.05  10 R 19.36 +/- 0.13
04:18:11.9      7.48  120 R 19.90 +/- 0.05
04:20:58.2     10.25  120 I 18.11 +/- 0.02
----------------------------------------------------------

Both astrometry and photometry is calibrated and quoted with respect
to USNO-B.

Further observations are ongoing.


GRB_name: GRB090813A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9785
SUBJECT: GRB 090813: Enhanced Swift-XRT position
DATE:    09/08/13 11:51:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 615 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 090813, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 225.77887, +88.56795 which is equivalent
to:

RA (J2000): 15h 03m 6.93s
Dec (J2000): +88d 34' 04.6"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090813A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9786
SUBJECT: GRB090813: Swift/UVOT upper limits
DATE:    09/08/13 13:16:46 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL) and J.R. Cummings (NASA/UMBC) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 090813 88s 
after the BAT trigger (Cummings et al., GCN Circ 9781). No new source is 
detected within the XRT error circle or at the optical position reported 
by Cenko (GCN Circ. 9783) in any of the individual or combined UVOT 
filters.

The 3-sigma upper limits of detected a source at the position of the 
optical afterglow reported by Cenko (GCN Circ. 9783) in the first white 
band finding chart (fc) observation, and in consecutive coadded 
observations for each of the UVOT filters are as follows:

Filter  T_start(s)  T_stop(s)  Exp(s)  Mag 3-sig UL
wh (fc)    88         237      147       > 20.55
wh         581        1894     264       > 21.35
vv         631        1943     156       > 19.39
bb         556        1869     136       > 20.29
uu         300        2017     382       > 20.44
w1         681        1992     156       > 19.73
m2         656        1967     156       > 19.41
w2         607        1919     156       > 19.83

The values quoted above are not corrected for the Galactic extinction due 
to the large reddening of E(B-V) = 0.17 in the direction of the burst 
(Schlegel et al., 1998). The photometry is on the UVOT photometric system 
described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB090813A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9787
SUBJECT: Konus-Wind observations of GRB090813
DATE:    09/08/13 13:30:59 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline
on behalf of the Konus-Wind team, report:

GRB 090813 (Swift trigger=359884: Cummings et al., GCN 9781)
triggered Konus-Wind at T0=15041.925 s UT (04:10:41.925)

The burst started with a double-peaked structure with a
duration of ~2 s.
Another, softer peak, with a duration of ~1.5 s,
was observed at T0 + 6s.

The Konus-Wind light curves of this GRB are available at
http://www.ioffe.ru/LEA/GRBs/GRB090813_T15041/

As observed by Konus-Wind the burst had
a fluence of 2.4(-0.4,+0.5)x10-6 erg/cm2, and
a 64-ms peak flux, measured from T0,
of 3.3(-0.6,+0.7)x10-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst (from T0 to T0+8.448 s)
is well fitted (in the 20 keV - 1 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.37(-0.28,+0.35),
and Ep = 104(-23,+41)keV (chi2 = 58/61 dof).

Fitting by GRB (Band) model yields to the same alpha and Ep values
with the high energy photon index beta < -9.

The spectrum at the maximum count rate, measured from T0 to T0+0.256 s,
is well fitted (in the 20 keV - 1 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.85(-0.29,+0.34),
and Ep = 195(-43,+71)keV (chi2 = 20/23 dof).

All the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB090813A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9788
SUBJECT: GRB 090813, Swift-BAT refined analysis
DATE:    09/08/13 13:55:52 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 090813 (trigger #359884)
(GRB 090813, Cummings et al., GCN Circ. 9781). The BAT
ground-calculated position is RA, Dec = 225.065, 88.571 deg which is
RA(J2000) = 15h 00m 15.6s
Dec(J2000) = +88d 34' 15.8"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.

The mask weighted lightcurve had three main spikes, at T+0, T+1 and
T+6.5 sec, each with a duration of about 1 sec. T90 (15-350 keV) was
7.1 +- 0.6 sec (estimated error including systematics). The three
spikes were progressively softer.

