# GCN_circulars

GRB_name: GRB120803A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13565
SUBJECT: GRB 120803A: Swift detection of a possible burst
DATE:    12/08/03 07:55:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU), K. L. Page (U Leicester),
D. M. Palmer (LANL) and T. Sakamoto (NASA/UMBC) report on behalf of
the Swift Team:

At 07:22:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120803A (trigger=529582).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 269.565, -6.715 which is 
   RA(J2000) = 17h 58m 16s
   Dec(J2000) = -06d 42' 53"
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 ~1000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 07:24:43.1 UT, 147.0 seconds after
the BAT trigger. No source was detected in 1.0 ks of promptly
downlinked data, which covered 91% of the BAT error circle. 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 149 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.94. 

This event is of low significance (7.3 sigma) in the BAT trigger image,
and no XRT source has been found in the 91% of the BAT error circle
covered by the immediately-available data. It is unusual for a real 
long GRB to lack an XRT counterpart.  Therefore, we cannot confirm the 
reality of this event until we receive the complete downlinked data. 

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: GRB120803B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13566
SUBJECT: GRB 120803B: Swift detection of a burst
DATE:    12/08/03 11:21:49 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. L. Racusin (NASA/GSFC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), O. M. Littlejohns (U Leicester) and
K. L. Page (U Leicester) report on behalf of the Swift Team:

At 11:06:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120803B (trigger=529606).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 314.224, +53.282 which is 
   RA(J2000) = 20h 56m 54s
   Dec(J2000) = +53d 16' 57"
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 30 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 11:07:22.4 UT, 75.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 314.23606, 53.30380 which is equivalent
to:
   RA(J2000)  = 20h 56m 56.65s
   Dec(J2000) = +53d 18' 13.7"
with an uncertainty of 3.7 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 5.67
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 149 seconds with the White filter
starting 78 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 3.5% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
1.71. 

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: GRB120803B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13567
SUBJECT: GRB 120803B: FTN possible afterglow candidate
DATE:    12/08/03 12:40:19 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell, D. Bersier (LJMU),
N.R. Tanvir (U. Leicester) report on behalf of a larger
collaboration:

The 2-m Faulkes Telescope North automatically began observing
GRB 120803B (Racusin et al. GCN Circ. 13566) on August 03 2012,
11:09:06 UT corresponding to 180 seconds post burst trigger
with BVRi' filters. Within the XRT error circle, in the i-band
filter we found the following uncatalogued possibly fading source,

R.A. = 20:56:56.46
Dec = +53:18:14.4   (J2000)

with an uncertainty of about 1".
The detection is marginal, with an estimated magnitude of
19.5 +/- 0.5 in the i band at a mean time of 13.2 minutes
(100 s exposure) calibrated against nearby USNOB-1 stars.
The source is no longer visible in the latest frames.
In the R band we see nothing down to 21.4 mag at 32.5 minutes
post burst. The faintness and colour of the source might
partially be explained by the relatively large foreground
extinction, E(B-V)=1.7.


GRB_name: GRB120803A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13568
SUBJECT: GRB 120803A: Swift-BAT refined analysis
DATE:    12/08/03 13:59:39 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120803A (trigger #529582)
(Racusin, et al., GCN Circ. 13565).  The BAT ground-calculated position is
RA, Dec = 269.531, -6.733 deg, which is 
   RA(J2000)  =  17h 58m 07.4s 
   Dec(J2000) = -06d 43' 58.0" 
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 54%.
 
The mask-weighted light curve shows a single peak starting at ~T+0,
peaking ~T+3 sec, and returning to baseline at ~T+20 sec.
T90 (15-350 keV) is 10.0 +- 3.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.40 to T+11.40 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.86 +- 0.35.  The fluence in the 15-150 keV band is 3.0 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.40 sec in the 15-150 keV band
is 0.4 +- 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/529582/BA/

We note that in our original circular (13565) that this event was labeled
as a "possible" GRB.  Given that the BAT detection significance
in ground proccessing has risen to 8.0 sigma, that the lightcurve shape
is consistant with a GRB, and that it is off the Galactic Plane,
we are confident that this trigger is due to a real GRB. 


GRB_name: GRB120803A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13569
SUBJECT: GRB 120803A: Swift-XRT Observations
DATE:    12/08/03 14:11:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, K.L. Page (U. Leicester) and J.L. Racusin (NASA/GSFC) report
on behalf of the Swift-XRT team:

We have analysed 2.5 ks of Photon Counting mode XRT data on GRB 120803A
from 155 s to 5.8 ks after the BAT trigger (Racusin et al., GCN Circ
13565). We find a single, uncatalogued X-ray source at RA,Dec =
269.5140, -6.7628 which is equivalent to:

   RA(J2000)  = 17h  58m 03.36s
   Dec(J2000) = -06d 45' 46.2"

with an uncertainty of 4 arc sec (radius, 90% containment). This
source is  4.2 arcmin from the original BAT position (GCN Circ 13565)
but only 2 arcmin from the refined BAT position (Ukwatta et al., GCN
Circ 13568), inside the refined BAT error circle.

The spectrum of this object can be modelled by an absorbed power-law
with a photon index of 1.1 (+0.9, -0.5). The absorption is consistent
with the Galactic value of 2.3e21 cm^-2 (Kalberla et al. 2005).

The source has a mean count-rate of 0.014 (+/- 0.0029) ct/sec, we cannot
tell at this time whether the source is fading. Further observations are
planned.

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


GRB_name: GRB120803B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13570
SUBJECT: GRB 120803B: MITSuME Akeno Optical upper limits
DATE:    12/08/03 14:36:09 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

R. Usui, Y.Aoki, S. Kurita, T. Yoshii, M. Hayashi,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech)  report
on behalf of the MITSuME collaboration:

We observed GRB 120803B ( Racusin et al., GCN Circular #13566) 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 2012-08-03 11:07:28 UT ( ~ 82 sec after
the burst).  And we did not find any new point source
within the XRT error circle in the three bands.
The results of photometry (3sigma upper limits) are listed below.

The photon flux were calibrated against GSC2.3 catalog.

T0+[sec]      MID-UT     T-EXP[sec]       g'              Rc           Ic
-------------------------------------------------------------------------------------------
       82       11:09:51         240        > 18.0       > 18.0     > 17.3
      376       11:53:57        3600         >19.2
      376       11:53:32        3660                           >18.9
      376       11:53:02        3720
        >18.3
-------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]

[GCN OPS NOTE(04aug12): Per author's request, the "120803A" in the
Subject-line was changed to "120803B".]


GRB_name: GRB120803B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13571
SUBJECT: GRB 120803B: Enhanced Swift-XRT position
DATE:    12/08/03 15:12:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 117 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120803B, 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 = 314.23579, +53.30416 which is equivalent
to:

RA (J2000): 20h 56m 56.59s
Dec (J2000): +53d 18' 15.0"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB120803B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13572
SUBJECT: GRB 120803B: Swift-BAT refined analysis
DATE:    12/08/03 17:47:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120803B (trigger #529606)
(Racusin, et al., GCN Circ. 12566).  The BAT ground-calculated position is
RA, Dec = 314.223, 53.298 deg, which is 
   RA(J2000)  =  20h 56m 53.6s 
   Dec(J2000) = +53d 17' 54.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 58%.
 
The mask-weighted light curve shows a FRED-like pulse starting at ~T-5 sec,
peaking at ~T+6 sec, and returning to baseline ~T+60 sec (or possibly T+90 sec).
T90 (15-350 keV) is 37.5 +- 7.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.67 to T+49.16 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.84 +- 0.36, 
and Epeak of 117.8 +- 77.4 keV (chi squared 53.7 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.5 +- 0.5 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+4.49 sec in the 15-150 keV band is
1.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.36 +- 0.08 (chi squared 60.5 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/529606/BA/


GRB_name: GRB120804A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13573
SUBJECT: GRB 120804A: Swift detection of a short burst
DATE:    12/08/04 01:07:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), S. T. Holland (STScI), J. A. Kennea (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 00:54:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120804A (trigger=529686).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 233.929, -28.761 which is 
   RA(J2000) = 15h 35m 43s
   Dec(J2000) = -28d 45' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a fast double-peaked
structure with a duration of about 1.5 sec.  The peak count rate
was ~15000 counts/sec (15-350 keV), at ~0.5 sec after the trigger. 

The XRT began observing the field at 00:55:47.8 UT, 93.6 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 233.94815, -28.78102 which is
equivalent to:
   RA(J2000)  = 15h 35m 47.56s
   Dec(J2000) = -28d 46' 51.7"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 94 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 (9.29 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.9
(+1.89/-1.67) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 96 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.23. 

Burst Advocate for this burst is A. Y. Lien (yarleen 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: GRB120803A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13574
SUBJECT: GRB 120803A: MITSuME Okayama Optical upper limits
DATE:    12/08/04 05:30:48 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 collaboration:

We observed the field of GRB 120803A (Racusin et al., GCNC 13565)
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 2012-08-03 14:07:49 UT (~6.8 h after the burst)
We did not find any new point source within the XRT circle
(Evans et al., GCNC 13569) 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
------------------------------------------------------
0.30747    14:45:01    3960.0   >19.7  >19.6  >18.8
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120803B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13575
SUBJECT: GRB 120803B: MITSuME Okayama Optical upper limits
DATE:    12/08/04 05:31:28 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 collaboration:

We observed the field of GRB 120803B (Racusin et al., GCNC 13566)
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 2012-08-03 11:46:48 UT (~41 min after the burst)
We did not find any new point source within the XRT circle
(Goad et al., GCNC 13571) in all the three bands.
We also could not detect the previously reported afterglow (Guidorzi et al.,
GCNC 13567).

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
------------------------------------------------------
0.06994    12:46:50    6360.0   >20.5  >20.2  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120804A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13577
SUBJECT: GRB 120804A: Enhanced Swift-XRT position
DATE:    12/08/04 06:42:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 797 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120804A, 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 = 233.94813, -28.78248 which is equivalent
to:

RA (J2000): 15h 35m 47.55s
Dec (J2000): -28d 46' 56.9"

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: GRB120802A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13578
SUBJECT: GRB 120802A: EVLA Observations
DATE:    12/08/04 06:59:47 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer and E. Berger (Harvard) report:

"We observed the position of GRB 120802A (Holland et al. GCN 13555)
with the EVLA beginning on 2012 Aug 03.65 UT (1.32 days after the burst).
No significant radio emission is detected at the enhanced Swift-XRT
position (Evans et al. GCN 13558) to three-sigma upper limits of 39 uJy and
60 uJy, at 6 GHz and 22 GHz, respectively."


GRB_name: GRB120804A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13579
SUBJECT: GRB 120804A: GROND upper limits
DATE:    12/08/04 09:07:02 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120804A (Swift trigger 529686; Lien et al.,
GCN 13573) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 02:22 UT on 2012-08-04, 1.5 hrs after the GRB
trigger. We do not detect any sources within the XRT position reported by
Osborne et al (GCN 13577). We do note that observations were severely
limited by unfavorable weather conditions, including moon-illuminated
visible cirrus towards the field.

Based on six co-added exposures of 370s (g'r'i'z') and 240s (JHK) taken
at a mean airmass of 1.3 and a mean seeing of 3.0", we derive the following
upper limits (all AB system):

g' > 21.9
r' > 22.1
i' > 22.0
z' > 21.9
J' > 20.6
H' > 20.0
K' > 19.5

The magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS
stars (JHK). The above upper limits are not corrected for the Galactic 
extinction
of E(B-V) = 0.23 mag along the line of sight (Schlegel et al. 1998).


GRB_name: GRB120804A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13580
SUBJECT: GRB 120804A: Swift-XRT refined Analysis
DATE:    12/08/04 13:07:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 9.2 ks of XRT data for GRB 120804A (Lien  et al. GCN
Circ. 13573), from 78 s to 28.8 ks after the  BAT trigger. The data
comprise 33 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 13577).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.11 (+/-0.03).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.98 (+0.21, -0.20). The
best-fitting absorption column is  3.5 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 9.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.3 x 10^-11 (7.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.5 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 9.3 x 10^20 cm^-2
Excess significance: 5.3 sigma
Photon index:      1.98 (+0.21, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00529686.

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


GRB_name: GRB120804A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13581
SUBJECT: GRB 120804A: Swift-BAT refined analysis
DATE:    12/08/04 13:20:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120804A (trigger #529686)
(Lien, et al., GCN Circ. 13573).  The BAT ground-calculated position is
RA, Dec = 233.951, -28.768 deg, which is 
   RA(J2000)  =  15h 35m 48.1s 
   Dec(J2000) = -28d 46' 06.1" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 24%.
 
The mask-weighted light curve shows two overlapping peaks starting
at ~T-0.2 sec, peaking at ~T+0.1 and ~T+0.5 sec, and ending at ~T+1.0 sec.
T90 (15-350 keV) is 0.81 +- 0.08 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.16 to T+0.83 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.08.  The fluence in the 15-150 keV band is 8.8 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.16 sec in the 15-150 keV band
is 10.8 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/529686/BA/


GRB_name: GRB120804A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13582
SUBJECT: GRB 120804A: Swift/UVOT Upper Limits
DATE:    12/08/04 13:40:29 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (PSU) and A. Y. Lien (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120804A
97 s after the BAT trigger (Lien et al., GCN Circ. 13573).
No optical afterglow consistent with the XRT position (Osborne et al.,
GCN Circ. 13577) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

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

white_FC            97          247          147         >21.4
u_FC               310          560          246         >20.7
white               97         5665          453         >22.0
v                  640         6077          432         >20.6
b                  566         6706          243         >20.9
u                  310         6692          659         >21.3
w1                 689         6487          413         >20.3
m2                4646         6282          393         >21.3
w2                4237         5872          393         >21.0

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


GRB_name: GRB120803B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13583
SUBJECT: GRB 120803B: Swift-XRT refined Analysis
DATE:    12/08/04 23:08:34 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) and J. L. Racusin (NASA/GSFC) report on behalf
of the Swift-XRT team:

We have analysed 4.4 ks of XRT data for GRB 120803B (Racusin  et al.
GCN Circ. 13566), from 79 s to 17.5 ks after the  BAT trigger. The data
comprise 31 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN. Circ 13571).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.25 (+0.07, -0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.2 (+/-0.4). The
best-fitting absorption column is  8.5 (+4.7, -2.8) x 10^21 cm^-2,
consistent with the Galactic value of 5.7 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 8.4 x 10^-11 (1.1 x
10^-10) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.5 (+4.7, -2.8) x 10^21 cm^-2
Galactic foreground: 5.7 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.2 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00529606.

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


GRB_name: GRB120804A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13584
SUBJECT: GRB 120804A: MITSuME Okayama Optical upper limits
DATE:    12/08/05 00:54:39 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 collaboration:

We observed the field of GRB 120804A (Lien et al., GCNC 13573)
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 2012-08-04 11:04:43 UT (~10.2 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 13577) 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
------------------------------------------------------
0.46585    12:05:03    6240.0   >19.9  >19.8  >19.1
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120804A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13585
SUBJECT: GRB 120804A: Swift-BAT Spectral lag analysis
DATE:    12/08/05 03:36:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

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

We report the spectral lag analysis for GRB 120804A (GCN Circ. 13573 & 13581)
based on the BAT data.  Using 8-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 16 +-12 msec, and -5 +-6 msec
for the 25-50 keV to 100-350 keV bands for both peaks combined.
These lag values place this burst in the short burst category.


GRB_name: GRB120804A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13586
SUBJECT: GRB 120804A: Gemini-North observations
DATE:    12/08/05 05:57:28 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock and E. Berger (Harvard) report on behalf of a larger 
collaboration:

We observed the position of the X-ray afterglow of the short GRB 120804A 
(Lien et al., GCN 13573) using GMOS on the Gemini-North 8-m telescope. 
Observations began at 05:47 UT on 2012 August 4 (approximately 4.9 hours 
after the BAT trigger).  We obtained 11x180s of observations in both the 
r and i filters.  We find a pair of faint sources in the i band 
observations within the enhanced XRT position (Osborne et al., GCN 
13577) with coordinates (J2000):

S1:  15:35:47.48, -28:46:56.2
S2:  15:35:47.53, -28:46:57.6

with astrometric errors of about 0.3" relative to 2MASS.  S1 is slightly 
brighter than S2 in i.  Neither source is detected in r.  Further 
observations are planned in order to search for variability of these 
sources.

We thank the Gemini staff, particularly Chad Trujillo, for their 
assistance with these observations.


GRB_name: GRB120804A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13587
SUBJECT: GRB 120804A:  EVLA Detection
DATE:    12/08/05 15:06:22 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

W. Fong, A. Zauderer, E. Berger (Harvard) report on behalf of a larger 
collaboration:

"We observed the position of the short GRB 120804A (Lien et al., GCN 
13573) with the EVLA at 5.8 GHz beginning 2012 Aug 4.97 UT (dt=0.93 d 
after the trigger).  We detect a radio source within the Swift-XRT error 
circle (Osborne et al., GCN 13577) at the position

RA    15:35:47.49 (+/- 0.01)
Dec  -28:46:56.7  (+/- 0.1)

Followup observations are planned."


GRB_name: GRB120805A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13588
SUBJECT: GRB 120805A: Swift detection of a burst
DATE:    12/08/05 21:57:05 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), S. T. Holland (STScI),
J. A. Kennea (PSU), O. M. Littlejohns (U Leicester),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 21:28:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120805A (trigger=530031).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 216.533, +5.802 which is 
   RA(J2000) = 14h 26m 08s
   Dec(J2000) = +05d 48' 08"
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 50 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 21:30:13.0 UT, 123.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 216.54056, 5.82571 which is equivalent
to:
   RA(J2000)  = 14h 26m 09.73s
   Dec(J2000) = +05d 49' 32.6"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 89 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.22
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of  90 seconds with the White filter
starting 126 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.03. 

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: GRB120805A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13589
SUBJECT: GRB 120805A: TAROT Calern observatory optical observations
DATE:    12/08/05 22:01:24 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120805A detected by SWIFT
(trigger 530031) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 77.2s after the GRB trigger
(19.3s after the notice). The elevation of the field decreased from
20 degrees above horizon and weather conditions
were moonlight.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the BAT error box
with a limiting magnitude of:
t0+77.2s to t0+137.2s : R > 15.9

The second image is 30.0s exposure in tracking mode:
t0+152.6s to t0+182.6s : R > 16.2

We co-added a series of exposures:
t0+152.6s to t0+851s : R > 17.4

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=353.7578 lat=+58.9832
and the galactic extinction in R band is about 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120805A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13590
SUBJECT: GRB120805A: Liverpool Telescope observations
DATE:    12/08/05 23:35:45 GMT
FROM:    David Bersier at Liverpool John Moores U  <dfb@astro.livjm.ac.uk>

David Bersier (LJMU), Drejc Kopac (Ljubljana) report

The Liverpool Telescope (La Palma) started robotic observations of GRB
120805A 3 minutes after detection by Swift (Troja et al, GCN 13588). We
find no credible afterglow candidate in the XRT error circle. We find
upper limits of 18.9 in the r band 30 minutes after burst and 18.7 in the
i band 47 minutes after burst.

[GCN OPS NOTE(06aug12): Per author's request, in the Subject-line the "120521C"
has been changed to "120805A".]


GRB_name: GRB120805A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13591
SUBJECT: GRB 120805A: 1.23m CAHA observations
DATE:    12/08/05 23:49:45 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), N. Huelamo (CAB-CSIC), R. Sanchez-Ramirez
(IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK), T. Kruehler (DARK),
A.J. Castro-Tirado (IAA-CSIC), J.C. Tello (IAA-CSIC), M. Jelinek
(IAA-CSIC), report on behalf of a larger collaboration:

"I-band observations conducted with the Calar Alto 1.23m telescope at
21:41:19.1--22:04:02.4 UT (obs started ~13 minutes post GRB) for GRB
120805A reveal no object inside the XRT position (GCN Circ. 13588) down to
I~18 (Vega). However, we note the presence an object located at
RA(J2000)=14:26:09.12, DEC(J2000)=05:49:31.7 (error of ~0.5" in both
coordinates) with a magnitude of I~17.5 which seems not to be at the SDSS.
Given the lack of a refined XRT position yet, we are cautious about the
possible relation of this object with the GRB 120805A optical afterglow."


GRB_name: GRB120805A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13592
SUBJECT: GRB 120805A: Swift-XRT refined Analysis
DATE:    12/08/06 09:57:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 6.1 ks of XRT data for GRB 120805A (Troja  et al. GCN
Circ. 13588), from 126 s to 13.6 ks after the  BAT trigger. The data
comprise 115 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
216.5411, +5.82554 which is equivalent to:

RA (J2000): 14 26 09.86
Dec(J2000): +05 49 31.9

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

The light curve can be modelled with a series of power-law decays. The
light curve initially rises, with an index alpha=-1.497 (+0.951,
-0.003). At T+191 s it breaks to an alpha of 2.33 (+0.14, -0.12) before
breaking again at T+2805 s to a final decay with index alpha=0.3
(+/-0.7).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.43 (+0.22, -0.20). The
best-fitting absorption column is  2.1 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 2.2 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 5.1 x 10^-11 (6.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      2.1 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: 3.7 sigma
Photon index:      1.43 (+0.22, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00530031.

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


GRB_name: GRB120802A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13593
SUBJECT: GRB 120802A: Swift/UVOT Upper Limits
DATE:    12/08/06 12:36:40 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI)
reports on behalf of the Swift/UVOT team:

     The Swift/UVOT observed the field of GRB 120802A starting 70 s
after the BAT trigger (Holland et al., 2012, GCNC 13555).  Settled
observations started at 87 s.  We do not detect any source inside the
UVOT-enhanced XRT error circle (Evans et al., 2012, GCNC 13558).
Preliminary magnitudes 3-sigma upper limits at this location for the
finding charts (FC) and the co-added images, are

Filter       TSTART   TSTOP   Exp Time    3-sigma UL
----------------------------------------------------
white (FC)      87      237        147         >20.8
    u (FC)     300      550        246         >19.9
----------------------------------------------------
    v          630   16,594       1317         >20.5
    b          555     6625        332         >20.4
    u          300     6548        658         >20.5
 uvw1          678   17,567        492         >20.4
 uvm2         4504   17,499       1279         >21.2
 uvw2         4095   11,737       1279         >21.4
white           87   10,731       1268         >22.1
----------------------------------------------------

    The quoted magnitudes and upper limits have not been corrected for
the Galactic extinction along the line of sight to this burst of
E_{B-V} = 0.14 mag (Schlafly et al. 2011, ApJS, 737, 103).


GRB_name: GRB120805A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13594
SUBJECT: GRB 120805A: Swift-BAT refined analysis
DATE:    12/08/06 13:44:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), E. Troja (NASA/GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+330 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120805A (trigger #530031)
(Troja, et al., GCN Circ. 13588).  The BAT ground-calculated position is
RA, Dec = 216.536, 5.853 deg, which is 
   RA(J2000)  =  14h 26m 08.5s 
   Dec(J2000) = +05d 51' 09.7" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.
 
The mask-weighted light curve shows several overlapping peaks starting at
~T-8 sec, peaking at ~T+8 sec, and returning to baseline around T+110 sec.
T90 (15-350 keV) is 48.00 +- 22.63 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.39 to T+32.61 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.20 +- 0.28.  The fluence in the 15-150 keV band is 8.2 +- 1.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+8.11 sec in the 15-150 keV band
is 0.37 +- 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/530031/BA/


GRB_name: GRB120728A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13595
SUBJECT: GRB 120728A: Fermi GBM observation
DATE:    12/08/06 17:24:10 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) reports on behalf of the Fermi GBM Team:

"At 22:25:13.737 UT on 28 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120728A (trigger 365207115 / 120728934)
which was also detected by the Swift/BAT (Cummings et al. 2012, GCN 13525).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 110 degrees.

The GBM light curve consists of multiple pulses
with a duration (T90) of about 32.8 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+23.6 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.66 +/- 0.10 and
the cutoff energy, parameterized as Epeak, is 119.80 +/- 30.80 keV.

The event fluence (10-1000 keV) in this time interval is
(5.29 +/- 0.27)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+13.12 s in the 10-1000 keV band
is 3.58 +/- 0.28 ph/s/cm^2.

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


GRB_name: GRB120805A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13598
SUBJECT: GRB 120805A: Swift/UVOT Upper Limits
DATE:    12/08/06 19:09:10 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and E. Troja (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120805A
127 s after the BAT trigger (Troja et al., GCN Circ. 13588).
No optical afterglow consistent with the refined XRT position (Burrows
et al., GCN Circ. 13592) 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              127         7557          579         >22.0
v                 1339        11924         1248         >20.8
b                 1265         7352          490         >21.5
u                 1240         7146          490         >20.5
w1                1216        13611         1253         >21.3
m2                1364        12829         1141         >21.6
w2                1487         7763          432         >21.6

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: GRB120804A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13601
SUBJECT: GRB 120804A: ATCA 34GHz upper limit
DATE:    12/08/07 03:17:14 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of
Sydney/CAASTRO), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI)

We observed GRB120804A (GCN 13573) with the Australia Telescope
Compact Array at 34GHz for 56 minutes centered on 04:35UT Aug 06 2012
(T0+2.15days).

We detect no radio source at the location of the GRB afterglow seen by
the EVLA (GCN 13587) and place a 3sigma upper limit of 200uJy on the
flux of an afterglow at 34GHz.

Further observations are planned.

These observations were obtained as part of ATCA project C2689. We
thank the observatory staff for their support and scheduling the
observations. The Australia Telescope is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.

[GCN OPS NOTE(07aug12): Per author's request, the "120824A" in the Subject-line
was changed to "120804A".]


GRB_name: GRB120807A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13602
SUBJECT: GRB 120807A: Swift detection of a burst
DATE:    12/08/07 07:23:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

F. E. Marshall (NASA/GSFC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), B.P. Gompertz (U Leicester),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 07:09:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120807A (trigger=530267).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 241.211, -47.490 which is 
   RA(J2000) = 16h 04m 51s
   Dec(J2000) = -47d 29' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak 
structure with a duration of about 15 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 07:10:49.4 UT, 71.6 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 241.2594,
-47.4797 which is equivalent to:
   RA(J2000)  = 16h 05m 02.26s
   Dec(J2000) = -47d 28' 47.0"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 123 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 (4.94 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 3.5
(+4.80/-2.19) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. 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 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: GRB120807A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13603
SUBJECT: GRB 120807A: Enhanced Swift-XRT position
DATE:    12/08/07 11:02:53 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1862 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120807A, 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 = 241.26016, -47.47972 which is equivalent
to:

RA (J2000): 16h 05m 2.44s
Dec (J2000): -47d 28' 47.0"

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

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

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


GRB_name: GRB120807A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13604
SUBJECT: GRB 120807A: Swift-BAT refined analysis
DATE:    12/08/07 11:58:57 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120807A (trigger #530267)
(Marshall, et al., GCN Circ. 13602).  The BAT ground-calculated position is
RA, Dec = 241.273, -47.455 deg, which is 
   RA(J2000)  =  16h 05m 05.6s 
   Dec(J2000) = -47d 27' 16.3" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
 
The mask-weighted light curves shows a single pulse starting at ~T-5 sec,
peaking at ~T+2 sec, and ending at ~T+20 sec.  T90 (15-350 keV) is
20.0 +- 5.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.24 to T+24.07 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.81 +- 0.30.  The fluence in the 15-150 keV band is 2.9 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.65 sec in the 15-150 keV band
is 0.9 +- 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/530267/BA/


GRB_name: GRB120807A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13605
SUBJECT: GRB 120807A: TAROT La Silla observatory optical observations
DATE:    12/08/07 14:39:04 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120807 detected by SWIFT
(trigger 530267) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 31.5s after the GRB trigger
(15.2s after the notice). The elevation of the field decreased from
8 degrees above horizon and weather conditions
were poor (due to the low elevation).

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the enhanced Swift-XRT position
(Evans et al. GCNC 13603) with a limiting magnitude of:
t0+31.5s to t0+91.5s : R > 15.5

Further images does not show OT anymore at about the
same limiting magnitude until 1500 seconds after the
trigger.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=333.3260 lat= +3.6420
and the galactic extinction in R band is about 4 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120804A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13606
SUBJECT: GRB 120804A: Gemini-North detection of an optical afterglow and putative host galaxy
DATE:    12/08/07 16:04:57 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We re-observed the location of the short-duration GRB 120804A (GCN
13573) with the Gemini Multi-Object Spectrograph (GMOS) mounted on the
Gemini-North 8-meter telescope to check for the presence of a fading
optical source. We obtained 16x180-sec of i-band observations in good
seeing conditions (FWHM=0.65") starting on 2012 August 07.30 UT, 3.3
days after the BAT trigger and 3.0 days after our initial observations
(GCN 13586).

Digital image subtraction of the two GMOS epochs using the ISIS
software package reveals a fading source slightly offset from the
center of S1, suggesting this to be the optical afterglow of GRB
120804A. There are no additional residuals in or around the refined
XRT position (improved upon from GCN 13577;
http://www.swift.ac.uk/xrt_positions/00529686/). Both S1 and S2 appear
to be extended, indicating that S1 is likely to be the
host galaxy of GRB 120804A and S2 is likely unrelated to the GRB.

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


GRB_name: GRB120807A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13607
SUBJECT: GRB 120807A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/08/07 17:15:41 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

A RAPTOR wide-field monitor located in Maui observed the location
of Swift trigger 530267 (Marshall et al., GCN 13602) during the period
that the Swift BAT was observing gamma-ray emission.  The 10 s exposure
began at 07:09:38.7 UTC -- 1 s after the Swift trigger and 1 s before
the gamma-ray emission reached peak intensity.  We detect no new object
at the location of the refined Swift XRT location (Beardmore et al., GCN
13603) to a 3-sigma limiting magnitude of 10.3.  Our unfiltered images
are calibrated to the Tycho-2 V-band.


GRB_name: GRB120807A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13608
SUBJECT: GRB 120807A: Fermi/LAT upper limit
DATE:    12/08/07 22:00:53 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

Weikang Zheng and Carl Akerlof (Umich), report on behalf of the ROTSE
collaboration:

We analyzed Fermi/LAT data of GRB 120807A (Marshall et al., GCN 13602)
as a follow-up of routine search in Swift trigger catalogs in our LAT
data processing pipeline using both the matched filter technique
(Akerlof et al. 2010, ApJ, 725, L15; 2011 ApJ, 726, 22; 2012,
arXiv:1205.3066; Zheng et al. 2012, ApJ 745,72; 2012, arXiv:1203.5113)
and likelihood method. We do NOT detect high energy photon emission from
both methods by using a standard data selection (with Energy above 100
MeV) in 47.5s duration.

