# GCN_circulars

GRB_name: GRB140730A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16643
SUBJECT: GRB 140730A: Prompt enhanced Swift-XRT position
DATE:    14/07/30 20:14:28 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 140730A, we find an
enhanced XRT position of the afterglow: RA, Dec: 56.3982, -66.5456
which is equivalent to:
   RA (J2000)  = 03 45 35.56
   Dec (J2000) = -66 32 44.0
with an uncertainty of 2.3 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/607742.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140730A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16644
SUBJECT: GRB 140730A: Enhanced Swift-XRT position
DATE:    14/07/31 01:30:27 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 140730A, 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 = 56.39911, -66.54516 which is equivalent
to:

RA (J2000): 03h 45m 35.79s
Dec (J2000): -66d 32' 42.6"

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

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140730A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16645
SUBJECT: GRB 140730A: Swift/UVOT Upper Limits
DATE:    14/07/31 01:35:22 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and C. B. Markwardt (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140730A
68 s after the BAT trigger (Markwardt et al., GCN Circ. 16642).
No optical afterglow consistent with the XRT position
(Evans GCN Circ. 16643)
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            68          218          147         >21.2
u_FC               280          530          246         >19.6
white               68         6182          396         >21.3
v                  784         6593          413         >19.5
b                  709         5978          216         >20.3
u                  280         5772          462         >20.0
w1                 660         5568          236         >21.1
m2                5162         6798          393         >20.4
w2                4753         6388          393         >20.6

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: GRB140730A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16646
SUBJECT: GRB 140730A: Swift-XRT refined Analysis
DATE:    14/07/31 10:04:03 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), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de
Pasquale (INAF-IASFPA), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A.
Kennea (PSU) and C.B. Markwardt report on behalf of the Swift-XRT team:

We have analysed 6.1 ks of XRT data for GRB 140730A (Markwardt et al.
GCN Circ. 16642),  from 50 s to 39.5 ks after the  BAT trigger. The
data comprise 17 s in Windowed Timing (WT) mode (the first 7 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 Goad
et al. (GCN Circ. 16643).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.4 (+0.4, -0.3), followed by a break at T+234 s to an
alpha of 0.57 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.92 (+0.25, -0.23). The
best-fitting absorption column is  3.0 (+1.1, -1.0) x 10^21 cm^-2, in
excess of the Galactic value of 7.6 x 10^20 cm^-2 (Willingale et al.
2013). 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:      3.0 (+1.1, -1.0) x 10^21 cm^-2
Galactic foreground: 7.6 x 10^20 cm^-2
Excess significance: 3.8 sigma
Photon index:      1.92 (+0.25, -0.23)

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 10.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.9 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/00607742.

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


GRB_name: GRB140730A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16647
SUBJECT: GRB 140730A: LCO-Sutherland observations
DATE:    14/07/31 15:02:56 GMT
FROM:    Simone Dichiara at Ferrara U/Italy  <dichiara@fe.infn.it>

S. Dichiara, C. Guidorzi (U. Ferrara), C.G. Mundell (LJMU),
A. Gomboc (U. Ljubljana) on behalf of a large collaboration report:

One of the Las Cumbres Observatory 1-m telescopes in Sutherland
(South Africa) began observing Swift GRB 140730A (Markwardt et al.
GCN Circ 16642) on July 31 at 01:16:34 UT, i.e.
~5.5 hours after the BAT trigger, with the r' and i' filters.

Within the enhanced XRT error circle (Goad et al. GCN Circ. 16644)
we found nothing down to the following limit:

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)   (s)
-------------------------------------------------
5.64           120x5       r'        > 20.0
5.83           120x5       i'        > 19.8
-------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB140729A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16648
SUBJECT: Konus-Wind observation of GRB 140729A
DATE:    14/07/31 15:14:09 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration, hard-spectrum GRB 140729A
(Fermi-LAT detection: Arimoto and Bissaldi, GCN 16633;
IPN triangulation: Hurley et al., GCN 16637)
triggered Konus-Wind at T0=2213.751 s UT (00:36:53.751).

The burst light curve shows a single pulse with a duration of ~16 s
followed by a weak tail seen up to T0+33s.
The emission is seen up to ~2 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.0(-0.2,+0.3)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+2.656 s,
of 4.5(-1.6,+1.7)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.65(-0.29,+0.36),
and Ep = 592(-122,+187) keV (chi2 = 76/89 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.7 (chi2 = 76/88 dof).

The spectrum near the peak count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.68(-0.29,+0.35),
and Ep = 619(-132,+233) keV (chi2 = 51/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.0 (chi2 = 51/59 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140729_T02213/

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


GRB_name: GRB140709A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16650
SUBJECT: GRB 140709A, the review of the sky area in plate archives
DATE:    14/08/01 12:43:56 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)report: 
We have undertaken the review of the sky area in vicinity of 
GRB 140709A (P.A. Evans et al. GCN Circ.16548) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19840822/200650 GUA040C000445A 12.5 16.10 1350-12048943
19840825/201235 GUA040C000458A 16.0 16.95 1350-12054971
19840905/193326 GUA040C000485A 22.5 16.20 1350-12052525
19850711/224521 GUA040C000678A 16.0 16.75 1350-12052468
19850711/230927 GUA040C000679A 16.0 16.95 1350-12054971
Plates: â€“the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 12 minutes area around 
       the location given in P.A. Evans et al. GCN Circ.16548: 
       RA(J2000)= 20h 18m 38.96s, Dec(J2000)= +51d 13' 29.9"
Star USNOA2 - Comparison star.
  The preview images of 5 areas together with  
the 12x12 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/140709A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB140709B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16651
SUBJECT: GRB 140709B: TShAO optical upper limit
DATE:    14/08/01 17:36:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), W. Mundrzyjewski (Fesenkov Astrophysical Institute), 
A. Kusakin (Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report 
on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140709B  (Swenson et al., GCN 
16551) with Zeiss-1000 (West) telescope of Tien Shan Astronomical 
Observatory starting on July 9, (UT) 15:50:27, i.e. 35 minutes after GRB 
trigger. We took several images in R-filter.  Within enhanced XRT error 
circle  (Goad et al., GCN 16556) we do not detect any new object in 
stacked images.

Details of a photometry of stacked images are following

Date       UT start  t-T0,d  Exp,s   Filter Up_Lim (3 sigma)

2014-07-09 15:50:27  0.09193 13*600  R      20.5
2014-07-10 15:36:01  1.06090 13*600  R      19.8

The photometry is based on SDSS star J094401.61+633253.8 assuming
R=16.010+/-0.013 (using gri -> R Lupton transformations).


GRB_name: GRB140730A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16652
SUBJECT: GRB 140730A, Swift-BAT refined analysis
DATE:    14/08/01 19:12:39 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@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/UMBC),
C. B. Markwardt (GSFC), 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-240 to T+902 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140730A (trigger #607742)
(Markwardt, et al., GCN Circ. 16642).  The BAT ground-calculated position is
RA, Dec = 56.350, -66.580 deg which is
  RA(J2000)  =  03h 45m 24.0s
  Dec(J2000) = -66d 34' 48.7"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows several overlapping pulses. The first major
pulse starts at ~T-14s, peaks at  ~T-13 s, and ends at ~T-4 s. The second major pulse
starts at ~T+0 s, peaks at ~T+1s, and ends at ~T+5 s. The whole burst structure ends
at ~T+41 s. T90 (15-350 keV) is 41.3 +- 3.7 sec (estimated error including systematics).

The time-averaged spectrum from T-13.5 to T+29.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.50 +- 0.32.  The fluence in the 15-150 keV band is 2.8 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.17 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/607742/BA/


GRB_name: GRB140801A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16653
SUBJECT: GRB 140801A (FERMI trigger 428612396): MASTER brigth OT discovery
DATE:    14/08/01 20:52:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, D.Denisenko, M.Pruzhinskaya, V.Kornilov, 
D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, 
A.Kuznetsov, V.V.Chazov, A.Sankovich
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

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

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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 Tunka was pointed to the  GRB140801A (FERMI trig. 428612396) 54 
sec after notice time and 100 sec after trigger time at 2014-08-01 19:01:33 UT
in two polarizations.

MASTER-Tunka auto-detection system discovered bright OT 
source at (RA, Dec) = 02h 56m 16.44s +30d 56m 16.8s on 2014-08-01.79376 
UT. The OT unfiltered magnitude is 14.6m (limit 18.3m) within FERMI 
error-box  (trig. N 428612396).


Preliminary automatic photometry and astrometry

Date         Time           Ra                Dec       Mag
2014-08-01 19:01:31.886 02h 56m 16.42s , +30d 56m 16s.8 14.64
2014-08-01 19:03:02.863 02h 56m 16.43s , +30d 56m 17s.0 15.72
2014-08-01 19:04:38.384 02h 56m 16.43s , +30d 56m 17s.0 16.30


Our band is well described by a parity 0.8R+0.2B (USNO B1).

The discovery and reference images are available at:
http://master.sai.msu.ru/static/GRB/GRB140801_FERMI.png


The 5-sigma upper limit has been about 18.53mag
The message may be cited.


GRB_name: GRB140801A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16654
SUBJECT: GRB 140801A: archival upper limits on the host galaxy
DATE:    14/08/01 22:09:55 GMT
FROM:    Denis Denisenko at SAI MSU  <d.v.denisenko@gmail.com>

D. Denisenko, E. Gorbovskoy, V. Lipunov (Sternberg Astronomical
Institute, Moscow State University) report:

Since the error box of GRB 140801A (FERMI trigger 428612396) was not
covered by Sloan Digital Sky Survey, we have used the digitized
Palomar plates of this area to create the color-combined finder chart
and to estimate the upper limits on the host galaxy of this burst.
There are in total 12 plates available (POSS-I red and blue ones from
1953 and 1954, two Quick-V plates from 1982 and six POSS-II plates
from 1991-1995: 2 blue, 2 red and 2 infrared). There is nothing at the
position of MASTER optical transient (Gorbovskoy et al., GCN 16653) on
any individual plates, as well as on their combination to the limiting
magnitude ~22.5.

5'x5' color-combined finder chart centered at MASTER OT
J025616.43+305617.0 is uploaded to
http://master.sai.msu.ru/static/GRB/GRB140801A-BRIR5x5.jpg (position
of the OT is marked with dashes). We also note the nearby white dwarf
44" north of the OT which is marked by an arrow. It has the following
entries in the major catalogues:

USNO-B1.0 1209-0038230 (02 56 16.581 +30 57 02.09 pmRA=88 pmDE=32
B1=15.37 R1=15.54 B2=15.74 R2=16.06 I=16.20)
GALEX J025616.6+305702 (FUV=15.09+/-0.02 NUV=15.41+/-0.01)
2MASS J02561657+3057017 (J=16.12+/-0.09)

There is no mention of its variability in the literature. However, it
should be used with caution in photometric purposes.

This message can be cited.


GRB_name: GRB140801A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16655
SUBJECT: IPN triangulation of GRB 140801A (Fermi trigger 428612396)
DATE:    14/08/01 22:25:55 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN 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, and

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

GRB140801A (Fermi trigger 428612396) has been observed by Konus-Wind,
Fermi-GBM, and MESSENGER, so far, at around 68393 SOD (18:59:53) UT.
We have triangulated it to a preliminary, 3 sigma annulus centered at
RA, Dec (2000)=123.886, +21.098 degrees, whose radius is 70.951 +/-
0.125 degrees.  The bright MASTER OT (Gorbovskoy et al. GCN 16653) lies
0.0093 degrees from the center line of this annulus, and is therefore
likely to be the optical afterglow of this GRB.

A map has been posted at ssl.berkeley.edu/ipn3/140801A.  This localization
may be improved.

The spectral and temporal properties of this GRB will be given in
forthcoming GCN Circulars.


GRB_name: GRB140801A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16656
SUBJECT: GRB 140801A: NOT afterglow confirmation
DATE:    14/08/02 03:34:21 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), S. Schulze (PUC, MAS), M. El-Souri, S. Boye Nissen,
M. Sparre, J. P. U. Fynbo (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC,
DARK/NBI), P. Jakobsson (U. Iceland) report on behalf a larger
collaboration:

We observed the field of GRB 140801A (Fermi trigger 428612396) with
the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC. We
obtained a 200-s exposure in each of V, R, and I bands. Observations
started at 01:07:23 UT on August 2 (i.e. 6.12 hours after the burst).

The optical transient reported by Gorbovskoy et al. (GCN 16653) is
clearly detected in each of our images at the same position. And it
has decayed to R(Vega) ~ 20.6 mag at 6.15 hours post-trigger,
calibrated against two bright nearby USNO B1 stars. This measurement
is not corrected for foreground extinction.

The OT roughly decays as t^-1.5 during the MASTER observations (GCN
16653), and then changes to roughly as t^-0.9 assuming a simple
power-law decline since the MASTER's end-time. The whole behavior is
similar to that of previous GRB optical afterglows. We thus conclude
that this OT is very likely the optical afterglow of GRB 140801A.


GRB_name: GRB140801A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16657
SUBJECT: GRB 140801A: Redshift from the 10.4m GTC telescope
DATE:    14/08/02 04:56:21 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC, UPV/EHU), 
C.C. Thoene (IAA-CSIC), J.P.U. Fynbo (DARK/NBI), D. Xu (DARK/NBI), 
D. Perez-Valladares (GTC), and G. Gomez-Velarde (ULL-IAC, GTC) report on 
behalf of a larger collaboration:

We have observed the afterglow of the Fermi GRB140801A (Gorbovskoy et al. 
GCN 16653, Xu et al. GCN 16655) with the 10.4m GTC (+OSIRIS). Spectroscopic 
observations began at 3:35 UT (8.59 hr after the burst). The first 900 s spectrum 
was obtained with the R1000B grism, and covered the range between 3630 and 
7500 A, at a resolution of ~1000.

We detect a strong continuum with absorption features that correspond to NiII, 
MnII, FeII, MgII, and MgI at a common redshift of z=1.320, which we identify as the 
redshift of the GRB.

Further spectroscopic observations are ongoing.


GRB_name: GRB140801A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16658
SUBJECT: GRB 140801A: Fermi GBM observation
DATE:    14/08/02 05:37:24 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 18:59:53.26 UT on 1 August 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140801A (trigger 428612396 / 140801792).
An optical transient was detected by the MASTER II robotic telescope
(Lipunov et al. 2014, GCN 16653). The GBM on-ground location is
consistent with the OT location, which angle from the Fermi LAT
boresight is 80 degrees.

The GBM light curve consists of two bright pulses followed by a
short tail, with a duration (T90) of about 7 s (50-300 keV).

The time-averaged spectrum from T0-2.048 s to T0+12.288 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.42 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 125 +/- 2 keV
(Castor-statistics 697.99 for 610 d.o.f.).
A Band function fits the spectrum equally well (Castor-statistics
695.14 for 609 d.o.f.) with Epeak= 122 +/- 3 keV,
alpha = -0.40 +/- 0.04 and beta = -3.6 +/- 0.4.

The event fluence (10-1000 keV) in this time interval is
(1.22 +/- 0.01)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.832 s in the 10-1000 keV band
is 22.6 +/- 0.4 ph/s/cm^2.

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


GRB_name: GRB140801A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16659
SUBJECT: GRB 140801A : Virtual Telescope optical observations
DATE:    14/08/02 09:44:48 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi, the Virtual Telescope Project - Italy, reports:

I observed the field of GRB 140801A (Fermi trigger 428612396) with with the 17" 
robotic unit part of the Virtual Telescope (Ceccano, Italy) at 2 Aug. 2014, 
00:10:39 UT, 5.15 hours seconds after the burst.

An optical source is visible where described by Gorbovskoy et al. (GCN 16653) 
and D. Xu et al (GCN 16656) in a image coming from the sum of three, 180-seconds 
exposures, unfiltered. The position of the source is RA: 02 56 16.46 +30 56 17.9 
(J2000, mean residuals of 0.2") and the magnitude was estimated to be 19.6, 
assuming R mags for the reference stars from UCAC-4.

The message may be cited.


GRB_name: GRB140801A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16660
SUBJECT: Konus-Wind observation of GRB 140801A
DATE:    14/08/02 12:26:02 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, A. Tsvetkova, A.Lyssenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 140801A
(IPN triangulation: Hurley et al., GCN 16655;
Fermi-GBM detection: Pelassa, GCN 16658)
triggered Konus-Wind at T0=68394.769 s UT (18:59:54.769).

The light curve shows a multi-peaked structure with a total duration of ~7.5 s.
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst had a fluence
of 1.10(-0.04,+0.04)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+0.128 s, of 4.6(-0.6,+0.6)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+7.680 s)
is best fit in the 20 keV - 5 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.44(-0.17,+0.18),
and the peak energy Ep = 108(-4,+5) keV,
chi2 = 75/71 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep with an upper limit on beta of -4.2

The spectrum near the peak count rate (measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 5 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = +0.38(-0.56,+0.69),
and the peak energy Ep = 121(-12,+13) keV,
chi2 = 27/24 dof.

Assuming the redshift z=1.320 (de Ugarte Postigo et al., GCN 16657)
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:
the isotropic energy release E_iso is ~4.9x10^52 erg,
the peak luminosity L_iso is ~5.0x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~250 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140801_T68394/

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


GRB_name: GRB140801A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16661
SUBJECT: GRB 140801A: Swift-XRT observations
DATE:    14/08/02 14:20:53 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli and M. De Pasquale (INAF-IASFPA) report on behalf of the 
Swift-XRT team:

We have analysed 2.0 ks of XRT data for the FERMI/GBM detected burst GRB 
140801A (Pelassa, GCN Circ. 16658), from 36.4 ks to 48.0 ks after the 
GBM trigger. The data are entirely in Photon Counting (PC) mode. An 
X-ray source is found at the position of the optical transient detected 
by MASTER (Gorbovskoy et al.,  GCN Circ. 16653). Using 1893 s of PC mode 
data and 2 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 = 44.06877, +30.93799 which is equivalent to:

RA (J2000): 02h 56m 16.50s
Dec(J2000): +30d 56' 16.8"

with an uncertainty of 2.5 arcsec (radius, 90% confidence). This 
position is 0.8 arcsec from the MASTER position. We believe that this 
source, which has a mean count rate of 2.3e-02 ct/sec, is the X-ray 
afterglow of GRB 140801A but further observations are needed to 
determine a decaying behaviour.

The results of the XRT-team automatic analysis are available at 
http://www.swift.ac.uk/xrt_products/00020402.

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


GRB_name: GRB140801A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16662
SUBJECT: GRB 140801A: Swift/UVOT Upper Limits
DATE:    14/08/02 18:10:39 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and E. Troja (NASA/GSFC/UMCP) report on behalf
of the Swift/UVOT team:

The Swift/UVOT observed the field of the Fermi/GBM-detected burst GRB 140801A
beginning 36.4 ks after the trigger (Pelassa, GCN Circ. 16658). No optical
afterglow consistent with the XRT candidate (Maselli, GCN Circ. 16661) or
MASTER candidate (Gorbovskoy et al., GCN Circ. 16653) 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

uvw1             36391        47996         1944        >20.70

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.226 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140801A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16663
SUBJECT: GRB 140801A: BTA confirmation of redshift 
DATE:    14/08/02 19:11:44 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. Moskvitin, V. Komarova, T. Sokolova (SAO RAS),
A. J. Castro-Tirado (IAA-SCIC), J. Gorosabel (IAA-SCIC, UPV/EHU),
S. B. Pandey (ARIES), M. Glushkov (KFU), S. Boronina (SPbSU),
report on behalf of the larger collaboration:

At the night of August 1/2 we observed the GRB 140801A field (Fermi trigger
428612396) with BTA/Scorpio-I. Observations started at 21:10 UT (2.17 hours
after the GRB). The optical transient (Gorbovskoy et al., GCNC 16653; Xu et
al., GCNC 16656, Masi, GCNC 16659) is clearly detected in our V and Rc images
with the brightness R = 20.2 (2.85 hours after the trigger). Photometry
is based on the USNO-B1 star with the coordinates
R. A. = 02:56:16.58, Dec. =  +30:57:02.1 and R2 = 16.06.
The OT magnitude was not corrected for the Galactic extinction
E(B-V) = 0.09 in the direction of the object.

We also obtained an OT spectrum and measured the redshift on basis of several
lines. Our value z =1.319 +/- 0.003 is in a good agreement with that by
de Ugarte Postigo et al. (GCNC 16657).

We thank T. Fatkhullin for his great assistance in observations.


GRB_name: GRB140730A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16664
SUBJECT: GRB 140730A: GROND Upper limits
DATE:    14/08/02 23:55:14 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (TLS Tautenburg), C. Delvaux and Jochen Greiner (both MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 140730A (Swift trigger 607742; Markwardt et
al., GCN #16642) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 08:36 UT on 2014-08-02, 2.52 days after the GRB
trigger. They were performed at an average seeing of 1".2 and at an
average airmass of 1.4.

Based on images with exposure times of 2250 s in g'r'i'z' and 1200 s in
JHK, we do not detect a source within the Swift-XRT error circle reported
by Goad et al. (GCN #16644) down to to the following 3-sigma AB
magnitudes:

g' > 25.3 mag,
r' > 25.4 mag,
i' > 24.7 mag,
z' > 24.4 mag,
J > 21.0 mag,
H > 20.3 mag, and
K > 18.0 mag.

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


GRB_name: GRB140801A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16665
SUBJECT: GRB140801A: Swift/XRT further observations
DATE:    14/08/03 14:05:25 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli, M. De Pasquale (INAF-IASFPA) and E. Troja (NASA/GSFC/UMCP) 
report on behalf of the Swift-XRT team:

We report on further Swift XRT observations in the field of the 
FERMI/GBM-discovered GRB 140801A (Pelassa, GCN Circ. 16658). A new 
exposure of 2.0 ks has been obtained, 123 ks after the Fermi/GBM 
trigger. The X-ray counterpart reported by Maselli & De Pasquale (GCN 
Circ. 16661) is still detected at a count rate of 9.9 (+/-2.5) x 10^-3 
cts s^-1. This latest measurement corresponds to a decay slope of 0.8 
(+0.5, -0.4): thus we confirm that this source is the afterglow of GRB 
140801A.

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


GRB_name: GRB140801A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16666
SUBJECT: GRB 140801A: GROND Afterglow detection, unbroken decay
DATE:    14/08/03 22:14:51 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (TLS Tautenburg), C. Delvaux, and J. Greiner (both MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 140801A (Fermi trigger 428612396; Pelassa,
GCN #16658) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 09:43 UT on 2014-08-02, 0.61 days after the GRB
trigger. They were performed at an average seeing of 1".5 and at an
average airmass of 2.1.

Based on images with exposure times of 1584 s in g'r'i'z', we detect the
optical afterglow at the MASTER position reported by Gorbovskoy et al.
(GCN #16653) at the following AB magnitudes:

g' = 22.4 +/- 0.1 mag,
r' = 21.9 +/- 0.1 mag,
i' = 21.8 +/- 0.1 mag, and
z' = 21.2 +/- 0.2 mag.

Observations taken a day later show the afterglow to have decayed by about
0.75 magnitudes. The afterglow continues to decay with a slope of ~0.9 in
comparison to the magnitudes given by Xu et al. (GCN #16656) and Moskvitin
et al. (GCN #16663).

The given magnitudes are derived based on calibrating the images against
the GROND zeropoints 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: GRB140801A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16667
SUBJECT: GRB 140801A: AAO optical observations
DATE:    14/08/04 01:38:25 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), Molotov (KIAM), A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 140801A (Pelassa, GCN 16658)  with AS-32 (0.7m) 
telescope of Abastumani Observatory starting on Aug. 02 (UT) 21:54:52. We 
obtained several unfiltered frames under  of 60 s under average FWHM of 2.0 
arcsec. The optical afterglow (Gorbovskoy et al., GCN 16653; Xu et al., GCN 
16656, Masi, GCN 16659)  is well detected on the stacked image.

Details of a photometry of the  GRB 140801A are following:

date       UT start        t-T0           Filter    Exp.    OT        err
                                (mid, days)            (s)

2014-08-02 21:54:52  1.14962      None    26*60   22.13    0.18

The photometry is based on the USNO-B1 star ((J2000) 02:56:16.58 +30:57:02.1 
assuming R = 16.06) suggested by Moskvitin et al.,  (GCN 16663). Our 
photometry does not contradict un-broken decay of a light curve of GRB 
140801A (Kann et al., GCN 16666). 


GRB_name: GRB140808A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16668
SUBJECT: GRB 140808A: optical afterglow candidate iPTF14eag
DATE:    14/08/08 09:40:43 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
V. B. Bhalerao (IUCAA), S. B. Cenko (NASA/GSFC), D. A. Perley (Caltech), 
and J. Johansson (Stockholm University) report on behalf of the
intermediate Palomar Transient Factory (iPTF) collaboration:

Fermi GBM triggered on GRB 140808A (Fermi trigger 429152043 /
140808038) at 2014-08-08 00:54:00.62. At 04:08:50 (3.25 hours after
the burst), we began our search for optical counterparts using the
Palomar 48-inch Oschin telescope (P48). We began searching 13 fields
spanning 95 deg2, covering most of the 1-sigma statiscal+systematic
region of the final Fermi GBM localization. We estimate a 69% chance
that these fields contain the true location of the source.

Sifting through candidate variable sources using image subtraction
and standard iPTF vetting procedures, we detected several optical
transients:

iPTF14eag, at the coordinates:
 RA(J2000)  =  14h 44m 53.33s (221.222219 deg)
 Dec(J2000) = +49d 12' 51.1"  (+49.214207 deg)

This source was detected at R = 18.91 +/- 0.06 mag at 3.35 hours
after the burst, and faded to R = 19.29 +/- 0.10 by 4.91 hours.
Relative to the time of the burst, this decay fits a power law
with index alpha = -0.9 +/- 0.3.

There were no previous iPTF detections at this position through 2014
May 28, and there are no coincident sources in SDSS.

iPTF14eai, at the coordinates:
 RA(J2000)  =  14h 17m 29.91s (214.374606 deg)
 Dec(J2000) = +47d 07' 30.1"  (+47.125041 deg)

This candidate was detected at R = 19.37 +/- 0.11 mag at 3.27 hours
after the burst, and was possibly fading. It is coincident with the
r = 18.43 galaxy SDSS J141729.93+470729.7. Because the galaxy is not
resolved in our P48 images, we caution that the transient's magnitude
derived from image subtraction is tentative.

iPTF14eac, at the coordinates:
 RA(J2000)  =  14h 25m 07.98s (216.283253 deg)
 Dec(J2000) = +50d 32' 04.1"  (+50.534476 deg)

This source was detected at R = 18.30 +/- 0.06 at 3.44 hours after
the burst. There was an earlier possible R = 20.16 +/- 0.21 mag
detection from coadded P48 images on 2014 June 09. It is located in a
spiral arm of PGC2375699.

Given the rapid fading of iPTF14eag and the lack of a host or
quiescent counterpart, we propose it as an optical afterglow
candidate. We have requested Swift TOO observations. We encourage
spectroscopic and photometric follow-up to confirm the nature of the
source.

The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi429152043.pdf shows the
locations of our candidates and the 13 P48 fields in relation to the
Fermi GBM 1- and 2-sigma statistical+systematic contours.


GRB_name: GRB140808A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16669
SUBJECT: GRB 140808A: Fermi GBM detection
DATE:    14/08/08 16:33:39 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 00:54:00.62 UT on 08 August 2014, the Fermi Gamma-Ray Burst 
Monitor triggered and located GRB 140808A (trigger 429152043/140808038)
for which a possible counterpart was detected by iPTF14eag 
(Singer et al. 2014, GCN 16668). The GBM on-ground location, 
using the Fermi GBM trigger data, is consistent with the 
iPTF14eag location.

The angle from the Fermi LAT boresight is 63 degrees.

The GBM light curve one main episode which consists of several 
overlapping peaks, with a total duration of about 4.7 s (50-300keV). 
The time-averaged spectrum from T0+0 s to T0+5.0 s is well fit by 
a Band function parameterized as alpha=-0.4+/-0.1, beta=-2.9+/-0.3, 
Ep=115.2+/-7.7 keV.

The event fluence (10-1000 keV) in this time interval is
(3.2 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.5 s in the 10-1000 keV band is 9.3 +/- 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: GRB140808A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16670
SUBJECT: GRB 140808A: Swift-XRT observations
DATE:    14/08/08 18:47:37 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, P.A. Evans (U. Leicester) and S.B. Cenko (GSFC) report on
behalf of the Swift-XRT team:

We have analysed 3.0 ks of XRT data for the GBM-detected burst: GRB
140808A (Zhang, GCN Circ. 16669), from 41.9 ks to 52.0 ks after the GBM
trigger. The data are entirely in Photon Counting (PC) mode.  An X-ray
source is detected within the XRT field of view. Using 1513 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 = 221.22196, +49.21463 which is equivalent to:

RA (J2000): 14h 44m 53.27s
Dec(J2000): +49d 12' 52.7"

with an uncertainty of 3.3 arcsec (radius, 90% confidence). This
position is 1.6 arcsec from the iPTF position (Singer et al., GCN CIrc.
16668).  The source has a mean count rate of 1.5e-02 ct/sec; we cannot
determine at the present time whether it is fading. We note that this
count rate is just below the ROSAT All Sky Survey detection limit, so
this source would not have been listed in the RASS. However, given the
transient nature of the iPTF optical candidate, it seems likely this is
a new X-ray source. 

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020403.

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


GRB_name: GRB140808A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16671
SUBJECT: GRB 140808A: Redshift from the 10.4m GTC telescope
DATE:    14/08/08 23:46:38 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), A. de Ugarte Postigo (IAA-CSIC/DARK-NBI),
C. Thoene (IAA-CSIC), D. Perley (Caltech), A. Garcia Rodriguez (GTC),
report on behalf of a larger collaboration:

We observed the optical candidate iPTF14eag of the Fermi GRB140808A
(Singer et al. GCN 16668; Zhang, GCN 16669; Page et al. GCN 16670) with
the 10.4m GTC (+OSIRIS). Spectroscopic observations were carried out at
21:43:48--22:29:36 UT (20.8-21.9 hours post burst).

Three 900s spectra were obtained with the R1000B grism, covering the range
between 3630 and 7500 A, at a resolution of ~1000. A preliminary reduction
based on archival calibration lamps, reveals a strong DLA and several
absorption metallic lines (CII, SiIV, SiII, CIV, AlII) consistent with a
common redshift of z=3.29, which we identify as the redshift of the GRB.


GRB_name: GRB140808A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16672
SUBJECT: GRB 140808A: Swift/UVOT Upper Limits
DATE:    14/08/09 10:06:12 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and S. B. Cenko (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140808A
42 ks after the GBM trigger (Zhang et al., GCN Circ. 16669).
No optical afterglow consistent with the candidate optical position
(iPTF14eag; Singer et al. GCN Circ. 16668) 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          41951        47112           835         >22.3
v              42055        47902           857         >20.7
u              41848        51959           1212        >21.2

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


GRB_name: GRB140808A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16673
SUBJECT: Konus-Wind observation of GRB 140808A
DATE:    14/08/09 14:54:50 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A long-duration GRB 140808A
(Fermi-GBM detection: Zhang, GCN Circ. 16669)
triggered Konus-Wind at T0=3239.264 s UT (00:53:59.264).

The burst light curve shows two emission episodes, the first,
reported in GCN 16669, from ~T0-1.9 s to ~T0+3.6 s,
and the second, from ~T0+303 s to ~T0+336 s.
The second episode is also seen in the INTEGRAL (SPI-ACS) data but
it can't be unambiguously attributed to the GRB by the triangulation,
so far. The total duration of the burst is ~338 s.

The emission is seen up to ~5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140808_T03239/

As observed by Konus-Wind, the first episode
had a fluence of 3.12(-0.30,+0.33)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.312 s,
of 1.6(-0.4,+0.4)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first episode
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.95 (-0.26,+0.29)
and Ep = 127 (-18,+25) keV (chi2 = 91/78 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 90/77 dof)

The second episode had a fluence of 4.2(-1.2,+4.0)x10^-6 erg/cm2,
in the 20 keV - 10 MeV energy range.

The time-averaged spectrum of this episode
(measured from T0+303.36 to T0+336.128 s)
is best fit in the 20 keV - 5 MeV range
by the power law with exponential cutoff model
with  alpha = -1.22 (-0.37,+0.48)
and Ep = 376 (-158,+1558) keV (chi2 = 82/88 dof).

Assuming the second episode is related to the GRB the total fluence
is 7.3(-1.2,+4.0)x10^-6 erg/cm2. From the redshift z=3.29
(Gorosabel et al., GCN Circ. 16671)
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:
the isotropic energy release E_iso is ~1.7x10^53 erg,
the peak luminosity L_iso is ~3.8x10^52 erg/s.

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


GRB_name: GRB140809A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16674
SUBJECT: GRB 140809A (FERMI trigger 429246673): MASTER follow-up inspection
DATE:    14/08/09 19:47:19 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Shumkov,  D.Denisenko, E. Gorbovskoy, V. Lipunov,
M.Pruzhinskaya, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa,
A.Kuznetsov, V.V.Chazov
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University


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

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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 starting survey on the FERMI  GRB140809A 
error-box (ra=11 15 14 dec=+71 00 36 r=6.040000)  52916 sec after trigger 
time at 2014-08-09 17:53:06 UT.

  During the observations of the error box of possible GRB 140809A (Fermi 
trigger 429246673) MASTER-Tunka auto-detection system discovered OT source 
at (RA, Dec) = 11h 46m 55.24s +66d 09m 59.3s on 2014-08-09.63454 UT ( 
Shumkov et al., Atel #6379). The 
OT unfiltered magnitude is 17.0m (limit 19.1m). The OT is seen in 6 
images. There is no minor planet at this place. We have reference image 
without OT on 2014-04-21.58762 UT with unfiltered magnitude limit 20.0m.