The time-averaged spectrum from T-0.8 to T+7.3 sec is best fit by a
simple power-law model. The power law index of the time-averaged
spectrum is 1.69 +- 0.12. The fluence in the 15-150 keV band is 1.3 +-
0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.04 sec
in the 15-150 keV band is 8.5 +- 0.6 ph/cm2/sec. All the quoted errors
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/359884/BA/


GRB_name: GRB090813A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9790
SUBJECT: GRB 090813: Swift-XRT refined analysis
DATE:    09/08/13 15:43:56 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A. P. Beardmore (U. Leicester) and J. R. Cummings (NASA/UMBC) report
on behalf of the Swift-XRT team:

We have analysed 8.8 ks of XRT data for GRB 090813 (Cummings et
al., GCN Circ. 9781), from 84 s to 19.3 ks after the BAT trigger. The
data span four orbits, comprising 810 s in Windowed Timing (WT) mode
with the remainder in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN. Circ 9785).

The X-ray light curve initially follows a shallow decay, with a decay 
index of 0.22 +/ 0.10, before steepening to an index of 1.15 +/- 0.03 at 
about 450 s after the trigger.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 +/- 0.07. The
best-fitting absorption column is (2.23 +0.20 -0.19) x 10^21 cm^-2, in
excess of the Galactic value of 6.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.00 +0.11 -0.10 and
a best-fitting absorption column of (2.3 +/- 0.3) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.3 x 10^-11 (6.4 x 10^-11) erg cm^-2
count^-1.

If the light curve continues to decay with a power-law decay index of
1.15, the estimated count rate at T+24 hours will be 0.016 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of
6.9 x 10^-13 (1.0x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00359884.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090813A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9792
SUBJECT: GRB 090813: Fermi GBM observation
DATE:    09/08/13 16:48:15 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 04:10:42.59 UT on 13 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090813 (trigger 271829444  / 090813174), which 
was also detected by the SWIFT-BAT (Cummings et al. 2009, GCN 9781)
and Konus/Wind (Golenetskii et al., 2009, GCN Circular 9787).
The GBM on-ground location is consistent with the Swift position.
 
The angle from the Fermi LAT boresight is 35.3 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of two separate pulses with a 
duration (T90) of about 9 s (8-1000 keV). The time-averaged 
spectrum from T0-0.256 s to T0+8.960 s is well fit by a 
power law function with an exponential high energy cutoff. 
The power law index is -1.43 +/- 0.08 an the cutoff energy, 
parameterized as Epeak, is 161 +/- 26 keV
(chi squared 495 for 480 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(3.5 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+0.512 s in the 8-1000 keV band 
is 14.4 +/- 0.5 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 492 
for 479 d.o.f.) with Epeak= 95 +/- 30 keV, alpha = -1.25 +/- 0.18 
and beta = -2.0 +/- 0.1. 

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090814A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9793
SUBJECT: GRB 090814: Swift detection of a burst
DATE:    09/08/14 01:13:22 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (GSFC/GWU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), C. Gronwall (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
M. Stamatikos (OSU/NASA/GSFC) and M. A. Stark (PSU) report on behalf
of the Swift Team:

At 00:52:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 090814 (trigger=359951).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 239.611, +25.599 which is 
   RA(J2000) = 15h 58m 27s
   Dec(J2000) = +25d 35' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple weak peaks 
with a total duration of about 30 seconds.  The peak count rate
was ~500 counts/sec (15-350 keV), at 10 sec before the trigger. 

The XRT began observing the field at 00:54:58.3 UT, 159.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
239.6095, 25.6310 which is equivalent to:
   RA(J2000)  = 15h 58m 26.29s
   Dec(J2000) = +25d 37' 51.7"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 115 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
4.76e+20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.65e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 169 seconds after the BAT trigger. No credible
afterglow candidate has  been found in the initial data products. The
2.7'x2.7' sub-image covers 100% of  the XRT error circle. The 3-sigma
UL at the XRT position is 19.2 mag.   No correction has been made for
the expected extinction corresponding to E(B-V) of  0.08. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB090814A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9794
SUBJECT: GRB 090814: GROND Detection of an Optical Afterglow Candidate
DATE:    09/08/14 02:59:30 GMT
FROM:    Felipe Olivares Estay at MPE  <felipe@mpe.mpg.de>

GRB 090814: GROND Detection of an Optical Afterglow Candidate 

Adria Updike (Clemson University), Felipe Olivares, Paulo Afonso,
Abdullah Yoldas, Jochen Greiner (all MPE Garching) report on behalf of
the GROND team: 

We observed the field of GRB 090814 (Swift trigger 359951; Ukwatta et
al., GCN #9793) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La
Silla Observatory (Chile). 