The burst location was about 50 degree from the LAT boresight, and the
zenith angle was about 96 degrees at trigger time. This location is very
close to Galactic plane (gb = 333.3 and gb= 3.6 degree).

Using the likelihood method, we estimated the upper limit in LAT energy
range (0.1 - 10 GeV) is 1.27e-05 (photons cm^-2 s^-1) by assuming a
spectral index of -2.2.

The pipeline result is given in the following link:
http://rotse.net/LAT/SwiftTriggers/366016180/


GRB_name: GRB120802A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13609
SUBJECT: GRB 120802A: optical observations 
DATE:    12/08/07 23:37:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  GRB 120802A (Holland et al., GCN 13555) with 
0.45-m telescope ?f ISON-NM observatory  starting on  Aug. 02 (UT) 08:13:18 
(Elenin et al., GCN 13556).  We took  several unfiltered images of 30 s  and 
60 s exposures starting on Aug. 02, (UT)  08:13:18.  At the edge of the 
enhanced by UVOT field astrometry  XRT error circle 
(http://www.swift.ac.uk/xrt_positions/529486)  we marginally detect a source 
in coordinates 02:59:22.35  +13:46:07.2  (uncertainty of about 0.3 arsces in 
both coordinates).   A preliminary  photometry of  co-added frames is based 
on the USNO-B1.0 (R2)  nearby  stars is following:

T_start,     T0+,           Exposure, Object,
(UT)           mid, d         (s)

08:13:18    0.06905   6360          21.2+/-0.6

We suggest the source might be an optical afterglow of GRB 120802A, however 
at that time we cannot confirm the fading origin of the source. 


GRB_name: GRB120807A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13610
SUBJECT: GRB 120807A: Swift-XRT refined Analysis
DATE:    12/08/08 07:24:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), O.M.
Littlejohns (U. Leicester), G. Stratta (ASDC), P. D'Avanzo (INAF-OAB),
V. D'Elia (ASDC), J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows
(PSU) and F.E. Marshall report on behalf of the Swift-XRT team:

We have analysed 2.9 ks of XRT data for GRB 120807A (Marshall  et al.
GCN Circ. 13602), from 56 s to 75.9 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 Beardmore et al. (GCN. Circ
13603).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.29 (+0.15, -0.16).

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  1.04 (+0.25, -0.22) x 10^22 cm^-2,
in excess of the Galactic value of 4.9 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.8 x 10^-11 (1.4 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.04 (+0.25, -0.22) x 10^22 cm^-2
Galactic foreground: 4.9 x 10^21 cm^-2
Excess significance: 4.1 sigma
Photon index:      2.3 (+/-0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00530267.

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


GRB_name: GRB120804A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13611
SUBJECT: GRB 120804A: ATCA 34GHz upper limit
DATE:    12/08/08 10:29:43 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of
Sydney/CAASTRO), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI)

We observed GRB120804A (GCN 13573) with the Australia Telescope
Compact Array at 34GHz for 96 minutes centered on 04:35UT Aug 08 2012
(T0+4.15days).

We detect no radio source at the location of the GRB afterglow seen by
the EVLA (GCN 13587) and place a 3sigma upper limit of 120uJy on the
flux of an afterglow at 34GHz.

These observations were obtained as part of ATCA project C2689. We
thank the observatory staff for their support and scheduling the
observations. The Australia Telescope is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.


GRB_name: GRB120714B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13613
SUBJECT: GRB 120714B: GROND/FORS2 detection of a supernova
DATE:    12/08/09 18:34:32 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose (TLS), J. Greiner (MPE), J. Fynbo (DARK), A. Nicuesa Guelbenzu, 
S. Schmidl (both TLS), A. Rau (MPE), T. Kruehler (DARK), report on behalf 
of a larger collaboration:

GROND has been following the afterglow of GRB 120714B (Saxton et al., GCN 
13471) at z=0.398 (Fynbo et al., GCN 13477) since July 15 (Nicuesa 
Guelbenzu et al., GCN 13478). The light of the optical transient has been 
fading in all GROND optical bands during the first 1.5 days, was then 
flattening in r',i',z', and finally rising at about 3 days after the 
trigger (while it is flattening in g'). The data suggested that this 
behavior can be interpreted as an upcoming supernova component with a an 
early rise similar to the SN associated with GRB 011121 at z=0.36 (Bloom 
et al. 2002, ApJ 672, 45; Garnavich et al. 2003, ApJ 582, 924; Greiner et 
al. 2003, ApJ 599, 1223; Price et al. 2002, ApJ 572, 51).

Spectroscopy of the optical transient with VLT/FORS2 was performed on 
August 1/2, 18.3 days after the burst. Observations were done with the 
300V grism, covering the wavelength range from 445 to 865 nm, and lasted 
7200 sec. The spectrum reveals very broad features in the continuum with a 
prominent peak around 6500 A and broad lines of Si II and Ca II, in 
agreement with a broad-lined SN dominating the light of the optical 
transient. At present a decision between type Ib and Ic cannot be 
performed due to an uncomfortable presence of atmospheric features in the 
spectrum.

We thank the staff at ESO Paranal and ESO Garching for their excellent 
support and for performing the spectroscopy. GROND observations are 
continuing.


GRB_name: GRB120804A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13614
SUBJECT: GRB 120804A: Konus-Wind and Swift/BAT joint spectral analysis
DATE:    12/08/09 19:48:56 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. Baumgartner (GSFC/UMBC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), and T. Ukwatta (MSU)
on behalf of the Swift-BAT team,

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

The short GRB 120804A (Swift/BAT trigger #529686: Lien et al., GCN Circ.
13573, Baumgartner et al. GCN Circ. 13581) triggered Konus-Wind at
T0=3255.749 s UT (00:54:15.749), but since the incident angle on the
triggered detector was 99.2 deg (i.e. the burst accidentally triggered
the S2 detector which observes the northern ecliptic hemisphere,
although the burst came from the southern ecliptic hemisphere: b = -9.2
deg) the standard analysis of the Konus-Wind spectral data is impossible.

To derive the broad-band spectral parameters of this burst, we performed
joint spectral analysis of the Swift/BAT data and the Konus-Wind
3-channel spectral data (obtained in the waiting mode from the detector
S1), which covers the energy range from 24 keV to 1.4 MeV.

The time intervals of the spectral data are chosen for the Konus-Wind
from T0(BAT)-0.916 s to T0(BAT)+2.028 s (single KW bin which comprises
the burst) and for the Swift/BAT from T0(BAT)-0.16 s to T0(BAT)+0.83 s
(that is the BAT T100 interval), where T0(BAT) is the trigger time of
BAT at 00:54:14.18 UTC. The energy ranges which we used in the joint
spectral analysis are 24-1400 keV and 14-150 keV for the Konus-Wind and
the Swift/BAT respectively.  The spectral data of the two instruments 
are fitted with the spectral model multiplied by a constant factor to 
take into account the systematic effective area uncertainties in the 
response matrices of each instrument and the difference in the chosen 
intervals.

The spectrum is well fitted with a power-law with exponential cutoff
model: dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak). No systematic residual
from the best fit model is seen in the spectral data of each instrument.
The best fit spectral parameters are: alpha = -0.89 (-0.28, +0.24) and
Epeak = 135 (-29, +66) keV (chi2/dof = 56/58).

The energy fluence and 16-ms peak flux in the 15-1000 keV band
are 1.45 (-0.31,+0.30) x 10^-6 erg/cm2 and (6.0 Â± 2.7) x 10^-6 erg/cm2/s 
respectively.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120804_T03255/

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


GRB_name: GRB120803A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13615
SUBJECT: GRB 120803A: Confirmation of the X-ray afterglow
DATE:    12/08/10 07:37:50 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) and J.L. Racusin (NASA/GSFC) report
on behalf of the Swift-XRT team:

The Swift-XRT re-observed GRB 120803A on 2012 August 10, for 4.1 ks,
starting 5.7 days after the BAT trigger (Racusin et al., GCN Circ.
13565). The X-ray source reported by Evans et al. (GCN Circ. 13569) is
no longer detected, to a 3-sigma upper limit of 3.4e-3 ct/sec,
significantly below the level it was seen at previously.

We therefore conclude that this source was the afterglow of GRB 120803A.

The results of the automated analysis for this burst are available at
http://www.swift.ac.uk/xrt_products/00529582/

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


GRB_name: GRB120807A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13616
SUBJECT: GRB 120807A: Swift/UVOT Upper Limits
DATE:    12/08/10 14:32:49 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

GRB 120807A: Swift/UVOT Upper Limits

M. H. Siegel (PSU) 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 120807A
75 s after the BAT trigger (Marshall et al., GCN Circ. 13602).
No optical afterglow consistent with the XRT position (Beardmore et al., 
GCN Circ. 13603) 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            75          225          147         >20.6
u_FC               288          537          246         >20.4
white               75         1884          431         >21.8
v                  618         1935          156         >19.6
b                  543         1860          136         >20.4
u                  288         1835          363         >20.7
w1                 668         1810          136         >20.3
m2                1591         1611           19         >18.8
w2                 593         1910          117         >19.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.41 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120803A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13617
SUBJECT: GRB 120803A: optical upper limit
DATE:    12/08/10 18:19:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  possible Swift GRB 120803A (Racusin  et al., GCN 
13565; Evans  et al., GCN 13615) with 0.45-m telescope of  ISON-NM 
observatory  starting on  Aug. 03 (UT) 07:24:37.  We took  several 
unfiltered images of 30 s  exposures.  Within XRT error circle (Evans et 
al., GCN 13569) we do not detect any new source. A  photometry of  co-added 
frames is based on the USNO-B1.0 (R2)  nearby  stars is following:

T_start,     T0+,           Exposure, UL(3 sigma),
(UT)          mid, d         (s)

07:24:37    0.00258      4x30         17.3
07:24:37    0.01486    45x30         18.0


GRB_name: GRB120811A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13618
SUBJECT: Swift Trigger 530581: GRB 120811A or a galactic transient
DATE:    12/08/11 02:57:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B.-B. Zhang (PSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
C. Gronwall (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA)
and D. M. Palmer (LANL) report on behalf of the Swift Team:

At 02:35:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located a possible GRB (120811A, trigger=530581).  Swift did not slew to
the location.  The BAT on-board calculated location is 
RA, Dec 257.183, -22.736 which is 
   RA(J2000)  =  17h 08m 44s
   Dec(J2000) = -22d 44' 08"
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 30 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

This source was matched to a source 4U 1708-23 (== X Oph X-2)
in the on-board catalog, with an offset from 
the catalog position of 6 arcminutes.  However, the latest
position available is from the 1972 UHURU catalog, which has
a large position uncertainty consistent with this offset. 

At this time we cannot determine whether this is a GRB,
the catalogued 4U 1708-23, or some previously-unknown
Galactic transient. 

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


GRB_name: GRB120811B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13620
SUBJECT: IPN Triangulation of short hard GRB 120811B
DATE:    12/08/11 12:31:20 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

K. Hurley on behalf of the IPN,

V. Connaughton, M. Briggs, and C. Meegan, 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 hard GRB 120811B has been observed by Fermi (GBM: trigger
366337233), Konus-Wind, INTEGRAL (SPI-ACS), and Swift (BAT), so far, at
about 1230 s UT (00:20:30).

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:
     ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
      43.719 (02h 54m 53s) -30.233 (-30d 13' 58")
    Corners:
      43.568 (02h 54m 16s) -28.355 (-28d 21' 19")
      43.930 (02h 55m 43s) -27.828 (-27d 49' 40")
      43.853 (02h 55m 25s) -32.184 (-32d 11' 04")
      43.457 (02h 53m 50s) -32.775 (-32d 46' 30")
    ---------------------------------------------
The error box area is 1.39 sq. deg, and its maximum dimension is 4.96 deg.

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120811_T01231/IPN/

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


GRB_name: GRB120811B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13621
SUBJECT: Konus-Wind observation of GRB 120811B
DATE:    12/08/11 13:28:20 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short-duration hard GRB 120811B
(IPN localization: Golenetskii at al., GCN 13620)
triggered Konus-Wind at T0=01231.575s UT (00:20:31.575)

The light curve shows a double pulse,
a total duration of the burst is ~0.33 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120811_T01231/

As observed by Konus-Wind the burst
had a fluence of 4.6(-0.9,+1.0)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0,
of 2.8(-0.6,+0.7)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 7 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.14 (-0.28, +0.35),
and Ep = 1130(-230, +310) keV,
chi2 = 13.6/24 dof.

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


GRB_name: GRB120811C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13622
SUBJECT: GRB 120811C: Swift detection of a burst with an optical counterpart
DATE:    12/08/11 15:52:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. N. Barlow (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. Grupe (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 15:34:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120811C (trigger=530689).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 199.709, +62.291 which is 
   RA(J2000)  =  13h 18m 50s
   Dec(J2000) = +62d 17' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single bright peak
with a duration of about 35 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 15:36:00.8 UT, 68.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 199.6833, 62.3027 which is equivalent to:
   RA(J2000)  = +13h 18m 43.99s
   Dec(J2000) = +62d 18' 09.7"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 60 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 2.97e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 13:18:43.81 = 199.68253
  DEC(J2000) = +62:18:02.7  =  62.30076
with a 90%-confidence error radius of about 0.75 arc sec. This position is 7.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.40 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is B. N. Barlow (bnb2 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13623
SUBJECT: GRB 120811C: MASTER-Amur observations of fading OT
DATE:    12/08/11 20:32:22 GMT
FROM:    Denis Denisenko at SAI MSU  <d.v.denisenko@gmail.com>

D. Denisenko, E. Gorbovskoy, V. Lipunov, 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

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. Krushinski, I. Zalozhnich, A. Popov, A. Bourdanov, A. Punanova
Ural Federal University

H. Levato, C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez, F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)
report:

MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Blagoveschensk was pointed to GRB 120811C (Barlow et al.,
GCN 13622) 665 sec after GRB time, at 2012-08-11 15:45:57 UT.
Observations were performed simultaneously in two tubes with mutually
perpendicular polarizations. First two pairs of images were obtained with
130 and 160 sec exposures, followed by the set of 180-sec exposures.
On our images we find the fading optical transient at the coordinates:

  R.A. (J2000) = 13 18 44.01
  Dec. (J2000) = +62 18 02.7

which are consistent with the position of UVOT candidate afterglow
reported in GCN 13622.

Photometry of GRB 120811C afterglow was performed using SDSS
J131828.08+621651.3 (r=14.74) as the reference star. To improve the
signal-to-noise ratio, images were combined by four. The resulting
magnitudes of the afterglow in the Western tube with a better image
quality (FWHM=2.6-3.2") are listed in the Table below.

----------------------------------------------
T_mid UT | T-T0, s | Exptime |  Mag. | Mag.err
---------+---------+---------+-------+--------
15:51:48 | 1016    |  650    |  18.4 |  0.10
16:04:46 | 1794    |  720    |  18.9 |  0.17
16:18:37 | 2625    |  720    |  19.3 |  0.27
16:32:27 | 3455    |  720    |  19.0 |  0.24
16:46:16 | 4284    |  720    | <19.5 |  N/A
17:00:04 | 5112    |  720    | <19.5 |  N/A
----------------------------------------------

The detailed analysis of the complete data set is continuing.

This message can be cited.


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13624
SUBJECT: GRB 120811C: TAROT Calern observatory optical observations
DATE:    12/08/11 21:03:08 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120811C detected by SWIFT
(trigger 530689) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 3.98h after the GRB trigger.
The elevation of the field decreased from
50 degrees above horizon and weather conditions
were good.

We co-added a series of exposures but we do not find
any optical transcient at the afterglow position
(Barlow et al. GCNC 13622, Denisenko et al. GCNC 13623):

-------------------------------
T-T0 start | T-T0 End |  Mag. |
-----------+----------+-------+
    246 min |  313 min | >19.5 |
-------------------------------

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB120811C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13625
SUBJECT: GRB 120811C: Enhanced Swift-XRT position
DATE:    12/08/11 21:13:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1291 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120811C, 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 = 199.68285, +62.30068 which is equivalent
to:

RA (J2000): 13h 18m 43.88s
Dec (J2000): +62d 18' 02.4"

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: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13626
SUBJECT: GRB 120811C: RTT150 optical observations
DATE:    12/08/11 21:53:06 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

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

report:

We observed the field of the Swift-BAT GRB 120811C (Barlow et al. GCN
13622) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe,
TUBITAK National Observatory, Turkey), starting at 11 Aug, 18:52 UT,
i.e. approximately 3.3 hours after the burst, using TFOSC
instrument. We made a serie of 300-600s images in R and V.

The afterglow is detected at the position:

RA=13:18:43.83, DEC=62:18:02.6 (J2000)

with positional error about 0.1 arcsec, which is consistent with that
measured by UVOT and MASTER (Denisenko et al., GCN 13623).

We measured the afterglow magnitude as m_R=20.00+-0.05 (calibrated
relative to USNO-B1 stars). Observations are continuing.


GRB_name: GRB120811B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13627
SUBJECT: Improved IPN error box for short hard GRB 120811B
DATE:    12/08/11 22:11:15 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

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

V. Connaughton, M. Briggs, and C. Meegan, 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:

This burst (GCN 13620) was also observed by MESSENGER (GRNS). We have
triangulated it to an improved, but still preliminary 3 sigma error box
whose coordinates are:
    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
      43.658 (02h 54m 38s) -31.675 (-31d 40' 29")
    Corners:
      43.770 (02h 55m 05s) -32.366 (-32d 21' 59")
      43.820 (02h 55m 17s) -31.614 (-31d 36' 51")
      43.545 (02h 54m 11s) -30.978 (-30d 58' 42")
      43.495 (02h 53m 59s) -31.735 (-31d 44' 06")
    ---------------------------------------------
The error box area is 734  sq. arcmin, and its maximum
dimension is 84 arcmin.

This error box is fully contained within the previous IPN error box (GCN 
13620).

This box can be further improved.

An updated triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120811_T01231/IPN/


GRB_name: GRB120811C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13628
SUBJECT: GRB 120811C: Redshift from OSIRIS/GTC 
DATE:    12/08/11 23:14:09 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

C. C. Thoene (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK), 
J. Gorosabel, R. Sanchez-Ramirez (IAA-CSIC) and 
J. P. U. Fynbo (DARK) G. Gomez Velarde (GTC) report 
on behalf of a larger collaboration:

We observed the afterglow of GRB 120811C (Barlow et al., 
GCN 13622) with OSIRIS at the 10.4m GTC telescope starting at 
UT 22:07 (6.5 hr after the burst) for a total exposure time of 2400s. 
We used grism 1000B covering the wavelength range between 
3700 and 7800 Angstrom. 

Despite Calima, the continuum is clearly detected and the 
spectrum shows strong Ly alpha and Ly beta absorption as well 
as a number of absorption lines (SII, SiII, OI, CII, CIV, SiIV, AlII, 
AlIII, NiII, ZnII and SiII*) at a common redshift of z=2.671. 


GRB_name: GRB120811C
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13629
SUBJECT: GRB 120811C: Swift/UVOT Detection
DATE:    12/08/12 01:58:39 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 120811C
76 s after the BAT trigger (Barlow et al., GCN Circ. 13622).
A source consistent with the XRT position Evans et al., GCN Circ.
13625 is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  13:18:43.82 = 199.68258 (deg.)
    Dec (J2000) = +62:18:02.8  =  62.30077 (deg.)
with an estimated uncertainty of 0.52 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               76          226          147         18.59 +/- 0.05
v                  620         1243           78         18.49 +/- 0.19
b                  544          739           39         18.95 +/- 0.19
u                  288          538          246         18.61 +/- 0.09
w1                 670         1464           97        >20.0
m2                 819         1439           78        >20.5
w2                 595         1219           78        >19.7

The absence of a detection in the uv bands is consistent with the reported
redshift from Thoene et al., GCN Circ. 13628.

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: GRB120811C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13630
SUBJECT: GRB 120811C: Swift-XRT refined Analysis
DATE:    12/08/12 06:52:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 6.5 ks of XRT data for GRB 120811C (Barlow  et al. GCN
Circ. 13622), from 56 s to 40.2 ks after the  BAT trigger. The data
comprise 137 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 Evans et
al. (GCN. Circ 13625).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.12 (+0.13, -0.14). At T+224 s  the decay
flattens to an alpha of 0.44 (+0.12, -0.27) before breaking again at
T+1468 s to a final decay with index alpha=1.06 (+0.19, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.74 (+0.14, -0.13). The
best-fitting absorption column is  1.08 (+0.22, -0.20) x 10^21 cm^-2,
in excess of the Galactic value of 2.1 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.00 (+/-0.15) and a
best-fitting absorption column of 8.8 (+3.4, -3.1) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (4.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.8 (+3.4, -3.1) x 10^20 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 3.6 sigma
Photon index:      2.00 (+/-0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00530689.

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


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13631
SUBJECT: GRB 120811C: Bassano Bresciano Observatory optical observations
DATE:    12/08/12 07:26:59 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli, A.Quadri report:

We imaged the field of GRB 120811C detected 
by SWIFT(trigger 530689) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy.

The observations started 266min. after the 
GRB trigger,with our schmidt telescope 
D=320 mm F/D=3.1.

Weather conditions were good.

We co-added a series of 30 exposures.

We did not found any optical counterpart 
in the error box of the XRTcandidate
(Barlow et al. GCNC 13622).

Start      End       Vlim
266min     326min    19.2

Magnitudes were estimated with the UCAC-3 

The message may be cited.


GRB_name: GRB120811C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13632
SUBJECT: GRB 120811C: NOT redshift
DATE:    12/08/12 11:54:19 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

J. P. U. Fynbo (DARK/NBI), D. Xu (WIS), P. Jakobsson (U. Iceland), D.
Armstrong (U. Warwick), R. Cardenes (NOT) report on behalf of a larger
collaboration:

We observed the optical afterglow of GRB 120811C (Barlow et al., GCN
13622) using the 2.5m Nordic Optical Telescope (NOT) equipped with
ALFOSC. Spectroscopic observations started at  21:58 UT on 2012-08-11
(i.e., 6.4 hr after the BAT trigger) with exposure time of 3x1800s,
covering the wavelength range of ~3800A to ~8000A. The afterglow was
detected in each of the 1800s frames though the weather was dusty to a
certain degree.

The spectrum exhibits a clear Damped Lyman Alpha (DLA) absorption
feature at about 4460A. Redward of Lyman alpha the spectrum shows
quite a few significant absorption lines, including Si II, O I, C II,
C IV, Si IV, all at a common redshift of z=2.67, in good agreement
with the measurement in Thoene at al. (GCN 13628).


GRB_name: GRB120811A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13633
SUBJECT: GRB 120811A: Swift-BAT refined analysis
DATE:    12/08/12 12:26:25 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU), B.-B. Zhang (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120811A (trigger #530581)
(Zhang, et al., GCN Circ. 13618).  The BAT ground-calculated position is
RA, Dec = 257.184, -22.735 deg, which is 
   RA(J2000)  =  17h 08m 44.1s 
   Dec(J2000) = -22d 44' 06.7" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
 
The mask-weighted light curve shows two overlapping peaks starting at
~T-20 sec, peaking at ~T+2 sec, ending at ~T+25 sec with a flat section out to
~T+160 sec.  T90 (15-350 keV) is 166 +- 52 sec (estimated error including
systematics).
 
The time-averaged spectrum from T-14.16 to T+169.06 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.20.  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+0.43 sec in the 15-150 keV band
is 1.0 +- 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/530581/BA/

While the BAT lightcurve and spectral results are consistant with
a GRB origin for this trigger, given that the galactic coordinates
are (lon,lat)=(0.6,10.3) deg, we cannot rule out a galactic source origin.


GRB_name: GRB120811C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13634
SUBJECT: GRB 120811C: Swift-BAT refined analysis
DATE:    12/08/12 13:43:42 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), B. N. Barlow (PSU), S. D. Barthelmy (GSFC),
T. Sakamoto (GSFC/UMBC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), 
N. Gehrels (GSFC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120811C (trigger #530689)
(Barlow, et al., GCN Circ. 13622).  The BAT ground-calculated position is
RA, Dec = 199.690, 62.297 deg, which is 
   RA(J2000)  =  13h 18m 45.5s 
   Dec(J2000) = +62d 17' 50.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
 
The mask-weighted light curve shows a nearly symmetric peak starting at ~T-10 sec,
peaking at ~T+6 sec, and ending at ~T+40 sec.  T90 (15-350 keV) is 26.8 +- 3.7 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-9.7 to T+42.9 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.40 +- 0.30, 
and Epeak of 42.9 +- 5.7 keV (chi squared 59.5 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.0 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+5.27 sec in the 15-150 keV band is
4.1 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.04 +- 0.06 (chi squared 74.5 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/530689/BA/


GRB_name: GRB120811C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13635
SUBJECT: GRB 120811C: MASTER-Tunka OT observations
DATE:    12/08/13 07:05:34 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
  Irkutsk State University

  E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, 
N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, 
A.Kuznetsov, A.Sankovich
  Sternberg Astronomical Institute, Moscow 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.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 Tunka was pointed to the  GRB120811C (Barlow et al., GCN 13622) 
40 sec s after notice time and 676 sec after GRB time at 2012-08-11 15:46:08.449 UT. On our 
first (130s exposure) set we have found OT  within SWIFT-BAT error-box in 
two polarizations.

The preliminary robotic photometry (m=0.2B + 0.8R, Usno B magnitudes) is:

datetime                    coord2000           Band     mag   error

2012-08-11 15:46:08.449 13h 18m 43.90s , +62d 18m 02s.1 P| 17.3 0.2
2012-08-11 15:46:09.684 13h 18m 43.86s , +62d 18m 02s.3 P- 17.2 0.1
2012-08-11 15:49:12.268 13h 18m 43.76s , +62d 18m 02s.3 P| 17.6 0.2
2012-08-11 15:49:12.282 13h 18m 43.93s , +62d 18m 02s.6 P- 17.6 0.2
2012-08-11 15:52:52.452 13h 18m 43.75s , +62d 18m 01s.8 P| 17.8 0.2

So, MASTER-Net have simultaneous optical observations in four 
polarizations (see Denisenko et al., GCN 13623) of GRB120811C.

The message may be cited.


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13636
SUBJECT: GRB 120811C: RTT150 optical observations
DATE:    12/08/13 17:29:30 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

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

report:

We continued the observations of the field of the Swift-BAT GRB
120811C (Barlow et al. GCN 13622, Galeev et al., GCN 13626) with
Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey). The second epoch observations were started at 
12 Aug, 18:38 UT, i.e. approximately 27.05 hours after the burst. We made
a serie of 300s images in R using TFOSC instrument.

The afterglow was clearly detected in the combined image. Using
USNO-B1 stars as reference, we estimated the afterglow magnitude as
m_R=22.3+-0.2.

Fitting this point together with the data from RTT150 first epoch
observations (Galeev et al., GCN 13626), gives the power law decay
with index alpha = 1.04 +- 0.05, consistent with late time decay in
X-rays, as it was observed with XRT (Evans et al., GCN 13630).

When all RTT150 data are compared with the data of MASTER telescopes
(Denisenko et al., GCN 13623, Ivanov et al., 13635), the power law
break at few hours time scale is found, approximately consistent with
the position of second break observed in X-rays with XRT (Evans et
al., GCN 13630). However, better cross-calibration between RTT and
MASTER photometry should be done for more reliable light curve
modelling.

The light curve and direct images of the field can be found at:

http://hea.iki.rssi.ru/grb/120811c/indexeng.html


GRB_name: GRB120811C
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13637
SUBJECT: GRB 120811C: EVLA Observations
DATE:    12/08/13 20:49:36 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer and E. Berger (Harvard) report:

"We observed the position of GRB 120811C (Barlow et al. GCN 13622) with the
EVLA at 2012 Aug 11.79 UT (1.14 days after the burst). No significant radio
emission is detected at the enhanced Swift-XRT position (Evans et al. GCN
13625), the UVOT position (Kuin et al. GCN 13629) or optical position
(Denisenko et al. GCN 13623; Galeev et al. GCN 13626; Ivanov et al. GCN
13635), to a three-sigma upper limit of 76 uJy at 6.0 GHz."


GRB_name: GRB120805A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13638
SUBJECT: GRB 120805A: Enhanced Swift-XRT position
DATE:    12/08/14 08:26:46 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:

We have reinvestigated the XRT position of GRB 120805A. Using 2.6 ks of
XRT Photon Counting mode data and 2 UVOT images, we find an
astrometrically corrected X-ray position (using the XRT-UVOT alignment
and matching UVOT field sources to the USNO-B1  catalogue): RA, Dec =
216.53836, 5.82525 which is equivalent to:

RA (J2000):  14 26 09.21
Dec (J2000): +05 49 30.9

with an uncertainty of 2.7 arcsec (radius, 90% confidence). This
position is 10" from the unenhanced XRT position reported in GCN Circ.
13592. The size of the astrometric correction, which is responsible for
this shift, was such that the enhanced position was initially rejected 
and not circulated automatically. Position enhancement is described by 
Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 
1177).

This corrected position is our best XRT position, and is 1.5 arcsec from
the optical counterpart proposed in GCN Circ. 13591, supporting the
identification of that source as the afterglow. We thank Daniele
Malesani for drawing this to our attention.

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


GRB_name: GRB120805A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13639
SUBJECT: GRB 120805A: optical afterglow confirmation from the NOT
DATE:    12/08/14 12:10:51 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani, T. Kruehler (DARK/NBI), A. de Ugarte Postigo (IAA/CSIC and 
DARK/NBI), D. Xu (WIS), N. R. Tanvir (Univ. Leicester), J. Gorosabel 
(IAA/CSIC), P. Jakobsson (Univ. Iceland), S. Geier (NOT and DARK/NBI), 
T. Pursimo (NOT), report on behalf of a larger collaboration.

We observed the field of GRB 120805A (Troja et al., GCN 13588) on two 
epochs with the NOT optical telescope, located in La Palma (Canary 
Islands). The two observations were carried out on mean dates Aug 5.936 
and 13.896 UT, that is 1.0 hr and 8.0 days after the GRB, respectively.

The source first noticed by Gorosabel et al. (GCN 13591) is detected in 
both our images, and it varied significantly between the two epochs, as 
well as compared to the CAHA report (Gorosabel et al., GCN 13591). We 
note that the object position is now fully consistent with the revised 
XRT error circle (Evans, GCN 13638). We thus conclude that this source 
is the optical afterglow of GRB 120805A.

The source varied by only about 2 mag between the two NOT epochs 
(corresponding to a power-law decay slope of ~0.3), suggesting that in 
the later image the host galaxy could be contributing to the total light.

