# GCN_circulars

GRB_name: GRB130627B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14950
SUBJECT: GRB 130627B: Swift/UVOT Upper Limits
DATE:    13/06/28 21:31:13 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin and S. R. Oates (UCL-MSSL) report on behalf of
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of
GRB 130627B  3755 s after the BAT trigger (Oates et al.,
GCN Circ. No. 14936 and 14939).

No optical afterglow consistent with the XRT position
Evans et al. GCN Circ. No. 14947 is detected in the initial
UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC          3755         3905          147         >20.3
white             3755         5137          344         >20.9
v                 3911         5474          320         >19.5
b                 4733         4932          197         >20.1
u                 4526         4726          197         >19.7
w1                4321        11240          757         >20.3
m2                4116        10664         1082         >20.4
w2                5143         5343          197         >19.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.40 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130627A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14951
SUBJECT: GRB 130627A, Swift-BAT refined analysis
DATE:    13/06/28 23:48:10 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

G. Sato (ISAS), 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), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
S. R. Oates (UCL-MSSL), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130627A (trigger #559132)
(Oates, et al., GCN Circ. 14933).  The BAT ground-calculated position is
RA, Dec = 184.415, -37.114 deg which is
  RA(J2000)  =  12h 17m 39.7s
  Dec(J2000) = -37d 06' 51.8"
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 20%.

The mask-weighted light curve shows a single peak starting at ~T-4 sec,
peaking at ~T+2 sec, and ending at ~T+26.
T90 (15-350 keV) is 30.8 +- 12.3 sec (estimated error including systematics).

The time-averaged spectrum from T-5.2 to T+33.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.84 +- 0.32.  The fluence in the 15-150 keV band is 9.1 +- 1.9 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+1.88 sec in the 15-150 keV band
is 1.8 +- 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/559132/BA/


GRB_name: GRB130627B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14952
SUBJECT: GRB 130627B, Swift-BAT refined analysis
DATE:    13/06/28 23:48:31 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), 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), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
S. R. Oates (UCL-MSSL), D. M. Palmer (LANL), T. Sakamoto (AGU),
G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130627B (trigger #559139)
(Oates, et al., GCN Circ. 14936).  The BAT ground-calculated position is
RA, Dec = 181.914, -55.706 deg which is
  RA(J2000)  =  12h 07m 39.3s
  Dec(J2000) = -55d 42' 20.3"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.

The mask-weighted light curve shows a single peak starting at ~T-6 sec,
peaking at ~T+2 sec, and ending at ~T+22 sec.
T90 (15-350 keV) is 28.6 +- 5.8 sec (estimated error including systematics).

The time-averaged spectrum from T-10.5 to T+26.0 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.13 +- 1.03,
and Epeak of 47.6 +- 8.7 keV (chi squared 56.72 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.1 +- 0.8 x 10^-07 erg/cm2
and the 1-sec peak flux measured from T+1.82 sec in the 15-150 keV band is
0.8 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.79 +- 0.16 (chi squared 68.34 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/559139/BA/


GRB_name: GRB130701A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14953
SUBJECT: GRB 130701A: Swift detection of a burst
DATE:    13/07/01 04:31:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

N. P. M. Kuin (UCL-MSSL), D. Malesani (DARK/NBI),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU/NASA/GSFC) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:

At 04:17:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130701A (trigger=559482).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 357.216, +36.099 which is 
   RA(J2000) = 23h 48m 52s
   Dec(J2000) = +36d 05' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 8 sec.  The peak count rate
was ~10304 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 04:19:09.1 UT, 85.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 357.2287, 36.0997 which is equivalent to:
   RA(J2000)  = +23h 48m 54.89s
   Dec(J2000) = +36d 05' 58.9"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 37 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 250 seconds with the U filter starting
150 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 19.2 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
0.09. 

Burst Advocate for this burst is N. P. M. Kuin (n.kuin AT 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: GRB130701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14954
SUBJECT: GRB 130701A: optical afterglow from the NOT
DATE:    13/07/01 06:07:27 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

G. Leloudas (OKC, Stockholm and DARK/NBI), N. R. Tanvir (Univ. 
Leicester), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), P. Jakobsson 
(Univ. Iceland), O. Smirnova (NOT and Univ. Latvia), M. G. Pedersen 
(Univ. Aarhus), report:

We observed the field of GRB 130701A (Kuin et al., GCN 14953) with the 
NOT equipped with the ALFOSC camera. Observations were carried out in 
the R band and started on 2013 Jul 1.198 UT (28 min after the GRB). We 
detect a new object not visible in the DSS and SDSS surveys, at coordinates:

RA(J2000) = 23:48:55.09
Dec(J2000) = +36:06:01.4

The object had a magnitude R = 17.55 at 04:49 UT, calibrated against 
SDSS stars converted to Johnson R. The source decayed by 0.25 mag by 
04:58 UT, hence confirming it is the afterglow of GRB 130701A.


GRB_name: GRB130701A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14955
SUBJECT: GRB 130701A: Enhanced Swift-XRT position
DATE:    13/07/01 10:47:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 687 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130701A, 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 = 357.22942, +36.10058 which is equivalent
to:

RA (J2000): 23h 48m 55.06s
Dec (J2000): +36d 06' 02.1"

with an uncertainty of 2.0 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, MNRAS, 397, 1177).

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


GRB_name: GRB130701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14956
SUBJECT: GRB 130701A: VLT/X-shooter redshift
DATE:    13/07/01 12:47:53 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

D. Xu (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Malesani (DARK/NBI), P. Vreeswijk (Weizmann), V. D'Elia (INAF-OAR, ASI-ASDC), J. P. U. Fynbo (DARK/NBI), B. Milvang-Jensen (DARK/NBI), H. Flores (GEPI/Obs. de Paris), O. Hartoog (Amsterdam), P. Goldoni (APC, CEA/Irfu), L. Kaper (Amsterdam), S. D. Vergani (CNRS/GEPI)

We observed the afterglow of GRB 130701A (Kuin et al. GCN 14953, Leloudas et al. GCN 14954) with VLT/X-shooter, beginning at 2013-07-01 09:45 UT, about 5.5 hours after the burst. We obtained 2 spectra of 600s each, covering the wavelength range 3000-21000A.

From the acquisition image (Jul 1.404 UT, 5.40 hr after the GRB) we obtain a magnitude of R = 19.9 using the same calibration as in Leloudas et al. (GCN 14954).

Preliminary analysis of the spectrum reveals absorption lines of FeII
2344, 2374, 2382, MgII 2796, 2803, MgI 2852, CaII 3934, 3969 at a common redshift of z=1.155. We propose this to be the redshift of the GRB.

We thank the staff at Paranal, particularly Jonathan Smoker and Nestor Jimenez, for obtaining these observations.

[GCN OPS NOTE(01jul13) Per A.Breeveld's observation, the GRB name in the Subject-line was corrected.]


GRB_name: GRB130701A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14957
SUBJECT: GRB 130701A: Swift/UVOT Detection
DATE:    13/07/01 15:06:08 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and N. P. M. Kuin (UCL-MSSL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130701A
with the u filter 151 s after the BAT trigger (Kuin et al., GCN Circ. 
14953).
A source consistent with the enhanced XRT position (Beardmore et al., 
GCN Circ. 14955) and NOT position (Leloudas et al., GCN Circ. 14954) is 
detected in the initial UVOT exposures. There is a faint USNO-B1 source 
2.16" away (USNO-B1 1261-054544, with B2 mag of 21.10) which perhaps 
could be the host galaxy for the GRB.

Preliminary detections using the UVOT photometric system (Breeveld et 
al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

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

u_FC               151          400          246         15.52  0.1
v                 5950         6150          197         19.04  0.2
b                 5538         5737          197         19.66  0.2
w2                5744         5944          197         20.07  0.4

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.09 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130701A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14958
SUBJECT: Konus-Wind observation of GRB 130701A
DATE:    13/07/01 16:18:57 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration, soft-spectrum GRB 130701A
(Swift-BAT trigger 559482: Kuin, et al., GCN 14953)
triggered Konus-Wind at T0=15462.161 s UT (04:17:42.161)

The light curve shows a multi-peaked pulse from ~T0-0.5 s to ~T0+5 s.
The emission is seen up to 0.5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130701_T15462/

As observed by Konus-Wind, the burst
had a fluence of (5.8  0.2)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.896 s,
of (4.3  0.4)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1.2 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.1  0.1,
the peak energy Ep = 89  4 keV,
chi2 = 55.1/60 dof.

Assuming z=1.155 (Xu, et al., GCN 14956),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters of the burst:
the isotropic energy release E_iso ~ 2.1x10^52 erg,
the peak luminosity (L_iso)_max ~ 3.3x10^52 erg/s,
and the rest-frame peak energy Ep,i ~ 190 keV

All the quoted results are preliminary.


GRB_name: GRB130701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14959
SUBJECT: GRB 130701A, Swift-BAT refined analysis
DATE:    13/07/01 17:04:26 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

T. Sakamoto (AGU), 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), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+349 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 130701A (trigger #559482) (Kuin, et al., GCN Circ. 14953).
The BAT ground-calculated position is RA, Dec = 357.224, 36.100 deg
which is
   RA(J2000)  =  23h 48m 53.7s
   Dec(J2000) = +36d 05' 58.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90%
containment). The partial coding was 28%.

BAT mask-weighted light curve shows overlapping two-peak structure
starting from T-1 sec with first peak around T+1 sec and
second peak around T+3 sec. The episode ends around T+5 sec.
T90 (15-350 keV) is 4.38 +- 0.25 sec (estimated error
including systematics).

The time-averaged spectrum from T-1.14 to T+5.35 sec is best
fit by a power law with an exponential cutoff.  This fit gives a
photon index 0.90 +- 0.21, and Epeak of 89.2 +- 12.4 keV
(chi squared 40.06 for 56 d.o.f.).  For this model the total fluence
in the 15-150 keV band is 4.4 +- 0.1 x 10^-06 erg/cm2 and the 1-sec
peak flux measured from T+0.06 sec in the 15-150 keV band is
17.1 +- 0.7 ph/cm2/sec.  A fit to a simple power law gives a
photon index of 1.58 +- 0.05 (chi squared 76.39 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/559482/BA/


GRB_name: GRB130701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14960
SUBJECT: GRB 130701A: P60 Observations
DATE:    13/07/01 19:14:21 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report on behalf of a
larger collaboration:

We have observed the location of the Swift GRB130701A (Kuin et al., GCN
14953) with the robotic Palomar 60 inch telescope. Observations were
obtained in non-photometric conditions in the r', i', and z' filters
beginning at 06:52 UT on 2013 July 1 (2.58 hr after the Swift trigger).
Using nearby point sources from SDSS for photometric calibration, we
measure afterglow magnitudes of r' = 19.57 +/- 0.12 and i' = 19.36 +/-
0.10 at approximately this time.  Compared with the earlier detection from
the NOT (Leloudas et al., GCN 14954), this implies a power-law decay index
of alpha ~ 1.0.


GRB_name: GRB130701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14961
SUBJECT: GRB 130701A: Swift-XRT refined Analysis
DATE:    13/07/01 19:31:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), C.
Pagani (U. Leicester), A.P. Beardmore (U. Leicester), A. Maselli 
(INAF-IASFPA), V. Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), J.A.
Kennea (PSU) and N.P.M. Kuin report on behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 130701A (Kuin  et al. GCN
Circ. 14953),  from 91 s to 36.5 ks after the  BAT trigger. The data
comprise 214 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN. Circ 14955).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.02 (+0.03, -0.06), followed by a break at T+2249 s to
an alpha of 1.38 (+0.10, -0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.19 (+/-0.10). The
best-fitting absorption column is  1.29 (+0.22, -0.20) x 10^21 cm^-2,
in excess of the Galactic value of 6.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.97 (+0.16, -0.15)
and a best-fitting absorption column of 1.3 (+/-0.4) 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 (5.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 6.9 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index:      1.97 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.38, the count rate at T+24 hours will be 7.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.8 x
10^-13 (3.8 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/00559482.

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


GRB_name: GRB130701B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14962
SUBJECT: GRB 130701B: Fermi GBM detection
DATE:    13/07/01 22:11:12 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa (UAH) reports on behalf of the Fermi GBM Team:

"At 01:27:06.27 UT on July 1st 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130701B (trigger 394334829 / 130701060).

The on-ground calculated location, using the GBM trigger
data, is RA = 97.8, DEC = -60.1 (J2000 degrees,
equivalent to +06h 31m, -60d 07'), with an uncertainty
of 1.00 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 132 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 20 s (50-300 keV).
The time-averaged spectrum from T0-2.048 s to T0+12.288 s
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.04 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 564 +/- 55 keV
(Castor statistics 599.92 for 492 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.28 +/- 0.03)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+3.52 s in the 10-1000 keV band
is 10.5 +/- 0.4 ph/s/cm^2.

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


GRB_name: GRB130701A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14963
SUBJECT: GRB 130701A: MITSuME Akeno Optical observation
DATE:    13/07/02 11:43:41 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T. Yoshii, K. Ito, Y. Saito, Y. Yano, R. Usui, Y. Tachibana, 
S. Kurita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130701A (N. P. M. Kuin et al., GCNC 14953) with the 
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2013-07-01 14:33:09 UT ( ~10.3 h after
the burst). And we could not find any new point source within the XRT
error circle (N. P. M. Kuin et al., GCNC 14953) in all the three bands.

The results of photometry (3 sigma upper limits) are listed below.
We used GSC2.3 catalog for flux calibration.


band     T0+[hour]     MID-UT        T-EXP[sec]     magnitude
--------------------------------------------------------------------------------------------
g'             ~13.0           17:19:49         1680               >19.2
Rc           ~13.1           17:24:36         2880               >18.9
Ic             ~13.0           17:17:28         1320              >18.0
--------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [hour]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14964
SUBJECT: GRB 130623A: Second Swift-XRT  observation 
DATE:    13/07/02 13:46:06 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU) reports on behalf of the Swift team:

Swift reobserved the field of the ground-detected GRB 130623A 
(Cummings, GCN circ. 14921) again on 2013-June-30 for 10.25 ks. 
The source reported initially in Grupe et al. (circular 14926) 
seems to have faded. We do not detect the source anymore and 
can only measure a 3 sigma upper limit at a level of 
1.9e-3 counts/s in the XRT. 
This measurement suggests that the source reported in
Grupe et al. (circular 14926) may be the X-ray
afterglow of GRB 130623A.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020284.

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

[GCN OPS NOTE(02-Jul-13),  Per author's request, the typo
"...is may be the..." was changed to "...may be the...".]


GRB_name: GRB130627B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14966
SUBJECT: GRB 130627B: Swift afterglow confirmation
DATE:    13/07/03 07:35:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) and S. R. Oates (UCL-MSSL) report on behalf of
the Swift-XRT team:

Swift performed a second epoch observation of GRB 130627B (Oates et al.,
GCN Circ. 14936) on 2013 July 2nd, collecting 7.3 ks of Photon Counting
mode data from T0+390 ks to T0+415 ks. The X-ray object reported by
Evans et al. (GCN Circ. 14947) is no longer detected. The 3-sigma upper 
limit is 1.7 x 10^-3 ct/sec, which is well below the level of 
8.8(+/-2.0) x 10^-3 ct/sec at which the source was previously detected.

We therefore confirm that this object was the afterglow of GRB 130627B.

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


GRB_name: GRB130628A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14969
SUBJECT: GRB 130628A: Fermi GBM detection
DATE:    13/07/03 11:40:30 GMT
FROM:    David Byrne at UCD  <david.byrne.2@ucdconnect.ie>

D. Byrne (UCD), C. Meegan (UAH) and M. Burgess (UAH) report on behalf
of the Fermi GBM Team:

"At 12:44:02.12  UT on 28 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130628A (trigger 394116245/130628531)

High peak flux from the GRB caused GBM to issue a repoint request
that reoriented the satellite to place the GRB near the LAT boresight
for 2.5 hours, subject to Earth limb contraints.

The on-ground calculated location, using the GBM trigger
data, is RA = 6.29, DEC = -5.07 (J2000 degrees,
equivalent to 00 h 25m, -5 d 0'), with an uncertainty
of 1.71 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 67 degrees.

The GBM light curve consists of two pulses
with a duration (T90) of about 22 s (50-300 keV).
The time-averaged spectrum from T0-3.1 s to T0+25.6 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.51 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 128 +/- 11 keV.

The event fluence (10-1000 keV) in this time interval is
(9.9 +/- 0.3)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.8 s in the 10-1000 keV band
is 14.5 +/- 0.3 ph/s/cm^2.

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



-- 
David Byrne BSc.
School of Physics,
Science Center North,
University College Dublin,
Belfield, Dublin 4,
Ireland.


GRB_name: GRB130702A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14971
SUBJECT: GRB 130702A / Fermi394416326 : Fermi-LAT detection of a burst
DATE:    13/07/03 17:34:28 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

T. Cheung (NRL), G.Vianello (Stanford), S. Zhu (NASA/GSFC), J. Racusin
(NASA/GSFC), V. Connaughton (UAH) and B. Carpenter (NASA/GSFC) report
on behalf of the Fermi-LAT team:

At 00:05:23.079 UTC on July 02, 2013, Fermi GBM triggered on GRB
130702A / Fermi394416326 (trigger 394416326). The LAT detected high
energy emission from this GRB, which was also detected in the optical
band by iPTF (Singer et al., GCN 14967) and confirmed by FTN (Guidorzi
et al., GCN 14968).

The best LAT on-ground location is found to be:

RA, DEC = 216.4, 15.8 (J2000), with an error radius of 0.5 deg (90%
containment, statistical error only)

This position is 4 deg from the best GBM position (RA, Dec = 218.81,
+12.25 with a 4 deg radius), and 0.8 deg from the position of the
optical afterglow. A preliminary IPN triangulation of the burst using
GBM and Konus-Wind data gives an annulus with center RA, DEC =
260.8992, -20.7746 (J2000) of radius 50.85 degrees and a width of
(-32.73,+18.42) deg (3 sigma). The center of this annulus is 6.05 deg
(0.99 sigma) from the LAT location (Private Communication, with
possible IPN refinements using data from distant spacecraft).

The best LAT localization for the source was ~75 deg from the LAT
boresight at the time of the trigger, i.e., outside the nominal field
of view of the LAT (~65 deg), but it entered the FOV at T0+250 s to
exit again at T0 + 2200 s.

The data from the Fermi LAT in such time interval show a significant
increase in the event rate within 10 degree of the source location,
with a significance of more than 5 sigmas. This analysis has been
carried out with the P7SOURCE_V6 class. More than 5 photons above 100
MeV are observed within 2200 seconds. The highest energy photon is a
1.5 GeV event which is observed 260 seconds after the GBM trigger.

The Fermi LAT point of contact for this burst is Giacomo Vianello
(giacomov@stanford.edu).

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.


GRB_name: GRB130702A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14972
SUBJECT: GRB 130702A / Fermi394416326: Fermi GBM detection
DATE:    13/07/03 18:58:21 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU), V. Connaughton (UAH)
report on behalf of the Fermi GBM Team:

"At 00:05:23.08 UT on 2 July 2013, the Fermi Gamma-ray Burst
Monitor (GBM) triggered and located GRB 130702A (trigger 394416326 /
130702.004). The on-ground calculated location, using the Fermi GBM 
trigger data, is RA = 218.8, Dec = +12.25 (J2000 degrees, equivalent
to J2000 14h 35m, +12d 15'), with a statistical uncertainty of 4.0
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 75
degrees.

The GBM trigger is possibly associated with an optical transient
reported by Singer et al. (GCN 14697) and Guidorzi et al. (GCN 14698).
This event was also detected above 100 MeV by the Fermi LAT 
(Cheung et al., GCN 14971).

The GBM light curve shows a FRED-like burst with a duration (T90)
of about 59 s (50-300 keV). The burst has a 1.024-s peak flux of
7.03 +/- 0.86 ph/s-cm^2. The time-averaged spectrum from 
T0+0.003 to T0+16.384 s is well fit by power-law function with 
alpha = -1.65 +/- 0.02. The fluence (10-1000 keV) in this time 
interval is (6.3 +/- 2.0)E-06 erg/cm^2.

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


GRB_name: GRB130702A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14973
SUBJECT: Fermi GRB 130702A: Swift XRT and UVOT observations
DATE:    13/07/03 19:01:40 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

P. D'Avanzo (INAF-OAB), B. Porterfield, D. N. Burrows, M. Siegel  
(PSU), A. Melandri (INAF-OAB), P. A. Evans (Univ. Leicester) report on  
behalf of the Swift team:

The Fermi GBM and LAT instruments detected GRB 130702A at 00:05:23 UT  
on July 2, 2013 (Fermi trigger 394416326; Cheung et al. 2013, GCN Circ  
14971). Followup by the Palomar Transient Factory (PTF) located a  
possible optical counterpart, iPTF13bxl (Singer et al. 2013, GCN Circ.  
14967).  A subsequent TOO observation by Swift located a coincident X- 
ray counterpart, making this a likely counterpart of GRB 130702A  
(Singer et al. 2013, GCN Circ 14971). Here we report the results of  
the analysis of Swift XRT and UVOT data for this object.

We have analysed 3.4 ks of XRT data for this object,  from 89.1 ks to  
95.7 ks after the Fermi/GBM trigger.  The data are entirely in Photon  
Counting (PC) mode.  Using 3411 s of PC mode data and 5 UVOT images,  
we find an enhanced XRT position (using the XRT-UVOT alignment and  
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =  
217.31166, +15.77388 which is equivalent to:

RA (J2000): 14h 29m 14.80s
Dec(J2000): +15d 46' 26.0"

with an uncertainty of 1.5 arcsec (radius, 90% confidence). This  
position is consistent with the optical counterpart reported by Singer  
et al. 2013 (GCN Circ. 14967; see also Guidorzi et al. 2013, GCN Circ.  
14968).

The light curve displays variability consistent with a fading  
behaviour. More observations are scheduled to confirm whether the  
source is fading.

A spectrum formed from the PC mode data can be fitted with an absorbed  
power-law with a photon spectral index of 1.99 (+/-0.16). The best- 
fitting absorption column is  6.3 (+3.4, -3.1) x 10^20 cm^-2, in  
excess of the Galactic value of 1.7 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 3.6 x 10^-11 (4.2 x 10^-11) erg  
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:      6.3 (+3.4, -3.1) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: 2.4 sigma
Photon index:      1.99 (+/-0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00032876.


The Swift/UVOT began settled observations of the field of GRB 130702A  
89111 s after the GBM detection.  A source consistent with the P48  
position (Singer et al. 2013, GCN Circ. 14967) is detected in the  
initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  14:29:14.77 = 217.31155 (deg.)
    Dec (J2000) = +15:46:26.5  =  15.77403 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections using the UVOT photometric system (Breeveld et  
al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

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

white            89232        95967          3414         18.26 +/- 0.04

The magnitudes in the table are not corrected for the Galactic  
extinction due to the reddening of E(B V) = 0.04 in the direction of  
the burst (Schlegel et al. 1998).


This circular is an official product of the Swift team.


GRB_name: GRB130702A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14974
SUBJECT: IPN localization of GRB 130702A (= Fermi 394416326)
DATE:    13/07/03 19:03:54 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

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

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

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, report:

MESSENGER (GRNS), INTEGRAL (SPI-ACS), Fermi-GBM, and Konus-Wind have detected
GRB 130702A (= Fermi 394416326) so far.  We have triangulated this burst to an
annulus centered at RA, Dec (2000) = 293.0106 degrees, -18.3126 degrees,
whose radius is 82.0991 +/- 0.4594 degrees (3 sigma).  The distance
between the annulus center line and the iPTF optical transient reported
by Singer et al. (GCN 14967) is 0.16 degrees, strengthening the association
of the transient with the GRB.  A map has been posted at 
ssl.berkeley.edu/ipn3/130702 showing the annulus, the Fermi LAT position
(GCN 14971), and the optical transient.  This localization may be
improved.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14975
SUBJECT: GRB 130702A / Fermi394416326 : Nanshan optical observations
DATE:    13/07/03 19:20:27 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), A. Esamdin, L. Ma, X. Zhang (XAO) report:

We observed the field of GRB 130702A / Fermi394416326 (Singer et al.,
GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) using
the 1m telescope located at Mt. Nanshan, Xinjiang Astronomical
Observatory, China. We obtained 3x600s R-band frames, starting from
17:43:25 UT on 2013-07-03 (i.e., 1.735 days after the Fermi trigger).

The optical transient reported in Singer et al. (GCN 14967) is clearly
detected in each of the frames. However, it is slightly overlapped
with its nearby bright galaxy, SDSS J142914.57+154619.3, due to seeing
and technical constraints. The transient has decayed to R~18.9,
calibrated with two bright SDSS stars converted to Johnson R. The
continuous decay makes it likely the optical counterpart of GRB
130702A / Fermi394416326.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14976
SUBJECT: GRB 130702A / Fermi394416326 : Nanshan optical observations
DATE:    13/07/03 19:20:38 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), A. Esamdin, L. Ma, X. Zhang (XAO) report:

We observed the field of GRB 130702A / Fermi394416326 (Singer et al.,
GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) using
the 1m telescope located at Mt. Nanshan, Xinjiang Astronomical
Observatory, China. We obtained 3x600s R-band frames, starting from
17:43:25 UT on 2013-07-03 (i.e., 1.735 days after the Fermi trigger).

The optical transient reported in Singer et al. (GCN 14967) is clearly
detected in each of the frames. However, it is slightly overlapped
with its nearby bright galaxy, SDSS J142914.57+154619.3, due to seeing
and technical constraints. The transient has decayed to R~18.9,
calibrated with two bright SDSS stars converted to Johnson R. The
continuous decay makes it likely the optical counterpart of GRB
130702A / Fermi394416326.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14977
SUBJECT: GRB 130702A: TNG optical observations
DATE:    13/07/04 00:29:16 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), G. Andreuzzi, G. Mainella (INAF/FGG)
, report on behalf of the CIBO collaboration:

We observed the optical counterpart of the Fermi GRB 130702A (Cheung et
al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG
telescope located in Canary Islands, equipped with the DOLoRes imager.
Observations were carried out starting on 2013 Jul 3.955 UT (1.95 days
after the Fermi/GBM trigger).
In a single 300 seconds exposures obtained in the SDSS r band we clearly
detect the optical afterglow reported by Singer et al. (GCN 14697) with a
magnitude of r=19.1 (calibrated against nearby SDSS stars). Further
observations are ongoing.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14978
SUBJECT: GRB 130702A: NOT optical observations
DATE:    13/07/04 01:08:19 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MCSS), D. Xu (DARK/NBI), D. A. Kann (TLS Tautenburg), D. Malesani (DARK/NBI), S. Geier (NOT, DARK/NBI), P. Jakobsson (U. Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with 2.5m the Nordic Opitcal Telescope (NOT) equipped with ALFOSC. We obtained 1 x 120 s each in the r' and i' bands. Observations started at 23:36:59 UT on July 03 (i.e., 47.53 hrs after the burst).

The source reported in Singer et al. (GCN 14967) is clearly detected in both images. It has an r'-band magnitude of 19.13 +/- 0.01 mag  and an i' band magnitude of 18.82 +/- 0.01 mag (AB magnitude). The mid-exposure times are 47.5432 and 47.5900 hrs after trigger in r' and i',. The source faded by ~0.4 mag with respect to Singer et al. (GCN 14967). We create a light curve using the Rc/r' data of of Singer et al. (GCN 14967), Guidorzi et al. (GCN 14968) and Xu et al. (GCN 14975), and find a slope of alpha = 0.58, in agreement with that of Singer et al. Compared to all known GRB afterglows, the afterglow of GRB 130702A is among the brightest, of similar brightness as that of GRB130427A at the time of our observation (Xu et al. 2013, arXiv:1305.6832).

Calibration was done against SDSS J142915.86+154510.0 and SDSS J142911.60+154535.1 from SDSS DR9. We did not correct for Galactic foreground extinction.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14979
SUBJECT: GRB 130702A: CARMA 3mm detection
DATE:    13/07/04 06:15:19 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and M. Kasliwal (Carnegie) report on behalf of a 
larger collaboration:

We observed the location of the probable optical counterpart of Fermi 
GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; 
Collazzi & Connaughton, GCN 14972) with the Combined Array for Research 
in Millimeter Astronomy (CARMA) on 2013-07-04 between 00:28:21 and 
05:56:31 UT, 2.01-2.24 days after the GBM trigger, at a frequency of 93 
GHz (3 mm).  Weather conditions were poor initially but improved 
somewhat over the course of the integration.   In a preliminary 
reduction of the data we detect a millimeter source coincident with the 
location of the optical counterpart with a flux of approximately ~2 mJy.

We thank John Carpenter and the CARMA staff for their support.


GRB_name: GRB130702A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14980
SUBJECT: GRB 130702A: RATIR Optical and NIR Observations
DATE:    13/07/04 07:13:58 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et
al., GCN 14971; Collazzi & Connaughton, GCN 14972) with the Reionization
and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio Astronmico Nacional on Sierra San
Pedro Mrtir from 2013/07 4.16 to 2013/07 4.25 UTC (51.79 to 53.82 hours
after the BAT trigger), obtaining a total of 1.42 hours exposure in the r'
and i' bands and 0.60 hours exposure in the Z, Y, J, and H bands.

At the position of the source from Singer et al. (GCN 14967), in comparison
with SDSS DR9 and 2MASS, we obtain the following detections:

  r'    19.22 +/- 0.01
  i'    19.06 +/- 0.02
  Z    18.85 +/- 0.03
  Y    18.70 +/- 0.03
  J     18.72 +/- 0.03
  H    18.56 +/- 0.03

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  Further observations are underway.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130702A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14981
SUBJECT: GRB 130702A: Continued P60 observations
DATE:    13/07/04 08:05:48 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley, L. P. Singer (Caltech), and S. B. Cenko (GSFC) report:

We obtained additional observations of the location of the probable 
afterglow of GRB 130702A with the Palomar 60-inch robotic telescope.  A 
series of repeated imaging sequences were taken in B, g, r, i, and z 
filters during intermittent clouds.  Example photometry from one 
sequence is as follows:

  tstart(d)  exp(s) filt mag        unc
  2.20405    120     i = 19.129 +/- 0.05
  2.20565    120     r = 19.297 +/- 0.05
  2.20728    120     B = 19.635 +/- 0.07
  2.20888    120     z = 19.204 +/- 0.16
  2.21048    120     g = 19.519 +/- 0.08

Compared to our previous night's P60 observations (Singer et al., GCN 
14967) and referenced to the GBM trigger time (Collazzi et al., GCN 
14972), the fading is consistent with a power law with decay index of 
approximately alpha=1.1, steeper than that inferred during the first 24 
hours.


GRB_name: GRB130702A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14982
SUBJECT: GRB 130702A: further Swift-XRT observations
DATE:    13/07/04 09:31:33 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), P. A. Evans (Univ Leicester) report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for the Fermi GRB 130702A (Cheung et al. GCN 14971; Collazzi et al. GCN 14972), from 89.1 ks to 153.4 ks after the Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode. We confirm the fading of the X-ray afterglow reported in D'Avanzo et al. (GCN 14973).

The light curve can be modelled with a power-law decay with a decay index of alpha=0.57 (+0.21, -0.20). 


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


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14983
SUBJECT: GRB 130702A: NOT spectroscopy and redshift of the nearby bright galaxy
DATE:    13/07/04 13:10:00 GMT
FROM:    Giorgos Leloudas at Dark Cosmology Centre  <giorgos@dark-cosmology.dk>

G. Leloudas (OKC, Stockholm and DARK/NBI), J. P. U.  Fynbo (DARK/NBI), S. Schulze (PUC, MCSS), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Geier (NOT, DARK/NBI), Z. Cano(U. Iceland), P. Jakobsson (U. Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with the Nordic Opitcal Telescope (NOT) equipped with ALFOSC. In addition to our photometric observations (reported in Schulze et al., GCN 14978), we obtained an optical spectrum, with a total exposure of 2 x 1800 s, using Grism #4 and covering the wavelength range 3750 - 9000 AA at a resolution of 17 AA.

The slit was oriented to cover both the transient source (also dubbed iPTF13bxl) that has been suggested to be the afterglow of GRB 130702A, and the bright SDSS galaxy located 7.6" South of the source (SDSS J142914.57+154619.3; Singer et al., GCN 14967). 

The galaxy is found to be at z = 0.145, based on Ca II H & K absorption and emission by [OII] and Halpha. The emission features are weak and we do not detect Hbeta or [OIII]. Overall, and combined with the SDSS colors, this galaxy shows very weak star formation activity. 

This redshift is consistent with the redshift of the transient source reported by Mulchaey et al. (ATel 5191) and the description given there. The trace of our NOT spectrum at the location of the transient is mostly featureless and we cannot detect the emission lines reported by Mulchaey et al., probably due to a lower S/N.

The common redshift suggests that the transient source iPTF13bxl is associated with the galaxy SDSS J142914.57+154619.3. If this transient is indeed the afterglow of GRB 130702A at z = 0.145, it implies an E_iso = (3.0 +- 1.0) * 10^50 erg in the 10-1000 keV (Collazzi et al., GCN 14972).

We note that this is an unusual environment for a long GRB: located at a large offset (19.1 kpc in projection) from a relatively passive galaxy. However, we cannot exclude that more sources in the field, including the fainter (r ~ 23 mag) object at 0.6" from the transient (SDSS J142914.75+154626.0; Singer et al., GCN 14967) might be at the same redshift. A possible confirmation of the GRB nature of this transient will be the emergence of an associated supernova. At z = 0.145, a supernova similar to SN 1998bw will peak at R ~ 19.8 mag about 20 days after the GRB, and will be easily detectable. 


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14984
SUBJECT: GRB 130702A: further TNG observations
DATE:    13/07/04 15:44:22 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASI/ASDC), G. Tagliaferri, A. Melandri (INAF-OAB), D. Malesani (DARK/NBI), M. Della Valle (INAF-OAC), E. Pian (SNS) report on behalf of the CIBO collaboration:

We observed the optical counterpart of the Fermi GRB 130702A (Cheung et al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG telescope located in Canary Islands, equipped with the DOLoRes imager.