The new object is located 1.5" east and 17" north of the center of galaxy 
PGC 36760 = SDSS J114654.97+660942.3 (g=15.34 r=14.73 i=14.42) with 
z=0.0413. Discovery and reference images are available at: 
http://master.sai.msu.ru/static/OT/114655.24660959.3.png

It is   just a chance coincidence possible. Spectral and photometric 
confirmation is requested. Observations in X-rays and other wave bands are 
also strongly encouraged.

The OT search is continuated.

This message can be cited.


GRB_name: GRB140809A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16675
SUBJECT: GRB 140809A : Virtual Telescope optical observations
DATE:    14/08/09 20:26:09 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi, the Virtual Telescope Project - Italy, reports:

I observed the field of GRB 140809A (FERMI trigger
429246673) with with the 17" 
robotic unit part of the Virtual Telescope (Ceccano, Italy:
http://www.virtualtelescope.eu) at 9 Aug. 2014, 20:15:24 UT.

An optical source is visible where described by Shumkov et
al. (GCN 16674)  in 180-seconds integration images,
unfiltered. The position of the source is RA: 11 46 54.89
Decl.:+66 10 00.5 (J2000, mean residuals of 0.2") and the
magnitude was estimated to be 17.4 assuming R mags for the
reference stars from UCAC-4.

The message may be cited.


GRB_name: GRB140809A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16676
SUBJECT: Swift observations of possible GRB 140809A candidate
DATE:    14/08/10 14:15:04 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

NPM Kuin (UCL/MSSL), K.L.Page (U. Leicester) and F. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of Fermi Trigger
429246673 (GRB 140809A) as follow-up on the GRB candidate reported
detected by MASTER (Shumkov et al. (ATEL 6379) and confirmed by Masi
(GCN Circ. No 16675).  Swift observations started on  2014-08-10T00:55,
77.2 ks after the Fermi trigger.

We have analysed 2.0 ks of XRT data collected between 77.2-79.2 ks after
the trigger. No X-ray source was found, to an upper  limit of 4.0x10^-3
count s^-1 (3-sigma; 0.3-10 keV).

The UVOT observed the candidate field taking three v-band, one uvm2 and
one uvw2 exposure. The new source is found at the edge of a galaxy
(CG +11-15-003 at z=0.041372) and is only seen in the v-band, while the
uv bands appear dominated by galaxy emission. The source position is
consistent with that reported by Masi (GCN CIRC. No 16675).

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

 v            78122        79027          885         17.27 +/- 0.05
 m2           79032        79208          174         18.78 +/- 0.26
 w2           77214        78114          886         18.74 +/- 0.11

Times given relative to 2014-08-09T03:11:10.2.
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).

The source brightness remains close to the unfiltered magnitude reported by
MASTER, and has no X-ray counterpart.  Is therefore unlikely to be a GRB.


GRB_name: GRB140810A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16678
SUBJECT: GRB140810A: Fermi-LAT detection
DATE:    14/08/11 08:06:17 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

Elena Moretti (MPI Munich), Makoto Arimoto (Tokyo Tech),
Elisabetta Bissaldi (University & INFN Trieste), Sylvain Guiriec
(GSFC/CRESST/UMD) and Giacomo Vianello (Stanford University)
report on behalf of the Fermi-LAT team:


At UT 18:46:10.09 on August 10th, 2014, Fermi-LAT detected
high-energy emission from GRB 140810A, which was also
detected by Fermi-GBM (trigger 140810782/429389173).

The best LAT on-ground location is found to be

(RA, Dec) = 119.04, 27.55 (deg, J2000)

with an approximate error radius of 0.12 deg (90% containment,
statistical error only). The error circle is slightly asymmetric,
the Test Statistic localisation map (with 68% and 90% contours)
can be found here: http://fermigrb.stanford.edu/140810782.jpg.
The location could be updated later as more data become available
(at the moment of writing we can analyse up to 2000 s after the trigger).
The burst was 123 deg from the LAT boresight at the time of
the trigger and the high fluence detected by GBM caused the
GBM flight software to initiate a Fermi autonomous re-point
that placed the source in the LAT FoV about 330 s after the trigger.

The data from the Fermi-LAT show a significant increase
in the event rate that is spatially correlated
with the GBM emission with high significance.
More than 20 photons above 100 MeV and 3 photons
above 1 GeV are observed.
The highest-energy photon is a 16  GeV event,
which is observed about 1500 s after the GBM trigger.

A Swift ToO has been requested for this burst, but the burst can not
be observed due to Sun constrains.

The Fermi-LAT point of contact for this burst
is Elena Moretti (moretti@mpp.mpg.de)


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: GRB140810A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16679
SUBJECT: Konus-Wind observation of GRB 140810A
DATE:    14/08/11 09:25:04 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, A. Tsvetkova, A.Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 140810A (Fermi-LAT detection: Moretti et al., GCN 16678)
triggered Konus-Wind at T0=67571.433 s UT (18:46:11.433).

The light curve shows a multi-peaked structure with a total duration of ~100 s.
The emission is seen up to 10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 1.5(-0.1,+0.1)x10^-4 erg/cm2, and a 64-ms peak flux,
measured from T0+23.104 s, of 1.3(-0.1,+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+93.696 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 = -1.05 (-0.06,+0.05),
the high energy photon index beta = -2.35 (-0.16,+0.12),
the peak energy Ep = 239 (-26,+25) keV,
chi2 = 105/97 dof.

The spectrum near the peak count rate (measured from T0+16.640 to T0+29.959 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 = -0.86 (-0.10,+0.10),
the high energy photon index beta = -2.44 (-0.35,+0.17),
the peak energy Ep = 416 (-47,+63) keV,
chi2 = 87/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140810_T67571/

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


GRB_name: GRB140810A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16680
SUBJECT: GRB 140810A: Fermi GBM observation
DATE:    14/08/11 10:58:02 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

Oliver Roberts (UCD) and Matthew Stanbro (UAH)
report on behalf of the Fermi GBM Team:

"At 18:46:10.09  UT on the 10th of August 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140810A
(trigger 429389173 / 140810782), which was also detected by the LAT
(Bissaldi et al. 2014, GCN 16678). The trigger resulted in an
Autonomous Repoint Request (ARR) that was accepted. The GBM
on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight is 122 degrees.

The GBM light curve consists of multiple peaks with a duration (T90)
of about 82 s (50-300 keV). The time-averaged spectrum from
T0-3.58 s to T0+107.01 s is well fit by a power law function with an
exponential high-energy cutoff. The power law index is -1.01 +/- 0.01
and the cutoff energy, parameterised as Epeak, is 302 +/- 7 keV.

The event fluence (10-1000 keV) in this time interval is
(110.42 +/- 0.07)E-06 erg/cm^2. The 1.024-sec peak photon flux
measured from T0+6.6 s in the 10-1000 keV band, is
35.98+/-0.65 ph/s/cm^2.

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


GRB_name: GRB140809A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16681
SUBJECT: GRB140809A: Fermi GBM observation
DATE:    14/08/11 11:55:43 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

Oliver Roberts (UCD) and VÃ©ronique Pelassa (UAH)
reports on behalf of the Fermi GBM Team:

"At 03:11:10.20 UT on the 9th of August 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140809A
(trigger 429246673 / 140809133), for which a possible optical
transient was also detected by the MASTER II robotic telescope
(Lipunov et al. 2014, GCN 16674). The GBM on-ground location is
consistent with the OT position. The angle from the Fermi LAT
boresight is 40 degrees.

The GBM light curve consists of one bright pulse, followed by
a sequence of shorter, dimmer pulses with a duration (T90) of
about 70s (50-300 keV). The time-averaged spectrum from
T0-14.6 s to T0+70.1 s is adequately fit by a power law
function with an exponential high-energy cutoff. The power law
index is -0.99 +/- 0.14  and the cutoff energy, parameterised as
Epeak, is 507 +/- 192 keV.

The event fluence (10-1000 keV) in this time interval is
(2.10 +/- 0.04)E-06 erg/cm^2. The 1.024-sec peak photon flux
measured starting from T0+1.28 s in the 10-1000 keV band is
1.39 +/- 0.18 ph/s/cm^2.

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


GRB_name: GRB140808A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16682
SUBJECT: GRB 140808A: Confirmation of the Swift-XRT afterglow
DATE:    14/08/11 16:07:54 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and S.B. Cenko (NASA/GSFC) report on behalf of
the Swift-XRT team:

In GCN Circ. 16670, Page et al. reported the detection of an X-ray source
coincident with the iPTF optical source suggested to be the afterglow of
Fermi GRB 140808A (Singer et al., GCN Circ. 16668; Zhang, GCN Circ.
16669).

Starting 224 ks after the Fermi trigger, a second epoch of XRT data was
collected. The X-ray source is now no longer detected, having faded below
a 3-sigma upper limit of 2.46 x 10^-3 count s^-1 (0.3-10 keV). We
therefore confirm that this is the X-ray afterglow of GRB 140808A.

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


GRB_name: GRB140810A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16683
SUBJECT: IPN triangulation of GRB 140810A
DATE:    14/08/11 20:49:50 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN,

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,

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, 

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 140810A (Moretti et al. GCN 16678, Golenetskii et al. GCN 16679,
Roberts et al. GCN 16680) has been observed by Odyssey-HEND, MESSENGER
GRNS, Konus-Wind, INTEGRAL SPI-ACS, and Fermi GBM and LAT, so far.  We
have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:

  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   119.056 (07h 56m 13s) +27.413 (+27d 24' 47")
  Corners:
   119.076 (07h 56m 18s) +28.016 (+28d 00' 58")
   119.014 (07h 56m 04s) +26.723 (+26d 43' 23")
   119.470 (07h 57m 53s) +28.814 (+28d 48' 49")
   118.462 (07h 53m 51s) +25.183 (+25d 10' 57")
  ---------------------------------------------
The error box area is 1450  sq. arcmin., and its maximum/minimum
dimensions are 3.74/0.096 deg. 

This error box is consistent with the Fermi-LAT 90% confidence,
statistical-only error circle (GCN 16678), and constrains it slightly.
A map has been posted at ssl.berkeley.edu/ipn3/140810A.  This
localization may be improved.


GRB_name: GRB140808A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16684
SUBJECT: GRB 140808A / iPTF14eag optical follow-up at HCT
DATE:    14/08/12 06:27:45 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.ernet.in>

D. K. Sahu (IIA), V. Bhalerao (IUCAA), G. C. Anupama (IIA) report:

We imaged iPTF14eag, the optical counterpart of GRB 140808A (Singer et al., GCN Circ. 16668; Zhang, GCN Circ. 16669), with the  2m. Himalayan Chandra Telescope (HCT) â€‹ of the Indian Astronomical Observatory, Hanle, India. We obtained a total exposure of â€‹2700 sec in Bessell's R band, in the time range from UT 2014-08-08 15:37 to 16:38. The source was clearly detected with R = 20.6 +- 0.1. Combined with iPTF R band photometry (Singer et al., GCN Circ 16668), the decay fits a power law with slope -0.99 +- 0.02.

â€‹We thank the iPTF team for alerting us about this burst.â€‹


GRB_name: GRB140814A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16686
SUBJECT: GRB 140814A: MAXI/GSC detection
DATE:    14/08/14 12:55:45 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

D. Uchida (Oasaka U.), S. Nakahira, S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, 
Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M.Morii, J. Sugimoto, T. Takagi, 
A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi (Osaka U.),
H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba,
M. Fujita, F. Honda (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, A. Kawagoe (Chuo U.), M. Yamauchi, Y. Morooka (Miyazaki U.), 
K. Yamaoka (Nagoya U.), report on behalf of the MAXI team:

 The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient 
source at 2014-08-14T07:12:31 UT. 
Assuming that the source flux was constant over the transit,
we obtain the source position at

  (R.A., Dec) = (182.515 deg, 49.348 deg) = (12 10 03, +49 20 52) (J2000) 

with a statistical 90% C.L. elliptical error region with long and short radii 
of 0.33 deg and 0.27 deg respectively. 
The roll angle of long axis from the north direction is 126.0 deg 
counterclockwise. There is an additional systematic uncertainty of 0.1 deg 
(90% containment radius). The X-ray flux averaged over the scan was 
232 +- 45 mCrab (4-10keV, 1 sigma error).

 Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:

(R.A., Dec) = (182.052 deg, 48.309 deg) = (12 08 12, +48 18 32) (J2000)
(R.A., Dec) = (181.153 deg, 48.617 deg) = (12 04 36, +48 37 00) (J2000)
(R.A., Dec) = (182.777 deg, 50.186 deg) = (12 11 06, +50 11 07) (J2000)
(R.A., Dec) = (183.701 deg, 49.873 deg) = (12 14 48, +49 52 21) (J2000)

 There was no significant excess flux in the previous transit at UT 5:39 and 
in the next transit at 8:43 UT with an upper limit of 20 mCrab for each.
A burst spectrum is relatively soft, and a blackbody fit to the energy 
spectrum gives a temperature of about 1 keV.
Thus, a possibility of an X-ray burst can not be excluded.


GRB_name: GRB140814A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16687
SUBJECT: GRB 140814A: Swift-XRT and UVOT observations 
DATE:    14/08/14 22:58:47 GMT
FROM:    Angelica Vargas at PSU/Swift  <avargas@swift.psu.edu>

Hi all,
This a circular drat. UVOT information is missing. May we have further comments from UBS? 
Thanks,
Angie

GRB 140814A: Swift-XRT and UVOT observations

V.Mangano (PSU), [UBS]
report on behalf of the Swift team

Swift began observing the field of GRB 140814A  (Uchida et al,.  GCN Circ. on 2014-08-14 at 13:35:33 UT, 22.08 ks after the MAXI/GSC trigger. A tiled observation of four contiguous fields centered on the MAXI i.e., about 1 ks per field. Our mosaic covers the whole elliptical MAXI error circle (Uchida et al., GCN Circ. 16686).
In the XRT exposure, we do not find any new source, down to a three sigma upper limit of 3e-03 cts/s.

[UVOT par]
This circular is an official product of the Swift team.


GRB_name: GRB140814A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16688
SUBJECT: GRB 140814A: MASTER optical follow-up inspection
DATE:    14/08/15 12:09:00 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya,  V.Kornilov, D.Kuvshinov, 
N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, 
D.Denisenko, A.Sankovich
Lomonosov Moscow State University,
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, A. Gabovich
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 automaticaly inspected  GRB140814A  (Uchida et 
al., GCN 16686) error box. The observations was started at 2014-08-14 
17:36:16 UT i.e.  37425 sec (~10.3 h) after trigger time directly after 
sunset and proceeded within ~1 hour. We cover full MAXI error-box (Uchida 
et al. GCN 16686).  On our single and coadd images we not found credible 
optical transient brighter then 20.0m .

The 5-sigma upper limit has been about 18.5m on single 180 s image and 
20.0m on coadd of 10 images with total exposure 1800 s.

The message may be cited.


GRB_name: GRB140814A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16689
SUBJECT: GRB 140814A: Swift-XRT and UVOT observations  
DATE:    14/08/15 14:35:01 GMT
FROM:    Angelica Vargas at PSU/Swift  <avargas@swift.psu.edu>

GRB 140814A: Swift-XRT and UVOT observations 

A. Vargas, V. Mangano, M. Siegel (PSU)
report on behalf of the Swift team.
Please disregard GCN Circ. 16887, which was sent in error. We apologize for the inconvenience.

Swift began observing the field of GRB 140814A  (Uchida et al,.  GCN Circ. 16686) on 2014-08-14 at 13:35:33 UT, 22 ks after the MAXI/GSC trigger. Swift performed tiled observations of four contiguous fields, centered on the MAXI error ellipse, with an exposure of 1 ks per field. Our mosaic covers the whole elliptical MAXI error circle (Uchida et al., GCN Circ. 16686). 
In the XRT exposure, we do not find any new source, down to a three sigma upper limit of 3e-03 cts/s. 

UVOT began observing the field 22 ks after the MAXI/GSC trigger.  Observations of 871-937 seconds per tile were obtained in the u filter. No new source was detected down to a limiting magnitude of 20.

This circular is an official product of the Swift team.


GRB_name: GRB140815A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16690
SUBJECT: GRB 140815A: A long GRB detected by INTEGRAL
DATE:    14/08/15 22:58:11 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 8 s has been detected by IBAS in the 
IBIS/ISGRI data at 21:55:05 UT of 2014 August 15.

The refined coordinates (J2000) are:
R.A.=   86.895698
DEC.=   -8.672829

with an uncertainty of  2.5   arcmin (90% c.l.).

A preliminary analysis gave a peak flux of about 1 count/cm2/s (20-200 
keV, 1-s integration time) and a fluence in the same energy range of about 
3e-7 erg/cmq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB140815A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16691
SUBJECT: GRB 140815A: Swift-XRT observations
DATE:    14/08/16 15:16:17 GMT
FROM:    Angelica Vargas at PSU/Swift  <avargas@swift.psu.edu>

V. Mangano (PSU), A. Vargas (PSU)  reports on behalf of the Swift-XRT
team:

We have analysed 2.4 ks of XRT data for the INTEGRAL-detected burst:
GRB 140815A,  from 19.2 ks to 31.8 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. Using 2156 s of PC mode data
and 2 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 = 86.89221, -8.68015 which is equivalent to:

RA (J2000): 05h 47m 34.13s
Dec(J2000): -08d 40' 48.5"

with an uncertainty of 2.6 arcsec (radius, 90% confidence). This
position is 29 arcsec from the INTEGRAL position.  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/00020406.

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


GRB_name: GRB140815A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16693
SUBJECT: GRB 140815A: GROND afterglow candidate
DATE:    14/08/16 20:05:38 GMT
FROM:    Mohit Tanga at MPE/GROND  <mohit@mpe.mpg.de>

GRB 140815A: GROND afterglow candidate

J.F. Graham, M. Tanga and J. Greiner (all MPE Garching) report on behalf of
the GROND team:

We observed the field of GRB 140815A (Mereghetti et al., GCN #16690)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile).

Observations started at 08:17 UT on 16 August 2014, 10.37 hours after
the INTEGRAL trigger. They were performed at an average seeing of 1".3
and at an average airmass of 1.5.

We report the presence of a source within the XRT error circle
(Mangano et al., GCN #16691) at:

RA(J2000) = 86.89231 = 05h 47m 34.15s
Dec(J2000) = -8.68021 = -08d 40' 48.7"

which has the following preliminary magnitudes and upper limits (all in
AB) at a mid-time of 09:30 UT:

g' > 24.0
r' > 24.0
i' = 23.3 +/- 0.3
z' = 22.2 +/- 0.2
J  = 21.2 +/- 0.3
H  > 20.3
K  > 19.3

At the moment we cannot determine whether or not the source is fading.

Given magnitudes are calibrated against GROND zero points as well as 2MASS
field stars (JHK) and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=1.10 mag in
the direction of the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB140808A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16694
SUBJECT: GRB 140808A / PTFeag: VLA K-band observations
DATE:    14/08/16 21:12:47 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi (Texas Tech) and A. Horesh (Weizmann Inst.) report on behalf of a larger collaboration:

We imaged the position of PTF14eag (the optical afterglow candidate of
GRB 140808A; Singer et al., GCN 16668) with the Karl G. Jansky Very
Large Array (VLA) in K-band, starting at about 2.1 days after the Fermi 
trigger 429152043 / 140808038 (Zhang, GCN 16669). A provisional
reduction shows a source consistent with the location of PTF14eag. 
At this time, we estimate a preliminary flux of about  130 uJy at 22 GHz.
The image rms is about 19 uJy. 

Further observations are planned.


GRB_name: GRB140817A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16695
SUBJECT: GRB 140817A: Swift detection of a burst
DATE:    14/08/17 07:24:58 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B. Sbarufatti (INAF-OAB/PSU), J. R. Cummings (NASA/UMBC),
C. Gronwall (PSU) and D. M. Palmer (LANL) report on behalf of the
Swift Team:

At 07:02:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140817A (trigger=609736).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 127.256, +58.189 which is 
   RA(J2000) = 08h 29m 01s
   Dec(J2000) = +58d 11' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiply-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~16000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 07:03:36.4 UT, 95.2 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 100 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 5% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.15. 

Burst Advocate for this burst is B. Sbarufatti (boris.sbarufatti 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: GRB140817A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16696
SUBJECT: GRB 140817A: Swift-XRT position
DATE:    14/08/17 08:22:47 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/PSU) reports on behalf of the Swift-XRT team

Using promptly downlinked data we find a bright, fading X-ray
source with an enhanced position: RA,Dec = 127.2646, 58.1901
(degrees) which is equivalent to:

RA  (J2000) = 08 29 03.51
DEC (J2000) = +58 11 24.4

with an uncertainty of 2.2 arcsec (radius, 90% containment).
This location is 16.8 arcseconds from the BAT onboard position, inside the BAT
error circle.


GRB_name: GRB140817A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16697
SUBJECT: GRB 140817A: Enhanced Swift-XRT position
DATE:    14/08/17 10:09:35 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 448 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140817A, 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 = 127.26394, +58.19002 which is equivalent
to:

RA (J2000): 08h 29m 3.35s
Dec (J2000): +58d 11' 24.1"

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: GRB140817A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16698
SUBJECT: GRB 140817A draft circular on nearby galaxy
DATE:    14/08/17 16:46:49 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

GRB 140817A Close to nearby galaxy

J. R. Cummings, K. L. Page (U Leicester) on behalf of the Swift science team:

We note the presence of a low-redshift galaxy in DSS, SDSS, 2MASS (SIMBAD) whose
center is 98 arcseconds from the center of the Swift-XRT refined position error
circle (Osborne, GCN Circ. # 16697), MCG+10-12-141 at z ~ 0.018368. The angular
size of the galaxy is about 0.8 arcmin.


GRB_name: GRB140817A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16699
SUBJECT: GRB 140817A: Swift-BAT refined analysis
DATE:    14/08/17 17:16:02 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings, S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), 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-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140817A (trigger #609736)
(Sbarufatti, et al., GCN Circ. 16695).  The BAT ground-calculated position is
RA, Dec = 127.244, 58.191 deg which is
    RA(J2000)  =  08h 28m 58.5s
    Dec(J2000) = +58d 11' 27.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
  
The mask-weighted light curve shows multiple sharp peaks from T-20 to T+12 seconds,
then a return to background levels until about T+170 seconds where 2 overlapping
FRED peaks begin, lasting until about T+250 seconds.  T90 (15-350 keV) is
244 +- 13 sec (estimated error including systematics).
  
The time-averaged spectrum from T-21.26 to T+270.27 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.48 +- 0.08.  The fluence in the 15-150 keV band is 4.6 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+2.64 sec in the 15-150 keV band
is 7.2 +- 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/609736/BA/


GRB_name: GRB140817A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16700
SUBJECT: GRB 140817A: Fermi GBM Detection
DATE:    14/08/17 18:48:16 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

Oliver Roberts (UCD) and Charles Meegan (UAH) report on behalf of
the Fermi GBM Team:

"At 07:01:58.19 UT on the 17th of August 2014, the Fermi Gamma-Ray
 Burst Monitor triggered and located GRB 140817A (trigger 429951721
/ 140817293), which was also detected by the BAT and XRT on Swift
(Sbarufatti et al., Evans et al. and Cummings et al. 2014, GCNs
16695-99). The GBM on-ground location is consistent with the Swift
position. The angle from the Fermi LAT boresight is 124 degrees.

The GBM light curve consists of two bright peaks with a duration (T90)
of about 16 s (50-300 keV). The time-averaged spectrum from T0-9 s to
T0+16 s is adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.64 +/- 0.19  and the
cutoff energy, parameterised as Epeak, is 130 +/- 11 keV.

The event fluence (10-1000 keV) in this time interval is
(5.03 +/- 0.04)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+5.8 s in the 10-1000 keV band is 10.6 +/- 0.5 ph/s/cm^2.

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


GRB_name: GRB140817A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16701
SUBJECT: GRB 140817A: Swift-XRT refined Analysis
DATE:    14/08/17 19:25:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.9 ks of XRT data for GRB 140817A (Sbarufatti  et al.
GCN Circ. 16695),  from 79 s to 29.9 ks after the  BAT trigger. The
data comprise 590 s in Windowed Timing (WT) mode (the first 9 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
Osborne et al. (GCN Circ. 16697).

The late-time light curve (from T0+4.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.86 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.625 (+/-0.030). The
best-fitting absorption column is  2.45 (+0.15, -0.14) x 10^21 cm^-2,
in excess of the Galactic value of 8.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.79 (+0.11, -0.10)
and a best-fitting absorption column of 2.3 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.0 x 10^-11 (5.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 8.0 x 10^20 cm^-2
Excess significance: 6.1 sigma
Photon index:      1.79 (+0.11, -0.10)

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 0.033 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.3 x
10^-12 (1.7 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/00609736.

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


GRB_name: GRB140818A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16702
SUBJECT: GRB 140818A: MAXI/GSC detection
DATE:    14/08/18 06:29:01 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

F. Honda, K. Suzuki, H. Negoro (Nihon U.), M. Serino (RIKEN), 
S. Nakahira, S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), 
T. Mihara, M. Sugizaki, M.Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), 
N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, D. Uchida (Osaka U.),
Nakajima, K. Fukushima, T. Onodera, T. Namba, M. Fujita (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, A. Kawagoe (Chuo U.), M. Yamauchi, Y. Morooka (Miyazaki U.), 
K. Yamaoka (Nagoya U.), report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient 
source at 2014-08-18T08:31:56 UT. 
Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (199.554 deg, 6.888 deg) = (13 18 12, +06 53 15)  (J2000) 

with a statistical 90% C.L. statistical error of 0.07 deg and an additional systematic 
uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 1125 +- 62 mCrab mCrab (4-10keV, 1 sigma error).
A energy spectrum fit with the absorbed (Nh=2.5e20) power-law model gives 
a photon index of 1.03 (+0.13/-0.12).


GRB_name: GRB140818A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16703
SUBJECT: GRB 140818A Tiled Swift observations
DATE:    14/08/18 08:38:26 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
MAXI GRB 140818A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00029

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 MAXI 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: GRB140817A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16704
SUBJECT: Konus-Wind observation of GRB 140817A
DATE:    14/08/18 13:51:37 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, A. Tsvetkova, A.Lyssenko, and T. Cline
on behalf of the Konus-Wind team, report:

A long-duration GRB 140817A (Swift-BAT trigger 609736:
Sbarufatti et al., GCN 16695; Cummings et al., GCN 16699;
Fermi-GBM detection: Roberts & Meegan, GCN 16700)
triggered Konus-Wind at T0=25319.509 s UT (07:01:59.509).

The light curve shows a double-peaked structure from ~T0-0.5 s to ~T0+3.5 s,
the emission in this episode is visible up to ~8 MeV.
The subsequent broad, weak, soft pulse is visible in the instrument's
soft energy channel from ~T0+160 s to ~T0+270 s; it coincides in time with
the bright X-ray flare in the XRT light curve
(http://www.swift.ac.uk/xrt_products/00609736).

As observed by Konus-Wind, the burst had a fluence
of 3.4(-0.3,+0.3)x10^-6 erg/cm2, and a 64-ms peak flux,
measured from T0+2.816 s, of 3.0(-0.3,+0.3)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst (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 = -0.22 (-0.37,+0.40),
the high energy photon index beta = -2.8 (-7.2,+0.4),
the peak energy Ep = 118 (-18,+29) keV,
chi2 = 84/84 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140817_T25319/

All the quoted errors are at the 95% confidence level.
All the quoted values are preliminary.


GRB_name: GRB140818A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16705
SUBJECT: GRB 140818A: Correction to GCN 16702
DATE:    14/08/18 14:42:40 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

H. Negoro, F. Honda  (Nihon U.) report on behalf of the MAXI team:

The trigger time of MAXI-GSC detection of GRB 140818A reported in
GCN 16702 is incorrect. The correct trigger time is "2014-08-18T05:31:28 UT",
and about 79 sec after the Fermi-GBM detection (Triger Number 430032612).
The time and the location of Fermi-GBM and MAXI-GSC GRBs suggest that
that the bursts are the same origin.
We apologize for the mistake.


GRB_name: GRB140818A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16706
SUBJECT: GRB 140818A: Swift-XRT and UVOT potential afterglow detection
DATE:    14/08/18 15:05:41 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

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

Swift-XRT has observed the error circle of the MAXI GRB 140818A in a
series of observations tiled on the sky. The total exposure time is 2.3
ks spread over 4 fields; the maximum exposure within the sky observed
was 1.0 ks. The observations started 10.5 ks after the MAXI trigger (Honda
et al., GCN Circ. 16702). Within these data we detect a bright, 
uncatalogued
X-ray source at RA, Dec= 199.56275, 6.92254 which is equivalent to:
   RA (J2000) = 13h 18m 15.06s
   Dec (J2000) = +06d 55' 21.1"
with an uncertainty of 2.1 arcsec (radius, 90% confidence).  This is an
enhanced position, determined by using UVOT field stars to determine
the astrometry.The exposure at this location was 746 s.

This previously uncatalogued source is significantly brighter than the
RASS limit, and we thus consider it the likely GRB afterglow.

The results of the automatic processing for this source are available
at http://www.swift.ac.uk/xrt_products/TILED_GRB00029/index_1.php

The Swift/UVOT began settled observations of the field of GRB 140818A
10467 s after the MAXI trigger.
A source consistent with the XRT position is detected in the initial
UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  13:18:15.08 = 199.56285 (deg.)
     Dec (J2000) = +06:55:22.6  =   6.92295 (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

u                10467        11094          617         19.21  0.12

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: GRB140818A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16708
SUBJECT: GRB 140818A - Fermi GBM Detection
DATE:    14/08/18 18:08:23 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

Oliver Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 05:30:09.12 UT on the 18th of August 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140818A (trigger 430032612
/ 140818229), which was also detected by MAXI/GSC (H. Negoro et al.
GCN 16702 and GCN 16705). A possible afterglow has also been reported
by Swift-XRT and UVOT (C. Swenson et al. GCN 16706)  The GBM
on-ground location is consistent with the MAXI/GSC and Swift positions.
The angle from the Fermi LAT boresight is 35 degrees.

The GBM light curve consists of two peaks, with the second peak
at T~50s being brighter than the first. The duration (T90) of the
burst is about 109 s (50-300 keV). The time-averaged spectrum from
T0+25s to T0+135 s is adequately fit by a BAND function. The power
law index alpha is -0.69 +/- 0.04 . The power law index beta is
-2.39 +/- 0.10 . The cutoff energy, parameterised as Epeak, is
181 +/- 8 keV.

The event fluence (10-1000 keV) in this time interval is
(2.95 +/- 0.06)E-05 erg/cm^2. The 1.024-sec peak photon flux was
measured starting from T0+99.5 s in the 10-1000 keV band is
8.6 +/- 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: GRB140818B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16709
SUBJECT: GRB 140818B: Swift detection of a burst
DATE:    14/08/18 18:58:42 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

A. Vargas (PSU), D. N. Burrows (PSU), S. B. Cenko (GSFC),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), L. M. Z. Hagen (PSU),
J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC), J. L. Racusin (NASA/GSFC),
B. Sbarufatti (INAF-OAB/PSU) and C. A. Swenson (PSU) report on behalf
of the Swift Team:

At 18:44:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140818B (trigger=609885).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 271.148, -1.361 which is 
   RA(J2000) = 18h 04m 35s
   Dec(J2000) = -01d 21' 40"
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 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 18:46:05.6 UT, 109.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 271.13656, -1.38660 which is equivalent
to:
   RA(J2000)  = 18h 04m 32.77s
   Dec(J2000) = -01d 23' 11.8"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 100 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 3.53
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 113 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 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 expected
extinction corresponding to E(B-V) of 0.71. 

Burst Advocate for this burst is A. Vargas (avargas AT swift.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: GRB140817A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16710
SUBJECT: GRB 140817A: Swift/UVOT Afterglow Detection
DATE:    14/08/18 21:40:21 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and B. Sbarufatti (INAF-OAB/PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140817A
101 s after the BAT trigger (Sbarufatti et al., GCN Circ. 16695).
A fading source consistent with the UVOT-enhanced XRT position
(Osborne et al. GCN Circ. 16697) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  08:29:03.21 = 127.26336 (deg.)
  Dec (J2000) =  58:11:24.7  =  58.19020 (deg.)
with an estimated uncertainty of 0.53 arc sec. (radius, 90% confidence).

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              101         1017          334         20.3 +/- 0.17
white             5426        18414         1794        >21.6
v                  642         1068           58        >18.0
b                  568          762           39        >18.5
u                  313         4899          435        >20.5
w1                 692         1117           39        >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140818B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16711
SUBJECT: GRB 140818B: OSN I-band afterglow candidate
DATE:    14/08/18 22:50:24 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

F.J. Aceituno (OSN/IAA-CSIC), J. Gorosabel (IAA-CSIC/UPV-EHU) and A.J.
Castro-Tirado (IAA-CSIC/UMA), report on behalf of a larger collaboration:

We observed the field of GRB 140818B (Vargas et al., GCN 16709) with the
1.5m OSN telescope at Observatorio de Sierra Nevada (Spain). Several 300s
images were acquired in the I- and R-band starting on Aug 18, 20:15 UT
(i.e. 1.5 hours post burst). An optical source at the edge of the
Swift/XRT error box is detected at coordinates (J2000) RA: 18 04 32.47,
Dec: -01 23 09.8 (+/- 1"), which is not present in the corresponding DSS-2
image. A preliminary photometry  against  the USNO  B1.0  catalog yields
an I-band magnitude of 19.7 (Vega). At the moment we cannot determine if
the source if fading in brightness. Further observations are encouraged.