A picture showing the two NOT epochs is posted at this URL:

http://www.astro.ku.dk/~malesani/GRB/120805A/GRB120805A_comparison.jpg

We thank Phil Evans for discussion about the XRT localization of this 
afterglow.


GRB_name: GRB120804A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13640
SUBJECT: GRB120804A: Chandra observations and afterglow detection
DATE:    12/08/14 12:30:14 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

E. Troja (NASA/GSFC/UMCP), T. Sakamoto (NASA/GSFC/UMCB),
N. Gehrels (NASA/GSFC), D. Donato (NASA/GSFC/UMCP),
and J. L. Racusin (NASA/GSFC) report:

We observed the field of GRB 120804A (Lien et al., GCN Circ. 13573) with
the Chandra ACIS-S starting on August 13, 2012 10:52:08 UT (~9.4 d after
the GRB trigger) for a total exposure of 19.8 ks. Within the Swift/XRT
enhanced position (Osborne et al., GCN Circ. 13577) we clearly detect a
source at Ra, Dec = 233.94786, -28.7823 which is equivalent to:

RA (J2000) = 15h 35m 47.49s
Dec (J2000) = -28d 46' 56.3"

with an uncertainty of 0.6 arcsec (radius, sys+stat, 90% containment).
This position is consistent with the putative host galaxy S1
(Chornock et al., GCN Circ. 13586).

The X-ray afterglow is detected at a count rate of (1.6 +/- 0.3)E-03 cts/s
(0.5-8.0 keV). By using the spectral parameters derived from the Swift/XRT
observations (Stroh et al., GCN Circ. 13580) we estimate an observed X-ray
flux of (1.5 +/-0.3)E-14 erg/cm2/s in the 0.3-10 keV energy band.
Our measurement is consistent with the power-law decay of ~1.1 reported
by Stroh et al. (GCN Circ. 13580), and sets a lower limit to the jet-break
time of t_j>9 d.


We thank Harvey Tananbaum and the entire Chandra staff for approving and
rapidly executing this observation.


GRB_name: GRB120811A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13641
SUBJECT: GRB 120811A: Swift/XRT-UVOT Obseravations
DATE:    12/08/14 15:57:21 GMT
FROM:    Binbin Zhang at PSU  <buz12@psu.edu>

B.-B. Zhang (PSU), S. R. Oates (UCL-MSSL),  K. L. Page (U Leicester), P.A.
Evans (U. Leicester), D. N. Burrows (PSU), J. R. Cummings (GSFC/UMBC),  J. A.
Kennea (PSU),H. A. Krimm (GSFC/USRA), E. Helder (PSU) and S. D. Barthelmy
(GSFC) report on behalf of the Swift-XRT and Swift-UVOT team: 

We report further Swift XRT-UVOT observations of GRB 120811A (Zhang et al,  GCN
13618).

We performed 9.1 ks follow-up XRT observations of the field at T0+1.6 hr,
T0+0.27 day, T0+0.94 days and T0+3.1 days (where T0 = 2012 Aug 11 at 02:35:18
UT ), in order to determine whether or not the X-ray source had faded. We find
a fading source with count rates in the 0.3-10 keV band as follows :

T-T0                     Count Rate
(5.8+/-0.2)x10^3 s   0.05+/-0.01 count/s
(2.2+/-0.01)x10^4 s   0.02+/-0.01 count/s
(8.1+/-0.03)x10^4 s  0.02+/-0.001 count/s
(2.7+/-0.2)x10^5 s   < 0.005 count/s

The data are entirely in Photon Counting (PC) mode. Using 1227 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 =
257.16542, -22.71054 , which is equivalent to:

RA (J2000): 17h 08m 39.70s
Dec(J2000): -22d 42' 38.0"

with an uncertainty of 2.8 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay index of
alpha=0.31 (+0.13, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+/-0.5). The best-fitting
absorption column is  7.4 (+4.2, -3.0) x 10^21 cm^-2, in excess of the Galactic
value of 1.5 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is
5.5 x 10^-11 (9.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.4 (+4.2, -3.0) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      1.9 (+/-0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00530581.

The fact that the XRT source is fading suggests that Swift trigger 530581
(Zhang et al., GCN Circ. 13618) is most likely a GRB.

The Swift/UVOT began settled observations of the field of GRB 120811A 5627 s
after the BAT trigger (Zhang  et al., GCN Circ. 13618). No optical afterglow
consistent with the XRT position is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system(Breeveld et
al. 2011,AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

white           6243        6443         197        > 20.7    
v               6654        6853         197        > 19.1    
b               6038        7593         313        > 20.2    
u               5832        7468         393        > 20.0     
uvw1            5627        7263         393        > 19.9
uvw2            6449        6649         197        > 19.8    

The magnitudes in the table are not corrected for the Galactic extinction due
to the reddening of E(B-V) = 0.77 in the direction of the burst (Schlegel et
al. 1998).

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


GRB_name: GRB120811C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13642
SUBJECT: GCN for GRB 120811C
DATE:    12/08/14 20:33:25 GMT
FROM:    Peter Jenke at MSFC  <pjenke@aol.com>

Peter Jenke (MSFC/NPP) reports on behalf of the Fermi GBM Team:

"At 15:34:55.09 UT on 11 August 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120811C (trigger 366392098 / 120811649)
which was also detected by the Swift/BAT (Barthelmy et al. 2012, GCN 13622).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 133 degrees.

The GBM light curve consists of a single pulse 
with a duration (T90) of about 14.3 s (50-300 keV).
The time-averaged spectrum from T0-6.14 s to T0+10.24 s is
best fit by a power law function with an exponential high-energy cutoff.  
The power law index is -0.71 +/- 0.20 and the cutoff energy, 
parameterized as Epeak, is 54 +/- 3 keV.

The event fluence (10-1000 keV) in this time interval is
(2.98 +/- 0.08)E-06 ergs/cm^2. The 1-sec peak photon flux measured
starting from T0+3.072 s in the 10-1000 keV band
is 5.9304 +/- 0.55  ph/s/cm^2.

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


GRB_name: GRB120804A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13643
SUBJECT: GRB 120804A: Possible temporal break in the X-ray light-curve
DATE:    12/08/14 20:56:06 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We analyzed the Swift-XRT and Chandra observations of the short GRB
120804A (Lien et al. GCN 13573; Troja et al., GCN 13640). Using the data at
t>10^4 sec, when the light curve appears less susceptible to variability,
we find moderate evidence for a temporal break with a pre-break index of
alpha1= 0.7 +\- 0.1, a post-break index of alpha2= 1.9 +\- 0.5, and a break
time of about 2x10^5 sec. The F-test indicates 5% probability of chance
improvement with respect to a single power-law fit.  Plots are available
from:

https://www.cfa.harvard.edu/~rmargutt/flux_lightcurvefitBPL.pdf
https://www.cfa.harvard.edu/~rmargutt/flux_lightcurvefitSPL.pdf

Further X-ray observations are required to clarify the nature/presence of
the temporal break."


GRB_name: GRB120811B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13644
SUBJECT: GRB 120811B: Fermi GBM observation
DATE:    12/08/15 02:22:29 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) and Chip Meegan (USRA)
report on behalf of the Fermi GBM Team:

"At 00:20:31.288 UT on 11 August 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120811B (trigger 366337233 / 120811014),
which was also located by the IPN (S. Golenetskii et al. 2012, GCN 13627).
The GBM on-ground location is consistent with the IPN position.
The angle from the Fermi LAT boresight is 85 degrees.

The GBM light curve consists of two pulses
with a duration (T90) of about 0.448 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.384 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.29 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 1294 +/- 145 keV.

The event fluence (10-1000 keV) in this time interval is
(2.45 +/- 0.10)E-6 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.064 s in the 10-1000 keV band
is 21.0 +/- 1.3 ph/s/cm^2.

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


GRB_name: GRB120815A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13645
SUBJECT: GRB 120815A: Swift detection of a burst
DATE:    12/08/15 02:24:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. Pagani (U Leicester), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team:

At 02:13:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120815A (trigger=531003).  Swift will execute a delayed slew
due to Earth-limb observing constraint.  The BAT on-board calculated location
is RA, Dec 273.955, -52.134, which is 
   RA(J2000)  =  18h 15m 49s
   Dec(J2000) = -52d 08' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single pulse 
with a duration of about 10 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+40.6
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is C. Pagani (cp232 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: GRB120815A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13646
SUBJECT: GRB 120815A: TAROT La Silla observatory optical observations
DATE:    12/08/15 03:28:29 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120815A detected by SWIFT
(trigger 531003) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 34.7s after the GRB trigger
(15.4s after the notice). The elevation of the field decreased from
65 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+34.7s to t0+94.7s : R > 16.3

The second image is 30.0s exposure in tracking mode:
t0+108.0s to t0+138.0s : R > 18.4

We co-added a series of exposures from t0+108s to t0+1605s.
Due to the annouced slew delay announced by Pagani et
al. (GCNC 13645), we analyze the BAT error box.
We compared the co-added TAROT images with the
NOMAD1 catalog sources. Three non catalogued sources
could be an optical counterpart candidate:

ID ra(J2000)    dec(J2000)  Rmag
T1 18:15:57.33 -52:07:35.6  18.5
T2 18:15:58.58 -52:07:27.5  19.0
T3 18:15:35.22 -52:05:21.4  18.3

These sources does not appear in the R filtered DSS image.
The sources does not show any significant brightness
variation durong 20 min. but they are close to the
limiting magnitude in the individual images.
Few other fainter sources are also present in the
TAROT image.

More informations can be found at the following URL:

http://cador.obs-hp.fr/grb120815a

Magnitudes are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=342.0422 lat=-15.9869
and the galactic extinction in R band is about 0.3 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120815A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13647
SUBJECT: GRB 120815A: Swift-XRT observations
DATE:    12/08/15 03:47:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

The XRT began observing the field of GRB 120815A at 02:58:45.5 UT,
2686.8 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 273.95896,
-52.12978 which is equivalent to:
   RA(J2000)  = 18h 15m 50.15s
   Dec(J2000) = -52d 07' 47.2"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 17 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (8.55 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.6
(+1.61/-1.45) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB120815A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13648
SUBJECT: GRB 120815A: GROND afterglow candidate
DATE:    12/08/15 03:57:22 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

V. Sudilovsky (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 120815A (Swift trigger 531003; Pagani
et al., GCN 13645) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile). Observations started 150 seconds after the BAT
trigger, and were obtained at airmass 1.1 and a mean seeing of 1".3.

Based on exposures of 142 seconds in g'r'i'z' and 240 seconds in JHK
centered 348 seconds after the trigger, we detect an uncataloged source in
all bands at

RA (J2000): 18:15:49.82
DEC (J2000): -52:07:52.1

with an uncertainty of 0.3".

This position is close to the Swift XRT position (J. A. Kennea et al., 
GCN 13647).

We measure a preliminary magnitude:

i' ~ 17.6

The magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS
stars (JHK).


GRB_name: GRB120815A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13649
SUBJECT: GRB 120815A: VLT/X-shooter redshift
DATE:    12/08/15 05:40:11 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), S. Schulze (PUC and MCSS), A. de Ugarte Postigo 
(IAA/CSIC and DARK/NBI), D. Xu (WIS), V. D'Elia (INAF/Roma and 
ASI/ASDC), J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (Univ. Leicester), 
report on behalf of a larger collaboration:

We observed the field of GRB 120815A (Pagani et al., GCN 13645) with the 
VLT/X-shooter spectrograph. We confirm the presence of a bright, 
uncatalogued object consistent with the GROND position (Sudilovsky et 
al., GCN 13648). From the acquisition images, we measure R = 18.9 for 
the afterglow at an epoch of 1.67 hr after the GRB (calibrated to nearby 
USNO stars).

Our spectra cover the wavelength range 3000-25000 AA, and were taken 
starting on 2012 Aug 15.163 UT (1.69 hr after the GRB), for a total of 
40 min exposure. Continuum from the afterglow is detected with high S/N 
in all of the UVB, VIS, and NIR arms.

The spectrum shows a wide trough and a multitude of strong absorption 
lines, which we interpret as due to a DLA and metal transitions of N V, 
S II, Si II, O I, C IV, Si IV, Fe II, Al II, Al III, Mn II, Mg II, Mg I, 
among others, at a common redshift z = 2.358. At the same redshift, we 
also detect fine-structure lines of Ni II and Fe II, thus confirming 
conclusively that this is the GRB redshift. We also detect intervening 
systems at z = 1.539, 1.693, and 2.00. In particular, the system at z = 
1.539 displays exceptionally strong Mg II, Mg I, and Fe II absorption.

We acknowledge the expert support of the VLT observing staff at Paranal, 
in particular Maja Vuckovic, Marcelo Lopez, and Thomas Rivinius.
We also thank Alex Kann for discussion on the afterglow identification.

[GCN OPS NOTE(15aug12): Per author's request, ML and TR were added to the
last paragraph.]


GRB_name: GRB120815A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13650
SUBJECT: GRB 120815A: Enhanced Swift-XRT position
DATE:    12/08/15 06:31:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1694 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 120815A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 273.95807, -52.13142 which is equivalent
to:

RA (J2000): 18h 15m 49.94s
Dec (J2000): -52d 07' 53.1"

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: GRB120805A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13651
SUBJECT: GRB 120805A: Liverpool Telescope optical candidate detection
DATE:    12/08/15 07:30:58 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara) and C.G. Mundell (LJMU) report
on behalf of a large collaboration:

The Liverpool Telescope automatically observed GRB 120805A
(Troja et al. GCN Circ. 13588) as previously reported (Bersier
et al GCN Circ. 13590). We also detected the optical candidate
identified by Gorosabel et al. (GCN Circ. 13591) at the
following position, within the UVOT-enhanced XRT error circle
(Evans et al. GCN Circ. 13638):

RA(J2000) =  14:26:09.11
Dec(J2000)=  +05:49:32.1

with an uncertainty of 1". The optical afterglow candidate
is detected in both r' and i' filters with the following
magnitudes:


Mid time from  Total Exp   Filter    Magnitude
trigger (min)   (s)
------------------------------------------------
16.0            6x10        r'       20.9 +- 0.3
50.0           3x120        i'       20.9 +- 0.2
------------------------------------------------

Magnitudes are calibrated against nearby USNOB-1 stars.


GRB_name: GRB120815A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13652
SUBJECT: GRB 120815A: Swift-BAT refined analysis
DATE:    12/08/15 13:14:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.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),
C. Pagani (U Leicester), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120815A (trigger #531003)
(Pagani, et al., GCN Circ. 13645).  The BAT ground-calculated position is
RA, Dec = 273.976, -52.125 deg, which is 
   RA(J2000)  =  18h 15m 54.4s 
   Dec(J2000) = -52d 07' 29.0" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 28%.
 
The mask-weighted light curve shows a FRED pulse starting at ~T-0.3 sec,
peaking at ~T+0.5 sec, and ending at ~T+30 sec.  T90 (15-350 keV) is
9.7 +- 2.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.24 to T+11.97 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.29 +- 0.23.  The fluence in the 15-150 keV band is 4.9 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.17 sec in the 15-150 keV band
is 2.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/531003/BA/


GRB_name: GRB120815A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13653
SUBJECT: GRB 120815A: Swift-XRT refined Analysis
DATE:    12/08/15 20:04:33 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 8.5 ks of XRT data for GRB 120815A (Pagani  et al. GCN
Circ. 13645), from 2.7 ks to 39.5 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN. Circ 13650).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.89 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+0.12, -0.11). The
best-fitting absorption column is  5.5 (+4.2, -3.8) x 10^21 cm^-2, at a
redshift of 2.358, in addition to the Galactic value of 8.6 x 10^20
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 4.0 x
10^-11 (5.0 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 8.6 x 10^20 cm^-2
Intrinsic column:    5.5 (+4.2, -3.8) x 10^21 cm^-2 at z=2.358
Photon index:      1.85 (+0.12, -0.11)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00531003.

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


GRB_name: GRB120816A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13654
SUBJECT: GRB 120816A: Swift detection of a burst
DATE:    12/08/16 19:32:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (U Ferrara), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 19:18:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120816A (trigger=531223).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 282.126, -6.979, which is 
   RA(J2000) = 18h 48m 30s
   Dec(J2000) = -06d 58' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with a duration of about 5 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 19:20:47.3 UT, 132.6 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 282.14430, -6.93753 which is equivalent
to:
   RA(J2000)  = 18h 48m 34.63s
   Dec(J2000) = -06d 56' 15.1"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 162 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 (3.73 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.4
(+3.28/-2.78) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 134 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 0.00% of the XRT error circle. Because of the density of
catalogued stars, further analysis is required to report an upper limit for any
afterglow in the region. No correction has been made for the large, but
uncertain extinction expected. 

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


GRB_name: GRB120816A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13655
SUBJECT: GRB 120816A: ROTSE-III Optical Limits
DATE:    12/08/16 20:18:36 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich), W. Rujopakarn (Steward), T. Guver (Sabanci
University), report on behalf of the ROTSE collaboration:

ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, automatically responded to GRB 120816A (Swift trigger 531223;
Page et al., GCN 13654). An automated response took the first image at
19:23:18.6 UT, 285 s after the burst, under fair conditions. We took 10
5-sec, 10 20-sec and 50 60-sec exposures. These unfiltered images are
calibrated relative to USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or the XRT error circle; however, we are
limited as the field is severely crowded. Individual images have
limiting magnitudes ranging from 13.9-15.1; we set the following
specific limits.

start UT end UT t_exp(s) mlim Coadd?
----------------------------------------------------
19:23:18.6   19:23:23.6         5     13.9      N
19:23:45.6   19:23:50.6         5     14.2      N
19:24:13.1   19:24:18.1         5     14.3      N
19:25:34.5   19:25:54.5        20     14.8      N
19:35:05.4   19:40:22.7       600     15.1      Y


GRB_name: GRB120816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13656
SUBJECT: GRB 120816A: TAROT Calern observatory optical observations
DATE:    12/08/16 21:16:46 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120816A detected by SWIFT
(trigger 531223) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 526s after the GRB trigger
(delay due to the beginning of the night).
The elevation of the field increased from
36 degrees above horizon and weather conditions
were good.

We co-added a series of exposures but we do not
detect any OT at the XRT position (Page et al.
GCNC 13654):

 From t0+526s to t0+942s, R > 16.5

Galactic coordinates are lon= 26.384d lat= -2.527d
and the galactic extinction in R band is about 3 magnitudes
(estimated from D. Schlegel et al. 1998ApJ...500..525S).
Although the field is very dense, there are no star brighter
than 18th mag in the XRT error box.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB120816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13657
SUBJECT: GRB120816A: OPTIMA discovery of optical counterpart
DATE:    12/08/16 21:39:46 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau and Gottfried Kanbach (both MPE Garching) report on behalf of 
the OPTIMA-Burst Team:

"We observed the location of GRB 120816A (Page et al. GCN #13654) with 
OPTIMA-Burst (Kanbach et al. 2008, Astrophys. and Sp. Sci. Lib. Vol. 
351, 153) currently mounted at the 1.3m telescope at Skinakas 
Observatory, University of Crete. Observations started at 19:22:44 UT 
(249 sec after the burst) with unfiltered 20s exposures using the 
field-viewing CCD camera. Within the updated XRT error circle we find a 
fading source located at:

RA(J2000) = 18:48:34.4
Dec(J2000) = -06:56:16

with an approximate uncertainty of 1" in both coordinates.

We measure the following magnitudes:

T0+         white
--------------
249s        ~17.8
4844s    >19.1

calibrated against the R=15.2mag reference star USNO-B1.0 0830-0537586."


GRB_name: GRB120816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13658
SUBJECT: GRB 120816A: BOOTES-2 observations
DATE:    12/08/16 23:35:34 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Jelnek, J. C. Tello, J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC
Granada), on behalf of a larger collaboration, report:

"Following the detection of GRB 120816A (Page et al. GCNC 13654), the
BOOTES-2/TELMA 0.6m telescope (+COLORES) in southern Spain started to
observe the field about one hour after the GRB, as soon as the night
started, obtaining a series of unfiltered images. In particular, a
combination of 15x60s frames gathered around 20:24:35UT (i.e. T0+66min)
provides a limit of R > 18 at the position of the reported optical
counterpart (Rau and Kanbach GCNC 13657)."

This message can be quoted.


GRB_name: GRB120816A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13659
SUBJECT: GRB 120816A: Swift-BAT refined analysis
DATE:    12/08/17 02:28:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+192 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120816A (trigger #531223)
(Page, et al., GCN Circ. 13654).  The BAT ground-calculated position is
RA, Dec = 282.133, -6.981 deg, which is 
   RA(J2000)  =  18h 48m 32.0s 
   Dec(J2000) = -06d 58' 51.6" 
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.
 
The mask-weighted light curve shows a single peak starting at ~T+0 sec,
peaking at ~T+1 sec, and ending at ~T+8 sec.  T90 (15-350 keV) is
7.6 +- 3.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.97 to T+6.66 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.54 +- 0.40.  The fluence in the 15-150 keV band is 4.3 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.82 sec in the 15-150 keV band
is 2.1 +- 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/531223/BA/


GRB_name: GRB120816A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13660
SUBJECT: GRB 120816A: Enhanced Swift-XRT position
DATE:    12/08/17 05:34:39 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2433 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 120816A, 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 = 282.14298, -6.93791 which is equivalent
to:

RA (J2000): 18h 48m 34.31s
Dec (J2000): -06d 56' 16.5"

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: GRB120817A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13661
SUBJECT: GRB 120817A: Swift detection of a burst
DATE:    12/08/17 06:58:40 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.P. Gompertz (U Leicester), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), K. L. Page (U Leicester), D. M. Palmer (LANL)
and R. L. C. Starling (U Leicester) report on behalf of the Swift
Team:

At 06:49:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120817A (trigger=531267).  Swift could not immediately slew
due to an Earth limb pointing constraint. 
The BAT on-board calculated location is 
RA, Dec 250.706, -38.340 which is 
   RA(J2000) = 16h 42m 49s
   Dec(J2000) = -38d 20' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple-peaked
structure with a duration of about 25 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+50.1
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is B.P. Gompertz (bpg6 AT le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120817A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13662
SUBJECT: GRB 120817A: Swift-XRT observations
DATE:    12/08/17 08:45:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 120817A at 07:41:33.5 UT,
3110.8 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 250.69098,
-38.35404 which is equivalent to:
   RA(J2000)  = 16h 42m 45.84s
   Dec(J2000) = -38d 21' 14.5"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 65 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.88
x 10^21 cm^-2 (Kalberla et al. 2005). 


GRB_name: GRB120816A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13663
SUBJECT: GRB 120816A: Swift-XRT refined Analysis
DATE:    12/08/17 09:04:33 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K. L. Page (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 5.6 ks of XRT data for GRB 120816A (Page  et al. GCN
Circ. 13654), from 136 s to 12.5 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN. Circ 13660).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.94 (+0.08, -0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 (+0.26, -0.25). The
best-fitting absorption column is  6.4 (+1.5, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 3.7 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.8 x 10^-11 (9.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.4 (+1.5, -1.4) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.10 (+0.26, -0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00531223.

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


GRB_name: GRB120817A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13664
SUBJECT: GRB 120817A: FTN and FTS observations
DATE:    12/08/17 11:02:47 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell, C.J. Mottram,
F. Virgili (LJMU), A. Gomboc (U. Ljubljana) report on
behalf of a larger collaboration:

The 2-m Faulkes Telescope North (FTN) automatically began observing
GRB 120817A (Gompertz et al. GCN Circ. 13661) on August 17 2012,
06:53:57 UT corresponding to 4.2 minutes post burst trigger
with BVRi' filters. Within the XRT error circle (Perri et al.
GCN Circ. 13662), close to a USNOB1 object we detect a faint,
uncatalogued, possibly fading source at the following position

R.A. = 16:42:45.92
Dec = -38:21:12.4   (J2000)

with an uncertainty of about 1".
The detection is marginal, with an estimated magnitude of
19.3 +/- 0.4 in the R band at a mean time of 17.4 minutes
(60 s exposure) calibrated against nearby USNOB-1 stars.

The 2-m Faulkes Telescope South (FTS) began observing at 77 min
post burst. In a stacked R-band frame we find marginal evidence
for fading, with R=19.8 +- 0.3 mag at a mean time of 105 min
(total exposure of 360 s). The nearby USNOB1 object is compatible
with being constant between the two observations.

The comparison between the FTN and FTS R-band images is available at
http://www.fe.infn.it/u/guidorzi/GRB120817A_XRT_FT_candidate.jpg


GRB_name: GRB120816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13665
SUBJECT: GRB 120816A: Bassano Bresciano Observatory optical observations
DATE:    12/08/17 12:14:44 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli A.Quadri report:

We imaged the field of GRB 120816A detected 
by SWIFT(trigger 531223) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy.

The observations started 26.7 min. after the 
GRB trigger,with our schmidt telescope 
D=320 mm F/D=3.1.

Weather conditions were discrete.

We co-added 4 series of 30 x 120s exposures.

We did not appear any optical counterpart 
in the error box of the XRTcandidate
(Page et al.GCNC 13654).

Start       End       Vlim
27.6min     278min    17.7

Magnitudes were estimated with the USNO-B1 cat. 

The message may be cited.


GRB_name: GRB120815A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13666
SUBJECT: GRB 120815A: Swift/UVOT Detection of the Optical Afterglow
DATE:    12/08/17 12:25:18 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

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

     The Swift/UVOT observed the field of GRB 120815A starting 2672 s
after the BAT trigger (Pagani et al., 2012, GCNC 13645).  Settled
observations started at 2690 s.  We detect an uncatalogued source
inside the UVOT-enhanced XRT error circle (Goad et al., 2012, GCNC
13650) with preliminary coordinates

   RA (J2000)  18:15:49.88  =  273.95783 (deg)
  Dec (J2000) -52:07:52.1   =  -52.13114 (deg)

and an estimated uncertainty of 0.6 arcsec (radius, 90% confidence,
statistical + systematic).  The UVOT detection is consistent with the
optical afterglow reported by Sudilovsky et al. (2012, GCNC 13648)
Source magnitudes and 3-sigma upper limits at this location are given
below.  The afterglow is 4.27 arcsec northeast of the USNO-B1.0 source
0378-0977505, so the following photometry should be considered
preliminary.

Filter       TSTART   TSTOP   Exp Time       Mag  Err  Sigma
------------------------------------------------------------
    v         2847     3046        100     19.34 0.29    3.9
    b         3667     4120        226     20.11 0.24    4.7
    u         3462     3661        100    >20.5
 uvw1         3257     3457        100    >20.2
 uvm2         3052     3252        100    >19.9
 uvw2         4330     4530        100    >20.3
white         2690     2840         75     19.94 0.19    5.8
------------------------------------------------------------

    The quoted magnitudes and upper limits have not been corrected for
the Galactic extinction along the line of sight to this burst of
E_{B-V} = 0.10 mag (Schlafly et al. 2011, ApJS, 737, 103).


GRB_name: GRB120817A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13667
SUBJECT: GRB 120817A: Enhanced Swift-XRT position
DATE:    12/08/17 15:09:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2321 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 120817A, 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 = 250.68918, -38.35451 which is equivalent
to:

RA (J2000): 16h 42m 45.40s
Dec (J2000): -38d 21' 16.2"

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

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

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


GRB_name: GRB120816A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13668
SUBJECT: GRB 120816A: optical upper limit
DATE:    12/08/17 16:17:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Ivanov, V. Ivanov, V. Lysenko (Kuban State University), A. Pozanenko 
(IKI)

We observed the field of the Swift GRB 120816A (Page  et al., GCN 13654) 
with 20-inch telescope of Kuban State University Astrophysical Observatory 
on August 16 starting on (UT) 19:34:49. We took several series of 40 s and 
60 s exposures using R filter. In a stacked image we do not detect any new 
source in the enhanced XRT error circle (Osborne et al., GCN 13660), in 
particular we do not detect the OT candidate  (Rau et al., GCN 13657). A 
preliminary photometry is based on the nearby USNO-B1.0 (R2) stars:

 Start,         T0+         Filter, Exposure,    OT,   uplim (3 sigma)
  (UT)         (mid, d)             (s)
19:34:49   0.0115      R       40               n/d    16.0
19:36:01   0.0221      R     830               n/d    17.9
19:36:01   0.0539      R   3530               n/d    18.1


GRB_name: GRB120817A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13669
SUBJECT: GRB 120817A: Swift-BAT refined analysis
DATE:    12/08/17 18:23:39 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

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

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120817A (trigger #531267)
(Gompertz, et al., GCN Circ. 13661).  The BAT ground-calculated position is
RA, Dec = 250.692, -38.377 deg, which is 
   RA(J2000)  =  16h 42m 46.2s 
   Dec(J2000) = -38d 22' 36.8" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.
 
The mask-weighted light curve shows two slighly overlapping peaks starting
at ~T-2 sec, peaking at ~T+0.0 and ~T+11 sec, with a tail ending at ~T+65 sec.
T90 (15-350 keV) is 28.2 +- 6.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.24 to T+30.77 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.97 +- 0.16.  The fluence in the 15-150 keV band is 6.9 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band
is 0.8 +- 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/531267/BA/


GRB_name: GRB120817B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13670
SUBJECT: IPN Triangulation of  GRB 120817B (short/very intense)
DATE:    12/08/17 19:44:53 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

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

V. Connaughton, M. Briggs, and C. Meegan, 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,

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

and

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

The short-duration, hard, very intense GRB 120817B has been observed by 
Konus-Wind, Fermi (GBM: trigger 366868952), INTEGRAL (SPI-ACS), Suzaku 
(WAM), Swift(BAT) and MESSENGER (GRNS), so far, at about 14550  s UT 
(04:02:30).

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
      8.321 (00h 33m 17s) -26.514 (-26d 30' 51")
   Corners:
      8.445 (00h 33m 47s) -26.217 (-26d 13' 00")
      8.468 (00h 33m 52s) -26.456 (-26d 27' 23")
      8.196 (00h 32m 47s) -26.809 (-26d 48' 34")
      8.174 (00h 32m 42s) -26.571 (-26d 34' 17")
   ---------------------------------------------
The error box area is 235 sq. arcmin, and its maximum
dimension is 38 arcmin (the minimum dimension is 14 arcmin).

A Swift ToO has been requested.

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120817_T14553/IPN/

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


GRB_name: GRB120817B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13671
SUBJECT: GRB 120817B: Fermi GBM detection
DATE:    12/08/17 21:29:55 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) reports on behalf of the Fermi GBM Team:

"At 04:02:29.723 UT on 17 August 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120817B (trigger 366868952 / 120817168),
which was also located by IPN (S. Golenetskii et al. 2012, GCN 13670).
The GBM on-ground location is consistent with the IPN position.
The angle from the Fermi LAT boresight is 59 degrees.