Observations started at 00:59 UT on Aug 14 2009, 7 minutes after the
GRB trigger. They were performed at an average seeing of 1" and at an
average airmass of 2.2. 

We found a single point source within the Swift-XRT error circle
reported by Ukwatta et al. (GCN #9793) at 

RA (J2000) = 15 h 58 m 26.35 s
DEC (J2000) = +25d 37' 52.4" 

with an uncertainty of 0.5". The candidate afterglow has the following
preliminary AB magnitudes obtained from a first 140s g'r' exposure and
240s in the nIR: 

g' = 21.62 +/- 0.04
r' = 21.21 +/- 0.04
J > 21.1
H > 19.2 

calibrated against SDSS and 2MASS catalogs. No extinction correction
was applied. Ongoing data reduction suggests the source is fading.


GRB_name: GRB090814B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9795
SUBJECT: GRB 090814B: a long GRB localized by INTEGRAL
DATE:    09/08/14 03:07:20 GMT
FROM:    Volker Beckmann at ISDC  <Volker.Beckmann@obs.unige.ch>

V.Beckmann (ISDC, Versoix), D.Gotz (CEA-Saclay), S.Mereghetti,  
A.Paizis (IASF-Milano), A. Neronov, M. Beck (ISDC, Versoix), and J.  
Borkowski (CAMK, Torun) on
behalf of the IBAS Localization Team report:

A long GRB with duration of about 50 s has been detected by IBAS in
IBIS/ISGRI data at 01:21:33 UT on August 14th.

The refined coordinates (J2000) are:

  RA:   64.7488 [degrees]
  DEC: +60.5796 [degrees]

with an uncertainty of 2.9 arcmin (90% c.l.).

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB090814A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9796
SUBJECT: GRB 090814: Enhanced Swift-XRT position
DATE:    09/08/14 03:58:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2113 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 090814, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 239.61014, +25.63088 which is equivalent
to:

RA (J2000): 15h 58m 26.43s
Dec (J2000): +25d 37' 51.2"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, arXiv:0812.3662).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB090814A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9797
SUBJECT: GRB090814A: VLT spectroscopy
DATE:    09/08/14 05:07:03 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

P. Jakobsson (Univ. Iceland), A. de Ugarte Postigo (INAF-OAB),
J. Gorosabel (IAA-CSIC), N. Tanvir (Leicester),
L. Christensen (ESO), J.P.U. Fynbo (DARK/NBI)
report on behalf of a larger collaboration,

We have observed the field of GRB 090814A (Ukwatta et al. GCN 9793)
using FORS2 at the VLT (Paranal observatory) starting at 02:05 UT
(70 minutes after the burst). We detect the object identified by  
Updike et
al. (GCN 9794) with a magnitude of R~21.5.

The spectrum shows continuum down to at least 3900 Angstroms.
Non detection of Ly-alpha implies a limit of z < 2.2. We identify a
weak absorption system at z=0.696 through the detection of MgII and  
CaII.
This is therefore likely to be the redshift of the GRB but we note that
it could also be produced by an intervening system and thus the strict
redshift range for this GRB would be 0.696 < z < 2.2.

We acknowledge the excelent support from Parnal observatory, in
particular J. Smoker and L. Rivas.


GRB_name: GRB090813A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9798
SUBJECT: GRB 090813: correction to GCN 9787
DATE:    09/08/14 10:57:53 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, on behalf of Konus-Wind team, report:

The correct upper limit for the high energy spectral index (beta)
for the GRB (Band) model fit to Konus-Wind time integrated spectrum
of GRB 090813 is -2.23 (90% confidence level, 20-1000 keV range).


GRB_name: GRB090814A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9799
SUBJECT: GRB 090814A: Swift-BAT refined analysis
DATE:    09/08/14 12:55:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 090814A (trigger #359951)
(Ukwatta, et al., GCN Circ. 9793).  The BAT ground-calculated position is
RA, Dec = 239.613, 25.586 deg which is 
   RA(J2000)  =  15h 58m 27.2s 
   Dec(J2000) = +25d 35' 09.0" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.
 