In addition to what reported in D'Avanzo et al. (GCN 14977), further observations were carried out between Jul 3.955 UT and Jul 4.022 UT (1.95-2.02 days after the Fermi GBM trigger).

The optical afterglow is clearly detected in the SDSS g, r, and i bands with the following magnitudes:

g=19.3
r=19.1
i=19.0

calibrated against nearby SDSS stars.

We also obtained a 2400 seconds spectrum with the LR-B grism, covering the wavelength range 3900-8200 AA with a resolution of R~600. The spectrum has a high S/N and shows a blue continuum nearly featureless. Very faint emission lines can be interpreted as [OII] 3727.5, [OIII] 4959.0/5006.8 and Halpha 6562.8 at a common redshift of 0.145, consistent with what reported by Mulchaey et al. (ATel 5191) for the optical afterglow spectrum and by Leloudas et al. (GCN circ. 14983) for the spectrum of the nearby SDSS galaxy.


We acknowledge the TNG staff for excellent support, in particular G. Andreuzzi and G. Mainella.


GRB_name: GRB130702A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14985
SUBJECT: GRB130702A: Redshift of Afterglow Candidate iPTF13bxl
DATE:    13/07/04 16:09:08 GMT
FROM:    Mansi M. Kasliwal at Caltech/Carnegie  <mansikasliwal@gmail.com>

J. Mulchaey (Carnegie), M. M. Kasliwal (Carnegie), I. Arcavi
(Weizmann), E. Bellm (Caltech) and D. Kelson (Carnegie) report on
behalf of a larger collaboration:

We obtained a high SNR low-resolution spectrum of iPTF13bxl
(GCN#14967) with IMACS on the 6.5m Magellan telescope at Las Campanas
on 2013 July 3.97 covering 3800A-9500A.  We also obtained another
spectrum with the DBSP spectrograph on the 5m Hale telescope at
Palomar at July 4.16. The spectra show a blue continuum with weak
H-alpha and O III emission at z=0.145.


GRB_name: GRB130702A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14986
SUBJECT: Konus-Wind observation of GRB 130702A
DATE:    13/07/04 17:49:17 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long GRB 130702A (= Fermi 394416326; Optical and X-ray transient 
discovery:  Singer et al., GCN 14967; Fermi-LAT detection: Cheung et 
al., GCN 14971; Fermi GBM detection: Collazzi & Connaughton, GCN 14972; 
IPN localization: Huley et al., GCN 14974) was detected by Konus-Wind in 
the waiting mode.

The burst light curve shows a FRED-like pulse with a duration of ~26 s.

As observed by Konus-Wind, the burst had a fluence of
6.70(-0.80,+0.82)10^-6 erg/cm2 (in the 20 - 1200 keV energy range).

Fitting the K-W 3-channel time-integrated spectrum (from T0(GBM)-2.8 s
to T0(GBM)+23.7 s) by a simple power-law model yields a power law index 
of 1.87 +/- 0.11.

Assuming z = 0.145 (Kasliwal et al., GCN 14985; Leloudas et al. GCN
14983) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M =
0.27, Omega_Lambda = 0.73, the isotropic energy release is E_iso =
6.36(-1.03,+1.34)x10^50 erg in 1 keV to 10 MeV at the GRB rest frame
extrapolating the best power-law function fit.

All the quoted errors are at the 90% confidence level.
The results presented above are preliminary.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB130702A/


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14987
SUBJECT: GRB 130702A: WSRT radio detection
DATE:    13/07/05 09:35:55 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (University of Amsterdam) reports on behalf
of a large collaboration:

"We observed the position of the GRB 130702 afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at July 4 13.55 UT to
July 5 01.17 UT, i.e. 2.56 - 3.05 days after the burst (GCN 14972).
We detect a radio source with a flux density of 1.23 +/- 0.04 mJy
at the position of the optical counterpart (GCN 14967).

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


GRB_name: GRB130702A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14989
SUBJECT: GRB 130702A (= Fermi 394416326): correction of the GCN #14988 title
DATE:    13/07/05 15:08:22 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI) report on behalf larger GRB follow-up collaboration:

A title of GCN circular #14988 should be read as "GRB 130702A (= Fermi 
394416326): Maidanak optical observations"

We apologize for possible inconvenience.


GRB_name: GRB130702A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14990
SUBJECT: GRB 130702A: VLA detection
DATE:    13/07/05 20:23:22 GMT
FROM:    Alessandra Corsi at GWU  <corsi@email.gwu.edu>

A. Corsi (GWU), D. A. Perley (Caltech), and S. B. Cenko (GSFC) report:
 
We observed the location of iPTF13bxl, the optical counterpart to
GRB 130702A (Singer et al., GCN 14967), with the Karl G. Jansky Very
Large Array in C-band on 2013-07-04 UT, 2.29 days after the GBM trigger. 
We detect a radio source at this location with a flux of 1.49 mJy at 5.1 GHz, 
and 1.60 mJy at 7.1 GHz. The map noise is 0.011 mJy.


GRB_name: GRB130702A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14991
SUBJECT: GRB 130702A: Continued UVOT Observations
DATE:    13/07/05 23:04:12 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

GRB 130702A: Continued UVOT Observations

B. Porterfield (PSU), M. Siegel (PSU) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:

Swift reobserved the field of GRB 130702A on July 4 and July 5 2013. 
We confirm the slow fading of the source first reported by Singer et al. (GCN Circ. 
14973) and previously reported in UVOT by D'Avanzo et al. (GCN Circ. 14973).
We also note that we detect the transient in all four of UVOT's NUV filters,
which is consistent with the low redshift reported by Leloudas et al. (GCN Circ. 14983)
and D'Avanzo et al. (GCN Circ. 14984).

Preliminary detections using the UVOT photometric system (Breeveld et  
al. 2011, AIP Conf. Proc. 1358, 373) are:

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

u            151366       153361       1962      18.48+-0.05
u            203252       205246       1962      18.97+/-0.07
u            250292       255654       272       19.51+/-0.26
uvw1         249967       255532       629       19.29+/-0.17
uvm2         251591       252014       415       19.67+/-0.28
uvw2         284670       285309       629       19.26+/-0.14

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14992
SUBJECT: GRB 130702A: Xinglong TNT optical observation
DATE:    13/07/07 14:51:36 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, J. Y. Wei, Y.L. Qiu, J. Wang, J.S. Deng,  
C. Wu, X. H. Han on behalf of EAFON report:

We began to observe the optical counterpart of the Fermi GRB 130702A 
( Singer et al. GCN 14967; Collazzi et al. GCN 14972 ) 
with Xinglong TNT telescope between 14:10:35  and 15:37:22 UT 
on 5 June, 2013.  15*300 sec  R-band images were obtained. 
The optical counterpart was found with a magnitude of  R~19.7 mag, 
calibrated by USNO-B 1.0 R2 mag, at the mean time of 3.62 days after the burst.


GRB_name: GRB130702A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14993
SUBJECT: GRB 130702A: Continued RATIR Optical and NIR Observations
DATE:    13/07/07 16:21:05 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et
al., GCN 14971; Collazzi & Connaughton, GCN 14972) with the Reionization
and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio Astronmico Nacional on Sierra San
Pedro Mrtir on the nights of 2013/07/06 and 2013/07/07 (4.25 and 5.26 days
after the BAT trigger), obtaining a total of 1.4 hours exposure in the r'
and i' bands and 0.6 hours exposure in the Z, Y, J, and H bands each night.

At the position of the source from Singer et al. (GCN 14967), in comparison
with SDSS DR9 and 2MASS, we obtain the following detections:

          7/06                        7/07
 r'   19.86 +/- 0.02   19.94 +/- 0.02
 i'   19.89 +/- 0.03   20.02 +/- 0.02
 Z   19.68 +/- 0.05   19.76 +/- 0.04
 Y   19.46 +/- 0.05   19.69 +/- 0.05
 J   19.64 +/- 0.07   19.64 +/- 0.06
 H   19.36 +/- 0.08   19.69 +/- 0.08

The source appears to be slowly fading, approximately 0.1 mag/day, or
approximately as t^-0.35.  This is a significant flattening relative to the
bright fluxes we measured 2 days after the GRB (Butler et al.; GCN 14980).
 These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  Further observations are underway.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14994
SUBJECT: GRB130702A: NOT observation - the detection of an emerging supernova
DATE:    13/07/08 04:31:28 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MCSS), G. Leloudas (OKC, Stockholm and DARK/NBI), D. Xu, J. P. U. Fynbo (DARK/NBI), S. Geier (NOT, DARK/NBI) and P. Jakobsson (U Iceland) report on behalf a larger collaboration:

We observed the field of GRB 130702A (Singer et al., GCN 14967; Cheung et al., GCN 14971; Collazzi et al., GCN 14972) with the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC. We obtained 1 x 150 s in r' and 5 x 60 in i'. Observations started at 23:23:10 UT on July 07 (i.e. 5.97 days after the burst).

We measure r' = 20.03 and i' = 20.21 mag. The afterglow became clearly brighter in r'-band with respect to our observation from the night before. Compared to our first observation on 3 July (Schulze et al. GCN 14978), the colour changed from 0.13 to -0.19 mag. This colour evolution is consistent with Butler et al. (GCN 14993), who reported a colour change of -0.08 mag between 4.25 and 5.26 days after the burst. Such a colour evolution is not expected for a decaying optical afterglow but clearly points to an emerging supernova.

We obtained an optical low-resolution spectrum with the ALFOSC camera starting at 23:45:33 UT. We used grism #4 that covers the wavelength range from 3750 to 9000 AA.  The observation consisted of three individual spectra with a total exposure time of 3x1200 s. The flux-calibrated spectrum presents clear deviations from a power law. In particular, we identify two broad emission features peaking at 4900 and 5600 AA with a local minimum at 5200 AA (all observer frame). Assuming z=0.145 (Mulcaey et al. ATel 5191, GCN 14985; Leloudas et al. GCN 14983; D'Avanzo et al. GCN 14984), the spectrum resembles SN 1998bw at phase 7-8 days past explosion (Patat et al. 2001, ApJ, 555, 900).


GRB_name: GRB130628A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14995
SUBJECT: GRB 130628A: Suzaku WAM observation of the prompt emission
DATE:    13/07/08 11:25:03 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y. Ishida, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno,
S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano,
R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.),  S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA),
W. Iwakiri (RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:


The short GRB 130628A (Byrne et al. GCN 14969) was detected by the the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 12:44:04.634 UT (=T0). The observed light curve shows
a single peak with a duration (T90) of about 2.4 seconds. The fluence in
100 - 1000 keV was 3.70 (+0.65/-0.71) x 10^-6 erg/cm2. The 1-s peak flux
measured from T0+2 s was 2.93 (+0.54/-0.71) photons/cm2/s in the same
energy range.

Preliminary result shows that the time-averaged spectrum from T0-5 s to
T0+5 s is well fitted by a single power-law with a photon index of 2.11
(+0.41/-0.31) (chi2/d.o.f = 20.3/15).

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: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14996
SUBJECT: GRB 130702A: Maidanak optical observations
DATE:    13/07/09 10:46:20 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI), O. Burhonov (UBAI), I. Molotov (KIAM) 
report on behalf of larger GRB follow-up collaboration:

We continue observations of the afterglow  (Singer et al., GCN 14967) of GRB 
130702A  (Cheung  et al., GCN 14971; Collazzi  et al., GCN  14972) with 
AZT-22 telescope of Maidanak observatory.  A preliminary photometry of 
combined images is based on two SDSS stars suggested by Schulze et al. (GCN 
14978) and used in our previous observations (Pozanenko et al, GCN 14988)

T_start                     T0+       Filter, Exposure, OT
(UT)                          (mid, d)            (s)

2013-07-05T16:25:11  3.6592    R       6x600     19.61+/-0.02
2013-07-06T16:20:12  4.6540    R       6x600     19.71+/-0.03
2013-07-07T16:45:34  5.6717    R       6x600     19.83+/-0.04
2013-07-08T16:49:14  6.6759    R       6x300     19.81+/-0.05


The light curve is based on the photometry of this CGN circular and our 
previous observations (Pozanenko et al, GCN 14988)  and can be found at 
http://grb.rssi.ru/GRB130702A/GRB130702A_MAO_R_lc.png

One can see flattening of the lc after 4 days (initially reported by Butler 
et al., GCN 14993)  and possible re-brightening on 6.6 days which can 
confirm re-brightening of the afterglow (Schulze et al., GCN 14994) and 
emerging supernova. 


GRB_name: GRB130708A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14997
SUBJECT: GRB 130708A found in ground analysis of Swift-BAT data
DATE:    13/07/09 14:57:45 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift-BAT team

At 11:43:03.7 Swift-BAT triggered on GRB 130708A (trigger 560515). No
significant source was found onboard, and rate-trigger processing was
terminated prematurely by a pre-planned slew. A significant source was found
in ground analysis at RA, Dec 17.474, 0.003, which is:

RA (J2000)   01h 09m 53.7s
Dec (J2000)  00d 00' 11.9"

with an estimated 90% error radius of 2.4 arcmin.  This position is 5.0 degrees
from the location found by Fermi-GBM for trigger 394976587, which has an
estimated error of 2.2 degrees.  The partial coding was 11%.

We note that this position is 1.6 arcmin from a Seyfert I galaxy at Z = 0.16,
[VV2003c] J010946.5-000023.

The BAT lightcurve shows a double-peaked long GRB.  The T90 of the GRB was about
9 +/- 1 seconds, with a spectral power-law index of 1.38 +/- 0.28 and a fluence
of (7.8 +/- 1.8) x 10^-6 ergs/cm^2 in the 15-150 keV BAT energy range.  Error
estimates are 90% confidence.

A Swift TOO request has been approved to locate the afterglow with XRT.  Since
this burst was not located onboard, the usual automated analysis products are
not available.


GRB_name: GRB130702A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14998
SUBJECT: GRB 130702A: P200 Spectroscopic Confirmation of Associated Supernova
DATE:    13/07/10 00:28:32 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC), A. Gal-Yam (Weizmann Institute), M. M. Kasliwal
(OCIW), D. Stern (JPL), K. Markey, E. Alduena, A. Alduena, and S. Kuo
(Walden) report on behalf of a larger collaboration:

We have obtained further spectroscopy of the optical afterglow (Singer et
al., GCN 14967) of the Fermi-GBM (Collazzi et al., GCN 14972), Fermi-LAT
(Cheung et al., GCN 14971), and IPN (Hurley et al., GCN 14974) GRB
130702A.  Observations were obtained with the Double Spectrograph mounted
on the 5 m Palomar Hale telescope beginning at 5:27 UT on 2013 July 8 (6.2
days after the Fermi GBM trigger) and cover the wavelength range from
3400-8900 A.  Compared with our previous optical spectra (Mulchaey et al.,
GCN 14985), the source shows a significantly redder continuum.  Similar to
Schulze et al. (GCN 14994), a number of broad features are detected that
are reminiscent of canonical GRB-associated supernovae such as SN 2006aj
and SN 1998bw.  A plot of our most recent spectrum, alongside comparable
epochs from SN 2006aj (Modjaz et al., ApJL, 2006, 645, 21) and SN 1998bw
(Patat et al., ApJ, 2001, 555, 900), both retrieved from the Weizmann
Interactive Supernova Data Repository (WISEREP;
http://www.weizmann.ac.il/astrophysics/wiserep/) is available here:

http://astro.berkeley.edu/~cenko/public/grb/GRB130702A/GRB130702A_20130708.png


GRB_name: GRB130708A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14999
SUBJECT: GRB 130708A: Fermi GBM observation
DATE:    13/07/10 11:23:35 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) reports on behalf of the Fermi GBM Team:

At 11:43:04.27 UT on 08 July 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130708A (trigger 394976587/130708488)
which was also detected by the Swift/BAT (Cummings et al., GCN Circ. 14997).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of a single peak
with a duration (T90) of about 14 s (50-300 keV).
The time-averaged spectrum from T0 s to T0 + 8 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.9 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 158 +/- 16 keV

The event fluence (10-1000 keV) in this time interval is
(2.3 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.8 s in the 10-1000 keV band is 1.0 +/- 0.07 ph/s/cm^2.

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


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15000
SUBJECT: GRB 130702A: TNG spectroscopic observations of the emerging supernova
DATE:    13/07/10 13:35:24 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASI/ASDC, INAF-OAR), P. D'Avanzo (INAF-OAB), D. Fugazza (INAF-OAB), A. Melandri (INAF-OAB), M. Della Valle (INAF-OAC), G. Tagliaferri (INAF-OAB), D. Malesani (DARK/NBI), E. Pian (SNS), L. A. Antonelli, S. Piranomonte (INAF-OAR), A. Harutyunyan, D. Carosati (INAF/TNG) report on behalf of the CIBO collaboration:

We continued monitoring the optical counterpart of the Fermi GRB 130702A (Singer et al., GCN 14967, Cheung et al. GCN 14971; Collazzi et al. GCN 14972) with the Italian 3.6m TNG telescope located in the Canary Islands, equipped with the DOLoRes camera.

In addition to what reported in D'Avanzo et al. (GCN 14977, GCN 14984), further observations were carried out during the nights of Jul 5 and Jul 9 (4 and 8 days after the Fermi GBM trigger).

At a mean t-t0=7.92 days we detect the optical counterpart in the SDSS r band with a magnitude of 19.91 (calibrated against nearby SDSS stars). This value is consistent with our previous epoch obtained 4 days before, confirming the flattening of the optical light curve reported by (Perley et al. GCN 14981, Butler et al. GCN 14993, Schulze et al. GCN 14994, Pozanenko et al. GCN 14996).

We also obtained a 2000 seconds spectrum with the LR-B grism, starting at t-t0=7.92 days, covering the wavelength range 3900-8200 AA with a resolution of R~600. With respect to our previous epoch  observation which featured a blue, featureless continuum (D'Avanzo et al. GCN 14984), the spectrum is now considerably redder, and shows a number of broad features similar to GRB-associated supernovae. In particular, the shape of the continuum closely resembles the spectrum of SN 1998bw observed at a similar epoch, despite a prominent feature at 4300 AA rest frame, reminiscent of what seen in SN 2006aj (Pian et al. 2006, Nature, 442, 1011). This confirms the emerging of the supernova already reported by Schulze et al. (GCN 14994) and Cenko et al. (GCN 14998).

We acknowledge support from the TNG visiting astronomer K. Biazzo.

[GCN OPS NOTE(10jul13):  Per author's request, DF was added to the author list.]


GRB_name: GRB130708A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15001
SUBJECT: GRB 130708A: Swift XRT and UVOT Observations
DATE:    13/07/10 20:07:37 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASF Palermo) and A. Breeveld (MSSL-UCL) report on behalf of the Swift XRT and UVOT teams:

The Swift/XRT started observing the field of the BAT ground-detected GRB 130708A (Cummings, GCN Circ. 14997) on 2013-07-09 at 14:49:07 UT, 97564 s after the BAT trigger. In 3881 s of XRT data in Photon Counting mode we detected no significant X-ray source within the BAT error circle. The 3-sigma upper limit at the reported BAT position is 4.0E-03 cts/s.

The Swift/UVOT began settled observations of the field of GRB 130708A 97557 s after the BAT trigger. No optical afterglow consistent with the BAT position is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

white            97741       107968         1001         >21.6
v                97926       103874         1037         >20.1
u                97557       107909         1804         >21.4

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.03 in the direction of the burst (Schlegel et al. 1998).

This circular is an official product of the Swift XRT and UVOT teams.


GRB_name: GRB130702A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15002
SUBJECT: GMRT radio detection of GRB 130702A
DATE:    13/07/11 10:30:07 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

Poonam Chandra (NCRA-TIFR) reports:

We carried out Giant Metrewave Radio Telescope (GMRT) observations of
GRB 130702A at 1390 and 610 MHz bands on 2013 July 10.54 UT and 10.72 UT,
respectively. We detect the radio afterglow of the GRB in both bands.
The 1390 MHz band flux density of the afterglow is 792+/-44 uJy and 610 MHz
flux density of the afterglow is 457+/-75 uJy. The map resolutions at 1390
and 610 MHz bands are 2.67"x2.26" and  8.91"x5.50", respectively.
  
Further observations are planned. We thank GMRT staff for making these
observations possible.

-- 

**********************************************************************
Poonam Chandra                          Phone: +91 20 2571 9290
Tata Institute of Fundamental Research  Email: poonam@ncra.tifr.res.in
National Center for Radio Astrophysics  Home: ncra.tifr.res.in/~poonam
Post Bag 3, Pune University campus
Ganeshkhind, Pune 411 008, INDIA


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15003
SUBJECT: GRB 130702A: Maidanak optical observations
DATE:    13/07/11 16:11:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI), O. Burhonov (UBAI), I. Molotov 
(KIAM) report on behalf of larger GRB follow-up collaboration:

We continue observations of the afterglow  (Singer et al., GCN 14967) of 
GRB 130702A  (Cheung  et al., GCN 14971; Collazzi  et al., GCN  14972) 
with AZT-22 telescope of Maidanak observatory.  A preliminary photometry 
of combined images is based on two SDSS stars suggested by Schulze et 
al. (GCN 14978) and used in our previous observations (Pozanenko et al, 
GCNs 14988, 14996)

T_start              T0+       Filter, Exposure, OT
(UT)                 (mid, d)            (s)

2013-07-09T16:50:52  7.6771    R       7x600     19.73+/-0.04
2013-07-10T17:18:05  8.6931    R       6x600     19.64+/-0.03


The light curve can be found at 
http://grb.rssi.ru/GRB130702A/GRB130702A_MAO_R_lc.png

It is clearly visible in the lc a rising SN (Schulze et al., GCN 14994; 
Cenko et al., GCN 1998; D'Elia et al., GCN 15000).


GRB_name: GRB130626A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15004
SUBJECT: GRB 130626A: Retraction of possible X-ray afterglow 
DATE:    13/07/12 13:59:31 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and M. De Pasquale (UCL-MSSL) report on behalf of
the Swift-XRT team:

In GCN Circ. 14937, Page, Oates & De Pasquale reported the Swift detection
of a weak X-ray source within the BAT error circle of GRB 130626A.
Follow-up observations of this source, obtained between 5.8 x 10^5 and 1.3
x 10^6 s after the trigger, show it is still detected, at a level of (1.3
+/- 0.3) x 10^-3 count s^-1, compared to the initial detection of (2.0
+0.5/-0.4) x 10^-3 count s^-1 (errors at the 1-sigma confidence level).
Since the source has not faded significantly over this long time span, we
do not believe it to be the X-ray afterglow of GRB 130626A.

The 90% upper limit for any other source within the BAT error circle is 8
x 10^-4 count s^-1, corresponding to a flux of 3 x 10^-14 erg cm^-2 s^-1,
assuming a typical counts-to-observed-flux conversion factor of 4 x 10^-11
erg cm^-2 count^-1.

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


GRB_name: GRB130715A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15005
SUBJECT: GRB 130715A: Fermi GBM detection 
DATE:    13/07/16 16:16:04 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU)
reports on behalf of the Fermi GBM Team:

"At 21:44:09.64 UT on 15 July 2013, the Fermi Gamma-ray Burst
Monitor (GBM) triggered and located GRB 130715A (trigger 
395617452 / 130715.906). The on-ground calculated location, using 
the Fermi GBM trigger data, is RA = 287.4, Dec = -31.1 (J2000 
degrees, equivalent to J2000 19h 9m, -31d 3'), with a statistical 
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 96 degrees.

The trigger occurred during a nadir pointing maneuver of
the Fermi spacecraft.

The GBM light curve shows single continuous emission with a 
duration (T90) of about 48 s (50-300 keV).  The peak flux during 
this interval is 7.75 +/- 0.31 ph/s/cm^2. The time-averaged 
spectrum from T0+0.00 to T0+61.44 s is best fit by a Band function
with Epeak = 314.60 +/- 12.40, alpha = -0.58 +/- 0.03, 
beta = -2.44 +/- 0.12. The fluence (10-1000 keV) in this time interval 
is (4.7 +/- 0.061)E-05 erg/cm^2.

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


GRB_name: GRB130716A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15006
SUBJECT: GRB 130716A: Probable short-hard burst with delayed Swift data
DATE:    13/07/16 23:32:36 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

During a TDRSS-275 outage between 10:25 and 10:59 UT this morning, Swift-BAT
triggered on GRB 130716A (trigger #561974).  Due to the TDRSS outage, prompt
data was not available.  Data has now been received.  The burst occurred at
10:36:53 UTC.
  
The BAT refined position is RA, Dec179.581,63.057, which is:
RA (J2000)   11h 58m 19.4s
Dec (J2000)  63d 03' 25"
with an estimated uncertainty radius of 2.5 arcmin (90% confidence).  The
partial coding was 63%.

The BAT lightcurve shows a double overlapping peak, the first peak smaller,
with a total duration of about 0.8 seconds.

The XRT began observing the field at 10:38:55 UT, 122 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 179.5770, 63.0529 which is equivalent to:
    RA(J2000)  = +11h 58m 18.5s
    Dec(J2000) = +63d 03' 10.6"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 15.7 arcseconds from the BAT onboard position, within the BAT
error circle.

UVOT data is not yet available.

Burst Advocate for this burst is Stefan Immler (stefan.immler 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: GRB130716A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15007
SUBJECT: GRB 130716A: UVOT Upper Limits
DATE:    13/07/17 02:01:03 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and S. Immler (GSFC) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130716A
120s after the BAT trigger (Cummings et al., GCN Circ. 15006).  No
optical afterglow consistent with the XRT position is detected in
the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter    T_start(s)   T_stop(s)    Exp(s)   Mag
white (fc)     120       270         147    >20.47 
white          888      1038         147    >20.90 
v             5858      6057         196    >19.17 
b             5242      5442         196    >20.01
u (fc)         334       583         245    >19.86
uvw1          4832      5032         196    >19.61
uvm2          4627      4827         196    >19.64
uvw2          5653      5853         196    >20.05

The magnitudes in the table 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: GRB130716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15008
SUBJECT: GRB 130716A: Gemini-North imaging
DATE:    13/07/17 07:43:57 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, E. Berger and R. Chornock (Harvard) report:

"We observed the field of the short-duration GRB 130716A (Cummings et al.,
GCN 15006) with the Gemini Multi-Object Spectrograph mounted on the Gemini
North 8-m telescope starting on Jul 17.253 UT (19.45 hr after the burst).
We obtained ~15 min of r-band observations in 1" seeing. Calibrated to
stars in the SDSS DR9 catalog, we do not detect any optical source within
the reported XRT position to a 5-sigma limit of r>24.5 mag.

We thank the Gemini staff for their assistance with these observations."


GRB_name: GRB130702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15009
SUBJECT: GRB 130702A : Xinglong TNT continue optical observation 
DATE:    13/07/18 09:16:10 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, J. Y. Wei, Y.L. Qiu, J. Wang, J.S. Deng,  
C. Wu, X. H. Han on behalf of EAFON report:
 
We continue to observe the optical counterpart of the Fermi GRB 130702A 
( Singer et al. GCN 14967; Collazzi et al. GCN 14972 ) 
with Xinglong TNT telescope at  13:42:16.031 UT on 16 July, 2013 
under a bad weather.  6*300 sec  R-band images were obtained. 
The brightness of the optical afterglow was found with a magnitude 
of  R~19.6 +/-0.2 mag,  calibrated by USNO-B 1.0 R2 mag of the two stars
 (Schulze et al. GCN 14978; Pozanenko et al. GCN 15003),  
at the mean time of 14.57 days after the burst.


GRB_name: GRB130716A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15010
SUBJECT: GRB 130716A Swift-BAT Spectral lag analysis
DATE:    13/07/18 15:11:29 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

J. Norris (BSU), S. D. Barthelmy (GSFC), T. Sakamoto (AGU), N. Gehrels (GSFC)

We report the spectral lag analysis for GRB 130716A (GCN Circ. 15506) based on 
the BAT data.  Using 16-ms binned light curve, the spectral lag for the 25-50 keV 
to 100-350 keV bands is -2 (+50/-40) ms, and +11 (+25/-14) ms for the 15-25 keV to 
50-100 keV bands.  Although the lag value is not well constrained (relatively large 
errors), we believe this burst is more consistent with short burst category.  There is 
no evidence for extended emission.  


GRB_name: GRB130716A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15011
SUBJECT: GRB 130716A: Fermi GBM observation
DATE:    13/07/18 16:39:42 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (UCD) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 10:36:53.59 UT on 16 July 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130716A (trigger 395663816 / 130716442)
which was also detected by the Swift/BAT
(Cummings et al. 2013, GCN 15006).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of two overlapping pulses
with a duration (T90) of about 0.8 s (50-300 keV).
The time-averaged spectrum from T0-0.256 s to T0+0.576 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.23 (+0.28/-0.24) and
the cutoff energy, parameterized as Epeak, is 635 (+184/-112)  keV.

The event fluence (10-1000 keV) in this time interval is
(9.2 +/- 0.7)E-07 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.256 s in the 10-1000 keV band
is 6.2 +/- 0.9 ph/s/cm^2.

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


GRB_name: GRB130719A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15012
SUBJECT: GRB 130719A: Swift detection of a burst
DATE:    13/07/19 06:07:14 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

F. E. Marshall (NASA/GSFC), J. R. Cummings (NASA/UMBC),
V. D'Elia (ASDC), C. Gronwall (PSU), P. T. O'Brien (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 05:47:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130719A (trigger=562625).  Swift could not slew to the burst
due to a Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 89.039, -11.585 which is 
   RA(J2000) = 05h 56m 09s
   Dec(J2000) = -11d 35' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve is dominated by
variation from Vela X-1, which is also in the FOV, so nothing
can be stated about the burst light curve for this image
trigger at this time. 

Due to the Sun constraint, XRT and UVOT will not be able to
observe the burst location until July 26. 

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: GRB130722A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15013
SUBJECT: GRB 130722A: Swift detection of a burst
DATE:    13/07/22 08:30:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/UMCP), V. D'Elia (ASDC),
C. J. Mountford (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 08:19:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130722A (trigger=563213).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 260.670, -2.979 which is 
   RA(J2000) = 17h 22m 41s
   Dec(J2000) = -02d 58' 44"
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 120 sec.  The peak count rate
was ~8500 counts/sec (15-350 keV), at ~72 sec after the trigger. 

The XRT began observing the field at 08:21:10.4 UT, 111.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 260.6530, -2.9728 which is equivalent to:
   RA(J2000)  = +17h 22m 36.72s
   Dec(J2000) = -02d 58' 22.1"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 65 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 8.65e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 120 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
0.63. 

Burst Advocate for this burst is E. Troja (eleonora.troja 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: GRB130715A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15014
SUBJECT: GRB 130715A: Suzaku WAM observation of the prompt emission
DATE:    13/07/22 08:37:22 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y. Ishida, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno,
S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano,
R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.),  S. Sugita (Ehime U.), Y. E. Nakagawa,
M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN),
Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:

The long GRB 130715A (Andrew et al GCN15005) was detected by the the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 21:44:38.377 UT (=T0).

The observed light curve shows double-peaked structure starting at
T0-30s, ending at T0+62s with a duration (T90) of about 46 seconds.
The fluence in 100 - 1000 keV was 3.38(+0.31/-0.27)x10^-5 erg/cm^2.
The 1-s peak flux measured from T0s was 2.66(+0.49/-1.36) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-30s to
T0+62s is well fitted by a power-law with exponential cutoff model :
   dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha       1.66(+0.31/-0.65), and
   Epeak       527(+429/-274) keV (chi^2/d.o.f. = 10.2/13).

All the quoted errors are at statistical 90% confidence level, in which
the systematic uncertainties are 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: GRB130722A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15015
SUBJECT: GRB 130722A: Faulkes Telescope South optical candidate
DATE:    13/07/22 10:07:51 GMT
FROM:    Andrea Melandri at Liverpool John Moores U  <axm@astro.livjm.ac.uk>

A. Melandri (INAF/OAB), C. Guidorzi (U. Ferrara), J. Japelj (U.  
Ljubljana), D. Kopac (U. Ljubljana), C.G. Mundell (LJMU) and A. Gomboc  
(U. Ljubljana) report:

The 2-m Faulkes Telescope South automatically began observing GRB  
130722A (Troja et al. GCN Circ. 15013) on July 22 2013 at 08:21:29 UT  
(~130 s after the burst trigger).

We find a fading object at coordinates

RA(2000.0)=   17:22:36.47
Dec(2000.0)= -02:58:21.6   (error 1.3")

with the following magnitudes

Mid time from  Total Exp   Filter    Magnitude
trigger (min)   (s)
--------------------------------------------------------------
12.37           1x30        R       18.0 +- 0.1
18.07           1x60        R       18.3 +- 0.1
--------------------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars, performing  
aperture photometry of the proposed optical counterpart above together  
with the nearby object located at RA(2000.0)=17:22:36.54,  
Dec(2000.0)=-02:58:22.1. The latter might be related to the OT, has a  
distance of 1.2" from the candidate and a catalogued magnitude of  
R2=19.7. It looks extended and might be the host galaxy of GRB 130722A.


GRB_name: GRB130719A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15016
SUBJECT: GRB 130719A, Swift-BAT refined analysis
DATE:    13/07/22 11:24:38 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

M. Stamatikos (OSU), 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), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130719A (trigger #562625) (Marshall,
et al., GCN Circ. 15012).  The BAT ground-calculated position is
RA, Dec = 89.038, -11.591 deg which is
    RA(J2000)  =  05h 56m 09.2s
    Dec(J2000) = -11d 35' 29.0"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
  
The mask-weighted light curve shows a single weak approximately FRED peak.
T90 (15-350 keV) is 177.7 +- 20.5 sec (estimated error including systematics).
  
The time-averaged spectrum from T+6.2 to T+205.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.63 +- 0.17.  The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+82.68 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/562625/BA/


GRB_name: GRB130722A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15017
SUBJECT: GRB 130722A: Skynet/GORT observations
DATE:    13/07/22 17:21:26 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, K. McLin, L. Cominsky, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, J. Haislip, 
K. Ivarsen, D. James, A. LaCluyze, M. Maples, J. Moore, M. Nysewander, 
E. Speckhard, P. Taylor, and J. A. Crain report:

Skynet observed the Swift/BAT localization of GRB 130722A (Troja et al., 
GCN 15013, Swift trigger 563213) in the Rc and Ic bands with the 14" 
GLAST Optical Robotic Telescope (GORT) at the Hume observatory in 
California, beginning at t=100s post trigger and continuing until t~1hr. 
In stacked exposures, we marginally detect a source in both bands at the 
afterglow position reported by Melandri et al. (GCN 15015). Photometry 
is calibrated to 3 USNO-B1 stars in the field:

band     t[min]     exp[min]     mag
Rc       38         31           18.6 (+0.4, -0.3)
Ic       41         35           17.6 (+0.3, -0.2)

No further Skynet observations are scheduled.