GRB_name: GRB140818B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16712
SUBJECT: GRB 140818B: Enhanced Swift-XRT position
DATE:    14/08/19 00:18:06 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 990 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140818B, 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 = 271.13556, -1.38629 which is equivalent
to:

RA (J2000): 18h 04m 32.53s
Dec (J2000): -01d 23' 10.6"

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

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140818B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16713
SUBJECT: GRB140818B : GROND afterglow candidate
DATE:    14/08/19 02:45:09 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

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

We observed the field of GRB 140818B (Swift-60985; Vargas et al., GCN
16709) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,PASP
120, 405) mounted at the 2.2m MPG telescope at ESO La Silla Observatory
(Chile). Observations started at 23:43 UT on 2014-08-18, 5 hours after the
GRB trigger. They were performed at an average seeing of  1.23"  and at an
average airmass of 1.2.

Based on images with exposure times of  340s in gr'i'z and 370s in JHKs,
we detect a source inside the 1.9 error circle reported by Beardmore et
al. (GCN 16712) at

RA (J2000): 18h 04m 32.47s
Dec (J2000): -01d 23 09.7"

with an uncertainty of 0.5 and magnitudes

g > 24.1 mag,
r' = 22.1 +/- 0.1 mag,
i' = 21.8 +/- 0.1 mag,
z' = 21.4 +/- 0.1 mag.
J > 20.9 mag,
H > 20.7 mag, and
K > 19.2 mag.

The afterglow candidate reported by Aceituno et al. (GCN #16711) is also
detected inside the 3.9 XRT error circle (GCN 16711) but not inside the
1.9 XRT error circle (GCN 16712) with magnitudes :

r' = 22.4 +/- 0.1 mag,
i' = 21.6 +/- 0.1 mag,
z' = 20.9 +/- 0.1 mag.

The given magnitudes are derived based on calibrating the images against
the GROND zeropoints and 2MASS field stars are not corrected for the
Galactic foreground extinction corresponding to a reddening of E_(B-V) = 0.73
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140818B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16714
SUBJECT: GRB 140818B: Fermi GBM detection
DATE:    14/08/19 03:03:05 GMT
FROM:    Eric Burns at U of Alabama  <EricKayserBurns@gmail.com>

Eric Burns (UAH) reports on behalf of the Fermi GBM Team:

"At 18:44:15.70 UT on 18 August 2014, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 140818B (trigger 430080258
/ 140818781). which was also detected by the Swift/BAT
(Burrows et al. 2014, GCN 16709). The GBM on-ground
location is consistent with the Swift position. The angle
from the Fermi LAT boresight is 32 degrees.

The GBM light curve consists of one main peak followed by
multiple smaller peaks with a duration (T90) of about 23.6 s
(50-300 keV). The time-averaged spectrum from T0-6.14 s to
T0+20.5 s is best fit by a simple power law function with
index -1.7 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+0.26 s in the 10-1000 keV band
is 1.7 +/- 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: GRB140808A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16715
SUBJECT: Radio upper limit on the GRB 140808A with the GMRT
DATE:    14/08/19 08:37:16 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

Poonam Chandra (NCRA-TIFR) and A. J. Nayana (NCRA-TIFR)  report on behalf
of a larger collaboration:

We carried out the Giant Metrewave Radio Telescope (GMRT) observations of
GRB 1400808A in the 1390 MHz band on 2014 August 18.66 UT.
We do not detect the radio afterglow of the GRB at the optical position
(Singer et al. GCN 16668). The 3-sigma upper limit at the GRB position
  is 160 uJy and the map resolution is "4.03x1.89".

We thank GMRT staff for making these observations possible.


GRB_name: GRB140818B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16716
SUBJECT: GRB 140818B: Swift-XRT refined Analysis
DATE:    14/08/19 12:58:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B.P. Gompertz (U. Leicester), M. de Pasquale (INAF-IASFPA), A. Maselli 
(INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), V. Mangano
(PSU), M.C. Stroh (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester) and A. Vargas report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 140818B (Vargas  et al. GCN
Circ. 16709),  from 94 s to 52.9 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 Beardmore et al. (GCN Circ.
16712).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.64 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+/-0.3). The
best-fitting absorption column is  5.6 (+2.0, -1.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.5 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.6 x 10^-11 (7.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.6 (+2.0, -1.6) x 10^21 cm^-2
Galactic foreground: 3.5 x 10^21 cm^-2
Excess significance: 2.1 sigma
Photon index:      2.3 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
0.64, the count rate at T+24 hours will be 6.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 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/00609885.

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


GRB_name: GRB140818B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16717
SUBJECT: GRB 140818B: Swift/UVOT Upper Limits
DATE:    14/08/19 13:10:44 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and A. Vargas (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140818B
114 s after the BAT trigger (Vargas et al., GCN Circ. 16709).  No optical
afterglow consistent with the XRT position (Beardmore et al. GCN Circ.
16712), the OSN candidate (Aceituno et al. GCN Circ 16711), or the GROND
candidate (Knust et al. GCN Circ 16713) 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 early
exposures are:

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

white              113         5136          530         >21.32
v                  654         5546          254         >19.28
b                  581         4931          235         >20.11
u                  325         6007          506         >20.17
uvw1               704         5956          416         >19.92
uvm2              5551         5751          196         >19.53
uvw2               803         5341          235         >19.97

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.70 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140818B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16718
SUBJECT: GRB 140818B : Correction to GCN 16713
DATE:    14/08/19 13:15:25 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

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

The afterglow candidate reported in GCN 16713 is the same as the one
reported by Aceituno et al. (GCN 16711) located at the edge of the 1.9
arcsec XRT error  circle at:

RA (J2000): 18:04:32.47
Dec (J2000): -01:23:09.7

The GROND i-band magnitude suggests it has decayed by about 2 magnitudes
within 3.5 hours, thus confirming this source to be the afterglow of GRB
140818B.

The magnitudes of the second source reported correspond to a source at the
edge of the 3.9 arcsec XRT error circle at :

RA (J2000): 18:04:32.78
Dec (J2000): -01:23:08.43

We apologize for this mistake.


GRB_name: GRB140818A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16719
SUBJECT: Konus-Wind observation of GRB 140818A
DATE:    14/08/19 14:37:57 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

A long duration GRB 140818A (MAXI/GSC detection: Honda et al., GCN 
16702, 16705; Fermi-GBM detection: Roberts, GCN 16708) triggered 
Konus-Wind at T0=19880.472 s UT (05:31:20.472).

The burst light curve shows a rather weak pulse at ~T0-83 s followed by 
the main emission episode at ~T0-15 s. The total duration of the burst 
is ~126 s. The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140818_T19880/

As observed by Konus-Wind, the burst
had a fluence of 3.68(-0.21,+0.22)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+24.304 s,
of (2.29+/-0.49)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+41.216 s)
is best fit in the 20 keV - 3 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.11 (-0.13,+0.14)
and Ep = 219 (-21,+26) keV (chi2 = 68/68 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.7
(chi2 = 68/67 dof)

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


GRB_name: GRB140818B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16721
SUBJECT: GRB 140818B, Swift-BAT refined analysis
DATE:    14/08/19 19:08:38 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
A. Vargas (PSU) (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 140818B (trigger #609885)
(Vargas, et al., GCN Circ. 16709).  The BAT ground-calculated position is
RA, Dec = 271.168, -1.354 deg which is
  RA(J2000)  =  18h 04m 40.2s
  Dec(J2000) = -01d 21' 14.3"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 39%.

The mask-weighted light curve shows a single-peaked structure starts at ~T-4 sec and
peaks at ~ T+1 sec. The main pulse ends at ~T+2 sec, with some weak emission lasting
till ~T+18 sec. T90 (15-350 keV) is 18.1 +- 5.0 sec (estimated error including systematics).

The time-averaged spectrum from T-3.5 to T+18.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.99 +- 0.25.  The fluence in the 15-150 keV band is 5.4 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.31 sec in the 15-150 keV band
is 1.1 +- 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/609885/BA/


GRB_name: GRB140819A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16724
SUBJECT: GRB140819A: Deep GROND Upper Limits
DATE:    14/08/20 01:31:51 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

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

We observed the field of GRB 140819A (Fermi trigger 430148973; optical
candidate: Lipunov et al., GCN #16720) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG
telescope at ESO La Silla Observatory (Chile).

Observations started on August 19, 2014, at 23:42 UT, 9.9 hrs after the
GRB trigger. They were performed at an average seeing of 1.0" and at an
average airmass of 1.1.

We do not detect a source at the postion of the afterglow candidate
reported by Lipunov et al. (GCN #16720).

Based on a total exposure of 25 minutes in g'r'i'z'and 20 minutes in JHK,
at a midtime of 0.42 days after the burst, we measure the following
preliminary upper limits (AB magnitudes system):

g' > 25.0,
r' > 25.0,
i' > 24.1,
z' > 23.6,
J  > 20.9,
H  > 20.7, and
K  > 18.8.

These derived upper limits are significantly deeper than those reported
beforehand (Espartero et al., GCN #16772, Dichiara et al., GCN #16773).

The decay slope between the 10th magnitude detection at a minute after the
GRB and r' > 25 mag at 10 hours implies a decay slope > 2. Such a steep
slope over a prolonged period of time is unlikely. Note that if the
transient is not seen already in the second image taken by MASTER, an even
steeper slope is implied (assuming a magnitude limit of 12.6 for the
image).

We therefore propose the optical transient is unassociated with the GRB,
and may be due to, e.g., a glint off a tumbling object in near Earth
orbit.

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) = 0.58 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140808A
Detection_method: AMI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16725
SUBJECT: GRB 140808A/iPTF14eag: AMI 15 GHz detection
DATE:    14/08/20 09:16:00 GMT
FROM:    Gemma Anderson at U of Oxford  <gemma.anderson@astro.ox.ac.uk>

G. E. Anderson, T. D. Staley, R. P. Fender (University of Oxford),
M. M. Kasliwal (Carnegie), A. Horesh (Caltech)
We observed the position of iPTF14eag (Singer et al., GCN 16668),
which is the optical afterglow of the Fermi GBM detected GRB 140808A
(Zhang, GCN 16669), at 15 GHz with the Arcminute Microkelvin Imager
(AMI-LA). The observations started on 2014 August 18.61 to 18.78 UT,
corresponding to 10.6 days post-burst. We have detected the radio
counterpart (Corsi et al., GCN 16694) with a preliminary flux of
0.30 +/- 0.06 mJy.

An earlier observation conducted on 2014 August 12.61 to 12.78 UT,
corresponding to 4.6 days post-burst, yielded a marginal 3.8 sigma
detection of 0.15 +/- 0.04 mJy.

Further AMI monitoring is planned. We thank the AMI staff for scheduling
these observations.

These observations were made as part of the 4 PI SKY project.


GRB_name: GRB140818A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16726
SUBJECT: GRB 140818A: GROND confirmation of afterglow candidate
DATE:    14/08/20 13:22:12 GMT
FROM:    Fabian Knust at MPE/GROND  <fknust@mpe.mpg.de>

GRB 140818A: GROND confirmation of afterglow candidate

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

We observed the field of GRB 140818A (MAXI/GSC nova alert; Honda et al., GCN 16702) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).

Observations started at 23:15 UT on 2014-08-18, 15 hours after the GRB trigger. They were performed at an average seeing of  2.7" and at an average airmass of 1.9.

We detect an optical/NIR counterpart at the position of the Swift-XRT and UVOT afterglow candidate reported by Swenson et al. (GCN 16706) with magnitudes


g' = 22.4 +/- 0.2 mag,

r' = 21.7 +/- 0.1 mag,

i' = 22.0 +/- 0.2 mag,

z' > 21.9 mag,

J >  20.7mag,

H > 20.2 mag, and

K > 17.7 mag

all in AB system. GROND photometry indicates that the UVOT  source (Swenson et al., GCN 16706)   has faded, confirming it as the afterglow.


The given magnitudes are derived based on calibrating the images against SDSS zeropoints and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)=  0.036 mag in the direction of the burst (Schlegel et al. 1998). 

[GCN OPS NOTE(20aug14): Per author's request, the "draft" language was removed.]


GRB_name: GRB140818B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16728
SUBJECT: GRB 140818B:  ISON-Kislovodsk and ISON-Burakan optical upper limit
DATE:    14/08/20 14:50:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), E. Romas (ISON), V. Nevskiy (ISON), G. Ohanian 
(Byurakan Astrophisical Observatory), H. Andreasyan (Byurakan 
Astrophisical Observatory), A. Volnova (IKI),  I. Molotov (KIAM), 
report on  behalf of larger collaboration:

We observed the field of  GRB 140818B (Vargas et al., GCN 16709) with 
Santel-400AN   telescope of ISON-Kislovodsk observatory starting on (UT) 
18:54:36 and ISON-Burakan ORI-40 starting on (UT) 18:55:08. In the 
enhanced XRT position (Beardmore et al., GCN 16712)   we do not detect 
optical afterglow candidate (Aceituno et al., GCN 16711; Knust et al., 
GCN 16713) neither in the first image nor in the stacked images. 
Preliminary photometry is based on nearby USNO-B1.0 stars, R2 magnitudes:


Date       UT start   t-T0    Filter   Exp.   UL(3 sigma) Observatory
                      (mid, days)        (s)

2014-08-18 18:54:36  0.0198   None    7*100   19.0        Kislovodsk

2014-08-18 18:55:08  0.0174   None    21*60   18.5        Burakan


GRB_name: GRB140817A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16729
SUBJECT: GRB 140817A:  Khureltogot optical upper limit
DATE:    14/08/20 17:29:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI),  N. Tungalag (Research Center of Astronomy and 
Geophysics MAS),  S. Schmalz (AIP), A. Volnova (IKI), I.Molotov (KIAM) 
report on behalf of larger GRB follow-up collaboration:

We observed the  field of GRB 140817A (Sbarufatti et al., GCN 16695) 
with ORI-40 telescope of Khureltogot observatory.  We started 
observation on Aug. 17 (UT) 14:20:48 and obtained 60 unfiltered images 
of 60 s exposure. Within enhanced XRT error circle  (Osborne et al., GCN 
16697) we do not detect any new object and in particular the afterglow 
candidate (Marshall et al., GCN 16710). Details of a photometry of the 
stacked image is following

Date       UT start   t-T0    Filter   Exp.   UL(3 sigma)
                      (mid, days)        (s)

2014-08-17 14:20:48  0.3269   None    60*60   18.2

The photometry is based on USNO-B1.0 star 1481-0233222 assuming 
R=15.43.


GRB_name: GRB140817A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16731
SUBJECT: GRB 140817A: NOT optical observations
DATE:    14/08/21 16:01:53 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI), Jyri Lehtinen (Univ. Helsinki), and Pall 
Jakobsson (Univ. Iceland), report on behalf of a larger collaboration:

We observed the field of GRB 140817A (Sbarufatti et al., GCN 16695) with 
the Nordic Optical Telescope (NOT) equipped with the AlFOSC camera. 
Observations were carried out starting on 2014 Aug 20.23 UT (2.94 days 
after the GRB), at high airmass and in twilight, for a total exposure of 
15 min.

No source is detected at the position of the UVOT optical afterglow 
(Marshall & Sbarufatti, GCN 16710) nor within the XRT error circle 
(Sbarufatti, GCN 16696; Osborne et al., GCN 16697) down to a 3-sigma 
limiting magnitude of R = 21 (calibrated against the USNO-B1.0 catalog).

The galaxy MCG +10-12-141 at z ~ 0.018, around 1 arcmin away of the XRT 
position, is well detected in our images (Cummings & Page, GCN 16698). 
We note that a supernova similar to SN 1998bw would have R ~ 17.5 at z = 
0.018 at a comparable epoch. We thus disfavor the association of GRB 
140817A with the nearby galaxy.


GRB_name: GRB140824A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16732
SUBJECT: GRB 140824A: Swift detection of a burst
DATE:    14/08/24 08:55:04 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

A. P. Beardmore (U Leicester), H. A. Krimm (CRESST/GSFC/USRA),
C. J. Mountford (U Leicester) and K. L. Page (U Leicester) report on
behalf of the Swift Team:

At 08:40:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140824A (trigger=610501).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 206.644, +33.297 which is 
   RA(J2000) = 13h 46m 35s
   Dec(J2000) = +33d 17' 50"
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 5 sec.  The peak count rate
was ~2700 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 08:41:43.2 UT, 75.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 206.6168, 33.2935 which
is equivalent to:
   RA(J2000)  = 13h 46m 28.03s
   Dec(J2000) = +33d 17' 36.6"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 82 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 1.46
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 79 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
0.02. 

Burst Advocate for this burst is A. P. Beardmore (apb 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: GRB140824A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16733
SUBJECT: GRB 140824A: Swift/UVOT Upper Limits
DATE:    14/08/24 15:25:09 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 140824A
80 s after the BAT trigger (Beardmore et al., GCN Circ. 16732).
No optical afterglow consistent with the XRT position (Beardmore et al.
GCN Circ. 16732) 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            80          229          147         >21.0
u_FC               292          542          246         >20.2
white               80         6901          688         >21.9
v                 5676         7226          309         >20.1
b                 5061         6696          393         >20.9
u                  292         6491          639         >20.6
w1                4651         6286          393         >20.0
m2                5881        11294         1082         >21.4
w2                5471         7107          393         >20.9

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


GRB_name: GRB140824A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16734
SUBJECT: GRB 140824A: MITSuME Ishigakijima upper limits
DATE:    14/08/24 15:28:57 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 and OISTER collaboration:

We observed the field of GRB 140824A (Beardmore et al., GCNC 16732)
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 2014-08-24 11:50:27 UT (~3.2 h after the burst).
We did not find any new point source within the XRT circle
(Beardmore et al., GCNC 16732) in all the three bands.

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     Ic
-----------------------------------------------------
0.14409    12:07:58    1800.0   >21.7  >21.4  >20.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140824A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16735
SUBJECT: GRB 140824A: Enhanced Swift-XRT position
DATE:    14/08/24 15:46:54 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 1996 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140824A, 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 = 206.61710, +33.29376 which is equivalent
to:

RA (J2000): 13h 46m 28.10s
Dec (J2000): +33d 17' 37.5"

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: GRB140824A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16736
SUBJECT: GRB 140824A: Swift-BAT refined analysis
DATE:    14/08/24 17:21:26 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

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

Using the data set from T-240 to T+714 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140824A (trigger #610501)
(Beardmore, et al., GCN Circ. 16732).  The BAT ground-calculated position is
RA, Dec = 206.627, 33.285 deg which is
    RA(J2000)  =  13h 46m 30.4s
    Dec(J2000) = +33d 17' 05.1"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.

The mask-weighted light curve shows a single peak with a FRED-like profile, 
starting at T+0 and lasting approximately five seconds. T90 (15-350 keV) is 3.09 
+- 0.50 sec (estimated error including systematics).

The time-averaged spectrum from T+0.26 to T+3.64 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.98 +- 0.21.  The fluence in the 15-150 keV band is 1.9 +- 0.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.34 sec in the 15-150 keV band
is 1.2 +- 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/610501/BA/


GRB_name: GRB140824A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16737
SUBJECT: GRB 140824A: Swift-XRT refined Analysis
DATE:    14/08/24 21:55:03 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), V. Mangano (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU),
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U.
Leicester) and A.P. Beardmore report on behalf of the Swift-XRT team:

We have analysed 16 ks of XRT data for GRB 140824A (Beardmore  et al.
GCN Circ. 16732),  from 85 s to 35.6 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 16735).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.90 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.87 (+0.27, -0.25). The
best-fitting absorption column is  1.0 (+0.8, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.6 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.0 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 2.2 sigma
Photon index:      1.87 (+0.27, -0.25)

If the light curve continues to decay with a power-law decay index of
0.90, the count rate at T+24 hours will be 1.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.3 x
10^-14 (6.4 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/00610501.

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


GRB_name: GRB140824A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16738
SUBJECT: GRB 140824A: OSN optical limit
DATE:    14/08/24 22:08:45 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

F. Espartero (IAA-CSIC), F.J. Aceituno (OSN/IAA-CSIC), J. Gorosabel
(IAA-CSIC/UPV-EHU) and A.J. Castro-Tirado (IAA-CSIC/UMA), report on behalf
of a larger collaboration:

We observed the field of GRB140824A (Beardmore et al. 16732) with the 1.5m
OSN telescope at Observatorio de Sierra Nevada (Spain). The observations
were carried out in the Clear band on Aug 24.84965-24.88029 (11.72-12.45
hours post bust). We do not detect any optical source brighter than R~21
consistent with the XRT position (Evans et al. 16735).


GRB_name: GRB140824A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16739
SUBJECT: GRB 140824A: NOT optical upper limits
DATE:    14/08/24 22:56:03 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), S. Covino (INAF-OAB), J. P. U. Fynbo (DARK/NBI), A.
A. Djupvik, J. Harmanen (NOT), P. Jakobsson (U. Iceland) report on
behalf of a larger collaboration:

We observed the field of GRB 140824A (Beardmore et al., GCN 16732)
using the 2.5m Nordic Optical Telescope (NOT) equipped with ALFOSC. We
obtained 3x300s SDSS r-band and 6x200s SDSS z-band images with their
median time of 12.41 hr and 12.88 hr after the burst, respectively.

No optical source is detected at the XRT position (Evans et al., GCN
16735), down to the upper limits of r~24.0 mag and z~22.4 mag.
Near-infrared follow-ups are encouraged.


GRB_name: GRB140821A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16742
SUBJECT: GRB 140821A: Fermi GBM Detection
DATE:    14/08/25 16:44:54 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 23:56:02.84  UT on the 21st of August 2014, the Fermi Gamma-Ray Burst 
Monitor triggered and located GRB 140821A (trigger 430358165 / 140821997). 
The trigger resulted in an Autonomous Repoint Request (ARR) that was 
accepted. The GBM on-ground location is consistent with the Fermi flight 
software position.

The angle from the Fermi LAT boresight is 93 degrees.

The GBM light curve consists of single peak with a duration (T90) of about
32 s (50-300 keV). The time-averaged spectrum from T0+11 s to T0+43 s is
well fit by Band function parameterized as Ep=483+/-22 keV, 
alpha=-0.82+/-0.03 and beta=-2.4+/-0.1. 

The event fluence (10-1000 keV) in this time interval is
(6.314+/-0.067)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+29 s in the 10-1000 keV band is  19.5+/-0.6 ph/s/cm^2.

The burst spectrum may be contaminated by solar flare activity that is 
detected at energies below ~20 keV in many of the same GBM detectors. 
Although the solar emission has several peaks, the first of which is  
around T0+130 s, it may have significant overlap with the time of the
burst.

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


GRB_name: GRB140824B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16743
SUBJECT: GRB 140824B: Fermi GBM Detection
DATE:    14/08/25 16:46:21 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 14:33:12.04  UT on the 24th of August 2014, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 140824B (trigger 430583595 / 140824606), 
which has been followed up by MASTER II robotic telescope (Tyurina et al. 
GCNs 16740, 16741). The GBM on-ground location is consistent with the Fermi 
flight software position.

The angle from the Fermi LAT boresight is 79 degrees.

The GBM light curve consists of three main peaks with a total duration (T90) 
of about 109 s (50-300 keV). The time-averaged spectrum from T0+3 s to T0+112 s 
is well fit by Band function parameterized as Ep=186+/-20 keV, alpha=-0.9+/-0.1
and beta=-2.5+/-0.5.


The event fluence (10-1000 keV) in this time interval is
(1.5+/-0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+111 s in the 10-1000 keV band is  6.9+/-0.3 ph/s/cm^2.


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


GRB_name: GRB140824B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16746
SUBJECT: GRB 140824B: Swift observations
DATE:    14/08/26 14:33:02 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester), N. P. M. Kuin (UCL-MSSL) and J. R. Cummings 
(GSFC/UMBC) report on behalf of the Swift team:

We report on Swift follow-up observations of the Fermi/GBM GRB 140824B 
(Zhang, GCN Circ. 16743) centred at the position of the candidate 
optical counterpart reported by the MASTER II robotic telescope (Tyurina 
et al., GCNs 16740, 16741).

In 4.9 ks of XRT Photon Counting (PC) mode data, from 90.6 ks to 103.4 
ks after the Fermi/GBM trigger, no X-ray source is detected at the 
MASTER II position. The 3-sigma upper limit on the count rate is 1.8E-03 
cts/s, which is 9.2E-14 erg cm^-2 s^-1 using a typical flux conversion 
of 5E-11 erg cm^-2 count^-1.

The UVOT detected the reported candidate OT. The preliminary UVOT 
position is:
     RA  (J2000) =  01:11:01.14 =  17.75473 (deg.)
     Dec (J2000) = +60:33:38.6  =  60.56071 (deg.)
with an estimated uncertainty of 0.43 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            91250        91850          590         17.97  0.05
  white            96997        97610          603         17.94  0.05
  white          102774      103372          590         18.09  0.05
  v                   91857        92457          590         17.47  0.07
  v                   97617        98230          603         17.61  0.07
  u                   90644        91244          590         17.65  0.06
  u                   96991        96991          603         17.62  0.06
  u                 102158      102768          600         17.91  0.07

The magnitudes in the table are not corrected for the large, but 
uncertain Galactic extinction due to the reddening of E(B-V) = 0.79 in 
the direction of the burst (Schlegel et al. 1998). The UVOT magnitudes 
when compared to the reported unfiltered  magnitudes of 17.0 and 17.5 by 
MASTER, suggest a slowly varying source.

Based on the Swift observations, the optical transient detected by 
MASTER II is therefore unlikely to be the GRB afterglow.


GRB_name: GRB140824A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16747
SUBJECT: GRB 140824A: optical upper limit in CrAO
DATE:    14/08/26 18:11:29 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 140824A (Beardmore  et al., GCN 
16732) with ZTSh telescope of CrAO observatory starting on Aug. 24 (UT) 
17:48:55 (9.1 hours after burst trigger). We took several images in 
R-filter of 120 s exposure. Within  enhanced XRT position (Evans et al., 
GCN  16735) we do  not detect any source. Photometry of a combined image 
is following

Date        UT start,  t-t0     Filter   Exp.   OT      UL (3 sigma)
                       (mid, days)        (s)

2014-08-24 17:48:55    0.4105   R        39x120 n/d     23.5

The photometry is based on USNO-B1.0  star
1233-0239576 (13:46:31.55 +33:18:14.7) assuming R=19.66


GRB_name: GRB140818B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16748
SUBJECT: GRB 140818B: TLS observations
DATE:    14/08/27 09:23:17 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

S. Schmidl, S. Klose, D. A. Kann, U. Laux, L. Pfeifer, C. Pohl, and H.
Meusinger (all TLS Tautenburg) report:

We observed the field of GRB 140818B (Swift trigger 609885, Vargas et al.,
GCN 16709) with the 1.34m Tautenburg Schmidt telescope.

Starting at 20:34 UT (1.83 hr after the trigger), we obtained in total 12
x 120s Rc-band images. Observations were obtained at a mean airmass of 1.75.

In a stack of all available images, we detect the source reported by
Aceituno et al. (GCN 16711). Using USNO-B1 field stars for calibration, we
derive a preliminary magnitude (Vega magnitude system) of

Rc = 20.9 +/- 0.2,

at a midtime of 2.08 hr after the burst.

The given magnitude is not corrected for the large Galactic foreground
extinction corresponding to a reddening of E_(B-V) = 0.73 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140824B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16750
SUBJECT: IPN Triangulation of GRB 140824B
DATE:    14/08/27 16:09:57 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, V. Pelassa, and A. Goldstein,
on behalf of the Fermi GBM 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:

The long-duration GRB 140824B (Zhang, GCN 16743) has
been observed by Konus-Wind, Fermi(GBM trigger 430583595), and INTEGRAL 
(SPI-ACS), so far, at about 52392 s UT (14:33:12).

We have triangulated it to a Konus-GBM annulus centered at
RA(2000)=355.371 deg (23h 41m 29s)  Dec(2000)=-1.147 deg (-1d 08' 51"),
whose radius is 61.534  1.149 deg (3 sigma).

The OT reported by MASTER (Tyurina et al., GCNs 16740, 16741) is well 
outside of the annulus (at 3.6 deg from the annulus center line). 
Therefore, we conclude that this OT is not related to the burst (as was 
already suggested by Tyurina et al. (GCN 16741) and Pagani et al. (GCN 
16746) basing on the optical observations).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140824_T52472/IPN/


GRB_name: GRB140828A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16751
SUBJECT: GRB 140828A: Swift detection of a burst
DATE:    14/08/28 07:11:06 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), P. A. Evans (U Leicester),
A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester), T. Sakamoto (AGU)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 06:54:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140828A (trigger=610953). 
The BAT on-board calculated location is 
RA, Dec 142.011, +14.590 which is 
   RA(J2000) = 09h 28m 03s
   Dec(J2000) = +14d 35' 24"
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 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 22:33 UT on 2014 September 29. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB140825A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16752
SUBJECT: IPN Triangulation of GRB 140825A (very intense/long)
DATE:    14/08/28 18:06:34 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

S. Golenetskii, R. Aptekar, 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,

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

D. M. Smith, on behalf of the RHESSI GRB team, report:

The long-duration, very intense GRB 140825A has been observed by 
Konus-Wind, MESSENGER (GRNS), Mars Odyssey (HEND), Swift (BAT), RHESSI, 
and INTEGRAL (SPI-ACS), so far, at about 24925 s UT (06:55:25). 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:
     88.715 (05h 54m 51s) -11.830 (-11d 49' 48")
   Corners:
     88.611 (05h 54m 27s) -11.630 (-11d 37' 48")
     88.657 (05h 54m 38s) -11.950 (-11d 57' 01")
     88.818 (05h 55m 16s) -12.029 (-12d 01' 46")
     88.772 (05h 55m 05s) -11.710 (-11d 42' 36")
   ---------------------------------------------
The error box area is 169 sq. arcmin, and its maximum
dimension is 27 arcmin (the minimum one is 9 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140825_T24925/IPN/

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


GRB_name: GRB140828A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16754
SUBJECT: GRB 140828A: Fermi GBM observation
DATE:    14/08/29 07:52:08 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 06:54:12.18 UT on 28 August 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140828A (trigger 430901655 / 140828288), which
was also detected by the Swift/BAT (Melandri et al. 2014, GCN 16751)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 57 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0-6.1 s to T0+16.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.5 +/- 0.1  and
the cutoff energy, parameterized as Epeak, is 140 +/- 30 keV.

The event fluence (10-1000 keV) in this time interval is
(3.5 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+2.43 s in the 10-1000 keV band
is 3.5 +/- 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: GRB140825A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16755
SUBJECT: Konus-Wind observation of GRB 140825A
DATE:    14/08/29 17:23:14 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration, intense GRB 140825A
(IPN triangulation: Hurley et al., GCN 16752)
triggered Konus-Wind at T0=24925.66 s UT (06:55:25.660).

The burst light curve shows several peaks with a total duration of ~14 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.7(-0.2,+0.2)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+1.984 s,
of 1.4(-0.2,+0.2)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+10.752 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.94(-0.07,+0.08),
the high-energy photon index beta = -3.42(-1.36,+0.40),
the peak energy Ep = 142(-7,+7) keV,
chi2 = 86/84 dof.

The spectrum near the peak count rate
(measured from T0+2.048 to T0+2.560 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.44(-0.15,+0.21),
the high-energy photon index beta = -3.42(-1.61,+0.59),
the peak energy Ep = 208(-23,+18) keV,
chi2 = 41/44 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140825_T24925/

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


GRB_name: GRB140828A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16756
SUBJECT: GRB 140828A, Swift-BAT refined analysis
DATE:    14/08/29 22:54:54 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

C. B. Markwardt (GSFC), 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 (GSFC/UMBC), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(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 140828A (trigger #610953)
(Melandri, et al., GCN Circ. 16751).  The BAT ground-calculated position is
RA, Dec = 142.029, 14.569 deg which is 
  RA(J2000)  =  09h 28m 07.0s 
  Dec(J2000) = +14d 34' 09.2" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.

The mask-weighted light curve shows a single peak starting at T-7 sec, peaking 
at T+1 sec and ending at T+10 sec.  There is a hint of an emission peaking 
at T+14 sec.  T90 (15-350 keV) is 18.8 +- 4.0 sec (estimated error including 
systematics).