The mask-weighted light curve shows a few semi-overlapping peaks starting
at ~T-18 sec, peaking at ~T-13 sec, peaking at ~T+8 sec, and ending
at ~T+115 sec.  There is possible 10-sec precursor peak (3 sigma) at ~T-145 sec.
T90 (15-350 keV) is 80 +- 8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-16.4 to T+73.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.81 +- 0.19.  The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-12.68 sec in the 15-150 keV band
is 0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/359951/BA/


GRB_name: GRB090814A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9800
SUBJECT: GRB 090814A, RIMOTS optical upper limits
DATE:    09/08/14 13:16:44 GMT
FROM:    Arata Daikyuji at Miyazaki U  <daikyu524@astro.miyazaki-u.ac.jp>

A.Daikyuji, K.Noda, H.hayasi, K.Kono,
N.Ohmori, E.Sonoda, M.Yamauchi
(University of Miyazaki)

We have observed the field covering the error circle of
GRB 090814A (Swift trigger 359951, GCN 9793, T. N. Ukwatta et al.)
with the unfiltered CCD camera on the 30-cm telescope
at University of Miyazaki.
The observation was started 00:59 UT, about 11 hr
after the Swift trigger time.
We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,
There is no new source at the reported position.
((GCN9794(Adria Updike et al.))

the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames Limit (mag.)
--------------------------------------------------------------
11:08:33    11:09:03         1            16.2
11:08:33    11:48:08        36            17.3
---------------------------------------------------------------


GRB_name: GRB090814A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9801
SUBJECT: GRB 090814A: Swift-XRT Team Refined Analysis
DATE:    09/08/14 13:33:54 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) & T. N. Ukwatta (GSFC/GWU) report on behalf of 
the Swift-XRT team: 

We have analysed the first four orbits of data collected for GRB 090814A, 
from 165 s to 25.7 ks after the BAT trigger. These data comprise 258 s in 
Windowed Timing (WT) mode and 7.8 ks in Photon Counting mode. The enhanced 
XRT position for this burst was given by Beardmore et al. in GCN Circ. 
9796.

The light curve can be modelled with a series of power-law decays, 
starting with alpha1 = 2.60 +/- 0.08 until ~T+830 s, at which point the 
decay flattens slightly to alpha2 = 1.91 +/- 0.20. The light curve 
flattens again at ~T+5.4 ks, to a slope of alpha3 = 0.51 +/- 0.48. With 
the limited data at this time, alpha3 has a relatively large uncertainty.

The spectrum extracted from the WT data can be fitted with an absorbed 
power-law, with Gamma = 2.78 +0.12/-0.11, absorbed by the Galactic column 
of NH = 4.76 x 10^20 cm^-2 (Kalberla et al. 2005), together with an 
intrinsic column (assuming z = 0.696; Jakobsson et al., GCN Circ. 9797) of 
(2.0 +/- 0.4) x 10^21 cm^-2. Note, however, that this redshift 
determination is uncertain. The total (including Galactic) column at z = 0 
would be (1.3 +/- 0.2) x 10^21 cm^-2. Alternatively, the spectrum is 
better fitted (at >3 sigma) by a broken power-law with Gamma1 = 0.47 
+0.72/-1.59 below a break energy of 0.62 +0.09/-0.08 keV, followed by 
Gamma2 = 2.62 +/- 0.09; this fit only requires the Galactic column. The 
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced 
from the broken power-law fit is 2.5 x 10^-11 (3.0 x 10^-11) erg cm^-2 
count^-1.

If the light curve continues to decay with a power-law decay index of 
0.51, the count rate at T+24 hours will be 0.0041 count s^-1, 
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x 10^-13 
(1.2 x 10^-13) erg cm^-2 s^-1. 