GRB_name: GRB130722A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15018
SUBJECT: GRB 130722A: Swift-XRT refined Analysis
DATE:    13/07/22 21:30:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), A. Melandri (INAF-OAB), B.
Sbarufatti (INAF-OAB/PSU), P. D'Avanzo (INAF-OAB), J.A. Kennea (PSU),
V. Mangano (PSU) and E. Troja report on behalf of the Swift-XRT team:

We have analysed 7.3 ks of XRT data for GRB 130722A (Troja  et al. GCN
Circ. 15013),  from 117 s to 17.7 ks after the BAT trigger. The data
comprise 739 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
260.65405, -2.97376 which is equivalent to:

RA (J2000): 17 22 36.97
Dec(J2000): -02 58 25.5

with an uncertainty of 3.5 arcsec (radius, 90% confidence).

The late-time light curve (from T0+3.6 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.10 (+/-0.11).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.21 (+/-0.05). The
best-fitting absorption column is  4.18 (+0.18, -0.17) x 10^21 cm^-2,
in excess of the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.89 (+0.16, -0.15)
and a best-fitting absorption column of 4.9 (+0.9, -0.8) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.8 x 10^-11 (7.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.9 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 7.3 sigma
Photon index:      1.89 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.10, the count rate at T+24 hours will be 0.023 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (1.8 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/00563213.

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


GRB_name: GRB130722A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15019
SUBJECT: GRB 130722A: Enhanced Swift-XRT position
DATE:    13/07/22 21:53:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 6812 s of XRT Photon Counting mode data and 11 UVOT
images for GRB 130722A, 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 = 260.65190, -2.97283 which is equivalent
to:

RA (J2000): 17h 22m 36.46s
Dec (J2000): -02d 58' 22.2"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130722C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15020
SUBJECT: GRB 130722C Tiled Swift observations
DATE:    13/07/22 21:57:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
ANTARES GRB 130722C. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00017

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the ANTARES event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB130722A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15021
SUBJECT: GRB 130722A: MITSuME Okayama upper limits
DATE:    13/07/23 00:58:08 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME collaboration:

We observed the field of GRB 130722A (Troja et al., GCNC 15013)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2013-07-22 11:15:06 UT (~2.9 h after the burst).
We could not detect the previously reported afterglow
(Melandri et al., GCNC 15015; Trotter et al., GCNC 15017) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.23056    13:51:20    9000.0   >18.7  >18.8  >18.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130722A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15022
SUBJECT: GRB 130722A: Swift/UVOT Detection
DATE:    13/07/23 02:38:51 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130722A
120 s after the BAT trigger (Troja et al., GCN Circ. 15013).
A decaying source consistent with the optical position
(Melandri et al. GCN Circ. 15015)
is detected in the initial UVOT exposures.
As noted by Melandri et al., there is a catalogued source
near the position of the optical afterglow.
The magnitudes and uncertainties reported below have been
adjusted to accommodate the possibility that the nearby
source accounts for all or none of the UVOT count rate
observed at late times.

The preliminary UVOT position is:
  RA(J2000)  =  17:22:36.47 = 260.65196
  DEC(J2000) = -02:58:21.6  =  -2.97268
with an estimated uncertainty of 0.7 arcsec (radius, 90% confidence).
The uncertainty has been adjusted slightly due to the
possible contamination of the nearby source by up to 10%.

The preliminary detection and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

white_FC           120          270          147          19.6 (+0.12/-0.20)
v                 4209         5844          393         >19.7
b                 3594        17728         2039         >20.9
u                  332        16943         2059         >21.0
w1                4619        16030         1218         >21.2
w2                4004         5640          393         >21.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.63 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130722A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15023
SUBJECT: Konus-Wind observation of GRB 130722A
DATE:    13/07/23 07:54:01 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 130722A
(Swift-BAT trigger 563213: Troja, et al., GCN 15013)
triggered Konus-Wind at T0=30001.378 s UT (08:20:01.378).

The light curve  from ~T0-6 s to ~T0+55 s shows two main
emission pulses peaked at ~T0+1 s and ~T0+31 s, respectively.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130722_T30001/

As observed by Konus-Wind, the burst
had a fluence of (2.35  0.12)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.256s,
of (1.84  0.22)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The 3-channel time-integrated spectrum
(measured from T0-6.663 to T0+55.191 s)
can be modeled, in the 20 keV - 1.35 MeV range,
by cutoff power law with the following model parameters:
the photon index alpha = -0.92  0.03
and the peak energy Ep = 179  5 keV,

The spectrum at the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit, in the 20 keV - 5 MeV range,
by cutoff power law with the following model parameters:
the photon index alpha = -0.76  0.12
and the peak energy Ep = 219  15 keV,
chi2 = 90.3/76 d.o.f.

All the quoted results are preliminary.


GRB_name: GRB130722C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15024
SUBJECT: Retraction of GCN Circ. 15020 (GRB 130722C Tiled Swift observations)
DATE:    13/07/23 13:22:22 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page and C.J. Mountford (U. Leicester) report on behalf of the
Swift-XRT team:

GCN Circ. 15020, stating that Swift was performing tiled observations of
GRB 130722C, was the result of a system error. There is no GRB 130722C. We
apologise for any inconvenience caused.


GRB_name: GRB130702A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15025
SUBJECT: GRB 130702A in the Ep,i - Eiso plane
DATE:    13/07/23 13:50:35 GMT
FROM:    Lorenzo Amati at INAF-IASF/Bologna  <amati@iasfbo.inaf.it>

L. Amati (INAF - IASF Bologna), S. Dichiara, F. Frontera, C. Guidorzi
(University of Ferrara), Luca Izzo (ICRANet, Rome), M. Della Valle
(INAF-Osservatorio Astronomico di Capodimonte) report:

A preliminary analysis of the spectral data of GRB130702A provided by the 
Fermi/GBM integrated over the whole duration of the event (63.3 s from 
T0-3.0 to T0 +60.3; detectors n7 and n8) suggests that the spectrum can be 
fit with a simple power-law with index ~2.1+/-0.1, which is significantly 
softer than the value obtained by considering only the brightest part of 
the event (Collazzi & Connaughton GCN 14972; Golenetskii et al. GCN 
14986). This result indicates that the spectral peak energy, Ep, is close 
to the low energy threshold of the instrument or lower than it. After 
fitting the spectrum with a Band function with alpha fixed at different 
values and by assuming the redshift of 0.145 (e.g., Leloudas et al. GCN 
14983; Mulchaey et al. GCN 14985), we find a 90% upper limit to the 
cosmological rest-frame peak energy, Ep,i, of ~15-20 keV and and 
isotropic-equivalent radiated energy, Eiso, of ~(6.5+/-0.10)x10^50 erg 
(flat FLRW Universe with H0=70 km/s/Mpc and Omega_M = 0.3).

Based on these estimates, GRB 130702A is consistent with the Ep,i - Eiso 
correlation holding for typical long GRBs and lies in the region bridging 
classical cosmological long GRBs with closer and weaker GRB-SN events like 
GRB060218/SN2006aj and XRF020903 (see 
http://www.iasfbo.inaf.it/~amati/grb130702a.pdf).


GRB_name: GRB130725A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15028
SUBJECT: Swift Trigger 563980 is GRB 130725A 
DATE:    13/07/25 15:14:06 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

B.-B. Zhang (PSU/UAH), S. D. Barthelmy (GSFC), M. M. Chester (PSU), D. Grupe (PSU),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), S. R. Oates (MSSL-UCL), H. A. Krimm (USRA/CRESST/GSFC),
J. A. Kennea (PSU), Daniele Malesani (DARK/NBI), M. H. Siegel (PSU) and F. E. Marshall (NASA/GSFC) 
report on behalf of the Swift Team:


At 11:37:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130725A (trigger=563980). Swift slewed to the burst.
This burst was not identified in real-time due to telemetry gaps.


The BAT on-board calculated location is
RA, Dec 230.034,+0.624 which is  
  RA(J2000) = 15h 20m 8s
  Dec(J2000) = +00d 37' 26"
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 15 sec.  The peak count rate
was ~600 counts/sec (15-350 keV), at ~5 sec after the trigger.


The XRT began observing the field at 12:28:46 UT, 3094 seconds after
the BAT trigger. Using 2.28 ks of ground-linked XRT data, we found an
uncatalogued X-ray source located at RA, Dec = 230.033,+0.627, which is 
equivalent to:

RA(J2000)  = +15h 20m 07.92s
Dec(J2000) = 00d 37' 40.2"
with an uncertainty of 4.0 arc seconds (radius, 90% containment). 

UVOT took a finding chart exposure of 150 seconds with the White filter 3097 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 0.06.

Further analysis is on-going.  This circular is an official product of the Swift  team.


GRB_name: GRB130725B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15029
SUBJECT: GRB 130725B: Swift detection of a burst
DATE:    13/07/25 18:06:07 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

C. A. Swenson (PSU), M. M. Chester (PSU), D. Grupe (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU) and B.-B. Zhang (UAH)
report on behalf of the Swift Team:

At 17:39:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130725B (trigger=564028).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 214.232, -11.140 which is 
   RA(J2000) = 14h 16m 56s
   Dec(J2000) = -11d 08' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  BAT light curve data are currently unavailable. 

Using promptly downlinked data we find a bright, uncatalogued X-ray
source located at RA, Dec 214.24096, -11.12909 which is equivalent to:
   RA(J2000)  = 14h 16m 57.83s
   Dec(J2000) = -11d 07' 44.7"
with an uncertainty of 4.4 arcseconds (radius, 90% containment). 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 (5.15 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.4
(+4.04/-3.23) x 10^21 cm^-2 (90% confidence). 

UVOT data are unavailable at this time. 

Burst Advocate for this burst is C. A. Swenson (cswenson 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: GRB130719A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15030
SUBJECT: GRB 130719A: Skynet/PROMPT observations
DATE:    13/07/25 18:43:14 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, A. LaCluyze, J. Haislip, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor, 
and J. A. Crain report

Skynet observed the Swift/BAT localization of GRB 130719A (Marshall et 
al., GCN 15012, Swift trigger #562625) with four 16" telescopes of the 
PROMPT array at CTIO, Chile.  Starting at 2013-07-19, 19:17 UT and 
continuing until 09:20 UT (t=3.53-4.84h post-trigger), it took ~28 
160-sec exposures in each of the BVRI bands. We did not detect a 
credible afterglow candidate within the 3 arcmin radius of the Swift/BAT 
error circle, which was centered on RA 05:56:09.4, Dec -11:35:04.

We stacked all the images in each band and obtained 3-sigma limiting 
magnitudes on any afterglow at t~4.2h:
Filter       B       V       R       I
Mag        >21.2   >20.6   >20.7   >20.3

Magnitudes are Vega magnitudes, calibrated to 3 USNO-B1/NOMAD stars in 
the field, and have not been corrected for the expected line-of-sight 
Milky Way dust extinction E(B-V)~0.7 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130725A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15031
SUBJECT: GRB 130725A, Swift-BAT refined analysis
DATE:    13/07/25 19:05:30 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), B.-B. Zhang (PSU/UAH)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+731 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130725A (trigger #563980)
(Zhang, et al., GCN Circ. 15028).  The BAT ground-calculated position is
RA, Dec = 230.060, 0.624 deg which is
     RA(J2000)  =  15h 20m 14.4s
     Dec(J2000) = +00d 37' 26.8"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 39%.

The mask-weighted light curve shows a double-peaked structure lasting from
approximately T+0 to T+20 seconds.  This is followed by lower-level emission out
to ~T+100 seconds. The source went out of the field of view at ~T+450 seconds,
following a pre-planned slew. T90 (15-350 keV) is 101.8 +- 20.5 sec (estimated
error including systematics).

The time-averaged spectrum from T-9.83 to T+103.40 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.60 +- 0.30.  The fluence in the 15-150 keV band is 9.7 +- 1.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.11 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/563980/BA/


GRB_name: GRB130725B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15032
SUBJECT: GRB 130725B: Swift/UVOT Detection of an Optical Counterpart
DATE:    13/07/25 21:56:37 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H Siegel and C. A. Swenson (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130725B
72 s after the BAT trigger (Swenson et al., GCN Circ. 15029).
A source consistent with the XRT position
(Swenson et al. GCN Circ. 15029)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  14:16:57.76 = 214.24068 (deg.)
  Dec (J2000) = -11:07:41.8  = -11.12827 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

white               72          221          147         17.29 +/- 0.03
u                  284          534          246         17.96 +/- 0.07

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.061 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130725A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15033
SUBJECT: GRB 130725A: MITSuME Ishigakijima Optical Observation
DATE:    13/07/26 01:04:02 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130725A (Zhang et al., GCNC 15028)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2013-07-25 13:34:52 UT (~2.0 h after the
burst). We detected the afterglow candidate within the XRT error circle
(Zhang et al., GCNC 15028) in only Rc band.

Photometric result and three sigma upper limits of the OT are listed below.
We used SDSS catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc  Rc_err  Ic
----------------------------------------------------------------------
0.10534    14:08:53   2280.0    >21.3   20.8 0.2   >19.8
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130725B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15034
SUBJECT: GRB 130725B: GROND Detection of the Optical/NIR Afterglow
DATE:    13/07/26 05:30:18 GMT
FROM:    Felipe Olivares Estay at MPE  <felipe@mpe.mpg.de>

M. Tanga (MPE Garching), F. Olivares E. (UNAB, MCSS), and J. Greiner
(MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 130725B (Swift trigger 564028; Swenson et al.,
GCN #15029) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La
Silla Observatory (Chile).

Observations started at 00:47 UT on July 26, 2013, 7.1 hours after the
GRB trigger. They were performed at an average seeing of 1.5" and at
an average airmass of 1.2.

We detect the afterglow at the position of Siegel et al. (GCN #15032), and
based on the first images with total exposures of 4.4 minutes in g'r'i'z'
and 8 minutes in JHK, we estimate preliminary magnitudes (all in AB) of

g' = 21.1 +/- 0.1 mag,
r' = 20.5 +/- 0.1 mag,
i' = 20.4 +/- 0.1 mag,
z' = 20.4 +/- 0.1 mag,
J = 20.4 +/- 0.3 mag,
H = 19.9 +/- 0.3 mag, and
K = 19.5 +/- 0.4 mag.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E(B-V) = 0.061 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130725A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15035
SUBJECT: GRB 130725A - Faulkes Telescope South Observations
DATE:    13/07/26 08:43:47 GMT
FROM:    Andrea Melandri at Liverpool John Moores U  <axm@astro.livjm.ac.uk>

F.J. Virgili (LJMU), C. Guidorzi (U. Ferrara),  J. Japelj, D. Kopac  
(U. Ljubljana), A. Melandri (INAF-OAB) report:

"The 2-m Faulkes Telescope South robotically followed up GRB 130725A  
(SWIFT trigger 563980; Zhang et al. GCN 15028) beginning 111.9 min  
after the GRB trigger time. No optical counterpart is detected within  
the XRT error circle to the following conservative limits:

Midtime from GRB    Exposure    Filter    Magnitude
      (min)                        (s)
-------------------------------------------------------------------------
      112.2                  3x10s           r'         > 18.9
      117.1                  1x10s           i'         > 17
-------------------------------------------------------------------------

Values are calibrated against nearby SDSS field stars.


GRB_name: GRB130725A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15036
SUBJECT: GRB 130725A: Swift/UVOT Upper Limits
DATE:    13/07/26 11:49:46 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) and B.-B. Zhang (PUS/UAH)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130725A 
(Zhang et al., GCN Circ. 15028) 3097 s after the BAT trigger (trigger=563980).
No optical afterglow consistent with the XRT position is 
detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC          3097         3247          147         >21.1
white             3097         4480          344         >21.0
v                 3255        10746         1278         >20.4
b                 4075         5690          373         >20.4
u                 3870        17226         1118         >21.0
w1                3665        16476         1279         >21.0
m2                3460        11458         1089         >21.0
w2                4486         9832         1082         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130725B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15038
SUBJECT: GRB 130725B - UVOT-enhanced XRT position
DATE:    13/07/26 13:28:49 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@gmail.com>

B. Sbarufatti (INAF-OAB/PSU), C. Swenson (PSU), P.A. Evans and 
M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team:

Using 4385 s of XRT Photon Counting mode data and 5 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 =
214.24065, -11.12845 which is equivalent to:

RA (J2000):  14 16 57.76
Dec (J2000): -11 07 42.4

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, MNRAS, 397, 1177).


GRB_name: GRB130725B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15039
SUBJECT: GRB130725B: REM-ROS2 optical observations
DATE:    13/07/26 13:48:28 GMT
FROM:    Dino Fugazza at INAF-OAB  <dino.fugazza@brera.inaf.it>

D. Fugazza, S. Covino, G. Tagliaferri (INAF-OAB), V. D'Elia (INAF-OAR) 
report on behalf of the CIBO team:

We observed the field of GRB 130725B (Swenson et al., GCN 15029) 
simultaneously in the optical and near-infrared with the the 60-cm 
robotic telescope REM at La Silla Observatory (Chile). The observations 
started at 23:41:40 UT on July 25 2013, about 6.03 hours after the GRB 
and lasted for about 45 min.
We detect the afterglow reported by Siegel et al. (GCN 15032) and Tanga 
et al. (GCN 15034) with the upgraded ROS2 optical camera. In the NIR 
with REMIR camera the afterglow was not detected.
ROS2 is able to observe simultaneously in the g', r', i', and z' filters 
and preliminary magnitudes (AB) are:

g' = 20.65  0.07
r' = 20.32  0.07
i' = 20.08  0.09

The magnitudes are calibrated against the APASS catalogue.


GRB_name: GRB130725B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15040
SUBJECT: GRB 130725B: Swift-XRT refined Analysis
DATE:    13/07/26 15:10:08 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/PSU) and C. A. Swenson (PSU) report on behalf
of the Swift-XRT team:

We have analysed 8.2 ks of XRT data for GRB 130725B (Swenson  et al.
GCN Circ. 15029),  from 53 s to 35.0 ks after the  BAT trigger. The
data comprise 235 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. Using 6414 s of PC mode data and 9 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 214.24059, -11.12851
which is equivalent to:

RA (J2000): 14h 16m 57.74s
Dec(J2000): -11d 07' 42.6"

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

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.09 (+0.15, -0.18), followed by a break at T+534 s to
an alpha of 0.95 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.17, -0.16). The
best-fitting absorption column is  8.3 (+4.2, -3.2) x 10^20 cm^-2,
consistent with the Galactic value of 5.2 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 3.6 x 10^-11 (4.5 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.3 (+4.2, -3.2) x 10^20 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Photon index:      1.97 (+0.17, -0.16)

If the light curve continues to decay with a power-law decay index of
0.95, the count rate at T+24 hours will be 0.012 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x
10^-13 (5.5 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/00564028.

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


GRB_name: GRB130725B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15041
SUBJECT: GRB 130725B, Swift-BAT refined analysis
DATE:    13/07/26 15:24:07 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), C. A. Swenson (PSU),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+454 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130725B (trigger #564028)
(Swenson, et al., GCN Circ. 15029).  The BAT ground-calculated position is
RA, Dec = 214.233, -11.124 deg which is
     RA(J2000)  =  14h 16m 55.9s
     Dec(J2000) = -11d 07' 26.3"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask-weighted light curve shows a single FRED burst peaking at T+1 sec
and decaying to baseline by about T+8 sec. T90 (15-350 keV) is 10.0 +- 3.6
sec (estimated error including systematics).

The time-averaged spectrum from T-0.3 to T+12.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.23 +- 0.17.  The fluence in the 15-150 keV band is 3.9 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.29 sec in the 15-150 keV band
is 2.2 +- 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/564028/BA/


GRB_name: GRB130725A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15042
SUBJECT: GRB 130725A: Swift-XRT refined Analysis
DATE:    13/07/26 15:28:18 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

B.-B. Zhang (PSU/UAH)  reports on behalf of the Swift-XRT team:

We have analysed 6.8 ks of XRT data for GRB 130725A,  from 3.1 ks to
17.2 ks after the  BAT trigger. The data are entirely in Photon
Counting (PC) mode. Using 3850 s of PC mode data and 5 UVOT images, we
find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
230.03240, +0.62761 which is equivalent to:

RA (J2000): 15h 20m 07.78s
Dec(J2000): +00d 37' 39.4"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.7 (+0.4, -0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+0.6, -0.5). The
best-fitting absorption column is  9 (+11, -5) x 10^20 cm^-2,
consistent with the Galactic value of 4.3 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 2.9 x 10^-11 (4.5 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9 (+11, -5) x 10^20 cm^-2
Galactic foreground: 4.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.5 (+0.6, -0.5)

If the light curve continues to decay with a power-law decay index of
0.7, the count rate at T+24 hours will be 2.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.5 x
10^-14 (1.3 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/00563980.

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


GRB_name: GRB130725B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15044
SUBJECT: GRB 130725B:  Swift trigger time correction
DATE:    13/07/26 17:26:01 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) reports on behalf of the Swift team:

The BAT trigger time for GRB 130725B (GCN Circ. 15029) was incorrectly 
identified.  The correct trigger time is 17:39:28 UT.  We apologize for 
any inconvenience.


GRB_name: GRB130725B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15045
SUBJECT: GRB 130725B: Swift/UVOT Observations
DATE:    13/07/26 17:50:43 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

S. R. Oates (UCL-MSSL) and C. A. Swenson (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130725B
72 s after the BAT trigger (Swenson et al. GCN Circ. 15029;
Swenson GCN Circ. 15044).

A source consistent with the enhanced XRT position (Sbarufatti and Swenson GCN Circ. 15040)
is detected in the initial UVOT exposures in all filters except for uvm2 and uvw2.
The non-detection in these filters suggests a redshift ~<2.

The preliminary UVOT position is:
   RA  (J2000) =  14:16:57.76 = 214.24068 (deg.)
   Dec (J2000) = -11:07:41.8  = -11.12827 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

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

white               72          221          147         16.67 +/- 0.03
v                  614         6315          252         19.16 +/- 0.27
b                  540          559           19         18.20 +/- 0.28
u                  284          534          246         17.35 +/- 0.06
w1                 663         6725          236         20.01 +/- 0.36
m2                6320        16621         1003        >21.1
w2                4265         4465          197        >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.061 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130727A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15046
SUBJECT: GRB 130727A: Swift detection of a burst
DATE:    13/07/27 17:18:52 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. C. Stroh (PSU), N. Gehrels (NASA/GSFC) and D. M. Palmer (LANL)
report on behalf of the Swift Team:

At 16:45:19.52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130727A (trigger=564342).  Swift could not slew to the burst
due to an Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec  330.800, -65.575 which is 
  RA(J2000) = 22h 03m 12s
  Dec(J2000) = -65d 34' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  BAT light curve data are currently unavailable. 

Due to an observing constraint, Swift will not slew until T0+49.6
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is M. C. Stroh (stroh AT astroh.org). 
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: GRB130727A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15047
SUBJECT: GRB 130727A: Swift-XRT and Swift-UVOT prompt observations
DATE:    13/07/27 18:25:06 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M. C. Stroh and M. M. Chester (PSU) report on behalf of the Swift team:

Swift-XRT observed the field of GRB 130727A (Stroh et al., GCN Circ. 15046) starting 3484.5 s after the BAT trigger, due to an observing constraint. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA,Dec = 330.7994, -65.5387 (degrees) which is equivalent to:

RA  (J2000) = 22 03 11.85
DEC (J2000) = -65 32 19.5

with an uncertainty of 2.5 arcsec (radius, 90% containment). This location is 130.7 arcseconds from the BAT onboard position, inside the BAT error circle.

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, MNRAS, 397, 1177).

UVOT took a finding chart exposure of 150 seconds with the White filter starting 3494 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 none of the XRT error circle. 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 0.03. 


GRB_name: GRB130727A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15048
SUBJECT: GRB 130727A: Swift-XRT observations
DATE:    13/07/27 18:38:48 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (ASDC), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU) and G. Cusumano
(INAF-IASF PA) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 130727A at 17:43:24.0 UT,
3484.5 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source with an enhanced position: RA, Dec
330.7988, -65.5384 which is equivalent to:
   RA(J2000)  = 22h 03m 11.70s
   Dec(J2000) = -65d 32' 18.4"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 131 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 (2.79 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.3
(+1.54/-1.39) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB130727A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15049
SUBJECT: GRB 130727A: Swift-BAT refined analysis
DATE:    13/07/27 19:42:16 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),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), M. C. Stroh (PSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+831 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130727A (trigger #564342)
(Strohe, et al., GCN Circ. 15046).  The BAT ground-calculated position is
RA, Dec = 330.790, -65.540 deg, which is 
   RA(J2000)  =  22h 03m 09.5s 
   Dec(J2000) = -65d 32' 23.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-5 sec and ening at ~T+30 sec.  T90 (15-350 keV) is 13.57 +- 0.81 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-1.08 to T+24.38 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.65 +- 0.05.  The fluence in the 15-150 keV band is 3.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+7.42 sec in the 15-150 keV band
is 7.0 +- 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/564342/BA/


GRB_name: GRB130727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15050
SUBJECT: GRB 130727A: Faulkes Telescope South optical afterglow
DATE:    13/07/27 19:44:30 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), F. Virgili (LJMU) on behalf of
a large collaboration report:

The 2-m Faulkes Telescope South automatically began observing GRB
130727A (Stroh et al. GCN Circ. 15046) on July 27 2013 at 17:01:22 UT
(~16 min after the burst trigger).

Within the XRT error circle (Perri et al. GCN Circ. 15048) we
find a fading uncatalogued object at coordinates

RA(2000.0)=   22:03:11.66
Dec(2000.0)= -65:32:18.7   (error 0.5")

with the following magnitudes

Mid time from  Total Exp   Filter    Magnitude
trigger (min)   (s)
--------------------------------------------------------------
16.0            10          R       19.3 +- 0.3
47.1           180          R       20.1 +- 0.1
--------------------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB130727A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15051
SUBJECT: GRB 130727A: Enhanced Swift-XRT position
DATE:    13/07/28 00:52:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1995 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130727A, 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 = 330.79842, -65.53856 which is equivalent
to:

RA (J2000): 22h 03m 11.62s
Dec (J2000): -65d 32' 18.8"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130727A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15052
SUBJECT: GRB 130727A: GROND observations
DATE:    13/07/28 01:24:11 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

V. Sudilovsky, K. Varela, and J. Greiner
(all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 130727A (Swift trigger 564342; Stroh et al.,
GCN #15046) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La
Silla Observatory (Chile).

Observations started at 23:40 UT on July 27, 2013, 7 hours after the
GRB trigger. They were performed at an average seeing of 2.3" and at
an average airmass of 2.2.

We detect the afterglow reported by Guidorzi et al. (GCN #15050), and
based on images with total exposures of 1500s in g'r'i'z'
and 1200s in JHK, we estimate preliminary magnitudes (all in AB) of

g' = 22.3 +/- 0.1 mag,
r' = 21.8 +/- 0.1 mag,
i' = 21.6 +/- 0.1 mag,
z' = 21.0 +/- 0.2 mag,
J = 20.4 +/- 0.3 mag,
H > 20.1 mag, and
K > 19.4 mag.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E(B-V) = 0.03 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130727A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15053
SUBJECT: GRB 130727A: Fermi GBM detection
DATE:    13/07/28 01:49:33 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

A. Goldstein (ORAU/NASA MSFC) reports on behalf of the Fermi GBM Team:

At 16:45:20.91 UT on 27 July 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130727A (trigger 396636323 /130727698)
which was also detected by the Swift BAT (Stroh et al. 2013, GCN 15046).
The GBM on-ground location is consistent with the Swift position;
the angle from the Fermi LAT boresight is 134 degrees.

The GBM light curve consists of one main pulse with substructure
with a duration (T90) of about 13.0 s (50-300 keV).  The 
time-averaged spectrum from T0=-1.0 s to T0+12.0 s is adequately fit 
by a Band function with Epeak = 118 +/- 17 keV, alpha = -1.1 +/- 0.1, 
and beta = -2.2 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is 
(8.9 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured starting 
from T0+6.1 s in the 8-1000 keV band is 11.1 +/- 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: GRB130727A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15054
SUBJECT: GRB 130727A: Swift-XRT refined Analysis
DATE:    13/07/28 02:35:06 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M. C. Stroh (PSU) reports on behalf of the Swift-XRT team:

We have analysed 3.9 ks of XRT data for GRB 130727A (Stroh  et al. GCN
Circ. 15046),  from 3.5 ks to 15.8 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN. Circ 15051).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.89 (+/-0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+/-0.18). The
best-fitting absorption column is  1.6 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 2.8 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 3.7 x 10^-11 (5.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: 4.6 sigma
Photon index:      2.01 (+/-0.18)

If the light curve continues to decay with a power-law decay index of
0.89, the count rate at T+24 hours will be 0.020 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.4 x
10^-13 (1.0 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/00564342.

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


GRB_name: GRB130727A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15055
SUBJECT: Konus-Wind observation of GRB 130727A
DATE:    13/07/28 10:40:40 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 130727A
(Swift-BAT trigger 564342: Stroh, et al., GCN 15046)
triggered Konus-Wind at T0=60324.015 s UT (16:45:24.015)

The light curve shows multiple overlapping peaks from ~T0-2 s to ~T0+12 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130727_T60324/

As observed by Konus-Wind, the burst
had a fluence of (9.0  1.1)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.064 s,
of (2.9  0.4)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.23  0.22,
the high energy photon index beta = -2.21  0.12,
the peak energy Ep = 113  22 keV,
chi2 = 116/97 dof.

All the quoted results are preliminary.


GRB_name: GRB130727A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15056
SUBJECT: GRB 130727A: Swift/UVOT Detection
DATE:    13/07/28 15:00:47 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and M. Stroh (PSU) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130727A
3495 s after the BAT trigger (Stroh et al., GCN Circ. 15046).
A source consistent with the XRT position (Goad et al. GCN Circ. 15051)
is detected in initial UVOT Finding Chart (FC) exposure taken in white
filter, and it is also detected in summed UVOT exposures taken with white
and u filters. The same source is marginally detected (confidence level
~2 sigma) in b and uw1 filters.

Its UVOT position (J2000) is

RA = 22h 03m 11.62s = 330.79842
Dec = -65d 32m 18.8s = -65.53856.

with an estimated uncertanties of 0.7 arcseconds. The position of the
optical source is consistent with that given by the Faulkes Telescope
(Guidorzi et al., GCN 15050).

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for
the early exposures are:

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

white_FC          3495         3645          147          21.27  0.34
white             3495         4876          344          21.35  0.24
v                 3651        16978          880         >20.96
b                 4471         4671          197          21.44  0.60
u                 4266        11215          934          20.99  0.26
w1                4061        10452         1082          21.89  0.54
m2                3856         5452          355         >20.50
w2                4882        16473         1082         >21.80

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130722A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15057
SUBJECT: GRB 130722A: RATIR Optical Observations
DATE:    13/07/29 05:13:38 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

 Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Chris
Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB),
Antonino Cucchiara (UCSC), Eleonora Troja (GSFC), Enrico Ramirez-Ruiz
(UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez
(UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley
(GSFC) report:

We observed the field of GRB 130722A (Melandri, et al., GCN 15013) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/07 23.23 to 2013/07 23.39 UTC (21.24 to
25.00 hours after the BAT trigger), obtaining a total of 2.33 hours
exposure in the i' band.

We detect the candidate GRB host galaxy from Melandri et al. (GCN 15015)
noting also that the source is extended. In comparison with USNO-B1, we
obtain:

 i'     19.58 +/- 0.02

This magnitude is in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  We do not detect the candidate OT,
although it is likely blended with the host galaxy. In comparison with the
Faulkes measurement one night earlier, the OT has thus faded by at least
1.5 magnitudes.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15058
SUBJECT: GRB 130727A: Watcher optical limit
DATE:    13/08/01 15:19:44 GMT
FROM:    Martin Topinka at UCD, Dublin  <martin.topinka@gmail.com>

Martin Topinka, Lorraine Hanlon, Martin Jelinek and Seamus Meehan, on behalf of the Watcher telescope team, report:

We followed the Swift detection of GRB 130727A (Stroh et al., GCN Circ. 15046, Swift trigger 564342) with the Watcher robotic telescope (D=40cm) located at Boyden Observatory, near Bloemfontein in South Africa.

We started imaging the field at 16:59:43 UT on 2013-07-27 (14m 23s after the BAT trigger, 25s after receiving the GCN trigger) taking 60s exposures in the clear filter (C) using an Andor CCD camera.

No optical counterpart is detected within the XRT/UVOT error circle (Goad et al./De Pasquale et al., GCN Circ. 15051/15056) in any of the individual 60s images either in a combined image covering time from 17:01:55 UT to 17:11:40 UT with the total exposure of 540s. Image analysis yields the limiting magnitude of ~18.9 +/- 0.1.

Start | End | Exposure | Filter | Limiting mag. | Limiting mag. error
17:01:55 UT | 17:11:40 UT | 540s | C | > 18.9 | 0.1

This message is quotable in publications.


GRB_name: GRB130803A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15059
SUBJECT: GRB 130803A: Swift detection of a burst
DATE:    13/08/03 10:13:29 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), D. M. Palmer (LANL) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 10:02:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130803A (trigger=565263).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 220.241, -2.467 which is 
   RA(J2000) = 14h 40m 58s
   Dec(J2000) = -02d 28' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 50 sec.  The peak count rate
was ~4750 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 10:04:22.8 UT, 90.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 220.25472, -2.49296 which is equivalent
to:
   RA(J2000)  = 14h 41m 01.13s
   Dec(J2000) = -02d 29' 34.7"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 105 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.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.16 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 7
(+6.70/-4.79) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 93 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 none of
the XRT error circle. 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 0.05. 