The time-averaged spectrum from T-5.8 to T+18.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.6 +- 0.7, 
and Epeak of 54 +- 11 keV (chi squared 70.26 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.51 sec in the 15-150 keV band is
2.2 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.78 +- 0.13 (chi squared 81.57 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/610953/BA/


GRB_name: GRB140818B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16757
SUBJECT: GRB140818B, the review of the sky area in plate archives
DATE:    14/08/30 19:39:14 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V. Golovnya (Main Astro Obs, Kyiv) 
report: 
We have undertaken the review of the sky area in vicinity of 
GRB140818B (Vargas et al., GCN 16709; Beardmore et al., 
GCN 16712) on astronegatives, collected in Ukrainian NAS 
Main astronomical observatory plate archive (1976-1996). 
All the plates with the possible object appearance are 
digitized using Microtek ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed scanners and have been 
placed into Golosiiv Plate Archive database DBGPA with open 
access to them. The list of plates is given in the table: 
yyyymmdd/TimeUT --Plates--              Exp. LM  USNOA2 0825 
19910613/222704 GUA040C001802A 22.5 15.9   -11812892 
19910709/205250 GUA040C001826A 23.5 15.7   -11814106 
19820715/175441 TAS040A000284    23.0 17.3   -11812584 
  No any object has been found in the point with the mentioned 
coordinates of GRB. But the image of some object have found near GRB position on the two of selected plates. 
Brighness of the object is estimated as V=15.0 and V=16.5: 
  Plates                   RA,(J2000),Dec          V 
GUA040C001802A 18:04:32.08 -01:22:57.0 15.0 
TAS040A000284    18:04:32.63 -01:22:55.6 16.5 
Plates:  
GUA040Câ€“the plates archive identifier of DWA (D/F=400/2000, 
         M=103"/mm) of the Ukrainian NAS Main Astro obs. 
         (Marsden's number - 83) the plate number [1]. 
TAS040A -the plates archive identifier of DAZ (D/F=400/3000, 
         M=68.8"/mm) of the Tashkent Astro obs. 
         (Marsden's number - 186) the plate number [1]. 
Exp.   - Duration of the maximum exposure (minutes). 
LM - Limited V mag, derived in the 2,5 arcmin area around 
       the location given in GCN Circ.16712: 
       RA(J2000): 18h 04m 32.53s, Dec(J2000): -01d 23' 10.6" 
USNOA2 - Comparison star. 
  The preview images of 3 areas together with  
the 2,5x2,5 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/140818B/index.html 
The images with full resolution are available via e-mail on 
demand. 
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0), http://gua.db.ukr-vo.org 


GRB_name: GRB140829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16758
SUBJECT: GRB 140829A: iPTF optical observations
DATE:    14/08/31 00:50:32 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), D. A. Perley (Caltech),
and M. M. Kasliwal (Carnegie Observatories/Princeton), report on behalf of
the intermediate Palomar Transient Factory (iPTF) collaboration:

Fermi GBM triggered on GRB 140829A (Fermi trigger 431039250 / bn140829880)
at 2014-08-29 21:07:27.47. At 2014-08-30 03:25:48, 6.3 hours after the
burst, we began searching for optical counterparts using the Palomar
48-inch Oschin telescope (P48). We imaged 17 fields covering an area of
124 deg2, covering most of the 1-sigma statistical+systematic region of the
final Fermi GBM localization. We estimate a 61% chance that these fields
contain the true location of the source.

Sifting through candidate variable sources using image subtraction and
standard iPTF vetting procedures, we detected several faint optical
transients.

iPTF14ejs, at r=20.15+/-0.06 mag and possibly fading by 0.2+/-0.09 mag by
8.6 hours after the burst, is coincident with the galaxy SDSS
J164214.15+500743.1. It is at the coordinates:
  RA(J2000)  =  16h 42m 14.14s (250.558918 deg)
  Dec(J2000) = +50d 07' 43.3"  (+50.128685 deg)

We acquired a spectrum of iPTF14ejs using the Low Resolution Imaging
Spectrometer (LRIS) on the Keck 10m telescope. A provisional reduction
shows broad Balmer features characteristic of an AGN at a redshift of
z=0.483, and therefore it is not a GRB afterglow.

The remaining candidates do not show any clear photometric evolution over
the course of our observations:

iPTF14ejo, at r=20.32+/-0.07 mag, is coincident with the galaxy
SDSS J173008.24+545502.8. It is at the coordinates:
  RA(J2000)  =  17h 30m 08.26s (262.534415 deg)
  Dec(J2000) = +54d 55' 04.2"  (+54.917842 deg)

iPTF14eju, at r=20.66+/-0.12 mag, is 4.8" to the southwest of an r=18.43
unresolved point source that is present in archival iPTF images. It is at
the coordinates:
  RA(J2000)  =  17h 13m 25.08s (258.354509 deg)
  Dec(J2000) = +50d 10' 04.7"  (+50.167985 deg)

iPTF14ejp, at r=20.37+/-0.09 mag, is coincident with PGC 2393059. It is at
the coordinates:
  RA(J2000)  =  16h 56m 59.87s (254.249449 deg)
  Dec(J2000) = +51d 22' 21.7"  (+51.372682 deg)

iPTF14ejw, at r=20.27+/-0.10 mag, is coincident with the galaxy
SDSS J164524.99+625127.7 . It is at the coordinates:
  RA(J2000)  =  16h 45m 24.20s (251.350842 deg)
  Dec(J2000) = +62d 51' 27.7"  (+62.857694 deg)

iPTF14ejn, at r=20.31+/-0.07 mag, is coincident with the galaxy
SDSS J172732.49+540754.0. It is at the coordinates:
  RA(J2000)  =  17h 27m 32.49s (261.885373 deg)
  Dec(J2000) = +54d 07' 54.2"  (+54.131732 deg)

iPTF14ejv, at r=20.82+/-0.20 mag, is coincident with the galaxy
SDSS J174853.28+580652.3. It is at the coordinates:
  RA(J2000)  =  17h 48m 53.26s (267.221896 deg)
  Dec(J2000) = +58d 06' 52.8"  (+58.114678 deg)

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi431039250.pdf
shows the locations of our candidates and the P48 fields in relation to
the Fermi GBM 1- and 2-sigma statistical+systematic contours.


GRB_name: GRB140829A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16759
SUBJECT: GRB 140829A: Fermi GBM Detection
DATE:    14/08/31 20:50:38 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

M. Stanbro (UAH) reports on behalf of the Fermi GBM Team:

"At 21:07:27.47 UT on 29 August 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140829A (trigger 431039250 / 140829880).
The GBM error circle was also observed with iPTF in search of an optical
counterpart of the GRB; no credible counterpart was found (Singer et. al.,
2014, GCN 16758).

The GBM light curve consists of a double pulse with a duration (T90)
of about 19 s (50-300 keV). The time-averaged spectrum from T0-3.1 s
to T0+18.4 s is well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.5 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 324 +/- 43 keV.

The event fluence (10-1000 keV) in this time interval is
(5.12 +/- 0.41)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+11.52 s in the 10-1000 keV band
is 2.9 +/- 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: GRB140831A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16760
SUBJECT: GRB 140831A: iPTF observations of a possible short burst detected by Fermi GBM
DATE:    14/09/01 02:05:16 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
D. A. Perley (Caltech), S. B. Cenko (NASA/GSFC), and Paolo DAvanzo
(INAF-OAB) report on behalf of a larger collaboration:

Fermi GBM triggered on the possibly short GRB 140831A (Fermi trigger
431168350 / bn140831374) at 2014-08-31 08:59:07.220. At 09:16:58, 18
minutes after the burst, we began searching for optical counterparts using
the Palomar 48-inch Oschin telescope (P48). We imaged 10 fields covering
an area of 74 deg^2.

The final GBM localization, which was available 4.1 hours after the
trigger, shifted by 12 deg relative to the prompt on-ground localization.
As a result, the P48 fields lie mostly between the 1- and 2-sigma
statistical+systematic contours of the final Fermi GBM localization. We
estimate a 6% prior probability that these fields contain the true
location of the source.

Because this burst coincidentally occurred within the routine iPTF survey
footprint, we have Sloan g observations preceding the burst. The target
of opportunity observations were undertaken in the Mould R filter.

Sifting through candidate variable sources using image subtraction and
standard iPTF vetting procedures, we found three rapidly evolving
candidates and followed up two with Low Resolution Imaging Spectrometer
(LRIS) on the Keck I telescope (PI: Perley). None of the candidates appear
to be related to the trigger.

The first candidate, iPTF14emq, is at the coordinates:
  RA(J2000)  =   0h 00m 59.16s (  0.246512 deg)
  Dec(J2000) = +32d 48' 45.7"  (+32.812683 deg)
Relative to the time of the burst, we measure:
  -1.31 hours:  g > 21.08
  -0.83 hours:  g > 20.21
  +0.37 hours:  R = 21.04 +/- 0.12
  +0.61 hours:  R = 20.88 +/- 0.11
The Keck spectrum was that of a spiral galaxy at z=0.17 (i.e., host light
only). Subsequent Keck/LRIS gR imaging and Gemini/GMOS griz imaging showed
no source to deep limits, R >~ 26. This suggests the source faded too
quickly and even faster than could be expected from an afterglow. We
submitted a Swift TOO. In 4.8 ks of exposure starting 17.5 ks after the
burst, no X-ray emission was detected to a 3-sigma limit of 2.1e-3
counts/s. There is some excess in the UVOT image, probably due to the
nearby galaxy and background from the bright stars in the field. Since
none of our observations were able to confirm the source and given the
proximity to bright stars, we suspect that iPTF14emq is a ghost-like
optical artifact in the P48 images, unrelated to the GRB.

The second candidate, iPTF14ems, is at the coordinates:
  RA(J2000)  =  23h 26m 56.36s (351.734833 deg)
  Dec(J2000) = +35d 35' 21.7"  (+35.589374 deg)
Relative to the time of the burst, the P48 photometry is:
  -21.5 hours:  g > 20.09
  +0.13 hours:  R = 17.26 +/- 0.01
  +3.23 hours:  R = 20.28 +/- 0.08
The Keck spectrum exhibits broad Balmer emission lines at z=0, showing
iPTF14ems to be a stellar flare.

The third candidate, iPTF14emo, is at the coordinates:
  RA(J2000)  =  23h 28m 40.90s (352.170424 deg)
  Dec(J2000) = +31d 14' 06.5"  (+31.235126 deg)
The P48 photometry is:
  -1.31 hours:  g = 21.02 +/- 0.13
  -0.83 hours:  g = 21.35 +/- 0.19
  +0.37 hours:  R > 20.91
We infer that this source is unrelated to the GRB because the g-band
detection preceded the GBM trigger.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi431168350.pdf
shows the locations of our optical transients and the P48 fields in
relation to the Fermi GBM 1- and 2-sigma statistical+systematic contours.


GRB_name: GRB140901A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16761
SUBJECT: IPN Triangulation of GRB 140901A (short/hard/very intense)
DATE:    14/09/02 11:36:07 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley, and V. Pal'shin on behalf of the IPN team,

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

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

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team, report:

A short-duration, hard spectrum, very intense GRB 140901A has been 
observed by Fermi(GBM trigger 431293300), Mars Odyssey (HEND), and 
INTEGRAL (SPI-ACS), so far, at about 70897 s UT (19:41:37).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    15.816 (01h 03m 16s) -32.755 (-32d 45' 19")
  Corners:
    15.165 (01h 00m 40s) -32.225 (-32d 13' 30")
    14.965 (00h 59m 52s) -32.345 (-32d 20' 44")
    16.481 (01h 05m 55s) -33.279 (-33d 16' 43")
    16.682 (01h 06m 44s) -33.156 (-33d 09' 20")
  ---------------------------------------------
The error box area is 1125 sq. arcmin, and its maximum
dimension is 1.66 deg (the minimum one is 12 arcmin).
The Sun distance was 139 deg.

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140901_T70897/IPN/

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


GRB_name: GRB140901A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16762
SUBJECT: GRB 140901A: Fermi GBM detection
DATE:    14/09/02 19:03:37 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH) reports on behalf of the Fermi GBM Team:

"At 19:41:37.57 UT on September 1 2014, the Fermi Gamma-Ray Burst 
Monitor triggered and located 
GRB 140901A (trigger 431293300/140901821). The GBM on-ground 
location, using the Fermi GBM trigger data, is consistent with
the IPN Triangulation (K. Hurley et al. 2014, GCN 16761).

The angle of the burst direction to the Fermi LAT boresight is 
97 degrees.

The GBM light curve consists of a single peak with a duration
(T90) of about 0.16 s (50-300 keV).
The time-averaged spectrum from T0+0.0 s to T0+0.19 s is
adequately fit by a Band function with Epeak = 1250 +/- 70 keV,
Alpha =-0.30 +/- 0.04 and Beta = -3.0 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(4.8 +/- 0.1)E-06 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band
is 50 +/- 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: GRB140903A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16763
SUBJECT: GRB 140903A: Swift detection of a possible burst
DATE:    14/09/03 15:56:04 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. R. Cummings (NASA/UMBC), D. N. Burrows (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 15:00:30 UT, BAT triggered on a possible GRB at
RA, dec = 238.036, +27.578 (J2000). 

However, due to a TDRSS telemetry gap, no further 
data is available at this time. 

No XRT source was detected in 90 s of downlinked data taken approximately 1.5ks
after the trigger time. We are waiting for the full dataset to detect and localise 
the XRT counterpart. 

No UVOT data is available at this time. 

The full data set will be available following the next ground pass. 

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


GRB_name: GRB140903A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16764
SUBJECT: GRB 140903A: Preliminary Swift/XRT localization
DATE:    14/09/03 17:26:47 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU) and J. R. Cummings (NASA/UMBC) report on behalf of the 
Swift/XRT Team:

Swift/XRT began observing the position of GRB 140903A at 15:01:29UT, 
approximately 59 seconds after the BAT trigger (GCN #16763). In 
preliminary data we find an uncatalogued fading source at the following 
location: RA/Dec(J2000) = 238.01597, 27.603287, which is equivalent to:

RA(J2000) = 15h 52m 3.83s,
Dec(J2000) = 27d 36m 11.8s,

with an estimated uncertainty of 10 arc-seconds radius (90% confidence). 
The light-curve appears to show rapid fading, consistent with this X-ray 
source being a GRB afterglow. We will publish an improved position for 
this burst when more data become available.


GRB_name: GRB140903A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16765
SUBJECT: GRB 140903A: Confirmed Swift detection of a short burst
DATE:    14/09/03 17:32:26 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (NASA/UMBC) reports on behalf of the Swift Team:

At 15:00:30 UT, BAT triggered on GRB 140903A.  The onboard BAT localization
was at RA, dec = 238.036, +27.578, which is

RA (J2000)   15h 52m 08.6s    
Dec (J2000)  +27d 34' 41"

with an estimated 90% uncertainty radius of 3 arcmin.

The BAT lightcurve shows a single peak about 0.45 seconds long.


GRB_name: GRB140903A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16766
SUBJECT: GRB 140903A: Coincident galaxy cluster in archival images
DATE:    14/09/03 18:53:21 GMT
FROM:    Derek Fox at PSU  <dfox@astro.psu.edu>

Derek B. Fox (PSU) and J. R. Cummings (NASA/UMBC) report:

"The BAT (Cummings, GCN 16765) and XRT (Kennea & Cummings, GCN 16764)
localizations of GRB 140903A (Cummings et al., GCN 16763) are located
within 2.5' (<0.2 Mpc projected) of the center of the galaxy cluster
NSC J155202+273349, as cataloged by the Northern Optical Cluster
Survey (Gal et al. 2003, AJ, 125, 2064). While the photometric
redshift for the cluster is provided as z=0.2955 in the catalog, four
of the five SDSS-resolved galaxies nearest the XRT position have
spectroscopic redshifts (SDSS and 2MASX surveys, as retrieved from the
NASA Extragalactic Database) within the range z=0.074 +/- 0.001. In
particular, the two nearest galaxies with known redshifts are SDSS
J155208.34+273631.8 at z=0.073 (1.05' distance) and 2MASX
J15520787+2735016 at z=0.075 (1.47' distance).

Given past associations (and proposed associations) of short bursts
with evolved galaxies and galaxy clusters at z<~0.3 we consider the
presence of this coincident galaxy cluster at z~0.074 suggestive."

This research has made use of the NASA/IPAC Extragalactic Database
(NED) which is operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.


GRB_name: GRB140903A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16767
SUBJECT: GRB 140903A: Swift-XRT refined Analysis
DATE:    14/09/03 20:57:43 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <ucasmd0@ucl.ac.uk>

M. De Pasquale, A. Maselli (IASF-Palermo), J. R. Cummings (NASA/UMBC)
reports on behalf of the Swift-XRT team:

We have analysed 2.9 ks of XRT data for GRB 140903A (Cummings  et al.
GCN Circ. 16763),  from 74 s to 7.3 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. Using 3407 s of PC mode data
and 7 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 = 238.01361, +27.60259 which is equivalent to:

RA (J2000): 15h 52m 03.27s
Dec(J2000): +27d 36' 09.3"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.21 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.71 (+0.21, -0.20). The
best-fitting absorption column is  1.2 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.3 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:         1.2 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 3.3 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:         1.71 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
0.21, the count rate at T+24 hours will be 0.11 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x
10^-12 (5.3 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/00611599.

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


GRB_name: GRB140903A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16768
SUBJECT: GRB 140903A: Swift-BAT refined analysis
DATE:    14/09/04 01:33:48 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings, N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
  
Using the data set from T-61 to T+159 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140903A (trigger #611599)
(Cummings, et al., GCN Circ. 16763).  The BAT ground-calculated position is
RA, Dec = 238.021, 27.608 deg which is
    RA(J2000)  =  15h 52m 05.0s
    Dec(J2000) = +27d 36' 27.6"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
  
The mask-weighted light curve shows a single FRED peak.  T90 (15-350 keV) is
0.30 +- 0.03 sec (estimated error including systematics).
  
The time-averaged spectrum from T-0.01 to T+0.35 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.99 +- 0.12.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.33 sec in the 15-150 keV band
is 2.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

This burst was short but we note that it was not particularly hard.
  
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/611599/BA/


GRB_name: GRB140903A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16769
SUBJECT: GRB140903A: Discovery Channel Telescope Optical Detection
DATE:    14/09/04 05:28:27 GMT
FROM:    John Capone at UMD  <jicapone@astro.umd.edu>

J. Capone (UMD), V. Toy (UMD), S.B. Cenko (NASA-GSFC), A. Cucchiara
(NASA-GSFC), E. Troja (NASA-GSFC), A. Kutyrev (NASA-GSFC), S. Veilleux
(UMD), and S. Gezari (UMD) report on behalf of a larger collaboration:

We observed the field of GRB140903A (Cummings et al., GCN 16763) with the
Large Monolithic Imager (LMI) on the 4.3m Discovery Channel Telescope (DCT)
at Happy Jack, AZ. We observed in r' for a total of 600 seconds beginning
at 2014-09-04 03:10 UTC (approximately 12 hours after the Swift trigger).

A source is clearly detected at the location of the x-ray afterglow (De
Pasquale et al, GCN 16767). Using nearby point sources from SDSS for
calibration, we measure a preliminary magnitude of r' = 20.2 +/- 0.3. This
value is not corrected for Galactic extinction in the direction of the GRB.
 We also note the presence of a 9th magnitude star ~10 arcseconds from the
afterglow candidate.

We thank the staff of the Discovery Channel Telescope for assistance with
these observations.


GRB_name: GRB140903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16770
SUBJECT: GRB 140903A: P60 Optical Observations
DATE:    14/09/04 06:09:46 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

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

We observed the field of the Swift short GRB 140903A (Cummings et al., GCN 16763) with the robotic Palomar 60 inch telescope.  Observations were obtained in the g', r', and i' filters beginning at 3:13 UT on 4 September 2014 (12.2 hr after the Swift trigger time).

We detect a faint source at the northern edge of the revised XRT error circle (De Pasquale et al., GCN 16767), with (J2000) coordinates

  RA: 15:52:03.28  Dec: +27:36:10.7

and an estimated uncertainty of ~ 0.5" in each coordinate. Visual comparison reveals that this is the same source identified by Capone et al. in the Discovery Channel Telescope imaging reported in GCN 16769.

Using nearby point sources from SDSS for calibration, we estimate a magnitude of r' = 20.0 for the source at this time.  We caution, however, that the photometry is strongly affected by the presence of the nearby bright star.  We estimate an uncertainty of ~ 0.5 mag, but accurate photometry will need to await a more thorough analysis.

Since our observations overlap with those reported by Capone et al., we cannot confirm any variability in this object.  Inspection of the archival SDSS images does not reveal an obvious source at this location, but the images are strongly affected by the nearby bright star, and thus the depth may be insufficient for a meaningful comparison.  We encourage additional follow-up to determine if this is indeed the optical afterglow of GRB 140903A.


GRB_name: GRB140903A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16771
SUBJECT: GRB 140903A: Swift-BAT Spectral lag analysis
DATE:    14/09/04 06:32:31 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

We report the spectral lag analysis for GRB 140903A (GCN Circ. 16764 & 16765) 
based on the BAT data.  Using 4-ms binned light curve, the spectral lag for 
the 50-100 keV to 100-350 keV bands is 16 +- 7 ms, and 21 +- 7 ms for the 15-25 keV 
to 50-100 keV bands.  There is no evidence for extended emission.  Those lag values 
are consistent with the short end of the long-burst lag distribution.  Although the 
lag analysis suggests GRB 140903A is consistent with a long GRB population, a further 
observation is needed to understand the nature of this burst.  


GRB_name: GRB140903A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16772
SUBJECT: GRB 140903A: Swift/UVOT Upper Limits
DATE:    14/09/04 10:35:34 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and J. R. Cummings (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140903A 76 
s after the BAT trigger (Cummings et al., GCN Circ. 16763).
No optical afterglow consistent with the XRT position (De Pasquale et 
al. GCN Circ. 16767) or optical position given by Cenko et al. (GCN 
Circ. 16770), is detected in the initial UVOT exposures. The analysis is 
complicated by the wings of the bright star mentioned by Capone et al. 
(GCN Circ. 16767), and thus the upper limits should be treated with caution.
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            77          227          147         >20.01
u_FC               289          539          246         >17.4
white               77        17449          944         >21.0
v                  618        29425         1322         >18.9
b                  544        17228         1376         >20.0
u                  289        23404         1138         >18.2
w1                1097        22967         1121         >18.4
m2                 643         6613          255         >18.8
w2                5562        28728         1918         >18.6

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: GRB140901B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16773
SUBJECT: GRB 140901B found in ground analysis of BAT data
DATE:    14/09/04 13:59:36 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift science team:

At 06:17:24 Swift-BAT rate-triggered on GRB 140901B (trigger # 611389).
Fermi-GBM also triggered on this event (trigger 431245045).  No source
was found onboard.  In ground analysis, a significant source was found
at RA, Dec 112.184, -29.209, which is
    RA (J2000)   07h 28m 44.2s
    Dec (J2000) -29d 12' 31"
with an estimated 90% uncertainty radius of 2.0 arcmin.  This location
is 3.0 degrees from the reported GBM location
(http://gcn.gsfc.nasa.gov/other/431245045.fermi), within the GBM error
circle.

The background in BAT was high, since Swift was near the SAA.  The BAT
lightcurve shows a single FRED peak, with T90 about 10 +- 1 sec.

The BAT spectrum with 10.0 seconds of data is best fit by a simple power-
law function with a photon index of 1.20 +- 0.22.  Using this model, the
fluence was (9.5 +- 1.3) x 10^-7 ergs/cm^2.  Errors are 90% confidence.

A Swift TOO request has been submitted, but this burst is already 3.5
days old, and moreover is rather close to the Sun.


GRB_name: GRB140903A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16774
SUBJECT: GRB 140903A: tentative spectroscopic redshift
DATE:    14/09/04 14:30:39 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (NASA-GSFC), S.B. Cenko (NASA-GSFC), 
D. A. Perley (Caltech), J. Capone (UMD), and V. Toy (UMD) 
report on behalf of a larger collaboration:

On September 4.20 UT we observe the candidate afterglow of the short GRB 
140903A (Cummings et al. GCN 16763, Kennea et al. GCN 16764, Capone et al. 
GCN 16769) with the Gemini-North telescope equipped with the GMOS camera. 
A set of 2x600s exposures were obtained in spectroscopic mode: our spectra 
covered the wavelength range 4000-8100 Angstroms at a resolution of R~1200. 

We clearly identify a strong absorption doublet feature at the observed wavelength 
7954, 7965 Angstrom and a weak emission line at 6570 Angstrom.
We tentatively interpret these features as NaID in absorption and H-beta line 
in emission at the common redshift of z=0.351.
No other clear features are visible neither in emission nor in absorption, 
therefore we suggest this to be the redshift of the host galaxy of GRB 140903A.


We thank the Gemini staff, in particular Jess Ball, for their prompt
assistance with these observations.


GRB_name: GRB140901B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16775
SUBJECT: GRB 140901B: Fermi GBM detection
DATE:    14/09/04 17:30:20 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 06:17:22.79 UT on 01 September 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140901B (trigger 431245045 / 140901262), which
was also detected by the Swift/BAT (Cummings 2014, GCN 16773)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 34 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 65 +/- 14 s (50-300 keV).
The time-averaged spectrum from T0-0 s to T0+65 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.2 +/- 0.2  and
the cutoff energy, parameterized as Epeak, is 219 +/- 82 keV.

The event fluence (10-1000 keV) in this time interval is
(3.8 +/- 0.6)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.9 s in the 10-1000 keV band
is 2.6 +/- 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: GRB140903A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16776
SUBJECT: GRB 140903A:  Pan STARRS images of the field
DATE:    14/09/04 22:23:37 GMT
FROM:    Andrew S. Fruchter at STScI  <fruchter@stsci.edu>

A.S. Fruchter reports:

The field of GRB 140903A was observed on numerous occasions in multiple filters by the Pan STARRS survey.   An object is visible at the location reported by Cenko et al. (GCN 16770) in the r, i, z and y filter stacks.   The proximity of the object to a bright star makes accurate photometry extremely difficult.   However, in the i and z bands, where the object is most clearly visible against the scattered light from the nearby star, I estimate magnitudes of 20.0 +/- 0.2 in both filters.     This agrees well with that reported by Cenko et al in the r band., suggesting that this source is stable.


GRB_name: GRB140903A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16777
SUBJECT: GRB 140903A: 6 GHz VLA detection
DATE:    14/09/04 22:47:57 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong (U. Arizona) reports:

"We observed the position of the short-duration GRB 140903A (Cummings et
al., GCN 16763; GCN 16765) with the Karl G. Jansky Very Large Array (VLA)
beginning on 2014 Sept 4.040 UT (9.70 hr post-burst) at a mean frequency of
6 GHz. In 1 hour of observations, we detect a ~0.11 mJy radio source at the
position:

RA(J2000) = 15:52:03.21
Dec(J2000) = +27:36:10.7

with an uncertainty of 0.3" in each coordinate. This position is coincident
with the reported optical source (Capone et al., GCN 16769; Cenko et al.,
GCN 16770; Cucchiara et al., 16774; Fruchter, GCN 16776).

Further observations are planned. We thank the VLA staff for quickly
executing these observations."


GRB_name: GRB140903A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16778
SUBJECT: GRB 140903A: MAXI/GSC upper limit
DATE:    14/09/05 03:31:00 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

M. Serino (RIKEN), T. Sakamoto (AGU), N. Kawai (Tokyo Tech), 
S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida,  Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, D. Uchida (Osaka U.),
H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, A. Kawagoe (Chuo U.),
M. Yamauchi, Y. Morooka, D. Itoh (Miyazaki U.),
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC scanned the field of GRB 140903A 
triggered by Swift BAT (Cumming et al. GCN Circ. 16763) 
at 15:00:42 (12 sec after the trigger) UT on 2014-09-03.  
The durations of the scan was 44 sec.  
No obvious source was detected by MAXI/GSC at the location of BAT.  
The 3 sigma upper limit of the scan derived by the MAXI/GSC data is 
8.4 x 10^-10 erg/cm2/s (4-10 keV).  
This upper limit is roughly consistent with the power-law 
interpolation of the BAT prompt emission flux (T ~ 0-0.3 s) and 
the first XRT point (t ~ 100 s), assuming that the BAT spectrum 
(power-law with photon index 1.99, Palmer et al. GCN Circ. 16768) 
extends down to soft X-ray emission with  no spectral break.
It suggests that no strong soft extended emission was associated 
with this GRB (Sakamoto et al. GCN Circ. 16771).


GRB_name: GRB140903A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16779
SUBJECT: GRB 140903A:  ISON-Kislovodsk observations
DATE:    14/09/05 04:11:18 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI), N. Polyakov (ISON), E. Romas (ISON), I. Molotov (KIAM), report on  behalf of larger collaboration:

We observed the field of  GRB 140903A (Cummings et al., GCN 16763) with Santel-400AN   telescope of ISON-Kislovodsk observatory starting on Sep. 03 (UT) 18:54:36. In the enhanced XRT position (De Pasquale et al., GCN 16767) we do not detect the object (Capone  et al., GCN 16769; Cenko  et al., GCN 16770;  Fruchter, GCN 16776). A preliminary upper limit after subtraction of the nearby bright star is 16m. A formal upper limit of a point-like source in the image away of the bright nearby star is following

Date       UT start   t-T0    Filter   Exp.   UL(3 sigma) 
                     (mid, days)        (s)

2014-09-03 18:22:05  0.14057  None     100    18.6       

The photometry is based on SDSS stars

SDSS J155213.13+273321.7 R_Lupton 15.392 &#177; 0.013
SDSS J155218.31+273433.5 R_Lupton 14.792 &#177; 0.013
SDSS J155155,39+273948,9 R_Lupton 15.421 &#177; 0.013


GRB_name: GRB140818B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16780
SUBJECT: GRB 140818B: TShAO optical upper limit
DATE:    14/09/05 06:16:20 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

A. Pozanenko (IKI), I. Rewa, W. Mundrzyjewski, A. Kusakin (Fesenkov Astrophysical Institute), A. Volnova (IKI),  report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140818B  (Vargas et al., GCN 16709)with Zeiss-1000 (East) telescope of Tien Shan Astronomical Observatory starting on Aug. 19, (UT) 17:05. We took several images in R-filter.  Within enhanced XRT error circle  (Beardmore et al., GCN 16712) we do not detect the afterlow (Aceituno et al., GCN 16711; Knust et al., GCN 16713). The source mentioned by Knust et al. (GCN 16713) is clearly visible in a stacked image in coordinates (J2000) 18:04:32.76 -01:23:08.9 (uncertainty  is 0.2 arcsec in both coordinates)  and has brightness of R=22.1+/-0.1.

Details of a photometry of the stacked image are following

Date       UT start  t-T0,d  Exp,s   Filter Up_Lim (3 sigma)
                     (mid)

2014-08-19 16:11:12  0.9317  20*600  R      22.9


The photometry is based on nearby USNO-B1.0 stars, R2 magnitudes.


GRB_name: GRB140903A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16781
SUBJECT: GRB 140903A: FTN observations
DATE:    14/09/05 10:23:04 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

S. Dichiara, C. Guidorzi (U. Ferrara), J. Japelj (U. Ljubljana)
on behalf of a large collaboration report:

The 2-m telescope Faulkes Telescope North in Hawaii began observing
Swift GRB 140903A (Cummings et al. GCN Circ 16763) on September 04
at 06:35:20 UT, i.e. ~15.6 hours after the BAT trigger, with
the r' and i' filters.
We detect the optical source reported by Capone et al. (GCN 16769),
Cenko et al. (GCN 16770), Fruchter (GCN 16776) within an estimated
magnitude of r'=20.4 +- 0.5.
Given the measured values and relatively large uncertainties,
nothing can be inferred on the possible fading.


GRB_name: GRB140901B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16782
SUBJECT: GRB 140901B: Swift XRT observation
DATE:    14/09/05 13:30:05 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L. Izzo (URoma/ICRA) and A. Maselli (INAF-IASFPA)  
report on behalf of the Swift-XRT
team:

XRT began a target of opportunity observation of GRB140901B, detected  
by Swift-BAT (Cummings, GCN Circ. 16773) and Fermi-GBM (Zhang, Circ.  
16775). Swift slewed to the burst on 2014-09-05.

Observations with the XRT began at 01:23:58 UT, i.e., 330 ks after the  
trigger, and comprised a total of 2.97 ks in photon counting mode.

We do not detect any X-ray sources, within the BAT error circle  
(Cummings, GCN Circ. 16773), with S/N>2. We place a 3-sigma upper  
limit on the count rate at the BAT position of 3.85E-03 cts/s.

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


GRB_name: GRB140903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16783
SUBJECT: GRB 140903A: NOT optical and NIR observations
DATE:    14/09/05 14:11:50 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), S. Geier (ESO), D. Malesani, J. P. U. Fynbo
(DARK/NBI), J. Harmanen (NOT), A. J. Levan (U. Warwick), P. Jakobsson
(U. Iceland) report on behalf of a large collaboration:

We observed the field of the short GRB 140903A (Cummings et al., GCN
16763) using the 2.5m Nordic Optical Telescope (NOT) equipped with
StanCam and NOTCam. We observed for a total of 20 and 30 min in the R-
and H- bands, respectively. The middle times of the observations are
29.898 hr and 30.315 hr after the BAT trigger, respectively.

The previously reported object (Capone et al., GCN 16769; Cenko  et
al., GCN 16770;  Fruchter, GCN 16776; Dichiara et al., GCN 16781) is
clearly detected in our R- and H-band stacked images. We found
R=20.1+/-0.5 mag calibrated with nearby SDSS stars and H=16.1+/-0.3
mag calibrated with the nearby 2MASS stars.

Note that a fuzzy source is present at the same position in the SDSS
field, especially in z-band. Together with the pre- and post-burst
observations, the optical brightness of the object either varies
slowly or remains constant (see also Fruchter, GCN 16776), which
implies that what we're observing in optical is basically the host
galaxy of the burst.

[GCN OPS NOTE(05sep14): Per author's request, the affilliation of SG
was changed to ESO.]


GRB_name: GRB140903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16784
SUBJECT: GRB 140903A: Possible optical variability
DATE:    14/09/05 14:49:26 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), S.B. Cenko, A. Cucchiara (NASA-GSFC), D.A. Perley (Caltech) report for a larger collaboration: 

"We observed the location of the short GRB 140903A (Cummings et al. GCN 16763, 16765) with Gemini-N beginning at 5 Sep 2014, 05:16 UT. At this epoch we obtained observations in iJ and K utilising GMOS-N and NIRI. The source reported by Capone et al. (GCN 16769) and Cenko et al. (GCN 1677) is well detected in all bands. 