The results of the XRT-team automatic analysis are available at 
http://www.swift.ac.uk/xrt_products/00359951.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090814A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9802
SUBJECT: GRB 090814A: Swift/UVOT Observations
DATE:    09/08/14 13:52:07 GMT
FROM:    Peter Curran at MSSL  <pac@mssl.ucl.ac.uk>

P.A. Curran (MSSL-UCL), T. N. Ukwatta (GSFC/GWU), report on behalf of
the Swift/UVOT team:


The Swift/UVOT began settled observations of the field of GRB 090814A
170s after the BAT trigger (Ukwatta  et al., GCN 9793). The proposed
optical counterpart (Updike et al. , GCN 9794) is marginally detected in
the u and white UVOT exposures. No optical afterglow consistent with the
enhanced XRT position (Beardmore et al., GCN 9796)  is detected in the
other UVOT exposures.


Preliminary magnitudes and 3-sigma upper limits using the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627) for for the
first finding charts (FC) and subsequent exposures are:

Filter  T_start(s) T_stop(s)   Exp(s)  Mag

u       328    577          246 > 20.16 (FC)
wh      170    319          147 > 20.70 (FC)    

u       328    8144         834 21.05 +/- 0.35
b       584    8340         599 > 21.30
v       658    7528         607 > 20.18  
w1      708    7939         529 > 20.66
m2      683    7733         529 > 20.5
w2      708    7939         607 > 20.81    
wh      170    7117         699 21.54 +/- 0.27


The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.078 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090814B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9803
SUBJECT: GRB 090814B: Swift-XRT detection of a possible afterglow.
DATE:    09/08/14 14:28:39 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and W.H. Baumgartner (GSFC/UMBC) report on
behalf of the Swift-XRT team:

The Swift-XRT observed the field of the INTEGRAL GRB 090814B (Beckmann
et al. GCN. Circ. 9795), gathering 900-s of data in the interval T0+9 ks
to T0+14 ks.

In the INTEGRAL error circle we find a single, uncatalogued X-ray source
at RA,Dec=64.7546, 60.5901 which is equivalent to:

RA (J2000): 04h 19m 01.10s
Dec (J2000): +60d 35' 24.34"

with an uncertainty of 3.8 arcsec (radius, 90% confidence).

The source has a count-rate of ~0.03 count/sec, but we are unable to
determine at the present time whether the source is fading.

The spectrum comprises only 24 photons, but it can be well modelled
with an absorbed power-law with photon index Gamma=0.8 (+/-1.3) and a
column density of 9.0 (+16.0, -5.4) x 10^21 cm^-2, in excess of the
Galactic value if 3.6 x 10^21 cm^-2 (Kalberla et al. 2005).

Swift will conduct a further 4-ks observation of this source today.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090814C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9804
SUBJECT: GRB 090814C: Fermi GBM detection
DATE:    09/08/14 15:40:30 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 08:49:41.22 UT on 14 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090814C (trigger 271932583 / 090814368).
The on-ground calculated location, using the GBM trigger 
data, is RA = 332.5, DEC = 58.9 (J2000 degrees, 
equivalent to 22h 10m, 58d 54'), with an uncertainty 
of 5.5 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 61 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of a single peak
with a duration (T90) of about 0.25 s (8-1000 keV). 
The time-averaged spectrum from T0-0.064 s to T0+0.192 s is 
well fit by a power law function with an exponential
high energy cutoff.  The power law index is -0.39 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 790 +/- 120 keV
(C-stat 500 for 479 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(6.6 +/- 0.4)E-07 erg/cm^2. The 0.64-sec peak photon flux measured 
starting from T0 s in the 8-1000 keV band 
is 9.1 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090814B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9806
SUBJECT: GRB 090814B: Liverpool Telescope Observations
DATE:    09/08/14 16:28:54 GMT
FROM:    Zach Cano at ARI/John Moores Liverpool  <zec@astro.livjm.ac.uk>

C. Guidorzi (U. Ferrara), Z. Cano (Liverpool JMU), A. Gomboc
(U. Ljubljana), C.G. Mundell, I.A. Steele, A. Melandri, S. Kobayashi,
C.J. Mottram, D.F. Bersier, R.J. Smith (Liverpool JMU)
report on behalf of a large collaboration:

On 2009 August 14 at 02:57:31 UT the 2-m Liverpool Telescope
automatically began observing the INTEGRAL GRB 090814B (Beckmann et al.,
GCN Circ. 9795) using the g',r' and i' filters.