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: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15060
SUBJECT: GRB 130603B: Second epoch of HST WFC/F160W imaging
DATE:    13/08/03 11:26:03 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

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

"We inspected the second epoch of HST WFC3/F160W imaging of the short GRB
130603B obtained on 2013 July 3.24 UT.  Digital image subtraction relative
the first epoch (on 2013 June 13.15 UT) reveals that the near-IR point
source coincident with the afterglow position has faded away, confirming
our original suggestion that it is associated with GRB 130603B (Berger et
al. 2013 arXiv:1306.3960).  The subtraction also confirms our brightness
measurement, with m(F160W)=25.8 AB mag.  Coupled with an early steep
decline in the optical band based on additional Magellan/IMACS observations
at 32.2 hr post-burst, with r>24.8 AB mag (see also Cucchiara et al. 2013,
arXiv:1306.2028; Tanvir et al. 2013, arXiv:1306.4971) this confirms the
likely kilonova origin of this source."


GRB_name: GRB130803A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15061
SUBJECT: GRB 130803A: Faulkes Telescope South Observations
DATE:    13/08/03 14:18:21 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF/OAB), C. Guidorzi (U. Ferrara) and C. G. Mundell  
(LJMU) report on behalf of a large collaboration:

Tha Faulkes Telescope South robotically observed the field of GRB  
130803A starting ~ 2.9 minutes after the Swift trigger (Page et al.,  
GCN 15059). We find no credible afterglow candidate in the XRT error  
circle.

We estimate a 3 sigma upper limit of R>20.0 (texp=30s) ~3.5 minutes  
and I>21.9 (texp=700s) ~40 minutes after the burst.

Magnitudes are calibrated against nearby USNOB-1 stars.


GRB_name: GRB130803A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15062
SUBJECT: GRB 130803A: Enhanced Swift-XRT position
DATE:    13/08/03 17:56:56 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2053 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 130803A, 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 = 220.25273, -2.49195 which is equivalent
to:

RA (J2000): 14h 41m 0.66s
Dec (J2000): -02d 29' 31.0"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130803A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15063
SUBJECT: GRB 130803A, Swift-BAT refined analysis
DATE:    13/08/03 19:03:46 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

GRB 130803A, Swift-BAT refined analysis
  
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),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130803A (trigger #565263) (Page, et al.,
GCN Circ. 15059).  The BAT ground-calculated position is
RA, Dec = 220.256, -2.499 deg which is
    RA(J2000)  =  14h 41m 01.4s
    Dec(J2000) = -02d 29' 58"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 30%.
  
The mask-weighted light curve shows two well-separated symmetrical peaks.  The
first, larger peak starts at about T0-2 seconds and lasts until about T+8 seconds.
The second peak, which was softer, starts about T0+41 seconds and lasts until about
T0+48 seconds.  T90 (15-350 keV) is 44 +- 2 sec (estimated error including
systematics).
  
The time-averaged spectrum from T-1.24 to T+45.76 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.69 +- 0.14.  The fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+2.09 sec in the 15-150 keV band
is 5.1 +- 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/565263/BA/


GRB_name: GRB130803A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15064
SUBJECT: GRB 130803A; Fermi GBM observation
DATE:    13/08/04 00:35:04 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 130803A: Fermi GBM observation

Hoi-Fung Yu (MPE) report on behalf of the Fermi GBM Team:

"At 10:02:53.75 UT on 03 Aug 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130803A (trigger 397216976 / 130803419),
which was also detected by the Swift BAT and XRT (Page et al. 2013,
GCN 15059). The GBM on-ground location is consistent with the Swift
position. The angle from the Fermi LAT boresight is 86 degrees.

The GBM light curve consists of a single pulse,
with a duration (T90) of about 7.6 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+4.9 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power-law index is -0.85 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 141.6 +/- 12.2 keV.

The event fluence (10-1000 keV) in this time interval is
(2.5 +/- 0.1)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.6 s in the 10-1000 keV band
is 7.1 +/- 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: GRB130803A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15065
SUBJECT: GRB 130803A: Swift/UVOT Upper Limits
DATE:    13/08/04 02:09:13 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and K. L. Page (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130803A
93 s after the BAT trigger (Page et al., GCN Circ. 15059).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 15062)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

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

white_FC            93          243          147         >21.0
u_FC               305          555          246         >20.3
white               93         6186          560         >21.7
v                  636        11010         1142         >20.8
b                  561         5981          413         >21.0
u                  305         5776          639         >20.7
w1                3936        16308          788         >21.4
m2                5167        11916         1082         >21.2
w2                4757         6392          393         >20.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst


GRB_name: GRB130803A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15066
SUBJECT: GRB130803A: GROND detection of possible host
DATE:    13/08/04 05:53:17 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

K.Varela (MPE Garching), P.Afonso (American River College) and J.Greiner
(MPE Garching)report on behalf of the GROND team :

We observed the field GRB 130803A (Swift trigger 565263; Page et al.,
GCN 15059) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al.2008,
PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 23:13 UT on August 3, about 13.2 hours after
the trigger at a mean seeing of 1.8 arcsec and a mean airmass of 1.3. We
detect an extended source inside the enhanced 1.4'' XRT error circle
(Swift webpage). This could be the GRB host, though at the moment no
statement about variability can be made.

For stacked integration times of 100 min. in JHK and ~ 125min in griz, we
present the following preliminary magnitudes and ULs at the 3 sigma level:

g' = 25.6 +/- 0.4 mag,
r' = 24.4 +/- 0.3 mag,
i' = 23.8 +/- 0.2 mag,
z' = 23.4 +/- 0.3 mag,
J > 23.2 mag,
H > 22.5 mag, and
K > 22.2 mag.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E(B-V) = 0.05 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130803A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15067
SUBJECT: GRB 130803A: RATIR Optical and NIR Observations
DATE:    13/08/04 07:00:59 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh
Bloom (UCB), Antonino Cucchiara (UCSC), Eleonora Troja (GSFC), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130803A (Page, et al., GCN 15059) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/08 4.15 to 2013/08 4.25 UTC (17.51
to 19.98 hours after the BAT trigger), obtaining a total of 1.53 hours
exposure in the r' and i' bands and 0.63 hours exposure in the Z,
Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with SDSS DR9
and 2MASS, we obtain the following upper limits (3-sigma):

  r'    > 23.29
  i'    > 23.24
  Z     > 22.27
  Y     > 21.70
  J     > 20.90
  H     > 20.24

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB. Our upper limits are consistent
with the detections and upper limits reported by Varela, et al. (GCN 15066).

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130803A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15068
SUBJECT: GRB 130803A: Swift-XRT refined Analysis
DATE:    13/08/04 09:13:24 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz
(U. Leicester), B. Sbarufatti (INAF-OAB/PSU), P. D'Avanzo (INAF-OAB),
V. D'Elia (ASDC), J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU)
and K.L. Page report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 130803A (Page  et al. GCN
Circ. 15059),  from 75 s to 61.7 ks after the  BAT trigger. The data
comprise 7 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN. Circ
15062).

The late-time light curve (from T0+3.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.87 (+/-0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.40 (+0.24, -0.23). The
best-fitting absorption column is  8.7 (+1.6, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 4.2 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 4.5 x 10^-11 (1.3 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.7 (+1.6, -1.4) x 10^21 cm^-2
Galactic foreground: 4.2 x 10^20 cm^-2
Excess significance: 9.7 sigma
Photon index:      2.40 (+0.24, -0.23)

If the light curve continues to decay with a power-law decay index of
0.87, the count rate at T+24 hours will be 9.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-13 (1.2 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/00565263.

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


GRB_name: GRB130804A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15070
SUBJECT: GRB 130804A; Fermi GBM observation
DATE:    13/08/06 00:21:07 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 130804A: Fermi GBM observation

Hoi-Fung Yu (MPE), Adam Goldstein (ORAU/NASA MSFC) and Veronique Pelassa (UAH)
report on behalf of the Fermi GBM Team:

"At 00:33:15.53 UT on 04 August 2013, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 130804A (trigger 397269198 / 130804023).

High peak flux from the GRB caused GBM to issue a repoint request
that reoriented the satellite to place the GRB near the LAT boresight
for 2.5 hours, subject to Earth limb contraints.

The on-ground calculated location, using the GBM trigger data, is
RA = 280.0, DEC = -76.2 (J2000 degrees, equivalent to 18h 40m,
-76d 09'), with an uncertainty of 2.3 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 21 degrees.

The GBM light curve consists of two main pulses with sub-structures,
with a duration (T90) of about 0.96 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+1.024 s is
adequately fit by a Band function with Epeak = 545 +/- 110 keV,
alpha = -0.77 +/- 0.09, and beta = -2.22 +/- 0.31.

The event fluence (10-1000 keV) in this time interval is
(1.89 +/- 0.10)E-6 erg/cm^2. The 64 ms peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 42.0 +/- 1.7 ph/s/cm^2.

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


GRB_name: GRB130806A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15071
SUBJECT: GRB 130806A: Swift detection of a burst
DATE:    13/08/06 03:08:35 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.P. Gompertz (U Leicester), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC)
and C. A. Swenson (PSU) report on behalf of the Swift Team:

At 02:51:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130806A (trigger=565562).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 35.872, +67.530 which is 
   RA(J2000) = 02h 23m 29s
   Dec(J2000) = +67d 31' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 02:52:40.2 UT, 66.2 seconds after
the BAT trigger. Using promptly downlinked data we find a possible
X-ray source located at RA, Dec 35.92827, 67.53242 which is equivalent
to:
   RA(J2000)  = 02h 23m 42.8s
   Dec(J2000) = 67d 31' 56.7"
with an uncertainty of 9.0 arcseconds (radius, 90% containment). This
location is 78 arcseconds from the BAT onboard position, within the
BAT error circle. We cannot determine whether the source is
fading at the present time. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 68 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
1.19. 

Burst Advocate for this burst is B.P. Gompertz (bpg6 AT 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: GRB130806A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15072
SUBJECT: GRB 130806A: Enhanced Swift-XRT position
DATE:    13/08/06 10:10:23 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1580 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 130806A, 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 = 35.92894, +67.53196 which is equivalent
to:

RA (J2000): 02h 23m 42.95s
Dec (J2000): +67d 31' 55.1"

with an uncertainty of 2.2 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, MNRAS, 397, 1177).

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


GRB_name: GRB130803A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15073
SUBJECT: GRB130803A: GROND observations
DATE:    13/08/06 10:32:42 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

K. Varela (MPE Garching), M. Tanga (MPE Garching), P. Afonso (American
River College) and J. Greiner (MPE Garching) report on behalf of the
GROND team:

We observed a second epoch of the field of GRB 130803A (Swift trigger
565263; Page et al., GCN 15059) simultaneously in g'r'i'z'JHKs with GROND
(Greiner et al.2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope
at La Silla Observatory (Chile).

Observations started at 23:34 UT on August 5, about 61.7 hours after
the trigger at a mean seeing of 1.5 arcsec and a mean airmass of 1.3. We
confirm the detection of the source inside the enhanced 1.4'' XRT error
circle (Swift webpage) reported in a previous GCN (Varela et al.,
GCN15066),
and measure consistent magnitudes as compared to the first epoch
(the g'-band magnitude contained an error and should read g' = 24.6 +/- 0.4).
Thus, we consider this source as the potential host of GRB 130803A.


GRB_name: GRB130804A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15075
SUBJECT: IPN localization of GRB 130804A
DATE:    13/08/06 17:13:25 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,

K. Hurley on behalf of the IPN,

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

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on 
behalf of the AGILE MCAL team,  and

D. M. Smith, J. McTiernan, and W. Hajdas, on behalf of the RHESSI team, 
  report:

The short-duration, hard spectrum, intense GRB 130804A (Yu, Goldstein, 
and Pelassa , GCN Circ. 15070) was observed by Fermi (GBM), Suzaku 
(WAM), Swift (BAT), AGILE (MCAL), Konus-Wind, and RHESSI at about 1995 s 
UT (00:33:15.353). The burst was outside the coded field of view of the BAT.

We have triangulated this burst to a narrow Konus-GBM annulus centered 
at RA(2000)=324.539 deg (21h 38m 09s)  Dec(2000)=-9.265 deg (-9d 15' 
53"), whose radius is 71.038  0.041 deg (3 sigma) and to a wide GBM-WAM 
annulus centered at RA(2000)=RA(2000)=102.159 deg (06h 48m 38s) 
Dec(2000)=-31.166 deg (-31d 09' 56"), whose radius is 68.583  5.163 deg 
(3 sigma).

These annuli intersect to form a long arc, whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   303.653 (20h 14m 37s) -79.591 (-79d 35' 28")
  Corners:
   276.360 (18h 25m 26s) -75.021 (-75d 01' 15")
   275.920 (18h 23m 41s) -75.010 (-75d 00' 37")
   349.555 (23h 18m 13s) -79.299 (-79d 17' 56")
   349.905 (23h 19m 37s) -79.175 (-79d 10' 29")
  ---------------------------------------------
The arc area is 1.29 sq. arcmin, and its maximum
dimension is 15.8 deg (the minimum one is 2.9 arcmin).
The Sun distance was ~117 deg.


The center of the GBM location (Yu, Goldstein, and Pelassa , GCN Circ. 
15070) is 5.9 deg from the center of the IPN arc.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130804_T01995/IPN/


GRB_name: GRB130806A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15076
SUBJECT: GRB 130806A, Swift-BAT refined analysis
DATE:    13/08/06 22:31:21 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), B.P. Gompertz (U Leicester), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (MSU) (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 130806A (trigger #565562)
(Gompertz, et al., GCN Circ. 15071).  The BAT ground-calculated position is
RA, Dec = 35.907, 67.525 deg which is
     RA(J2000)  =  02h 23m 37.7s
     Dec(J2000) = +67d 31' 30.5"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.

The mask-weighted light curves shows a faint initial 2-sec long peak
starting at T-5 sec, followed by the main peak from T-1 to T+2 sec.
T90 (15-350 keV) is 6.1 +- 0.5 sec (estimated error including systematics).

The time-averaged spectrum from T-4.5 to T+2.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.50 +- 0.22.  The fluence in the 15-150 keV band is 1.7 +- 0.2 x 10^-07
erg/cm2. The 1-sec peak photon flux measured from T+0.32 sec in the 15-150 keV
band is 1.3 +- 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/565562/BA/

We note that the fluence ratio in a simple power-law fit between the
25-50 keV band and the 50-100 keV band is 1.41.  This fluence ratio is larger
than 1.32 which can be achieved in the Band function of alpha=-1.0, beta=-2.5,
and Epeak=30 keV.  Thus, preliminary analysis shows that Epeak of the burst
is very likely around or below 30 keV.  Therefore the burst can be classified
as an X-ray flash (e.g. Sakamoto et al. 2008, ApJ, 679, 570).  A fit to a Band
model gives nearly the same reduced chi-squared as a simple power=law fit.  The
Band fit gives Epeak = 18.9 (+3.2, -5.8) and beta = -2.6  0.3.  The alpha
parameter is not constrained by the fit.


GRB_name: GRB130806A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15077
SUBJECT: GRB 130806A: MITSuME Okayama upper limits
DATE:    13/08/07 04:33:15 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME collaboration:

We observed the field of GRB 130806A (Gompertz et al., GCNC 15071)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2013-08-06 12:29:43 UT (~9.6 h after the burst).
We did not find any new point source within the enhanced XRT error circle
(Beardmore et al., GCNC 15072) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.54100    15:50:36    4020.0   >19.4  >19.5  >18.7
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130806A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15078
SUBJECT: GRB 130806A: Swift-XRT refined Analysis
DATE:    13/08/07 05:26:22 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and B.P. Gompertz (U Leicester) report on
behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 130806A (Gompertz  et al.
GCN Circ. 15071),  from 77 s to 57.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN. Circ
15072).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.57 (+0.08, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+0.6, -0.5). The
best-fitting absorption column is  6.8 (+4.7, -2.9) x 10^21 cm^-2,
consistent with the Galactic value of 3.9 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 6.1 x 10^-11 (9.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.8 (+4.7, -2.9) x 10^21 cm^-2
Galactic foreground: 3.9 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.6 (+0.6, -0.5)

If the light curve continues to decay with a power-law decay index of
0.57, the count rate at T+24 hours will be 2.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.5 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/00565562.

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


GRB_name: GRB130806A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15079
SUBJECT: GRB 130806A: MITSuME Akeno Optical observation
DATE:    13/08/07 06:31:51 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T. Yoshii, K. Ito, Y. Saito, Y. Yano, R. Usui, Y. Tachibana, 
S. Kurita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130806A (B.P. Gompertz et al., GCNC 15071) with the 
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2013-08-06 14:11:23 UT ( ~11.3 h afterthe burst).
And we could not find any new point source within the XRT
error circle (A.P. Beardmore et al., GCNC 15072) in all the three bands.

The results of photometry (3 sigma upper limits) are listed below.
We used GSC2.3 catalog for flux calibration.


T0+[hour]      MID-UT        T-EXP[sec]           g'                Rc                Ic
----------------------------------------------------------------------------------------------------
   ~15.0         17:50:01          5580               >21.3         >20.4           >19.7
----------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [hour]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15080
SUBJECT: GRB 130623A: GROND detection of the optical/NIR afterglow
DATE:    13/08/07 08:35:34 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

K. Varela (MPE Garching), A.C. Updike (Roger Williams University),
J. Elliott (MPE Garching), J. Greiner (MPE Garching) and
D.A. Kann (TLS Tautenburg) report on behalf of the GROND team:

We observed the field of GRB 130623A (Cummings et al., GCN #14921)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

The first epoch observation started at 09:15 UT on 25 June 2013,
33.7 hrs after the GRB trigger. They were performed at an average
seeing of 1."5 and at an average airmass of 1.6. We find a single
point source at the edge of the 4."5 Swift-XRT error circle reported
by Grupe et al. (GCN #14926) at

RA  (J2000) = 01:23:26.17 = 20.859063
DEC (J2000) = -77:46:24.0 = -77.773361

with an uncertainty of 0.3" in each coordinate.

Based on a total exposure of 50 minutes in g'r'i'z' and 40 minutes in JHK,
we estimate preliminary magnitudes (all in AB) of

g' = 22.5 +/- 0.1 mag,
r' = 22.4 +/- 0.1 mag,
i' = 22.2 +/- 0.1 mag,
z' = 21.9 +/- 0.1 mag,
J = 21.3 +/- 0.3 mag,
H = 20.5 +/- 0.3 mag, and
K > 20.2 mag.

The second epoch observations started at 08:29 UT on 05 August 2013,
42 days after the GRB trigger. They were performed at an average seeing of
1."3 and at an average airmass of 1.5. The source found in the first epoch
is not detected anymore: Based on a total exposure of 75 minutes in g'r'i'z'
and 60 minutes in JHK, we estimate preliminary upper limits (all in AB) of

g'  > 25.7
r'  > 25.2
i'  > 24.3
z'  > 24.0
J  > 21.8
H  > 20.9
Ks > 20.4

The fading by nearly 3 mag in the r'-band  proves it to have been the
afterglow of GRB 130623A. The clear detection down to the g'-band
implies a redshift smaller than 3.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.05 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130804A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15081
SUBJECT: Konus-Wind observation of GRB 130804A
DATE:    13/08/07 10:41:35 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The bright, short-duration GRB 130804A
(Fermi-GBM detection: Yu, Goldstein, and Pelassa, GCN 15070;
IPN triangulation: Golenetskii at al., GCN 15075)
triggered Konus-Wind at T0=1997.053 s UT (00:33:17.053).

The burst light curve from ~T0-0.2 s to ~T0+1 s shows three major pulses
with the brightest, hard-spectrum pulse peaked at ~T0.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130804_T01997/

As observed by Konus-Wind, the burst
had a fluence of (1.8  0.2)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0,
of (3.4  0.3)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The 3-channel time-integrated spectrum
(measured from T0-0.256 to T0+1.024 s)
can be modeled, in the 25 keV - 1.5 MeV range,
by the cutoff power law with the following model parameters:
the photon index alpha = -0.94  0.06,
and the peak energy Ep = 434  37 keV.

All the quoted results are preliminary.


GRB_name: GRB130807A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15082
SUBJECT: GRB 130807A: Swift detection of a GRB or Galactic transient
DATE:    13/08/07 10:50:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), D. N. Burrows (PSU),
P. A. Evans (U Leicester), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and R. L. C. Starling (U Leicester)
report on behalf of the Swift Team:

At 10:25:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130807A (trigger=565651).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 269.801, -27.613 which is 
   RA(J2000) = 17h 59m 12s
   Dec(J2000) = -27d 36' 44"
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 at least 30 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 10:27:08.2 UT, 85.0 seconds after
the BAT trigger. Although a bright and variable source is apparent 
in the promptly downloaded light curve, the instrument did not
centroid on the source in the initial 2.5-s promptly downloaded
image, and the XRT stayed in WT mode for the remainder of the 
short first snapshot until Swift slewed away from the target. 
We therefore will have to wait until the second orbit to 
localize the XRT counterpart. 

UVOT took a finding chart exposure of 166 seconds with the U filter starting
145 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. Because of the density of catalogued stars, further analysis
is required to report an upper limit for any afterglow in the sub-image. The
8'x8' region for the list of sources generated on-board covers 100% of the BAT
error circle. Because of the density of catalogued stars, further analysis is
required to report an upper limit for any afterglow in the region. No
correction has been made for the large, but uncertain extinction expected. 

Due to the proximity of this source to the Galactic center 
(3.3 degrees from the center) it is more likely that this is a 
Galactic source rather than a cosmological GRB.  Determination
of the nature of this source will require the full downlinked data. 

Burst Advocate for this burst is A. Melandri (andrea.melandri 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: GRB130807A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15083
SUBJECT: GRB 130807A, Swift-BAT refined analysis
DATE:    13/08/08 14:35:14 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (MSU) (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 130807A (trigger #565651)
(Melandri, et al., GCN Circ. 15082).  The BAT ground-calculated position is
RA, Dec = 269.801, -27.616 deg, which is
    RA(J2000)  =  17h 59m 12.4s
    Dec(J2000) = -27d 36' 56.7"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.

Based on the currently available event data, the mask-weighted light 
curve shows an initial FRED-like peak starting at T-10 sec, peaking at 
T=0 sec and decaying to background by T+50 sec.  This is followed by at 
least two more weaker peaks, one from roughly T+90 sec to T+130 sec and 
the second beginning at T+160 sec and continuing until the data cuts off 
at T+243 seconds.  The two later peaks are coincident with flares seen 
in the Swift/XRT data.  We note also that the Swift satellite slewed 
away from the source location at ~T+300 seconds, while an XRT flare was 
still ongoing. Since we do not have all of the data, we cannot determine 
T90 at this time.

The time-averaged spectrum from T-12.18 to T+163.82 sec is best fit by a 
power law with an exponential cutoff.  This fit gives a photon index 
0.31 +- 0.89,
and Epeak of 75.9 +- 35.2 keV (chi squared 56.96 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-06 
erg/cm2
and the 1-sec peak flux measured from T-4.68 sec in the 15-150 keV band is
0.4 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.46 +- 0.17 (chi squared 63.40 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level.

The current analysis of the BAT data does not allow us to distinguish 
between the interpretations of this event as either a GRB or galactic 
transient. These results will be updated as more event data becomes 
available.

Examination of archival images from the Swift/BAT transient monitor 
through 3:03 UT, August 6, 2013 (~31.5 hours before the trigger) shows 
no sign of earlier emission from the location of trigger 565651.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/565651/BA/


GRB_name: GRB130806A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15084
SUBJECT: GRB 130806A: Swift/UVOT Upper Limits
DATE:    13/08/08 14:49:32 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and B. P. Gompertz (U Leicester) report on
behalf of the Swift/UVOT team:

    The Swift/UVOT began settled observations of the field of GRB
130806A starting 69 s after the BAT trigger (Gompertz et al. 2013,
GCNC 15071).  We do not detect any new source consistent with the
UVOT-enhanced XRT position (Beardmore et al. 2013, GCNC 15072) in any
of the UVOT exposures.  Preliminary 3-sigma upper limits using the
UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358,
373) for the finding chart (FC) exposures and initial summed exposures
are presented below.

-------------------------------------------------
Filter      TSTART      TSTOP   Exposure      Mag
-------------------------------------------------
white (FC)      69        218        147    >20.6
   u (FC)     282        305         23    >18.2
-------------------------------------------------
   b         3571     11,831       1028    >21.3           
   u         4801     11,172       1082    >21.4
   v         4187       5823        393    >19.9
uvw1         4597     10,259       1116    >21.2
uvm2         4391     15,843       1066    >20.9
uvw2         3982       5618        393    >20.7
white         3776       5411        393    >21.8
-------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 1.02 mag (Schlafly et al. 2011, ApJS, 737,
103).  GRB 130806A was 6 degrees above the Galactic Plane, so this
extinction value is highly uncertain.


GRB_name: GRB130807A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15085
SUBJECT: GRB 130807A: Swift-XRT refined analysis
DATE:    13/08/08 19:48:08 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF/OAB), D.N. Burrows (PSU), P. Romano (INAF-IASFPA),  
H.A. Krimm (GSFC/USRA), J.P. Osborne, P.A. Evans (U. Leicester), N.  
Gehrels (GSFC) report on behalf of the Swift team.


We have analysed 14.4 ks of XRT data for GRB 130807A (Melandri et al.  
GCN Circ. 15082), from 88 s to 80 ks after the  BAT trigger. The XRT  
position for this burst is RA, Dec = 269.8007, -27.6159 which is  
equivalent to:

RA (J2000): 17h 59m 12.16s
Dec (J2000): -27d 36' 57.5"

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

In the first orbit (WT mode) the source is initially detected at a  
rate of ~10 XRT count/s, rising to ~100 c/s at the end of the first  
orbit. During this period the spectrum can be fit by an absorbed power- 
law model with a photon index of 1.56 +/- 0.08. The source showed an  
absorption column of (8.6 +/- 1.0) x 10^21 cm^-2, slightly in excess  
with respect to the Galactic value of 6 x 10^21 cm^-2 (Kalberla et al.  
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion  
factor deduced from this spectrum  is 8.0 x 10^-11 (1.2 x 10^-10) erg  
cm^-2 count^-1.

In the second orbit (PC mode) the source had become much fainter  
(~0.03 c/s), and much softer, with a photon index of 2.3 (+0.5,  
-0.4).The source still showed an absorption column (9.0 +/- 5.0 x  
10^21 cm^-2) consistent with the Galactic value. The counts to  
observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from  
this spectrum  is 5.0 x 10^-11 (1.7 x 10^-10) erg cm^-2 count^-1.  
Starting with the second orbit, the light curve rose from a count rate  
of ~0.015 c/s after ~4 ks to a maximum of ~0.06 c/s at ~10 ks (with  
slope of -1.5 +/- 0.1). After that it decayed with a slope of 0.9 +/-  
0.1, reaching the count rate of ~0.012 c/s at ~75 ks.

The light curve behaviour (at late times) is unusual, but not  
unprecedented, for a GRB. The BAT and XRT spectral indices are similar  
to those observed for GRB 060124 (BAT spectrum gamma = 1.89 +/- 0.19,  
XRT-WT spectrum gamma = 1.40+/-0.01, XRT-PC spectrum gamma =  
2.1+/-0.1; Romano et al., 2006, A&A, 456, 917) and for the transient  
supermassive black hole Swift J1644+57 (Burrows et al., 2011, Nature,  
476, 421), but inconsistent with what generally observed for a  
Supergiant Fast X-ray Transient. The dynamical range of GRB 130807A  
(~3300) is similar to what observed for GRB 060124 or for a typical  
SFXT, but very different from what was observed for Swift J1644+57.

The source was not detected in the BAT transient monitor (15-50 keV)  
before 3:03 UT, August 6, 2013, the most recent monitor epoch  
currently available. Events like Swift J1644+57 or SFXTs are usually  
detected in X-rays for several days before the trigger, Swift J1644+57  
behaved similarly. It is therefore likely that BAT trigger 565651 was  
a somewhat unusual GRB rather than a Galactic or extragalactic  
transient, in spite of its proximity to the Galactic center.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/possible_GRBs/00565651/source1


GRB_name: GRB130807A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15086
SUBJECT: GRB130807A: Swift/UVOT observations
DATE:    13/08/08 19:53:04 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130807A
145 s after the BAT trigger (Melandri et al., GCN Circ. 15082).
No optical source consistent with the XRT position (Melandri et al.,
GCN Circ. 15085) is detected in the UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric
system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent summed exposures are:

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

white_FC          3572         3722          147         >20.3
white             3572         5573          541         >21.1
v                 4348         5984          393         >19.3
b                 3732         5369          393         >20.3
u_FC               145          311          163         >19.7
u                  145         5164          360         >19.9
w1                4759         4959          197         >19.6
m2                4552         6078          284         >19.7
w2                4143         5780          393         >20.2

The magnitudes in the table are not corrected for the strong Galactic
extinction corresponing to the reddening of E(B-V) = 2.03 in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130807A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15087
SUBJECT: Correction to GCN Circ. 15086 "GRB130807A: Swift/UVOT observations"
DATE:    13/08/08 20:08:00 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) reports on behalf of the Swift/UVOT team:

In the previous GCN Circ. 15086 "GRB130807A: Swift/UVOT observations",
the sentence "No optical source" should be changed into "No uncatalogued
optical source".

I apologize for the mistake.


GRB_name: GRB130812A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15088
SUBJECT: GRB 130812A: Swift detection of a burst
DATE:    13/08/12 22:38:46 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
V. Mangano (PSU), C. B. Markwardt (NASA/GSFC) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 22:22:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130812A (trigger=566228).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 92.402, -13.295 which is 
   RA(J2000)  =  06h 09m 37s
   Dec(J2000) = -13d 17' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of about 10 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:24:09.6 UT, 77.0 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 92.3955,
-13.2875 which is equivalent to:
   RA(J2000)  = 06h 09m 34.92s
   Dec(J2000) = -13d 17' 15.1"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 35 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 (1.51 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.5
(+1.52/-1.37) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
138 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 19.2 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
0.23. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.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: GRB130812A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15089
SUBJECT: GRB 130812A: Enhanced Swift-XRT position
DATE:    13/08/13 08:46:24 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2469 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130812A, 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 = 92.39590, -13.28816 which is equivalent
to:

RA (J2000): 06h 09m 35.02s
Dec (J2000): -13d 17' 17.4"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130812A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15090
SUBJECT: GRB 130812A: Swift-XRT refined Analysis
DATE:    13/08/13 10:39:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), P. D'Avanzo
(INAF-OAB), A. Maselli (INAF-IASFPA), V. Mangano (PSU), M.C. Stroh
(PSU), D.N. Burrows (PSU), J.P. Osborne (U. Leicester) and V. D'Elia
report on behalf of the Swift-XRT team:

We have analysed 8.9 ks of XRT data for GRB 130812A (D'Elia  et al. GCN
Circ. 15088),  from 62 s to 22.3 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Evans et al. (GCN. Circ
15089).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.86 (+/-0.03).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+0.17, -0.16). The
best-fitting absorption column is  3.0 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.1 x 10^-11 (6.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.0 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 4.3 sigma
Photon index:      2.04 (+0.17, -0.16)

If the light curve continues to decay with a power-law decay index of
0.86, the count rate at T+24 hours will be 7.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.9 x
10^-13 (4.6 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/00566228.

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


GRB_name: GRB130812A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15091
SUBJECT: GRB 130812A: GROND upper limits
DATE:    13/08/13 13:19:03 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

K. Varela (MPE Garching), D.A. Kann (TLS Tautenburg), J. Greiner 
(MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 130812A (Swift trigger 566228; 
D'Elia et al. 2013, GCN #15088) simultaneously in g'r'i'z'JHK with 
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 
2.2 m MPG/ESO telescope at La Silla Observatory (Chile).

Observations started at 10:13 UT on 13 Aug. 2013, 11.8 hrs after the 
GRB trigger. They were performed at an average seeing of 2.5" and at 
an average airmass of 1.4.

In 212 sec exposure in g'r'i'z' and 360 sec exposure in JHK 
we do not detect a source within the 1.8 arcsec Swift-XRT error 
circle reported by Evans et al. (2013; GCN #15089) down to
(all in the AB system)

g' > 22.4,

r' > 22.6,

i' > 21.9,

z' > 21.7,

J > 20.3,

H > 19.4 and

K > 18.8

The given limits are derived based on calibrating the images against 
GROND zeropoints and 2MASS field stars and are not corrected for the 
Galactic foreground extinction corresponding to a reddening of 
E_(B-V)= 0.23 in the direction of the burst (Schlegel et al. 1998). 


GRB_name: GRB130812A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15092
SUBJECT: GRB 130812A, Swift-BAT refined analysis
DATE:    13/08/13 16:12:20 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-144 to T+431 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130812A (trigger #566228)
(D'Elia, et al., GCN Circ. 15088).  The BAT ground-calculated position is
RA, Dec = 92.387, -13.285 deg which is 
  RA(J2000)  =  06h 09m 32.8s 
  Dec(J2000) = -13d 17' 06.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows multiple spikes peaking at T0, T0+4 sec and T0+7 sec.  
T90 (15-350 keV) is 7.6 +- 0.5 sec (estimated error including systematics).

The time-averaged spectrum from T-0.3 to T+8.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.52 +- 0.11.  The fluence in the 15-150 keV band is 5.9 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.14 sec in the 15-150 keV band
is 2.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis will be available at
http://gcn.gsfc.nasa.gov/notices_s/566228/BA/


GRB_name: GRB130812A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15093
SUBJECT: GRB 130812A: Swift/UVOT Upper Limits
DATE:    13/08/13 16:15:52 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and V. D'Elia (ASDC) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130812A 
139 s after the BAT trigger (D'Elia et al., GCN Circ. 15088).
No optical afterglow consistent with the XRT position (Evans et al. GCN 
Circ. 15089) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding 
chart (FC) exposure and subsequent exposures are:

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

u_FC               139          389          246         >20.3
v                  445        12868         1191         >20.5
b                  394        11236         1459         >21.7
u                  139         7030          884         >20.8
w1                 494         6825          491         >20.5
m2                 469         6619          452         >20.3
w2                 421        12142         1376         >21.3

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.23 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130812B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15094
SUBJECT: IPN Triangulation of GRB 130812B (long/soft)
DATE:    13/08/13 16:40:43 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

IPN Triangulation of GRB 130812B (long/bright)

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,

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

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

The long-duration, soft spectrum, intense GRB 130812B has been observed 
by Konus-Wind, Suzaku (WAM), MESSENGER (GRNS), and Swift (BAT), so far, 
at about 39315 s UT (10:55:15). The burst was outside the coded field of 
view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
     7.671 (00h 30m 41s) -79.083 (-79d 04' 59")
  Corners:
     1.389 (00h 05m 33s) -80.672 (-80d 40' 18")
     3.895 (00h 15m 35s) -80.482 (-80d 28' 56")
    12.167 (00h 48m 40s) -77.409 (-77d 24' 32")
    10.472 (00h 41m 53s) -77.656 (-77d 39' 21")
  ---------------------------------------------
The error box area is 2954 sq. arcmin, and its maximum
dimension is 3.8 deg (the minimum one is 14 arcmin).
The Sun distance was 112 deg.