A comparison between these images and the acquisition images taken on 4 Sept 2014 (Cucchiaria et al. GCN 16774) is indicative of a fading by 0.12 +/- 0.04 mag. An image subtraction shows a residual consistent with this fading, although both photometry and image subtraction are complicated by the presence of the nearby bright star.

This decay is very slow in comparison to most GRB afterglows and implies a significant contribution from the underlying host galaxy, consistent with its pre-trigger detection (Fruchter GCN 16776, Xu et al. GCN 16783). We note that the source remains largely point like in our observation, and the centroid of the subtraction residual is offset only ~0.1" from the centre of the combined host+afterglow source."


GRB_name: GRB140903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16785
SUBJECT: GRB 140903A: Confirmation of Optical Fading from Discovery Channel Telescope
DATE:    14/09/06 05:06:52 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA-GSFC), J. Capone, V. Toy (UMD), A. Cucchiara, E. Troja, A. Kutyrev (NASA-GSFC), S. Veilleux, and S. Gezari (UMD) report on behalf of a larger collaboration:

We obtained additional r'-band imaging of the candidate optical afterglow (Capone et al., GCN 16769) of the Swift short burst GRB 140903A (Cummings et al., GCN 16763) with the Discovery Channel Telescope, beginning at 2:55 UT on 6 September 2014 (2.5 d after the Swift trigger).  Performing digital image subtraction using our most recent epoch as a template, we detect significant fading in this source, confirming the results of Levan et al. (GCN 16784).  Assuming no afterglow contamination in our latest epoch, we measure an afterglow brightness of r' = 21.7 at the time of our first DCT images (~ 12 hr after the Swift trigger).  This suggests the early emission was heavily contaminated by the host galaxy, consistent with the results of Fruchter et al. (GCN 16776) and Xu et al. (16783).  A figure showing our subtraction image can be found at:

http://asd.gsfc.nasa.gov/Brad.Cenko/grb140903A_dct.pdf

The detection of optical variability, together with a coincident radio detection (Fong, GCN 16777), confirm the host association of z = 0.351 for GRB 140903A (Cucchiara et al., 16774).  We encourage additional follow-up (e.g., super/kilonova searches) to help clarify the nature of the progenitor system of this event.


GRB_name: GRB140906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16786
SUBJECT: GRB 140906A: iPTF optical transient candidates
DATE:    14/09/06 18:23:21 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), V. Bhalerao (IUCAA), M. M. Kasliwal (Carnegie
Observatories/Princeton), S. B. Cenko (NASA/GSFC) report on behalf of the
intermediate Palomar Transient Factory (iPTF) collaboration:

Fermi detected GRB 140906A (Fermi trigger 431669501 / bn140906175) at
2014-09-06 04:11:38.70. At 04:39:25, 0.46 hours after the burst, we began
searching for optical counterparts using the Palomar 48-inch Oschin
telescope (P48).

We imaged 17 fields covering an area of 125 deg^2 inside the 1-sigma
statistical+systematic region of the final Fermi GBM localization. We
estimate a 38% prior probability that these fields contain the true
location of the source. Sifting through candidate variable sources using
image subtraction and standard iPTF vetting procedures, we detected the
following optical transient candidates.

iPTF14etv is at the coordinates:
 RA(J2000)  =  16h 48m 34.01s (252.141728 deg)
 Dec(J2000) = +55d 33' 05.2"  (+55.551437 deg)
There was no source detected at this position when the iPTF survey visited
the field 7 days ago. Relative to the time of the burst, we measure:
 -6.91 days:   R > 20.46
 +1.40 hours:  R = 18.87 +/- 0.07
 +1.43 hours:  R = 19.14 +/- 0.06
We caution that the two triggered P48 observations were separated in time
by only ~100 s due to a scheduler glitch. Therefore, it is possible that
iPTF14etv is a solar system object. Further imaging is required to test
this possibility.

iPTF14etw is at the coordinates:
 RA(J2000)  =  16h 03m 11.58s (240.798240 deg)
 Dec(J2000) = +53d 00' 49.3"  (+53.013688 deg)
This position coincides with PGC 2429550, an elliptical galaxy at a
redshift of z=0.0838. The P48 photometry is:
 +1.13 hours:  R = 19.53 +/- 0.09
 +1.16 hours:  R = 19.61 +/- 0.14
 +2.00 hours:  R = 19.99 +/- 0.16
Relative to the time of the burst, this fits a power-law decay with
alpha = -0.7 +/- 0.3. However, the absolute magnitude of M_R ~ -18 inferred
from the putative host galaxy is very faint for an optical afterglow (see
Kann et al. 2011, http://dx.doi.org/10.1088/0004-637X/734/2/96).

We encourage further observations to determine the nature of these two
sources.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi431669501.pdf
shows the locations of our candidates and the P48 fields in relation to
the Fermi GBM 1-sigma statistical+systematic contour.


GRB_name: GRB140906A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16787
SUBJECT: GRB 140906A - Fermi GBM Detection
DATE:    14/09/07 09:55:02 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD), V. Pelassa and V. Connaughton (UAH) report on
behalf of the Fermi GBM Team:

At 04:11:38.70 UT on the 6th of September 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140906A
(trigger 431669501/140906175).

The angle from the Fermi LAT boresight is 90 degrees.

The on-ground calculated location, using the GBM trigger data, is
RA = 248.4, DEC = +49.5 (J2000 degrees, equivalent to
 +16h 33m, +49d 30'), with an uncertainty of 7.7 degrees (radius,
1-sigma containment, statistical only; there is additionally a
systematic error which is currently estimated to be 2 to 3 degrees).

Early follow-up observations of the GBM location error box by the
intermediate Palomar Transient Factory yielded two possible optical
counterparts (Singer et al 2014, GCN 16786).

The GBM light curve consists of a single peak followed by a fainter
tail, with a duration (T90) of 39s (50-300 keV).
The time-averaged spectrum from T0-6.1 s to T0+13.3 s (interval of
brightest emission) is best fit by a power law function with an
exponential high-energy cutoff. The power law index is -1.2 +/- 0.2
and the cutoff energy, parameterized as Epeak, is 127 +/- 33 keV.

The event fluence (10-1000 keV) in this time interval is
(1.90 +/- 0.25)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+1.216 s in the 10-1000 keV band
is 3.1 +/- 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: GRB140907A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16788
SUBJECT: GRB 140907A: Swift detection of a burst with an optical counterpart
DATE:    14/09/07 16:34:45 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. A. Krimm (CRESST/GSFC/USRA), V. D'Elia (ASDC), C. Gronwall (PSU),
L. Izzo (URoma/ICRA), K. L. Page (U Leicester), D. M. Palmer (LANL)
and T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 16:07:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140907A (trigger=611933).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 48.147, +46.595 which is 
   RA(J2000) = 03h 12m 35s
   Dec(J2000) = +46d 35' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single spiky peak
structure with a duration of about 40 sec.  The peak count rate
was ~3100 counts/sec (15-350 keV), at ~15 sec after the trigger. 

The XRT began observing the field at 16:08:32.3 UT, 83.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
48.1461, 46.6051 which is equivalent to:
   RA(J2000)  = 03h 12m 35.06s
   Dec(J2000) = +46d 36' 18.2"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 36 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 3.13
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 5.46e-10 erg cm^-2 s^-1 (0.2-10
keV). 

Automated analysis of the UVOT data products is not available, however
there appears to be a new bright optical source at the XRT position in
the prompt finding chart exposure.  More information will be available
when the full dataset is received. 

Burst Advocate for this burst is H. A. Krimm (hans.krimm 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: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16789
SUBJECT: GRB 140907A : Optical observations from Nanshan
DATE:    14/09/07 18:03:54 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), X. Gao (Urumqi No.1 Senior High School, Xinjiang),
G.-J. Feng, A. Esamdin, L. Ma (XAO), Z.-J. Xu (Nanjing Putian
Telecommunications Co. Ltd., Jiangsu) report:

We observed the field of GRB 140907A (Krimm et al., GCN 16788) using
the 35cm robotic telescope and the 1m optical telescope located at
Nanshan, Xinjiang, China. The observations started at 16:18:42 UT on
2014-09-07 at the 35cm telescope without any filter, and 16:34:28 UT
at the 1m telescope in the R filter.

The afterglow is well detected in our images at coordinates

R.A. (J2000) = 03:12:34.98
Dec. (J2000) = +46:36:17.2

Error radius: ~ 0.7 arcsec

which is fully consistent with the UVOT position. Generally, the
afterglow has been decaying, and follows are the preliminary
measurements from the 35cm telescope:

     Mid-Time              Mag
2014/09/07.68001     16.7
2014/09/07.68083     16.7
2014/09/07.68164     16.7
2014/09/07.68244     16.9
2014/09/07.68325     17.0
2014/09/07.68405     17.1
2014/09/07.68485     17.0
2014/09/07.68565     16.9
2014/09/07.68646     17.2

with a typical error of 0.2 magnitude, calibrated with the R-band
catalog of NET CMC-14.

Observations are ongoing.


GRB_name: GRB140906B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16790
SUBJECT: GRB 140906B: Fermi GBM Detection of a Long GRB
DATE:    14/09/07 19:18:41 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 10:18:02.36 UT on the 6th of September 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140906B
(trigger 431691485/140906429). The trigger resulted in an Autonomous
Repoint Request (ARR) that was accepted. The GBM on-ground location
is consistent with the Fermi flight software position.

The on-ground calculated location, using the GBM trigger data, is
RA = 187.09, DEC = +1.02 (J2000 degrees, equivalent to
 +16h 33m, +49d 30'), with an uncertainty of 2 degrees (radius,
1-sigma containment, statistical only; there is additionally a
systematic error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 47 degrees.

The GBM light curve consists of several bright emission episodes,
with a duration (T90) of about 23 seconds (50-300 keV). The
time-averaged spectrum from T0+0 s to T0+23 s is well fit by a
power law function with an exponential high-energy cutoff. The power
law index is -1.4 +/- 0.1 and the cutoff energy, parameterized as
Epeak, is 330 +/- 48 keV.

The event fluence (10-1000 keV) in this time interval is
(9.91 +/- 0.07)E-06 erg/cm^2. The 1.024-sec peak photon flux
measured starting from T0+15 s in the 10-1000 keV band is
11.0+/-0.3 ph/s/cm^2.

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


GRB_name: GRB140907A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16791
SUBJECT: GRB140907A: Swift UVOT detection
DATE:    14/09/07 20:08:13 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

NPM Kuin (UCL/MSSL), and H. A. Krimm (CRESST/GSFC/USRA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140907A
(Krimm et al., GCN Circ. No. 16788) 107 seconds after the trigger.

There is a candidate afterglow in the rapidly available 2.7'x2.7'
sub-image at
RA(J2000)  =  03:12:34.98 = 48.14575
DEC(J2000) = +46:36:17.5  = 46.60486
with a 90%-confidence error radius of about 0.75 arc sec, consistent
with the optical position from Xu et al. (GCN.Circ.No <http://gcn.circ.no/>.
16789).

Preliminary magnitudes observed in the initial images using the UVOT
photomatric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
are:

Filter  T_start(s) T_stop(s) Exp(s)   Mag
white   107        257       150      16.66 +/- 0.04
u       321        534       213      16.61 +/- 0.06

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16792
SUBJECT: GRB 140907A : Virtual Telescope optical observations
DATE:    14/09/07 22:07:14 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi and P. L. Catalano, the Virtual Telescope Project - Italy, report:

We started observations of GRB 140907A (Krimm et al., GCN 16788) with the 17" 
robotic unit part of the Virtual Telescope (Ceccano, Italy) at 21:46:00 UT.

An optical source is visible where described by D. Xu et al. (GCN 16789) in a 
image coming from the sum of tfour, 300-seconds exposures, unfiltered. The 
position of the source is RA: 03 12 35.00 Decl.: +46 36 17.6 (J2000, mean 
residuals of 0.2") and the magnitude was estimated to be around 20.0, assuming R 
mags for the reference stars from UCAC-4.

The message may be cited.


GRB_name: GRB140907A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16793
SUBJECT: GRB140907A: MITSuME Okayama Optical Observation
DATE:    14/09/08 00:47:19 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 the MITSuME and OISTER collaboration:

We observed the field of GRB 140907A (Krimm et al., GCNC 16788)
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 2014-09-07 16:21:50 UT (~15 min after the burst).
We detected the previously reported afterglow (Xu et al., GCNC 16789;
Kuin and Krimm, GCNC 16791) in all the three bands.

Photometric results of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err  Rc  Rc_err  Ic  Ic_err
-----------------------------------------------------------------------
0.01381    16:27:01     540.0     18.2 0.2    17.2 0.1    16.6 0.1
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140907A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16794
SUBJECT: GRB 140907A: MITSuME Ishigakijima Optical Observation
DATE:    14/09/08 00:47:24 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 and OISTER collaboration:

We observed the field of GRB 140907A (Krimm et al., GCNC 16788)
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 2014-09-07 16:18:10 UT (~11 min after the burst).
We detected the previously reported afterglow (Xu et al., GCNC 16789;
Kuin and Krimm, GCNC 16791) in all the three bands.

Photometric results of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]  g'    g'_err  Rc    Rc_err  Ic    Ic_err
--------------------------------------------------------------------------
0.01128    16:23:22     540.0    17.97 0.05    17.07 0.03    16.44 0.03
0.14407    19:34:36     540.0    19.73 0.12    19.36 0.11    18.48 0.11
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140907A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16795
SUBJECT: GRB 140907A: Enhanced Swift-XRT position
DATE:    14/09/08 01:03:06 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 2873 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140907A, 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 = 48.14575, +46.60472 which is equivalent
to:

RA (J2000): 03h 12m 34.98s
Dec (J2000): +46d 36' 17.0"

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

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16796
SUBJECT: GRB 140907A: Swift-XRT refined Analysis
DATE:    14/09/08 07:35:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), M.C. Stroh (PSU),
D.N. Burrows (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), C.
Pagani (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo
(INAF-OAB) and H.A. Krimm report on behalf of the Swift-XRT team:

We have analysed 8.8 ks of XRT data for GRB 140907A (Krimm  et al. GCN
Circ. 16788),  from 73 s to 40.5 ks after the  BAT trigger. The data
comprise 89 s in Windowed Timing (WT) mode (the first 9 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 Goad et al.
(GCN Circ. 16795).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.1 (+0.8, -0.7), followed by a break at T+119 s to an
alpha of 0.822 (+0.023, -0.025).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.14, -0.13). The
best-fitting absorption column is  3.8 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.1 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.9 x 10^-11 (6.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.8 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 3.1 x 10^21 cm^-2
Excess significance: 1.9 sigma
Photon index:      2.01 (+0.14, -0.13)

If the light curve continues to decay with a power-law decay index of
0.822, 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 9.1 x
10^-13 (1.4 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/00611933.

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


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16797
SUBJECT: GRB 140907A: redshift from the 10.4m GTC telescope
DATE:    14/09/08 08:01:07 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A.J. Castro-Tirado (IAA-CSIC/ISA-UMA), J. Gorosabel (IAA-CSIC/UPV-EHU) and
A. Garcia-Rodriguez (GTC-IAC), report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 140907A (Krimm et al. GCN 16788;
Kuin et al. GCN 16791; Masi et al. GCN 16792, Kuroda et al. GCN 16793)
with the 10.4m GTC (+OSIRIS). Spectroscopic observations started at
05:29:33 UT (13.4 hours post GRB). Two 500s spectra were obtained with the
R1000B and R1000R grisms, covering the range between 3800 and 9900 A, at a
resolution of ~1000. A preliminary reduction based on archival calibration
lamps, reveals the Mg II doublet plus several Fe II lines at a common
redshift of z = 1.21, which we identify as the redshift of the GRB.


GRB_name: GRB140907A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16798
SUBJECT: GRB 140907A: Fermi GBM Detection
DATE:    14/09/08 15:32:05 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 16:07:11.80 UT on 07 September 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140907A (trigger 431798834 / 140907672), which
was also detected by the Swift/BAT (Krimm et al 2014, GCN 16788)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 16 degrees.

The GBM light curve consists of a single pulse with multiple peaks.
The total duration (T90) is about 35 +/- 10 s (50-300 keV).
The time-averaged spectrum from T0-12 s to T0+22 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.97 +/- 0.08  and
the cutoff energy, parameterized as Epeak, is 113 +/- 7 keV.

The event fluence (10-1000 keV) in this time interval is
(5.5 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+8.9 s in the 10-1000 keV band
is 4.2 +/- 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: GRB140907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16799
SUBJECT: GRB 140907A: Swift-BAT refined analysis
DATE:    14/09/08 16:12:53 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. Sakamoto (AGU), 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 (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(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 140907A (trigger #611933)
(Krimm, et al., GCN Circ. 16788).  The BAT ground-calculated position is
RA, Dec = 48.133, 46.596 deg which is
    RA(J2000)  =  03h 12m 31.9s
    Dec(J2000) = +46d 35' 43.8"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 65%.

The mask-weighted light curve shows a single peak with superimposed spikes,
running from approximately T-10 to T+40 sec.  T90 (15-350 keV) is 79.2 +- 31.4 sec
(estimated error including systematics).

The time-averaged spectrum from T-91.2 to T+39.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.72 +- 0.07.  The fluence in the 15-150 keV band is 4.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+17.47 sec in the 15-150 keV band
is 2.5 +- 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/611933/BA/


GRB_name: GRB140907A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16800
SUBJECT: GRB 140907A: T100 observations
DATE:    14/09/08 16:49:15 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), U. Temiz, H. Avdan (Cukurova Univ.), T. Guver
(Istanbul Univ.), E. Gogus (Sabanci Univ.), S. Eryilmaz (TUG), K. Yakut
(Ege Univ.), H. Kirbiyik (TUG) report on behalf of a larger collaboration


 We observed the field of Swift GRB 140907A (Krimm et al., GCN#16788) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting September, 7, 23:54:47 UT (~ 7.794 hours after the
trigger). Observations were carried out in the R filter. The afterglow is
clearly detected in 300 s in the R band images.


Using USNO-B1 star USNO-B1 1366-0072923 (R.A.=48.155, Dec=+46.614) in the
field, the magnitude of the OT was estimated as follows;

t-t0 (hr) exp.(s) filt mag err (+/-)

7.794 300 R 19.65 0.20


 We are grateful to TUBITAK National Observatory for prompt scheduling the
observations and technical support.


GRB_name: GRB140906C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16801
SUBJECT: IPN Triangulation of GRB 140906C (short/hard)
DATE:    14/09/08 21:17:16 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

The short-duration, hard spectrum, intense GRB 140906C has been observed 
by Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), AGILE (MCAL), and 
MESSENGER (GRNS), so far, at about 85869 s UT (23:51:09). 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:
   314.964 (20h 59m 51s)  +2.354 ( +2d 21' 14")
  Corners:
   315.062 (21h 00m 15s)  +0.809 ( +0d 48' 31")
   314.873 (20h 59m 30s)  +0.650 ( +0d 39' 00")
   314.902 (20h 59m 36s)  +3.944 ( +3d 56' 39")
   315.099 (21h 00m 24s)  +4.119 ( +4d 07' 07")
  ---------------------------------------------
The error box area is 2273 sq. arcmin, and its maximum
dimension is 4.6 deg (the minimum one is 12 arcmin).
The Sun distance was 148 deg.

This box can be improved.

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


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16802
SUBJECT: GRB 140907A: Discovery Channel Telescope observations
DATE:    14/09/09 03:26:20 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (NASA-GSFC),S.B. Cenko (NASA-GSFC), J. Capone (UMD), 
V. Toy (UMD),   E. Troja (NASA-GSFC), A. Kutyrev (NASA-GSFC), S. Veilleux
(UMD), and S. Gezari (UMD) report on behalf of a larger collaboration:

"On September 08.37UT (approximately 16.5h after the discovery) we observed 
the optical counterpart of GRB 140907A (Krimm et al. GCN 16788, Xu et al. 
GCN 16789, Kuin et al. GCN 16791) with the Large Monolithic Imager (LMI) on 
the 4.3m  Discovery Channel Telescope (DCT) at Happy Jack, AZ. We observed in 
g', r', and i' bands for a total of 6, 6 and 4 minutes respectively.

Using a set of stars from the APASS catalogue we derived the following 
magnitude for the afterglow:

g' = 21.54 +- 0.17
r' = 20.92 +- 0.15
i' = 20.42 +- 0.16

We thank the DCT staff, in particular S. Strosahl and H. Larson for 
their support in performing these observations."


GRB_name: GRB140907A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16803
SUBJECT: GRB 140907A: MITSuME Akeno Optical Observation
DATE:    14/09/09 07:25:07 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y. Tachibana, Y. Saito, T. Yoshii, H. Ohuchi, Y. Yano,
S. Kurita, Y. Ono, T. Fujiwara, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 140907A (Krimm et al., GCN Circular #16788) 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 2014-09-07 17:05:39 UT (~1 h after the burst).
We detected the previously reported optical afterglow (Xu et al., GCN Circular #16789, Kuin and Krimm, GCN Circular #16791, Kuroda et al., GCN Circular #16793) in the g',Rc and Ic band.

The measured magnitudes are listed below.

T0+[day]  MID-UT  T-EXP[sec]    g'                Rc             Ic
------------------------------------------------------------------------------
0.04064  17:09:16  360      19.2+/-0.2  18.2+/-0.2  17.3+/-0.1
0.07348  18:07:29  300          >19.2           >18.3       >17.7
------------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140907A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16804
SUBJECT: GRB 140907A: Nishi-Harima NIR Observations
DATE:    14/09/09 07:55:31 GMT
FROM:    Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo  <arai@nhao.jp>

J. Takahashi, A. Arai, S. Honda, Y. Takagi,  K. Morihana (Univ. of Hyogo)
report on behalf of Nayuta team and OISTER collaboration:

We observed the field of GRB 140907A (H. A. Krimm et al., GCN 16788)
with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m
telescope at the Nishi-Harima Astronomical Observatory.

The observations were started at 19:00 UT on 2014-09-07.
We detected the near-infrared afterglow in J, H and Ks bands.

Photometric results of our observations are shown below.
We used 2MASS 03123451+4635419, 03123283+4635411, and 03123016+4635375
as reference stars for photometry.

# MID-UT  Tmid-T0 T-EXP  J_mag    H_mag    Ks_mag
-----------------------------------------------------------------------
19:07:32    3.0    600   17.5 +/- 0.2   17.0 +/- 0.1   16.6 +/- 0.3
------------------------------------------------------------------------
Tmid-T0: Elapsed time after the burst (hours)
T-EXP: Total Exposure time (seconds)


GRB_name: GRB140906C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16805
SUBJECT: Refined IPN Triangulation of GRB 140906C
DATE:    14/09/09 12:14:15 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,

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

J. Goldsten, on behalf of the MESSENGER NS 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,

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

D. M. Smith, on behalf of the RHESSI GRB team, report:

The short-duration, hard spectrum GRB 140906 (Golenetskii et al., GCN 
16801) was also observed by RHESSI and Odyssey. Using Odyssey data 
reduces the size of the previous error box by about a factor of 6:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   314.961 (20h 59m 51s)  +1.939 ( +1d 56' 21")
  Corners:
   315.057 (21h 00m 14s)  +1.949 ( +1d 56' 57")
   314.869 (20h 59m 29s)  +2.439 ( +2d 26' 22")
   314.866 (20h 59m 28s)  +1.929 ( +1d 55' 45")
   315.057 (21h 00m 14s)  +1.428 ( +1d 25' 41")
  ---------------------------------------------
The error box area is 355 sq. arcmin, and its maximum
dimension is 1.0 deg (the minimum one is 11 arcmin).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140906_T85872/IPN/

Some further improvement in this error box is possible.


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16806
SUBJECT: GRB 140907A: MASTER optical observations
DATE:    14/09/09 13:03:53 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya, V.Kornilov, D.Kuvshinov, 
N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, 
D.Denisenko,  A.Sankovich
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A. Gabovich
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

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

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 Blagoveschensk was pointed to the  GRB140907A 6987 sec after 
notice time and 7504 sec after trigger time at 2014-09-07 18:12:13 UT 
directly after weather conditions became suitable. On our first (180s 
exposure)  set we found optical transient  within Swift error-box (ra=03 
12 34 dec=+46 36 18 r=0.050000) on coadditional images in two epoch.
The protometry results available at Table 1.


Table 1.

Date and  Time start  T_trig-Tmid  Exptime    Mag   err.mag

2014-09-07 18:12:13.4   7809        540      19.0     0.2
2014-09-07 19:23:43.6  12547       1260      19.4     0.2

The  approximate power law index (alpha) from 7000 to 13000 seconds after 
the trigger is  about 0.81 +- 0.1  (F ~ t^-alpha).

Another two MASTER-II robotic telescop located in Kislovodsk and Tunka 
made upper limit observations only in earlier time due to weather 
conditions and high zenith distance of object.  MASTER II  in Tunka was 
pointed to the  GRB140907A  1021 sec after trigger time at 2014-09-07 
16:24:10 directly after weather conditions became suitable. On our first 
(180s exposure) image we haven't found optical transient up to 16m. MASTER 
II in Kislovodsk starting observations  GRB140907A 17 sec after notice 
time and 77 sec after trigger time at 2014-09-07 16:08:25 using FERMI GBM 
coordinates. However OT position was not covered by MASTER-II. The 
telescope pointing by Swift trigger 22 sec after notice time and 540 after 
trigger time at 2014-09-07 16:16:08.  On first (110s exposure) image we 
haven't found optical transient up to 12.5 m. The zenith distance of 
object z~85 d.

Our white (clear) band is well described by a parity 0.8R+0.2B (USNO B1).


GRB_name: GRB140906C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16807
SUBJECT: Konus-Wind observation of GRB 140906C
DATE:    14/09/09 15:37:27 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The short-duration GRB 140906C (IPN triangulation: Golenetskii et al.,
GCN 16801 and Hurley et al., GCN 16805) triggered Konus-Wind
at T0=85872.815 s UT (23:51:12.815).

The burst light curve shows two peaks with a total duration of ~0.16 s. 
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140906_T85872/

As observed by Konus-Wind, the burst
had a fluence of 2.2(-0.5,+0.6)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.064 s,
of 4.4(-1.4,+1.7)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.128 s)
is best fit in the 20 keV - 10 MeV range
by a simple power law function with index = -1.76 (-0.11,+0.13)
(chi2 = 24.2/23 dof).
Fitting by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields the same alpha
and a lower limit on the Ep: Ep > 248 keV (chi2 = 22/22 dof).

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


GRB_name: GRB140909A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16808
SUBJECT: GRB 140909A: Swift detection of a GRB 
DATE:    14/09/09 17:59:24 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

David Palmer reports on behalf of the Swift Team:

In two successive 64-second images, beginning at 06:56:51, BAT detected a source at a consistent
location.  Although the individual images were below threshold, the combined detection
is highly significant, in excess of 8 sigma.  A 320 s image that includes the data
from both 64 s images indicates additional flux outside of the 128 s time interval.

The BAT on-board calculated location is RA,dec = 193.638,63.494 (J2000), which is
  RA(J2000) =  12h 54m 33s
  Dec(J2000) = +63d 29 38

As is usual for image triggers, there is no obvious variation in the BAT lightcurve.

Because the individual images were below threshold, Swift did not automatically
slew to the location.  However, a ToO has been requested.

-- 
David Palmer  palmer@lanl.gov   (505)665-6863 (voice)   (505)665-4414 (fax)


GRB_name: GRB140907A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16809
SUBJECT: GRB 140907A: TShAO observations
DATE:    14/09/09 20:54:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Pozanenko (IKI), W. Mundrzyjewski (Fesenkov 
Astrophysical Institute), V. Tereshenko (Fesenkov Astrophysical 
Institute)  report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140907A  (Krimm et al., GCN 
16788)with Zeiss-1000 (East) telescope of Tien Shan Astronomical 
Observatory starting on Sep. 07, (UT) 17:05. We took several images in 
R-filter.  Within enhanced XRT error circle  (Goadet al., GCN 16795) we 
clearly detect the afterglow(Xu et al., GCN 16789; Kuin and Krimm, GCN 
16791).
Preliminary photometry of first and last exposures is following

Date       UT start  t-T0,d  Exp,s   Filter OT    OT_err
                      (mid)

2014-09-07 17:33:41 0.06357  600     R     18.94 0.08
2014-09-07 23:22:46 0.30598  600     R     20.22 0.07

The photometry is based on nearby USNO-B1.0 stars, R2 magnitudes. 
Preliminary light curve of the afterglow of GRB 140907A obtained between 
(UT) 17:33:41 and  23:22:46   can be found in 
http://grb.rssi.ru/GRB140907A/GRB14907A_lc.png .

Within the time interval ( 17:33:41 - 23:22:46  ) the LC might be 
approximated by power law with a power law index ~-2 which could suggest 
the jet-brake within this interval.


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16810
SUBJECT: GRB 140907A: 1.23m CAHA optical observations
DATE:    14/09/10 00:32:37 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Ugarte (UPV-EHU), S. Perez-Hoyos (UPV-EHU), A. Sanchez-Lavega
(UPV-EHU), R. Hueso (UPV-EHU), J. Gorosabel (IAA-CSIC/UPV-EHU) report on
behalf of the BEGIRA project:

We observed the GRB 140907A (GCN 16788) optical afterglow (GCN 16789, GCN
16791, GCN 16792, GCN 16793, GCN 16797, GCN 16800, GCN 16802, GCN 16803,
GCN 16804, GCN 16806, GCN 16809) with the 1.23m CAHA telescope. The
observations were carried out in the R and I-bands on Sep 8.96168-9.21435
UT (30.96-37.05 hours post GRB). The optical afterglow is clearly detected
with a magnitude I(Vega)=21.4, calibrated against the USNO B1.0 catalog.


GRB_name: GRB140909A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16811
SUBJECT: GRB 140909A: Swift-XRT observations
DATE:    14/09/10 07:13:30 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

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

We have analysed 5.0 ks of XRT data for the Swift/BAT-detected burst:
GRB 140909A,  from 44.0 ks to 56.5 ks after the  Swift/BAT trigger. The
data are entirely in Photon Counting (PC) mode.  An X-ray source is
detected within the Swift/BAT error circle. Using 1945 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 = 193.61156, +63.51677 which is equivalent to:

RA (J2000): 12h 54m 26.78s
Dec(J2000): +63d 31' 00.4"

with an uncertainty of 7.2 arcsec (radius, 90% confidence). This
position is 92 arcsec from the Swift/BAT position.  The source has a
mean count rate of 6.9e-03 ct/sec; we cannot determine at the present
time whether it is fading.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020417.

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


GRB_name: GRB140909A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16812
SUBJECT: GRB 140909A: Swift/UVOT Upper Limits
DATE:    14/09/10 19:02:50 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

GRB 140909A: Swift/UVOT Upper Limits

M. H. Siegel (PSU) and E. Sonbas (Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140909A
44028 s after the BAT trigger (Palmer et al., GCN Circ. 16808).
No optical afterglow consistent with the XRT position
(Pagani et al. GCN Circ. 16811) is detected in the initial UVOT exposure.
The preliminary 3-sigma upper limit using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposure is:

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

white            44028        56310         3213         >22.0

The magnitude is not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.015 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140903A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16813
SUBJECT: GRB 140903A: Chandra detection of the afterglow
DATE:    14/09/10 21:26:39 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto (AGU), E. Troja (GSFC/UMCP), N. Gehrels (GSFC), 
J. Norris (BSU), S. D. Barthelmy (GSFC), J. L. Racusin (GSFC), 
N. Kawai (Tokyo Tech), A. Fruchter (STScI)

A Chandra ToO observation of a short GRB 140903A (Cummings et al., GCN Circ. 16763; 
Cummings et al., GCN Circ. 16765) started on September 6 08:54 UT (~2.7 days after the 
GRB trigger) for a total of 19.8 ksec.  The X-ray afterglow was clearly detected at 
a position (RA, Dec) = (238.013519, +27.60303) which is equivalent to:

RA (J2000) = 15 52 03.24
Dec (J2000) = +27 36 10.9

The 1-sigma statistical error is 0.05 and 0.04 arcsec on RA and Dec respectively.  
The systematic error of the Chandra aspect solution is 0.3 arcsec (radius, 68% 
containment; i.e, http://cxc.harvard.edu/cal/ASPECT/celmon/) which dominates  
the localization uncertainty. 

The Chandra location is consistent with the enhanced XRT position (De Pasquale et al., 
GCN Circ. 16767) and the reported NIR, optical and radio afterglow/host candidate 
(Capone et al., GCN Circ. 16769; Cenko et al., GCN Circ. 16785; Cenko et al., 
GCN Circ. 16770; Fruchter et al., GCN Circ. 16776; Fong, GCN Circ. 16777; 
Dichiara et al., GCN Circ. 16781; Xu et al. GCN Circ. 16783; Levan et al. GCN Circ. 16784).  
Our Chandra detection confirms the association of the reported NIR, optical and radio 
candidate to GRB 140903A.  Further Chandra observations are planned.  

We would like to thank the Chandra operation team for rapidly approving and making 
this observation.