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

The GBM light curve shows a single pulse
with a duration (T90) of about 0.192 s (50-300 keV).
The time-averaged spectrum from T0-0.032 s to T0+0.064 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.65 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 1377 +/- 173 keV.

The event fluence (10-1000 keV) in this time interval is
(1.85 +/- 0.06)E-6 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band
is 46.6 +/- 1.6 ph/s/cm^2.

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


GRB_name: GRB120817B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13672
SUBJECT: GRB 120817B: LCO Optical Observations
DATE:    12/08/18 05:30:45 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

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

"We observed the IPN error region of the short GRB 120817B (GCN #13670)
with the Wide-Field CCD camera mounted on the du Pont 2.5-m telescope at
Las Campanas Observatory.  The observations started on 2012 August 18.158
UT (23.7 hour after the burst) using the R-band filter, and covered the
entire error region using two pointings with an exposure time of 900 sec
per pointing.  A comparison to the Digital Sky Survey reveals no new
sources to the limit of the survey (R~21 mag)."


GRB_name: GRB120817A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13673
SUBJECT: GRB 120817A: Swift-XRT refined Analysis
DATE:    12/08/18 09:13:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.7 ks of XRT data for GRB 120817A (Gompertz  et al.
GCN Circ. 13661), from 3.1 ks to 22.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN. Circ
13667).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.70 (+/-0.18).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.4, -0.3). The
best-fitting absorption column is  5.9 (+2.6, -1.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.9 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.8 x 10^-11 (8.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.9 (+2.6, -1.9) x 10^21 cm^-2
Galactic foreground: 2.9 x 10^21 cm^-2
Excess significance: 2.5 sigma
Photon index:      2.0 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00531267.

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


GRB_name: GRB120817B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13674
SUBJECT: Konus-Wind observation of GRB 120817B
DATE:    12/08/18 11:45:16 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short-duration hard-spectrum intense GRB 120817B
(IPN localization: Golenetskii at al., GCN 13670;
Fermi/GBM detection: Xiong, GCN 13671)
triggered Konus-Wind at T0=14553.388s UT (04:02:33.388)

The light curve shows a single pulse,
a total duration of the burst is ~0.08 s.
The emission is seen up to ~6.5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120817_T14553/

As observed by Konus-Wind the burst
had a fluence of 4.1(-1.0,+1.1)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0,
of 1.2(-0.3,+0.3)x10-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.064 s)
is best fit in the 20 keV - 7 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.82 (-0.18, +0.21),
and Ep = 1740(-520, +890) keV,
chi2 = 7.5/12 dof.

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


GRB_name: GRB120816B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13675
SUBJECT: IPN Triangulation of  GRB 120816B (short/exceptionally intense)
DATE:    12/08/18 14:32:17 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

K. Hurley on behalf of the IPN,

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

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

The short-duration, hard, exceptionally intense GRB 120816B has been 
observed by Konus-Wind, INTEGRAL (SPI-ACS), Suzaku (WAM), and 
Swift(BAT), at about 86299 s UT (23:58:19). The burst was outside the 
coded field of view of the BAT.

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Corners:
    341.155 (22h 44m 37s)  +2.156 ( +2d 09' 22")
    342.478 (22h 49m 55s)  -0.731 ( +0d 43' 51")
    334.205 (22h 16m 49s)  -5.388 ( -5d 23' 15")
    332.423 (22h 09m 42s)  -2.756 ( -2d 45' 20")
   ---------------------------------------------

The error box area is 10.030 sq. deg

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120816_T86298/IPN/

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


GRB_name: GRB120816B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13676
SUBJECT: Konus-Wind observation of GRB 120816B
DATE:    12/08/18 14:52:56 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short-duration hard-spectrum exceptionally intense GRB 120816B
(IPN localization: Golenetskii at al., GCN 13675)
triggered Konus-Wind at T0=86298.852s UT (23:58:18.852)

The light curve shows a single multi-peaked pulse.
A total duration of the burst in is ~0.8 s (80-350 keV range)
with a hint of a soft extended tail lasting till ~T0+50 s.
The emission in the main phase of the burst is seen up to ~9 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120816_T86298/

As observed by Konus-Wind the burst
had a fluence of 9.7(-0.5,+0.5)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0,
of 2.3(-0.2,+0.2)x10-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst (measured from T0 to T0+0.768 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.61 (-0.04, +0.04),
and Ep = 2320(-130, +140) keV,
chi2 = 100/89 dof.

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


GRB_name: GRB120815A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13677
SUBJECT: GRB 120815A: MASTER-ICATE observations
DATE:    12/08/18 15:44:50 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

H. Levato and C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez and F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

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

K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk
Irkutsk State University

V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

V. Krushinski, I. Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University


MASTER-ICATE robotic very wide field cameras (FOV=2x384 square degrees, 
D=72mm,
f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in Argentina
(Observatorio Astronomico Felix Aguilar, http://93.180.27.230:8080/) were
pointed to the GRB120815A (C. Pagani, GCN 13645) 37 s after notice
time and 60 s after GRB time at 2012-08-15 02:13:58 UT. We haven't found 
optical transient  within
SWIFT error-box  our first (5 s exposure) set. The 5-sigma upper limit has 
been about 12.0 mag
The 5-sigma upper limit on coadd first 30 images is about 13.0 mag.

Our cameras are continuously imaging the sky with 5 sec exposures.

This message can be cited.


GRB_name: GRB120816A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13678
SUBJECT: GRB 120816A: Swift/UVOT Detection of the Optical Afterglow
DATE:    12/08/18 16:32:59 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) and K. L. Page (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of GRB 120815A starting 117 s
after the BAT trigger (Page et al., 2012, GCNC 13654). We detect
an uncatalogued source inside the enhanced XRT error circle
(Osborne et al., 2012, GCNC 13660) with preliminary coordinates

   RA (J2000) = 18:48:34.5 = 282.14359 (deg)
  Dec (J2000) = -06:56:16.4 = -6.93788 (deg)

and an estimated uncertainty of 0.6 arcsec (radius, 90% confidence,
statistical + systematic). The UVOT detection is consistent with
the optical afterglow reported by Rau et al. (2012, GCNC 13657).
Source magnitudes and 3-sigma upper limits at this location are
given below (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373).

Filter       TSTART   TSTOP    Exp Time      Mag  Err
-----------------------------------------------------
white          134      284         147      18.5  0.2
white          573     6306         598      19.9  0.2
    v          117     6716         500     >19.0
    b          548    11345        1174     >19.6
    u          293     7286         672     >21.1
 uvw1          672     7126         490     >21.1
 uvm2          647     6921         490     >19.5
 uvw2          599     6511         490     >19.8
-----------------------------------------------------

The quoted magnitudes and upper limits have not been corrected for
the Galactic extinction along the line of sight to this burst of
E_{B-V} = 0.703 mag.


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13679
SUBJECT: GRB 120811C: optical observations
DATE:    12/08/18 22:18:42 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  GRB 120811C (Barlow et al., GCN  13622) with 
0.45-m telescope of ISON-NM observatory  starting on  Aug. 12 (UT) 03:25:07. 
We took  several unfiltered images of 30 s exposures.  The optical afterglow 
(Denisenko et al., GCN 13623) is marginally detected in co-added frames at 
coordinates (J2000) 13:18:43.98 +62:18:03.4 with uncertainty of 0.5 arcsec 
in both coordinates.  A preliminary  photometry of co-added frames is based 
on the USNO-B1.0 (R2)  nearby  stars is following:

T_start,     T0+,           Exposure,  OT,              UL (3 sigma)
(UT)           mid, d         (s)

03:25:07   0.5095      1800           21.5 +/-0.5   21.2


GRB_name: GRB120817B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13680
SUBJECT: GRB 120817B: Swift-XRT observations
DATE:    12/08/19 00:41:08 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) reports on behalf of the Swift team:

At 22:41:45 UT, August 17, 2012, Swift began a Target of Opportunity observation of GRB 120817B (Golenetskii et al. GCN 13670).

We have analysed 2.8 ks of XRT data, beginning 67 ks after the GRB trigger. The data are entirely in Photon Counting mode. No new source is detected in the XRT data. The 3-sigma upper limit is 0.005 counts/sec which is 2.7e-13 erg cm^-2 s^-1 for a typical GRB spectrum.

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


GRB_name: GRB120819A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13681
SUBJECT: GRB 120819A: Swift detection of a burst
DATE:    12/08/19 13:22:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
C. Pagani (U Leicester) and K. L. Page (U Leicester) report on behalf
of the Swift Team:

At 13:10:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120819A (trigger=531428).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 235.888, -7.305 which is 
   RA(J2000)  =  15h 43m 33s
   Dec(J2000) = -07d 18' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a duration of about 30 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 13:12:50.5 UT, 156.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 235.90848, -7.30910 which is equivalent
to:
   RA(J2000)  = 15h 43m 38.04s
   Dec(J2000) = -07d 18' 32.8"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 74 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 (8.93 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.4
(+2.74/-2.85) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 158 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 77% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.17. 

Burst Advocate for this burst is 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: GRB120819A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13682
SUBJECT: GRB 120819A: MASTER optical observations 
DATE:    12/08/19 16:10:19 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

  V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
  Blagoveschensk Educational State University, Blagoveschensk


K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
  Irkutsk State University

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

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

  V.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  GRB120819A (Beardmore et 
al., GCN 13681) sec after GRB time at 2012-08-19 13:12:10.052 UT.
On our first (20s exposure) set we 
haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 16.5 mag
The reduction is continuated.
The message may be cited.


GRB_name: GRB120819A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13683
SUBJECT: GRB 120819A: afterglow candidate from NOT
DATE:    12/08/19 23:13:43 GMT
FROM:    Giorgos Leloudas at Dark Cosmology Centre  <giorgos@dark-cosmology.dk>

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

We observed the field of GRB 120819A (Beardmore et al., GCN 16381) with the NOT equipped with ALFOSC. Observations were carried out in the R and z bands, for a total of 20 and 40 min exposure, respectively.

Within the current XRT position (see http://www.swift.ac.uk/xrt_positions/index.php), we detect a source at the following coordinates (J2000):

RA = 15:43:37.84
Dec = -07:18:32.9

with an error of about 0.5". Assuming R = 18.05 for the nearby USNO star at RA = 15:43:38.183, Dec = -07:17:51.72, the object has R = 23.0 +- 0.1. The mean time of the R-band observation is Aug 19.913 UT, that is 8.75 hr after the GRB.

Given the faintness of the source and the lack of information on its temporal behaviour, we cannot state whether this object is related to GRB 120819A.


GRB_name: GRB120819A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13684
SUBJECT: GRB 120819A: Enhanced Swift-XRT position
DATE:    12/08/20 04:49:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2836 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 120819A, 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 = 235.90756, -7.30909 which is equivalent
to:

RA (J2000): 15h 43m 37.81s
Dec (J2000): -07d 18' 32.7"

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: GRB120819A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13685
SUBJECT: GRB 120819A: MITSuME Okayama Optical upper limits
DATE:    12/08/20 04:58:44 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 the MITSuME collaboration:

We observed the field of GRB 120819A (Beardmore et al., GCNC 13681)
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 2012-08-19 13:12:11 UT (~2.0 min after the burst)
We did not find any new point source within the enhanced XRT circle
(Beardmore et al., GCNC 13681) in all the three bands.
We also could not detect the previously reported afterglow (Malesani et al.,
GCNC 13683).


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
------------------------------------------------------
0.01186    13:27:19    1620.0   >19.1  >19.4  >18.8
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120819A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13686
SUBJECT: GRB 120819A: MITSuME Ishigakijima upper limits
DATE:    12/08/20 04:58:56 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 120819A (Beardmore et al., GCNC 13681)
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 2012-08-19 13:13:11 UT, (~3.0 min after the burst)
We did not find any new point source within the enhanced XRT circle
(Beardmore et al., GCNC 13681) in all the three bands.
We also could not detect the previously reported afterglow (Malesani et al.,
GCNC 13683).


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
------------------------------------------------------
0.01544    13:32:28    1980.0   >21.5  >21.6  >20.3
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120819A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13687
SUBJECT: GRB 120819A: Swift-XRT refined Analysis
DATE:    12/08/20 05:47:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

O.M. Littlejohns (U. Leicester), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA), V. Mangano (INAF-IASFPA), D.N. Burrows (PSU), J.A.
Kennea (PSU), M.C. Stroh (PSU), J.P. Osborne (U. Leicester), K.L. Page
(U. Leicester) and A.P. Beardmore report on behalf of the Swift-XRT
team:

We have analysed 10 ks of XRT data for GRB 120819A (Beardmore  et al.
GCN Circ. 13681), from 159 s to 23.0 ks after the  BAT trigger. The
data comprise 67 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 13684).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.75 (+0.12, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.7 (+/-0.4). The
best-fitting absorption column is  3.3 (+2.0, -1.5) x 10^21 cm^-2, in
excess of the Galactic value of 8.9 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.2 x 10^-11 (6.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      3.3 (+2.0, -1.5) x 10^21 cm^-2
Galactic foreground: 8.9 x 10^20 cm^-2
Excess significance: 2.6 sigma
Photon index:      1.7 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00531428.

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


GRB_name: GRB120819A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13688
SUBJECT: GRB 120819A: GROND afterglow confirmation
DATE:    12/08/20 07:29:10 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120819A (Swift trigger 531428; Beardmore et 
al., GCN 13681) simultaneously in g'r'i'z'JHKs with GROND (Greiner et 
al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La 
Silla Observatory (Chile).

Observations started at 23:46 UT on 2012-08-19, 10.5 hrs after the GRB 
trigger. Based on co-added images spanning 2 hours taken at a mean 
airmass of 1.3 and seeing of 1.6", we confirm the presence of the NOT 
afterglow candidate (Malesani et al., GCN 13683). We derive preliminary 
magnitudes (all AB system) of this source:

   g' = 23.7 +- 0.1
   r' = 23.1 +- 0.1
   i' = 22.5 +- 0.1
   z' = 22.2 +- 0.1
   J  = 21.5 +- 0.3
   H  > 20.2
   Ks > 20.1

We note that although these magnitudes do not suggest fading, the large 
uncertainties from the USNO calibration used by Malesani et al. do not 
preclude this possibility.

The consistency with the enhanced XRT position (Evans et al., GCN 
13684), combined with the power-law like SED, confirm that this source 
is the afterglow of GRB 120819A.

The g' band detection does not suggest substantial Ly-alpha or dust 
effects, implying that the redshift of this burst is likely smaller than 
3.0.

The magnitudes are derived based on GROND zeropoints (g'r'i'z') and 
2MASS stars (JHK). The magnitudes are not corrected for the expected 
Galactic reddening along the line of sight of E_(B-V)= 0.16 mag 
(Schlegel et al. 1998).


GRB_name: GRB120819A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13689
SUBJECT: GRB 120819A: Swift-BAT refined analysis
DATE:    12/08/20 12:25:42 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120819A (trigger #531428)
(Beardmore, et al., GCN Circ. 13681).  The BAT ground-calculated position is
RA, Dec = 235.887, -7.304 deg, which is 
   RA(J2000)  =  15h 43m 32.8s 
   Dec(J2000) = -07d 18' 13.5" 
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 30%.
 
The mask-weighted light curve shows multiple peaks starting at ~T-2 sec,
with the largest peak at ~T+0 sec, and returning to baseline at ~T+180 sec.
T90 (15-350 keV) is 71 +- 21 sec (estimated error including systematics).
 
The time-averaged spectrum from T+4.42 to T+82.88 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.49 +- 0.23.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.20 sec in the 15-150 keV band
is 0.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/531428/BA/


GRB_name: GRB120819A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13690
SUBJECT: GRB 120819A: Bassano Bresciano Observatory optical observations
DATE:    12/08/20 13:05:16 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla, R.Girelli and A.Quadri report:

We imaged the field of GRB 120819A detected 
by SWIFT(trigger 531428) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy.

The observations started 6h 35min. after the 
GRB trigger(delay due to expecting the night)
with our Schmidt telescope D=400mm F/D=3.1.

Weather conditions were good.

We co-added 2 series of 15 unfiltered CCD exposures of 120s each.

We did not appear any reasonable optical counterpart 
in the error box of the XRTcandidate (Beardmore et al., GCNC 13681) 
at our limiting magnitude.

Start      End       M.lim.
395min     454min    19.5

Magnitudes were estimated with the USNO-B1 cat. 


The message may be cited.


GRB_name: GRB120819A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13691
SUBJECT: GRB 120819A: MASTER final limits 
DATE:    12/08/20 13:27:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk


K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

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

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  GRB120819A (Beardmore et al., GCN 
13681) 25 sec after notice time and 115 sec after GRB time at 2012-08-19 
13:12:10.052 UT (Yurkov et. al, GCN 13682).

Unfiltered observations were carried out on high zenith distance (78 deg. 
at the observations beginning moment and above).
The unfiltered magnitude is calibrated relative to USNO B1.0 (0.8 R + 0.2 
B).
After the data processing  we have the following results:


             Start      Middle    Stop    T-Tgrb Coadd Exp.time  Limit
2012-08-19 13:12:10  13:12:20  13:12:30    125     1       20   16.5
2012-08-19 13:12:10  13:15:00  13:17:51    285     6      140   17.8
2012-08-19 13:19:08  13:39:35  14:00:02   1785    10     1800   18.5

The message may be cited.


GRB_name: GRB120817B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13692
SUBJECT: GRB 120817B:  BAT location in ground analysis and refined analysis
DATE:    12/08/20 14:35:48 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 04:02:29 on August 17, 2012, Swift-BAT triggered (BAT trigger # 531259) on
the IPN burst GRB 120817B (Golenetskii et al., GCN Circ # 13670).  No source
was found onboard.  In ground analysis of the failed-trigger event sample, a
significant source was found at RA, Dec 8.310, -26.428, which is

RA (J2000)   00h 33m 14.4s   
Dec (J2000)  -26d 25m 42s

The estimated 90% confidence position error is 2.8 arcmin radius.  This
position was 5.5% coded in the BAT FOV.  It is 5 arcmin from the center of
the IPN triangulation, within the IPN error box.

As seen in BAT, the burst was a single spike 0.10 +/- 0.02 seconds long.

The time-averaged spectrum from T+0.2 to T+0.3 sec is best fit by a simple
power-law model.  The best-fit photon index is 0.60 +/- 0.3.  The total
fluence in the 15-150 keV band was (1.7 +/- 0.4) x 10^-7 ergs/cm^2.  The
errors quoted are at the 68% confidence level.


GRB_name: GRB120811C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13693
SUBJECT: GRB 120811C: optical observations
DATE:    12/08/20 15:14:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Litvinenko (UBAI), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  GRB 120811C (Barlow et al., GCN  13622) with 
0.4-m telescope of ISON-Kitab observatory  starting on  Aug. 11 (UT) 
15:53:49.  We took  several unfiltered images of 30 s exposures.  The 
optical afterglow  (Denisenko et al., GCN 13623) is clearly detected in 
single initial frames.  A photometry of some co-added frames is based  on 
the SDSS stars

SDSS id                             RA                 Dec 
R
J131912.45+621444.3 13 19 12,453  +62 14 44,35   16.63
J131815,89+621830,6 13 18 15,896  +62 18 30,67   16.64

is following:

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

15:53:49    0.01392    4x30          17,90 +/-0.13
15:56:05    0.01569    5x30          17.95 +/-0.13
15:58:55    0.01841  10x30          18.20 +/-0.10
16:04:35    0.02356  15x30          18.45 +/-0.11
16:13:06    0.03145  25x30          18.40 +/-0.07


GRB_name: GRB120817A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13694
SUBJECT: GRB 120817A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/08/20 16:27:28 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

A RAPTOR wide-field monitor located in Maui observed the location
of Swift trigger 531267 (Gompertz et al., GCN 13661) during the period
that the Swift BAT was observing gamma-ray emission.  The 10 s exposure
began at 06:49:38.0 UTC -- 4 s before the Swift trigger.  We detect no
new object at the location of the refined Swift XRT location
(Gompertz et al., GCN 13673) to a 3-sigma limiting magnitude of 10.3.
Our unfiltered images are calibrated to the Tycho-2 V-band.


GRB_name: GRB120817B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13695
SUBJECT: GRB 120817B - PTF Observations
DATE:    12/08/21 05:13:04 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), E. O. Ofek (Weizmann Institute) and D. B.
Fox (Penn State) report on behalf of a larger collaboration:

We have imaged the field of the IPN short-hard GRB120817B (Golenetskii et
al., GCN 13670) with the Palomar 48 inch Oschin telescope (P48) as part of
the Palomar Transient Factory (PTF).  Images were obtained in the Mould R
filter on 2012 Aug 19.4 and 20.4 UT.

Inside the error localization derived from ground-based analysis of the
Swift BAT (Cummings et al., GCN 13692), we find no new sources when
compared with Digitized Sky Survey images of the field on either night.
Digitally subtracting coadded frames from the two nights, we find no
fading sources within the field to a limiting magnitude of R > 20.5
(calibrated with respect to field stars from the USNO-B1 catalog).

Finally, we note that the error circle does not appear to contain any
bright, resolved (i.e. nearby) galaxies.  No known galaxies are listed in
the NASA Extragalactic Database within 5 arcmin of the center of the Swift
BAT localization.

[GCN OPS NOTE(22aug12):  Per author's request, "120718B" in the Subject-line
was changed to "120817B".]


GRB_name: GRB120821A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13696
SUBJECT: GRB 120821A: a long GRB detected by INTEGRAL
DATE:    12/08/21 14:47:21 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a long gamma ray burst lasting about 12 s has been detected by IBAS in the 
IBIS/ISGRI data at 13:23:45 UT of August 21

Its refined   coordinates (J2000) are:

RA:   255.2692    [degrees]
DEC:  -40.5212   [degrees]

with an uncertainty of 2 arcmin (90% c.l.).

The burst has a fluence of about  3e-7 erg/cm2  (20-200 keV)

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








=====================================================================
Sandro Mereghetti        INAF - Istituto di Astrofisica Spaziale
                                 e Fisica Cosmica - Milano
Tel. +39-02-23699323
Fax  +39-02-2666017       via Bassini 15, I-20133 Milano, ITALY

sandro@iasf-milano.inaf.it 
http://www.iasf-milano.inaf.it/~sandro/personal.html
===========================================================================


GRB_name: GRB120821A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13697
SUBJECT: GRB 120821A: GROND upper limits
DATE:    12/08/22 09:47:54 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

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

We observed the field of GRB 120821A (INTEGRAL trigger #6266; Mereghetti
et al., GCN #13696) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La
Silla Observatory (Chile).

Observations started at 23:47 UT, 10.4 hours after the GRB trigger. They
were performed at an average seeing of 1.1" and at an average airmass of
1.0.

The GROND JHK observations fully covered the INTEGRAL error circle,
whereas the g'r'i'z observations covered ~60% of the error circle. We do
not detect any obvious new source brighter than the detection limits of
DSS2 and 2MASS within the area covered by the 2arcmin INTEGRAL error
circle.


GRB_name: GRB120821A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13698
SUBJECT: GRB 120821A: Swift/UVOT Upper Limits
DATE:    12/08/22 11:38:06 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120821A
15ks after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 13696).
No optical afterglow consistent with the INTEGRAL position
(Mereghetti et al., GCN Circ. 13696) 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

u                17059        17241          179         >20.92
w1               16153        17053          886         >21.7
m2               15246        16146          886         >21.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 25.4 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120821A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13699
SUBJECT: GRB 120821A: Swift/XRT observations
DATE:    12/08/22 12:05:46 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri, S. Campana (INAF-OAB) report on behalf of the
Swift team:

The Swift XRT observed the error circle of the INTEGRAL-detected GRB
120821A (Mereghetti et al, GCN Circ. 13696) from 15.2 to 17.2 ks after the
trigger. The data comprise 2.0 ks of Photon Counting (PC) mode data. No
clear afterglow candidate is detected. We note however the presence of a
very faint and low-significance source within the INTEGRAL error circle
(Mereghetti et al, GCN Circ. 13696) at the following position: RA, Dec
=255.25762, -40.51365 which is equivalent to:

RA (J2000): 17h 01m 01.83s
Dec (J2000): -40d 30' 49.1"

with an uncertainty of 6.7 arcsec (radius, 90% confidence).

The source has a count rate of (4.5 +/- 2.1) x 10^-3 cts/s. This
corresponds to an observed 0.3-10 keV flux of (2.7 +/- 1.2) x 10^-13
erg/cm2/s (assuming a typical GRB spectrum with photon spectral index of
2). If we consider the Galactic absorption in this direction (1.1 x 10^22
cm^-2; Kalberla et al. 2005) this corresponds to an unabsorbed flux of
(5.5 +/- 2.5) x 10^-12 erg/cm2/s. Given the limited statistics, it is not
possible to determine whether the source is fading.


GRB_name: GRB120817B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13700
SUBJECT: GRB 120817B: Deep limit on the optical afterglow from du Pont and Magellan observations
DATE:    12/08/22 18:26:16 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, E. Berger (Harvard), D. Kelson, R. Williams (Carnegie) report:

"We re-observed the BAT-refined location of the IPN short-duration GRB
120817B (GCNs 13670, 13692) with the Inamori-Magellan Areal Camera and
Spectrograph (IMACS) mounted on the Magellan/Baade 6.5-m telescope starting
on 2012 Aug 21.410 UT, 4.2 days post-burst and 3.3 days after our initial
LCO/WFCCD observations (GCN 13672).  We obtained 2x300-sec exposures in
R-band in 0.92" seeing.  Digital image subtraction with our first
observations using the ISIS software package reveals no evidence for a
fading optical source in or around the BAT error circle.  Calculating the
zeropoint using a Stetson standard star field at the same airmass, we place
a 3-sigma limit of R(Vega)>23.3 mag on the optical afterglow of GRB 120817B
at 23.7 hours after the burst."


GRB_name: GRB120817A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13701
SUBJECT: GRB 120817A: Swift/UVOT Upper Limits 
DATE:    12/08/27 23:33:50 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) and B. P. Gompertz (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120817A
3115 s after the BAT trigger (Gompertz et al., GCN Circ. 13661).
No optical afterglow consistent with the XRT (Beardmore et al., GCN
13667) or the FTN positions (Guidorzi et al., GCN 13664) 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          3115         3265          147         >19.4
white             3115         4496          344         >20.4
v                 3272        10816         1278         >20.2
b                 4092        17166          945         >21.1
u                 3887        22943         1904         >21.1
w1                3682        22294         2164         >20.3
m2                3476        21386         1838         >20.2
w2                4503         9902         1082         >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.84 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120819A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13702
SUBJECT: GRB 120819A: Swift/UVOT Upper Limits
DATE:    12/08/29 21:35:17 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) 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 120819A
158 s after the BAT trigger (Beardmore et al., GCN Circ. 13681).
No optical afterglow consistent with the optical position
(Malesani et al. GCN Circ. 13683)
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           158          308          147         >21.1
white              158         5439          541         >21.7
v                 4214        22619         1278         >20.9
b                 3598        11864         1164         >21.1
u                 4829        17638         1858         >21.6
w1                4625        16836         1998         >21.4
m2                4418        22980         1629         >21.7
w2                4009        21706         1279         >21.8

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: GRB120830A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13704
SUBJECT: GRB 120830A: Fermi-LAT detection of a short burst
DATE:    12/08/30 22:21:58 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford), J. Racusin (NASA/GSFC), and D. Donato (NASA/GFSC),
report on behalf of the Fermi-LAT team:

Fermi-LAT detected high energy emission from the short GRB 120830A in
ground analysis. The GRB triggered the Fermi-GBM on August 30th, 2012 at
07:07:03.53 UTC (trigger 368003226/120830297). At the time of the GBM
trigger, the angle between the GRB position and the LAT boresight was 38
degrees. The burst was also detected and localized through IPN, which will
be reported in an upcoming circular.

A preliminary maximum-likelihood analysis during the GBM T90 of the E>75MeV
P7TRANSIENT_V6 LAT data revealed a significantly detected transient source.
We obtain the best LAT on-ground localization of:

RA(J2000) = 88.42 deg

Dec(J2000) = -28.81 deg

with an error radius of 0.86 deg (68% containment, statistical error only),
which is 0.28 deg from the IPN position.

There were 4 photons above 100 MeV within 1 second of the GBM trigger
during the GBM emission. The highest energy photon is a 500 MeV event which
is observed 0.8 seconds after the GBM trigger. The likelihood fit provides
a photon index of 2.66 +/- 0.86, and a flux (100 MeV-10 GeV) over this
interval of 2.2e-07 +/- 1.7e-07 (erg/cm^2/s).

A Swift TOO has been requested based upon the IPN localization.

The Fermi LAT point of contact for this burst is Davide Donato (
davide.donato-1@nasa.gov).

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


GRB_name: GRB120830A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13705
SUBJECT: IPN Triangulation of short GRB 120830A
DATE:    12/08/30 23:04:39 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

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

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

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

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

report

The short-duration GRB, detected by the Fermi-LAT as reported in
GCN 13704 (Vianello, Racusin and Donato), was also observed so far
by MESSENGER (GRNS), Konus-Wind, INTEGRAL (SPI-ACS), and
Fermi GBM (trigger: 368003226).

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:

  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    88.649 (05h 54m 36s) -28.984 (-28d 59' 04")

  Corners:
    88.489 (05h 53m 57s) -28.613 (-28d 36' 49")
    88.480 (05h 53m 55s) -28.808 (-28d 48' 29")
    88.810 (05h 55m 14s) -29.353 (-29d 21' 12")
    88.818 (05h 55m 16s) -29.160 (-29d 09' 36")
  ---------------------------------------------

The error box area is 215 sq. arcmin, its maximum dimension is 47 arcmin,
and it is fully contained within the LAT error circle.

A Swift ToO has been approved.

This box can be improved.

A triangulation map showing the error box and the LAT error circle is posted at
http://gammaray.nsstc.nasa.gov/gbm/science/ipn_plots/loc_ipn_lat_120830297.pdf

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


GRB_name: GRB120830A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13706
SUBJECT: GRB 120830A: early MASTER optical limit
DATE:    12/08/31 09:07:25 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

H. Levato and C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez and F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

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

K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk
Irkutsk State University

V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

V. Krushinski, I. Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University


MASTER-ICATE robotic very wide field cameras (FOV=2x384 square degrees, D=72mm, 
f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in Argentina 
(Observatorio Astronomico Felix Aguilar, http://93.180.27.230:8080/) were 
pointed to the FERMI GRB120830A (Vianello et al., GCN 13704) 18 s after 
notice time and 44 s after GRB time at 2012-08-30 07:07:47 UT(Levato et al., GCN 13703).
We cover IPN (Hurley et al., GCN 13705) and Fermi LAT error boxes.