This box can be improved.

The time history and spectrum will be given in a forthcoming GCN Circular.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130812_T39316/IPN/


GRB_name: GRB130812B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15095
SUBJECT: Konus-Wind observation of GRB 130812B
DATE:    13/08/13 16:53:48 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration - GRB 130812B
(IPN triangulation: Hurley at al., GCN 15094)
triggered Konus-Wind at T0=39316.109 s UT (10:55:16.109).

The light curve shows multiple pulses from ~T0-0.5 s to ~T0+16s
followed by a weak decaying emission during the next ~15 s.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130812_T39316/

As observed by Konus-Wind, the burst
had a fluence of (1.52  0.03)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.032s,
of (3.5  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+33.024 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.33  0.07,
the peak energy Ep = 78  3 keV,
chi2 = 90/98 dof.

The time-averaged spectrum of the bright phase of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.04  0.07,
the peak energy Ep = 90  2 keV,
chi2 = 75/97 dof.

All the quoted results are preliminary.


GRB_name: GRB130812B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15096
SUBJECT: Refined IPN Triangulation of GRB 130812B
DATE:    13/08/14 18:16:03 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,

J. Goldsten, on behalf of the MESSENGER NS GRB team,

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

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

GRB 130812B (Hurley et al., GCN 15094; Golenetskii et al., GCN 15095) 
was also observed by Odyssey. Using Odyssey data reduces the size of the 
previous error box by about a factor of eight:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
     7.405 (00h 29m 37s) -79.178 (-79d 10' 39")
  Corners:
     8.180 (00h 32m 43s) -78.635 (-78d 38' 07")
     7.610 (00h 30m 26s) -79.359 (-79d 21' 32")
     6.536 (00h 26m 09s) -79.717 (-79d 43' 02")
     7.206 (00h 28m 49s) -78.996 (-78d 59' 47")
  ---------------------------------------------
The area of this box is  349 sq. arcmin, and its maximum
dimension is 1.1 deg (the minimum one is 8 arcmin).

A new map has been posted at
http://www.ioffe.ru/LEA/GRBs/GRB130812_T39316/IPN/

Some improvement in this error box is possible.


GRB_name: GRB130816A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15097
SUBJECT: GRB 130816A: Swift detection of a burst
DATE:    13/08/16 02:10:37 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. T. Holland (STScI), P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), D. Malesani (DARK/NBI), V. Mangano (PSU),
C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU/NASA/GSFC) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:

At 01:46:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130816A (trigger=566545).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 197.167, -58.948 which is 
   RA(J2000) = 13h 08m 40s
   Dec(J2000) = -58d 56' 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 10 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:48:23.2 UT, 87.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 197.1399, -58.9452
which is equivalent to:
   RA(J2000)  = 13h 08m 33.59s
   Dec(J2000) = -58d 56' 42.6"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 51 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 (3.87 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4
(+4.03/-3.22) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 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. 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 large, but uncertain extinction expected. The
crowded field also makes the identification of a new source more difficult. 

Burst Advocate for this burst is S. T. Holland (sholland AT stsci.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: GRB130816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15098
SUBJECT: GRB 130816A: REM NIR candidate afterglow
DATE:    13/08/16 02:53:17 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, D. FUgazza, V. D'Elia report on behalf of the REM team:

We observed the field of GRB 130816A (Holland et al., GCN 15097) simultaneously in the optical and near-infrared with the the 60-cm robotic telescope REM at La Silla Observatory (Chile). The observations started at 01:47:56 UT, about 1 min after the GRB.

We detect a faint source compatible with the XRT position and not present in the 2MASS catalogue with coordinates:

RA (J2000) = 13:08:33.80
DEC (J2000) = -58:56:41.2

with an estimated uncertainty of +- 0.5 arcsec.
Preliminary photometry indicates that the sources was at H = 15.0 +- 0.20 (Vega) about 100 s after the burst. 

Further observations are in progress to assess its variability.


GRB_name: GRB130816B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15099
SUBJECT: GRB 130816B: Swift detection of a burst
DATE:    13/08/16 05:06:44 GMT
FROM:    Michael Stamatikos at OSU/GSFC  <michael.stamatikos-1@nasa.gov>

M. Stamatikos (OSU/NASA/GSFC), P. D'Avanzo (INAF-OAB),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 04:53:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130816B (trigger=566561).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 170.093, -57.558 which is 
   RA(J2000) = 11h 20m 22s
   Dec(J2000) = -57d 33' 28"
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 20 sec.  The peak count rate
was ~2440 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:54:48.8 UT, 70.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 170.01845, -57.55829 which is
equivalent to:
   RA(J2000)  = 11h 20m 04.43s
   Dec(J2000) = -57d 33' 29.8"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 143 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.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.04
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 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 none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. Because of the density of
catalogued stars, further analysis is required to report an upper limit for any
afterglow in the region. No correction has been made for the large, but
uncertain extinction expected. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 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: GRB130816A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15100
SUBJECT: GRB 130816A: Enhanced Swift-XRT position
DATE:    13/08/16 10:12:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1820 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130816A, 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 = 197.14081, -58.94476 which is equivalent
to:

RA (J2000): 13h 08m 33.79s
Dec (J2000): -58d 56' 41.1"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130816A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15101
SUBJECT: GRB 130816A: GROND confirmation of afterglow
DATE:    13/08/16 10:39:08 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

K. Varela (MPE Garching), D.A. Kann, S. Klose (both TLS Tautenburg), 
J. Elliott and J. Greiner (both MPE Garching) report on behalf of 
the GROND team:
  
We observed the field of GRB 130816A (Holland et al., GCN #15097)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory 
(Chile). 
  
Observations started at 01:49 UT on 16 August 2013, 3 min after the GRB
trigger. We confirm the presence of the NIR source inside the 2.2 arcsec
Swift-XRT error circle (Holland et al.) found by Covino et al. 
(GCN 15098).
  
Based on the first 140 sec g'r'i'z and 240 sec JHK exposure,
we estimate preliminary magnitudes (all in AB) of      
  
g' = 21.8 +/- 0.2 mag,
r' = 20.3 +/- 0.1 mag,
i' = 19.5 +/- 0.1 mag,         
z' = 18.9 +/- 0.1 mag,         
J = 18.0 +/- 0.1 mag,
H = 17.4 +/- 0.1 mag, and      
K = 17.1 +/- 0.1 mag,
  
calibrated against GROND zero points (g'r'i'z') and 2MASS (JHK).
Correcting for the Galactic foreground extinction corresponding to 
a reddening of E_(B-V)= 0.80 in the direction of the burst 
(Schlegel et al. 1998), the SED is well fit with a powerlaw of
slope 0.8, typical of GRB afterglows.

The object rapidly faded (by about 1.5 mag) during the following 
40 min., leaving no doubt that this is the afterglow of GRB 130816A.


GRB_name: GRB130816B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15102
SUBJECT: GRB 130816B: Enhanced Swift-XRT position
DATE:    13/08/16 12:58:00 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1915 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130816B, 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 = 170.01621, -57.55740 which is equivalent
to:

RA (J2000): 11h 20m 3.89s
Dec (J2000): -57d 33' 26.7"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130816B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15103
SUBJECT: GRB 130816B: Swift-XRT refined Analysis
DATE:    13/08/16 17:06:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B.P. Gompertz (U. Leicester), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA), A. Melandri (INAF-OAB), M.C. Stroh (PSU), D.N. Burrows
(PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester) and M. Stamatikos report on behalf of the Swift-XRT team:

We have analysed 7.7 ks of XRT data for GRB 130816B (Stamatikos  et al.
GCN Circ. 15099),  from 77 s to 24.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN. Circ 15102).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.98 (+0.13, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+0.5, -0.4). The
best-fitting absorption column is  5.3 (+2.8, -1.3) x 10^21 cm^-2,
consistent with the Galactic value of 4.0 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.6 x 10^-11 (8.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.3 (+2.8, -1.3) x 10^21 cm^-2
Galactic foreground: 4.0 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.1 (+0.5, -0.4)

If the light curve continues to decay with a power-law decay index of
0.98, the count rate at T+24 hours will be 5.8 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x
10^-14 (4.9 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00566561.

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


GRB_name: GRB130816A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15104
SUBJECT: GRB 130816A: Fermi GBM observation
DATE:    13/08/16 21:10:16 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) and G. Younes (NASA/USRA)
report on behalf of the Fermi GBM Team:

At 01:46:28.52 UT on 16 August 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located the precursor to GRB130816A (trigger
398310391/130816074)
which was detected by the Swift/BAT (Holland et al. 15097, GCN 14527).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of the precursor and the main pulse
with a duration (T90) of about 32  s (50-300 keV).
The time-averaged spectrum from T0+23 s to T0+32 s is
adequately fit by a simple power law function with index -1.83 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(1.3 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+27 s in the 10-1000 keV band is 1.9 +/- 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: GRB130816A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15105
SUBJECT: GRB 130816A, Swift-BAT refined analysis
DATE:    13/08/17 00:56:28 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), S. T. Holland (STScI),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130816A (trigger #566545)
(Holland , et al., GCN Circ. 15097). The BAT
ground-calculated position is
RA, Dec = 197.093, -58.996 deg which is
   RA(J2000)  =  13h 08m 22.3s
   Dec(J2000) = -58d 59' 46.8"
with an uncertainty of 2.6 arcmin, (radius, sys+stat,
90% containment). The partial coding was 35%.

BAT mask-weighted light curve shows a two-peak structure.
The first peak starts around T-28 sec and lasts for about
5 sec. The second peak starts around T-3 sec and ends
around T+3 sec. BAT triggered on the second peak
and the first peak may be considered as a precursor
to the burst. T90 (15-350 keV) is 29.97 +- 1.36 sec
(estimated error including systematics).

The time-averaged spectrum from T-28.06 to T+2.56 sec
is best fit by a simple power-law model.  The power
law index of the time-averaged spectrum is
1.86 +- 0.34.  The fluence in the 15-150 keV band
is 4.3 +- 1.0 x 10^-07 erg/cm2. The 1-sec peak photon
flux measured from T-0.04 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/566545/BA/


GRB_name: GRB130816A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15106
SUBJECT: GRB 130816A: Swift-XRT refined Analysis
DATE:    13/08/17 02:10:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), V. Mangano
(PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani
(U. Leicester) and S.T. Holland report on behalf of the Swift-XRT team:

We have analysed 2.8 ks of XRT data for GRB 130816A (Holland  et al.
GCN Circ. 15097),  from 99 s to 11.2 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN. Circ 15100).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.62 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.3). The
best-fitting absorption column is  6.2 (+2.0, -1.7) x 10^21 cm^-2, in
excess of the Galactic value of 3.9 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.7 x 10^-11 (9.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.2 (+2.0, -1.7) x 10^21 cm^-2
Galactic foreground: 3.9 x 10^21 cm^-2
Excess significance: 2.3 sigma
Photon index:      2.1 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
0.62, the count rate at T+24 hours will be 7.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.7 x
10^-13 (7.1 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/00566545.

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


GRB_name: GRB130816B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15107
SUBJECT: GRB 130816B: GROND afterglow candidate
DATE:    13/08/17 08:19:40 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

K. Varela (MPE Garching), S. Klose (TLS Tautenburg)
and J. Greiner (both MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 130816B (Stamatikos et al., GCN #15099)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory
(Chile).

Observations started at 23:12 UT on 16 August 2013, 18.3 hours after the
GRB trigger. They were performed at an average seeing of 1.6" and at and
average airmass of 2.20. We find a source inside the 1.9" Swift-XRT error
circle (Osborne et al., GCN #15102) at coordinates

RA(J2000) = 11:20:03.96
DEC (J200.0) = -57:33:27.1

with an uncertainty of 0.5" in each coordinate.

Based on the first 460 sec g'r'i'z and 480 sec JHK exposure,
we estimate preliminary magnitudes (all in AB) of

g' > 23.5 mag
r' = 23.1 +/- 0.2 mag,
i' = 22.5 +/- 0.2 mag,
z' = 21.6 +/- 0.1 mag,
J = 20.5 +/- 0.3 mag,
H = 20.5 +/- 0.3 mag,
K = 19.9 +/- 0.4 mag,

calibrated against GROND zero points (griz) and 2MASS (JHK) and
are not corrected for the Galactic foreground extinction corresponding to
a reddening of E_(B-V)= 0.56 mag in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130816B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15108
SUBJECT: GRB 130816B, Swift-BAT refined analysis
DATE:    13/08/17 16:08:14 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

M. Stamatikos (OSU), 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),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
G. Sato (ISAS), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+963 sec from
the recent telemetry downlink, we report further
analysis of BAT GRB 130816B (trigger #566561)
(Stamatikos, et al., GCN Circ. 15099). The BAT
ground-calculated position is
RA, Dec = 170.049, -57.527 deg which is
   RA(J2000)  =  11h 20m 11.8s
   Dec(J2000) = -57d 31' 37.7"
with an uncertainty of 1.6 arcmin, (radius,
sys+stat, 90% containment).The partial
coding was 98%.

BAT mask-weighted light curve shows a single peak
starting from ~T-10 sec peaking around T+0 sec
and ending at ~T+4 sec. T90 (15-350 keV) is
10.00 +- 3.61 sec (estimated error including
systematics).

The time-averaged spectrum from T-6.50 to T+6.50 sec
is best fit by a power law with an exponential cutoff.
This fit gives a photon index 0.45 +- 0.93, and
Epeak of 47.3 +- 10.8 keV (chi squared 35.98 for
56 d.o.f.). For this model the total fluence in
the 15-150 keV band is 2.7 +- 0.4 x 10^-07 erg/cm2
and the 1-sec peak flux measured from T+0.50 sec
in the 15-150 keV band is 0.9 +- 0.1 ph/cm2/sec.
A fit to a simple power law gives a photon index
of 1.82 +- 0.17 (chi squared 44.98 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/566561/BA/


GRB_name: GRB130816B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15110
SUBJECT: GRB 130816B: Swift/UVOT Upper Limits 
DATE:    13/08/19 19:48:10 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

     The Swift/UVOT began settled observations of the field of GRB
130816B starting 75 s after the BAT trigger (Stamatikos et al. 2013,
GCNC 15099).  We do not detect any new source consistent with the
GROND afterglow position (Varela et al. 2013, GCNC 15107) in any of
the UVOT exposures.  Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for the finding chart (FC) exposures and initial summed exposures are
presented below.

---------------------------------------------------
Filter       TSTART      TSTOP    Exposure      Mag
---------------------------------------------------
white (FC)       75        225         147    >20.7
    u (FC)      287        537         246    >19.9
---------------------------------------------------
    v           618     12,639        1295    >20.4
    b           543       7299         530    >20.7
    u           692     19,298         923    >20.5
 uvw1           667     18,676        1238    >20.8
 uvm2           642     13,534        1227    >20.8
 uvw2           593     24,128         882    >20.7
white           567       7498         672    >21.5
---------------------------------------------------

     The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.50 mag (Schlafly et al. 2011, ApJS, 737,
103).  GRB 130816B was 3 degrees above the Galactic Plane, so this
extinction value is highly uncertain.


GRB_name: GRB130816A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15111
SUBJECT: GRB 130816A: Swift/UVOT Upper Limits
DATE:    13/08/19 19:49:29 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) reports on behalf of the Swift/UVOT team:

     The Swift/UVOT began settled observations of the field of GRB
130816A starting 91 s after the BAT trigger (Holland et al. 2013, GCNC
15097).  We do not detect any new source consistent with the REM
afterglow position (Covino et al. 2013, GCNC 15098) in any of the UVOT
exposures.  Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for the finding chart (FC) exposures and initial summed exposures are
presented below.

---------------------------------------------------
Filter       TSTART      TSTOP    Exposure      Mag
---------------------------------------------------
white (FC)       91        241         147    >20.8
    u (FC)      303        554         246    >19.9
---------------------------------------------------
    v           633       1924         156    >19.2
    b           559       1850         136    >20.0
    u           707       1825         117    >19.5
 uvw1           682       1801         117    >19.3
 uvm2           658       1944         151    >19.4
 uvw2           609       1900         156    >19.7
white           584       1875         284    >21.1
---------------------------------------------------

     The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.70 mag (Schlafly et al. 2011, ApJS, 737,
103).  GRB 130816A was 4 degrees above the Galactic Plane, so this
extinction value is highly uncertain.


GRB_name: GRB130822A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15112
SUBJECT: GRB 130822A: Swift detection of a short burst
DATE:    13/08/22 16:12:35 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

D. Kocevski (NASA/GSFC/ORAU), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
V. Mangano (PSU), F. E. Marshall (NASA/GSFC), C. Pagani (U Leicester),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
B. Sbarufatti (INAF-OAB/PSU), R. L. C. Starling (U Leicester) and
G. Tagliaferri (INAF-OAB) report on behalf of the Swift Team:

At 15:54:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130822A (trigger=567163).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 27.940, -3.219 which is 
   RA(J2000) = 01h 51m 46s
   Dec(J2000) = -03d 13' 08"
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 0.1 sec.  The peak count rate
was ~3700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 15:55:30.7 UT, 73.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 27.9218, -3.2085 which
is equivalent to:
   RA(J2000)  = 01h 51m 41.22s
   Dec(J2000) = -03d 12' 30.6"
with an uncertainty of 3.1 arcseconds (radius, 90% containment). This
location is 75 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.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.76
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
294 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 19.2 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
0.03. 

Burst Advocate for this burst is D. Kocevski (daniel.kocevski 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: GRB130821A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15113
SUBJECT: GRB 130821A: Fermi GBM Detection
DATE:    13/08/22 16:51:18 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH) reports on behalf of the Fermi GBM Team:

"At 16:10:28.011 UT on August 21 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130821A (trigger 398794231/130821674),
which resulted in an Autonomous Repoint Request (ARR) that was accepted and
the LAT slewed to the GBM position.
The GBM on-ground location, using the Fermi GBM trigger
data, is RA = 308.2, Dec = -15.5 (J2000 degrees, equivalent to
J2000 20h 32m, -15d 30'), with a statistical uncertainty of 1 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 of the burst direction to the Fermi LAT boresight is 37 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 84 s (50-300 keV).
The time-averaged spectrum from T0-3 s to T0+49 s is
well fit by a Band function with Epeak of 165 +/- 5 keV,
Alpha = -0.54 +/- 0.03 and Beta = -2.01 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(6.60 +/- 0.08)E-05 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+32 s in the 10-1000 keV band
is 27.6 +/- 0.4 ph/s/cm^2.

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

[GCN OPS NOTE(25aug13); Per operator's request, the "A" suffix
was added to the GRB name.]


GRB_name: GRB130822A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15114
SUBJECT: GRB 130822A: Weihai optical upper limit
DATE:    13/08/22 18:32:54 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D.-Y. Ren, C. Cao, S.-M. Hu (SDU) report:

We observed the field of GRB 130822A (Kocevski et al., GCN 15112)
using the 1m telescope located in Weihai, Shandong, China.
Observations started at 17:05:49 UT on 2013-08-22 (i.e., 1.19 hr after
the BAT trigger) and 3x500s SDSS r'-band frames were obtained in a
cloudy weather.

No optical source is detected within the XRT error circle (Kocevski et
al., GCN 15112) in the stacked image down to r'>~20 mag, calibrated
with SDSS field.


GRB_name: GRB130821A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15115
SUBJECT: GRB 130821A: Fermi-LAT detection of a burst 
DATE:    13/08/22 18:34:02 GMT
FROM:    Daniel Kocevski at SLAC  <dankocevski@gmail.com>

D. Kocevski (NASA/GSFC), N. Omodei (Stanford), J. Racusin (NASA/GSFC), S. Zhu (U. of Maryland), S. Guiriec (NASA/GSFC), Eleonora Troja (NASA/GSGC/UMCP) report on behalf of the Fermi-LAT team:

At 16:10:28.011 UT on 21 Aug 2013, Fermi-LAT detected high energy emission from GRB 130821A, which was also detected by Fermi-GBM (trigger 398794231/130821674 -- GCN 15113). The GBM detection triggered an autonomous repoint of the spacecraft.

The best LAT on-ground location is found to be RA=314.1, DEC=-12.0 (J2000) with an error radius of 0.1 deg (68% containment, statistical error only).

The burst was about 37 deg from the LAT boresight at the time of the trigger and the spacecraft slew brought the source within the LAT field of view for the next 2400 seconds. The data from the Fermi-LAT show long lasting emission with >40 photons above 100 MeV observed out to 2000s seconds with a TS of >170. Multi-peaked emission lasting roughly 40 seconds can be seen using the non-standard LAT Low Energy (LLE) with a significance of ~13 sigma. The highest energy LAT photon has an energy of ~6 GeV arriving 219 seconds after the trigger.

A Swift TOO request has been submitted.

The Fermi LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski@nasa.gov).

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.


GRB_name: GRB130822A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15116
SUBJECT: GRB 130822A, Swift-BAT refined analysis
DATE:    13/08/23 01:23:49 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
D. Kocevski (NASA/GSFC/ORAU), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
(i.e. the Swift-BAT team):
  
Using the data set from T-60 to T+123 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130822A (trigger #567163)
(Kocevski, et al., GCN Circ. 15112).  The BAT ground-calculated position is
RA, Dec = 27.931, -3.193 deg which is
    RA(J2000)  =  01h 51m 43.4s
    Dec(J2000) = -03d 11' 34.0"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
  
The mask-weighted light curve shows a single peak.  T90 (15-350 keV) is
0.04 +- 0.01 sec (estimated error including systematics).
  
The time-averaged spectrum from T-0.004 to T+0.044 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.64 +- 0.29.  The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-08 erg/cm2.
The 1-sec peak photon flux measured from T-0.48 sec in the 15-150 keV band is
0.3 +- 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/567163/BA/


GRB_name: GRB130822A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15117
SUBJECT: GRB 130822A: Enhanced Swift-XRT position
DATE:    13/08/23 02:28:29 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 465 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130822A, 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 = 27.92181, -3.20865 which is equivalent
to:

RA (J2000): 01h 51m 41.23s
Dec (J2000): -03d 12' 31.1"

with an uncertainty of 2.6 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, MNRAS, 397, 1177).

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


GRB_name: GRB130822A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15118
SUBJECT: GRB 130822A: Swift/UVOT Upper Limits
DATE:    13/08/23 09:44:03 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and D. Kocevski (NASA/GSFC/ORAU) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130822A 81 
s after the BAT trigger (Kocevski et al., GCN Circ. 15112).
No optical afterglow consistent with the XRT position (Beardmore et al. 
GCN Circ. 15117) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding 
chart (FC) exposure and subsequent exposures are:

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

white_FC            81          231          147         >20.8
u_FC               295          544          246         >20.7
white               81         1543          392         >21.4
v                  624         1420           97         >19.3
b                  550         1170           58         >20.1
u                  295         1145          265         >20.9
w1                 674         1470           97         >19.7
w2                 600          620           19         >19.4

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.03 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130822A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15119
SUBJECT: GRB 130822A: WHT ACAM observations
DATE:    13/08/23 12:00:09 GMT
FROM:    Klaas Wiersema at U Leicester  <kw113@leicester.ac.uk>

K. Wiersema (Leicester), A. Levan (Warwick), D. Malesani (DARK) report on behalf of
a larger collaboration:

We observed the position of short GRB 130822A (Kocevski et al., GCN 15112) using the 4.2m William Herschel
Telescope with the ACAM instrument and a Sloan r filter. We do not identify a source in or near the refined
XRT error circle (Beardmore et al., GCN 15117) in a dataset of 20x50 seconds exposures (0.365 days after burst),
taken under poor weather conditions. An upper limit of r=21.9 is found at the XRT position.
We note the presence of a moderately bright galaxy (r=18.15) offset approximately 22" from the GRB location 
and with a photometric redshift of z=0.1. If associated with would correspond to an offset of 40 kpc.


GRB_name: GRB130822A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15120
SUBJECT: GRB 130822A: Swift-XRT refined Analysis
DATE:    13/08/23 12:12:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), J.A. Kennea
(PSU), V. Mangano (PSU), M.C. Stroh (PSU), K.L. Page (U. Leicester), C.
Pagani (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo
(INAF-OAB) and D. Kocevski report on behalf of the Swift-XRT team:

We have analysed 7.2 ks of XRT data for GRB 130822A (Kocevski  et al.
GCN Circ. 15112),  from 85 s to 41.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN. Circ
15117). The source is fading with alpha >0.5.


If the light curve continues to decay with a power-law decay index of ,
the count rate at T+24 hours will be 2.8 x 10^-5 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00567163.

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


GRB_name: GRB130822A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15121
SUBJECT: GRB 130822A: Gemini Observations
DATE:    13/08/23 20:43:44 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA / GSFC), D. A. Perley (Caltech), A. Cucchiara (UCSC), W.
Fong (CfA), and A. J. Levan (U. Warwick) report on behalf of a larger
collaboration:

We have imaged the location of the X-ray afterglow (Beardmore et al., GCN
15117) of the short GRB 130822A (Kocevski et al., GCN 15112) with the
Gemini Multi-Object Spectrograph on the 8 m Gemini North telescope.  We
obtained a total integration of 600 s in the i' filter beginning at 12:56
UT on 23 August 2013 (0.88 d after the Swift trigger).  We detect no
sources within the enhanced XRT error circle.  Using nearby point sources
from SDSS for calibration, we calculate an upper limit of i' > 24.5 mag at
this time.


GRB_name: GRB130822A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15122
SUBJECT: GRB 130822A: 5.8 GHz VLA upper limit
DATE:    13/08/24 00:46:26 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, B. A. Zauderer and E. Berger (Harvard) report:

"We observed the field of the short-duration GRB 130822A (Kocevski et
al., GCN 15112) with the Karl G. Jansky Very Large Array (VLA)
beginning on 2013 Aug 23.33 UT (15.9 hr post-burst) at a mean
frequency of 5.8 GHz. In 1 hour of observations, we do not detect any
radio source within or around the XRT position (Beardmore et al., GCN
15117). We therefore place a 3-sigma limit of ~30 microJy on the radio
afterglow of GRB 130822A at 15.9 hr after the burst.

We thank the VLA staff for quickly executing these observations."


GRB_name: GRB130821A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15123
SUBJECT: GRB 130821A: Swift-XRT observation
DATE:    13/08/24 09:04:45 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, P.A. Evans (U. Leicester), V. D'Elia (ASDC), J. Gelbord (Eureka
Scientific) and J.L. Racusin (NASA/GSFC) report on behalf of the Swift-XRT
team:

Swift perfomed a Target of Opportunity observation of the Fermi GBM and
LAT-detected GRB 130821A (GCN Circ. 15113, 15115), between 100.7 and 136.5
ks after the trigger. Within the LAT error circle (0.1 degrees at 1-sigma;
statistical error only), in 9.9 ks of data there is a weak source with a
count rate of (1.3 +0.4/-0.3) x 10^-3 count s^-1 with a position of RA,
Dec 314.1601, -12.043481, which is equivalent to
RA(J2000)  =  20h 56m 38.44s
Dec(J2000) = -12d 02' 36.53"
(5.5 arcsec uncertainty, 90% containment). We cannot determine whether the
source is fading.

We note, however, that in a ~10 ks observation faint background sources
are expected, and there are two other detections (one uncatalogued, one a
possible quasar) of a similar count rate outside the LAT 1-sigma error
circle. The logN-logS work by Mateos et al. (2008, A&A, 492, 51) indicate
we would expect to find around one source of this brightness within the
~0.03 deg^2 of the LAT error circle, while Elvis et al. (2009, ApJS, 184,
158) provide a slightly higher sky density, suggesting up to 3 sources
might be expected. It is therefore likely that the source detected in this
XRT observation is a serendipitous background object.

Excluding this possible, weak source, the 3-sigma upper limit on the XRT
count rate within the LAT error circle is 1.8 x 10^-3 count s^-1
(equivalent to an observed flux of 7.3 x 10^-14 erg cm^-2 s^-1 over 0.3-10
keV, assuming a typical counts to flux conversion factor of 4 x 10^-11 erg
cm^-2 count^-1).

We also note that, within the XRT field of view, although outside the LAT
1-sigma error circle, there is an X-ray source with a UVOT-enhanced
position of RA, Dec 313.92706, -11.96634, which is equivalent to
RA(J2000)  =  20h 55m 42.49s
Dec(J2000) = -11d 57' 58.8"
(2.3 arcsec uncertainty, 90% containment). This position is 4 arcsec away
from the catalogued XMM Slew Survey object XMMSL1 J205542.2-115756. The
1-sigma uncertainty on the positions in the slew catalogue is 8 arcsec;
thus, this X-ray source is consistent with being XMMSL1 J205542.2-115756
and is unrelated to GRB 130821A.

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


GRB_name: GRB130821A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15124
SUBJECT: GRB 130821A: Weihai optical upper limit
DATE:    13/08/24 15:56:19 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D.-Y. Ren, C. Cao, S.-M. Hu (SDU) report:

We observed the XRT field of GRB 130821A (Jenke et al., GCN 15113;
Kocevski et al., GCN 15115; Page et al., GCN 15123) centered at
RA(J2000)  =  20h 56m 38.44s and Dec(J2000) = -12d 02' 36.53", using
the 1m telescope located in Weihai, Shandong, China. We obtained
9x300s SDSS r'-band frames under cloudy conditions at a mean time of
14:20 UT on 2013-08-24 (i.e., 2.997 days after the burst).

No optical source is detected within the XRT error circle in the
stacked image, down to r'>20.8 mag, calibrated with nearby SDSS field.


GRB_name: GRB130821A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15125
SUBJECT: Konus-Wind observation of GRB 130821A
DATE:    13/08/26 16:46:37 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 130821A
(Fermi-GBM detection: Jenke, GCN 15113;
Fermi-LAT detection: Kocevski, et al., GCN 15115)
triggered Konus-Wind at T0=58258.022 s UT (16:10:58.022).

The light curve shows multiple pulses from ~T0-40 to ~T0+80 s.
The emission is seen up to ~9 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130821_T58258/

As observed by Konus-Wind, the burst
had a fluence of (9.9  0.9)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+6.784 s,
of (1.3  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+78.080 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.33  0.11,
the high energy photon index beta = -2.25  0.19,
the peak energy Ep = 260  47 keV,
chi2 = 84.6/97 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+12.544 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.11  0.07,
the high energy photon index beta = -2.33  0.10,
the peak energy Ep = 255  22 keV,
chi2 = 96.9/97 dof.

All the quoted results are preliminary.


GRB_name: GRB130822A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15126
SUBJECT: GRB 130822A Swift-BAT Spectral lag analysis
DATE:    13/08/27 01:32:20 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

J. Norris (BSU), S. D. Barthelmy (GSFC), T. Sakamoto (AGU), N. Gehrels (GSFC)

We report the spectral lag analysis for GRB 130822A (Kocevski, et al., GCN Circ. 15112) 
based on the BAT data.  Using 1-ms binned light curve, the spectral lag for the 15-25 keV 
to 50-100 keV bands is 2.6 (+3.5/-3.2) ms.  Since the lag value is consistent with zero, we 
believe this burst belongs to a short burst category.  There is no evidence for extended 
emission.  


GRB_name: GRB130821A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15127
SUBJECT: IPN triangulation of GRB130821A
DATE:    13/08/28 17:00:07 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley on behalf of the Mars Odyssey GRB team,

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, 
D. Svinkin, 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,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,

D. M. Smith, J. McTiernan, R. Schwartz, and W.
Hajdas, on behalf of the RHESSI GRB team, 

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

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

GRB 130821A, observed by the Fermi GBM (GCN 15113) and LAT (GCN 15115),
was also observed by Konus-Wind (GCN 15125), RHESSI, INTEGRAL SPI-ACS,
and Mars Odyssey-HEND.  We have triangulated it to an annulus centered
at RA(2000)=297.840 deg (19h 51m 22s)  Dec(2000)=-21.890 deg (-21d 53'
24"), whose radius is 18.673 +/- 0.049 deg (3 sigma).  The minimum
distance between the center of the LAT one sigma error circle (GCN
15115) and the IPN annulus center line is 0.266 degrees; the circle lies
entirely outside the annulus. The two Swift XRT sources reported by
Page et al. (GCN 15123) also lie outside the IPN annulus, and are
therefore unlikely to be associated with the GRB.  A map has been posted at
ssl.berkeley.edu/ipn3/130821.  

Only minor improvement in the IPN localization is possible.


GRB_name: GRB130828A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15128
SUBJECT: GRB 130828A: Fermi-LAT detection of a burst
DATE:    13/08/29 03:25:30 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G.Vianello (Stanford), E.Sonbas (NASA/GSFC/Adiyaman Univ.) report on
behalf of the Fermi-LAT team:

At 07:20:00.15 on 2013-08-28 Fermi LAT detected high energy emission
from GRB 130828A, which was also detected by Fermi-GBM (trigger
399367203).

The best LAT on-ground location is found to be RA, DEC 259.83, +28.00
(J2000) with an error radius of 0.3 deg (68% containment, statistical
error only), this was 40 deg from the LAT boresight at the time of the
trigger, and triggered an autonomous repoint of the spacecraft.

The data from the Fermi LAT show a significant increase (>> 5 sigma)
in the event rate within 2.3 degree of the best HITL GBM location
after the GBM trigger that is spatially and temporally correlated with
the GBM emission with high significance. More than 30 photons above
100 MeV and 2 photons above 1 GeV are observed within 1000 seconds.
The highest energy photon is a 1.5 GeV event which is observed 225
seconds after the GBM trigger.