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16814
SUBJECT: GRB 140907A: Mondy optical observations
DATE:    14/09/11 16:53:02 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), E. Klunko (ISTP), M. Eselevich (ISTP), I. Korobtsev 
(ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of the Swift GRB 140907A  (Krimm et al., GCN 
16788) with with AZT-33IK telescope of Sayan observatory (Mondy). We 
obtained several images on Sep., 08 and Sep. 9.  Within enhanced XRT 
error circle  (Goadet al., GCN 16795) we clearly detect the afterglow 
(Xu et al., GCN 16789; Kuin and Krimm, GCN 16791).
Preliminary photometry is following:

date        UT start  t-T0        Filter  Exp.    OT      OT_err
                       (mid, days)          (s)

2014-09-08  15:38:52  1.00888     R       82*60   21.26   0.08
2014-09-09  14:35:11  1.97786     R      120*60   22.50   0.20

The photometry is based on the same USNO-B1.0  stars which were used in 
GCN 16809:

ID           RA           Dec         R2
1366-0072961 03:12:42.62  +46:36:01.4 15.84
1365-0072251 03:12:34.50  +46:35:42.0 14.55
1365-0072223 03:12:30.14  +46:35:37.7 15.57

The light curve can be found in
http://grb.rssi.ru/GRB140907A/GRB14907A_lc1.png


GRB_name: GRB140903A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16815
SUBJECT: Possible radio detection of  GRB 140903A with the GMRT
DATE:    14/09/12 08:44:42 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

A. J. Nayana (NCRA-TIFR)  and Poonam Chandra (NCRA-TIFR) report:

We carried out the Giant Metrewave Radio Telescope (GMRT) observations of
GRB 1400903A (Cummings et al. GCN 16763) in the 1390 MHz band on 2014
September 11.05 UT. We detect a 3.1-sigma source at the GRB position 
(Cenko et al.
16770) with a flux density of 102+/-33 uJy. This is most likely the 
radio afterglow of
GRB 140903A. We are carrying out further observations to confirm this 
detection.

We thank GMRT staff for making these observations possible.


GRB_name: GRB140909A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16816
SUBJECT: GRB 140909A: Confirmation of the Swift-XRT afterglow
DATE:    14/09/12 10:36:45 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) and E. Sonbas (Adiyaman U.) report on behalf of 
the Swift team:

A second epoch of XRT data was collected on the field of the Swift/BAT 
ground detected GRB 140909A (Palmer, GCN Circ. 16808), from 148 ks to 
252 ks after the  Swift/BAT trigger.

The X-ray source reported in GCN Circ. 16811, Pagani et al., at a mean 
count rate of 6.9e-03 ct/sec, is now no longer detected, having faded 
below a 3-sigma upper limit of 2.3 x 10^-3 count s^-1 (0.3-10 keV). We 
therefore confirm that this is the X-ray afterglow of GRB 140909A

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


GRB_name: GRB140907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16818
SUBJECT: GRB 140907A: Continued DCT Observations
DATE:    14/09/13 15:49:21 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko, A. Cucchiara (NASA-GSFC), J. Capone, V. Toy (UMD), E. Troja, A. Kutyrev (NASA-GSFC), S. Veilleux, and S. Gezari (UMD) report on behalf of a larger collaboration:

We re-observed the field of the Swift GRB 140907A (Krimm et al., GCN 16788) with the Large Monolithic Imager on the 4.3m Discovery Channel Telescope (DCT).  Observations were obtained in the r' filter beginning at 11:28 UT on 2014 Sep 10 (~ 2.8 d after the Swift trigger) for a total exposure time of 720 s. 

Using nearby point sources from the APASS catalog for calibration, we measure a magnitude of r' = 22.79 +/- 0.07 mag for the optical afterglow (Xu et al., GCN 16789; Kuin et al., GCN 16791).  Compared with our previous epoch of DCT imaging, we infer a corresponding power-law decay index of alpha = 1.2 +/- 0.1.


GRB_name: GRB140916A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16819
SUBJECT: GRB 140916A: Swift detection of a burst
DATE:    14/09/16 10:58:29 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), D. Malesani (DARK/NBI) and
K. L. Page (U Leicester) report on behalf of the Swift Team:

At 10:43:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140916A (trigger=612804).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 40.405, -39.711 which is 
   RA(J2000) = 02h 41m 37s
   Dec(J2000) = -39d 42' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This is an image trigger so details of the 
lightcurve can not yet be determined. 

The XRT began observing the field at 10:46:18.3 UT, 150.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 40.39910, -39.68686 which
is equivalent to:
   RA(J2000)  = 02h 41m 35.78s
   Dec(J2000) = -39d 41' 12.7"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 87 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 1.26e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 160 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
0.01. 

Burst Advocate for this burst is J. L. Racusin (judith.racusin 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: GRB140916A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16820
SUBJECT: GRB 140916A: Prompt enhanced Swift-XRT position
DATE:    14/09/16 11:25:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 140916A, we find an
enhanced XRT position of the afterglow: RA, Dec: 40.3999, -39.6865
which is equivalent to:
   RA (J2000)  = 02 41 35.98
   Dec (J2000) = -39 41 11.4
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/612804.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140916A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16821
SUBJECT: GRB 140916A: FTS observations
DATE:    14/09/16 16:06:06 GMT
FROM:    Simone Dichiara at Ferrara U/Italy  <dichiara@fe.infn.it>

S. Dichiara, C. Guidorzi (U. Ferrara), J. Japelj (U. Ljubljana)
on behalf of a large collaboration report:

The 2-m Faulkes Telescope South in Siding Spring
(Australia) began observing Swift GRB 140916A (Racusin et al.
GCN Circ 16819) on September 16 at 11:52:12 UT, i.e.
~1.14 hours after the BAT trigger, with the r' and i' filters.

Within the enhanced XRT error circle (Evans et al. GCN Circ. 16820)
we find no optical counterpart to the following limiting magnitude:

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)   (s)
-------------------------------------------------
1.26          60x7       r'        > 20.4
1.44          60x5       i'        > 18.7
-------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB140916B
Detection_method: iPTF
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16822
SUBJECT: GRB 140916B: iPTF Optical Observations
DATE:    14/09/16 18:28:07 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), V. Bhalerao (IUCAA), M. M. Kasliwal (Carnegie
Observatories/Princeton), and S. B. Cenko (NASA/GSFC) report on behalf of
the intermediate Palomar Transient Factory (iPTF) collaboration:

Fermi detected GRB 140916B (Fermi trigger 432538612 / bn140916234) at
2014-09-16 05:36:49.80. At 09:28:17, 3.86 hours after the burst, we began
searching for optical counterparts using the Palomar 48-inch Oschin
telescope (P48).

We imaged 20 fields covering an area of 146 deg^2 inside the 1-sigma
statistical+systematic region of the final Fermi GBM localization. We
estimate a 53% prior probability that these fields contain the true
location of the source. Sifting through candidate variable sources using
image subtraction and standard iPTF vetting procedures, we detected the
following optical transient candidates.

iPTF14fok is located near a galaxy with unknown redshift, at the
coordinates:
 RA(J2000)  =  3h 43m 14.11s (55.808775 deg)
 Dec(J2000) = -8d 17' 33.5"  (-8.292649 deg)
At R = 19.57 +/- 0.07 mag, the lightcurve from 4.17 to 5.85 hours after
the burst is consistent with no evolution or with a decline by ~0.1 mag.

iPTF14fow is located near the nuclear region of a galaxy with unknown
redshift, at the coordinates:
 RA(J2000)  =  4h 24m 54.71s (66.227963 deg)
 Dec(J2000) = -6d 47' 09.7"  (-6.786030 deg)
At R = 20.14 +/- 0.14 mag, the source shows no clear photometric evolution.

Further observations are encouraged to determine the nature of these
sources.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi432538612.pdf
shows the locations of our candidates and the P48 fields in relation to
the Fermi GBM 1- and 2-sigma statistical+systematic contours.


GRB_name: GRB140916A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16823
SUBJECT: GRB 140916A: MITSuME Okayama upper limits
DATE:    14/09/16 19:38:44 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 and OISTER collaboration:

We observed the field of GRB 140916A (Racusin et al., GCNC 16819)
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 2014-09-16 17:07:26 UT, (~6.4 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans, GCNC 16820) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.30614    18:04:37    3840.0   >18.9  >19.5  >18.7
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140916A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16824
SUBJECT: GRB 140916A: Enhanced Swift-XRT position
DATE:    14/09/16 22:39:06 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 8554 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 140916A, 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 = 40.39949, -39.68645 which is equivalent
to:

RA (J2000): 02h 41m 35.88s
Dec (J2000): -39d 41' 11.2"

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: GRB140916A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16825
SUBJECT: GRB 140916A: Swift-XRT refined Analysis
DATE:    14/09/16 22:58:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), V.
Mangano (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
J.L. Racusin report on behalf of the Swift-XRT team:

We have analysed 13 ks of XRT data for GRB 140916A (Racusin  et al. GCN
Circ. 16819),  from 141 s to 30.7 ks after the BAT trigger. The data
comprise 218 s in Windowed Timing (WT) mode (the first 8 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 Osborne et
al. (GCN Circ. 16820). The late-time light curve (from T0+5.3 ks) is
consistent with a constant source of mean count rate 5.4e-01 ct/sec. A
power-law fit gives an index of -0.04 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.70 (+/-0.11). The
best-fitting absorption column is  1.51 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 1.7 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.05 (+/-0.09) and a
best-fitting absorption column of 1.34 (+0.26, -0.25) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (4.3 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.34 (+0.26, -0.25) x 10^21 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: 7.8 sigma
Photon index:      2.05 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
-0.04, the count rate at T+24 hours will be 0.23 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.6 x
10^-12 (9.9 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00612804.

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


GRB_name: GRB140916A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16826
SUBJECT: GRB 140916A: UKIRT J-band observations
DATE:    14/09/16 23:19:37 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong, P. Milne, N. Smith and J. Andrews (U. Arizona) report on behalf of
the Arizona Transient Exploration and Characterization (AZTEC)
collaboration:

"We observed the field of the Swift-detected GRB 140916A (Racusin et al.,
GCN 16819) with UFTI mounted on the 3.8-m United Kingdom Infrared Telescope
(UKIRT) on Mauna Kea beginning on 2014 Sep 16.561 UT (2.7 hr post-burst).
In 36-min of J-band imaging, we do not detect any near-IR source in or
around the enhanced XRT position (Evans et al., GCN 16820; Osborne et al.,
GCN 16824). Calibrated to 2MASS, we therefore place a 3-sigma limit of
J(VEGA)>21 mag on the near-IR afterglow of GRB 140916A at 2.7 hr post-burst.

We thank T. Carroll for assistance with these observations."


GRB_name: GRB140916A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16827
SUBJECT: GRB 140916A: Swift-BAT refined analysis
DATE:    14/09/17 00:23:32 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Stamatikos (OSU), 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 (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), 
J. L. Racusin (NASA/GSFC), T. Sakamoto (AGU), J. Tueller (GSFC), T. N. Ukwatta (LANL) 
(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 140916A (trigger #612804)
(Racusin, et al., GCN Circ. 16819).  The BAT ground-calculated position is
RA, Dec = 40.384, -39.688 deg which is 
  RA(J2000)  =  02h 41m 32.2s 
  Dec(J2000) = -39d 41' 18.6" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 16%.

The mask-weighted light curve shows a single peak starting at T-3 sec, peaking 
at T+3 sec and ending at T+100 sec.  T90 (15-350 keV) is 80.1 +- 15.6 sec 
(estimated error including systematics).

The time-averaged spectrum from T-6.6 to T+89.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.15 +- 0.27.  The fluence in the 15-150 keV band is 1.7 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.80 sec in the 15-150 keV band
is 1.3 +- 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/612804/BA/


GRB_name: GRB140916A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16828
SUBJECT: GRB 140916A: Swift/UVOT Upper Limits
DATE:    14/09/17 00:26:30 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140916A
160 s after the BAT trigger (Racusin et al., GCN Circ. 16819).
No optical afterglow consistent with the XRT position
(Evans GCN Circ. 16820)
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           160          310          147         >21.5
u_FC               318          568          246         >20.7
white              160         6731          608         >22.3
v                  648        12894         1415         >21.2
b                  574        19208          857         >20.8
u                  318        24969         2113         >21.4
w1                 697        30730         2826         >21.9
m2                 844        30169         2742         >21.7
w2                 796        29263         2203         >22.1

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: GRB140916B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16830
SUBJECT: GRB 140916B: LOT and iPTF follow-up of optical afterglow candidates 
DATE:    14/09/18 02:13:09 GMT
FROM:    Kuiyun Huang at ASIAA  <ljhuang@asiaa.sinica.edu.tw>

GRB 140916B: LOT and iPTF follow-up of optical afterglow candidates

L. P. Singer (Caltech), K.Y. Huang (NCU/NTNU/ASIAA), Y. Urata (NCU),
V. Bhalerao (IUCAA), M. M. Kasliwal (Carnegie Observatories/Princeton),
and S. B. Cenko (NASA/GSFC) report on behalf of a larger collaboration:

We have continued to observe the optical afterglow candidates reported by
iPTF (Singer et al., GCN 16822) in connection with GRB 140916B, which was
detected by Fermi. We obtained images of iPTF14fok with the Lulin
One-meter Telescope (LOT), the Palomar 48-inch Oschin telescope (P48), and
the robotic Palomar 60-inch telescope (P60). We report the following
observations, relative to the time of the burst:

  LOT, +13.16 hours:   r = 19.87 +/- 0.18
  P60, +29.67 hours:   r = 19.02 +/- 0.22

The source has not faded significantly from the initial P48 detection 4.17
hours after the burst of R = 19.57 +/- 0.07 mag. We therefore conclude
that it is unrelated to the GRB, possibly an old foreground supernova.

This message can be cited.


GRB_name: GRB140919A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16831
SUBJECT: GRB 140919A: Swift detection of a burst
DATE:    14/09/19 15:38:25 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

M.E. Gropp (PSU), S. B. Cenko (GSFC), C. Gronwall (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC), V. Mangano (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
J. L. Racusin (NASA/GSFC) and B. Sbarufatti (INAF-OAB/PSU) report on
behalf of the Swift Team:

At 15:15:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140919A (trigger=613160).
The BAT on-board calculated location is
RA, Dec 221.556, -32.154 which is
    RA(J2000) = 14h 46m 13s
    Dec(J2000) = -32d 09' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 100 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger.

Due to an observing constraint, Swift will not slew until T0+48.2
minutes. There will be no XRT or UVOT data until this time.

Burst Advocate for this burst is M.E. Gropp (mgropp742 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: GRB140919A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16832
SUBJECT: GRB 140919A: Swift-XRT observations
DATE:    14/09/19 16:36:48 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 140919A at 16:07:15.9 UT,
3120.4 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 221.53822,
-32.17586 which is equivalent to:
   RA(J2000)  = 14h 46m 09.17s
   Dec(J2000) = -32d 10' 33.1"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 95 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 7.65
x 10^20 cm^-2 (Willingale et al. 2013). 


GRB_name: GRB140919A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16833
SUBJECT: GRB 140919A: Swift/UVOT observations
DATE:    14/09/19 17:22:26 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC, MSSL-UCL) and M.E. Gropp (PSU) report 
on behalf of the Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3124 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. We note that within the XRT error 
circle (Perri et al., GCN Circ. 16832) there is a point source which is also 
observed in the DSS. The 2.7'x2.7' sub-image covers 25% of the BAT error circle. 
The typical 3-sigma upper limit has been about 19.6mag. The 8'x8' region for the 
list of sources generated on-board covers 100% of the BAT error circle. The 
list of sources is typically complete to about 18mag. 

No correction has been made for the expected extinction corresponding to
E(B-V) of 0.09. 


GRB_name: GRB140919A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16834
SUBJECT: GRB 140919A: Enhanced Swift-XRT position
DATE:    14/09/19 19:23:43 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 1892 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140919A, 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 = 221.53734, -32.17629 which is equivalent
to:

RA (J2000): 14h 46m 8.96s
Dec (J2000): -32d 10' 34.7"

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: GRB140919A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16835
SUBJECT: GRB 140919A: Fermi GBM observation
DATE:    14/09/20 02:54:19 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa (UAH) and D. Yu (MPE) report on behalf of the Fermi GBM Team:

"At 15:15:13.54 UT on 19 September 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140919A (trigger 432832516 / 140919636),
which was also detected by the Swift/BAT (Gropp et al. 2014, GCN 16831).
The GBM on-ground location is consistent with the Swift position.
The angle of the Swift position from the Fermi LAT boresight is 34.6 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 109 s (50-300 keV).
The time-averaged spectrum from T0-5.12 s to T0+123.91 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.80 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 103 +/- 18 keV
(Castor statistics 1085.8 for 610 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.20 +/- 0.06)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+5.248 s in the 10-1000 keV band
is 3.6 +/- 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: GRB140919A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16836
SUBJECT: GRB 140919A: GROND afterglow candidate
DATE:    14/09/20 03:46:13 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

S. Schmidl (TLS Tautenburg), J. Bolmer and J. Greiner (both MPE Garching)
report on behalf of the GROND team:

We observed the field of GRB 140919A (Swift trigger 613160; Gropp et al.,
GCN #16831) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 23:29 UT on 2014-09-19, 8.2 hrs after the GRB
trigger. They were performed at an average seeing of 1.7" and at an
average airmass of 2.1.

We detect a source inside the enhanced 1.5" Swift-XRT error cicle, at

RA  (J2000) =  14:46:08.96
DEC (J2000) = -32:10:34.6

with an uncertainty of 0.5" in each coordinate.

Based on total exposures of 7.7 minutes in g'r'i'z'and 24.0 minutes in
JHK, at a midtime of 9.2 hrs after the burst, we measure the following
preliminary magnitudes and upper limits (AB magnitude system):

g' = 19.8 +/- 0.1,
r' = 19.5 +/- 0.1,
i' = 19.4 +/- 0.1,
z' = 19.3 +/- 0.1,
J  = 18.9 +/- 0.1,
H  = 19.0 +/- 0.2, and
K  > 18.9.

At present we cannot decide if the source is fading.

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) = 0.09 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140919A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16837
SUBJECT: GRB 140919A: Swift/UVOT Detection
DATE:    14/09/20 11:53:48 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and M.E. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140919A
3125 s after the BAT trigger (Gropp et al., GCN Circ. 16831).
A fading source consistent with the optical and enhanced XRT position
(Schmidl et al. GCN Circ. 16836; Beardmore et al., GCN Circ 16834)
is detected in the initial UVOT exposures. Initial identification 
was complicated by the presence of a point source in the 
DSS close to the optical position. Photometry is therefore also 
complicated by the presence of this point source. 

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(FC)         3125         3275          147         16.62 +/- 0.05
white            45180        45480          295         19.40 +/- 0.11
v                 4848         5047          197         17.33 +/- 0.10
b                 8834         9134          295         18.34 +/- 0.09
u                 5462         5613          148         16.86 +/- 0.07
w1                5258         5458          197         16.98 +/- 0.09
m2                5052         5252          197         17.12 +/- 0.11

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: GRB140919A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16838
SUBJECT: GRB 140919A: Swift-XRT refined Analysis
DATE:    14/09/20 15:19:03 GMT
FROM:    Matthew Gropp at PSU/Swift  <mgropp742@gmail.com>

M.E. Gropp (PSU) reports on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 140919A (Gropp  et al. GCN
Circ. 16831),  from 3.1 ks to 57.4 ks after the  BAT trigger. The data
comprise 99 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. 16834).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.00 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.05 (+/-0.10). The
best-fitting absorption column is  1.54 (+0.30, -0.29) x 10^21 cm^-2,
in excess of the Galactic value of 7.6 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.54 (+0.30, -0.29) x 10^21 cm^-2
Galactic foreground: 7.6 x 10^20 cm^-2
Excess significance: 4.5 sigma
Photon index:      2.05 (+/-0.10)

If the light curve continues to decay with a power-law decay index of
1.00, the count rate at T+24 hours will be 0.061 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-12 (2.7 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/00613160.

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


GRB_name: GRB140919A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16839
SUBJECT: GRB 140919A, Swift-BAT refined analysis
DATE:    14/09/20 21:03:58 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), M.E. Gropp (PSU),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC),
(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 140919A (trigger #613160)
(Gropp, et al., GCN Circ. 16831).  The BAT ground-calculated position is
RA, Dec = 221.540, -32.153 deg which is
  RA(J2000)  =  14h 46m 09.5s
  Dec(J2000) = -32d 09' 11.5"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 14%.

The mask-weighted light curve shows a multi-peaked structure starts at ~ T-1 s and
ends at ~T+175 s. The structure includes roughly three peaks at ~T+3 s, ~T+40 s,
and ~T+90 s, respectively. T90 (15-350 keV) is 151.3 +- 25.6 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.7 to T+174.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.74 +- 0.12.  The fluence in the 15-150 keV band is 5.9 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+38.97 sec in the 15-150 keV band
is 2.0 +- 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/613160/BA/


GRB_name: GRB140927A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16842
SUBJECT: GRB 140927A: Swift detection of a burst
DATE:    14/09/27 05:35:42 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

R. L. C. Starling (U Leicester), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (NASA/GSFC), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and
T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 05:15:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140927A (trigger=613775).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 291.845, -65.388 which is 
   RA(J2000) = 19h 27m 23s
   Dec(J2000) = -65d 23' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a spiky
structure with a duration of about 30 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 05:17:13.7 UT, 122.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 291.79216, -65.39285 which is
equivalent to:
   RA(J2000)  = 19h 27m 10.12s
   Dec(J2000) = -65d 23' 34.3"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 81 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 (7.56 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4
(+3.21/-2.72) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
123 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
0.08. 

Burst Advocate for this burst is R. L. C. Starling (rlcs1 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: GRB140927A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16843
SUBJECT: GRB 140927A: Enhanced Swift-XRT position
DATE:    14/09/27 15:09:54 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 2980 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140927A, 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 = 291.79158, -65.39357 which is equivalent
to:

RA (J2000): 19h 27m 9.98s
Dec (J2000): -65d 23' 36.9"

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: GRB140927A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16844
SUBJECT: GRB 140927A: Swift-XRT refined Analysis
DATE:    14/09/27 17:35:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (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), M. de Pasquale
(INAF-IASFPA) and R.L.C. Starling report on behalf of the Swift-XRT
team:

We have analysed 7.1 ks of XRT data for GRB 140927A (Starling  et al.
GCN Circ. 16842),  from 108 s to 29.7 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 Evans et al. (GCN Circ.
16843).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.76 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.79 (+0.25, -0.23). The
best-fitting absorption column is  1.6 (+1.0, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 7.6 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.9 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+1.0, -0.8) x 10^21 cm^-2
Galactic foreground: 7.6 x 10^20 cm^-2
Excess significance: 1.7 sigma
Photon index:      1.79 (+0.25, -0.23)

If the light curve continues to decay with a power-law decay index of
0.76, the count rate at T+24 hours will be 4.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-13 (2.3 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/00613775.

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


GRB_name: GRB140927A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16845
SUBJECT: GRB 140927A: Swift-BAT refined analysis
DATE:    14/09/27 21:49:44 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@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 (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), R. L. C. Starling (U Leicester)
J. Tueller (GSFC), T. N. Ukwatta (LANL) (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 140927A (trigger #613775)
(Starling, et al., GCN Circ. 16842).  The BAT ground-calculated position is
RA, Dec = 291.802, -65.400 deg which is
  RA(J2000)  =  19h 27m 12.5s
  Dec(J2000) = -65d 23' 58.4"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 54%.

The mask-weighted light curve shows a multi-peaked structure starts at ~ T0 and
ends at ~ T+9 s. The structure has roughly two main peaks, at ~ T+3.8 s and ~ T+7.7 s,
respectively. T90 (15-350 keV) is 6.26 +- 1.43 sec (estimated error including systematics).

The time-averaged spectrum from T+0.43 to T+8.70 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.82 +- 0.30.  The fluence in the 15-150 keV band is 2.7 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+7.70 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/613775/BA/


GRB_name: GRB140927A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16846
SUBJECT: GRB 140927A: Swift-UVOT analysis
DATE:    14/09/27 22:34:48 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. Swenson (PSU) and R. L. C. Starling (U Leicester) report on
behalf of the Swift UVOT team:

Analysis of the field of GRB 140927A shows a bright DSS source
located at RA, DEC= 291.79237,-65.39323, which is 1.7" from the
enhanced XRT position (Evans et al., GCN Circ. 16843). No elongation
or fading of the known source is observed in the first 10e4 seconds
of UVOT observations, meaning that any potential afterglow contribution
is being overpowered by the known source.


GRB_name: GRB140928A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16847
SUBJECT: GRB 140928A: Fermi-LAT detection
DATE:    14/09/28 21:32:01 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

R. Desiante (Udine University & INFN Trieste), E. Bissaldi (University & INFN Trieste), D. Kocevski (NASA/GSFC), J.  L. Racusin (NASA/GSFC),
F. Longo (University & INFN Trieste) and M. Arimoto (Tokyo Tech) report on behalf of the Fermi-LAT team:

At 10:29:53.55 on September 28, 2014, Fermi-GBM (trigger 433592996/140928437) triggered on GRB 140928A, which entered the Fermi-LAT 
field of view at T0+1550 s, and was observed until T0+3200 s, during which the LAT detected high-energy emission.

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

RA, Dec = 43.81 , -56.08 (J2000)

with an error radius of 0.16 deg (90% containment, statistical error only). This was 110 deg from the LAT boresight at the time of the trigger.

The data from the Fermi-LAT show a significant increase in the event rate at a position consistent with the GBM localization.

More than 20 photons above 100 MeV are observed from 1550 s (when the GRB entered the LAT FOV) to 3200s (when the spacecraft entered 
the SAA) after the GBM trigger. 

The highest-energy photon is a 35 GeV event which is observed 3100 seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Makoto Arimoto (arimoto@hp.phys.titech.ac.jp).

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: GRB140928A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16848
SUBJECT: GRB 140928A: Swift-XRT observations
DATE:    14/09/29 08:35:47 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

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

We have analysed 2.5 ks of XRT data for the Fermi/LAT-detected burst:
GRB 140928A (Desiante et al.,  GCN Circ. 16847) from 40.7 ks to 52.7 ks
after the  Fermi/LAT trigger. The data are entirely in Photon Counting
(PC) mode.  An X-ray source is detected within the Fermi/LAT error
circle. Using 2472 s of PC mode data and 2 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 = 43.69878, -55.92883
which is equivalent to:

RA (J2000): 02h 54m 47.71s
Dec(J2000): -55d 55' 43.8"

with an uncertainty of 1.5 arcsec (radius, 90% confidence). This
position is 588 arcsec from the Fermi/LAT position.  The light curve is
consistent with a constant source of mean count rate 1.9e-01 ct/sec. 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.83 (+0.26, -0.24). The
best-fitting absorption column is  2.4 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 4.2 sigma
Photon index:      1.83 (+0.26, -0.24)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020418.

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


GRB_name: GRB140928A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16849
SUBJECT: GRB 140928A: GROND Afterglow Candidate
DATE:    14/09/29 09:43:28 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of the Fermi LAT-detected GRB 140928A (Fermi GBM
trigger 433592996; Desiante et al., GCN #16847) simultaneously in
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the
2.2m MPG telescope at ESO La Silla Observatory (Chile).

Observations started at 08:43.51 UT on 2014-09-29, 22.23 hrs after the GRB
trigger. They were performed at an average seeing of 1".5 and at an
average airmass of 1.2.

We detect a source inside the enhanced 1".5 Swift-XRT error circle (Pagani
et al., GCN #16848), at

RA  (J2000) =  02:54:47.72
DEC (J2000) = -55:55:44.0

with an uncertainty of 0".5 in each coordinate.

Based on total exposures of 460 s in g'r'i'z' and 480 s in JHK, we measure
the following preliminary magnitudes and upper limits (AB magnitude
system):

g' = 21.3 +/- 0.1,
r' = 20.8 +/- 0.1,
i' = 20.7 +/- 0.1,
z' = 20.4 +/- 0.1,
J  = 20.2 +/- 0.2,
H  = 20.1 +/- 0.2, and
K  > 18.8.

We propose this source to be the optical/NIR afterglow of GRB 140928A. At
present we cannot decide if the source is fading.

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) = 0.01 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140928A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16850
SUBJECT: GRB 140928A: Fermi GBM detection
DATE:    14/09/29 11:18:44 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 10:29:53.55 UT on 28 September 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140928A (trigger 433592996  / 140928437) which 
was also detected by Fermi/LAT (Desiante et al. 2014, GCN 16847) and Swift
(Pagani et al. 2014, GCN 16848). The GBM on-ground location is consistent 
with the LAT/Swift position.

The angle from the Fermi LAT boresight is 110 degrees.

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

The GBM light curve shows a structured pulse 
with a duration (T90) of about 14 s (50-300 keV).
The time-averaged spectrum from T0-3.072 s to T0+8.192 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.12 +/- 0.13  and
the cutoff energy, parameterized as Epeak, is 732 +/- 72 keV.

The event fluence (10-1000 keV) in this time interval is
1.02 +/- 0.04)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+5.12  s in the 10-1000 keV band
is 4.8 +/- 0.3 ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 671 +/- 82 keV, 
alpha = -0.05 (+0.16/-0.13) and beta = -2.6 (+0.3/-0.4).

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


GRB_name: GRB140928A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16851
SUBJECT: GRB 140928A: LCO-Cerro Tololo observations
DATE:    14/09/29 13:27:52 GMT
FROM:    Drejc Kopac at Math Phys U,Slovenia  <drejc.kopac@fmf.uni-lj.si>

D. Kopac (LJMU), C. Guidorzi (U. Ferrara), C. Mundell (LJMU), on behalf 
of a large collaboration report:

Using the Las Cumbres Observatory Global Telescope Network (LCOGTN) 1-m 
telescope in Cerro Tololo (Chile), we began observing Fermi GRB 140928A, 
which was detected also by the Fermi/LAT (Desiante et al., GCN 16847). 
Optical observations in r' and i' filters (5 x 120s sequences) started 
on September 29 at 05:16:17 UT, i.e. ~18.8 hours after the Fermi/GBM 
trigger.

At the position consistent with the XRT position (Pagani et al., GCN 
16848) and with the GROND position (Varela et al., GCN 16849) we detect 
an un-catalogued source with a preliminary magnitude of R = 20.1 +/- 0.2 
at t_mid = 18.9 hours since the Fermi/GBM trigger time. The magnitude is 
calibrated against nearby USNO-B1 stars.


GRB_name: GRB140928A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16852
SUBJECT: IPN Triangulation of GRB 140928A
DATE:    14/09/29 17:12:11 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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,

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, 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:

The long-duration GRB 140928A (Desiante et al., GCN Circ. 16847) has 
been observed by Fermi (GRB trigger 433592996; von Kienlin et al., GCN 
Circ. 16850), Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), and 
Swift (BAT), so far, at about 37794 s UT (10:29:54). The burst was 
outside the coded field of view of the BAT.

We have triangulated it to a Konus-GBM annulus centered at 
RA(2000)=14.055 deg (00h 56m 13s) Dec(2000)=+2.376 deg (+2d 22' 33"), 
whose radius is 63.085 +/- 0.902 deg (3 sigma) and to a  Konus-MESSENGER 
annulus centered at RA(2000)=26.945 deg (01h 47m 47s) Dec(2000)=+14.819 
deg (+14d 49' 08"), whose radius is 72.142 +/- 0.121 deg (3 sigma).

The Swift (XRT) source (Pagani et al., GCN Circ. 16848) is inside the 
annuli, at the distance between the source and the central line of the 
Konus-MESSENGER annulus of 17 arcsec.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140928_T37793/IPN/

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


GRB_name: GRB140928A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16853
SUBJECT: GRB 140928A: LCO-Cerro Tololo further observations
DATE:    14/09/30 10:36:59 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), D. Kopac, C. Mundell (LJMU),
S. Dichiara (U. Ferrara) on behalf  of a large collaboration report:

Using the Las Cumbres Observatory Global Telescope Network (LCOGTN) 1-m
telescope in Cerro Tololo (Chile), we re-observed Fermi GRB 140928A
(Desiante et al., GCN 16847; von Kienlin and Meegan GCN 16850)
in the r' filter starting on September 30, 07:14:36 UT, i.e. ~1.86
days after the Fermi trigger time.

The optical afterglow (Varela et al., GCN 16849; Kopac et al. GCN 16851)
is still clearly detected with R = 21.2 +/- 0.1 mag at a mid time
of 1.88 days post burst (total exposure of 1680 s).
The magnitude is calibrated against nearby USNO-B1 stars.

A comparison with our previous report (Kopac et al.) suggests an
average power-law decay index alpha = 1.2 +- 0.2.


GRB_name: GRB140928A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16854
SUBJECT: Konus-Wind observation of GRB 140928A
DATE:    14/09/30 15:33:47 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration, intense GRB 140928A (Fermi-LAT detection: Desiante et 
al., GCN 16847;
Fermi-GBM detection: von Kienlin and Meegan, GCN 16850;
IPN triangulation: Hurley et al., GCN 16852)
triggered Konus-Wind at T0=37793.602 s UT (10:29:53.602).

The burst light curve shows two emission episodes with a total duration 
of ~69 s.
The first emission episode lasts from ~T0-6 s to ~T0+15 s
and the second episode lasts from ~T0+42 s to ~T0+63 s
(Fermi-GBM missed the second episode probably due to the Earth occultation).
The IPN data confirm the second episode belongs to the same GRB.
The emission is seen up to ~15 MeV.

As observed by Konus-Wind, the burst
had a fluence of 8.6(-1.4,+1.3)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+9.248 s,
of 1.7(-0.3,+0.3)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+57.856 s)
is best fit in the 20 keV - 10 MeV range
by a GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.17(-0.09,+0.12),
the high energy photon index beta = -2.09(-0.32,+0.16),
the peak energy Ep = 304(-66,+80) keV,
chi2 = 73/84 dof.