We haven't found  optical transient on our first (5 s 
exposure) set and on coadd image made of 60 images and complete exposure of 300 
seconds.
The coverage map is available 
http://master.sai.msu.ru/static/GRB120830A_IPN_LAT.jpeg

The 5-sigma upper limit on single image has  been about 11.0 mag and 12.0 mag 
on coadd image.
Our cameras are continuously imaging the sky with 5 sec exposures.
Weather conditions were not so good (feeble cloudiness).
This message can be cited.


GRB_name: GRB120830A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13707
SUBJECT: Konus-Wind observation of GRB 120830A
DATE:    12/08/31 10:57:46 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short-duration hard-spectrum GRB 120830A
(Fermi-LAT detection: Vianello et al., GCN 13704;
IPN localization: Hurley at al., GCN 13705)
triggered Konus-Wind at T0=25623.562s UT (07:07:03.562)

The light curve shows a single pulse with a duration of ~0.9 s.
The emission 2is seen up to ~5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120830_T25623/

As observed by Konus-Wind the burst
had a fluence of 4.8(-0.7,+1.1)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.080 s,
of 1.6(-0.5,+0.5)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured T0 to T0+0.256 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model, for which
alpha = 0.25 (-0.35, +0.45),
and Ep = 1070(-200, +240) keV,
chi2 = 27/22 dof.

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


GRB_name: GRB120830A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13708
SUBJECT: GRB 120830A: Fermi GBM observation
DATE:    12/08/31 18:12:23 GMT
FROM:    David Tierney at UCD  <david.tierney@ucd.ie>

D. Tierney (UCD)
reports on behalf of the Fermi GBM Team:

"At 07:07:03.53 UT on 30 August 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120830A (trigger 368003226 / 120830297).

The burst was located by the Fermi LAT
(G. Vianello et al. 2012, GCN 13704) and
the IPN (Hurley at al. 2012, GCN 13705)
The burst was also independently detected by
Konus-Wind (S. Golenetskii et al. 2012, GCN 13707).
and by INTEGRAL SPI-ACS.

The GBM light curve consists of a single peak
with a duration (T90) of 1.28 +/- 0.23 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+1.088 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.40 (+0.08/-0.07) and
the cutoff energy, parameterized as Epeak,
is 1214.00 (+155.00/-133.00) keV

The event fluence (10-1000 keV) in this time interval is
(3.253 +/- 0.113)E-06 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.128 s in the 10-1000 keV band
is 10.07 +/- 0.89 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 1212.00 (+140.00/-140.00) keV, alpha = -0.40 (+0.08/-0.07)
and an upper limit on beta (2 sigma error) = -4.35 (+2.46)

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


GRB_name: GRB120830A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13709
SUBJECT: GRB 120830A: Swift-XRT and UVOT observations
DATE:    12/08/31 18:43:14 GMT
FROM:    Wayne Baumgartner at GSFC  <wayne@milkyway.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC), M. Siegel (PSU),
F. E. Marshall (NASA/GSFC), J. L. Racusin (NASA/GSFC), J. A. Kennea
(PSU), and D. N. Burrows (PSU) report on behalf of the Swift team:

Swift observed the the error circle for the Fermi/LAT and IPN detected
GRB 120831A (Vianello et al., GCN Circ. 13704, Hurley et al. GCN Circ
13705). Two 4 ks XRT observations were taken to cover the IPN error
region, beginning about 60 ks and 72 ks after the burst.  Together
these two XRT observations cover 100% of the IPN error box.

One uncatologed X-ray source is found within the IPN error box at RA,
Dec = 88.501667, -28.701333 which is equivalent to:

RA (J2000): 05h 54m 00.40s
Dec (J2000): -28d 42' 04.8"

with an uncertainty of 8 arcsec (radius, 90% confidence).  The XRT
source has a significance of 2.5 sigma, and the count rate during this
observation in photon counting mode was 2.53e-3 +/- 1.0e-3 cts sec^-1.

The Swift/UVOT began settled observations of the first of the two
fields for GRB 120830A 59804 s after the LAT/IPN trigger.  No data are
available yet for the second field.  A source consistent with the XRT
source is detected in the initial UVOT exposures.  There is no
corresponding source in the USNO-B1.0 catalog.

The preliminary UVOT position is:
     RA  (J2000) =  05:54:00.65 =  88.50270 (deg.)
     Dec (J2000) = -28:42:06.4  = -28.70178 (deg.)
with an estimated uncertainty of 0.55 arc sec. (radius, 90% confidence).

Preliminary results 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            59804        67310         3679         20.42 +/- 0.04

The magnitude in the table is not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.032 in the direction of the burst
(Schlegel et al. 1998).

There is no convincing evidence for UVOT variability of the source.

Further Swift observations are planned to determine whether the source
is fading.


GRB_name: GRB120830A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13710
SUBJECT: GRB 120830A: catalog source at Uvot position
DATE:    12/09/01 09:28:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

Vladimir Lipunov, Lomonosov Moscow State University, SAI

There is one infrared source at Swift Uvot OT canddate position 
(Baumgartner et al., GCN 13709) in WISE All-Sky data Release J055400.58-284205 with 0.9 arcsec
  offset.

There is one nonstar object (Jmag = 22.3)in the Guide Star Catalog with 
offset 0.1 arcsec.

Both objects may be same.

This message can be cited.


GRB_name: GRB120830A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13711
SUBJECT: GRB 120830A: Further Swift Observations
DATE:    12/09/01 16:41:42 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), V. D'Elia (ASDC), M. Siegel (PSU),
and W. H. Baumgartner (GSFC/UMBC) report on behalf of the Swift team:
  
Swift observed again the Fermi/LAT-detected GRB 120830A (Vianello et
al., GCN Circ. 13704; Hurley et al., GCN Circ 13705).

A new 4 ks XRT observation was taken to check for variability of the
source reported in Baumgartner et al. (GCN Circ. 13709). The
observation began about 129 ks after the burst. The x-ray source previously
detected at low confidence with a count rate of (2.53 +/- 1.0)e-3
cts/s is no longer detected with a three sigma upper limit of
2.18e-03 cts/s.

UVOT made a second observation of GRB 120830A starting
129 ks after the LAT/IPN trigger. The flux of the UVOT source
previously detected has not changed, indicating
that it is unlikely to be the afterglow of the GRB.
As noted by Lipunov (GCN Circ. 13710), the
source position is consistent with a WISE catalogued source.

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

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag
white            59804        67310         3679         20.42 +/- 0.04
white           128849       136335         3883         20.43 +/- 0.04

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.032 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120802A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13712
SUBJECT: GRB 120802A: optical observations in CrAO
DATE:    12/09/04 13:10:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU/IKI), L. Elenin (KIAM),  V. Rumyantsev (CrAO), 
A.Pozanenko (IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  GRB 120802A (Holland et al., GCN 13555) with 
Shajn telescope of CrAO starting on Aug. 15 (UT) 23:00:26. We took several 
images in R-filter under mean seeing of 2.8".  In a stacked image we do not 
detect the object suggested as optical counterpart of GRB 120802A (Elenin et 
al., GCN 13609) up to 22.5 m. Thus we can confirm the object reported in 
(Elenin et al., GCN 13609) is most probably is an afterglow of  GRB 120802A. 
A photometry of  the filed is based on nearby USNO-B1.0 (R2) stars:

   T0+,    Filter      Exposure, OT,  UL (3 sigma)
  mid, d                  (s)

13.625    R           3540          n/d         22.5

We are grateful for CCD PL4240 provided by ISON for Shajn telescope.


GRB_name: GRB120819A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13713
SUBJECT: GRB 120819A: optical upper limit
DATE:    12/09/04 13:14:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

Yu. Krugly, V. Chiorny (Institute of Astronomy of Kharkiv National 
University), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko (IKI) 
report on behalf of larger collaboration:

We observed the afterglow of GRB 120819A (Beardmore  et al. GCN 13681) with 
0.7m  telescope of Institute of Astronomy, Kharkiv National Univ. starting 
on Aug. 19 (UT) 18:27:41. A set of images were taken in R-filter.   We do 
not detect optical afterglow (Malesani et al. GCN 13683; Sudilovsky et 
al.GCN 13688). The photometry is based on the nearby USNO-B1.0 (R2) stars:

   T0+,      Filter   Exposure,  OT,   UL (3 sigma)
 mid, d                  (s)

0.22102    R        2160          n/d    20.3


GRB_name: GRB100706A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13714
SUBJECT: LIVE CURVE grbGRB 100706a
DATE:    12/09/05 13:30:54 GMT
FROM:    Stan Otwinowski at UCLA/CERN  <Stanislaw.Otwinowski@cern.ch>

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GRB_name: GRB120804A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13715
SUBJECT: XMM observations of the short GRB120804A
DATE:    12/09/05 19:53:38 GMT
FROM:    Raffaella Margutti at Harvard  <raffaella.margutti@gmail.com>

R. Margutti (Harvard), V. Mangano (INAF IASF-Palermo), E. Berger, and  W.
Fong (Harvard) report:

"We observed  the short GRB120804A (GCN 13573) with XMM-Newton
starting on 2012 August 22, 21:51:29 UT (18.8 days after the burst).
GRB120804A is clearly detected at a level of 6 sigma with count-rate of
(4.3 +\- 0.7)e-3 cps (0.2-10 keV) in the pn. The pn net exposure time is
25.5 ks.
Using our best estimate of the intrinsic neutral hydrogen absorption
(NH_int=3.2e21 cm-2) and the Galactic absorption in the direction of the
burst (NH_gal=9.3e20 cm-2, Kalberla et al., 2005), this translates into
an unabsorbed 0.3-10 keV flux of  2.4e-14 erg/s/cm2. Our analysis
does not support the presence of a jet break for t< 18.8 days.
Combining the Swift-XRT (GCN 13580), Chandra (GCN 13640, 13643) and
XMM observations, for t>10^4 s the X-ray afterglow of GRB120804A is
best modeled by a simple power-law decay with index=1.0 +\- 0.1.

We thank the XMM-Newton staff for approving this observation."


GRB_name: GRB120907A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13716
SUBJECT: GRB 120907A: Swift detection of a burst with optical counterpart
DATE:    12/09/07 00:38:43 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. L. Racusin (NASA/GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), S. T. Holland (STScI), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 00:24:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120907A (trigger=532871).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 74.741, -9.314 which is 
   RA(J2000)  =  04h 58m 58s
   Dec(J2000) = -09d 18' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single pulse
with a duration of about 5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 00:25:45.1 UT, 82.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 74.7494, -9.3143 which
is equivalent to:
   RA(J2000)  = 04h 58m 59.86s
   Dec(J2000) = -09d 18' 51.3"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 29 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 5.35
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
142 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 04:59:00.01 =  74.75005
  DEC(J2000) = -09:18:54.2  =  -9.31505
with a 90%-confidence error radius of about 0.63 arc sec. This position is 4.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.63 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.09. 

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: GRB120907A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13717
SUBJECT: GRB 120907A: ROTSE-III Optical Limits
DATE:    12/09/07 00:59:19 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich), H. Flewelling (IfA/Hawaii), report on behalf of the ROTSE
collaboration: 

ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, automatically responded to GRB 120907A (Swift trigger 532871;
Racusin et al., GCN 13716). An automated response took the first image at
00:31:23.7 UT, 420 s after the burst, under fair conditions. We took 10
5-sec, 10 20-sec and 0 60-sec exposures. These unfiltered images are
calibrated relative to USNO A2.0 (R). Imaging is on going. 

We do not detect the candidate afterglow reported in GCN 13716. Individual
images have limiting magnitudes ranging from 14.0-15.4; we set the following
specific limits. 

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?

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

00:31:23.7   00:31:07.0         5      14.8            420       N

00:31:23.7   00:33:35.0        50      15.8            420       Y

00:33:40.0   00:38:20.0       200      16.4            557       Y


GRB_name: GRB120907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13718
SUBJECT: GRB 120907A MASTER optical observations 
DATE:    12/09/07 02:35:27 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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.Krushinski, I.Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed  to the  GRB120907A 375 s after notice 
time and 389  sec after GRB time at 2012-09-07 00:30:52  UT in a two 
polarizations.
We are marginaly see SWIFT-UVOT optical transient (J. L. Racusin et. al. 
GCN 13716) on out first images.
The unfiltred OT magnitude is about 17.5 mag.
The long pointing time  was due to some technical issues.
The message may be cited.


GRB_name: GRB120907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13719
SUBJECT: GRB 120907A: NOT optical observations
DATE:    12/09/07 06:51:15 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (DARK/NBI), D. Xu (WIS) and S. Schulze (PUC and MCSS) report on behalf of a larger collaboration:

We observed the field of the Swift GRB 120907A (Racusin et al., GCN 13716) with the NOT telescope equipped with StanCam. Eight I-band images with integration times of 120 s each were obtained on 2012-09-07 starting at 03:49 UT, which is roughly 3.4 hours after the trigger.

The optical afterglow (Racusin et al., GCN 13716) is clearly detected in our images. We derive a preliminary magnitude of

I = 20.2 +/- 0.1
 
centered at approximatly 3.6 hours after the trigger and assuming that the USNO star at RA(J2000) = 04:58:58.52, decl.(J2000) = -09:18:00.7 has an I-band magnitude of 15.28. An additional systematic uncertainty in the absolute brightness of about 0.3 mag is expected due to the calibration against the USNO catalog.

We are grateful to the NOT staff and observer, Anlaug Amanda Djupvik, for obtaining these observations.


GRB_name: GRB120907A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13720
SUBJECT: GRB 120907A: Swift-BAT refined analysis
DATE:    12/09/07 14:46:18 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120907A (trigger #532871)
(Racusin, et al., GCN Circ. 13714).  The BAT ground-calculated position is
RA, Dec = 74.736, -9.323 deg which is 
   RA(J2000)  =  04h 58m 56.7s 
   Dec(J2000) = -09d 19' 21.2" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.
 
The mask-weighted light curve shows 2 or 3 somewhat overlapping peaks
starting at ~T-1 sec, peaking at ~T+1 sec, and ending at ~T+20 sec.
T90 (15-350 keV) is 16.9 +- 8.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.04 to T+18.76 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.73 +- 0.25.  The fluence in the 15-150 keV band is 6.7 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 2.9 +- 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/532871/BA/


GRB_name: GRB120907A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13721
SUBJECT: GRB 120907A: Fermi GBM detection
DATE:    12/09/07 15:27:07 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (MSFC/USRA) reports on behalf of the Fermi GBM Team:

"At 00:24:24.51 UT on 07 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120907A (trigger 368670267 / 120907017)
which was also detected by the Swift/BAT (Barthelmy et al. 2012, GCN 13716).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 110 degrees.

The GBM light curve consists of a single pulse with a duration (T90)
of about 5.8 s (50-300 keV).
The time-averaged spectrum from T0-1.4 s to T0+0.7 s is
best fit by a power law function with an exponential high-energy cutoff.
The power law index is -0.75 +/- 0.25 and the cutoff energy,
parameterized as Epeak, is 154.50 +/- 32.90 keV.

The event fluence (10-1000 keV) in this time interval is
(7.8 +/- 1.1)E-07 ergs/cm^2. The 1-sec peak photon flux measured
starting from T0-1.1 s in the 10-1000 keV band
is 4.3 +/- 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: GRB120907A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13722
SUBJECT: GRB 120907A: Enhanced Swift-XRT position
DATE:    12/09/07 16:07:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 4509 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 120907A, 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 = 74.74990, -9.31501 which is equivalent
to:

RA (J2000): 04h 58m 59.98s
Dec (J2000): -09d 18' 54.0"

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: GRB120907A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13723
SUBJECT: GRB 120907A: Spectroscopy from OSIRIS/GTC
DATE:    12/09/07 16:35:20 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

R. Sanchez-Ramirez, J. Gorosabel (IAA-CSIC), A. de Ugarte Postigo 
(IAA-CSIC, DARK/NBI) and J.M. Gonzalez Perez (GTC) report 
on behalf of a larger collaboration:

We have obtained spectroscopy of the afterglow of GRB 120907A 
(Racusin et al. GCN 13716) with OSIRIS/ GTC (La Palma, Spain) on 
Sep 7.20647-7.23893 UT (4.55-5.33 hours post GRB). The observation 
consisted of 3x900s exposures using the R1000R grating, covering the 
range from 5100 to 10000 A with a resolution of ~1100.

In the combined spectrum we detect several absorption features 
corresponding to FeII, MgII, MgI and CaII at a common redshift of z=0.970, 
which we identify as the redshift of the GRB.

We acknowledge the excellent support of the GTC staff.


GRB_name: GRB120907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13724
SUBJECT: GRB 120907A: Swift-XRT refined Analysis
DATE:    12/09/07 16:38:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 16 ks of XRT data for GRB 120907A (Racusin  et al. GCN
Circ. 13716), from 93 s to 46.4 ks after the  BAT trigger. The data
comprise 76 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN. Circ 13722).

The late-time light curve (from T0+4.5 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.02 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.91 (+0.13, -0.12). The
best-fitting absorption column is  10.0 (+3.1, -2.9) x 10^20 cm^-2, in
excess of the Galactic value of 5.4 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      10.0 (+3.1, -2.9) x 10^20 cm^-2
Galactic foreground: 5.4 x 10^20 cm^-2
Excess significance: 2.7 sigma
Photon index:      1.91 (+0.13, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00532871.

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


GRB_name: GRB120907A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13725
SUBJECT: GRB 120907A: Swift/UVOT Detection
DATE:    12/09/07 19:17:57 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) 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 120907A
142 s after the BAT trigger (Racusin et al., GCN Circ. 13716).
A source consistent with the enhanced XRT position (Goad et al. GCN Circ. 13722)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  04:59:00.00 =  74.75002 (deg.)
  Dec (J2000) = -09:18:54.0  =  -9.31501 (deg.)
with an estimated uncertainty of 0.52 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

v                  449         6811        471         >19.5
b                  398         567          39         19.02 +/- 0.29
u                  142         392         246         17.67 +/- 0.08
w1                 498         666          40         18.27 +/- 0.32
m2                 473         1122         79         18.68 +/- 0.36
w2                 424         642          39         18.56 +/- 0.37

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: GRB120907A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13726
SUBJECT: GRB 120907A: EVLA observations
DATE:    12/09/08 16:47:19 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer and E. Berger (Harvard) report:

"We observed the position of GRB 120907A (GCN 13716) with the EVLA
beginning 2012 September 7.46 UT (10.5 hours after the burst). No
significant radio emission is detected at the enhanced Swift-XRT position
(GCN 13724), the UVOT position (GCN 13725) or optical position (GCN 13719).
Preliminary analysis indicates a three-sigma upper limit of 75 uJy at 5.8
GHz. Further observations are planned."


-- 
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
3rd Yr Graduate Student in Astronomy
Harvard-Smithsonian Center for Astrophysics
A-107, 60 Garden St, Cambridge (617)-495-5989
http://www.cfa.harvard.edu/~tlaskar
Mobile: (617)-899-9361
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~


GRB_name: GRB120909A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13727
SUBJECT: GRB 120909A: Swift detection of a burst
DATE:    12/09/09 01:54:56 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Immler (CRESST/GSFC/UMD), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. T. Holland (STScI), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 01:42:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120909A (trigger=533060).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 275.685, -59.426 which is 
   RA(J2000)  =  18h 22m 44s
   Dec(J2000) = -59d 25' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows one, possibly two, peaks
with a duration of about 5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 01:43:36.6 UT, 93.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 275.7388, -59.4485 which is equivalent to:
   RA(J2000)  = +18h 22m 57.31s
   Dec(J2000) = -59d 26' 54.6"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 127 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 7.55e-09 erg cm^-2 s^-1 (0.2-10
keV). 

Because of an earth limb constraint, Swift slewed away before UVOT 
could take its initial exposures.  Subsequent orbits will include 
UVOT observations. 

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


GRB_name: GRB120909A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13728
SUBJECT: Skynet/PROMPT Observations of GRB120909A
DATE:    12/09/09 02:24:04 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

J. Haislip, A. LaCluyze, K. Ivarsen, D. Reichart, J. Moore, H. T. 
Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. 
Speckhard, A.Trotter, and J. A. Crain report:

Skynet observed the field of GRB120909A (GCN 13727, Swift trigger #533060) 
with the PROMPT telescopes located at CTIO in Chile beginning ~4 minutes 
after the burst. We detect a fading, uncataloged source at RA 18:22:56.72 
DEC -59:26:54.0, roughly coinciding with the location of the Swift trigger 
with an initial magnitude of ~16.3 in R, calibrated to the NOMAD catalog.

Further observations are ongoing.


GRB_name: GRB120909A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13729
SUBJECT: GRB 120909A: GROND detection of the afterglow
DATE:    12/09/09 02:41:37 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120909A (Swift trigger 533060; Immler et al.,
GCN #13727) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 01:44 UT, September 09, 140s after the burst, and
are continuing. They were performed at an average seeing of 1".6 and at an
average airmass of 1.2 .

We found a single point source within the 4".8 Swift-XRT error circle
reported by Immler et al. (GCN #13727) at

RA (J2000) = 18h 22m 56.72s

DEC (J2000) = -59d 26' 54".1

with an uncertainty of 0".5 in each coordinate, which is consistent with
the position reported by Haislip et al. (GCN #13728)   .

Based on the first 141s of total exposures in g'r'i'z' and 240s in JHK,
we estimate preliminary magnitudes (all in AB) of

g' = 18.4 +- 0.1,
r' = 16.6 +- 0.1,
i' = 15.8 +- 0.1,
z' = 15.5 +- 0.1,
J = 14.8 +- 0.1,
H = 14.5 +- 0.1, and
K = 14.3 +- 0.1.

Based on the the significantly lower flux in g', this suggests a 
redshift z>3.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.08 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120909A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13730
SUBJECT: GRB 120909A: X-Shooter redshift 3.93
DATE:    12/09/09 05:22:52 GMT
FROM:    Olga Hartoog at U of Amsterdam  <O.E.Hartoog@uva.nl>

O. E. Hartoog (Uva, NL), D. Malesani (DARK/NBI), K. Wiersema (U. Leicester,
UK), T. Kruehler (DARK/NBI),  S. Schulze (PUC and MCSS), A. de Ugarte
Postigo (IAA/CSIC and DARK/NBI), V. D'Elia (INAF/Roma and ASI/ASDC), J. P.
U. Fynbo (DARK/NBI), report on behalf of the X-shooter GRB GTO
collaboration:

We observed the optical counterpart of GRB 120909A (Immler et al., GCN
13727; Haislip et al., GCN 13728; Sudilovsky et al., GCN 13729) with the
ESO VLT equipped with the X-shooter spectrograph. Observations were carried
out starting on 2012 Sep 9.14 UT (1.7 hr after the GRB), for a total
exposure time of 20 min, covering the wavelength range 3000-25000 AA.

We detect several absorption features, including Ly-a, FeII, NiII, SiII,
SII, AlII, AlIII, CII, OI, CIV, ZnII all at a common redshift z = 3.93. In
particular, the presence of fine-structure lines (Fe II*, SiII*, OI*, OI**,
CII*) makes the redshift securely associated to the GRB.

We acknowledge support from the VLT staff, in particular Giovanni Carraro
and Giacomo Beccari.


GRB_name: GRB120908A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13731
SUBJECT: GRB 120908A: MAXI/GSC detection
DATE:    12/09/09 09:45:22 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

M. Morii (Tokyo Tech), K. Yamaoka (Waseda U.), H. Negoro (Nihon U.),
S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, M. Serino, T. Yamamoto, J. Sugimoto, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech),
A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.),
M. Nakajima, M. Asada, N. Serita (Nihon U.),
Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.),
M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.), 
report on behalf of the MAXI team:

MAXI/GSC triggered a bright uncatalogued X-ray transient source at UT 2012-09-08T22:35:13.
Assuming that the source flux was constant over the transit,
we obtain the source position at 

(R.A., Dec) = (230.64 deg, -25.79 deg) = (15 22 32, -25 47 42) (J2000)

with a statistical 90% C.L. elliptical error region
with long and short radii of 0.46 deg and 0.31 deg, respectively.
The position angle of long axis is -30 deg.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).

The preliminary flux of the transient source was 78 +- 19 mCrab (4 - 10 keV).
There was no significant detection at the transit location in the
previous and the next orbit (92 min before and after the detection)
with an upper limit of 20 mCrab.
There is no known bright X-ray source at the detected position.

Follow-up observations are encouraged.


GRB_name: GRB120909A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13732
SUBJECT: GRB 120909A: Enhanced Swift-XRT position
DATE:    12/09/09 13:23:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1720 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 120909A, 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 = 275.73656, -59.44863 which is equivalent
to:

RA (J2000): 18h 22m 56.78s
Dec (J2000): -59d 26' 55.1"

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

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

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


GRB_name: GRB120909A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13733
SUBJECT: GRB 120909A: Swift-BAT refined analysis
DATE:    12/09/09 15:03:07 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
S. Immler (CRESST/GSFC/UMD), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-41 to T+556 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120909A (trigger #533060)
(Immler, et al., GCN Circ. 13727).  The BAT ground-calculated position is
RA, Dec = 275.735, -59.432 deg which is 
   RA(J2000)  =  18h 22m 56.5s 
   Dec(J2000) = -59d 25' 55.2" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.
 
The mask-weighted light curve shows multiple overlapping peaks. The burst was
already occurring when Swift-BAT came out of the SAA at ~T-40 sec.
The observed peaks occurred at ~T-38, ~T+1, ~T+28, and ~T+48 sec.
The burst returned to baseline at ~T+200 sec.  There is a possible peak
at ~T+490 to ~T+580 sec, at which point Swift had to slew due to an observing
constraint and the location went out of the BAT FoV.
 
The time-averaged spectrum from T-38.98 to T+95.17 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.39 +- 0.06.  The fluence in the 15-150 keV band is 6.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.88 sec in the 15-150 keV band
is 1.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/533060/BA/


GRB_name: GRB120909A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13734
SUBJECT: GRB 120909A: Swift-XRT refined Analysis
DATE:    12/09/09 15:55:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

V. Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), 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), B. Sbarufatti
(INAF-OAB/PSU) and S. Immler report on behalf of the Swift-XRT team:

We have analysed 9.3 ks of XRT data for GRB 120909A (Immler  et al. GCN
Circ. 13727), from 3.3 ks to 33.3 ks after the BAT trigger. The data
comprise 173 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN. Circ 13732).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.19 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+/-0.09). The
best-fitting absorption column is  1.9 (+0.8, -0.7) x 10^22 cm^-2, at a
redshift of 3.93, in addition to the Galactic value of 6.5 x 10^20
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.5 x
10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 6.5 x 10^20 cm^-2
Intrinsic column:    1.9 (+0.8, -0.7) x 10^22 cm^-2 at z=3.93
Photon index:      2.04 (+/-0.09)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00533060.

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


GRB_name: GRB120909A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13735
SUBJECT: GRB 120909A: Swift/UVOT Detection
DATE:    12/09/09 18:02:19 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and S. Immler (CRESST/GSFC/UMD) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120909A
3308 s after the BAT trigger (Immler et al., GCN Circ. 13727).
A source consistent with the optical position (Sudilovsky et al. GCN 
Circ. 13729), is detected in the initial UVOT exposures.

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

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

white             3308         4690          344         20.75  0.20
v                 3465        16690         1261        >20.2
b                 4285        23216          937        >21.5
u                 4080        22450         1848        >21.4
w1                3875        21536         1968        >21.6
m2                3670        17445         1820        >21.4
w2                4696        15776         1082        >21.6

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: GRB120909A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13736
SUBJECT: Konus-Wind observation of GRB 120909A
DATE:    12/09/09 18:28:23 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 120909A (Swift-BAT trigger #533060:
Immler et al., GCN 13727; Ukwatta et al., GCN 13733)
was detected by Konus-Wind in the waiting mode
starting at 6069 s UT (01:41:09), ~54s before the T0(BAT).

The burst light curve shows a multi-peaked structure
with a total duration of ~115s.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB120909A/

As observed by Konus-Wind, the burst had a fluence
of (2.3  0.2)x10-5 erg/cm2 and a peak energy flux,
measured on the 2.944-s scale, of (6.1  0.8)x10-7 erg/cm2
(both in the 20 - 1500 keV energy range).

Modelling the K-W 3-channel time-integrated spectrum
(from T0(BAT)-54s to T0(BAT)+61 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.23  0.04, and Ep = 335  25 keV

Assuming X-Shooter redshift of z=3.93 (Hartoog et al., GCN 13730)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, 
Omega_Lambda = 0.73:
the isotropic energy release E_iso is (6.9  0.5)x10^53 erg,
the isotropic peak luminosity L_iso_max is (9.0  1.2)x10^52 erg/s,
and Ep_rest is (1650  120) keV.

All the quoted errors are estimated at the 1 sigma confidence level.


GRB_name: GRB120909A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13737
SUBJECT: GRB 120909A: Fermi GBM observation
DATE:    12/09/09 19:49:34 GMT
FROM:    Vandiver Chaplin at UAH/Fermi-GBM  <chapliv@email.uah.edu>

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

At 01:41:22.40 UT on 09 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120909A (trigger 368847685 / 120909070), 
which was also detected by the Swift/BAT (Immler et al. 2012, GCN 13727)
The GBM on-ground location is consistent with the Swift position.
The angle to the Fermi LAT boresight is 66 degrees.

The GBM light curve consists of several peaks between T0
and T0+100 seconds, with a total duration (T90) of about 
112 s (50-300 keV).

The time-averaged spectrum from T0-2.8 s to T0+104.7 s is
best fit by a power law with exponential cutoff having 
an index of -1.3 +/- 0.1 and cutoff energy 370 +/- 140 keV.
The event fluence (10-1000 keV) in this time interval is
(2.1 +/- 0.2)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.26 s in the 10-1000 keV band
is 3.0 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB120909A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13738
SUBJECT: GRB 120909A: Pi of the Sky upper limits
DATE:    12/09/09 21:17:21 GMT
FROM:    Lech Wiktor Piotrowski at U Warsaw  <lewhoo@fuw.edu.pl>

T.Batsch,A.Cwiek,A.Majcher,A.Majczyna,K.Nawrocki,M.Sokolowski,G.Wrochna 
(NCBJ, Swierk),
M.Cwiok,L.W.Piotrowski,M.Zaremba,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz (Warsaw University of Technology),
from the "Pi of the Sky" collaboration ( http://grb.fuw.edu.pl ).

The wide field "Pi of the Sky South" telescope, installed in
the private observatory of Alain Maury in San Pedro de Atacama 
(http://grb.fuw.edu.pl/pi/index.html#spda_site.htm) observed coordinates 
of the GRB 120909A, starting 10 s exposure 94 s after the reported SWIFT 
BAT detection. No new source was identified. The limiting magnitude is 
11.6, based on the reference star magnitudo in V filter.