The Fermi LAT point of contact for this burst is Eda Sonbas
(esonbas@slac.stanford.edu).

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.


GRB_name: GRB130828A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15129
SUBJECT: GRB 130828A: Fermi GBM detection
DATE:    13/08/29 03:32:12 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU) reports on behalf of the
Fermi GBM Team:

"At 07:20:00.15 UT on 28 August 2013, the Fermi Gamma-ray Burst
Monitor (GBM) triggered and located GRB 130828A (trigger 399367203 /
130828.306). The on-ground calculated location, using the Fermi GBM
trigger data, is RA = 258.14, Dec = +29.76 (J2000 degrees, equivalent
to J2000 17h 12m, +29d 45' ), with a statistical 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 46 degrees.

The burst was strong enough to trigger an Automatic Repointing
Request (ARR) on the Fermi spacecraft.  The GRB position was 
placed in the center of the LAT Field-of-view for 2.5 hours (subject
to Earth angle constraints).

The GBM light curve shows consists of several pulses, and is
possibly on top of a particle event.  We find a duration (T90)
of about 159 +/- 23 s (50-300 keV). We find the 1.024s peak flux
during this time to be (7.39 +/- 0.37) ph/s/cm^2.  The time-averaged
spectrum from T0-4.10 to T0+159.75 s is best fit by a Band function
with Epeak = 320.7 +/- 21.0 keV, alpha = -0.90 +/- 0.03, and
beta = -2.22 +/- 0.03. The fluence (10-1000 keV) in this time 
interval is (6.05 +/- 0.09)E-05 erg/cm^2.

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


GRB_name: GRB130828A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15130
SUBJECT: GRB 130828A Tiled Swift observations
DATE:    13/08/29 12:26:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 130828A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00018

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB130829A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15131
SUBJECT: GRB 130829A: Swift detection of a burst
DATE:    13/08/29 18:20:10 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Grupe (PSU), D. N. Burrows (PSU), S. T. Holland (STScI),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
C. J. Mountford (U Leicester), P. T. O'Brien (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 05:43:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130829A (trigger=568417).  Swift could not slew to the
burst location due to a Sun constraint.  Due to this source's apparent 
proximity to the Galaxy NGC 4144, this was originally reported as a 
transient and no GCN circular was issued. 

Using the data set from T-239 to T+303 sec from the recent telemetry downlink,
we report the detection of BAT GRB 130829A (trigger #568417).  
The BAT ground-calculated position is
RA, Dec = 182.426, 46.520 deg which is
   RA(J2000)  =  12h 09m 42.1s
   Dec(J2000) = +46d 31' 10.8"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). 
The partial coding was 84%. 

The mask-weighted light curve shows a long peak starting from ~T+34 and 
ending at ~T+77. T90 (15-350 keV) is 42.56 +- 7.08 sec (estimated error 
including systematics). 

The time-averaged spectrum from T+30.86 to T+87.50 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.12.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-06 erg/cm2. 
The 1-sec peak photon flux measured from T+50.90 sec in the 15-150 keV band
is 0.6 +- 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/568417/BA/

The nominal (Simbad) coordinates of galaxy NGC 4144 are
2.8 arcmin East and 3.8 arcmin North of the BAT GRB location. 
This places the entire BAT error circle outside of the bright
visible area of the galaxy, but the position would be consistent
with an extended spherical halo. 

Due to an observing constraint, Swift XRT or UVOT cannot observe
this region until September 24th, 2013. 

Burst Advocate for this burst is D. Grupe (dxg35 AT 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: GRB130828A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15132
SUBJECT: IPN triangulation of GRB 130828A
DATE:    13/08/29 18:34:05 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

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

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

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

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

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

GRB 130828A (GCN 15128, 15129, 15130) has been observed by Fermi,
INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER GRNS, Suzaku, and Swift
(outside the coded field of view), so far.  We have triangulated it to
an annulus centered at RA(2000)=340.597 deg (22 h 42 m 23 s),
Dec(2000)=-9.971 deg (-9 d 58 m 17 s), whose radius is 86.782 +/- 0.092
degrees (3 sigma).  This annulus intersects the Fermi-LAT 1 sigma error
circle (GCN 15128) to form an error box whose area (280 sq.  arcmin.) is 
about 3.6 times smaller than that of the LAT error circle , and whose
corners are
         RA(2000)                    Dec(2000)
     259.541=17 h 18 m 09 s      27.843= 27 d 50 ' 34 "
     259.649=17 h 18 m 35 s      28.254= 28 d 15 ' 13 "
     259.722=17 h 18 m 53 s      27.716= 27 d 42 ' 56 "
     259.875=17 h 19 m 30 s      28.297= 28 d 17 ' 50 "

A map has been posted at ssl.berkeley.edu/ipn3/130828A.

Some improvement in this triangulation is possible.


GRB_name: GRB130828A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15133
SUBJECT: Correction to GCN 15132 - GRB 130828A
DATE:    13/08/29 18:46:18 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

The title of GCN 15132 should have been "IPN triangulation of GRB 130828A",
rather than 130821A.  I apologize for the confusion and thank Kim Page for
catching this quickly.


GRB_name: GRB130829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15134
SUBJECT: GRB 130829A: NOT optical observations
DATE:    13/08/29 22:49:43 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), J. P. U. Fynbo (DARK/NBI),
A. A. Djupvik (NOT), Y. Martinez-Osorio (NOT) report on behalf of a
larger collaboration:

We observed the BAT field of GRB 130829A (Grupe et al., GCN 15131)
using the 2.5 Nordic Optical Telescope (NOT) equipped with StanCam. We
obtained 4x300s R-band frames at a mean time of 20:46 UT on
2013-08-29, i.e., 15.05 hr after the BAT trigger. Observations were
carried out at high airmass, and the resulting seeing was about 1
arcsec. Our images cover 96% of the BAT error circle.

Our image reaches a depth comparable to the SDSS, roughly R = 22.7.
Visual comparison between our data and the SDSS image reveals no new
source within the BAT error circle.


GRB_name: GRB130828A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15135
SUBJECT: GRB 130828A: Swift XRT and UVOT observations  
DATE:    13/08/30 01:53:41 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU), Craig Swenson, and Mike Siegel 
report on behalf of the Swift team:


Swift-XRT has observed the error circle of the Fermi/LAT GRB 
130828A (Vianello & Sonbas, GCN Circ 15128)
in a series of observations tiled on the sky. In 2.5 ks of data, 
beginning 105 ks after the Fermi/LAT trigger, we detect an 
uncatalogued X-ray source at RA, Dec = 259.73234, 27.99570 which 
is equivalent to:
 RA (J2000)  = 17h 18m 55.76s
 Dec (J2000) = +27d 59' 44.5"
with an uncertainty of 4.1 arcsec (radius, 90% confidence).
This source is within the LAT error circle given in GCN circular
15128).

At the present time we cannot determine whether the source is 
fading, therefore we cannot be certain whether this is the 
afterglow of GRB 130828A or a serendipitous source.

The source was detected in observations with target ID 00020292. 
The results of the automated XRT processing of this source are 
available at 
http://www.swift.ac.uk/xrt_products/TILED_GRB00018/20292/index_1.php

The Swift UVOT observed this field for 2.5 ks in the u filter.
There are two sources at the edge of the XRT error circle, one is a
Seyfert 1.9 galaxy, SDSS J171855.44+275947.4, which may be the
counter part of the X-ray source. However, the origin of the X-ray
source  is unclear at this point.


This circular is an official product of the Swift team.


GRB_name: GRB130829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15136
SUBJECT: GRB 130829A: AAO optical observations
DATE:    13/08/30 12:48:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R.Inasaridze (AAO), O. Kvaratskhelia (AAO), V. 
Ayvazian(AAO), I. Molotov (KIAM), A. Pozanenko (IKI)  report on behalf 
of  larger GRB follow-up collaboration:

We observed the field of the Swift GRB 130829A (Grupe et al., GCN 15131) 
with AS-32 (0.7m) telescope of Abastumani Observatory  on Aug. 29 
starting (UT) 18:56. We obtained several unfiltered images of 120 s 
exposure. Our images cover 100% of the BAT error circle. In the BAT 
error localization  GRB 130829A (Grupe et al., GCN 15131) we do not 
identify any new source in comparison with SDSS.  A photometry of 
combined image against nearby SDSS stars (R magnitude, transformed by 
Lupton gri -> R transformation) is following

Date        T_start    t-t0,      exp,    OT  UL
             (UT)       mid, d     s
2013-08-29  18:55:48   0.56442    9x120   n/d 20.6


GRB_name: GRB130822A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15137
SUBJECT: GRB 130822A: optical upper limits
DATE:    13/08/30 13:20:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R.Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian(AAO), Yu. Krugly (IA KhNU), I. Slyusarev (IA KhNU), I. Molotov 
(KIAM), V. Linkov (ISON), A. Pozanenko (IKI)  report on behalf
of  larger GRB follow-up collaboration:

We observed the field of Swift GRB 130822A (Kocevski et al., GCN 15112) 
on Aug., 22 with AS-32 (0.7m) telescope of Abastumani Observatory, 
SANTEL-400AN (0.4m) telescope of ISON-Kislovodsk observatory, and AZT-8 
(0.7m) telescope of Institute of Astronomy, Kharkiv National University. 
We obtained several unfiltered frames with exposures of 120 s (AS-32), 
100 s and 60 s (SANTEL-400AN), and several frames with filter R with 
exposure of 120 s (AZT-8).  Within the enhanced XRT circle (Beardmore et 
al., GCN 15117) we did not detect any source on stacked images.

The details of the photometry are the following:

Telescope t_start, UT  filter exptime,s    t-t0, mid, days    uplim

AZT-8     21:39:21     R      55*120       0.28000            20.6
S-400     22:31:37     None   23*100       0.30332            19.3
AS-32     23:46:59     None   40*120       0.36513            21.9

The photometry is based on SDSS stars, R mag (R mag obtained via
transformations ugriz in BVRI (Lupton, 2005):

SDSS id             R      R_err
J015202.75-031421.9 12.80  0.012
J015134.64-031348.8 13.95  0.013
J015148.69-030854.9 14.62  0.013


GRB_name: GRB130828A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15138
SUBJECT: IPN triangulation of GRB 130828A - error box
DATE:    13/08/30 19:49:09 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, 
D. Svinkin, 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,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

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

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

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

GRB 130828A (GCN 15128, 15129, 15130, 15132, 15133) was also observed
by Mars Odyssey-HEND.  We have triangulated this burst to the following
3 sigma error box, whose area is 28 square arcminutes:

   RA(2000)                       Dec(2000)
259.728=17 h 18 m 54 s     28.196= 28 o 11 '  46 "
259.867=17 h 19 m 28 s     28.316= 28 o 18 '  58 "
259.707=17 h 18 m 49 s     28.115= 28 o 06 '  54 "
259.846=17 h 19 m 23 s     28.235= 28 o 14 '  06 "

The Swift XRT source (GCN 15135) lies outside this error box.

A map has been posted at ssl.berkeley.edu/ipn3/130828A.


GRB_name: GRB130831A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15139
SUBJECT: GRB 130831A: Swift detection of a burst with an optical counterpart
DATE:    13/08/31 13:21:11 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

L. M. Z. Hagen (PSU), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), D. Grupe (PSU), J. A. Kennea (PSU),
V. Mangano (PSU), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), P. T. O'Brien (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
E. Troja (NASA/GSFC/UMCP) and B.-B. Zhang (UAH) report on behalf of
the Swift Team:

At 13:04:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130831A (trigger=568849).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 358.649, +29.448 which is 
   RA(J2000) = 23h 54m 36s
   Dec(J2000) = +29d 26' 53"
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 50 sec.  The peak count rate
was ~10000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 13:06:22.3 UT, 125.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 358.62398,
29.42849 which is equivalent to:
   RA(J2000)  = 23h 54m 29.76s
   Dec(J2000) = +29d 25' 42.6"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 105 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 4.80
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 8.87e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
190 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 23:54:29.89 = 358.62453
  DEC(J2000) = +29:25:46.2  =  29.42950
with a 90%-confidence error radius of about 0.74 arc sec. This position is 5.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.56 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is L. M. Z. Hagen (lea.zernow.hagen 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: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15140
SUBJECT: GRB 130831A: Faulkes Telescope North and South optical afterglow
DATE:    13/08/31 13:38:30 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB) on behalf of
a large collaboration report:

The 2-m Faulkes Telescopes North and South automatically began observing 
GRB
130831A (Hagen et al. GCN Circ. 15139) on August 31 2013 at 13:09:01 UT
(~4.7 min after the burst trigger).

We clearly detect the fading optical afterglow reported by Swift/UVOT
with R=14.1 +- 0.1 mag at 4.75 minutes since the BAT trigger time,
calibrated against nearby USNOB-1 catalogue stars.


GRB_name: GRB130831B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15141
SUBJECT: GRB 130831B: Swift detection of a burst
DATE:    13/08/31 14:13:29 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Malesani (DARK/NBI), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
D. Grupe (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
V. Mangano (PSU), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), D. M. Palmer (LANL),
M. H. Siegel (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (UAH) report
on behalf of the Swift Team:

At 13:48:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130831B (trigger=568855).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 192.446, -29.177 which is 
   RA(J2000) = 12h 49m 47s
   Dec(J2000) = -29d 10' 35"
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 30 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 13:50:26.7 UT, 127.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 192.42070, -29.18380 which is
equivalent to:
   RA(J2000)  = 12h 49m 40.97s
   Dec(J2000) = -29d 11' 01.7"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 83 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 (6.20 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.6
(+1.89/-1.67) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 129 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
0.08. 

Burst Advocate for this burst is D. Malesani (malesani AT dark-cosmology.dk). 
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: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15142
SUBJECT: GRB 130831A: Weihai optical observations
DATE:    13/08/31 14:29:36 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), C. M. Zhang, C. Cao, S. M. Hu (SDU) report:

We observed the field of GRB 130831A (Hagen et al., GCN 15139) using
the 1m telescope located in Weihai, Shandong Province, China, and
2x600s SDSS r'-band frames were obtained.

The optical afterglow is well detected at the UVOT position in each of
the two images with rather fast decaying rate. Following photometry is
calibrated with nearby SDSS stars:

Mag     MagErr   MeanTime(T-Ttrigger, hr)
14.35    0.04           0.3356
15.66    0.05           0.6575


GRB_name: GRB130831A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15143
SUBJECT: GRB 130831A: MITSuME Akeno Optical observation
DATE:    13/08/31 15:03:11 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T. Yoshii, K. Ito, Y. Saito, Y. Yano, R. Usui, Y. Tachibana, 
S. Kurita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130831A (L. M. Z. Hagen et al., GCNC 15139) with the 
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.
And we continue observing .

The observation started on 2013-08-31 13:06:14 UT ( 118 sec after the burst).
And we detected the previously reported afterglow .
But weather condition was not so good.
The measured magnitudes were listed below.

T0+[sec]       MID-UT        T-EXP[sec]              g'                            Rc                          Ic 
------------------------------------------------------------------------------------------------------------------------------
  ~118           13:07:41         300              15.40+/-0.23        15.16+/-0.33            analyzing
------------------------------------------------------------------------------------------------------------------------------
(The photon flux were calibrated against GSC2.3 catalog.)


GRB_name: GRB130831A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15144
SUBJECT: GRB 130831A: Gemini-North Redshift
DATE:    13/08/31 15:37:32 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick Observatory), D. Perley (Caltech) 
report on behalf of a larger collaboration:

"We observed the afterglow of GRB 130831A (Hagen et al. 
GCN 15139, Guidorzi et al. GCN 15140) with the GMOS spectrograph 
on Gemini-North, beginning approximately 50 min after the BAT trigger.

We obtained 2x900s exposure spectra under exquisite conditions 
using the B600 grism, covering the 3860-6649 Angstrom wavelength range.

In our preliminary analysis we detect MgII2796,2803 doublet and 
MgI2853 absorption lines at z=0.4791.

No other strong features are detected in absorption or in emission, 
therefore we suggest this as the redshift of GRB 130831A.


We thank the Gemini-N staff, in particular Adam Smith and 
Anthony Matulonis, for their support."


GRB_name: GRB130831A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15145
SUBJECT: Konus-Wind observation of GRB 130831A
DATE:    13/08/31 18:50:31 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration soft-spectrum GRB 130831A
(Swift-BAT trigger 568849: Hagen, et al., GCN 15139)
triggered Konus-Wind at T0=47062.044 s UT (13:04:22.044)

The light curve shows a smooth pulse peaked at ~T0+1.6 s
followed by a weaker emission till ~T0+35~s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130831_T47062/

As observed by Konus-Wind, the burst
had a fluence of (7.6 Â± 0.4)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+1.600 s,
of (2.5 Â± 0.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.61 Â± 0.06,
the high energy photon index beta = -3.3 Â± 0.3,
the peak energy Ep = 55 Â± 4 keV,
chi2 = 118/97 dof.

The spectrum at the maximum count rate (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.51 Â± 0.10,
the high energy photon index beta = -2.8 Â± 0.1,
the peak energy Ep = 67 Â± 4 keV,
chi2 = 91/96 dof.

Assuming Gemini-North redshift z=0.4791 (Cucchiara & Perley, GCN 15144),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters of GRB 130831A:
the isotropic energy release E_iso is (4.6 Â± 0.2)x10^51 erg,
the peak luminosity (L_iso)_max is (2.7 Â± 0.3)x10^51 erg/s,
and the rest-frame peak energy Ep,i = (81 Â± 6) keV

All the quoted results are preliminary.


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15146
SUBJECT: GRB 130831A : Xinglong 60cm optical observation
DATE:    13/08/31 19:39:25 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   X. H. Han, Y. L. Qiu,  J. Y. Wei,  J. Wang,  
J. S. Deng and C. Wu on behalf of EAFON report:

We began to observe GRB 130831A (Hagen et al. GCN 15139)  
with Xinglong 60cm telescope at  15:42:00 (UT), 
about 2.7 hours after the burst.  
A series of white and R-band images were obtained. 

The OT reported by (Hagen et al. GCN 15139, Guidorzi et al. GCN 15140, 
Xu et al. GCN 15142;  Yoshii et al. GCN 15143, Cucchiara  et al. GCN 15144) 
was detected in all images.  The brightness of this OT was about R=16.6 mag 
at  2.7 hours  after the burst,  calibrated by USNO B1.0 R2 mag.

This message may be cited.


GRB_name: GRB130831A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15147
SUBJECT: GRB 130831A: Enhanced Swift-XRT position
DATE:    13/08/31 20:40:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2474 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 130831A, 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 = 358.62461, +29.42990 which is equivalent
to:

RA (J2000): 23h 54m 29.91s
Dec (J2000): +29d 25' 47.6"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130831A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15148
SUBJECT: GRB 130831A: Skynet/PROMPT-SSO detections
DATE:    13/08/31 21:08:52 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, A. LaCluyze, J. Moore, N. Frank, D. Reichart, T. 
Berger, H. T. Cromartie, R. Egger, A. Foster, K. Ivarsen, M. Maples, M. 
Nysewander, and J. A. Crain report:

Skynet observed the Swift/BAT localization of GRB 130831A (Hagen et al., 
GCN 15139, Swift trigger #568849) with four 17" telescopes of the 
newly-commissioned PROMPT array at Siding Spring Observatory, NSW, 
Australia. Starting at 2013-08-31, 13:39 UT and continuing until 17:41 
UT (t=35.5m-4.65h post-trigger), it took 615 80-s exposures in the BVRI 
bands. We detect a bright fading afterglow in all four bands at RA 
23:54:29.8, Dec 29:25:46.4 (J2000), within the error circle of the 
Enhanced Swift-XRT localization (Evans et al., GCN 15147).

A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130831a.png

Magnitudes are in the Vega system, calibrated to 6 APASS stars in the 
field, and have not been corrected for the modest expected line-of-sight 
Milky Way dust extinction E(B-V)=0.046 (Schlegel et al. 1998).

Skynet observations are ongoing.


GRB_name: GRB130831B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15149
SUBJECT: GRB 130831B: Enhanced Swift-XRT position
DATE:    13/08/31 21:35:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2499 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130831B, 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 = 192.42038, -29.18331 which is equivalent
to:

RA (J2000): 12h 49m 40.89s
Dec (J2000): -29d 10' 59.9"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15150
SUBJECT: GRB 130831A: Montarrenti Observatory optical observations
DATE:    13/09/01 01:07:49 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

Simone Leonini, G. Guerrini, P. Rosi and L.M. Tinjaca Ramirez (Montarrenti 
Observatory, Siena, Italy) report:

We observed the optical afterglow of GRB 130831A (Swift trigger 568849, Hagen 
et al., GCN Circ. 15139) and slow fading over the four hours span of 
observations with the automatic 0.53m RC telescope + U47 detector at 
Montarrenti Observatory (Siena, Italy, IAU code C88).

The observations were started at 2013-08-31 20:18:04 UT (approximately 7 hours 
post-burst) and continued to 00:29:36 UT on 2013-09-01 stacking 2 unfiltered 
CCD exposures of 60s for each run.

The OT was detected in all frames. The resulting time-series are as follows:

2013 Aug 31.84588 UT R=18.22 +/- 0.21 
2013 Aug 31.90427 UT R=18.55 +/- 0.21
2013 Aug 31.94019 UT R=18.47 +/- 0.22
2013 Aug 31.96977 UT R=18.63 +/- 0.23
2013 Aug 31.99955 UT R=18.95 +/- 0.22
2013 Sep 01.02056 UT R=19.09 +/- 0.21


Magnitudes were obtained using Astrometrica software using USNO-B1 catalogue 
for positions and photometry. An ensemble between 38 and 66 stars were used for 
the magnitude comparison.

The position of the GRB (within the error box given by Swift) is the 
following:

RA    (J2000)  23h 54m 29.90s +/-0.13
Decl. (J2000) +29Â° 25' 46.8"  +/-0.14

The message may be cited.


GRB_name: GRB130831A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15151
SUBJECT: GRB 130831A: Swift-XRT refined Analysis
DATE:    13/09/01 01:21:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), V. Mangano (PSU), M.C. Stroh (PSU), D.N.
Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) and
L.M.Z. Hagen report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 130831A (Hagen  et al. GCN
Circ. 15139),  from 115 s to 23.9 ks after the BAT trigger. The data
comprise 73 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 15147).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.0 (+0.4, -0.6). At T+239 s  the decay
flattens to an alpha of -0.1 (+0.3, -0.6) before breaking again at
T+783 s to a final decay with index alpha=1.09 (+0.09, -0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.53 (+0.12, -0.11). The
best-fitting absorption column is  consistent with the Galactic value
of 4.8 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a
photon index of 1.78 (+0.12, -0.08) and a best-fitting absorption
column of 5.2 (+2.8, -0.4) x 10^20 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.9 x 10^-11 (4.4 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.2 (+2.8, -0.4) x 10^20 cm^-2
Galactic foreground: 4.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.78 (+0.12, -0.08)

If the light curve continues to decay with a power-law decay index of
1.09, the count rate at T+24 hours will be 0.024 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.5 x
10^-13 (1.1 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/00568849.

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


GRB_name: GRB130831A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15152
SUBJECT: GRB 130831A: Optical Observations via Virtual Telescope
DATE:    13/09/01 01:54:33 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy) report:

On Sept 1.0599 2013 UT, we imaged the field around GRB 130831A (GCN 15139) 
remotely using the the 0.43m-f/6.8 robotic unit part of the Virtual
Telescope robotic facility in Italy, about 12 hours after the burst.

The source is visible on 300 seconds unfiltered CCD images
following coordinates (J2000):

R.A. = 23 54 29.89
Decl. +29 25 46.6

We also performed photometry, assuming R-mags from UCAC-4 for the stars in the
field, getting an estimate for the magnitude of 19.1 (CR).

Observations are ongoing.


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15153
SUBJECT: GRB 130831A: optical observations
DATE:    13/09/01 01:56:19 GMT
FROM:    Luca Izzo at ICRA  <Luca.Izzo@ICRA.it>

L. Izzo and L. D'Avino report:

We have observed the optical afterglow of GRB 130831A using a 0.32m =
f/9.3 Ritchey-Chretien telescope of the iTelescope network, at Siding =
Spring =96 Australia.

We have detected the afterglow in the R and V, but not in the B band. =
After an ensemble photometry, using nearby SDSS stars, and correction =
from SDSS to V and R filters, we have obtained  the following =
magnitudes:

R =3D 15.58 +- 0.09  (78 min post-trigger =96 240s exposure)

V =3D 16.89 +- 0.09  (92 min post-trigger =96 180 s exposure)

The R-composite image can be seen at
http://blacksabburst.files.wordpress.com/2013/08/r_median.png


GRB_name: GRB130831B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15154
SUBJECT: GRB 130831B: Swift-XRT refined Analysis
DATE:    13/09/01 04:13:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U.
Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA) and D. Malesani report on behalf of the Swift-XRT team:

We have analysed 6.8 ks of XRT data for GRB 130831B (Malesani  et al.
GCN Circ. 15141),  from 112 s to 35.4 ks after the  BAT trigger. The
data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Goad et al. (GCN. Circ 15149).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.24 (+0.12, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.07 (+0.16, -0.15). The
best-fitting absorption column is  1.6 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 6.2 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 3.7 x 10^-11 (5.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 6.2 x 10^20 cm^-2
Excess significance: 4.2 sigma
Photon index:      2.07 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.24, the count rate at T+24 hours will be 9.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-13 (5.0 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/00568855.

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


GRB_name: GRB130831A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15155
SUBJECT: GRB 130831A, Swift-BAT refined analysis
DATE:    13/09/01 04:15:22 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), L. M. Z. Hagen (PSU),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-61 to T+243 sec from the
recent telemetry downlink, we report further analysis
of BAT GRB 130831A (trigger #568849) (Hagen, et al.,
GCN Circ. 130831A). The BAT ground-calculated position is
RA, Dec = 358.635, 29.431 deg which is
   RA(J2000)  =  23h 54m 32.4s
   Dec(J2000) = +29d 25' 51.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 28%.

BAT mask-weighted light curve shows a bright peak
starting from ~T-1 sec peaking around T+3 sec
and ending at ~T+12 sec. Two more very weak
emission can be seen around T+20 sec and T+32 sec.
T90 (15-350 keV) is 32.5 +- 2.5 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.86 to T+41.38 sec
is best fit by a simple power-law model. The power
law index of the time-averaged spectrum is 1.93 +- 0.05.
The fluence in the 15-150 keV band is
6.5 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak photon
flux measured from T+2.30 sec in the 15-150 keV band
is 13.6 +- 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/568849/BA/


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15156
SUBJECT: GRB 130831A: THO optical observation
DATE:    13/09/01 06:48:23 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen, Harri Vilokki and Tuomo Salmi 
(Taurus Hill Observatory, Varkaus, Finland) report:

We have detected GRB 130831A optical afterglow at Taurus Hill Observatory
A95 (Varkaus, Finland). We used 0.35m C-14 OTA telescope (f =3910 mm),
NextGen 0.5X, Paramount ME and SBIG ST-8XME CCD camera. 
The observation was started 6.65 hours after the Swift trigger. Six unfiltered
images with 600 sec exposure time were made.

The afterglow was detected at following position RA 23 54 29.7 and
DEC +29 25 46.6.

The following magnitude was obtained from the observation using NOMAD1
1194-0619856 (R=16.240) as the comparison:

Tmid(h)+T0    Filter              Exp. time          Mag                Mag err. 
7.218              unfiltered        6x600              18.01CR         0.08

A png preview of the observation showing the position of the afterglow is 
available at this URL: 
www.kassiopeia.net/wp-content/uploads/2013/09/GR130831A_comparison.png


GRB_name: GRB130901A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15157
SUBJECT: Swift Trigger 569022: a possible GRB
DATE:    13/09/01 09:39:14 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), D. Grupe (PSU), C. J. Mountford (U Leicester),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 09:13:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located possible GRB 130901A or a Galactic source (trigger=569022).  
Swift slewed immediately to the detected source position.  The BAT on-board 
calculated location is 
RA, Dec 263.611, -30.402 which is 
   RA(J2000) = 17h 34m 27s
   Dec(J2000) = -30d 24' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve does not show significant 
variation, which is not unusual for an image-based trigger. 

The XRT began observing the field at 09:15:20.0 UT, 123.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 263.6018, -30.3961 which is equivalent to:
   RA(J2000)  = +17h 34m 24.43s
   Dec(J2000) = -30d 23' 46.0"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 35 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 0.1 s image was 3.68e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 4 seconds with the White filter
starting 131 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image cover 100%
of the XRT error circle.  Results from the list of sources
generated on-board are not available at this time. 

This burst occurred at Galactic coordinates l = 357.47, b = 1.29, that
is only 2.8 deg away from the Galactic Center. At this stage, we
cannot confirm whether this is a Galactic or extragalactic transient. 

Burst Advocate for this burst is D. Malesani (malesani AT dark-cosmology.dk). 
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: GRB130831B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15158
SUBJECT: GRB 130831B: GROND upper limits
DATE:    13/09/01 15:08:32 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

V. Sudilovsky, M. Tanga, and J. Greiner
(all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 130831B (Swift trigger 568855;
Malesani et al. 2013, GCN #15141) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the
2.2 m MPG/ESO telescope at La Silla Observatory (Chile).

Observations started at 23:22 UT on 31 Aug. 2013, 10 hours after the
GRB trigger. They were performed at an average seeing of 2.2" and at
an average airmass of 2.2.

Based on five co-added images with individual exposures of 6 min in
g'r'i'z' and 4 min exposure in JHK, we do not detect a source within the
3.6 arcsec Swift-XRT error circle reported by Malesani et al.
(2013; GCN #15141) down to (all in the AB system)

g' > 23.4,
r' > 23.2,
i' > 22.6,
z' > 22.3,
J > 20.8,
H > 20.2, and
K > 19.6

The given limits are derived based on calibrating the images against
GROND zeropoints and 2MASS field stars and are not corrected for the
Galactic foreground extinction corresponding to a reddening of
E_(B-V)= 0.08 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15159
SUBJECT: GRB 130831A: CARMA mm upper limit
DATE:    13/09/01 16:58:42 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

B. A. Zauderer, T. Laskar , and E. Berger (Harvard) report on behalf of the
CARMA Key Project, "A Millimeter View of the Transient Universe" and a
larger collaboration:

"We observed the position of the optically bright GRB 130831A
(Hagen et al. GCN 15139; Xu et al. GCN 15142) with the Combined Array for
Research in Millimeter Astronomy (CARMA) beginning 2013 September 1.30
(dt = 0.76 d).  At a mean frequency of 90 GHz, in marginal weather
conditions,
we obtain a 3-sigma upper limit of 0.78 mJy.  We thank the CARMA observers
and staff for their support."


GRB_name: GRB130831B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15160
SUBJECT: GRB 130831B: Swift/UVOT Upper Limits
DATE:    13/09/01 17:28:26 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and D. Malesani (DARK/NBI)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130831B
130 s after the BAT trigger (Malesani et al., GCN Circ. 15141).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 15149)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

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

white_FC           130          279          147         >20.3
u_FC               288          537          246         >19.6
white              130         6384          439         >20.9
v                  618         5490          274         >19.7
b                  543         6312          274         >20.5
u                  288         6106          501         >20.3
w1                 667         5901          274         >20.2
m2                 642         5695          255         >20.9
w2                 593         5285          274         >20.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130831A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15161
SUBJECT: GRB 130831A: T100 observations
DATE:    13/09/01 19:05:58 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), U. Temiz (Cukurova Univ.), T. Guver (Sabanci
Univ.), Z. Eker (Akdeniz Univ.), S. Kaynar (TUG), E. Gogus (Sabanci Univ.),
H. Kirbiyik (TUG)  report on behalf of a larger collaboration

We observed the field of Swift  GRB 130831A (Hagen et al. GCN#15139)
with  the  1.0 meter  T100  telescope  (TUBITAK National  Observatory,
Antalya - Turkey),  starting August, 31; 18:27:23 UT (~ 5.4 hours after
the trigger). Observations were carried out in the R filter under moderate
weather conditions. We detected a new source in 300 s R band
image at a position that is consistent with Swift/UVOT (Hagen et al.
GCN#15139)
Using USNO-B1 star USNO-B1 1193-0589854  (RA=  23:54:29.226, Dec=
+29:23:08.41) in the field, the magnitude of the OT were estimated as;

t-t0 (hr)         exp.(s)      filt            mag             err (+/-)
5.38               300           R           17.98             0.034
5.48               300           R           17.99             0.035

Further observations using the same filter are ongoing.

We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their technical support.


GRB_name: GRB130831A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15162
SUBJECT: GRB 130831A: VLA Observations
DATE:    13/09/01 21:36:31 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer, and E. Berger (Harvard) report:

"We observed the position of GRB 130831A (Hagen et al; GCN 15139) with
the VLA beginning on 2013 September 1.19 UT (0.64 days after the burst). No
significant radio emission is detected at the enhanced Swift-XRT position
or the optical position, to a three-sigma upper limit of 38 uJy at 5.8 GHz
and 71 uJy at 21.8 GHz."


GRB_name: GRB130831B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15163
SUBJECT: GRB 130831B, Swift-BAT refined analysis
DATE:    13/09/01 21:51:29 GMT
FROM:    Tilan Ukwatta at MSU  <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),
A. Y. Lien (NASA/GSFC/ORAU), D. Malesani (DARK/NBI),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+902 sec from the
recent telemetry downlink, we report further analysis
of BAT GRB 130831B (trigger #568855) (Malesani, et al.,
GCN Circ. 15141). The BAT ground-calculated position is
RA, Dec = 192.454, -29.187 deg which is
   RA(J2000)  =  12h 49m 48.9s
   Dec(J2000) = -29d 11' 13.5"
with an uncertainty of 2.1 arcmin, (radius, sys+stat,
90% containment). The partial coding was 14%.

BAT mask-weighted light curve shows a multi peak
episode starting from ~T-12 sec highest peak
around T+1 sec and ending at ~T+30 sec.
T90 (15-350 keV) is 37.8 +- 10.4 sec
(estimated error including systematics).