The spectrum near the peak count rate
(measured from T0+6.912 to T0+16.896 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.11(-0.08,+0.09),
the high energy photon index beta = -2.27(-0.34,+0.17),
the peak energy Ep = 318(-46,+59) keV,
chi2 = 84/93 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140928_T37793/

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


GRB_name: GRB140930A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16855
SUBJECT: GRB 140930A/MAXI J2259+524: MAXI-GSC detection
DATE:    14/09/30 17:27:16 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

H. Negoro (Nihon U.), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), 
T. Mihara, M. Sugizaki, M. Morii, M. Serino, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), 
N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, D. Uchida (Osaka U.), 
M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, A. Kawagoe (Chuo U.), 
M. Yamauchi, Y. Morooka (Miyazaki U.), 
K. Yamaoka (Nagoya U.) ,
report on behalf of the MAXI team:

A bright uncatalogued X-ray transient source was detected with MAXI/GSC 
at UT 2014-09-30T14:26. Assuming that the source flux was constant over 
the transit, we obtain the source position at

(R.A., Dec) = (344.875 deg, 52.428 deg) = (22 59 30, +52 25 40) (J2000), 
equivalently (l, b) = (106.186 deg, -6.766 deg), 

with a 90% C.L. statistical error of 0.40 deg and an additional systematic 
uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 136 +- 30 mCrab (4-10 keV, 
1 sigma error). There was no significant excess flux in the previous transit 
at UT 2014-09-30T12:54.

The nature of the source is quite unknown. Since the source is located 
near the Galactic plane (l ~ -6.8 deg), this event might be an X-ray burst 
from a low mass X-ray binary near the Galactic plane. We tentatively name 
the source GRB 140930A and MAXI J2259+524 (originally, MAXI J2256+527
in the MAXI ML. "New-transient: 115").


GRB_name: GRB140928A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16856
SUBJECT: GRB140928A: Gemini-South observation
DATE:    14/09/30 17:27:54 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

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

"On September 30.18 UT (1.75 days after the burst) we observed the field 
of the Fermi/LAT GRB 140928A (Desiante et al. GCN 16847, Varela et al. 
GCN 16849) with the Gemini-South telescope equipped with the GMOS 
spectrograph. We obtain 2x1200s exposure under non optimal conditions 
(1.5-2 arcseconds seeing) with the R400 grating, covering the 6000-10000 
Angstrom wavelength range.

We detect a featureless continuum down to 6000A, no features are 
detected neither in emission nor in absorption.

We thank Cristiano Guidorzi for providing a finding chart and the Gemini 
staff for carry out this observations."


GRB_name: GRB140930B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16857
SUBJECT: GRB 140930B: Swift detection of a short burst
DATE:    14/09/30 19:56:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. De Pasquale (INAF-IASFPA), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
C. B. Markwardt (NASA/GSFC), A. Maselli (INAF-IASFPA),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 19:41:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140930B (trigger=614094).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 6.355, +24.275, which is 
   RA(J2000)  =  00h 25m 25s
   Dec(J2000) = +24d 16' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 2 sec.  The peak count rate
was ~11,000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 19:44:58.9 UT, 196.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 6.34833, 24.29681 which is
equivalent to:
   RA(J2000)  = 00h 25m 23.60s
   Dec(J2000) = +24d 17' 48.5"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 81 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 (3.45 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.8
(+3.58/-3.02) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 201 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
0.03. 

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


GRB_name: GRB140930B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16858
SUBJECT: GRB 140930B: MASTER early optical observations 
DATE:    14/09/30 20:01:31 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya,  V.Kornilov, D.Kuvshinov, 
N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, 
D.Denisenko, A.Sankovich
Lomonosov Moscow State University,
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, A. Gabovich
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 Blagoveschensk was pointed to the  GRB140930B 21 sec after 
notice time and 39 sec after trigger time at 2014-09-30 19:42:21 UT in two 
polarizations. On our first (10s exposure)  set we haven't found optical 
transient  within SWIFT error-box (ra=00 25 25 dec=+24 16 28 r=0.050000).
The 5-sigma upper limit has been about 16.0 mag


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB140930B 36 sec after notice 
time and 54 sec after trigger time at 2014-09-30 19:42:36 UT  in two 
polarizations. On our first (10s exposure)  set we haven't found optical 
transient  within SWIFT error-box (ra=00 25 25 dec=+24 16 27 r=0.050000).
The 5-sigma upper limit has been about 15.5 mag

The observations on both observatories is continued.


GRB_name: GRB140930B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16859
SUBJECT: GRB 140930B: Prompt enhanced Swift-XRT position
DATE:    14/09/30 20:39:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 140930B, we find an
enhanced XRT position of the afterglow: RA, Dec: 6.3478, 24.2948 which
is equivalent to:
   RA (J2000)  = 00 25 23.46
   Dec (J2000) = +24 17 41.3
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/614094.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB140930B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16860
SUBJECT: GRB 140930B: 1.23m CAHA optical observations
DATE:    14/09/30 22:49:49 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), S. Mottola (DLR), on
behalf of a larger collaboration report:

We observed the GRB 140930B (De Pasquale GCN 16857) field with the 1.23m
CAHA telescope. The observations were carried out in the R-band on Sep
30.82728-30.86076 UT (9.6-57.8 minutes post GRB). A very preliminary
analysis does not reveal any optical source consistent with the enhanced
XRT position (Evans et al. GCN 16859) brighter than R(Vega)~21, calibrated
against the USNO B1.0 catalog. A further analysis is ongoing.


GRB_name: GRB140930B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16861
SUBJECT: GRB 140930B: WHT detection of candidate afterglow
DATE:    14/10/01 00:03:34 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick) and
M. Fraser (IoA, U. Cambridge) report:

We observed the position of GRB 140930B (De Pasquale et al.
GCN 16857) with ACAM on the WHT.  Observations began at
22:40 UT, approximately 3.0 hr post burst.

We detect a faint point source consistent with the
revised X-ray position (Evans et al. GCN 16859) with
a magnitude r~21.8 and position 00:25:23.45 +24:17:39.0
(provisional calibration).  We note that no source is visible at 
this location in the SDSS observations of the field and therefore 
suggest it is likely to be the afterglow of this burst.


GRB_name: GRB140930B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16862
SUBJECT: GRB 140930B: ISON-Kislovodsk observations
DATE:    14/10/01 00:47:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

K. Polyakov (ISON), A. Pozanenko (IKI), A. Volnova (IKI),  I. Molotov 
(KIAM), report on  behalf of larger collaboration:

We observed the field of  GRB 140930B (De Pasquale et al., GCN 16857) 
with Santel-400AN   telescope of ISON-Kislovodsk observatory starting on 
Sep. 30 (UT) 19:52:24, i.e. ~10.5 minutes after burst trigger. We took 
30 unfiltered images of 120 s exposure. In the enhanced XRT position 
(Evans et al. GCN 16859) we do not detect the optical candidate (Tanvir 
et al., GCN 16861). A preliminary upper limit of the first image is 
19.5m (at mid time (UT) 19:53:24) and is based on nearby USNO-B1.0 
stars, R2 magnitudes.


GRB_name: GRB140930B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16863
SUBJECT: GRB 140930B: MMT confirmation of the optical afterglow
DATE:    14/10/01 06:47:14 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong (U. Arizona), M. Calkins (SAO), and E. Berger (Harvard) report:

"We observed the location of the short-duration GRB 140930B (De Pasquale et
al., GCN 16857) with MMTCam mounted on the 6.5-m MMT starting on 2014 Oct
1.144 UT (7.76 hr post-burst). We obtained 4x300-sec of r-band observations
in 1" seeing. We detect a source at the position of the candidate optical
afterglow (Tanvir et al., GCN 16861) with a magnitude of r~24.0 +/- 0.2
(calibrated to SDSS), indicating that the source faded by ~2.2 mag between
3.0 hr and 7.8 hr post-burst. The fading confirms that this source is the
optical afterglow of GRB 140930B. Assuming a single power-law decline
between these two epochs, the decay index is alpha~-2.1.

We thank Nelson Caldwell for the rapid scheduling of these observations."


GRB_name: GRB140928A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16864
SUBJECT: GRB 140928A: MAXI-GSC detection
DATE:    14/10/01 09:35:35 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

M. Morii, M. Serino (RIKEN), M. Nakajima, H. Negoro (Nihon U.),
S. Nakahira, S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, D. Uchida (Osaka U.),
K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, A. Kawagoe (Chuo U.),
M. Yamauchi, Y. Morooka (Miyazaki U.),
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

MAXI/GSC observed the field of GRB 140928A at a scan transit centered 
at 2014-09-28 10:41:09 UT with a triangular response of 123-s duration.
This center time is 675 sec after the Fermi/GBM trigger time (2014-09-28 10:29:53.55 UT, GCN  #16850).
The source was located on the edge of the FoV where the source PSF was only partially covered in the    sensitive region of the GSC.
We therefore estimated the flux using PSF fitting of the photon image.
We marginally detected the afterglow of this GRB with
29 +17/-14 mCrab (4-10 keV) and 13 +11/-8  mCrab (2-4 keV) (1 sigma errors).
Here, we assumed the source constancy during the scan transit.
We did not detect this source at the previous scan (centered at 09:08:25 UT)
and the following scan (centered at 12:13:46 UT), with upper limits of 14 mCrab and 35 mCrab (90% C.L., 4-10 keV),
respectively.


GRB_name: GRB140930B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16865
SUBJECT: GRB 140930B: Enhanced Swift-XRT position
DATE:    14/10/01 10:28:53 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 1478 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140930B, 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 = 6.34767, +24.29398 which is equivalent
to:

RA (J2000): 00h 25m 23.44s
Dec (J2000): +24d 17' 38.3"

with an uncertainty of 2.3 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: GRB140930B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16866
SUBJECT: GRB 140930B: Swift-XRT refined Analysis
DATE:    14/10/01 10:56:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.5 ks of XRT data for GRB 140930B (De Pasquale  et
al. GCN Circ. 16857),  from 182 s to 14.3 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 Goad et al. (GCN
Circ. 16859).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.13 (+0.21, -0.19). At T+952 s  the decay
flattens to an alpha of 0.95 (+0.23, -0.47) before breaking again at
T+6412 s to a final decay with index alpha=3.3 (+2.3, -1.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.71 (+0.16, -0.15). The
best-fitting absorption column is  6.0 (+4.3, -2.6) x 10^20 cm^-2,
consistent with the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.8 x 10^-11 (4.2 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.0 (+4.3, -2.6) x 10^20 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.71 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
3.3, the count rate at T+24 hours will be 5.8 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x
10^-16 (2.4 x 10^-16) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00614094.

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


GRB_name: GRB140930B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16867
SUBJECT: GRB 140930B: Keck NIR imaging
DATE:    14/10/01 11:07:31 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley and J. Jencson (Caltech) report:

We imaged the location of short-duration GRB 140930B (De Pasquale et 
al., GCN 16857) using the Multi-Object Spectrometer for Infrared 
Exploration (MOSFIRE) on the Keck I 10 meter telescope between 08:44 and 
09:04 on 2014-10-01 (UT).   We acquired 9 x 35-second exposures in 
Ks-band and 9 x 44-second exposures in J-band.   A faint point-like 
source is detected at RA=00:25:23.433, dec=+24:17:39.41 (J2000), a 
location consistent with the afterglow locations previously reported by 
Evans et al. (GCN 16865) and Tanvir et al. (GCN 16861).  Photometry 
relative to 2MASS gives approximate magnitudes (Vega) of:

  J = 22.2 +/- 0.2    (tmid = 13.31 hr)
  Ks = 20.8 +/- 0.3   (tmid = 13.12 hr)

We thank M. Kasliwal and T. Prince for the observing time.


GRB_name: GRB140930B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16868
SUBJECT: Konus-Wind observation of GRB 140930B
DATE:    14/10/01 13:06:20 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A short-duration, hard-spectrum GRB 140930B (Swift-BAT detection: 
Pasquale et al., GCN 16857) triggered Konus-Wind at T0=70907.149 s UT 
(19:41:47.149).

The burst light curve shows a single pulse with a duration of ~1.0 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140930_T70907/

As observed by Konus-Wind, the burst
had a fluence of 8.1(-2.5,+5.1)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.010 s,
of 3.4(-1.1,+2.3)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.6 (-0.5,+0.6)
and Ep = 1302 (-459,+2009) keV (chi2 = 99/92 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.6
(chi2 = 98/91 dof)

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


GRB_name: GRB140930B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16869
SUBJECT: GRB 140930B: Swift/UVOT Upper Limits
DATE:    14/10/01 13:22:17 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 140930B 
201s after the BAT trigger (De Pasquale et al., GCN Circ. 16857).
No optical afterglow consistent with the XRT position (Goad et al., GCN 
Circ. 16865) or the optical position (Tanvir et al., GCN Circ. 16861) 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           201          351          147         >20.2
white              201         2579          528         >20.9
v                  507         2629          253         >18.8
b                  433         2787          311         >19.9
u                  407         2702          253         >19.4
w1                 383         2678          253         >19.4
m2                 358         2653          214         >19.3
w2                 483         2605          253         >19.7

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: GRB140930B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16870
SUBJECT: GRB 140930B Swift-BAT refined analysis
DATE:    14/10/01 13:28:23 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

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

Using the data set from T-61 to T+174 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140930B (trigger #614094)
(De Pasquale, et al., GCN Circ. 16857).  The BAT ground-calculated position is
RA, Dec = 6.360, 24.298 deg which is
    RA(J2000)  =  00h 25m 26.4s
    Dec(J2000) = +24d 17' 53.3"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 24%.

The mask-weighted light curve shows a single FRED-like peak with structure,
beginning at ~T-0.1 sec, peaking at T+0 sec and decaying to background by
T+1.0 sec.   There is no clear sign of extended emission.
T90 (15-350 keV) is 0.84 +- 0.12 sec (estimated error including systematics).

The time-averaged spectrum from T-0.10 to T+0.86 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.64 +- 0.19.  The fluence in the 15-150 keV band is 4.2 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band
is 4.0 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.   The position of GRB 140930B in the BAT hardness-duration diagram places
it clearly in the short hard burst part of the diagram.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/614094/BA/


GRB_name: GRB140630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16871
SUBJECT: GRB 140930A/MAXI J2259+524: MASTER  optical observations 
DATE:    14/10/01 14:59:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya,  V.Kornilov, D.Kuvshinov, N.Tyurina, 
N.Shatskiy, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Denisenko, 
Lomonosov Moscow State University,
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, A. Gabovich
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)



Three MASTER system telescopes (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveshchensk, Tunka and Kislovodsk have observed GRB140630A 
(Negoro et. al GCN 16855).

MASTER II  robotic telescope located in Blagoveschensk was pointed to the 
GRB140930A 21 sec after notice time and 6331 sec after trigger time at 
2014-09-30 16:12:34 UT in two polarizations. On our single and coadd 
images we  not found credible optical transient within MAXI error-box 
(Negoro et. al GCN 16855). The 5-sigma upper limit on single (180 s) 
images has been about 18.1 mag. The 5-sigma upper limit on coadd of 13 
image with total exposure 2340 s is about 19.5m

MASTER II  robotic telescope located in Kislovodsk was pointed to the 
GRB140930A 22 sec after notice time and 6332 sec after trigger time at 
2014-09-30 16:12:35 UT in two polarizations. On our single and coadd 
images we not found credible optical transient within MAXI error-box. The 
5-sigma upper limit on single (180 s) images has been about 18.5 mag. The 
5-sigma upper limit on coadd of first 12 image with total exposure 2160 s 
is about 20.5m

MASTER II  robotic telescope  located in Tunka was pointed to the 
GRB140930A 93 sec after notice time and 6415 sec after trigger time at 
2014-09-30 16:13:58 UT in two polarizations. On our single and coadd 
images we not found credible optical transient within MAXI error-box. The 
5-sigma upper limit on single (180 s) images has been about 17.9 mag. The 
5-sigma upper limit on coadd of 13 image with total exposure 2340 s is 
about 20.0 m

The upper limits received by MASTER are given in the table below:

t_start      | t-t_mid     | exptime | filt | lim  | site | coadd
-------------+-------------+---------+------+------+------+-------
16:12:35.693 | 6485 sec    |     180 | P    | 18.5 | K    |     1
16:12:35.693 | 6485 sec    |     540 | P    | 19.5 | K    |     3
16:19:43.551 | 8075 sec    |    2160 | C    |~20.5 | K    |    12
16:12:34.498 | 6484 sec    |     180 | P    | 18.1 | B    |     1
17:20:44.913 | 12010 sec   |    2520 | C    | 19.5 | B    |    14
16:13:58.211 | 6568 sec    |     180 | P    | 17.9 | T    |     1
16:32:51.181 | 9877 sec    |    2340 | C    |~20.0 | T    |    13

Our white (clear) band is well described by a parity 0.8R+0.2B (USNO B1).


The MASTER-NET coverage map available here:
http://master.sai.msu.ru/static/GRB/GRB140930A/GRB140930A_cm.png

The MASTER image of MAXI error box with upper limit ~20m available here 
(10Mb):
http://master.sai.msu.ru/static/GRB/GRB140930A/GRB140930A_img.jpeg

The message may be cited.


GRB_name: GRB140930B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16872
SUBJECT: GRB 140930B: GROND observations
DATE:    14/10/01 20:16:18 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

J. Graham (MPE Garching), A. Nicuesa Guelbenzu (TLS Tautenburg), J. Bolmer 
and J. Greiner (both at MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140930B (Swift trigger 614094; De Pasquale et 
al., GCN #16857) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at La Silla 
Observatory (Chile).

Observations started at 02:25 UT on 1 October 2014, around 7 hours after 
the GRB trigger. They were performed at an average seeing of 1.4" and at 
an average airmass of 1.9.

We detect the afterglow candidate reported by Tanvir et al. (GCN #16861) 
and confirmed by Fong et al. (GCN #16863). At a midtime of 03:00 UT we 
measure a preliminary AB magnitude of

r' = 23.2 +/- 0.2 mag.

The analysis of the other GROND photometric bands is still on-going. We 
note that the photometry is slightly affected by a bright star next to the 
afterglow.

The given magnitude is calibrated against SDSS field stars and not 
corrected for the expected Galactic foreground extinction corresponding to 
a reddening of E_(B-V)=0.04 mag in the direction of the burst (Schlegel et 
al. 1998).


GRB_name: GRB140930B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16873
SUBJECT: GRB 140930B: Gemini South Spectroscopy
DATE:    14/10/02 02:11:11 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko, A. Cucchiara (NASA/GSFC), N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), and D. A. Perley (Caltech) report on behalf of a larger collaboration:

We obtained a spectrum of the optical afterglow (Tanvir et al., GCN 16861; Fong et al., GCN 16863) of the short GRB 130930B (De Pasquale et al., GCN 16857) with the Gemini Multi-Object Spectrograph mounted on the 8 m Gemini South telescope.  Observations began at 4:01 UT on 2014 October 1 (8.3 hr after the Swift trigger) and cover the wavelength range from 3700-8300 A.

We detect a weak continuum trace at the location of the afterglow over most of the observed wavelength range (lambda >~ 4000 A), but no obvious emission or absorption features.


GRB_name: GRB140930B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16875
SUBJECT: GRB 140930B: MASTER early possible OT detection
DATE:    14/10/02 06:41:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya,  V.Kornilov, D.Kuvshinov, N.Tyurina, 
P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Denisenko
Lomonosov Moscow State University,
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, A. Gabovich
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)


Two MASTER II twin  robotic telescope (MASTER-Net: 
http://observ.pereplet.ru)  located in  Blagoveschensk  and Kislovodsk was 
pointed to the  GRB140930B (Pasquale et. al GCN 16857) 21 and 36 sec after
notice time and  39 and 54 sec after trigger time respectively.

So we have 4 first images in four different polarization started after 21 
sec (Blagoveschensk) and 36 sec (Kislovodsk) with 10 sec exposure.
We found 3-sigma OT    on one  tube image in Blagoveschensk at the
WHT  position (Tanvir et. al, GCN16861, Fong et. al. GCN16863) with m = 
16+-0.5 mag. The OT seen at one first image only.
The image with OT is available at 
http://master.sai.msu.ru/static/GRB/GRB140930B_MASTER_OT.png

We do not see OT (Tanvir et. al GCN16857, Fong et. al. GCN16857) on three
tube images on single and coadd images.
The analysis strongly is complicated by presence of very bright star (USNO 
B1 1142-0005722 ~14m) close to OT position. 
The upper limits received by MASTER are given in the table below:


t_start      | t-t_mid    | exptime | filt | lim  | site | coadd
--------------------------+---------+------+------+------+-------
19:42:21.909 | 44 sec     |      10 | P/   | 16.4 | A    |     1
19:42:21.909 | 44 sec     |      10 | P\   | 15.7 | A    |     1*
19:42:36.837 | 59 sec     |      10 | P|   | 15.6 | K    |     1
19:42:36.837 | 59 sec     |      10 | P-   | 16.0 | K    |     1
19:42:21.909 | 70 sec     |      40 | P/   | 17.3 | A    |     3
19:42:36.837 | 98 sec     |      50 | P-   | 16.9 | K    |     3
19:42:21.909 | 130 sec    |     130 | P/   | 18.5 | A    |     6
19:44:26.834 | 243 sec    |     120 | P-   | 18.0 | K    |     3
19:42:36.837 | 188 sec    |     170 | P-   | 18.6 | K    |     6
19:42:36.837 | 692 sec    |    1060 | P-   | 19.9 | K    |    13
19:42:21.909 | 698 sec    |    1160 | P/   | 19.7 | A    |    14
20:29:14.938 | 6120 sec   |    5400 | C    |~21.5 | K    |    30

* possible OT

C is  our white (clear) band which is well described by a parity 0.8R+0.2B (USNO B1).

P/ and P\ is a polarization filter which are oriented at an angle 45 and 
135 degrees to RA axis respectivel. P- and P| is a polarization filter 
which are oriented at an angle 0 and 90 degrees to RA axis respectivel.

This message may be cited.


GRB_name: GRB140928A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16876
SUBJECT: GRB 140928A: Swift-XRT follow-up observations
DATE:    14/10/02 09:00:09 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) reports on behalf of the Swift team:

A second epoch of XRT data was collected on the field of the 
Fermi/LAT-detected burst: GRB 140928A (Desiante et al., GCN Circ. 16847) 
from 271 ks to 296 ks after the  Swift/BAT trigger.

The X-ray source reported in GCN Circ. 16848, Pagani et al., coincident 
with the optical source reported in GCN Circ. 16849, Varela et al., GCN 
Circ. 16851, Kopac et al., and GCN Circ. 16856, Cucchiara et al., 
measured during the first epoch of XRT observations at a mean count rate 
of 1.9 x 10^-1 count s^-1 has now faded to a mean count rate of 9.5 x 
10^-3 count s^-1 (0.3-10 keV). We therefore confirm that this is the 
X-ray afterglow of GRB 140928A.

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


GRB_name: GRB141004A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16878
SUBJECT: GRB 141004A: Swift detection of a burst with an optical counterpart
DATE:    14/10/04 23:29:48 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
L. Izzo (URoma/ICRA), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf
of the Swift Team:

At 23:20:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141004A (trigger=614390).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 76.730, +12.833 which is 
   RA(J2000)  =  05h 06m 55s
   Dec(J2000) = +12d 49' 59"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single FRED
structure with a duration of about 8 sec.  The peak count rate
was ~17000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 23:21:54.2 UT, 59.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 76.73435, 12.81935 which is equivalent
to:
   RA(J2000)  = 05h 06m 56.24s
   Dec(J2000) = +12d 49' 09.7"
with an uncertainty of 4.3 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.  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 (3.14 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 5.3
(+5.50/-4.31) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 64 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 05:06:56.14 =  76.73391
  DEC(J2000) = +12:49:11.3  =  12.81981
with a 90%-confidence error radius of about 0.61 arc sec. This position is 2.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.39 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.32. 

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: GRB141004A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16879
SUBJECT: GRB 141004A: a long GRB detected by INTEGRAL
DATE:    14/10/05 00:20:44 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma-ray burst lasting about 10 s has been detected by IBAS in the 
IBIS/ISGRI data at 23:21:02 of October 4, 2014

The refined coordinates (J2000) are:

R.A.= 76.7496 deg
DEC.= +12.8235  deg

with an uncertainty of 2    arcmin (90% c.l.).

THis burst has also been detected by Swift (D'Elia et al. GCN 16878)

A plot of the light curve will  be posted at 
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB141004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16880
SUBJECT: GRB 141004A: 1.23m CAHA optical observations
DATE:    14/10/05 01:02:09 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), S. Mottola (DLR), on
behalf of a larger collaboration report:

We observed the GRB 141004A (D'Elia et al. GCN 16878) field with the 1.23m
CAHA telescope. The observations were done in the Ic-band starting on Oct
4.9969 UT (34.6 minutes post GRB). A preliminary analysis detects a faint
optical object located at (RA, DEC)=05:06:56.17, 12:49:10.8 (+/-0.7"), so
consistent with the UVOT position. We estimate a preliminary Vega
magnitude of Ic~19.2, calibrated against the USNO B1.0 catalog.


GRB_name: GRB141004A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16881
SUBJECT: GRB 141004A: TNG photometric and spectroscopic observations
DATE:    14/10/05 02:49:18 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (INAF/OAR & ASI/ASDC), S. Covino (INAF/OAB), M. Cecconi and  
Carmen Padilla (INAF/TNG) report on behalf of the CIBO collaboration:


We observed the optical afterglow of GRB 141004A (D'Elia et al., GCN  
16878; Mereghetti et al. GCN 16879) on 2014 October 5 with the 3.6m  
TNG telescope located in the Canary Islands, equipped with the DOLORES  
operated in both imaging and spectroscopic mode. The observations were  
carried out under good weather conditions (seeing about 1.5) at high  
airmass.

In a 180 s image started at 01:41 UT (~2.3 hr after the GRB), the  
afterglow has a magnitude r = 20.9 +/- 0.1 (AB), calibrated against  
the APASS catalog. No correction has been applied for the Galactic  
extinction. The position of the afterglow is
RA: 05:06:56.17
Dec: 12:49:10.54,
consistent with the UVOT detection (D'Elia et al. GCN 16878) and with  
the CAHA observation (Gorosabel et al., GCN 16880). We also detect a  
fainter object (possibly extended) 5" eastward to the afterglow.


We also obtained two optical spectra, each one lasting 1200 s, using  
the grism LR-B covering the wavelength range 3000 - 8000 AA. The  
observations started at 01:00 UT (~1.7 hr after the GRB). Using a  
preliminary wavelength calibration, in the co-added spectrum we detect  
a faint continuum extending down to 4000 A. No obvious absorption or  
emission features are detected in our preliminary analysis of the  
afterglow spectrum.


GRB_name: GRB141005A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16882
SUBJECT: GRB 141005A: Swift detection of a burst
DATE:    14/10/05 05:27:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), L. Izzo (URoma/ICRA),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 05:13:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141005A (trigger=614415).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 291.108, +36.069, which is 
   RA(J2000)  =  19h 24m 26s
   Dec(J2000) = +36d 04' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 5 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 05:14:39.5 UT, 92.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 291.09313, 36.09517 which
is equivalent to:
   RA(J2000)  = 19h 24m 22.35s
   Dec(J2000) = +36d 05' 42.6"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 103 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 1.56
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 250 seconds with the U 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 18.0 mag. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.17. 

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: GRB141004A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16883
SUBJECT: GRB 141004A: Enhanced Swift-XRT position
DATE:    14/10/05 06:33:18 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 2078 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 141004A, 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 = 76.73357, +12.81944 which is equivalent
to:

RA (J2000): 05h 06m 56.06s
Dec (J2000): +12d 49' 10.0"

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: GRB141005A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16884
SUBJECT: GRB 141005A: P60 probable afterglow deteaction
DATE:    14/10/05 06:53:57 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

The Palomar 60-inch robotic telescope automatically triggered on the 
Swift-BAT alert for GRB 141005A (GCN 16882, D'Elia et al.) and began 
observations of the field at 05:16:28 UT, 202 seconds after the BAT 
trigger.  A sequence of cycling 60-second r, i, and z band images were 
acquired, ending at 05:33:20 UT.

In the initial images we identify a source inside the SPER XRT error 
circle at the following position:

RA  = 19:24:22.392
dec = +36:05:42.26
(J2000, +/- 0.3")

The source is faint and probably fading, from r = 20.6 +/- 0.2 and i = 
20.0 +/- 0.2 in the initial exposures to r = 21.4 +/- 0.3 and i = 21.3 
+/- 0.4 in the final exposures.   The source is also present in archival 
imaging of the field from SDSS.  Measuring the flux of the source in the 
same aperture in these images yields magnitudes of g=21.9, r=21.6, 
i=21.3, z=20.7.

These observations suggest a faint optical afterglow superimposed on a 
host galaxy or Galactic foreground star.  More observations are 
encouraged to characterize this object.


GRB_name: GRB141005A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16885
SUBJECT: GRB 141005A: RATIR Optical Observations
DATE:    14/10/05 07:29:03 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 (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 141005A (D'Elia, et al., GCN 16882) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/10 5.22 to 2014/10 5.27 UTC (0.05
to 1.34 hours after the BAT trigger), obtaining a total of 1.07 hours
exposure in the r and i bands.

We note evidence of the source reported by P60 (Perley, et al., GCN 16884),
with marginal evidence for fading throughout the epoch of RATIR
observations.
Further analysis is ongoing.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB141004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16886
SUBJECT: GRB 141004A: Monte Agliale Observatory optical observations
DATE:    14/10/05 08:55:29 GMT
FROM:    Fabrizio Ciabattari at Monte Agliale Obs  <fabciaba@alice.it>

F. Ciabattari, S. Donati, E. Mazzoni, G. Petroni and M. Rossi (Monte Agliale Observatory, Borgo a 
Mozzano, Italy) report:

We observed the field of GRB 141004A (D'Elia et al. GCN 16878) with the automatic
0.5m f/4.6 Newtonian telescope + FLI Proline PL4710 camera at
Monte Agliale Observatory (Borgo a Mozzano, Italy, MPC code 159).
The observations started at 2014-10-04 23:25:05 UT (~ 4 minutes after the
burst trigger) and we co-added 19 unfiltered CCD exposures of 30 seconds each.

We detect a new source of mag. R = 17.6 +/-0.2 (USNO-B1 catalogue, not corrected
for Galactic extinction in the direction of the GRB) at the following position:


R.A.(J2000) = 05h 06m 56.18s
Dec.(J2000) = +12d 49' 10.9"

FITS files are available on request from fabciaba@alice.it
The message may be cited.


GRB_name: GRB141004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16887
SUBJECT: GRB 141004A: RATIR Optical Observations
DATE:    14/10/05 09:34:12 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 (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 141004A (D'Elia, et al., GCN 16878) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro MÃ¡rtir from 2014/10 5.30 to 2014/10 5.35
UTC (7.82 to 9.15 hours after the BAT trigger), obtaining a total of
1.07 hours exposure in the r and i bands.

We detect the source reported by Swift/UVOT (D'Elia, et al., GCN 16878)
and the 3.6m TNG telescope (D'Elia, et al., GCN 16881). We obtain the
following detections:

  r     22.35 +/- 0.13
  i     22.11 +/- 0.12

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the earlier TNG
observations we note that the GRB has faded with an approximate
temporal power-law index of t^(-1.0).

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB141005A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16888
SUBJECT: GRB 141005A: Enhanced Swift-XRT position
DATE:    14/10/05 10:38:56 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 2816 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 141005A, 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 = 291.09317, +36.09496 which is equivalent
to:

RA (J2000): 19h 24m 22.36s
Dec (J2000): +36d 05' 41.9"

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: GRB141005A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16889
SUBJECT: GRB 141005A: Fermi GBM Detection
DATE:    14/10/05 15:32:52 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 05:13:06.97 UT on the 5th of October 2014, the Fermi
Gamma-Ray Burst Monitor triggered and located GRB 141005A
(trigger 434178789 / 141005217) which was also detected by
Swift (V. D'Elia et al. 2014, GCN 16682). The GBM on-ground
location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 107 degrees.

The GBM light curve shows a single pulse with a duration (T90)
of about 3 seconds (50-300 keV). The time-averaged spectrum
from T0-0.26 s to T0+3.07 s is best fit by a power law
function with an exponential high-energy cutoff. The power law
index is -0.30 +/- 0.11  and the cutoff energy, parameterised
as Epeak, is 138 +/- 8 keV.

A Band function fits the spectrum equally well with
Epeak= 119 +/- 10 keV, alpha = -0.06 +/- 0.2 and
beta = -2.7 +/- 0.3.

The event fluence (10-1000 keV) in this time interval is
2.6 E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+1.5 seconds in the 10-1000 keV band
is 3.7 +/- 0.2 ph/s/cm^2.

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

---------------------------------------------------------------------------------------------------------------------------------------------
Dr. Oliver J. Roberts BSc PhD
Space Science and Advanced Materials Research Group,
School of Physics,
University College Dublin,
Belfield,
Dublin 4,
Ireland
+353(0)1-716-2202


GRB_name: GRB141004A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16890
SUBJECT: GRB 141004A: Swift/UVOT Detection
DATE:    14/10/05 16:07:41 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (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 141004A
65 s after the BAT trigger (D'Elia et al., GCN Circ. 16878).The GRB was
also detected by Integral (Mereghetti et al, GCN Circ. 16879), and in the
optical by CAHA (Gorosabel et al, GCN Circ. 16880), TNG (D'Elia et al.,
GCN Circ. 16881), at Monte Agliale Observatory (Ciabatta et al. GCN Circ.
16886) and by RATIR (Littlejohns et al., GCN Circ. 16887).  A source
consistent with the XRT position (Osborne et al. GCN Circ. 16883)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  05:06:56.14 =  76.73393 (deg.)
    Dec (J2000) = +12:49:11.3  =  12.81981 (deg.)
with an estimated uncertainty of 0.43 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               65          215          147         17.64 +/- 0.07
v                  606         1922          156         18.94 +/- 0.24
b                  532         1156           58         18.94 +/- 0.20
u                  277          527          246         17.93 +/- 0.09
w1                 656         1453           97         18.67 +/- 0.24
m2                 806         7273          216        >20.5
w2                 582        13683          582         20.69 +/- 0.35

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.32 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16891
SUBJECT: GRB141004A: NOT imaging and spectroscopy
DATE:    14/10/05 16:28:34 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MAS), T. Kruehler (ESO Chile), D. Xu, J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (U Leicester), P. Jakobsson (U. Iceland), S. Galleti (INAF-OAB) report on behalf a larger collaboration:

We observed the field of GRB 141004A (D'Elia et al. GCN 16878, Mereghetti et al. GCN 16879) with the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC. Observations started at 01:52:22 UT on October 5 (i.e., 2.52 hr after the burst). We obtained a 200-s image in the R band.