We acknowledge support received from Alain Maury at SPdA Observatory.

This message can be cited.


GRB_name: GRB120909A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13739
SUBJECT: GRB 120909A: TAROT La Silla observatory optical observations
DATE:    12/09/10 09:07:00 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120909A detected by SWIFT
(trigger 533060) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 40s after the GRB trigger
(14s after the notice). The elevation of the field decreased
from 54 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We detect the optical transient discovered by
Haislip et al. (GCNC 13728).

Relative photometric analysis is done using R=14.37
for the star NOMAD1 0305-0869420 (R.A.=275.7585731
Decl=-59.4476147 J2000).

The careful analysis of the trail is compatible with a
constant magnitude of R=17.1 from T+40s to T+100s.
There is not optical peak during the gamma peak
at T+48s reported by Ukwatta et al. (GCNC 13733).

After the trailed image, a technical problem caused the
lost of images until T+439s. Following images have been
acquired using the classical diurnal drift.

Summary of the first observations is:

Start  Stop  Rmag  Error
   40s  100s  17.1    0.1 (continuous photometry)
  439s  529s  16.5    0.1
  539s  629s  18.9    0.1
  640s  729s  19.1    0.2
  744s  834s  19.3    0.2
  845s  935s  19.7    0.2

Magnitudes are not corrected for galactic dust extinction
(which should be about 0.4 magnitude in the R band according
to D. Schlegel et al. 1998ApJ...500..525S).

This message may be cited.


GRB_name: GRB120908A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13740
SUBJECT: GRB 120908A: Swift Observations
DATE:    12/09/10 14:55:07 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (CRESST/GSFC/UMD), C. Pagani (U. Leicester), and
A. A. Breeveld (MSSL-UCL) report on behalf of the Swift team:

Swift began a Target of Opportunity observation of the MAXI/GSC
discovered burst GRB 120908A (Morii et al. GCN 13731) at 2012-09-09
13:41:43 UT.

We have analyzed 3.7 ks of XRT data, starting ~54 ks after the MAXI
trigger. The data are entirely in Photon Counting mode, centered on
the MAXI position and partially covering the MAXI error region.
No new source is detected in the XRT data. The 3-sigma upper limit
is 0.004 counts/sec which is 2.4e-13 erg cm^-2 s^-1 for a typical GRB
spectrum.

The Swift/UVOT began settled observations of the field 54.4 ks after
the MAXI trigger (Morii et al., GCN Circ. 13731). No optical afterglow
consistent with the MAXI position given in that circular 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            54383        66117         2345         >21.7

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


GRB_name: GRB120908A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13741
SUBJECT: GRB 120908A: Fermi GBM detection
DATE:    12/09/10 18:08:47 GMT
FROM:    Sinead McGlynn at Excellence Cluster/TUM  <smcglynn@tum.de>

Sinead McGlynn (MPE/TUM)
reports on behalf of the Fermi GBM Team:

"At 22:31:00.02  UT on 08 September 2012, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 120908A (trigger 368836263/120908938). GBM was triggered over 4 minutes earlier than the bright X-ray source reported as a MAXI/GSC detection by Morii et al. (GCN 13731). 

The on-ground GBM location is consistent with the MAXI/GSC reported location. As a result, and due to the presence of extended soft emission in the GBM data at the time of the MAXI/GSC detection, we associate the GBM trigger with GRB 120908A.

The angle from the Fermi LAT boresight is 87 degrees.

The GBM light curve consists of two spiky pulses with a duration (T90) of about 66  s (50-300 keV).
The time-averaged spectrum from T0-5.38 s to T0+15.1 s is best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.21 +/- 0.11 and the cutoff energy, parameterized as Epeak, is 205.9 +/- 43.1 keV. In addition, weak longer-lived soft emission is observed close to the MAXI trigger time (200-300s post GBM trigger) up to approximately 50 keV.

The event fluence (10-1000 keV) in this time interval is (1.7 +/- 0.2)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+6 s in the 10-1000 keV band is 2.7 +/- 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: GRB120908A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13742
SUBJECT: GRB 120908A and GRB 120909A : Fermi/LAT upper limit
DATE:    12/09/10 19:20:18 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

Weikang Zheng and Carl Akerlof (Umich), report on behalf of the ROTSE
collaboration:

We analyzed Fermi/LAT data of GRB 120908A (Morii et al., GCN 13731)
and GRB 120909A (Immler et al., GCN 13727)
as a follow-up of routine search in Swift trigger catalogs in our LAT
data processing pipeline using both the matched filter technique
(Akerlof et al. 2010, ApJ, 725, L15; 2011 ApJ, 726, 22; 2012,
arXiv:1205.3066; Zheng et al. 2012, ApJ 745,72; ApJ, 756, 64)
and likelihood method. We do NOT detect high energy photon emission
from both methods in the two GRBs.

A standard data selection method is applied when extracting the LAT
photon data with energy E > 100 MeV, and a duration of T0 - T0+47.5s
after the trigger. A zenith angle cut of <105 degree is applied to
all photons.

For GRB 120908A, the burst location was about 72 degrees from the
LAT boresight, and the zenith angle was about 64 degrees at trigger time.
Using the likelihood method, we estimated the upper limit in LAT energy
range (0.1 - 10 GeV) is 8.3e-09 (photons cm^-2 s^-1) by assuming a
spectral index of -2.2.
The pipeline result of GRB 120908A is given in the following link:
http://www.rotse.net/LAT/SwiftTriggers/368836516/

For GRB 120909A, the burst location was about 65 degrees from the
LAT boresight, and the zenith angle was about 98 degrees at trigger time.
Using the likelihood method, we estimated the upper limit in LAT energy
range (0.1 - 10 GeV) is 2.0e-08 (photons cm^-2 s^-1) by assuming a
spectral index of -2.2.
The pipeline result of GRB 120909A is given in the following link:
http://www.rotse.net/LAT/SwiftTriggers/368847726/


GRB_name: GRB120907A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13743
SUBJECT: GRB 120907A:  SMA upper limits
DATE:    12/09/11 02:18:39 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

G. Petitpas (SAO), A. Zauderer, T. Laskar, E. Berger (Harvard) report
on behalf of the SMA Rapid Transients (SMART) Key Project:

"We observed the position of GRB 120907A (Racusin et al; GCN 13716)
with the Submillimeter Array (SMA) beginning 2012 Sep 7.63 UT (dt ~ 0.6 
d).  At a mean frequency of 230 GHz, we do not detect significant radio 
emission within the enhanced Swift/XRT error circle (Goad et al; GCN 
13702) to a 3-sigma upper limit of 2.7 mJy.  Beginning 2012 Sep 8.5 UT 
(dt ~ 1.5 d), we repeated our observations, and report a 3-sigma upper 
limit of 2.4 mJy.

We thank the SMA Observatory staff for its support."


GRB_name: GRB120911A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13744
SUBJECT: GRB 120911A: Swift detection of a burst
DATE:    12/09/11 07:34:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. K. Cannizzo (NASA/UMBC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), C. Guidorzi (U Ferrara),
C. B. Markwardt (NASA/GSFC), A. Maselli (INAF-IASFPA),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. H. Siegel (PSU) and E. Troja (NASA/GSFC/ORAU) report on behalf of
the Swift Team:

At 07:08:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120911A (trigger=533268).  Swift could not immediately slew
due to the Earth limb constraint.  The BAT on-board calculated location is 
RA, Dec 357.961, +63.099 which is 
   RA(J2000) = 23h 51m 51s
   Dec(J2000) = +63d 05' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex structure
with a duration of at least 30 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+51.6
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB120911A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13745
SUBJECT: GRB 120911A: ROTSE-III Optical Limits
DATE:    12/09/11 07:45:30 GMT
FROM:    Wiphu Rujopakarn at U AZ/Steward  <rujopakarn@gmail.com>

W. Rujopakarn (Steward), T. Guver (Sabanci U), report on behalf of the
ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
120911A (Swift trigger 533268; Cannizzo et al., GCN 13744), producing
images beginning 9.2 s after the GCN notice time. An automated
response took the first image at 07:09:04.2 UT, 30.4 s after the
burst, under fair conditions. We took 10 5-sec, 10 20-sec and 40
60-sec exposures. These unfiltered images are calibrated relative to
USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle; however, we are limited as the field
is somewhat crowded. Individual images have limiting magnitudes
ranging from 15.5-16.6; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
07:09:04.2   07:09:09.2         5     15.5           30.4       N
07:09:04.2   07:10:46.4        50     16.9           30.4       Y


GRB_name: GRB120911A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13746
SUBJECT: GRB 120911A: Swift-XRT observations
DATE:    12/09/11 09:07:47 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

S. Campana (INAF-OAB), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU) and G. Tagliaferri
(INAF-OAB) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 120911A at 08:04:07.0 UT,
3333.2 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 357.98152,
63.09831 which is equivalent to:
   RA(J2000)  = 23h 51m 55.56s
   Dec(J2000) = +63d 05' 53.9"
with an uncertainty of 4.4 arcseconds (radius, 90% containment). This
location is 33 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 6.66
x 10^21 cm^-2 (Kalberla et al. 2005). 


GRB_name: GRB120911A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13747
SUBJECT: GRB 120911A: Faulkes Telescope North observations
DATE:    12/09/11 12:00:22 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

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

The 2-m Faulkes Telescope North automatically began observing
GRB 120911A (Cannizzo et al. GCN Circ. 13744) on September 11 2012,
08:17:24 UT corresponding to ~70 minutes post burst trigger
with BVRi' filters. Within the XRT error circle (Campana et al.
GCN Circ. 13746), we don't see any uncatalogued object down
to the following limits:

Mid time from       Exposure        Filter       Limit
GRB (hr)            (s)
----------------------------------------------------------
1.37                240             R > 20.9
1.45                220             i' > 21.2
----------------------------------------------------------

We note the presence of a faint, uncatalogued object
in the i' band, lying at 5.8" from the XRT centroid, with
a magnitude of i=21.0 +- 0.2 (calibrated against USNOB1 nearby
stars) at the following position:

RA(J2000) =  23:51:56.06
Dec(J2000)= +63:05:49.2

with an error of 0.6". Presently we cannot make any statement
about its temporal behaviour.


GRB_name: GRB120911A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13748
SUBJECT: GRB 120911A: Enhanced Swift-XRT position
DATE:    12/09/11 12:16:14 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2099 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 120911A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 357.97897, +63.09874 which is equivalent
to:

RA (J2000): 23h 51m 54.95s
Dec (J2000): +63d 05' 55.5"

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: GRB120911A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13749
SUBJECT: GRB 120911A: Swift-BAT refined analysis
DATE:    12/09/11 13:18:13 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. K. Cannizzo (NASA/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+863 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120911A (trigger #533268)
(Cannizzo, et al., GCN Circ. 13744).  The BAT ground-calculated position is
RA, Dec = 357.966, 63.090 deg, which is 
   RA(J2000)  =  23h 51m 51.9s 
   Dec(J2000) = +63d 05' 25.6" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 23%.
 
The mask-weighted light curve shows two barely overlapping peaks starting
at ~T-4 sec, peaking at ~T+1 and ~T+17 sec, and ending at ~T+50 sec.
T90 (15-350 keV) is 17.8 +- 3.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.84 to T+24.10 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.71 +- 0.16.  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-0.30 sec in the 15-150 keV band
is 2.7 +- 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/533268/BA/


GRB_name: GRB120911A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13750
SUBJECT: GRB 120911A: Swift-XRT refined Analysis
DATE:    12/09/11 16:15:12 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and J. K. Cannizzo (NASA/UMBC) report on
behalf of the Swift-XRT team:

We have analysed 7.2 ks of XRT data for GRB 120911A (Cannizzo  et al.
GCN Circ. 13744), from 3.3 ks to 17.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN. Circ
13748).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.31 (+0.22, -0.21).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+/-0.4). The
best-fitting absorption column is  8.4 (+3.4, -1.8) x 10^21 cm^-2,
consistent with the Galactic value of 6.7 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 5.4 x 10^-11 (1.0 x
10^-10) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.4 (+3.4, -1.8) x 10^21 cm^-2
Galactic foreground: 6.7 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.0 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00533268.

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


GRB_name: GRB120911A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13751
SUBJECT: GRB 120911A: Swift/UVOT Upper Limits
DATE:    12/09/11 18:48:50 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and J. K. Cannizzo (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120911A
3323 s after the BAT trigger (Cannizzo et al., GCN Circ. 13744).
No optical afterglow consistent with the XRT position (Beardmore et al.
GCN Circ. 13748) 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          3323         3473          147         >20.5
white             3323        11009         1229         >21.6
v                 3479        15918         1278         >19.9
b                 4300        10097         1160         >21.5
u                 4095         5730          393         >20.4
w1                3890         5526          393         >20.0
m2                3684         5320          393         >21.1
w2                4710        11585          757         >20.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.12 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120911A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13752
SUBJECT: GRB 120911A: Fermi/LAT upper limit
DATE:    12/09/11 21:05:23 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

Weikang Zheng and Carl Akerlof (Umich), report on behalf of the ROTSE
collaboration:

We analyzed Fermi/LAT data of GRB 120911A (Cannizzo et al., GCN 13744)
as a follow-up of routine search in Swift trigger catalogs in our LAT
data processing pipeline using both the matched filter technique
(Akerlof et al. 2010, ApJ, 725, L15; 2011 ApJ, 726, 22; 2012,
arXiv:1205.3066; Zheng et al. 2012, ApJ 745,72; ApJ, 756, 64)
and likelihood method. We do NOT detect high energy photon emission
from both methods.

A standard data selection method is applied when extracting the LAT
photon data with energy E > 100 MeV, and a duration of T0 - T0+47.5s
after the trigger. A zenith angle cut of <105 degree is applied to
all photons.

The burst location of GRB 120911A was only ~14 degrees from the
LAT boresight, almost in the center of the LAT field of view, and
the zenith angle was about 40 degrees at trigger time.
Using the likelihood method, we estimated the upper limit in LAT energy
range (0.1 - 10 GeV) is 1.1e-05 (photons cm^-2 s^-1) by assuming a
spectral index of -2.2.
The pipeline result of GRB 120911A is given in the following link:
http://www.rotse.net/LAT/SwiftTriggers/369040116/


GRB_name: GRB120911A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13753
SUBJECT: GRB120911A: MITSuME Okayama Optical upper limits
DATE:    12/09/12 06:18:19 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 collaboration:

We observed the field of GRB 120911A (Cannizzo et al., GCNC 13744)
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 2012-09-11 13:46:32 UT, (~6.6 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Beardmore et al., GCNC 13748) 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
------------------------------------------------------
0.31808    14:46:35    5940.0   >20.6  >19.8  >19.2
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120911A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13754
SUBJECT: GRB 120911A: Fermi GBM observation
DATE:    12/09/12 07:02:43 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team:

"At 07:08:33.99 UT on 11 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120911A (trigger 369040116 / 120911298).
which was also detected by the Swift/BAT (Cannizzo et al. 2012, GCN 13744).

The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 11 degrees.

The GBM light curve consists of two pulses
with a duration (T90) of about 22 s (50-300 keV).
The time-averaged spectrum from T0-4.6 s to T0+22.0 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.36 +/- 0.26 and
the cutoff energy, parameterized as Epeak, is 64.2 +/- 5.1 keV

The event fluence (10-1000 keV) in this time interval is
(2.34 +/- 0.04)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.38 s in the 10-1000 keV band
is 4.31 +/- 0.27 ph/s/cm^2.

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


GRB_name: GRB120911B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13755
SUBJECT: IPN Triangulation of GRB 120911B (long/bright)
DATE:    12/09/12 20:35:44 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley on behalf of the Mars Odyssey and MESSENGER GRB teams,

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

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi,
on behalf of the AGILE MCAL 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, intense GRB 120911B has been observed by INTEGRAL 
(SPI-ACS), AGILE (MCAL), Konus-Wind, and Mars Odyssey (HEND), so far, at 
about 23175 s UT (06:26:15).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   172.146 (11h 28m 35s) -37.696 (-37d 41' 46")
  Corners:
   172.616 (11h 30m 28s) -38.705 (-38d 42' 20")
   172.297 (11h 29m 11s) -38.543 (-38d 32' 34")
   171.709 (11h 26m 50s) -36.675 (-36d 40' 31")
   172.013 (11h 28m 03s) -36.848 (-36d 50' 53")
  ---------------------------------------------
The error box area is 0.380 sq. deg, and its maximum
dimension is 2.15 deg.

This box can be improved.

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


GRB_name: GRB120911B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13756
SUBJECT: GRB 120911B: Fermi-LAT detection of a burst
DATE:    12/09/12 22:29:28 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), G. Vianello (SLAC), D. Kocevski (NASA/GSFC), N. Omodei (Stanford), and M. Ohno (ISAS/JAXA), report on behalf of the Fermi-LAT team:

We report on ground analysis of the IPN detected GRB 120911B (GCN 13755) at 06:26:15 UT. The center of the IPN error box was at the edge of the LAT field of view, 67 degrees from the LAT boresight at the trigger time. The best LAT localized position is RA/Dec = 172.03, -37.51 (J2000), with a error radius of 0.3 deg (68% containment), using LAT source class events from 0-40 s after the trigger. This is within the IPN error box, 0.2 deg from the center.

The burst left the LAT field of view ~100 seconds after the trigger and returned ~4100 s later.

The LAT data show a significant increase in counts at energies >100 MeV, starting several seconds after the trigger, with a single peaked structure. The non-standard LAT Low Energy (LLE) event class shows two-peaks with a tail lasting to approximately T0+60 s.

A spectral fit of the LAT data in the 0-40 s window yields a photon index of -2.5 +/- 0.2 (68% containment, statistical only) and a flux of (2.0 +/- 0.4) x 10^-7 ph/s-cm^2 in the 100 MeV - 10 GeV energy range.

Fermi-GBM did not trigger on this GRB due to high geo-magnetic latitude, but it was clearly detectable in ground analysis. The GBM team will describe the observations in a subsequent circular.

The Fermi LAT point of contact for this burst is Masanori Ohno (ohno@hep01.hepl.hiroshima-u.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: GRB120911B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13757
SUBJECT: GRB 120911B: Fermi GBM observation
DATE:    12/09/12 23:37:58 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE), W. Paciesas (USRA), V. Plassa (UAH)
and V. Chaplin (UAH) report on behalf of the Fermi GBM Team:

"We report on the ground analysis of the IPN detected GRB 120911B (GCN 13755) 
in the GBM data.

The GBM light curve consists of a precursor starting at ~ 06:25:14 UT (T0) 
which is followed by a bright and hard main emission ~ 50 s later, lasting
for another ~ 40 s.
The duration (T90) is of about 69 s (50-300 keV).
The time-averaged spectrum from T0 to T0+132 s is best fit by a Band function
with Epeak = 1200 +/- 55 keV, alpha = -1.01 +/- 0.01,
and beta = -2.72 +/- 0.14.

The event fluence (10-1000 keV) in this time interval is
(1.973 +/- 0.026)E-04 erg/cm^2. The 4-sec peak photon flux measured
starting from T0+70 s in the 10-1000 keV band
is 33.04 +/- 0.7 ph/s/cm^2.

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


GRB_name: GRB120911B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13758
SUBJECT: Konus-Wind observation of GRB 120911B
DATE:    12/09/13 06:51:03 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense hard GRB 120911B
(IPN detection and localization: Hurley at al., GCN 13755;
Fermi-LAT detection: Racusin et. al., GCN 13756;
Fermi-GBM observation: Gruber et. al., GCN 13757)
triggered Konus-Wind at T0=23172.213s UT (06:26:12.213)

The light curve shows a bright hard pulse with a duration
of ~30 s followed by a tail of weaker and softer extended
emission during the next ~150 s; additionally,
a soft weak precursor is observed around T0-55 s.
The emission in the main bursting episode is seen up to 9 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120911_T23172/

As observed by Konus-Wind, the burst
had a fluence of 3.0(-0.1,+0.1)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+15.232 s,
of 3.8(-0.4,+0.4)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the main emission episode
(measured from T0 to T0+34.048 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 = -0.86 (-0.03, +0.03),
the high energy photon index beta = -2.6 (-0.2, +0.2),
the peak energy Ep = 950(-50, +50) keV,
chi2 = 78.4/82 dof.

The spectrum at the maximum count rate
(measured from T0+14.080 to T0+15.616 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 = -0.63 (-0.08, +0.09),
the high energy photon index beta = -2.9 (-1.6, +0.3),
the peak energy Ep = 1000(-120, +130) keV,
chi2 = 81.1/82 dof.


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


GRB_name: GRB120911A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13759
SUBJECT: GRB 120911A: optical upper limit ISON-NM
DATE:    12/09/13 07:13:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (SAI MSU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  the Swift GRB 120911A (Cannizzo  et al., GCN 
13744) with 0.45-m telescope of ISON-NM observatory  starting on  Sep. 11 
(UT) 07:10:42, i.e ~130 s after burst trigger.  We took  several unfiltered 
images of 30 s and 60 s exposures.  Within enhanced XRT afterglow position 
(Beardmore et al., GCN 13748) we do not detect any new object.   A 
preliminary  photometry of single and co-added frames is based  on the 
USNO-B1.0 (R2)  nearby  stars is following:

  T0+,          Exposure,  OT,         UL (3 sigma)
  mid, d         (s)

 0.0017          30             n/d           18.4
 0.0028      5x30             n/d           19.1
 0.0175    60x30             n/d           20.2
 0.0590    30x120           n/d           20.6


GRB_name: GRB120911A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13760
SUBJECT: GRB 120911A: optical upper limit CrAO
DATE:    12/09/13 07:18:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of  the Swift GRB 120911A (Cannizzo  et al., GCN 
13744) with  AZT-11 telescope of CrAO observatory  starting on  Sep. 11 (UT) 
21:10:38.  We took  several images in R-filter of 180 s exposure.  Within 
enhanced XRT afterglow position (Beardmore et al., GCN 13748) we do not 
detect any new object.   A preliminary  photometry of co-added frame is 
based  on the USNO-B1.0 (R2)  nearby  stars is following:

T0+,        Filter   Exposure,   OT,         UL (3 sigma)
mid, d                 (s)

0.6130     R        20x180       n/d          20.9 


GRB_name: GRB120907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13761
SUBJECT: GRB 120907A: optical observations of ISON-Kislovodsk 
DATE:    12/09/13 18:53:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Nevski (ISON-Kislovodsk Observatory), A. Volnova (SAI MSU/IKI), I. 
Molotov (KIAM), A. Pozanenko (IKI)  report on behalf of larger 
collaboration:

We observed the field of  GRB 120907A (Racusin  et al., GCN 13716) with 
Santel-400AN (0.4-m f/3)  telescope f ISON-Kislovodsk observatory  starting 
on  Sep. 07 (UT) 00:34:32, i.e. ~10.2 minutes after burst  trigger.  We took 
several unfiltered images  of 30 s and 60 s exposures.  In a stacked images 
we clearly detect optical afterglow of   GRB 120907A (Racusin  et al., GCN 
13716; Gorbovskoy et al., GCN 13718; Kruehler et al., GCN 13719). A 
preliminary photometry of  stacked  frames is based  on the USNO-B1.0 (R2) 
nearby  stars:

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

00:34:32  0.00899 10x30    none      18.55+/-0.09
00:51:45  0.02120   5x60    none      18.95+/-0.13
00:58:09  0.02980   8x60    none      19.52+/-0.20
01:16:32  0.04339   8x60    none      19.50+/-0.20


GRB_name: GRB120913A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13762
SUBJECT: GRB 120913A: Swift detection of a burst
DATE:    12/09/13 20:27:23 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. A. Helder (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), N. Gehrels (NASA/GSFC),
C. Gronwall (PSU), D. Grupe (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 20:18:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120913A (trigger=533568).  Swift did not slew because
of the Sun observing constraint. 
The BAT on-board calculated location is 
RA, Dec 146.437, +26.977 which is 
   RA(J2000)  =  09h 45m 45s
   Dec(J2000) = +26d 58' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of at least 40 sec.  (At T+30s, Swift
executed a pre-planned slew that moved the GRB outside of the BAT FOV)
The peak count rate was ~2600 counts/sec (15-350 keV), at ~23 sec 
after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 22:34 UT on 2012 September 27. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB120913B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13763
SUBJECT: GRB 120913B: Swift detection of a burst
DATE:    12/09/14 00:04:22 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. A. Helder (PSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
D. Grupe (PSU), S. T. Holland (STScI), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 23:55:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120913B (trigger=533613).  Swift did not slew because of the
Sun observing constraint. 
The BAT on-board calculated location is 
RA, Dec 213.644, -14.535 which is 
   RA(J2000)  =  14h 14m 35s
   Dec(J2000) = -14d 32' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of about 70 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~5 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 20:57 UT on 2012 December 14. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB120913B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13764
SUBJECT: Skynet/PROMPT observations of GRB120913B
DATE:    12/09/14 00:33:59 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, K. Ivarsen, J. Haislip, D. Reichart, J. Moore, H. T. 
Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. 
Speckhard, A.Trotter, and J. A. Crain report:

Skynet observed the field of GRB120913B (GCN 13763, Swift trigger #533613) 
with four of the PROMPT telescopes located at CTIO in Chile in BVRI 
beginning ~58 seconds after the burst. We detect a fading source at RA 
14:14:38.46 DEC -14:30:57.2, within the BAT error circle.

The object peaked at a magnitude of ~15.9 in R (calibrated to nearby SDSS 
catalog stars) at ~4.2 minutes after the burst before beginning to fade.

Further observations are ongoing.


GRB_name: GRB120913B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13765
SUBJECT: GRB 120913B: TAROT La Silla observatory optical detection
DATE:    12/09/14 00:41:33 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120913B detected by SWIFT
(trigger 533613) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 30.6s after the GRB trigger
(17.7s after the notice). The elevation of the field decreased
from 26 degrees above horizon and weather conditions
were good.

We detect a new fading source in the error box given
by SWIFT. We detected the candidate couterpart
mentioned by LaCluyze et al. (GCNC 13764)
at the following position (+/- 2 arcsec):

RA(J2000) = 14h 14m 38.57s
DEC(J2000) -14d 30' 55.8"

OT raised until R=15.8 5 min after the GRB.
Now the afterglow is fading.

Magnitudes were estimated with the nearby NOMAD1 star
0754-0289300 (R.A.=213.6332611 Decl=-14.5238889 J2000)
R=15.99. MAgnitutes are not corrected for galactic dust
extinction.

N.B. Galactic coordinates are lon=331.3041 lat=+43.7095
and the galactic extinction in R band is about 0.2 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120913B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13766
SUBJECT: GRB 120913B: TAROT La Silla observatory optical photometry
DATE:    12/09/14 01:16:07 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We continue to observe the afterglow of GRB 120913B
(LaCluyze et al. GCNC 13764). A rapid photometric
analysis gives the following magnitudes:

t0+Mid(s)  Rmag
    159     16.5
    200     16.3
    281     15.8
    351     15.9
    451     16.2
    652     16.6
   1054     17.0

We measure an optical decay alpha=-1 from
observations after 300s, i.e. after the
optical peak.

Considering the optical decay, optical
predicted magnitudes are:

2012-09-14T00:56 UT R=18.4 (t0+1h)
2012-09-14T01:56 UT R=19.1 (t0+2h)
2012-09-14T02:56 UT R=19.6 (t0+3h)
2012-09-14T03:56 UT R=20.0 (t0+4h)
2012-09-15T00:56 UT R=21.0 (t0+1day)

These predictions can help spectrometry
observations.


GRB_name: GRB120913B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13767
SUBJECT: Continued Skynet/PROMPT observations of GRB120913B
DATE:    12/09/14 03:07:04 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, K. Ivarsen, J. Haislip, D. Reichart, J. Moore, H. T. 
Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. 
Speckhard, A.Trotter, and J. A. Crain report:

Skynet continued observing the field of GRB120913B (GCN 13763, Swift 
trigger #533613) in BVRI using four of the PROMPT telescopes located at 
CTIO in Chile until the object set.

A preliminary light curve of the first night's data from PROMPT can be 
found at: http://skynet.unc.edu/grb/grb120913b.png


GRB_name: GRB120913B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13768
SUBJECT: GRB 120913B: REM NIR early time detection
DATE:    12/09/14 08:07:13 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

S. Covino, D. Fugazza, A. Melandri,  on behalf of the REM team report:

We imaged the field of GRB120913B (Helder et al., GCN 13763) with the NIR camera only with the H filter. The REM telescope is at present under substantial maintenance and the optical camera and some of the subsystems are still off-line.

Observations started at UT 23:56:47, about 49 sec after the GRB, and frames were unfortunately not properly focussed. Yet the afterglow (LaClyyze et al., GCN 13764; Klotz et al., GCN 13765) is detectable and approximately 2 min after the GRB was at H = 13.72 +- 0.15, calibrated by means of isolated unsaturated 2MAS stars in the field.


GRB_name: GRB120913A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13769
SUBJECT: GRB 120913A: Swift-BAT refined analysis
DATE:    12/09/14 13:23:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), E. A. Helder (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120913A (trigger #533568)
(Helder, et al., GCN Circ. 13762).  The BAT ground-calculated position is
RA, Dec = 146.400, 26.959 deg, which is 
   RA(J2000)  =  09h 45m 36.1s 
   Dec(J2000) = +26d 57' 32.4" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
 
The mask-weighted light curve shows three slightly overlapping FRED peaks
starting at ~T-5 sec, peaking at ~T+1, ~T+23, & ~T+40 sec, and ending at ~T+42 sec.
Due to a slew, the burst location left the BAT FoV at ~T+115 sec.
T90 (15-350 keV) is 30.1 +- 4.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.72 to T+39.80 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.18 +- 0.15.  The fluence in the 15-150 keV band is 8.7 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+22.45 sec in the 15-150 keV band
is 2.3 +- 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/533568/BA/


GRB_name: GRB120913B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13770
SUBJECT: GRB 120913B: FRAM early follow up and detection
DATE:    12/09/14 13:49:57 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek (IAA Granada, Spain),
Petr Kubanek, Martin Masek, Jakub Cerny, Jan Ebr and
Michael Prouza (FZU Praha, Czech Rep.)
on behalf of the FRAM team, coordinated by FZU Praha

report:

The 30cm FRAM telescope, located at Pierre Auger
observatory in Malargue, Argentina, followed the GRB
120913B (Helder et al. GCNC13763, Swift trigger
#533613). Observations started 24.4s after the GRB
trigger.

10s R-band (lambda_eff = 640nm) images with a limit of
~16.0 were obtained. We identify the optical transient
reported by LaCluyze et al. (GCNC13764) and Klotz et
al. (GCNC13765) with a magnitude R = 16.3 +/- 0.2 on a
sum of 8x10s images obtained between 271 and 364s after
the GRB.