We do not detect any uncatalogued source inside the Swift-XRT error
circle (Evans et al. GCN Circ 9803) down to the following values:

Mid Time   Delay from GRB   Total Exp  Filter   Upper limit
(UT)       (hours)          (s)                 Magnitude
-----------------------------------------------------------
03:26:17    2.08            600         R         > 21.3
03:27:52    2.11            540         I         > 21.0
---------------------------------------------------------

Magnitudes have been calibrated from the nearby USNOB-1 star
04:19:01.476, +60:35:18.11 using R2=18.34 and I=17.14.

We note the considerable Galactic reddening along the GRB
direction: E(B-V)=1.14 (Schlegel et al. 1998).


GRB_name: GRB090814B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9807
SUBJECT: GRB 090814B: Swift/UVOT Upper Limits
DATE:    09/08/14 17:39:59 GMT
FROM:    Peter Curran at MSSL  <pac@mssl.ucl.ac.uk>

P.A. Curran (MSSL-UCL) and W.H. Baumgartner (GSFC/UMBC) report on behalf
of the Swift/UVOT team:


Swift/UVOT observed the field of the INTEGRAL GRB 090814B (Beckmann et
al. GCN. Circ. 9795), gathering 950s of data in the from interval T0+9ks
to T0+14 ks.

No optical afterglow consistent with the Swift XRT position (Evans et
al., GCN 9803)  is detected in the UVOT exposures.  Preliminary 3-sigma
upper limits, using the UVOT photometric system (Poole et al. 2008,
MNRAS, 383, 627), are:

Filter   T_start(s)   T_stop(s)   Exp(s)   Mag
u        8044       14166       506      >20.32
w2       8485       8933        441      >20.30

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB090814B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9808
SUBJECT: GRB 090814B: I-band observations from 1.23m CAHA telescope
DATE:    09/08/14 17:50:52 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), A. de Ugarte Postigo (INAF-OAB), V. Terron
(IAA-CSIC), M. Fernandez (IAA-CSIC), S. Guziy (IAA-CSIC), S. Castillo
(Univ. Malaga), M. Jelinek (IAA-CSIC), P. Kubanek (IAA-CSIC & IPL Univ.
Valencia), A.J. Castro-Tirado (IAA-CSIC), report;

We carried out I-band observations of the INTEGRAL GRB 090814B  (Beckmann
et al. GCN 9795) with the 1.23m Calar Alto telescope as follows;

---------------------------------------------------------
    Date         Time since GRB    Exp.     Lim.
 Start - End      Start - End      Time     Mag.
    (UT)              (Sec)        (Sec)   (3 sigma)
---------------------------------------------------------
14.0606 - 14.0739   342 - 1492     5 x 180  19.8
14.0745 - 14.0865  1544 - 2583     3 x 300  19.8
14.0871 - 14.0963  2635 - 3430     2 x 360  20.0
14.0973 - 14.1912  3518 - 11631   10 x 700  20.3
---------------------------------------------------------

No optical object is detected in the XRT position determined by Swift
(Evans et al. GCN 9803) for the upper limits given above. The combination
of all the images sets an upper limit of I = 20.6 with a total exposure
time of 9520s and a mean observing epoch of Aug 14.1259 UT.


GRB_name: GRB090814A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9809
SUBJECT: GRB090814A: NOT optical follow-ups
DATE:    09/08/14 23:02:39 GMT
FROM:    Dong Xu at DARK,NBI  <dong@astro.ku.dk>

D. Xu, J.P.U. Fynbo (DARK/NBI), P. Jakobsson (Univ. Iceland), Tiina 
Liimets (NOT) report on behalf of a larger collaboration:

We observed the field of GRB 090814A (Ukwatta et al. GCN 9793; Updike et 
al., GCN 9794) with the Nordic Optical Telescope equipped with ALFOSC. 
We obtained 3x600 s R-band frames staring on August 14th,  21:15:11 UT, 
20.38 hr after the burst.

The optical afterglow is clearly detected in each frame. The magnitude 
is R~22.4 calibrated against the reference star, #1156-0231252 with 
R2=19.25,  of the USNO B1 catalog.