The afterglow reported in D'Elia et al. (GCN 16878) and Gorosabel et al. (GCN 16880) is clearly detected. It has an R-band magnitude of 20.6 mag (not corrected for foreground extinction), calibrated against several USNO stars. The mid-exposure time is 2.55 hr after the trigger. Compared to DElia et al (GCN 16881), the brightness of the afterglow did not decrease.

In addition, we obtained an optical spectrum, with a total exposure of 3 x 1800 s, using Grism #4 and covering the wavelength range 3750 - 9000 AA at a resolution of 17 AA. Observations started at 02:17:23 UT (i.e. 2.9 hr after the burst). The continuum is detected down to ~3750 AA. No absorption line is visible in the spectrum. A tentative emission line is detected at 5866.4 AA, which could be [OIII]-5007 at z=0.17 or [OII] at z=0.57. A higher S/N spectrum is needed to elucidate the nature of this feature.


GRB_name: GRB141004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16892
SUBJECT: GRB 141004A: Swift-BAT refined analysis
DATE:    14/10/05 17:11:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
V. D'Elia (ASDC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(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 141004A (trigger #614390)
(D'Elia, et al., GCN Circ. 16878).  The BAT ground-calculated position is
RA, Dec = 76.721, 12.828 deg, which is 
   RA(J2000)  =  05h 06m 53.0s 
   Dec(J2000) = +12d 49' 41.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single FRED peak starting with a weak
emission at T-1 sec, the FRED peak starting at T_0.0, peaking at T+0.1 sec,
and returning to baseline at ~T+20 sec.  T90 (15-350 keV) is 3.92 +- 1.07 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.84 to T+5.34 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.86 +- 0.08.  The fluence in the 15-150 keV band is 6.7 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.06 sec in the 15-150 keV band
is 6.1 +- 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/614390/BA/


GRB_name: GRB141005A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16893
SUBJECT: GRB 141005A: Swift-BAT refined analysis
DATE:    14/10/05 17:19:05 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (GSFC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(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 141005A (trigger #614415)
(D'Elia, et al., GCN Circ. 16882).  The BAT ground-calculated position is
RA, Dec = 291.103, 36.098 deg, which is 
   RA(J2000)  =  19h 24m 24.7s 
   Dec(J2000) = +36d 05' 54.1" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 6%.
 
The mask-weighted light curve shows a single peak starting at ~T-1 sec,
peaking at ~T+2 sec, and ending at ~T+7 sec.  T90 (15-350 keV) is 4.34 +- 1.08 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+0.19 to T+5.66 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.33 +- 0.18.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.68 sec in the 15-150 keV band
is 4.2 +- 0.8 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/614415/BA/


GRB_name: GRB141005A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16894
SUBJECT: GRB 141005A: Swift/UVOT Upper Limits
DATE:    14/10/05 17:20:24 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (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 141005A
94 s after the BAT trigger (D'Elia et al., GCN Circ. 16882).
This GRB was observed also by Fermi GBM (Roberts, GCN Circ. 16889), and
in the r and i bands (P60: Perley et al., GCN Circ. 16884, RATIR:
Littlejohn et al.,GCN Circ. 16885). A nearby galaxy was reported by
Perley et al., and is also seen in the UVOT images.
No optical afterglow consistent with the XRT position (Beardmore et
al. GCN Circ. 16888), or the P60 position is detected in the initial
UVOT exposures, although the event data for the UVOT b-band show a
slight brightening peaking around T+700s..
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                94          344          246         >20.1
v                 5960         7392          393         >19.4
b                  349         6980          639         >20.2
u                   94         6775          786         >20.6
w1                5138         6570          393         >19.9
m2                4932         7445          441         >20.2
w2                5754         7186          393         >20.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.17 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141005A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16895
SUBJECT: GRB 141005A: Swift-XRT refined Analysis
DATE:    14/10/05 17:28:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), M. de Pasquale (INAF-IASFPA), A.
Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), D.N. Burrows (PSU),
J.A. Kennea (PSU) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 141005A (D'Elia  et al. GCN
Circ. 16882),  from 79 s to 29.1 ks after the  BAT trigger. The data
comprise 120 s in Windowed Timing (WT) mode (the first 7 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 Beardmore
et al. (GCN Circ. 16888).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.33 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.03 (+0.23, -0.21). The
best-fitting absorption column is  3.3 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.3 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.03 (+0.23, -0.21)

If the light curve continues to decay with a power-law decay index of
1.33, the count rate at T+24 hours will be 3.4 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.3 x
10^-14 (1.9 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/00614415.

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


GRB_name: GRB141004A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16896
SUBJECT: GRB 141004A: Swift-XRT refined Analysis
DATE:    14/10/05 21:30:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U.
Leicester), A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), V.
Mangano (PSU) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 141004A (D'Elia  et al. GCN
Circ. 16878),  from 46 s to 54.0 ks after the  BAT trigger. The data
comprise 5 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.
16883).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.66 (+0.08, -0.11), followed by a break at T+3318 s to
an alpha of 1.9 (+0.7, -0.6).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.79 (+0.21, -0.12). The
best-fitting absorption column is  consistent with the Galactic value
of 3.1 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.2 x 10^-11 (5.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+/-1.1) x 10^21 cm^-2
Galactic foreground: 3.1 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.79 (+0.21, -0.12)

If the light curve continues to decay with a power-law decay index of
1.9, the count rate at T+24 hours will be 4.5 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-14 (2.6 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/00614390.

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


GRB_name: GRB141005A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16897
SUBJECT: Konus-Wind observation of GRB 141005A
DATE:    14/10/06 18:30:02 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration GRB 141005A (Swift-BAT trigger 614415:
D'Elia, GCN 16882; Krimm et al., GCN 16893;
Fermi-GBM detection: Roberts, GCN 16889)
triggered Konus-Wind at T0=18787.727 s UT (05:13:07.727).

The burst light curve shows a single pulse with a duration of ~3 s.
The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.3(-0.2,+0.3)x10^-6 erg/cm2,
and a 64-ms peak energy flux, measured from T0+0.390 s,
of 1.6(-0.5,+0.5)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.34(-0.49,+0.58),
and Ep = 104(-14,+18) keV (chi2 = 33/55 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.37 (chi2 = 31/54 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141005_T18787/

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


GRB_name: GRB141005A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16898
SUBJECT: GRB 141005A: GROND observations
DATE:    14/10/06 19:22:24 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

S. Schmidl (TLS Tautenburg), J. F. Graham, and J. Greiner
(both MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 141005A (Swift trigger 614415; V. D'Elia et
al., GCN #16882) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

We detect a source consistant with the position reported by Perley et al.
(GCN #16884). From coadded observations, starting on October 05 and
spanning from 23:50 to 00:04 UT, we report the following preliminary
magnitudes and upper limits (AB magnitude system) of:

g' > 21.6,
r' = 21.7 +/- 0.2,
i' = 21.7 +/- 0.2,
z' = 21.2 +/- 0.2,
J  > 20.5,
H  > 19.9, and
K  > 18.2.

Given magnitudes and upper limits are calibrated against SDSS as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.17 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141004A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16899
SUBJECT: GRB 141004A: GROND observations
DATE:    14/10/06 19:23:19 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

S. Schmidl (TLS Tautenburg), J. F. Graham, and J. Greiner
(both MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 141004A (Swift trigger 614390; V. D'Elia et
al., GCN #16878) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

We detect the afterglow at the UVOT position reported by V. D'Elia et al.
(GCN #16878). From coadded observations, starting on October 06 and
spanning from 05:31 to 09:09 UT, we report the following preliminary AB
magnitudes of:

g' = 24.6 +/- 0.3,
r' = 24.0 +/- 0.2,
i' = 23.5 +/- 0.2, and
z' = 23.4 +/- 0.2.

Given magnitudes are calibrated against GROND zeropoints and
are not corrected for the expected Galactic foreground extinction
corresponding to a reddening of E_(B-V)=0.32 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB141004A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16900
SUBJECT: GRB 141004A: Fermi GBM observation
DATE:    14/10/06 19:47:12 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 23:20:54.42 UT on 4 October 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141004A (trigger 434157657 / 141004973),
which was also detected by the Swift/BAT (D'Elia et al. 2014, GCN 16878)
and the INTEGRAL/IBIS (Mereghetti et al 2014, GCN 16879).
The GBM on-ground location is consistent with the Integral position, which
lies at an angle of 100.4 degrees from the Fermi LAT boresight.

The GBM light curve consists of a short FRED peak followed by a faint tail
with a duration (T90) of about 3 s (50-300 keV).
The time-averaged spectrum from T0-0.320 s to T0+0.768 s (main peak) is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.3 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 147 +/- 28 keV
(Castor stat 398.59 for 365 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(2.2 +/- 0.2)E-06 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.000 s in the 10-1000 keV band
is 18 +/- 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: GRB141005A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16901
SUBJECT: GRB 141005A: Additional P60 imaging and afterglow confirmation
DATE:    14/10/07 06:04:59 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report:

We obtained a second epoch of imaging at the location of the optical 
afterglow (Perley et al., GCN 16884; Littlejohns et al., GCN 16885; 
Schmidl et al., GCN 16898) of GRB 141005A (D'Elia et al., GCN 16882) 
with the robotic Palomar 60 inch telescope.  Observations were obtained 
in the r', i', and z' filters beginning at 2:31 UT on 2014 October 6 
(0.89 d after the burst).

A source is clearly detected at the location of the afterglow candidate 
originally reported in GCN 16884 (Perley et al).  As noted therein, a 
source is also present at this location in pre-outburst SDSS imaging of 
this field.

To search for variability at this location, we performed digital image 
subtraction with the P60 data, using the images from 2014 October 6 as a 
reference template.  We find clear evidence for fading in the i-band 
(and marginal evidence in r and z-bands), confirming that this source is 
indeed the optical afterglow of GRB 141005A but is blended with a bright 
(i' ~ 21.7 mag) host galaxy or foreground object.   Assuming no 
contribution of the afterglow to our template images, we measure i' = 
20.24 +/- 0.10 at 5:18 UT on 2014 October 5 (i.e., 5 min after the Swift 
trigger).


GRB_name: GRB141004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16902
SUBJECT: GRB141004A: Host galaxy redshift form GTC
DATE:    14/10/07 10:39:48 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), 
D. Malesani (DARK/NBI), S. Schulze (PUC, MAS), R. Sanchez-Ramirez 
(UPV/EHU, IAA-CSIC), J. Gorosabel (UPV/EHU, IAA-CSIC),
C.A. Alvarez Iglesias (GTC, IAC), J. Molgo (GTC), and M. Rivero (GTC) 
report on behalf of a larger collaboration:

We obtained spectroscopy of the optical counterpart of GRB 141004A 
(D'Elia et al., GCN 16878, Mereghetti et al., GCN 16879) with OSIRIS at 
the 10.4m GTC telescope on October 7, starting at 5:10 UT (~30 hr after 
the GRB). In a preliminary reduction of a 2x600 s exposure with the 
R1000R grism (covering from 5100 to 10000 A with a resolution of ~1000), 
we detected several emission lines corresponding to [O II], H-beta and 
[O III] at a common redshift of 0.573. This confirms that the tentative 
emission line detection reported by Schulze et al. (GCN 16891) was 
indeed real and that it corresponds to the [O II] 3727/3729 doublet. 

We also detect emission from another galaxy within the slit at a similar 
redshift of 0.571, with a projected distance of 22" to the East, which 
corresponds to ~150 kpc at that redshift, probably belonging to the same 
galaxy group. The nearby galaxy reported by D'Elia et al. (GCN 16881) 
shows multiple emission features at a redshift of 0.279, and it is therefore 
unrelated to the GRB.


GRB_name: GRB141005A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16903
SUBJECT: GRB 141005A: iTelescope.Net T21 Optical Observation
DATE:    14/10/07 12:57:06 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. Kawamura, T. Sakamoto, A. Yoshida (AGU)

We observed the field of GRB 141005A detected by Swift (trigger #614415; 
D'Elia et al., GCN Circ. 16882) with the iTelescope.Net (http://www.itelescope.net) 
T21 (0.43 m Planewave) telescope located at the New Mexico Skies Observatory 
(NM, USA).  

60 images of 20 sec exposures and 20 images of 60 sec exposures were taken in the 
R filter starting from October 5 05:27:55 (UT) about 15 minutes after the trigger 
and stopped on October 5 06:33:49 (UT).  We do not detect the optical afterglow 
both in the individual images and the stacked image at the enhanced X-ray 
afterglow position (Beardmore et al., GCN Circ. 16888).  The estimated five sigma 
upper limit of the combined image (total exposure of 2400 sec) is ~18.4 using 
the USNO-B1 catalog.


GRB_name: GRB141011A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16905
SUBJECT: GRB 141011A: Fermi GBM detection
DATE:    14/10/11 15:49:36 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 06:46:20.36 UT on 11 October 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141011A (trigger 434702783 / 141011282).

The trigger resulted in an Autonomous Repoint Request (ARR)
that was accepted and the spacecraft slewed to the GBM in-flight location.

The on-ground calculated location, using the GBM trigger
data, is RA = 254.9, DEC = -8.3 (J2000 degrees,
equivalent to 16h 59m, -08d 18'), with an uncertainty
of 2.7 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 32 degrees.

The GBM light curve consists of a short structured pulse
with a duration (T90) of about 0.1 s (50-300 keV).
The time-averaged spectrum from T0-0.16 s to T0+0.080 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.50 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 603 (+78/-63)keV

The event fluence (10-1000 keV) in this time interval is
(1.05 +/- 0.05)E-06 erg/cm^2. The 0.016-sec peak photon flux measured
starting from T0-0.16 s in the 10-1000 keV band
is 70 +/- 4 ph/s/cm^2.

A Band function fits the spectrum equally well with 
Epeak= 573 (+90/-75) keV, alpha = -0.5 +/- 0.1 and beta = -2.7 (+0.4/-4.2).

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


GRB_name: GRB141011A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16906
SUBJECT: IPN Triangulation of GRB 141011A (short/hard)
DATE:    14/10/13 11:35:49 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

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

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

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

The short-duration, hard-spectrum, bright GRB 141011A (von Kienlin, GCN 
Circ. 16905) has been observed by Fermi (GBM trigger 434702783), 
Konus-Wind, MESSENGER (GRNS), Mars Odyssey (HEND), Swift (BAT), and 
INTEGRAL (SPI-ACS), so far, at about 24380 s UT (06:46:20). 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:
   257.939 (17h 11m 45s)  -9.681 ( -9d 40' 52")
  Corners:
   257.903 (17h 11m 37s)  -9.336 ( -9d 20' 10")
   257.999 (17h 12m 00s)  -9.336 ( -9d 20' 09")
   257.975 (17h 11m 54s) -10.026 (-10d 01' 34")
   257.878 (17h 11m 31s) -10.027 (-10d 01' 36")
  ---------------------------------------------
The error box area is 236 sq. arcmin, and its maximum
dimension is 42 arcmin (the minimum one is 6 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141011_T24377/IPN/

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


GRB_name: GRB141011A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16907
SUBJECT: Konus-Wind observation of GRB 141011A
DATE:    14/10/13 11:51:35 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The short-duration, hard-spectrum GRB 141011 (Fermi-GBM detection: von 
Kienlin, GCN Circ. 16905; IPN triangulation: Golenetskii et al., GCN 
Circ. 16906) triggered Konus-Wind at T0=24377.666 s UT (06:46:17.666).

The burst light curve shows a short pulse with
a total duration of ~0.1 s.
The emission is seen up to ~4 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141011_T24377/

As observed by Konus-Wind, the burst
had a fluence of 1.24(-0.20,+0.02)x10^-6 erg/cm2,
and a 2-ms peak flux, measured from T0-0.012 s,
of 7.1(-1.7,+0.7)x10^-5 erg/cm2/s
(both in the 20 keV - 1.2 MeV energy range).

Modeling the K-W 3-channel time-integrated spectrum
(from T0-0.014 s to T0+0.048 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields
alpha = 0.1(-0.4, +0.4), and
Ep = 521(-75,+120) keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the quoted values are preliminary.


GRB_name: GRB141015A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16909
SUBJECT: GRB 141015A: Swift detection of a burst
DATE:    14/10/15 09:26:18 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Troja (NASA/GSFC/UMCP), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), P. A. Evans (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC) and R. L. C. Starling (U Leicester) report
on behalf of the Swift Team:

At 09:12:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141015A (trigger=615399).  Swift did not slew because of Moon constraint. 
The BAT on-board calculated location is 
RA, Dec 87.507, +18.316 which is 
   RA(J2000)  =  05h 50m 02s
   Dec(J2000) = +18d 18' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 10 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 15:56 UT on 2014 October 15. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB141015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16910
SUBJECT: GRB 141015A: Swift/XRT localization
DATE:    14/10/15 15:39:14 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Troja (NASA/GSFC/UMCP), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), P. A. Evans (U Leicester), J. A. Kennea (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 09:12:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141015A (trigger=615399).  The position was reloaded up to Swift
using the "grb" mode of the TOO command (now that the location is out of Moon
constraint).  As such, Swift responds by generating the standard set
of real-time TDRSS messages (and hence the GCN Notices). 
We are issuing this Circular with the results from XRT and UVOT. 

The XRT began observing the field at 15:07:56.6 UT, 21297.3 seconds
after the BAT trigger. Using promptly downlinked data we find an
uncatalogued X-ray source located at RA, Dec 87.51746, 18.32965 which
is equivalent to:
   RA(J2000)  = 05h 50m 04.19s
   Dec(J2000) = +18d 19' 46.7"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 60 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 5.59
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 21238 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. 

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: GRB141015A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16911
SUBJECT: GRB 141015A: ISON-NM early optical observations
DATE:    14/10/15 17:27:15 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov 
(KIAM), A. Pozanenko (IKI) report on behalf of larger GRB  follow-up 
collaboration:

We observed the field of the Swift   GRB 141015A (Troja et al., GCN 
16909) with 0.4-m telescope of ISON-NM observatory starting on Oct., 15 
(UT) 09:16:55, i.e. ~4 minutes after burst triger. We obtained 14 
unfiltered images of 120 s exposure. We do not detect any source within 
XRT error circle (Troja et al., GCN 16910):

UT start   t-T0         Exp.      Filter  UL (3sigma)
          (mid.,days)    (s)
09:16:55  0.0068        5*120    Clear   18.4
09:16:55  0.0131       14*120    Clear   19.0

The photometry is based on nearby USNO-B1.0 stars

USNO-B1.0      RA             DEC            R2
1083-0107546   087,552978    +18,360067     14,78
1083-0107529   087,547650    +18,355839     15,18
1083-0107484   087,534895    +18,341425     15,00
1083-0107360   087,503081    +18,336089     14,71


GRB_name: GRB141015A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16912
SUBJECT: GRB 141015A: Super-LOTIS early observations
DATE:    14/10/15 17:55:40 GMT
FROM:    Adria C. Updike at Roger Williams U  <aupdike@rwu.edu>

Adria C. Updike (Roger Williams University) and Dieter H. Hartmann (Clemson University) report on behalf of the AZTEC collaboration:

We observed the field of the Swift GRB 141015A (Troja et al., GCN 16909) with the 0.6-m Super-LOTIS telescope at Kitt Peak National Observatory in Arizona under good conditions.  Super-LOTIS began taking images 81 seconds after the trigger and continued for 37 minutes, obtaining 10 sec, 20 sec, and 60 sec images in the R band.  We do not detect any source within the XRT error circle (Troja et al., GCN 16910):

UT midtime     Exp Time        Filter      Upper Limit
-------------------------------------------------------------------
09:15:01          4 x 10 sec         R           16.5
09:16:50          5 x 20 sec         R           17.4
09:23:35         10 x 60 sec        R           19.0

with photometry based on the USNO B1.0 catalog.


GRB_name: GRB141015A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16913
SUBJECT: GRB 141015A: Enhanced Swift-XRT position
DATE:    14/10/15 18:18:50 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 1819 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 141015A, 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 = 87.51892, +18.32940 which is equivalent
to:

RA (J2000): 05h 50m 4.54s
Dec (J2000): +18d 19' 45.8"

with an uncertainty of 2.3 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: GRB141015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16914
SUBJECT: GRB 141015A: RATIR Optical Upper Limits
DATE:    14/10/15 18:40:51 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 (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 141015A (Troja, et al., GCN 16909) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/10 15.39 to 2014/10 15.53 UTC (0.05
to 3.59 hours after the BAT trigger), obtaining a total of 2.44 hours
exposure in the r and i bands.

For a source within the Swift/XRT error circle (Troja, et al., GCN 16910),
we obtain the following upper limits (3-sigma):

  r     > 23.07
  i     > 22.48

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

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB141015A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16915
SUBJECT: GRB 141015A: LCO-McDonald observations
DATE:    14/10/15 20:50:22 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

J. Japelj (U. Ljubljana) and C. Guidorzi (U. Ferrara) on behalf of a large collaboration report:

We observed the position of GRB 141015A (Troja et al. GCN Circ. 16909) with the 1-m McDonald telescope (Fort Davis, US), a member of the Las Cumbres Observatory network. Observations started on October 15 at 09:51:01 UT, i.e., 38 minutes after the GRB trigger time (GCN Circ. 16909) and were done with the g', r' and i' filters.

We did not find a new source within the enhanced XRT error circle (Evans et al. GCN Circ. 16913) down to the following limits:

Mid time from  Total Exp   Filter    Magnitude
trigger (min)          (s)
-----------------------------------------------------------
54.4                       600        r'        > 19.6
59.2                       600        i'        > 18.7
-----------------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB141015A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16916
SUBJECT: GRB 141015A: Swift-BAT refined analysis
DATE:    14/10/15 22:18:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

A. Y. Lien (GSFC/UMBC), 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), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), J. Tueller (GSFC),
T. N. Ukwatta (LANL)
(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 141015A (trigger #615399)
(Troja, et al., GCN Circ. 16909).  The BAT ground-calculated position is
RA, Dec = 87.535, 18.370 deg, which is 
   RA(J2000)  =  05h 50m 08.5s 
   Dec(J2000) = +18d 22' 12.5" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
 
The mask-weighted light curve shows s single FRED-like pulse starting 
at ~T_0, peaking at ~T+1 sec, and ending at ~T+12 sec.  T90 (15-350 keV)
is 11.0 +- 4.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.00 to T+13.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.90 +- 0.37.  The fluence in the 15-150 keV band is 1.6 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.00 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/615399/BA/


GRB_name: GRB141015A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16917
SUBJECT: GRB 141015A: MITSuME Okayama upper limits
DATE:    14/10/16 06:05:45 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 and OISTER collaboration:

We observed the field of GRB 141015A (Troja et al., GCNC 16909)
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 2014-10-15 13:44:05 UT, (~4.5 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans, GCNC 16913) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.29816    16:22:18    5760.0   >20.1  >19.8  >19.0
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141015A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16918
SUBJECT: GRB 141015A: Swift/UVOT Upper Limits
DATE:    14/10/16 12:56:09 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) 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 141015A 
21301 s after the BAT trigger (Troja et al., GCN Circ. 16909).
No optical afterglow consistent with the XRT position (Evans et al. GCN 
Circ. 16913) 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         21301        21451          147         >20.5
white            21301        23280         1033         >21.5
v                27071        27978          885         >19.8
b                21461        22368          885         >20.8
w1               28890        29661          759         >20.1
m2               27983        28883          886         >20.3
w2               23286        23906          610         >20.1

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.51 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB141017A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16919
SUBJECT: GRB 141017A: Swift detection of a burst
DATE:    14/10/17 18:50:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (GSFC/UMBC),
V. Mangano (PSU), K. L. Page (U Leicester),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU) and
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 18:25:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141017A (trigger=615672).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 93.629, -58.554 which is 
   RA(J2000)  =  06h 14m 31s
   Dec(J2000) = -58d 33' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two main peaks
with a duration of about 60 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~50 sec after the trigger. 

The XRT began observing the field at 18:26:52.0 UT, 84.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 93.6284, -58.5836 which is equivalent to:
   RA(J2000)  = +06h 14m 30.82s
   Dec(J2000) = -58d 35' 01.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 106 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 4.83e-09 erg cm^-2 s^-1 (0.2-10
keV). 

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 expected extinction corresponding to E(B-V) of
0.04. 

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: GRB141017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16920
SUBJECT: GRB 141017A: Zadko observatory - Gingin optical observations
DATE:    14/10/17 20:32:44 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz, D. Turpin (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR),
D. Coward (UWA),
M. Boer, B. Gendre, K. Siellez, H. Dereli, O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 141017A detected by SWIFT
(trigger 615672) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 42 min after the GRB trigger.
The elevation of the field increased from
58 degrees above horizon and weather conditions
were excellent.

We examined a series of exposures obtained between
42 min and 110 min. In the error box given by SWIFT XRT
(Marshall et al. GCNC 16919) we detect a source of
magnitude R=22.4 (+/-0.4) which does not seem to be variable.
Its position is 06:14:31.2 -58:34:56 J2000.
We do not believe that it is the afterglow of GRB 141017A.

We conclude the afterglow of GRB 141017A is fainter
than R=22.4 42 minutes after the trigger.

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB141017A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16921
SUBJECT: GRB 141017A: Enhanced Swift-XRT position
DATE:    14/10/17 23:29:03 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 3763 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 141017A, 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 = 93.62994, -58.58229 which is equivalent
to:

RA (J2000): 06h 14m 31.19s
Dec (J2000): -58d 34' 56.2"

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

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB141017A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16922
SUBJECT: GRB 141017A: Swift-XRT refined Analysis
DATE:    14/10/18 06:50:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.7 ks of XRT data for GRB 141017A (Marshall  et al.
GCN Circ. 16919),  from 77 s to 18.8 ks after the  BAT trigger. The
data comprise 120 s in Windowed Timing (WT) mode (the first 6 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 Goad
et al. (GCN Circ. 16921).

The late-time light curve (from T0+4.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.82 (+/-0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.45 (+0.15, -0.14). The
best-fitting absorption column is  2.1 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 3.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.02 (+/-0.11) and a
best-fitting absorption column of 1.9 (+0.4, -0.3) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.5 x 10^-11 (4.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+0.4, -0.3) x 10^21 cm^-2
Galactic foreground: 3.8 x 10^20 cm^-2
Excess significance: 7.2 sigma
Photon index:      2.02 (+/-0.11)

If the light curve continues to decay with a power-law decay index of
0.82, the count rate at T+24 hours will be 0.034 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-12 (1.6 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/00615672.

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


GRB_name: GRB141015A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16923
SUBJECT: GRB 141015A: MITSuME Akeno upper limits
DATE:    14/10/18 09:26:48 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y. Yano, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi,
S. Kurita, Y. Ono, T. Fujiwara, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 141015A (E. Troja et al., GCN Circular #16909) 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 2014-10-15 14:40:07 UT (~5.5 h after the burst).
We did not find any new point source within the enhanced XRT circle 
(P. A. Evans et al., GCN Circular #16913) in all the three bands.

The measured magnitudes are listed below.

T0+[sec]     MID-UT    T-EXP[sec]        g'         Rc        Ic
------------------------------------------------------------------------------
31113        18:00:29      1440           >20.7  >20.1  >19.3
------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB141017A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16924
SUBJECT: GRB 141017A: Swift/UVOT Detection
DATE:    14/10/18 11:06:06 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141017A
92 s after the BAT trigger (Marshall et al., GCN Circ. 16919).
A source consistent with the XRT position (Goad et al. GCN Circ. 16921) 
is detected in the initial UVOT white filter exposures.

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)          92          242          150         20.54 +/- 0.25
white              859         1009          159        >20.91
v                  633        13060          691        >20.0
b                  559        17991         1306        >21.4
u                  304         7171          717        >20.7
w1                 683         6966          471        >20.3
m2                5133         6761          388        >20.1
w2                6152        12850         1082        >21.1

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: GRB141015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16925
SUBJECT: GRB 141015A: Swift-XRT afterglow confirmation and refined Analysis
DATE:    14/10/19 08:10:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

E. Troja (NASA/GSFC/UMCP) reports on behalf of the Swift-XRT team:

We have analysed 9.0 ks of XRT data for GRB 141015A (Troja  et al. GCN
Circ. 16909),  from 21.3 ks to 271.2 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 16913). 

The GRB light curve in the initial observation was at a level of ~0.02
ct/sec in XRT. In subsequent observations the GRB is undetected, with
an upper limit of 0.004 ct/sec, we therefore confirm that this was the
afterglow of GRB 141015A.
 
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.38 (+0.51, -0.20). The
best-fitting absorption column is  consistent with the Galactic value
of 5.6 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 6.0 x 10^-11 (7.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.6 (+/-3.8) x 10^21 cm^-2
Galactic foreground: 5.6 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.38 (+0.51, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00615399.

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


GRB_name: GRB141017A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16926
SUBJECT: GRB 141017A: GROND Afterglow Confirmation
DATE:    14/10/19 12:57:11 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, A. Nicuesa Guelbenzu (both TLS Tautenburg), and J. Greiner
(MPE Garching)  report on behalf of the GROND team:

We observed the field of GRB 141017A (Swift trigger 615672; Marshall et
al., GCN #16919) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at La Silla
Observatory (Chile).

Observations started at 02:50 UT on 18 October 2014, around 8.5 hours
after the GRB trigger. They were performed at an average seeing of 1".7
and at an average airmass of 1.9.

Based on images with exposure times of 4130 s in g'r'i'z' (centered 0.459
days after the GRB) and 4800 s in JHK (centered 0.426 days after the GRB),
we detect a source within the Swift-XRT error circle reported by Goad et
al. (GCN #16921) at position

RA (J2000) = 06:14:31.28
Dec. (J2000) = -58:34:56.5

with an error of 0".5 and the following 3-sigma AB magnitudes:

g' = 24.3 +/- 0.2 mag,
r' = 23.6 +/- 0.2 mag,
i' = 23.4 +/- 0.2 mag,
z' = 23.2 +/- 0.3 mag,
J > 22.0 mag,
H > 21.4 mag, and
K > 20.3 mag.

The object has faded strongly compared to the early UVOT detection (Oates
et al., GCN #16924) and the Zadko Gingin detection (Klotz et al., GCN
#16920), confirming it as the afterglow. At this time, we cannot conclude
if this object might already be the host galaxy of GRB 141017A. Comparison
with an epoch taken 75 minutes earlier at lower S/N shows no significant
evidence for fading, but the spectrum is well-described by a spectral
slope with beta = 1 and a possible drop-out in g' (redshift z > 2.2).

Given magnitudes are derived based on calibrating the images against GROND
zeropoints (g'r'i'z') and 2MASS field stars (JHK) and are not corrected
for the Galactic foreground extinction corresponding to a reddening of
E_(B-V) = 0.04 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16927
SUBJECT: GRB 141017A, Swift-BAT refined analysis
DATE:    14/10/19 14:15:17 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), 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 (GSFC/UMBC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+700 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141017A (trigger #615672)
(Marshall, et al., GCN Circ. 16919).  The BAT ground-calculated position is
RA, Dec = 93.601, -58.596 deg which is
   RA(J2000)  =  06h 14m 24.2s
   Dec(J2000) = -58d 35' 45.9"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.

The mask-weighted light curve shows a double-peaked structure.
The first peak starts at ~T-1 s, peaks at ~T+1 s, and ends at ~T+3s.
The second peak starts at ~T+40s, peaks at ~T+46s, and ends at ~T+60s.
T90 (15-350 keV) is 55.7 +- 2.8 sec (estimated error including systematics).

The time-averaged spectrum from T-1.2 to T+65.1 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.05 +- 0.28,
and Epeak of 80.4 +- 17.2 keV (chi squared 39.44 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.1 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+46.60 sec in the 15-150 keV band is
6.7 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.66 +- 0.06 (chi squared 55.80 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/615672/BA/


GRB_name: GRB141020A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16928
SUBJECT: GRB 141020A: Swift detection of a burst with an optical counterpart
DATE:    14/10/20 08:01:15 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

S. B. Cenko (GSFC), A. P. Beardmore (U Leicester),
M. M. Chester (PSU), H. A. Krimm (CRESST/GSFC/USRA),
P. T. O'Brien (U Leicester) and K. L. Page (U Leicester) report on
behalf of the Swift Team:

At 07:48:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141020A (trigger=615873).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 225.009, +55.334 which is 
   RA(J2000) = 15h 00m 02s
   Dec(J2000) = +55d 20' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 30 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 07:50:06.5 UT, 87.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 224.99514, 55.31391 which is equivalent
to:
   RA(J2000)  = 14h 59m 58.83s
   Dec(J2000) = +55d 18' 50.1"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 77 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 1.25
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 91 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 14:59:59.15 = 224.99647
  DEC(J2000) = +55:18:46.8  =  55.31299
with a 90%-confidence error radius of about 0.75 arc sec. This position is 4.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.73 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 S. B. Cenko (brad.cenko 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.)