This message may be cited


GRB_name: GRB120913A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13771
SUBJECT: GRB 120913A: Fermi GBM observation
DATE:    12/09/15 01:44:42 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa and V. Connaughton (UAH) report on behalf of the Fermi GBM Team:

"At 20:18:22.89 UT on 13 spetember 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120913A (trigger369260305  / 120913846), which was
also detected by the Swift/BAT (E.A. Helder et al. 2008, GCN 13762).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 97 degrees.

The GBM light curve consists of 2 peaks at T0 and T0+20s with a duration (T90)
of about 41s (50-300 keV).

The event fluence (10-1000keV) from T0-3.584 s to T0+33.280 s is
(1.8 +/- 0.3)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting
from T0+21.568 s in the 10-1000 keV band is 3.8 +/- 0.2 ph/s/cm^2.

The first peak is harder but fainter than the second peak, which is
best fit by a
power law function with an exponential high-energy cutoff. The power law
index is -1.25 +/- 0.38 and the cutoff energy, parameterized as Epeak, is
26 +/- 4 keV (C-stat 372 for 366 d.o.f.).

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


GRB_name: GRB120913B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13772
SUBJECT: GRB 120913B: Swift-BAT refined analysis
DATE:    12/09/15 02:15:18 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), E. A. Helder (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+882 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120913B (trigger #533613)
(Helder, et al., GCN Circ. 13763).  The BAT ground-calculated position is
RA, Dec = 213.660, -14.508 deg, which is 
   RA(J2000)  =  14h 14m 38.3s 
   Dec(J2000) = -14d 30' 27.9" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 59%.
 
The mask-weighted light curve shows two main pulses riding on top of a broad peak.
The burst starts at ~T-50 sec, with peaks at ~T+5 and ~T+39 sec, and ending at ~T+140 sec.
T90 (15-350 keV) is 126 +- 4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-51.70 to T+111.79 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.63 +- 0.04.  The fluence in the 15-150 keV band is 1.11 +- 0.02 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+38.46 sec in the 15-150 keV band
is 3.2 +- 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/533613/BA/


GRB_name: GRB120913B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13773
SUBJECT: GRB 120913B: Fermi GBM observation
DATE:    12/09/15 02:44:26 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 23:55:58.77 UT on 13 september 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120913B (trigger 369273361 / 120913997), which
was also detected by the Swift/BAT (E.A. Helder et al. 2008, GCN 13763)
The GBM on-ground location is consistent with the Swift position.
 The angle from the Fermi LAT boresight is 66 degrees.

The GBM light curve consists of 2 peaks at T0-10 and T0+30s on top of a
longer plateau, with a duration (T90) of about 110 s (50-300 keV).
The time-averaged spectrum from T0-40.961 s to T0+98.306 s is
best fit by a Band function with Epeak = 163 +/- 23 keV,
alpha = -1.19 +/- 0.06, and beta = -1.97 +/- 0.07
(Cstat 604 for 483 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(2.9 +/- 0.7)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+37.632 s in the 10-1000 keV band
is 5.0 +/- 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: GRB120807A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13776
SUBJECT: Corrections to the Fermi-LAT upper limits for GRB 120807A, 120908A, 120909A, and 120911A
DATE:    12/09/17 21:22:46 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

Weikang Zheng and Carl Akerlof (Umich), report on behalf of the ROTSE
collaboration (the authors are not affiliated with the Fermi Collaboration),

The recent GCN Circulars we reported about Fermi-LAT upper limits for
GRB 120807A (GCN 13608), 120908A (GCN 13742), 120909A (GCN 13742), and
120911A (GCN 13752) contain an error about the upper limits estimation
due to a wrong method. We apologize for the confusion. We thank Giacomo
Vianello from LAT group for pointing it out and making suggestion to
correct it. We've updated our pipeline result with the appropriate
method (see The Fermi LAT team, Ackermann et al., 2012, ApJ, 754, 121).
We report the corrected upper limit result (100 MeV -300 GeV; T0-T0
+47.5s) for the 4 GRBs again:

GRB 120807A : 5.42e-05 ph/cm2/s
GRB 120908A : 1.79e-04 ph/cm2/s
GRB 120909A : 8.70e-05 ph/cm2/s
GRB 120911A : 3.81e-05 ph/cm2/s


GRB_name: GRB120916A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13777
SUBJECT: GRB 120916A: Fermi-LAT detection of a burst
DATE:    12/09/18 02:41:43 GMT
FROM:    Masanori Ohno at ISAS/JAXA  <ohno@astro.isas.jaxa.jp>

G. Vianello (SLAC), M. Ohno (Hiroshima U.), and V. Connaughton (UAH)  
report on behalf of the Fermi-LAT team:

On Sept. 16, 2012, Fermi LAT detected high energy emission from GRB  
120916A, which was also detected by Fermi-GBM (trigger 120916173).  
Fermi GBM triggered at T0 = 04:08:40 UTC, although emission from the  
GRB is clearly seen starting at ~T0-60 s. GBM did not trigger on this  
earlier emission period owing to the triggering being disabled while  
Fermi was passing through a region of high geomagnetic latitude. The  
GRB was also detected by the IPN which provided us a preliminary  
position (private communication, circular to appear).

The best LAT on-ground location is found to be RA, Dec 205.81, 36.66  
(J2000) with an error radius of 0.3 deg (68% containment, statistical  
error only), this was 29 deg from the LAT boresight at the time of the  
trigger. This localization has been found using LAT SOURCE data class  
in a time interval of ~500 seconds around the GRB time.

The LAT data show a significant increase in counts at energies >100  
MeV, starting around T0, i.e., several seconds after the beginning of  
the low-energy emission. A standard likelihood analysis yields a  
photon index of -2.0 +/- 0.5 and a flux of (1.6 +/- 1.0) x 10^-9 erg/ 
cm^2/s (100 MeV - 10 GeV).

We note that the transient is not significantly detected using LAT  
TRANSIENT class data, even though the LAT TRANSIENT data appear by eye  
to follow the lightcurve seen at lower energies in the GBM. This lack  
of a significant signal in the LAT TRANSIENT data is due to the low  
signal-to-noise ratio in that class resulting from the high non-photon  
background corresponding to the high geomagnetic latitude.

The Fermi LAT point of contact for this burst is Masanori Ohno (ohno@hep01.hepl.hiroshima-u.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: GRB120916A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13778
SUBJECT: IPN Triangulation of long GRB 120916A
DATE:    12/09/18 11:19:03 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

V. Connaughton, M. Briggs, and C. Meegan, 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

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

The long-duration, moderately intense GRB 120916A (Fermi-LAT detection: 
Vianello, Ohno, and Connaughton, GCN 13777) has been observed by 
INTEGRAL (SPI-ACS), Konus-Wind, Fermi (GBM: trigger 369461323),
MESSENGER (GRNS),  Swift (BAT), and Suzaku (WAM), so far, at about 14866 
s UT (04:07:46). 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:
    205.631 (13h 42m 31s) +36.700 (+36d 42' 00")
   Corners:
    207.209 (13h 48m 50s) +35.578 (+35d 34' 41")
    204.206 (13h 36m 49s) +37.722 (+37d 43' 20")
    203.936 (13h 35m 45s) +37.776 (+37d 46' 33")
    206.960 (13h 47m 50s) +35.646 (+35d 38' 44")
   ---------------------------------------------
The error box area is 0.298 sq. deg, and its maximum
dimension is 3.42 deg. This elongated box intersects the LAT error circle

This box may be improved.

A triangulation map showing the error box and the LAT error circle is
posted at
http://www.ioffe.ru/LEA/GRBs/GRB120916_T14864/IPN/

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


GRB_name: GRB120918A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13779
SUBJECT: GRB 120918A: Swift detection of a burst
DATE:    12/09/18 11:26:07 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B. N. Barlow (PSU), W. H. Baumgartner (GSFC/UMBC), C. Gronwall (PSU),
D. M. Palmer (LANL), M. Stamatikos (OSU/NASA/GSFC) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 11:16:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120918A (trigger=534015).  Swift could not slew to the
burst because of the Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 181.054, -32.758 which is 
   RA(J2000) = 12h 04m 13s
   Dec(J2000) = -32d 45' 26"
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 50 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 17:37 UT on 2012 November 15. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is B. N. Barlow (bnb2 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120916A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13781
SUBJECT: Konus-Wind observation of GRB 120916A
DATE:    12/09/18 15:28:42 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 120916A
(Fermi-LAT detection: Vianello et al., GCN 13777;
IPN detection and localization: Hurley et al., GCN 13778)
triggered Konus-Wind at T0=14864.136s UT (04:07:44.136)

The light curve shows a multi-peaked structure with
a total duration of ~30 s followed by a weaker and softer pulse at ~T0+50 s.
The emission in the main bursting episode is seen up to 9 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120916_T14864/

As observed by Konus-Wind, the burst
had a fluence of 1.7(-0.3,+0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.864 s,
of 4.5(-1.5,+1.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+24.832 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 = -1.0 (-0.1, +0.2),
the high energy photon index beta = -4.2 (-5.8, +1.6),
the peak energy Ep = 335(-90, +65) keV,
chi2 = 71.5/90 dof.

The spectrum at the maximum count rate (measured from T0 to T0+8.448 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 = -0.7 (-0.2, +0.2),
the high energy photon index beta = -2.3 (-7.7, +0.2),
the peak energy Ep = 320(-70, +120) keV,
chi2 = 97.9/86 dof.


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


GRB_name: GRB120916A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13782
SUBJECT: GRB 120916A: Fermi GBM Observation
DATE:    12/09/18 16:54:24 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

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

At 04:08:40.75 UT on 16 September 2012, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 120916A
(trigger 369461323/120916173) which was also detected by
Fermi LAT (G. Vianello et al. GCN 13777), Konus-Wind
(S. Golenetskii et al. GCN 13781) and the IPN (K. Hurley
et al. GCN 13778).

The on-ground calculated location is consistent with the LAT
location.

The GBM light curve consists of 3 peaks with a duration (T90)
of about 53 s (50-300 keV). The last peak is softer and corresponds
to the trigger time, the earlier emission begins at ~T0-60 s.
GBM did not trigger on this earlier emission period owing to the
triggering being disabled while Fermi was passing through a
region of high geomagnetic latitude.

The time-averaged spectrum from T0-53 s to T0+0.2 s is best
fit by a Band function with Epeak = 312.40 (+51.30/-47.20)
keV, alpha = -0.99 (+0.06/-0.06), and beta = -1.90 (+0.09/-0.12).

The event fluence (10-1000 keV) in this time interval is
(1.95 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+-30.7205 s in the 10-1000 keV
band is 9.72 +/- 0.28 ph/s/cm^2.

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


GRB_name: GRB120918A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13784
SUBJECT: GRB 120918A: Swift-BAT refined analysis
DATE:    12/09/19 21:43:17 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), B. N. Barlow (PSU), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120918A (trigger #534015)
(Barlow, et al., GCN Circ. 13799).  The BAT ground-calculated position is
RA, Dec = 181.042, -32.762 deg, which is 
   RA(J2000)  =  12h 04m 10.1s 
   Dec(J2000) = -32d 45' 43.5" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 15%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-5 sec, the main peak at ~T+1 sec, and ending at ~T+40 sec.
T90 (15-350 keV) is 25.1 +- 2.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.86 to T+23.90 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.00 +- 0.39, 
and Epeak of 85.5 +- 36.3 keV (chi squared 55.6 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.7 +- 0.6 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T-0.28 sec in the 15-150 keV band is
4.5 +- 0.5 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.60 +- 0.09 (chi squared 63.5 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/534015/BA/


GRB_name: GRB120919A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13785
SUBJECT: GRB 120919A: Fermi GBM detection
DATE:    12/09/20 11:02:08 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

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

"At 07:24:41.98  UT on 19 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120919A (trigger 369732284 / 120919309).

The on-ground calculated location, using the GBM trigger
data, is RA = 213.4, DEC = -46.3 (J2000 degrees,
equivalent to 14 h 14 m, -46 d 18 '), with an uncertainty
of 1.1 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 63 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous re-point request (ARR) maneuver.

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

The GBM light curve shows a single bright pulse
with a duration (T90) of about 22.5 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+10.496 s is
best fit by a Band function with Epeak = 162 +/- 8 keV,
alpha = -0.76 +/- 0.04, and beta = -2.15 +/- 0.06

The event fluence (10-1000 keV) in this time interval is
(1.679 +/- 0.026)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+2.62 s in the 10-1000 keV band
is 25.3 +/- 0.3 ph/s/cm^2.

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

[GCN OPS NOTE(20sep12):  Per author's request, the fluence value
was changed from "(1.60 +/- 0.03)E-06" to "(1.679 +/- 0.026)E-05".]


GRB_name: GRB120919A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13786
SUBJECT: IPN Triangulation of long GRB 120919A
DATE:    12/09/20 15:18:00 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley on behalf of the Mars Odyssey and MESSENGER GRB teams,

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

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

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

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

V. Connaughton, M. Briggs, and C. Meegan, 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

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

The long-duration GRB 120919A (Fermi/GBM detection: Rau, GCN Circ. 
13785) was observed by Konus-Wind, MESSENGER (GRNS), Mars Odyssey 
(HEND), INTEGRAL (SPI-ACS), and AGILE (MCAL) at about 26682 s UT (07:24:42).

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
     214.768 (14h 19m 04s) -45.564 (-45d 33' 52")
    Corners:
     215.108 (14h 20m 26s) -45.474 (-45d 28' 26")
     214.693 (14h 18m 46s) -45.722 (-45d 43' 19")
     214.428 (14h 17m 43s) -45.653 (-45d 39' 09")
     214.843 (14h 19m 22s) -45.407 (-45d 24' 24")
    ---------------------------------------------
The error box area is 236  sq. arcmin, and its maximum
dimension is 31 arcmin (the minimum one is 12 arcmin).

This box can be improved.

The center of the GBM ground position given in
GCN Circ. 13785 is 1.2 deg from the center of this box.


GRB_name: GRB120919A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13787
SUBJECT: Konus-Wind observation of GRB 120919A
DATE:    12/09/20 15:26:34 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 120919A
(Fermi-GBM detection: Rau, GCN 13785;
IPN detection and localization: Hurley et al., GCN 13786)
triggered Konus-Wind at T0=26678.597s UT (07:24:38.597)

The light curve shows a single pulse with a duration of ~8 s
followed by a weaker and softer emission till ~T0+30 s.
The emission in the main bursting episode is seen up to 7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120919_T26678/

As observed by Konus-Wind, the burst
had a fluence of 1.4(-0.1,+0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+2.432s,
of 4.1(-0.5,+0.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -1.05 (-0.1, +0.1),
and Ep = 225(-19, +23) keV,
chi2 = 100.3/84 dof.

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


GRB_name: GRB120919B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13788
SUBJECT: IPN Triangulation of long GRB 120919B
DATE:    12/09/20 15:35:40 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley on behalf of the Mars Odyssey and MESSENGER GRB teams,

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

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

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

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

V. Connaughton, M. Briggs, and C. Meegan, 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, moderately intense GRB 120919B was observed by Fermi
(GBM: trigger 369710066), Konus-Wind, MESSENGER (GRNS), INTEGRAL
(SPI-ACS), and Mars Odyssey (HEND) at about 4463 s UT (01:14:23).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    302.633 (20h 10m 32s) -37.490 (-37d 29' 25")
   Corners:
    302.735 (20h 10m 56s) -37.483 (-37d 28' 59")
    302.857 (20h 11m 26s) -38.235 (-38d 14' 04")
    302.530 (20h 10m 07s) -37.497 (-37d 29' 50")
    302.401 (20h 09m 36s) -36.706 (-36d 42' 21")
   ---------------------------------------------
The error box area is 457  sq. arcmin, and its maximum
dimension is 1.57 deg (the minimum one is 10 arcmin).

This box can be improved.


GRB_name: GRB120919B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13789
SUBJECT: Konus-Wind observation of GRB 120919B
DATE:    12/09/20 15:52:27 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration, moderately intense GRB 120919B
(IPN detection and localization: Hurley et al., GCN 13788)
triggered Konus-Wind at T0=04499.597s UT (01:14:59.401)

The light curve shows multiple pulses in the time interval
starting at ~T0-30s and ending at ~T0+100s.
The emission in the main bursting episode is seen up to 8 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120919_T04499/

As observed by Konus-Wind, the burst
had a fluence of 3.1(-0.5,+0.7)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+13.056 s,
of 4.3(-0.9,+1.1)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+98.560 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 = -0.9 (-0.4, +0.5),
the high energy photon index beta = -2.3 (-2.7, +0.3),
the peak energy Ep = 250(-60, +190) keV,
chi2 = 86.9/83 dof.

The spectrum of the main bursting episode (measured from T0 to T0+16.640 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 = -1.0 (-0.2, +0.2),
the high energy photon index beta = -2.4 (-1.0, +0.3),
the peak energy Ep = 300(-70, +85) keV,
chi2 = 76.3/83 dof.

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


GRB_name: GRB120919A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13790
SUBJECT: GRB 120919A: Swift-XRT observations
DATE:    12/09/21 10:47:01 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

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

We have analysed 4.7 ks of XRT data for the GBM and IPN-detected burst
GRB 120919A (Rau et al. GCN Circ. 13785, Hurley et al. GCN Circ.
13786), from 133.7 ks to 157.6 ks after the IPN trigger. The data are
entirely in Photon Counting (PC) mode. Two uncatalogued X-ray sources
are detected within the IPN error box with the following refined XRT
positions :

Source 1 :

RA, Dec = 214.83981, -45.56220 which is equivalent to:

RA (J2000): 14h 19m 21.56s
Dec(J2000): -45d 33m 43.9s

with an uncertainty of 3.1 arcsec (radius, 90% confidence). This
position is 181 arcsec from the centre of the IPN error box. The
source is detected with a 0.3-10 keV count rate of 0.0067 +/- 0.0014
count/s, which corresponds to an observed flux of 2.7e-13 erg cm^-2
s^-1 for a typical GRB-like spectrum.

Source 2 :

RA, Dec =  214.79040, -45.56518 which is equivalent to:

RA (J2000): 14h 19m 09.70s
Dec(J2000): -45d 33m 54.66s

with an uncertainty of 5.5 arcsec (radius, 90% confidence). This
position is 57 arcsec from centre of the IPN error box. The source is
detected with a 0.3-10 keV count rate of 0.0037 +/- 0.0011 count/s,
which corrsponds to an observed flux of 1.5e-13 erg cm^-2 s^-1 for a
typical GRB-like spectrum.

We cannot determine whether either of the sources are fading at the
present time.

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


GRB_name: GRB120919A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13791
SUBJECT: GRB 120919A: Swift/UVOT Upper Limits
DATE:    12/09/21 13:24:16 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S.R. Oates (MSSL-UCL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120919A
134 ks after the IPN trigger (Hurley et al. GCN Circ. 13786)
No optical afterglow is found within the IPN error box nor 
at the location of the two uncatalogued XRT sources (Beardmore et al. GCN Circ. 13790). 
We note the presence of a catalogued USNO-B1 source within 4.5" of XRT source 1,
with a m2 magnitude 20.52 +\- 0.17.

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

m2              133695       157598         4891         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120919B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13792
SUBJECT: GRB 120919B: MASTER prompt optical observations 
DATE:    12/09/21 13:54:00 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

H. Levato and C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez and F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

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

K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk
Irkutsk State University

V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

V. Krushinski, I. Zalozhnich,  A. Popov, A. Bourdanov
Ural Federal University


MASTER-ICATE robotic Very Wide Field Cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in
Argentina (Observatorio Astronomico Felix Aguilar,
http://93.180.27.230:8080/) were pointed to the GRB120919B by FERMI 
369710066 trigger   30 s after notice time and 55 s after GRB time at 
2012-09-19 01:15:18 UT.
We cover full IPN-triangulations error-box (K. Hurley et. al. GCN13788)
We haven't found  optical transient  within IPN-triangulations error-box
   our first (5 s exposure) set and on coadd image with complete exposure
of 45 seconds durnig gamma-burst activity (Golenetskii et al., GCN 13789).

The 5-sigma upper limit on single image has  been about 11.7 mag and 12.5 
mag on coadded image.

Also, we are marginaly see ~2 sigma OT at position Ra 20:10:26.40 Dec 
+37:31:48.00 with magnitude 12.5+-0.5m .

The coverage map and OT image available here 
http://master.sai.msu.ru/static/GRB/GRB120919B_2x2deg.png

Our cameras are continuously imaging the sky with 5 sec exposures.

This message can be cited.


GRB_name: GRB120922A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13793
SUBJECT: GRB 120922A: Swift detection of a burst
DATE:    12/09/22 22:41:52 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. N. Yershov (UCL-MSSL), S. D. Barthelmy (GSFC),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. J. Mountford (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report
on behalf of the Swift Team:

At 22:30:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120922A (trigger=534394).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 234.756, -20.177 which is 
   RA(J2000) = 15h 39m 01s
   Dec(J2000) = -20d 10' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple-peaked
structure with a duration of at least 130 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~102 sec after the trigger. 

The XRT began observing the field at 22:32:25.0 UT, 116.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 234.7505, -20.1839 which is equivalent to:
   RA(J2000)  = +15h 39m 0.12s
   Dec(J2000) = -20d 11' 02.0"
with an uncertainty of 5.6 arcseconds (radius, 90% containment). This
location is 31 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 0.1 s image was 2.53e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 126 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
0.15. 

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


GRB_name: GRB120922A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13794
SUBJECT: GRB 120922A: Prompt enhanced Swift-XRT position
DATE:    12/09/22 23:28:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 120922A, we find an
enhanced XRT position of the afterglow: RA, Dec: 234.7483, -20.1821
which is equivalent to:
   RA (J2000)  = 15 38 59.60
   Dec (J2000) = -20 10 55.4
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/534394.

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: GRB120922A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13795
SUBJECT: GRB 120922A: GROND afterglow candidate
DATE:    12/09/23 00:29:21 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 120922A (Swift trigger 534394; Yershov et 
al., GCN 13793) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 23:30 UT on Sep 22, 60 min after the GRB trigger.
We detect a bright source within the enhanced Swift/XRT error circle 
reported by Evans (GCN 13794) at coordinates RA, DEC (J2000) = 
15:38:59.64, -20:10:54.2 (+/- 0.3 arcsec) with (AB mag)

r' = 19.5 +/- 0.1,

calibrated against the GROND zeropoint and not corrected for the Galactic 
foreground reddening of E_(B-V)= 0.15 mag in the direction of the burst 
(Schlegel et al. 1998).


GRB_name: GRB120923A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13796
SUBJECT: GRB 120923A: Swift detection of a burst
DATE:    12/09/23 05:28:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. N. Yershov (UCL-MSSL), S. D. Barthelmy (GSFC),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. J. Mountford (U Leicester), S. R. Oates (UCL-MSSL),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 05:16:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120923A (trigger=534402).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 303.795, +6.235 which is 
   RA(J2000)  =  20h 15m 11s
   Dec(J2000) = +06d 14' 05"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several overlapping peaks
with a total duration of about 35 sec.  The peak count rate
was ~700 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 05:18:26.0 UT, 139.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 303.79631, 6.22039 which is equivalent
to:
   RA(J2000)  = 20h 15m 11.11s
   Dec(J2000) = +06d 13' 13.4"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  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 9.80
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 143 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
0.16. 

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


GRB_name: GRB120923A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13797
SUBJECT: GRB 120923A: ROTSE-III Optical Limits 
DATE:    12/09/23 05:41:38 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich) and T. Guver (Sabanci U) report on behalf of the ROTSE
collaboration: 

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 120923A
(Swift trigger 534402; Yershov et al., GCN 13796), producing images
beginning 0.7 s after the GCN notice time. An automated response took the
first image at 05:17:43.7 UT, 97.4 s after the burst, under fair conditions.
We took 10 5-sec, 10 20-sec and 0 60-sec exposures. These unfiltered images
are calibrated relative to USNO A2.0 (R). Imaging is on going. 

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle. Individual images have limiting magnitudes
ranging from 15.4-16.3; we set the following specific limits. 

start UT       end UT      t_exp(s)   mlim     Coadd?

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

05:17:43     05:17:48           5      15.6        N

05:17:55     05:18:00           5      15.4        N

05:18:07     05:18:12           5      15.7        N

05:17:43     05:19:31           50     16.4        Y

 


GRB_name: GRB120923A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13798
SUBJECT: GRB 120923A: TAROT La Silla observatory optical observations
DATE:    12/09/23 06:00:56 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120923A detected by SWIFT
(trigger 534402) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 104.6s after the GRB trigger
(16.8s after the notice). The elevation of the field decreased
from 16 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT at the XRT position (Yershov et al.
GCNC 13796) with a limiting magnitude of:

t0+105s to t0+165s : R > 16.0

We co-added a series of exposures:
t0+178s to t0+329s : R > 17.9

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

Note that there is NOMAD1 0962-0583888 (R.A.=303.7958222
Decl=+06.2200278 J2000) R=17.9 very close to the XRT position.
This source is detected on TAROT images but the sampling of
TAROT (3.3 arcsec/pixel) does not allow to separate an OT
from this star.

This message may be cited.


GRB_name: GRB120922A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13799
SUBJECT: GRB 120922A: TAROT La Silla observatory optical observations
DATE:    12/09/23 06:35:19 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120922A detected by SWIFT
(trigger 534394) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 56 min after the GRB trigger
(starting at twilight). The elevation of the field decreased
from 46 degrees above horizon and weather conditions
were good.

Co addition of TAROT images from 56 to 85 minutes
after the GRB, shows the optical candidate reported
by Knust et al. (GCNC 13795) at magnitude R~20
(close to the limiting magnitude of TAROT).
Note the source NOMAD1 0698-0330778 (R.A.=234.7496389
Decl=-20.1828917 J2000) R=19.79 few arcsec southeastern
from the OT.

This message may be cited.


GRB_name: GRB120922A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13800
SUBJECT: GRB 120922A: Enhanced Swift-XRT position
DATE:    12/09/23 07:37:00 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1474 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120922A, 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 = 234.74858, -20.18203 which is equivalent
to:

RA (J2000): 15h 38m 59.66s
Dec (J2000): -20d 10' 55.3"

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: GRB120923A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13801
SUBJECT: GRB 120923A: Enhanced Swift-XRT position
DATE:    12/09/23 07:49:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1113 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120923A, 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 = 303.79480, +6.22131 which is equivalent
to:

RA (J2000): 20h 15m 10.75s
Dec (J2000): +06d 13' 16.7"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB120923A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13802
SUBJECT: GRB 120923A: Gemini afterglow detection, high-z candidate
DATE:    12/09/23 10:33:17 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), D.A. Perley (Caltech), N.R. Tanvir (U. Leicester) and A. Cucchiara (UCSC) report for a larger collaboration:

"We observed the location of GRB 120923A (Yershov et al. GCN 13796) with Gemini-North, beginning approximately 1.4 hours after the burst. Observations were obtained in riz (with GMOS) and YJHK (with NIRI). In our optical and Y-band observations we detect no source in the refined XRT error circle (Goad et al. GCN 13801), with a preliminary z-band limit of z~24. However, in our JHK observations we clearly detect a source at a location of

RA(J2000): 20:15:10.78
DEC(J2000): 06:13:16.3
(uncertainty ~0.5")

Which is seen to fade in two epochs of J-band observations separated by ~3 hours, confirming it as the counterpart of GRB 120923A. The colours of this source in the IR are blue, with H-K~0.1 mag. This is strongly suggestive of a break between the Y and J-band, similar to GRB 090423, and may indicate that GRB 120923A lies at z~8.

We thank Michael Hoenig for excellent support for these observations.

Further observations are ongoing."


GRB_name: GRB120922A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13803
SUBJECT: GRB 120922A: Swift/UVOT Observations
DATE:    12/09/23 10:33:30 GMT
FROM:    Vladimir Yershov at MSSL  <vny@mssl.ucl.ac.uk>

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

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 864 seconds after the BAT trigger. There is a candidate
afterglow in the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  =  15:38:59.60 = 234.74832
  DEC(J2000) = -20:10:54.3  = -20.18175
with a 90%-confidence error radius of about 0.65 arc sec. This position
is 2.0 arc sec. from the center of the XRT error circle. The estimated
magnitude is 18.91 with a 1-sigma error of about  0.16. No correction
has been made for the expected extinction corresponding to E(B-V) of
0.15.


GRB_name: GRB120922A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13804
SUBJECT: GRB 120922A: Swift-XRT refined Analysis
DATE:    12/09/23 10:42:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A. Melandri (INAF-OAB), D.N. Burrows (PSU), J.A. Kennea (PSU), M.C.
Stroh (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), B. Sbarufatti (INAF-OAB/PSU), G. Stratta
(ASDC) and V.N. Yershov report on behalf of the Swift-XRT team:

We have analysed 9.3 ks of XRT data for GRB 120922A (Yershov  et al.
GCN Circ. 13793), from 120 s to 19.4 ks after the  BAT trigger. The
data comprise 484 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 13794).

The light curve can be modelled with a series of power-law decays. The
light curve initially rises, with an index alpha=-1.5 (+0.0, -1.3). At
T+130 s it breaks to an alpha of 3.09 (+0.09, -0.08). The light curve
breaks again at T+243 s to a decay with alpha=3.83 (+0.09, -0.10), 
before a final break at T+737 s s after which the decay index is 0.85
(+0.04, -0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.33 (+/-0.04). The
best-fitting absorption column is  2.15 (+/-0.09) x 10^21 cm^-2, in
excess of the Galactic value of 7.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.11 (+0.13, -0.12)
and a best-fitting absorption column of 1.06 (+0.28, -0.27) 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 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.06 (+0.28, -0.27) x 10^21 cm^-2
Galactic foreground: 7.7 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.11 (+0.13, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00534394.

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


GRB_name: GRB120923A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13805
SUBJECT: GRB 120923A: Swift/UVOT Upper Limit
DATE:    12/09/23 12:50:40 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120923A 
143 s after the BAT trigger (Yershov et al., GCN Circ. 13796).
No optical afterglow consistent with the XRT or Gemini position (Goad et 
al., GCN Circ. 13801, Levan et al., GCN Circ. 13802) is detected in the 
initial UVOT exposure.
A preliminary 3-sigma upper limit using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding 
chart exposure is:

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

white              143          293          147         >21.3

The magnitude in the table is not corrected for the Galactic extinction 
due to the reddening of E(B-V) = 0.16 in the direction of the burst 
(Schlegel et al. 1998).