Compared with the previous measurement of R~21.5 around 70 mins after 
the burst (Jakobsson et al., GCN 9797), the afterglow is decaying quite 
shallowly, with a power-law slope of ~0.3, being consistent with the 
X-ray decaying law during the same period (Page & Ukwatta, GCN 9801).


GRB_name: GRB090814B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9810
SUBJECT: GRB 090814B: Confirmation of the X-ray afterglow
DATE:    09/08/15 08:16:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and W.H. Baumgartner (GSFC/UMBC) report on
behalf of the Swift-XRT team:

The Swift-XRT conducted a second observation of GRB 090814B (Beckmann et
al. GCN. Circ. 9795), gathering 3.3 ks of data between T0+48 ks and
T0+60 ks. The source reported by Evans & Baumgartner (GCN Circ. 9803)
has faded to a level of 0.11 Â± 0.03 count/sec, with a power-law decay
index of alpha=0.7+/-0.3. This source is thus confirmed as the afterglow
of GRB 090814B.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020107.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB090813A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9811
SUBJECT: GRB 090813: CrAO optical obsevations
DATE:    09/08/15 09:29:00 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU), E. Pavlenko, O. Antoniuk, V. Rumyantsev (CrAO), A. 
Pozanenko (IKI)  report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 090813 (Cummings et al. GCN 9781) 
starting (UT) Aug. 13 23:57:26 with Shajn telescope of  CrAO under favorable 
weather condition and seeing ~1.6".
At the place of optical afterglow (Gorosabel et al. GCN 9782; Cenko et al. 
GCN 9783; Smith et al. GCN 9784) we detect a source which appears slightly 
E-W extended.

Preliminary photometry of the source in a combined image based on  USNO-B1.0 
star (RA(J2000)=15:02:47.99, Dec(J2000)=88:31:41.4) assuming R= 14.23 is 
following:

T0+     Filter, Exposure, mag.,     err.
(d)             (s)

0.8440   R       57x60     20.50 +/-0.06

Observations will be continued.


GRB_name: GRB090815A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9812
SUBJECT: GRB 090815: Fermi GBM detection
DATE:    09/08/15 13:11:29 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 07:12:12.45 UT on 15 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090815 (trigger 272013134 / 090815300).

The on-ground calculated location, using the GBM trigger 
data, is RA = 41.7, DEC = -2.0 (J2000 degrees, equivalent 
to 02h 47m, -02d 00'), with an uncertainty of 7.6 degrees 
(radius, 1-sigma containment, statistical only; there is 
additionally a systematic error which is currently estimated 
to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 87 degrees.

The GBM light curve shows two broad pulses with a duration 
(T90) of about 200 s (8-1000 keV). The time-averaged spectrum 
from T0-5.120 s to T0+24.576 s is well fit by a simple power 
law function with index -1.5 +/- 0.1 (chi squared 261 for 241 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(3.4 +/- 0.3)E-06 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+ 3.072 s in the 8-1000 keV band 
is 1.9 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB090815B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  9813
SUBJECT: GRB 090815B: Fermi GBM detection
DATE:    09/08/15 14:48:04 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 10:30:41.85 UT on 15 August 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090815B (trigger 272025043 / Y090815438).

The on-ground calculated location, using the GBM trigger data, 
is RA = 21.4, DEC = 53.4 (J2000 degrees, equivalent to 01h 26m, 53d 24'), 
with an uncertainty of 5.7 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic error which is 
currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 82 degrees.

The GBM light curve consists of two peaks with a duration (T90) 
of about 30 s (8-1000 keV). The time-averaged spectrum from 
T0-7.168 s to T0+23.552 s is well fit by a power law function 
with an exponential high energy cutoff.  The power law index 
is -1.89 +/- 0.12 and the cutoff energy, parameterized as Epeak, 
is 15.1 +/- 10.8 keV (chi squared 297 for 238 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(5.05 +/- 0.25)E-06 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+16.384 s in the 8-1000 keV band 
is 14.4 +/- 0.5 ph/s/cm^2.

A Band function fits the spectrum equally well (chi squared 296 
for 237 d.o.f.) with Epeak= 18.6 +/- 9.6 keV, alpha = -1.82 +/- 0.19 
and beta = -2.7 +/- 0.4. 

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