The time-averaged spectrum from T-13.9 to T+30.6 sec
is best fit by a simple power-law model.  The power
law index of the time-averaged spectrum is 1.88 +- 0.21.
The fluence in the 15-150 keV band is
1.4 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak photon
flux measured from T-0.05 sec in the 15-150 keV band
is 2.4 +- 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/568855/BA/


GRB_name: GRB130831A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15164
SUBJECT: GRB 130831A: Continued Skynet/PROMPT-SSO, PROMPT-CTIO and Yerkes-41 detections
DATE:    13/09/02 01:57:04 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, J. Moore, N. Frank, V. 
Hoette, D. Harper, R. Kron, K. Cudworth, E. Struble, R. Russell, T. 
Berger, H. T. Cromartie, R. Egger, A. Foster, K. Ivarsen, M. Maples, M. 
Nysewander, and J. A. Crain report:

Skynet continued observing the Swift-XRT localization of GRB 130831A 
(Hagen et al., GCN 15139, Swift trigger 568849) with the four 17" 
telescopes of the PROMPT array at Siding Spring Observatory, NSW, 
Australia, four 16" telescopes of the PROMPT array at Cerro Tololo, 
Chile, and the 41" telescope of Yerkes Observatory in Wisconsin, USA. 
Starting at 2013-08-31, 13:39 UT and continuing until 2013-09-01, 17:40 
UT (t=35.5m-28.2h post-trigger), Skynet took a total of 2,227 exposures 
of 60-160s in the BVRI (PROMPT) and g'i' bands (Yerkes). As we reported 
in Trotter et al. (GCN 15148), we detect a bright fading afterglow in 
all bands at RA 23:54:29.8, Dec 29:25:46.4 (J2000), within the error 
circle of the Enhanced Swift-XRT localization (Evans et al., GCN 15147).

We continue to detect a fading afterglow in stacked images, with R~20 
mag at t~15h, and R~20.6 mag at t~25h.

A preliminary light curve that includes our first-day PROMPT-CTIO and 
Yerkes data, and our second-day PROMPT-SSO data is at:
http://skynet.unc.edu/grb/grb130831a_2.png

BVRI magnitudes are in the Vega system, and g'i' magnitudes are in the 
AB system, calibrated to 3 APASS stars in the field. Photometry has not 
been corrected for the modest expected line-of-sight Milky Way dust 
extinction E(B-V)=0.046 (Schlegel et al. 1998).

Skynet observations are ongoing.


GRB_name: GRB130831A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15165
SUBJECT: GRB 130831A: RATIR Optical and NIR Observations
DATE:    13/09/02 02:52:18 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130831A (Hagen, et al., GCN 15139) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/09 1.16 to 2013/09 1.49 UTC (14.65 to
22.73 hours after the BAT trigger), obtaining a total of 5.16 hours
exposure in the r' and i' bands and 2.09 hours exposure in the Z, Y, J, and
H bands.

For a source within the Swift-XRT error circle (Evans et al., GCN 15147),
in comparison with SDSS DR9 and 2MASS, we obtain the following detections:

  r'    20.64 +/- 0.03
  i'    20.38 +/- 0.03
  Z    20.20 +/- 0.07
  Y    19.69 +/- 0.07
  J    19.87 +/- 0.09
  H    19.88 +/- 0.14

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San
Pedro Mrtir.


GRB_name: GRB130831A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15166
SUBJECT: GRB 130831A: Optical Observations via Virtual Telescope, follow-up
DATE:    13/09/02 11:21:46 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy)
report:

On Sept 1.9197 2013 UT, we imaged the field around GRB
130831A (GCN 15139) 
remotely using the the 0.43m-f/6.8 robotic unit part of the
Virtual
Telescope robotic facility in Italy, about 33 hours after
the burst.

We co-added 12, 300-seconds unfiltered CCD images and
detected the afterglow at the same position we gave in GCN
15152. 

We performed photometry, assuming R-mags from UCAC-4 for the
stars in the
field, getting an estimate for the magnitude of 20.7 (CR).


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15167
SUBJECT: GRB 130831A: Montarrenti Observatory optical follow-up
DATE:    13/09/02 12:43:02 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

Simone Leonini, G. Guerrini, P. Rosi and L.M. Tinjaca Ramirez (Montarrenti 
Observatory, Siena, Italy) report:

We continue to observe and detect the fading optical afterglow of GRB 130831A 
(Swift trigger 568849, Hagen et al., GCN Circ. 15139) with the automatic 0.53m 
RC 
telescope + U47 detector at Montarrenti Observatory (Siena, Italy, IAU code 
C88).

We stacked 4 unfiltered CCD exposures of 60s each and we detect the very faint 
OT at the same position previously measured (GCN 15150) obtaining the 
following 
photometry at t~34h :

2013 Sep. 01.95733 UT R=20.46 +/- 0.24 

Magnitudes were obtained using Astrometrica software using USNO-B1 catalogue 
for positions and photometry. An ensemble of 66 stars were used for the 
magnitude 
comparison.


GRB_name: GRB130831A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15168
SUBJECT: GRB 130831A:  Swift/UVOT Observations
DATE:    13/09/02 14:17:51 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (PSU) and L.M.Z. Hagen (PSU) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130831A
(Hagen et al., GCN Circ. 15139) 191 seconds after the BAT trigger.
A source consistent with the enhanced XRT position (Evans et al.,
GCN Circ. 15147) is detected in the initial UVOT exposures.

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for the first finding chart (FC) exposures and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag
v                498          818           58      14.4 +/- 0.1
v              10802        11709          885      18.0 +/- 0.1
v              46801        47000          196      > 18.9

b               448           767           58      14.9 +/- 0.1
b             23522         23925          393      19.2 +/- 0.2
b             40193         41100          885      20.1 +/- 0.2

u_FC            191            441         246      14.6 +/- 0.1
u               572            742          39      13.9 +/- 0.1
u             16594          23517        1645      18.3 +/- 0.1

w1              548            849          40      13.9 +/- 0.1
w1            15688          16588         886      18.1 +/- 0.1

m2              673            843          39      13.6 +/- 0.1
m2            11714          12387         663      17.5 +/- 0.1

w2              474            494          19      14.8 +/- 0.1
w2             9896          10796         886      17.5 +/- 0.1
w2            41107          46795        1009      19.3 +/- 0.2

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.04 in the direction
of the burst (Schlegel et al. 1998).


GRB_name: GRB130903A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15169
SUBJECT: GRB 130903A: A long GRB detected by INTEGRAL
DATE:    13/09/03 02:03:32 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 70 s  has been detected by IBAS in the 
IBIS/ISGRI data at 00:47:20 UT of September 3.

Its refined  coordinates (J2000)  are:

  R.A.: 82.1334 deg
  DEC.: -0.1252 deg

with an uncertainty of 1.5 arcmin (90% c.l.).

The burst had a FRED profile and a fluence of about 10^-6 erg/cmq (20-200 
keV).

A plot of the light curve will be posted at 
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB130903A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15170
SUBJECT: GRB 130903A: GROND Upper Limits
DATE:    13/09/03 12:20:34 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

V. Sudilovsky, D. A. Kann, and J. Greiner (all MPE Garching) report on
behalf of the GROND team:

We observed the field of GRB 130903A (INTEGRAL trigger 6930; Mereghetti et
al. 2013, GCN #15169) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La
Silla Observatory (Chile).

Observations started at 07:07 UT on 03 Sep. 2013, 6.3 hours after the GRB
trigger, as soon as the GRB field became visible. They were performed at
an average seeing of 1".5 and at an average airmass of 1.7.

Based on an image with an exposure time of 25 min in g'r'i'z' and 20 min
in JHK, centered 7.37 hours after the GRB, we do not detect any
uncatalogued sources within the 90 arcsec INTEGRAL error circle in
comparison to the SDSS and 2MASS catalogs.


GRB_name: GRB130903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15171
SUBJECT: GRB 130903A: ISON-Kislovodsk optical Upper Limits
DATE:    13/09/03 13:21:41 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI),  V. Nevskiy (ISON),  I. Molotov (KIAM), A. Pozanenko 
(IKI),  report on  behalf of larger collaboration:

We observed the field of GRB 130903A (INTEGRAL trigger 6930; Mereghetti et 
al. 2013, GCN 15169)  with SANTEL-400AN (0.4-m f/3)  telescope of 
ISON-Kislovodsk observatory.Observations started on  Sep. 09 (UT) 01:11:40, 
i.e. 34 minutes after burst triger.   We obtained  several unfiltered images 
of 100 s exposure. We do not detect any source within 1.5 arcmin of error 
circle localization (Mereghetti et al. 2013, GCN 15169) .  Photometry of 
combined image is following

T_start,                     T0+,       Exp.,   Filter,  UL (3 sigma)
(UT)                          mid (d)    (s)

01:11:40T01:11:40      0.02363  1000    none     >19.6

and based on  SDSS  stars, R (gri -> R  transformations by Lupton 2005):

#   SDSS                      R        Err_R
1  J052835.34-000624.7 15.543 0.013
2  J052817.12-000749.0 14.650 0.012
3  J052841.64-000642.3 14.233 0.013

 Within error circle (Mereghetti et al. 2013, GCN 15169) we note a presence 
of  probable bright galaxy  J052830.20-000723.9 r=19.706
(however marked in SDSS-DR9 as point like object). 


GRB_name: GRB130903A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15173
SUBJECT: GRB 130903A: Swift-XRT observations
DATE:    13/09/03 20:11:17 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU) and Stephen Holland (STSCI) report on behalf of the
Swift team:

We have analysed 3.2 ks of XRT data for the INTEGRAL-detected burst:
GRB 130903A,  from 39.6 ks to 46.4 ks after the  INTEGRAL trigger. The
data are entirely in Photon Counting (PC) mode.  An X-ray source is
detected within the INTEGRAL error circle (Mereghetti et al., GCN circ.
15169). Using 1789 s of PC mode data and 1 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 82.13013, -0.12667
which is equivalent to:

RA (J2000): 05h 28m 31.23s
Dec(J2000): -00d 07' 36.0"

with an uncertainty of 4.3 arcsec (radius, 90% confidence). This
position is 12 arcsec from the INTEGRAL position.  Currently the source
has a 0.3-10 keV count rate in the Swift XRT of (4.9+4.9-3.0)e-3
counts/s.
We cannot determine at the present time whether the source is fading.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020294.

The Swift UVOT observed the field of GRB 130903A in V and U for 2462
and 780s, respectively. No optical counterpart was found. The 3-sigma
upper limits at the position of the X-ray source are 20.6 in V and 20.4
in U.


This circular is an official product of the Swift team.


GRB_name: GRB130831A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15174
SUBJECT: GRB 130831A: JCMT SCUBA-2 sub-mm observation
DATE:    13/09/04 02:01:33 GMT
FROM:    Ian Smith at Rice U  <ian@spacsun.rice.edu>

I.A. Smith (Rice U.), R.P.J. Tilanus (Leiden Observatory), N.R. Tanvir
(U. of Leicester), D.A. Frail (NRAO) report:

We observed the location of GRB 130831A (Hagen et al., GCN Circ.
15139) using the SCUBA-2 sub-millimeter continuum camera on the
James Clerk Maxwell Telescope.  The observation started at 14:13 UT
on 2013-08-31, corresponding to 69 minutes after the burst trigger.
Exposures totaling 2.0 hours were made in good weather conditions.
No source was detected, with a preliminary RMS of 1.4 mJy/beam at
850 microns and 13.7 mJy/beam at 450 microns.

We thank Callie McNew for the prompt support of these observations.


GRB_name: GRB130903A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15175
SUBJECT: GRB 130903A: Fermi GBM observation
DATE:    13/09/04 04:12:11 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) and Charles Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 00:47:32.37 UT on 03 September 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130903A (trigger 399862055 / 130903033),
which was also detected by the INTEGRAL (Mereghetti et al., GCN 15169) and
Swift/XRT (Grupe et al., GCN 15173).
The GBM on-ground location is consistent with the INTEGRAL and Swift position.
The angle from the Fermi LAT boresight is 33 degrees.

The GBM light curve consists of multiple pulses
with a duration (T90) of about 69 +/- 7 s (50-300 keV).
The time-averaged spectrum from T0-2 s to T0+68 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.70 +/- 0.27 and
the cutoff energy, parameterized as Epeak, is 41 +/- 3 keV.

The event fluence (10-1000 keV) in this time interval is
(2.0 +/- 0.1)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.22 s in the 10-1000 keV band
is 1.3 +/- 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: GRB130903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15176
SUBJECT: GRB 130903A: MASTER early optical limit
DATE:    13/09/04 10:07:29 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy,  V. Lipunov, D. Denisenko, V. Kornilov,  A. 
Kuznetsov, D. Kuvshinov, N. Tyurina, N. Shatskiy, P. Balanutsa, D.
Zimnukhov, V.V. Chazov
Lomonosov Moscow State University, Sternberg Astronomical Institute

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V. Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk
Irkutsk State University

V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

V. Krushinski, I. Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University

H. Levato and C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez and F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB130903A 240 sec after notice 
time and 244 sec after GRB time at 2013-09-03 00:51:36 UT in two 
polarizations. Some delay was due to weather condition. On our first (40s 
exposure) set we haven't found optical 
transient  within INTEGRAL error-box (S.Mereghetti et. al. GCN-15169 ).
The 5-sigma upper limit has been about 15.0 mag in each of polarization.

On best coadd image (with use of the first 12 sets on 6 in each of 
polyarization)  with total exposition 900 sec and middle time 504 after 
GRB time upper limit is 17.5 mag.

More detailed information in the following table:

   T_start  T_finish  T_mid     t_mid-t_trig  Exptime   Filter Limit  Coadd
---------------------------------------------------------------------------
00:51:36  00:52:16  00:51:36     264 s        40 s       P|   15.0     no
00:51:36  00:52:16  00:51:36     264 s        40 s       P-   15.0     no
00:51:36  00:52:16  00:51:36     264 s        80 s    P| + P- 15.5      2
00:51:36  01:00:16  00:55:56     504 s       450 s       P|   17.0      6
00:51:36  01:00:16  00:55:56     504 s       450 s       P-   17.0      6
00:51:36  01:00:16  00:55:56     504 s       900 s    P| + P- 17.5     12

P-  and P| is a RA and DEC orientated polaroids.

The message may be cited.


GRB_name: GRB130903A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15177
SUBJECT: GRB 130903A: GROND Afterglow Discovery
DATE:    13/09/04 15:02:41 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

M. Tanga, V. Sudilovsky, D. A. Kann, and J. Greiner (all MPE Garching)
report on behalf of the GROND team:

We re-observed (Sudilovsky et al., GCN #15170) the field of GRB 130903A
(Mereghetti et al. 2013, GCN #15169) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG/ESO
telescope at La Silla Observatory (Chile).

Observations are centered at 09:19 UT on 04 Sep 2013, 35.53 hours after
the GRB trigger, with a total exposure time of 50 min in g'r'i'z' and 40
min in JHK. They were performed at an average seeing of 1".1 and an
average airmass of 1.3.

In the XRT error circle given by Grupe & Holland (GCN #15173), we detect a
source in our first epoch observations (Sudilovsky et al., GCN #15170) at
coordinates

RA (J2000) = 05:28:31.33
Dec. (J2000) = -00:07:38.4

with an error of 0".3 arcseconds.

For the first epoch, we derive preliminary magnitudes (AB system) of:

g' = 22.4 +/- 0.1,
r' = 22.2 +/- 0.1,
i' = 22.0 +/- 0.1,
z' = 21.7 +/- 0.1,
J > 21.6,
H > 20.8, and
K > 20.1.

The source is still detected in g'r'i'z' in the second epoch, but is seen
to have faded by 1 mag in the r' band. We therefore conclude that this is
the afterglow of GRB 130903A.

Magnitudes were obtained against the SDSS catalog in g'r'i'z' and against
the 2MASS catalog in JHK. They have not been corrected for the expected
Galactic extinction of E(B-V) = 0.14 mag in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130822A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15178
SUBJECT: GRB 130822A: nearby galaxy redshifts
DATE:    13/09/04 18:40:36 GMT
FROM:    Klaas Wiersema at U Leicester  <kw113@leicester.ac.uk>

K. Wiersema (Leicester), A. Levan (Warwick),  S. B.  Cenko (NASA/GSFC) 
and N. Tanvir (Leicester) report on behalf of a larger collaboration:

We acquired spectroscopy of two galaxies close to the afterglow position
of short GRB 130822A (Kocevski et al. GCN 15112), these galaxies have low chance
coincidence probability values (note that there are no sources found within the
XRT error circle, Cenko et al. GCN 15121).
These two galaxies, hereafter named G1 and G2, are located at approximate
positions (SDSS DR10):

G1
RA:   01:51:42.66
Dec: -03:12:25.48

G2
RA:   01:51:41.09
Dec: -03:11:07.47

A finder chart showing the locations of these galaxies (Gemini i' band; 
Cenko et al. GCN 15121) can be found here:
http://www.star.le.ac.uk/~kw113/G1G2.png

We acquired spectroscopy with ACAM on the William Herschel Telescope
(directly following the photometry observations reported in Wiersema
et al. GCN 15119) and GMOS on Gemini-North (starting at 13:35 UT on
2 September 2013). In both cases the slit was aligned such that both
galaxies were covered simultaneously by the slit. The ACAM spectrum
covers the range 3500-9400, the Gemini spectrum the range 3850-6730 A.

Galaxy G1 shows strong absorption complexes (G band, Mg b triplet, Fe 4668,
Ca II) as well as a single, weak, emission line (H beta), at a common redshift z=0.154.
Galaxy G2 shows stronger emission lines of H alpha and H beta, as well as absorption
complexes (G band, Na I, Mg b triplet) at a common redshift z=0.045.
At these redshifts, the offset from the afterglow to galaxy G1 is 58 kiloparsec,
and to G2 72 kiloparsec.
If the brighter, but somewhat further offset, galaxy G2 is the host galaxy, it would
place GRB 130822A within the Advanced LIGO / Virgo horizon.


GRB_name: GRB130831A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15179
SUBJECT: GRB 130831A: RATIR Optical and NIR Upper Limits
DATE:    13/09/04 18:43:54 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Alan M. Watson (UNAM), Owen Littlejohns (ASU), Nat Butler (ASU),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G.
Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirez-Ruiz (UCSC), Jos A. de
Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

We again observed the field of GRB 130831A (Hagen, et al., GCN 15139) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional
on Sierra San Pedro Mrtir from 2013/09 4.32 to 2013/09 4.34 UTC (90.60
to 91.04 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r' and i' bands and 0.15 hours exposure in the Z,
Y, J, and H bands.

For a source within the Swift-XRT error circle (Evans et al., GCN 15147),
in comparison with SDSS DR9 and 2MASS, we obtain the following upper limits
(3-sigma):

  r'    > 22.84
  i'    > 22.94
  Z     > 20.76
  Y     > 20.23
  J     > 20.09
  H     > 19.49

In comparison with earlier RATIR observations (Butler et al., GCN 15165)
the source has faded by 2.2 magnitudes in the r' band and 2.6 magnitudes
in the i' band. This implies a power-law decay steeper than t^-1.7. The
upper limits obtained in the Z, Y, J, and H bands are also consistent with
such a steep decay index. These magnitudes are in the AB system and not
corrected for Galactic extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130903A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15181
SUBJECT: GRB 130903A: Swift/UVOT Upper Limits
DATE:    13/09/05 20:58:15 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and Dirk Grupe (PSU)
report on behalf of the Swift/UVOT team:

     The Swift/UVOT began observations of the field of GRB 130903A
starting 44.1 ks after the INTEGRAL/IBAS trigger (Mereghetti et
al. 2013, GCNC 15169).  We do not detect any new source consistent
with the GROND afterglow position (Tanga et al. 2013, GCNC 15177) in
any of the UVOT exposures.  Preliminary 3-sigma upper limits using the
UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358,
373) for the summed exposures are presented below.

---------------------------------------------------
Filter       TSTART      TSTOP    Exposure      Mag
---------------------------------------------------
    v        44,128     51,114        2461    >21.2
    u        45,378     51,795        1442    >21.3
---------------------------------------------------

     The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.12 mag (Schlafly et al. 2011, ApJS, 737,
103).


GRB_name: GRB130907A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15183
SUBJECT: GRB 130907A: Swift detection of a burst with an optical counterpart
DATE:    13/09/07 21:53:31 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. J. Page (UCL-MSSL), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
V. N. Yershov (UCL-MSSL) report on behalf of the Swift Team:

At 21:41:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130907A (trigger=569992).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 215.877, +45.616 which is 
   RA(J2000) = 14h 23m 31s
   Dec(J2000) = +45d 36' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex multi-peaked
structure with a duration of about 120 sec.  The peak count rate
was ~60000 counts/sec (15-350 keV), at ~25 sec after the trigger. 

The XRT began observing the field at 21:42:19.3 UT, 66.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 215.8926, 45.6094 which is equivalent to:
   RA(J2000)  = +14h 23m 34.22s
   Dec(J2000) = +45d 36' 33.8"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 45 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 0.1 s image was 6.33e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 74 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 14:23:34.03 = 215.89181
  DEC(J2000) = +45:36:27.1  =  45.60753
with a 90%-confidence error radius of about 0.61 arc sec. This position is 7.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.55 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is M. J. Page (m.page AT 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: GRB130907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15184
SUBJECT: GRB 130907A: MASTER early OT observations
DATE:    13/09/07 22:14:19 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, 
N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, 
D.Denisenko, A.Sankovich
Sternberg Astronomical Institute, Moscow State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB130907A 18 sec  after notice 
time and 43 sec after GRB time at 2013-09-07  21:42:00 UT in two 
polarizations. On our first images we  found optical transient  within 
SWIFT error-box (Page et. al. GCN15183). The object approximate magnitude 
is about 15.0 mag.
Observations are made at very long zenith distance z=86 deg.

The observations and reduction is continued.
The message may be cited.


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15185
SUBJECT: GRB 130831A: ISON-UAFO optical observations
DATE:    13/09/07 23:20:51 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Matkin (UAFO, ISON), A. Stepura (UAFO, ISON), I. 
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB 
follow-up collaboration:

We observed the afterglow (Hagen et al., GCN  15139; Guidorzi et al., 
GCN 15140) of the Swift GRB 130831A (Hagen et al., GCN  15139) with 
SANTEL-650 (0.65m) and VT-50 (0.5m)  telescopes of UAFO/ISON-Ussuriysk 
observatory  starting on  Aug. 31  (UT) 13:14:32, i.e. 10.3  minutes 
after burst trigger.  We took unfiltered  images of 120s and 30s 
exposures  ending observations at (UT) 19:20:53.

In each initial frames we clearly detect afterglow. A preliminary 
photometry of the afterglow in the initial frames are following

T_start              T0+       Filter, Exposure, OT,    OT_err
(UT)                 (mid, d)            (s)

2013-08-31T13:14:32  0.00782   none    120       13.86  0.02
2013-08-31T13:l6:40  0.00931   none    120       13.75  0.02
2013-08-31T13:18:49  0.01080   none    120       13.78  0.02

The photometry is based on reference stars SDSS-DR9, (R mag, 
transformation by Lupton 2005)

N SDSS id   R(Lupton)errR
1 J235443.71+292539.3 13.491  0.016
2 J235438.60+292547.3 14.136  0.015
3 J235423.64+292452.8 17.120  0.016


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15186
SUBJECT: GRB 130831A: optical observation in Gissar AO
DATE:    13/09/07 23:43:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), N. Minikulov (Institute of Astrophysics), M.Gulyamov 
(Institute of Astrophysics), I. Molotov (KIAM), A. Pozanenko (IKI) 
report on behalf of  larger GRB follow-up collaboration:

We observed the afterglow  (Hagen et al., GCN  15139; Guidorzi et al., 
GCN 15140) of the Swift GRB 130831A (Hagen et al., GCN  15139)  with 
AZT-8 (0.7m) telescope of Gissar observatory in R filter starting on 
Aug. 31 (UT) 17:47:54. A preliminary photometry of combined image is 
based on  SDSS DR9 stars

T_start              T0+       Filter, Exposure, OT,    OT_err
(UT)                 (mid, d)            (s)

2013-08-31T17:47:54  0.21932   R       57x60     18.28  0.04

Reference stars SDSS-DR9, (R mag, transformation by Lupton 2005)

N SDSS id   R(Lupton)errR
1 J235443.71+292539.3 13.491  0.016
2 J235438.60+292547.3 14.136  0.015
3 J235423.64+292452.8 17.120  0.016


GRB_name: GRB130907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15187
SUBJECT: GRB 130907A: NOT redshift
DATE:    13/09/07 23:44:37 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), 
J. Gorosabel (IAA-CSIC/UPV-EHU), P. Jakobsson (U. Iceland) and J. Kajava (NOT) report 
on behalf of a larger collaboration:

We observed the optical afterglow of GRB 130907A (Page et al., GCN 15183; Gorbovskoy
et al., GCN 15184) with the NOT equipped with the AlFOSC spectrograph and camera. 
The transient is clearly detected in our acquisition images, taken in a clear filter, at the 
following coordinates:

RA(J2000) = 14:23:34.08
Dec(J2000) = +45:36:26.7

Using R-band values from nearby USNO stars, we get a magnitude R = 16.7 +- 0.1 at a 
mean time of 0.41 hr after the GRB, where the error is dominated by calibration 
uncertainties.

A single spectrum of 900 s covering the range from 3800 to 8000 AA, with a resolution of 
~700, was obtained with a mean epoch of 0.598 hr after the burst. The spectrum presents 
a strong continuum with deep spectral features of AlIII, FeII, MgII and MgI at a common 
redshift of z=1.238 (wavelength calibration based on archival data), which we identify as 
the redshift of the GRB.


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15188
SUBJECT: GRB 130831A: ISON-Kislovodsk optical observations
DATE:    13/09/07 23:52:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI),  V. Linkov (ISON), K. Polyakov (ISON), D. Ivanov 
(ISON), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of 
larger GRB follow-up collaboration:

We observed the afterglow (Hagen et al., GCN  15139; Guidorzi et al., 
GCN 15140) of the Swift GRB 130831A (Hagen et al., GCN  15139) with 
SANTEL-400AN  telescope of ISON-Kislovodsk observatory  starting on 
Aug. 31  (UT) 19:12:30.  We took several unfiltered  images. Preliminary 
photometry of combined images is following

T_start              T0+       Filter, Exposure, OT,    OT_err
(UT)                 (mid, d)            (s)

2013-08-31T19:12:30  0.26113   none    840       18.32  0.08
2013-08-31T19:28:20  0.27212   none    840       18.44  0.10
2013-08-31T19:47:24  0.29470   none    1760      18.47  0.13

The photometry is based on reference stars SDSS-DR9, (R mag, 
transformation by Lupton 2005)

N SDSS id   R(Lupton)errR
1 J235443.71+292539.3 13.491  0.016
2 J235438.60+292547.3 14.136  0.015
3 J235423.64+292452.8 17.120  0.016


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15189
SUBJECT: GRB 130831A: optical observation in Chuguev AO
DATE:    13/09/07 23:56:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), Yu. Krugly (IA KhNU), I. Slyusarev (IA KhNU), I. 
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB 
follow-up collaboration:

We observed the afterglow  (Hagen et al., GCN  15139; Guidorzi et al., 
GCN 15140) of the Swift GRB 130831A (Hagen et al., GCN  15139)  with 
AZT-8 (0.7m) telescope of Institute of Astronomy, Kharkiv National 
University in R filter starting on Sep. 01 (UT) 19:37:49.  A preliminary 
photometry of combined images is based on  SDSS DR9 stars

T_start              T0+       Filter, Exposure, OT,    OT_err
(UT)                 (mid, d)            (s)

2013-09-01T19:37:49  1.29474   R       28x120    21.26   0.07

Reference stars SDSS-DR9, (R mag, transformation by Lupton 2005)

N SDSS id   R(Lupton)errR
1 J235443.71+292539.3 13.491  0.016
2 J235438.60+292547.3 14.136  0.015
3 J235423.64+292452.8 17.120  0.016


GRB_name: GRB130831A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15190
SUBJECT: GRB 130831A: Maidanak optical observations
DATE:    13/09/08 00:17:41 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI), B. Hafizov (UBAI), O. Burhonov 
(UBAI) report on behalf of larger GRB follow-up collaboration:

We observed the afterglow  (Hagen et al., GCN  15139; Guidorzi et al., 
GCN 15140) of the Swift GRB 130831A (Hagen et al., GCN  15139)  with 
AZT-22 telescope equipped with SNUCAM of Maidanak observatory in R 
filter.  A preliminary photometry of combined images is based on  SDSS 
stars (see at the bottom):

T_start              T0+       Filter, Exposure, OT
(UT)                 (mid, d)            (s)

2013-09-02T13:58:23  2.0410    R       1x600     22.20 +/- 0.10
2013-09-04T18:47:13  4.2555    R       5x600     22.53 +/- 0.07
2013-09-05T18:57:03  5.2658    R       6x600     22.90 +/- 0.07

A preliminary lc of the afterglow GRB 130831A based on our GCNs ##15185, 
15186, 15188, 15189  and reported in this circular can be found in 
http://grb.rssi.ru/GRB130831A/grb130831A_lc_preliminary.PNG

A power-law decay of the lc between 0.1 days and 2 days after trigger is 
-1.68 +/- 0.06  and marginally consistent with power-law decay reported 
by Watson (GCN 15179).

Reference stars

N SDSS id   R(Lupton)errR
1 J235443.71+292539.3 13.491  0.016
2 J235438.60+292547.3 14.136  0.015
3 J235423.64+292452.8 17.120  0.016


GRB_name: GRB130907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15191
SUBJECT: GRB 130907A: Skynet DSO-14/Yerkes-41 detections of a possible afterglow
DATE:    13/09/08 02:40:43 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, A. LaCluyze, J. Moore, N. Frank, D. Reichart, A. 
Smith, D. Caton, L. Hawkins, V. Hoette, D. Harper, R. Kron, K. Cudworth, 
E. Struble, R. Russell, T. Linder, T. Berger, H. T. Cromartie, R. Egger, 
A. Foster, K. Ivarsen, M. Maples, M. Nysewander, and J. A. Crain report:

Skynet observed the Swift/XRT localization of GRB 130907A (Page et al., 
GCN 15183, Swift trigger 569992) with the 14" telescope at the 
Appalachian State University Dark Sky Observatory (DSO-14) in NC, USA (R 
and I bands), and with the 41" telescope of Yerkes Observatory in WI, 
USA (r' and i' bands).

Starting at 2013-09-08, 00:43 UT (t=3.03h post-trigger) and continuing 
until 17:41 UT (t=35.5m-4.65h post-trigger), Skynet took a total of 42 
160s exposures. We detect an uncatalogued optical source in stacked 
images at RA 14:23:34.03, Dec +45:36:26.7 (J2000), consistent with the 
afterglow position reported by de Ugarte Postigo et al. (GCN 15187), and 
~8" south of the Swift-XRT localization. At t=3.4h post-trigger, R~19.6 
mag. The time range of our observations is not sufficient to confirm 
whether the source is indeed fading.

A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130907a.png

R and I magnitudes are in the Vega system, and r' and i' are in the AB 
system, calibrated to 5 APASS stars in the field. Magnitudes have not 
been corrected for line-of-sight Milky Way dust extinction with expected 
E(B-V)=0.011 (Schlegel et al. 1998).

Skynet observations are ongoing.


GRB_name: GRB130907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15192
SUBJECT: GRB 130907A: RATIR Optical and NIR Afterglow Confirmation
DATE:    13/09/08 05:11:53 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

William H. Lee (UNAM), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130907A (Page et al., GCN 15183) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/09 8.14 to 2013/09 8.15 UTC (5.57
to 6.03 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r and i bands and 0.15 hours exposure in the Z,
Y, J, and H bands.

We detect a source at 14:23:34.01 +45:36:27.0 J2000 (+/- 0.5") with

  r = 20.01 +/- 0.03
  i = 19.30 +/- 0.02
  Z = 18.78 +/- 0.05
  Y = 18.48 +/- 0.06
  J = 18.13 +/- 0.06
  H = 17.63 +/- 0.05

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

This source is outside the Swift-XRT error circle, but is only 0.8
arcsec from the transient source reported by de Ugarte Postigo et al.
(GCN 15187) and 0.2 arcsec from the transient source reported by Trotter
et al. (GCN 15191). From the close positional coincidence and fading
magnitudes (r of 16.7, 19.6, and 20.0), we conclude all three
observations are of the optical transient.

The transient source is 0.5 arcsec from the faint galaxy SDSS
J142333.95+453626.2, but is 1-2 magnitudes brighter in riZ.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15193
SUBJECT: GRB 130907A: Skynet DSO-14/Yerkes-41/GORT confirmation of a fading afterglow
DATE:    13/09/08 06:28:32 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, J. Haislip, A. LaCluyze, K. McLin, L. Cominsky, 
A. B. Smith, D. Caton, L. Hawkins, V. Hoette, K. Cudworth, D. Harper, R. 
Kron, T. Linder, R. Russell, E. Struble, T. Berger, H. T. Cromartie, R. 
Egger, A. Foster, N. Frank, K. Ivarsen, M. Maples, J. Moore, M. 
Nysewander, and J. A. Crain report:

In Trotter et al. (GCN 15191), we reported Skynet observations of the 
Swift/XRT localization of GRB 130907A (Page et al., GCN 15183, Swift 
trigger 569992) with the 14" telescope at the Appalachian State 
University Dark Sky Observatory (DSO-14) in NC, USA (R and I bands), and 
with the 41" telescope of Yerkes Observatory in WI, USA (r' and i' 
bands). Skynet continued observing the field with the 14" GLAST Optical 
Robotic Telescope (GORT) at the Hume observatory in CA, USA.

 From t=5.9h - 8.2h post-trigger, GORT took a total of 54x160s exposures 
in the R and I bands. We confirm a fading afterglow at the position 
reported by de Ugarte Postigo et al. (GCN 15187) and by Lee et al. (GCN 
15192). The afterglow fades from I=18.1 mag at t=3.2h to I=19.2 mag at 
t=8.2h, consistent with a power-law index alpha~-0.9.

A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130907a_2.png

R and I magnitudes are in the Vega system, and r' and i' magnitudes are 
in the AB system, calibrated to 5 APASS stars in the field. Magnitudes 
have not been corrected for line-of-sight Milky Way dust extinction, 
with expected E(B-V)=0.011 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15194
SUBJECT: GRB 130907A: Early Tautenburg detections, red afterglow
DATE:    13/09/08 13:13:03 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

S. Schmidl (TLS Tautenburg), D. A. Kann (MPE Garching), S. Klose, S. 
Stecklum, F. Ludwig (all TLS Tautenburg), and J. Greiner (MPE Garching)
report:

We observed the field of the intense GRB 130907A (Swift trigger 569992,
Page et al., GCN #15183) with the 1.34m Tautenburg Schmidt telescope.

Starting at 22:02:18 UT (21 minutes after the trigger), we obtained in
total 3 x 120 sec Ic-band images and 12 Rc-band images of 120 sec and 60
sec exposure. Observations were obtained at high airmass of 2.6 - 3.2. The
afterglow is clearly detected on all frames.

Using the star at RA (J2000) = 14:23:28.93, Dec. (J2000) = +45:37:33.65,
for which we derive Rc = 15.10, Ic = 14.51 using SDSS magnitudes and the
transformations of Lupton (2005), we derive preliminary magnitudes for the
first image in each filter of:

Time (d) Filter mag error
0.0152  Ic  15.26 0.03
0.0172  Rc  16.57 0.03

not corrected for the very small reddening of 0.01 mag along the line of
sight (Schlegel et al. 1998).

We note Swift was slewing when GRB 130907A started, the extended raw BAT
light curve (http://gcn.gsfc.nasa.gov/notices_s/sw00569992000msbx.gif)
shows the GRB began about 120 seconds before Swift T_0. Adding this time
to our observing times, we find the data is well-described by a single
power-
law decay with alpha = 1.39 +/- 0.02. The detection by Trotter et al. (GCN
#15191) agrees excellently with the extrapolation of our data, while the
RATIR detection (Lee et al., GCN #15192), after transforming to Vega mag,
indicates that the decay has slowed, which is confirmed by Trotter et al.
(GCN #15193). The very early detection by Gorbovskoy et al. (GCN #15184)
lies several magnitudes under a back-extrapolation of our data.

We derive a very large Rc-Ic color of about 1.2 mag from the fit, 
indicating possible strong reddening (see also the Skynet light curve, GCN
#15193, and the multicolor RATIR mags, GCN #15192), which would be in
accordance with the very strong absorption lines detected by de Ugarte
Postigo et al. (GCN #15187).

This message may be cited.


GRB_name: GRB130907A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15195
SUBJECT: GRB 130907A: Swift/UVOT Detection
DATE:    13/09/08 17:37:39 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 130907A
74 s after the BAT trigger (Page et al., GCN Circ. 15183).
A source consistent with the XRT position (Page et al. GCN Circ. 15183) 
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  14:23:34.04 = 215.89183 (deg.)
  Dec (J2000) = +45:36:27.1  =  45.60753 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

white               74          224          147         15.45 +/- 0.02
v                  616          636           20         16.29 +/- 0.16
b                  542          562           20         16.78 +/- 0.12
u                  286          536          246         15.87 +/- 0.04
w1                 666         1113          117         18.54 +/- 0.31
m2     641         1606          117         >19.2
w2                 592          786         38         >18.7

The magnitudes in the table 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: GRB120916A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15196
SUBJECT: GRB 120916A: Fermi-LAT detection of a burst
DATE:    13/09/08 18:45:43 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford), D. Kocevski(NASA/Goddard), J. Racusin
(NASA/Goddard), and V. Connaughton (UAH) report on behalf of the
Fermi-LAT team:

On Sept. 8th, 2013, Fermi LAT detected high energy emission from GRB
130907A, which triggered Swift at T0 = 21:41:13 UT (GCN 15183).

Fermi was passing through the South Atlantic Anomaly around T0,
therefore data taking was disabled and neither Fermi/GBM nor Fermi/LAT
could trigger on the burst. Fermi exited the SAA and resumed data
taking at ~T0+1300 s.

The burst was ~150 deg from the LAT boresight when Fermi resumed data
taking, and entered the LAT FOV at ~T0+3400 s. A likelihood analysis
in the time interval T0+3400 s - T0+20 ks (with a ~8000 s exposure)
resulted in a detection of the source with a significance of ~6 sigma
at the NOT position (GCN Circ. 15187).

In particular, a 55 GeV photon compatible with the position of the
burst was observed at ~T0+18 ks.

The Fermi LAT point of contact for this burst is Daniel Kocevski
(daniel.kocevski@nasa.gov).

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.


GRB_name: GRB130907A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15198
SUBJECT: GRB 130907A: Enhanced Swift-XRT position
DATE:    13/09/08 20:33:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 11208 s of XRT Photon Counting mode data and 18 UVOT
images for GRB 130907A, 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 = 215.89216, +45.60725 which is equivalent
to:

RA (J2000): 14h 23m 34.12s
Dec (J2000): +45d 36' 26.1"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15199
SUBJECT: GRB 130907A: Swift-XRT refined Analysis
DATE:    13/09/08 21:53:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.A. Kennea (PSU), P.A. Evans (U. Leicester), B.P.
Gompertz (U. Leicester), J.P. Osborne (U. Leicester), V. D'Elia (ASDC),
A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), V. Mangano (PSU) and
M.J. Page report on behalf of the Swift-XRT team:

We have analysed 20 ks of XRT data for GRB 130907A (Page  et al. GCN
Circ. 15183),  from 70 s to 60.0 ks after the  BAT trigger. The data
comprise 3.7 ks 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 15198).

The late-time light curve (from T0+5.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.686 (+0.017, -0.016).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.761 (+0.015, -0.014). The
best-fitting absorption column is  1.96 (+0.05, -0.04) x 10^21 cm^-2,
in excess of the Galactic value of 1.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.98 (+/-0.06) and a
best-fitting absorption column of 1.85 (+0.17, -0.16) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.9 x 10^-11 (5.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.85 (+0.17, -0.16) x 10^21 cm^-2
Galactic foreground: 1.0 x 10^20 cm^-2
Excess significance: 17.7 sigma
Photon index:      1.98 (+/-0.06)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00569992.

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


GRB_name: GRB130907A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15200
SUBJECT: GRB 130907A: VLA detection
DATE:    13/09/08 22:25:42 GMT
FROM:    Alessandra Corsi at GWU  <corsi@email.gwu.edu>

A. Corsi (GWU) reports on behalf of a larger collaboration:
 
We imaged the position of GRB 130907A (Page et. al. GCN 15183) 
with the Karl G. Jansky Very Large Array (VLA) in K-band, starting at 
about 4 hours after the burst. A provisional reduction shows a source 
consistent with the location of the GRB optical afterglow reported by 
de Ugarte Postigo et al. (GCN 15187). At this time, we estimate a 
preliminary flux of about 1.2 mJy at 24.5 GHz.
 
Further observations are planned.


GRB_name: GRB130907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15201
SUBJECT: GRB 130907A: T21 optical observations
DATE:    13/09/08 22:35:10 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen, Harri Vilokki and Tuomo Salmi (Taurus
Hill Observatory, Varkaus, Finland) report:

We have detected GRB 130907A optical afterglow at iTelescope observatory
T21 (Mayhill, New Mexico) 0.43-m/6.8 astrograph and FLI-PL6303E CCD. 
Six unfiltered images and seven photometric R filter images with 300 sec
were made.

The afterglow was detected at the following position RA 14:23:34.06 and
DEC +45:36:27.1 J2000.

The following magnitudes were obtained from the observations using 
NOMAD1 1356-0257141 (R=15.220) as a comparison star:

Tmid(h)+T0     Filter             Exp. time     Mag             Mag err. 
4.70                 unfiltered        3x300         20.00CR       0.49
5.22                 R                   7x300         20.06R          0.47
5.77                 unfiltered        3x300         20.36CR       0.47


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15202
SUBJECT: GRB 130907A, Swift-BAT refined analysis
DATE:    13/09/09 01:35:56 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

J. R. Cummings (GSFC/UMBC),S. D. Barthelmy (GSFC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
M. J. Page (UCL-MSSL),D. M. Palmer (LANL),T. Sakamoto (AGU),
M. Stamatikos (OSU),J. Tueller (GSFC),T. N. Ukwatta (MSU)
(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 130907A (trigger #569992)
(Page, et al., GCN Circ. 15183).  The BAT ground-calculated position is
RA, Dec = 215.898, 45.602 deg which is
    RA(J2000)  =  14h 23m 35.5s
    Dec(J2000) = +45d 36' 08.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a very complicated structure with six main
peaks from T-55 sec to T+95 sec.  Each of these peaks shows several sub-peaks.
The strongest peak is at ~T+57 sec.  After T+95 sec, the count rate drops
significantly, but doesn't return all the way to the background level.  Then
there is another weak, soft peak from T+210 sec to T+240 sec. This late peak
is coincident with the start of a long flare seen in the XRT. There may be
further BAT emission beyond the end of the currently available event data.
T90 (15-350 keV) is 115.14 +- 0.67 sec (estimated error including systematics).

The time-averaged spectrum from T-50.7 to T+234.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.11 +- 0.02.  The fluence in the 15-150 keV band is 1.2 +- 0.0 x 10^-4 erg/cm2.
The 1-sec peak photon flux measured from T+57.66 sec in the 15-150 keV band
is 25.6 +- 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/569992/BA/


GRB_name: GRB130907A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15203
SUBJECT: Konus-Wind observation of GRB 130907A
DATE:    13/09/09 10:52:42 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 130907A
(Swift-BAT trigger 569992: Page, et al., GCN 15183;
Cummings, et al., GCN 15202)
triggered Konus-Wind at T0=77955.997 s UT (21:39:15.997),
or ~118 s before the BAT trigger.

The burst light curve shows multiple bright, partially overlapped
pulses from ~T0-4 s till ~T0+210~s.
The emission is seen up to ~15 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130907_T77955/

As observed by Konus-Wind, the burst
had a fluence of (7.9  0.5)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+139.008 s,
of (2.2  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+206.080 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.91  0.02,
the high energy photon index beta = -2.42  0.07,
the peak energy Ep = 394  11 keV,
chi2 = 90/92 dof.

The spectrum near the maximum count rate
(measured from T0+139.264 s to T0+143.872 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.65  0.03,
the high energy photon index beta = -2.22  0.05,
the peak energy Ep = 390  16 keV,
chi2 = 111/96 dof.

Assuming the NOT redshift z=1.238 (de Ugarte Postigo, et al., GCN 15187),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters of GRB 130907A:
the isotropic energy release E_iso is (3.3  0.1)x10^54 erg,
the peak luminosity L_iso is (2.0  0.1)x10^53 erg/s,
and the rest-frame peak energy Ep,i = (880  25) keV

All the quoted results are preliminary.


GRB_name: GRB130907A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15204
SUBJECT: GRB 130907A: INTEGRAL/SPI-ACS light curve
DATE:    13/09/09 15:33:25 GMT
FROM:    Volker Beckmann at APC  <beckmann@apc.univ-paris7.fr>

V. Savchenko, V. Beckmann (APC), C. Ferrigno, E. Bozzo, M. Beck (ISDC),
J. Borkowski (CAMK/Torun), D. Gtz (CEA/Saclay), S. Mereghetti (INAF/IASF-Milano), A. von Kienlin, A. Rau  (MPE), and K. Hurley (SSL/Berkeley)

GRB 130907A, detected by Swift/BAT (Palmer et al. GCN 15183), Fermi/LAT (Vianello et al. GCN 15196) and Konus-Wind (Frederiks et al, GCN 15203), has been independently detected by the SPI Anti-Coincidence System (ACS) on-board INTEGRAL. The SPI-ACS light curve reveals the rich multi-peak structure of this burst starting at 2013-09-07T21:39:16. Several bright peaks are followed by a major activity episode at about T0+100s. The maximum count-rate of 94,000 counts/sec (approximately corresponding to 1e-5 erg/cm2/s in the 75 keV-1 MeV range, Vigano and Mereghetti 2009) over the time bin length of 50 msec is reached at T0+115s. The total duration of this GRB is
about 250 seconds.

The SPI-ACS light curve of this GRB is available at:
http://www.isdc.unige.ch/integral/ibas/cgi-bin/ibas_acs_web.cgi/?trigger=2013-09-07T21-39-16.00-00000-00000-0

All SPI-ACS light curves are available (both as images and data files) at http://isdc.unige.ch/Soft/ibas/ibas_acs_web.cgi.
The light curves, binned at 50 ms, are derived from 91 independent detectors with different lower energy thresholds (mainly between 50 keV and 150 keV). SPI-ACS has no upper energy threshold and can detect photons with energies up to at least 100 MeV. The ACS response varies as a function of the GRB incident angle. For these reasons we caution that the count rates cannot be easily translated into physical flux units.


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15205
SUBJECT: GRB 130907A:  Further Swift-BAT refined analysis
DATE:    13/09/09 19:41:01 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA), J. R. Cummings (GSFC/UMBC), D. M. Palmer (LANL),
C. B. Markwardt (GSFC) for the Swift-BAT team):

Using the complete data set from T-239 to T+963 sec, we report further analysis 
of BAT GRB 130907A (trigger #569992) (Page, et al., GCN Circ. 15183).  The 
initial report on the BAT data was presented in Cummings, et al., GCN Circ. 15202.

The burst started while Swift was slewing from another target, and the burst 
location came into the BAT coded field of view at about T-80 seconds. The 
initial pair of peaks at T-117 that triggered Konus-Wind (Golenetskii, et al., 
GCN Circ. 15203) and INTEGRAL/SPI-ACS  (Savchenko, et al., GCN Circ. 15204) were 
seen from outside the coded field in the non-weighted rates.

The mask-weighted light curve is described in Cummings, et al., GCN Circ. 15202. 
Although there are no discrete peaks later than T+240 seconds, the burst is 
still detected in the mask-weighted rate out to T+963 sec, when this data cuts 
off and continues to be detected onboard in a 64-second image starting at 
T+1388, and possibly later.  Since the BAT event data does not cover the full 
extent of the burst, we cannot reliably calculate T90 at this point, but it is 
at least 360 seconds.

The time-averaged spectrum from T-73.7 to T+767.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.17 +- 0.02.  The fluence in the 15-150 keV band is 1.4 +- 0.01 x 10^-4 
erg/cm2. We note that this time interval does not cover the entire burst 
duration, so should be considered a lower limit.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/569992/BA/


GRB_name: GRB130828A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15206
SUBJECT: GRB 130828A: Further Swift XRT observations  
DATE:    13/09/09 21:13:13 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU) reports on behalf of the Swift team:

We report on two follow-up observations of the field of GRB 130828A
which was discovered by the FERMI LAT as reported by Vianello & 
Sonbas (GCN circ 15128). The first Swift observation was performed 
on 2013-09-04 (obsID 20293) for 2.6ks and was centered on the 
X-ray source reported in Grupe et al. (GCN circ. 15135). This X-ray
source is still present in the new observation suggesting that 
these X-rays are emitted from the Seyfert 1.9 galaxy 
SDSS J171855.44+275947.4 as suggested by Grupe et al. Support
for this assumption comes from new IPN measurements by 
Hurley et al. (GCN circ. 15138) who published a new IPN error box. 
The X-ray source associated with SDSS J171855.44+275947.4 is 
significantly outside this error box.

We re-examined the Swift observation of the field which contains 
the IPN error box (obsID 20289) and found enhanced X-ray emission 
within the IPN error  box reported by Hurley et al. Applying the 
Bayesian statistics as  described by Kraft et al. (1991, ApJ, 374, 
344) suggesting a source  detection at the 3sigma level of 
(2.4+4.2-2.1)e-3 counts/s. The position of this marginally 
detected source is:

RA(hh mm ss.s) = 17h19m09.24s
Dec(dd mm ss.s) = +28:13:14.05

with an uncertainty of 8".

We re-observed the position of this source with Swift on 2013-09-07 
for a total of 5157s (obsID 20295). No source was detected in this
observation. The 3sigma upper limit at the position of the 
previously detected X-ray source within the IPN error box is 
1.3e-3 counts/s. This may suggest that the X-ray source found 
within the IPN error box during observation 20289 is the X-ray 
afterglow of GRB 130828A. Note, however, that considering the
3sigma errors given above, this upper limit is non-conclusive. 

No further Swift  observations are planned of this GRB.

This circular is an official product of the Swift team.


GRB_name: GRB130907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15207
SUBJECT: GRB 130907A: WSRT radio detection
DATE:    13/09/10 00:48:04 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (University of Amsterdam) reports on behalf
of a large collaboration:

"We observed the position of the GRB 130907A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at September 9 09.99 UT to
20.69 UT, i.e. 1.51 - 1.96 days after the burst (GCN 15183).
We detect a radio source with a flux density of 0.19 +/- 0.03 mJy
at the position of the optical counterpart (GCN 15187).

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


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15208
SUBJECT: GRB 130907A: RATIR Optical and NIR Observations
DATE:    13/09/10 05:56:06 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130907A (Page et al., GCN 15183) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/09 10.12 to 2013/09 10.16 UTC (53.18 to
54.12 hours after the BAT trigger), obtaining a total of 0.71 hours
exposure in the r and i bands and 0.30 hours exposure in the Z, Y, J, and H
bands.

For the source reported in Lee et al. (GCN 15192), in comparison with SDSS
DR9 and 2MASS, we obtain the following detections and upper limits
(3-sigma):

  r   21.92 +/- 0.12
  i   21.38 +/- 0.09
  Z   > 21.37
  Y   > 20.87
  J   > 20.58
  H   > 19.97

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source has faded by about two
magnitudes in all bands since our measurements two nights ago (Lee et al.,
GCN 15192).  We note that the source intensity in the r and i bands is now
comparable to the cataloged values for the spatially coincident galaxy SDSS
J142333.95+453626.2.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15209
SUBJECT: GRB 130907A: Continued RATIR Optical and NIR Observations
DATE:    13/09/11 05:14:23 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130907A (Page et al., GCN 15183) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/09 11.12 to 2013/09 11.16 UTC (77.18 to
78.08 hours after the BAT trigger), obtaining a total of 0.71 hours
exposure in the r and i bands and 0.30 hours exposure in the Z and Y.

For the source reported in Lee et al. (GCN 15192), in comparison with SDSS
DR9 and 2MASS, we obtain the following detections and upper limits
(3-sigma):

  r     22.40 +/- 0.14
  i     21.73 +/- 0.10
  Z     > 21.80
  Y     > 21.05

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source has faded by about 0.4
mags in the r and i bands relative to our observations last night (Butler
et al., GCN 15208).

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB120419A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15210
SUBJECT: GRB 120419A: Swift XRT confirmation of the afterglow
DATE:    13/09/11 08:38:22 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling and K.L. Page (U. Leicester) report on behalf of the Swift XRT team:

Swift performed a further pointing of INTEGRAL-detected burst GRB 120419A 
(Gotz et al., GCN Circ. 13241), on 10th September 2013 for a total exposure of 3.9 ks.

No source is detected at the position of the X-ray source previously localised with XRT
(Page et al., GCN Circ. 13242). We measure an upper limit on the count rate of 2.4e-3 
count s^-1. The source has therefore faded and we confirm this as the X-ray afterglow 
of GRB 120419A.


GRB_name: GRB130907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15211
SUBJECT: GRB 130907A: AMI radio detection
DATE:    13/09/11 13:29:18 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

G.E. Anderson, R.P. Fender, T.D. Staley (University of Southampton),
A.J. van der Horst and B.A. Rowlinson (University of Amsterdam)
report on behalf of a large collaboration:

"We observed the position of the GRB 130907A afterglow at 15 GHz with
the Arcminute Microkelvin Imager at September 8 09.90 UT to 11.90 UT,
i.e. 12.2 - 14.2 hours after the burst (GCN 15183).
We detect a radio source at the position of the optical counterpart
(GCN 15187) with a flux density of 1.06 +/- 0.11 mJy.

These observations were triggered via the system described in
Staley et. al (2013, MNRAS, 428, 3114).
Further follow-up observations are planned."


GRB_name: GRB130912A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15212
SUBJECT: GRB 130912A: Swift detection of a short burst
DATE:    13/09/12 08:57:42 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
D. Malesani (DARK/NBI), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 08:34:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130912A (trigger=570465).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 47.615, +13.974 which is 
   RA(J2000) = 03h 10m 28s
   Dec(J2000) = +13d 58' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a short spike
with substructure with a duration of about 0.5 sec.  The peak count rate
was ~11000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:36:31.7 UT, 93.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 47.59060, 13.99546 which is equivalent
to:
   RA(J2000)  = 03h 10m 21.74s
   Dec(J2000) = +13d 59' 43.7"
with an uncertainty of 3.8 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 in excess of the Galactic value (1.24 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.1
(+1.66/-1.48) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 98 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 none of
the XRT error circle. 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 0.28. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.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: GRB130912A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15213
SUBJECT: GRB 130912A: KAIT optical upper limit
DATE:    13/09/12 09:58:32 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the short-duration GRB 130912A
(D'Elia et al., GCN 15212) starting at 08:48:04 UT, ~13 minutes after
the burst. Observations were performed with an automatic sequence
in V, I, and clear filters (20 s exposure for each image). Due to
a technical issue, the first useful image begain ~35 minutes after the
burst. We do not detect any new source in the XRT error circle.
The estimated limiting magnitude in our first clear-band (close to R)
image is about 19.6 (calibrated to USNO B1.0) at a midtime of ~36
minutes after the burst.


GRB_name: GRB130912A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15214
SUBJECT: GRB 130912A: GROND observations
DATE:    13/09/12 11:49:50 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

M. Tanga (MPE Garching), S. Klose (TLS Tautenburg), V. Sudilovsky
(MPE Garching), R. Filgas (IEAP Prague), J. Greiner (MPE Garching)
report on behalf of the GROND team:

We observed the field of GRB 130912A (Swift trigger 570465; D'Elia et al.
2013, GCN #15212) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 08:50 UT on 12 Sep 2013, 16 min after the GRB
trigger. At the northern edge of the r=2.2 arcsec XRT error circle (D'Elia
et al., GCN #15173) we detect a faint source at coordinates

RA (J2000)   = 03:10:22.23
Dec. (J2000) = 13:59:48.7

with an error of 0".3 arcseconds.

However, the object seems to be constant over the first hour of
our observations, with a preliminary magnitude of r' = 22.0+-0.2 mag,
calibrated against the GROND zeropoint. Given the constant flux,
this might be the host galaxy of GRB 130912A.


GRB_name: GRB130912A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15215
SUBJECT: GRB 130912A: REM optical/NIR upper limits
DATE:    13/09/12 12:39:24 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza, A. Melandri (INAF-OAB), V. D'Elia (ASI/ASDC) report on behalf of the REM team:

We observed the field of the short GRB 130912A (D'Elia et al., GCN 15212) simultaneously in the optical and near infrared with the the 60-cm robotic telescope REM at La Silla Observatory (Chile). The observations started at 08:47:33 UT, 12.6 min after the GRB.

No source is detected within the XRT error circle nor at the position of the possible host galaxy reported by Tanga et al. (GCN 15214). The limiting magnitudes are r'=19.6 and H=16.1 (Vega; calibrated against the USNOB1 and the 2MASS catalogue, respectively) at a mid t-t0=17.5 minutes.


GRB_name: GRB130912A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15216
SUBJECT: GRB 130912A, Swift-BAT refined analysis
DATE:    13/09/12 13:43:47 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 130912A (trigger #570465) (D'Elia, et al.,
GCN Circ. 15212).  The BAT ground-calculated position is
RA, Dec = 47.606, 13.999 deg which is
    RA(J2000)  =  03h 10m 25.6s
    Dec(J2000) = +13d 59' 55.7"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 31%.
  
The mask-weighted light curve shows two overlapping peaks.  T90 (15-350 keV) is
0.28 +- 0.03 sec (estimated error including systematics).
  
The time-averaged spectrum from T+0.00 to T+0.32 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.20 +- 0.20.  The fluence in the 15-150 keV band is 1.7 +- 0.2 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.34 sec in the 15-150 keV band
is 2.2 +- 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/570465/BA/


GRB_name: GRB130912A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15217
SUBJECT: GRB 130912A: Enhanced Swift-XRT position
DATE:    13/09/12 15:48:56 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1499 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130912A, 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 = 47.59265, +13.99703 which is equivalent
to:

RA (J2000): 03h 10m 22.24s
Dec (J2000): +13d 59' 49.3"

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, MNRAS, 397, 1177).

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


GRB_name: GRB130912A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15218
SUBJECT: GRB 130912A: Skynet DSO-14/Yerkes-41/PROMPT-CTIO observations
DATE:    13/09/12 17:07:49 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, J. Haislip, A. LaCluyze, A. B. Smith, D. Caton, 
L. Hawkins, V. Hoette, K. Cudworth, D. Harper, R. Kron, T. Linder, R. 
Russell, E. Struble, T. Berger, H. T. Cromartie, R. Egger, A. Foster, N. 
Frank, K. Ivarsen, M. Maples, J. Moore, M. Nysewander, and J. A. Crain 
report:

Skynet observed the Swift/XRT localization of GRB 130912A (D'Elia et 
al., GCN 15212, Swift trigger 570465) with the 14" telescope at the 
Appalachian State University Dark Sky Observatory (DSO-14) in NC, USA (R 
and I bands), the 41" telescope of Yerkes Observatory in WI, USA (r' and 
i' bands), and with four 16" telescopes of the PROMPT array at CTIO, 
Chile (B, V, R, and I bands).

Starting at 2013-09-12, 08:47 UT and continuing until 10:26 UT 
(t=12m-111m post-trigger), Skynet took a total of 72 160s exposures. In 
stacked images, we do not detect an optical source in any band in or 
near the XRT error circle.  Our 3-sigma limiting magnitudes are 
tabulated below:

==================================
tmid  scope   expos  fil  limit
==================================
21m  DSO-14   2x160s  I  >18.7
24m  DSO-14   2x160s  R  >19.6
61m  Prompt5 10x160s  I  >20.6
61m  Prompt4 10x160s  R  >21.0
61m  Prompt1 10x160s  V  >21.3
61m  Prompt3 10x160s  B  >21.1
63m  Y-41    11x160s  i' >21.6
60m  Y-41     9x160s  r' >21.9
66m  Y-41     8x160s  g' >21.8
==================================

BVRI magnitudes are in the Vega System, and g'r'i' magnitudes are in the 
AB system, calibrated to 4 APASS stars in the field.  Magnitudes have 
not been corrected for line-of-sight Milky Way dust extinction, with 
expected E(B-V)=0.28 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130912A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15219
SUBJECT: GRB 130912A: Fermi GBM detection
DATE:    13/09/12 17:43:08 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

Bin-Bin Zhang (UAH), Suzanne Foley (UCD) and Narayana Bhat (UAH) 
report on behalf of the Fermi GBM Team:

"At 08:34:58.00 UT on 12 September 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located a short GRB 130912A (trigger 400667700 / 130912358),
which was also detected by the Swift (D'Elia et al., GCN 15212).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 102 deg from Swift/XRT 
position (Beardmore et al. GCN 15217).

The GBM light curve consists of a single pulse with of multiple peaks
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.448 s is
well fit by a Band function with alpha = -1.0 +/- 0.1, beta = -1.9 +/- 0.2
and Epeak= 1225 +/- 599 keV. The event fluence (10-1000 keV) in this time interval is
(2.29 +/- 0.14)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.13 s in the 10-1000 keV band is 4.5 +/- 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: GRB130907A
Detection_method: MASTER
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15220
SUBJECT: GRB 130907A: MASTER refined analysis
DATE:    13/09/12 18:46:58 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, A.Belinski, N.Tyurina, 
D.Kuvshinov, N.Shatskiy, P.Balanutsa, A.Kuznetsov, V.V.Chazov, 
A.Sankovich,  D.Zimnukhov
Sternberg Astronomical Institute, Moscow State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the  GRB130907A 18 sec  after notice
time and 43 sec after GRB time at 2013-09-07  21:42:00 UT in two
polarizations. The observations were performed at low elevation (zenith 
angle 84 deg)and under the changing transparency conditions. The OT (Page et. al. 
GCN15183) appears on the 4th image in the series and is visible on four 
consecutive  images (20, 30, 40 and 50 sec exposures) in both tubes with 
the signal-to-noise ratio from 3 to 6. Starting with T0+5 min, the image 
quality was further deteriorating with the OT visible only on the sum of 
two pairs of synchronous images.

Our photometry results are presented in Table 1.

Table 1.
-------
Start date and time     exptime   T_start-T_trig   T_mid-T_trig  P| mag.   err_P      P- mag    err_P-    P| + P-    err. (P| + P-)
-----------------------+--------+----------------+--------------+--------+---------+----------+---------+----------+---------------
2013-09-07 21:42:00.31    10        47               52           <10.5      ---       <10.5      ---      <11.0        ---
2013-09-07 21:42:22.79    10        69               74           <10.5      ---       <10.5      ---      <11.0        ---
2013-09-07 21:42:43.59    20        91               101          <11.0      ---       <11.0      ---      <11.5        ---
2013-09-07 21:43:16.66    20        123              133           12.2      0.2        13.0      0.3       12.5        0.2
2013-09-07 21:43:47.44    30        154              169           13.3      0.4        13.6      0.6       13.5        0.4
2013-09-07 21:44:29.95    40        197              217           13.7      0.5        13.7      0.6       13.9        0.5
2013-09-07 21:45:21.88    50        249              274           13.7      0.5        14.4      0.8       14.0        0.6
2013-09-07 21:46:23.87    60+80     311              387          <13.8      ---       <13.7      ---       13.9        0.6

*) All time intervals in seconds.  P| and P- is an unfiltered magnitude 
with RA and DEC orientated polaroid correspondingly.
The sign '<'  before magnitude means the value is upper limit.


The light curve and movie available here 
http://master.sai.msu.ru/static/GRB/GRB130907A/grb130907A.html

The epoch of our observations completely covers Swift BAT weak, soft peak 
from T+210 sec to T+240 sec (Cummings et. al. GCN15202).

Our first automatic and not so exact (due to difficult observing 
conditions) estimation of the  OT magnitude, given in the previous 
telegram (Gorbovskoy et. al GCN15184),  belongs to  epoch of the 5th 
exposure with t_mid=217 sec. after the trigger. This fact isn't clear from 
the telegram  text that could mislead some researchers.
We apologize for this inaccuracy.

The message may be cited.


GRB_name: GRB130912A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15221
SUBJECT: GRB 130912A: Swift-XRT refined Analysis
DATE:    13/09/12 20:57:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A. Maselli  (INAF-IASFPA), A.
Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), V. Mangano (PSU),
M.C. Stroh (PSU) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 6.6 ks of XRT data for GRB 130912A (D'Elia  et al. GCN
Circ. 15212),  from 104 s to 13.1 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN. Circ 15217).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.24 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.49 (+0.20, -0.12). The
best-fitting absorption column is  1.29 (+0.67, -0.05) x 10^21 cm^-2,
consistent with the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 5.0 x 10^-11 (5.8 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.29 (+0.67, -0.05) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.49 (+0.20, -0.12)

If the light curve continues to decay with a power-law decay index of
1.24, the count rate at T+24 hours will be 1.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.0 x
10^-14 (9.2 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00570465.

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


GRB_name: GRB130912A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15222
SUBJECT: GRB 130912A: P60 Observations
DATE:    13/09/12 21:02:47 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC), V. Sudilovsky, M. Tanga, and J. Greiner (MPE
Garching), report on behalf of a larger collaboration:

We have imaged the field of the Swift short GRB130912A (D'Elia et al., GCN
15212) with the robotic Palomar 60 inch telescope in the r', i', and z'
filters.  Observations began at 8:48 UT on 2013 September 12 (13 min after
the Swift trigger).

Within the enhanced XRT error circle (Beardmore et al., GCN 15217) we
detect the faint source reported by Tanga et al. (GCN 15214) in all three
filters.  Using calibration stars from GROND, we measure an AB magnitude
of r' = 21.77 +/- 0.20 mag at a mean time of 8:58 UT and r' = 22.09 +/-
0.25 at 09:28 UT (23 and 53 min after the Swift trigger, respectively).
The lack of significant variability implies either a shallow afterglow
decay index, or this source may be the host galaxy of GRB130912A, as
suggested by Tanga et al. (GCN 15214).


GRB_name: GRB130907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15223
SUBJECT: GRB 130907A: Continued RATIR Optical and NIR Observations
DATE:    13/09/13 04:41:50 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130907A (Page et al., GCN 15183) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/09 13.13 to 2013/09 13.16 UTC (125.49 to
126.24 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r and i bands and 0.15 hours exposure in the Z, Y, J, and H
bands.

For the source reported in Lee et al. (GCN 15192), in comparison with SDSS
DR9 and 2MASS, we obtain the following upper limits (3-sigma) in the AB
magnitude system (not corrected for Galactic extinction in the direction of
the GRB) :

  r     > 22.68
  i     > 22.62
  Z     > 21.30
  Y     > 20.70
  J     > 20.42
  H     > 19.69

We conclude from our most constraining limit (i-band), that the source has
faded by at least 0.9 mags since our observation 2 nights ago (Butler et
al., GCN 15209).  These magnitudes are now significantly fainter than the
DR9 catalog magnitudes of SDSS galaxy mentioned by Lee et al.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130912A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15224
SUBJECT: GRB 130912A: WHT confirmation of optical counterpart
DATE:    13/09/13 12:59:55 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

N.R. Tanvir, K. Wiersema (U. Leicester), A.J. Levan (U. Warwick) report for a larger collaboration:

"We observed the location of GRB 130912A (D'Elia et al. GCN 15212) with the William Herschel Telescope, beginning at approximately 05 UT on 13 September 2013,  roughly 20 hours after the burst trigger. At this epoch we obtained observations in the g,i and J-bands utilising ACAM and LIRIS.

At the location of the counterpart identified by Tanga et al. (GCN 15214) and Cenko et al. (GCN 15222) we detect no source in our g-band observations (limiting magnitude g~25), and a source which is only weakly detected in the i-band and J-band (i~24). This implies that the light observed at earlier epochs when the source was measured at r=22 was due to a significant contribution from the optical transient, and that any underlying host galaxy is faint."