GRB_name: GRB120922A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13806
SUBJECT: GRB 120922A: Swift-BAT refined analysis
DATE:    12/09/23 13:36:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU), V. N. Yershov (UCL-MSSL)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+303 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120922A (trigger #534394)
(Yershov, et al., GCN Circ. 13793).  The BAT ground-calculated position is
RA, Dec = 234.758, -20.181 deg, which is 
   RA(J2000)  =  15h 39m 02.0s 
   Dec(J2000) = -20d 10' 51.8" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 33%.
 
The mask-weighted light curve shows low-level emission starting at T-200 sec,
possibly sooner before the data capture started, with peaks at ~T_0, ~T+60, & ~T+105 sec,
and ending at ~T+205 sec.  T90 (15-350 keV) is 173 +- 33 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-22.58 to T+215.73 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.58 +- 0.36, 
and Epeak of 38.2 +- 0.0 keV (chi squared 54.3 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.2 +- 0.7 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+99.21 sec in the 15-150 keV band is
2.0 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.09 +- 0.08 (chi squared 61.1 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/534394/BA/


GRB_name: GRB120923A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13807
SUBJECT: GRB 120923A: Swift-BAT refined analysis
DATE:    12/09/23 13:37:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU), V. N. Yershov (UCL-MSSL)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120923A (trigger #534402)
(Yershov, et al., GCN Circ. 13796).  The BAT ground-calculated position is
RA, Dec = 303.781, 6.255 deg, which is 
   RA(J2000)  =  20h 15m 07.3s 
   Dec(J2000) = +06d 15' 16.8" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 79%.
 
The mask-weighted light curve shows the burst starting at ~T-5 sec, peaking
at ~T+25 sec, and ending at ~T+30 sec.  T90 (15-350 keV) is 27.2 +- 3.0 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-2.93 to T+26.64 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.29 +- 1.66, 
and Epeak of 44.4 +- 10.6 keV (chi squared 43.83 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.2 +- 0.8 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+24.67 sec in the 15-150 keV band is
0.6 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.80 +- 0.23 (chi squared 51.10 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/534402/BA/


GRB_name: GRB120922A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13808
SUBJECT: GRB 120922A: Swift/UVOT Detection
DATE:    12/09/23 17:08:12 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of
GRB 120922A  127 s after the BAT trigger (Yershov et al., GCN
Circ. 13793).  A source consistent with the XRT position (Evans et al.
GCN Circ. 13800),  and the initial optical detection by GROND (Knust
et al., GCN Circ. 13795)  is detected in the initial UVOT exposures
(Yershov et al. GCN Circ. 13803).

The uvot observations show a slow initial rise in brightness peaking
around 900s after the trigger.  The burst is only detected in the v,b and
white filters which is probably due to the high galactic reddening.

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              126          276          147        >20.67
white              865         1014          147         19.34 +/- 0.14
v                  615         1239           78         17.94 +/- 0.22
b                  541          733           78        >19.17
b                 1145         2030          119         19.62 +/- 0.36
u                  285          534          250        >19.98
u                  688         1139           40        >18.82
w1                 664        16852         1434        >20.95
m2                 639        11081         1232        >20.96
w2                 590        12900         1424        >21.20

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: GRB120922A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13809
SUBJECT: GRB 120922A: Fermi GBM detection
DATE:    12/09/23 18:23:16 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (MSFC/USRA) reports on behalf of the Fermi GBM Team:

"At 22:32:09.47 UT on 22 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120922A (trigger 370045932 / 120922939)
which was also detected by the Swift/BAT (Yershov et al. 2012, GCN 13793).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 85 degrees.

The GBM light curve consists of a multiple peaks with a duration (T90)
of about 180 s (50-300 keV).
The time-averaged spectrum from T0-121 s to T0+6 s is
best fit by a Band function with Epeak = 37.7 +/- 3.5 keV,
alpha = 1.6 +/- 0.7 , and beta = -2.3 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(6.5 +/- 0.4)E-06 ergs/cm^2. The 1-sec peak photon flux measured
starting from T0-1.8 s in the 10-1000 keV band
is 3.4 +/- 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: GRB120922A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13810
SUBJECT: GRB 120922A: GROND photometric redshift
DATE:    12/09/23 21:23:29 GMT
FROM:    Fabian Knust at MPE/GROND  <fabian.knust@hotmail.de>

F. Knust (MPE Garching), T. Kruehler (DARK/NBI), S. Klose (TLS Tautenburg) and J. Greiner (MPE Garching) report on behalf of the GROND team:

We report on further analysis of the GROND (Greiner et al. 2008, PASP 120, 405) optical/NIR imaging of the afterglow (Knust et al. GCN 13795, Klotz et al., GCN 13799, Yershov et al., GCN 13803, Kuin et al., GCN 13808) of GRB 120922A (Yershov et al., GCN 13793). Tying our photometric solution to field stars from the SDSS in the optical filters and 2MASS in the NIR, we derive the following AB magnitudes centered at a midtime of 00:01 UTC on September 23 (approx 1.5 hrs after the trigger):

g' = 20.53 +/- 0.05
r' = 19.69 +/- 0.04
i' = 19.44 +/- 0.04
z' = 19.28 +/- 0.04 
J = 18.92 +/- 0.06
H = 18.79 +/- 0.07
K = 18.63 +/- 0.10

After correcting these magnitudes for the expected Galactic foreground extinction corresponding to a reddening of E_B-V = 0.15 mag (Schlegel et al. 1998), the SED is well fit with a simple power law of spectral index \beta = 0.5 +/- 0.2 and no strong evidence for host-intrinsic reddening. The significant drop in flux in the g'-band suggests a photometric redshift of 3.1 +/- 0.2, consistent with the lack of detection in the bluer UVOT filters (Kuin et al., GCN 13808).


GRB_name: GRB120923A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13811
SUBJECT: GRB 120923A: GROND Upper limits
DATE:    12/09/24 03:01:34 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

F. Knust (MPE Garching), S. Klose, A. Nicuesa Guelbenzu (both TLS 
Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND 
team:

We observed the field of GRB 120923A (Swift trigger 534402; Yershov et 
al., GCN 13796) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 00:10 UT on Sep 24, 19 hrs after the GRB trigger, 
and are continuing. In a first 30 min exposure, at a mid time 00:35 UT, we 
do not detect any source at the position of the NIR transient reported by 
Levan et al. (GCN 13802) down to (AB mags, 3 sigma)

g' > 23.5,
r' > 23.7,
i' > 23.0,
z' > 23.0,
J  > 21.0,
H  > 20.4.

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


GRB_name: GRB120923A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13812
SUBJECT: GRB 120923A: Swift-XRT refined Analysis
DATE:    12/09/24 05:28:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), O.M. Littlejohns (U.
Leicester), B. Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), P.
D'Avanzo (INAF-OAB) and V.N. Yershov report on behalf of the Swift-XRT
team:

We have analysed 9.0 ks of XRT data for GRB 120923A (Yershov  et al.
GCN Circ. 13796), from 151 s to 57.5 ks after the  BAT trigger. The
data comprise 331 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 13801).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.84 (+0.11, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+0.47, -0.26). The
best-fitting absorption column is  1.08 (+1.30, -0.10) x 10^21 cm^-2,
consistent with the Galactic value of 9.8 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.2 x 10^-11 (5.1 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.08 (+1.30, -0.10) x 10^21 cm^-2
Galactic foreground: 9.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.78 (+0.47, -0.26)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00534402.

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


GRB_name: GRB120923A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13813
SUBJECT: GRB 120923A: EVLA Observations
DATE:    12/09/24 16:23:18 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, and T. Laskar (Harvard) report on behalf of a 
larger collaboration:

"We observed the position of GRB 120923A (Yershov et al; GCN 13796) 
beginning on 2012 Sep 24.02 UT (0.8 d after the burst) with the EVLA at 
a mean frequency of 5.8 GHz. We find no significant radio emission at 
the position of the near-IR counterpart (Levan et al; GCN 13802) or 
within the enhanced Swift/XRT error circle (Goad et al; GCN 13801) to a 
3-sigma limit of 28 uJy."


GRB_name: GRB120923A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13814
SUBJECT: GRB 120923A:  CARMA Observations
DATE:    12/09/24 16:24:29 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report on behalf of the CARMA Key 
Project "A Millimeter View of the Transient Universe":

"We observed the position of GRB 120923A (Yershov et al; GCN 13796) with 
the Combined Array for Research in Millimeter Astronomy (CARMA) 
beginning on 2012 Sep 23.99 UT (0.77 d after the burst).  Observations 
were obtained at a mean frequency of ~85 GHz.  We find no significant 
millimeter emission at the position of the near-IR counterpart (Levan et 
al; GCN 13802) or within the enhanced Swift/XRT error circle (Goad et 
al; GCN 13801) to a preliminary 3-sigma limit of 0.39 mJy."


GRB_name: GRB120923A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13815
SUBJECT: GRB 120923A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/09/24 22:42:24 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 534402 (Yershov, et al., GCN 13796).  The burst location was within
the field of our wide-field monitor located in Maui, HI, which began a 10 s
integration of the location at 05:16:05.26 UT, 1.0 s before the Swift trigger
time and during the gamma-ray emitting interval.  The next 10 s exposure began
at 05:16:23.26, 17.0 s after the Swift trigger and covering the peak emission
detected by the BAT (Markwardt, et al., GCN 13807).  The optical counterpart
(Levan, et al., GCN 13802) was not detected above our 3-sigma limiting
magnitude of 10.5 based on a comparison of our unfiltered image to the
Tycho-2 V-band catalog.


GRB_name: GRB120916A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13816
SUBJECT: GRB 120916A Suzaku WAM observation of the prompt emission
DATE:    12/09/25 05:23:37 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 120916A (Fermi-LAT detection: Vianello et al., GCN 13777;
IPN detection and localization: Hurley et al., GCN 13778) triggered
the Suzaku Wide-band  All-sky Monitor (WAM) which covers an energy range
of 50 keV - 5 MeV at 04:07:46.689 UT (=T0).

The observed light curve shows a multi-peaked main structure starting
at T0-2 s, ending at T0+30 s with the total duration (T90) is about 26
seconds.
A weaker and softer pulse followed the main component from T0+50 s to
T0+60 s.
The fluence of main pulse in 100 - 1000 keV was
1.11 (-0.09, +0.13) x 10^-5 erg/cm^2

The 1-s peak flux measured at T0+23 s was
5.25 (-0.41, +0.46) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s
to T0+28 s is well fitted by a power-law with exponential cutoff model:

dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha : 0.97(-1.01, +0.70)
  Epeak : 342 (-72, +106) keV (chi^2/d.o.f = 5.18/14).

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

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


GRB_name: GRB120923A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13817
SUBJECT: GRB 120923A: MITSuME Okayama Optical upper limits
DATE:    12/09/25 05:54:47 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 collaboration:

We observed the field of GRB 120923A (Yershov et al., GCNC 13796)
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 2012-09-23 10:00:39 UT (~4.7 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Goad et al., GCNC 13801) in all the three bands.
We also could not detect the previously reported afterglow (Levan et al.,
GCNC 13802).

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
------------------------------------------------------
0.23958    11:01:05    6360.0   >20.6  >20.2  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120923A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13818
SUBJECT: GRB 120923A: RAPTOR Early Afterglow Limits
DATE:    12/09/25 23:45:36 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made follow-up observations
of Swift trigger 534402 (Yershov, et al., GCN 13796).  Our narrow-field
instruments in Los Alamos, NM, began imaging at 05:17:43.06 UT, 96.8 s after
the Swift BAT trigger.  We do not detect the optical counterpart (Levan,
et al., GCN 13802) in any of our images.  The following table summarizes some
of our early observations.  Our unfiltered images are calibrated to the
USNO-B1 r-band.  The start time is seconds since the BAT trigger time.  The
magnitude limit is the 3-sigma detection threshold.

T-Start    Exp-Time   Mag-Limit
----------------------------------
96.82      5.9        17.3
106.83     5.4        17.6
143.24     5.4        17.5
161.53     5.1        17.5
181.82     10.1       18.2
220.22     10.4       18.1
284.22     10.9       18.1


GRB_name: GRB120921A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13819
SUBJECT: GRB 120921A: Fermi GBM detection of its 1000th GRB
DATE:    12/09/26 15:41:42 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

The GBM Team reports:

"At 21:03:03.77 UT on 21 September 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120921A (trigger 369954186 / 120921877).

The on-ground calculated location, using the GBM trigger data, is
RA = 96.4, DEC = -64.8 (J2000 degrees, equivalent to 06 h 26 m,  -64 d 
48 '),
with an uncertainty of 3.2 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 110 degrees.

This is a single-peaked burst with a duration (T90) of about
6 s (50-300 keV), with a moderate fluence (10-1000 keV) of about 2.5E-6 
erg/cm^2.

GRB 120921A is not a particularly interesting GRB except for the fact that
it is the 1000th GRB which triggered GBM.  It occurred after 4 years,
2 months, and 1 week of Fermi GBM operations.  The annual GBM
detection rate of 240 GRBs compares with 280 GRBs detected annually
by BATSE.  Although GBM has much less effective area than BATSE, its
versatile triggering scheme leads to more detections than expected
from scaling the BATSE rate by the relative collection areas.

GBM burst locations are distributed via GCN notices on timescales of
seconds after the trigger (Flight Software and Ground Automated),
with Human-in-the-loop final locations distributed as GCN notices
between 20 minutes and several hours after the trigger.  Recent
improvements in the ground processing of locations have led to a
decrease in processing time for the Ground Automated locations so that
most appear within 30 seconds of trigger time.

Final spectral results for this and all GBM GRBs will be published in the
GBM GRB Catalog.  Data from from the first ~500 GBM GRBs appear
in the first GBM GRB catalogs:

Paciesas, W.S. et al. 2011, ApJS, 199, 18 (general)
Goldstein, A. et al. 2011, ApJS, 199, 19 (spectral).

Preliminary duration, flux, and fluence information for all GBM GRBs is 
available
at the HEASARC in the days - week following the trigger
time:  http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html"

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


GRB_name: GRB120923A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13820
SUBJECT: GRB 120923A: optical upper limit
DATE:    12/09/26 20:24:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (SAI MSU, IKI), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  the Swift GRB 120923A (Yershov  et al., GCN 13796) 
with 0.45-m telescope of ISON-NM observatory  starting on  Sep. 23 (UT) 
05:18:58, i.e 172 s after burst trigger.  We took  several unfiltered images 
of 30 s and 60 s exposures.  We do not detect the optical counterpart (Levan 
et al., GCN 13802). A  photometry of  co-added frames is based  on the 
USNO-B1.0 (R2)  nearby  stars is following:

  T0+,          Exposure,  OT,         UL (3 sigma)
  mid, d         (s)

0.00447      9x30           n/d           19.7
0.02839    53x30           n/d           20.5


GRB_name: GRB120919A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13821
SUBJECT: Further Swift-XRT observations of the GRB 120919A field.
DATE:    12/09/27 15:23:15 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

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

Further XRT follow-up observations covering the field of the GBM and
IPN-detected burst GRB 120919A (Rau et al. GCN Circ. 13785, Hurley et
al.  GCN Circ.  13786) have been performed. The data total 15 ks in
Photon Counting (PC) mode, collected in three observations from 134 ks
to 573 ks after the trigger. The two X-ray sources identified within
the IPN error box after the inital XRT observation (Beardmore and
Oates, GCN C. 13790) show no evidence for fading. Likewise, none of
the additional sources seen in the XRT field, but outside the IPN
error box, show evidence for fading, implying we have not detected any
X-ray counterpart to this GRB. The 3 sigma detection limit is
approximately 2.5e-3 count/s (per 5ks observation), which corresponds
to a 0.3-10 keV flux limit of 1.0e-13 erg cm^-2 s^-1 (for a typical
GRB spectrum).


GRB_name: GRB120927A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13822
SUBJECT: GRB 120927A: Swift detection of a burst
DATE:    12/09/27 23:05:47 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

A. Maselli (INAF-IASFPA), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
S. T. Holland (STScI), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC) and
F. E. Marshall (NASA/GSFC) report on behalf of the Swift Team:

At 22:40:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120927A (trigger=534815).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 136.600, +0.417 which is 
   RA(J2000) = 09h 06m 24s
   Dec(J2000) = +00d 25' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a broad single-peaked
structure with a duration of about 50 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:43:20.0 UT, 154 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 136.614125, 0.415722 which is equivalent
to:
   RA(J2000)  = 09h 06m 27.20s
   Dec(J2000) = +00d 24' 56.6"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 158 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
BAT and XRT error circles. 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 A. Maselli (maselli 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: GRB120923A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13823
SUBJECT: GRB 120923A: JHK Observation
DATE:    12/09/28 06:48:44 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im (CEOU/SNU), H.-I. Sung (KASI), and Y. Urata (NCU)
on behalf of a larger collaboration.

We observed the field of GRB 120923A (Yershov et al. GCN 13796)
in JHK using KASINICS on the 1.8m telescope at the Bohyunsan
observatory in Korea.

The observation started at 2012-09-29 11:30:43 UT,
or about 6.25 hours after the BAT alert.
The stacked JHK images do not reveal a convincing detection
of the afterglow reported earlier (Levan et al. GCN 13802),
to the limits of ~20 AB mag in H and K (3-sigma).

[GCN OPS NOTE(03oct12): See GCN Circ 13825 for a correction.]


GRB_name: GRB120927A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13824
SUBJECT: GRB 120927A: Enhanced Swift-XRT position
DATE:    12/09/28 07:25:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 4566 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 120927A, 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 = 136.61376, +0.41620 which is equivalent
to:

RA (J2000): 09h 06m 27.30s
Dec (J2000): +00d 24' 58.3"

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: GRB120923A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13825
SUBJECT: GRB 120923A: Correction to GCN 13823
DATE:    12/09/28 07:33:43 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

  M. Im (CEOU/SNU) reports

  The UT date reported in GCN 13823 should be 2012-09-23,
  rather than 2012-09-29.
  We thank J. Fynbo for spotting the error.


GRB_name: GRB120927A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13826
SUBJECT: GRB 120927A: Swift-XRT refined Analysis
DATE:    12/09/28 11:05:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), O.M.
Littlejohns (U. Leicester), J.P. Osborne (U. Leicester), G. Stratta
(ASDC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU) and
A. Maselli report on behalf of the Swift-XRT team:

We have analysed 7.9 ks of XRT data for GRB 120927A (Maselli  et al.
GCN Circ. 13822), from 138 s to 29.1 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 Beardmore et al. (GCN. Circ
13824).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.94 (+0.04, -0.06), followed by a break at T+11.5 ks to
an alpha of 2.6 (+1.7, -0.7).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.75 (+0.18, -0.17). The
best-fitting absorption column is  2.8 (+/-0.7) x 10^21 cm^-2, in
excess of the Galactic value of 3.2 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.7 x 10^-11 (6.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.8 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: 6.2 sigma
Photon index:      1.75 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
2.6, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.8 x
10^-14 (1.3 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00534815.

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


GRB_name: GRB120927A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13827
SUBJECT: GRB 120927A: GROND upper limits
DATE:    12/09/28 14:57:53 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

A. Rossi (TLS Tautenburg), P. Schady and  J. Greiner (MPE Garching)  
report on behalf of the GROND team:

We observed the field of GRB 120927A (Swift trigger 534815; Maselli et  
al., GCN 13822) simultaneously in g'r'i'z'JHK with GROND (Greiner et  
al. 2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La  
Silla Observatory (Chile).

Observations started at  09:05 UT on Sep 28, 10.4 hrs after the GRB  
trigger, as soon the target became visible from La Silla. They were  
performed at an average seeing of 2.6 arcsec and at an average airmass  
of 2.3. It was only possible to observe for a total exposure time of  
7.2 min in the g'r'i'z' bands during morning twilight, whereas in the  
JHK bands we were able to observe for a total of 32 min.

Using our full data set, we do not detect any source within the  
refined XRT error circle (Beardmore et al., GCN 13824) in our stacked  
GROND images down to the following 3 sigma limiting magnitudes (AB)  
mags:

g' > 22.4
r' > 22.5
i' > 21.9
z' > 21.9
J  > 21.3
H  > 21.0
K  > 19.4

The g'r'i'z and JHK bands are calibrated against SDSS and 2MASS,  
respectively, and the above limits are not corrected for the Galactic  
foreground reddening of E_(B-V)= 0.04 mag in the direction of the  
burst (Schlegel et al. 1998).

We note the presence of a source south of the enhanced XRT position,  
which is already present in DSS2 images.


GRB_name: GRB120927A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13828
SUBJECT: GRB 120927A, Swift-BAT refined analysis
DATE:    12/09/28 17:04:37 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

GRB 120927A, Swift-BAT refined analysis
  
D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), A. Maselli (INAF-IASFPA),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120927A (trigger #534815)
(Maselli, et al., GCN Circ. 13822).  The BAT ground-calculated position is
RA, Dec = 136.606, 0.420 deg which is
    RA(J2000)  =  09h 06m 25.3s
    Dec(J2000) = +00d 25' 13.5"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).  The
partial coding was 64%.
  
The mask-weighted light curve shows multiple overlapping peaks with an overall
FRED profile starting about T-15 seconds and significant until about
T+32 seconds.  T90 (15-350 keV) is 43 +- 18 sec (estimated error including
systematics).
  
The time-averaged spectrum from T-37.94 to T+41.04 sec is best fit by a power
lawwith an exponential cutoff.  This fit gives a photon index 0.63 +- 0.38,
and Epeak of 66.1 +- 9.6 keV (chi squared 50.98 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.6 +- 0.3 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T-3.93 sec in the 15-150 keV band is
1.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.64 +- 0.08 (chi squared 77.30 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/534815/BA/


GRB_name: GRB120927A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13829
SUBJECT: GRB 120927A: Swift/UVOT Upper Limits 
DATE:    12/09/29 15:02:02 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) and A. Maselli (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120927A
158 s after the BAT trigger (Maselli et al., GCN Circ. 13822).
No optical afterglow consistent with the enhanced XRT position
(Beardmore et al. GCN Circ. 13824) 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) and subsequent exposures are:

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

white_FC           158          308          147         >20.3
u_FC               317          567          246         >19.5
white              158         6331          580         >21.0
v                  648         6625          317         >19.1
b                  572         6127          432         >20.1
u                  317         5921          659         >20.2
w1                 697         5717          413         >19.6
m2                 672         5511          225         >19.6
w2                 623         6537          432         >20.3

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: GRB121001A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13833
SUBJECT: GRB 121001A: possible optical counterpart
DATE:    12/10/01 20:32:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed field of the Swift  GRB 121001A = Swift trigger 535026 (D'Elia 
et al. GCN  13831) with Zeiss-600 telescope of Mt.Terskol observatory in R 
filter starting on Oct. 01 (UT) 18:39:20.  In a stacked image of first 13x60 
exposures we detect optical source in coordinates (J2000) RA=18 24 07.8 
Dec=-05 39 55.3 which is consistent with XRT error circle (GCN  13831). The 
optical source is absent in DSS2 plates. However at that time we cannot 
determine if the source is variable. Preliminary photometry of the source 
against nearby USNO B1.0 stars is 19.5R.  Finding chart can be found at
http://grb.rssi.ru/GRB121001A/GRB121001A_R_Z600_fc_1.png


GRB_name: GRB121001A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13834
SUBJECT: GRB 121001A: MASTER optical observations
DATE:    12/10/01 23:01:39 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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.Krushinski, I.Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed  to the Swift  GRB121001A 43 s after 
notice time and 209  sec after GRB time at  2012-10-01 18:26:31 UT in a 
two  polarizations.

We haven't found optical transient  within  SWIFT error-box (D'Elia
et al. GCN  13831)  on our first (20 s exposure) set.

The 5-sigma upper limit has been about 15.8  mag

Observations were carried out under the full moon and  on high zenith 
distance (~70 deg). Also a high  stars density  complicates the analysis.

The data reduction is continued.

The message may be cited.


GRB_name: GRB121001A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13836
SUBJECT: Swift Trigger 535026 is GRB 121001A: Swift-BAT refined analysis
DATE:    12/10/02 01:14:20 GMT
FROM:    Craig Markwardt at NASA/GSFC  <craigm@milkyway.gsfc.nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry 
downlink, we report that Swift trigger #535026 (D'Elia, et al., GCN 
Circ. #13831) is consistent with being a GRB.  We follow the designation 
of previous authors for the trigger as GRB 121001A (Zheng et al. GCN 
Circ. #13832; Andreev et al. GCN Circ. #13833; Gorbovskoy et al. GCN 
Circ. #13834).

Based on the analysis below, the burst has strong emission up to 100 
keV, and a FRED-like light curve profile with duration longer than 
100sec.  Neither of these is consistent with a neutron star 
thermonuclear X-ray burst (which would be blackbody emission with 
temperature kT ~ few keV).  The soft emission we reported in GCN Circ. 
#535026 is associated with an X-ray burst from HETE J1900.1-2455, 
another active X-ray binary in the BAT field of view.  Thus, we conclude 
that trigger #535026 is consistent with a GRB interpretation.

We report further BAT analysis of GRB 121001A (trigger #535026).
The BAT ground-calculated position is
RA, Dec = 276.029, -5.667 deg which is
      RA(J2000)  =  18h 24m 06.9s
      Dec(J2000) = -05d 40' 01.0"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The light curve shows a FRED-like profile, starting near T-25sec, rising 
to maximum at T-15sec, and gradually decaying to background near 
T+130sec.  T90 (15-350 keV) is 147 +- 24 sec (estimated error including 
systematics).

The time-averaged spectrum from T-30 to T+143 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.34 +- 0.15.  The fluence in the 15-150 keV band is 1.7 +- 
0.2 x 10^-6 erg/cm2.  The 1-sec peak photon flux measured from T+3.27 
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 BAT results for this circular represent a limited time window.  The 
results may be revised if additional downlinked data show more emission.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/535026/BA/


GRB_name: GRB121001A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13837
SUBJECT: GRB 121001A: Enhanced Swift-XRT Position
DATE:    12/10/02 07:12:24 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 2340 s of XRT Photon Counting mode data and 3 UVOT images of GRB 
121001A (D'Elia et al., GCN Circ. 13831), 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 = 276.03227, -5.66587 
which is equivalent to:

RA (J2000):  18 24 07.74
Dec (J2000): -05 39 57.1

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 is an official product of the Swift-XRT team.


GRB_name: GRB121001A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13838
SUBJECT: GRB 121001A: Swift-XRT refined Analysis
DATE:    12/10/02 12:29:53 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC) and P. Evans (U. Leicester)  report on behalf of the
Swift-XRT team:

We have analysed 6.7 ks of XRT data for GRB 121001A (D'Elia et al. GCN
Circ. 13831), from 111 s to 41.8 ks after the  BAT trigger. The data
comprise 93 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 2340 s of PC mode data and 3 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 = 276.03227, -5.66587
which is equivalent to:

RA (J2000): 18h 24m 07.74s
Dec(J2000): -05d 39' 57.1"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.30 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.28 (+0.25, -0.24). The
best-fitting absorption column is  7.6 (+2.4, -2.0) x 10^21 cm^-2, in
excess of the Galactic value of 4.5 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 7.6 x 10^-11 (9.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.6 (+2.4, -2.0) x 10^21 cm^-2
Galactic foreground: 4.5 x 10^21 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.28 (+0.25, -0.24)

If the light curve continues to decay with a power-law decay index of
1.30, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x
10^-13 (2.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00535026.

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


GRB_name: GRB121001A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13839
SUBJECT: GRB 121001A: Swift/UVOT Upper Limits
DATE:    12/10/02 17:12:45 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121001A
130 s after the BAT trigger (D'Elia et al., GCN Circ. 13831).
No optical afterglow consistent with the optical position
(Tello et al. GCN Circ. 13835) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

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

white_FC           130          280          147         >21.0
u_FC               288          538          246         >20.0
white              130         7415          824         >22.4
v                  618         6390          352         >20.2
b                  544         7210          526         >21.2
u                  288         7005          756         >20.7
w1                 668         6800          529         >20.4
w2                 767         7608          439         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.36 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121001A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13840
SUBJECT: GRB 121001A: GROND Afterglow Confirmation
DATE:    12/10/02 23:46:14 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of GRB 121001A (Swift trigger 535026, D'Elia et al.,
GCN # 13831) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started on October 01, 2012, at 23:37 UT, 5.23 hr after the
GRB trigger. They were performed at an average seeing of 2".7 (in r') and
at an average airmass of 1.2.

We found a source in the z', J, H and K bands at coordinates (J2000):

RA   =  18:24:07.84

Dec. = -05:39:55.30

with an error of 0".3 in each coordinate.

This is consistent with the afterglow positions reported by Andreev et al.
(GCN # 13833) and Tello et al. (GCN # 13835), but slightly outside the
refined XRT position reported by Evans et al. (GCN # 18837).

Based on 1380 s of total exposures in g'r'i'z' (mean time 0.2415 days
after the trigger) and 1920 s in JHK (mean time 0.2363 days after the
trigger) we estimate preliminary AB magnitudes (upper limits are 3 sigma) of

g' > 23.6,

r' > 22.9,

i' > 22.2,

z' = 21.7 +/- 0.2,

J  = 19.5 +/- 0.4,

H  = 18.4 +/- 0.1 and

K  = 17.94 +/- 0.06.

Given magnitudes are calibrated against GROND zeropoints in the optical as
well as 2MASS field stars in the NIR and are not corrected for the high
Galactic foreground reddening of E_(B-V) ~ 1.3 mag (Schlegel et al. 1998).

Our r'- and i'-band non-detections vs. the detections reported by Andreev
et al. (GCN # 13833) and Tello et al. (GCN # 13835) confirm that this is
the afterglow of GRB 121001A. Furthermore, the bright source we detect in
K is not detected in 2MASS, while nearby sources of similar magnitude are
clearly visible in 2MASS.


GRB_name: GRB120804A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13841
SUBJECT: GRB 120804A: Late-time Chandra observation
DATE:    12/10/04 17:56:15 GMT
FROM:    David Burrows at PSU/Swift  <dnburrows@gmail.com>

GRB 120804A: Late-time Chandra observation 

David N. Burrows (PSU), Bin-Bin Zhang (PSU) and Eleonora Troja
(NASA/GSFC/UMCP) report:

We re-observed the field of GRB 120804A (Lien et al., GCN Circ. 13573)
with the Chandra ACIS instrument, starting on September 18, 2012 
16:04:50 UT (~46 days after the GRB trigger), for a total exposure of 
60 ks. The X-ray afterglow is clearly detected at the 10 sigma level.  
The inferred flux is consistent with an extrapolation of 
the earlier Swift XRT observations (Troja et al., GCN Circ. 13640) and the 
XMM observation (Margutti et al. (GCN Circ. 13715), and shows a 
continuing decline in flux with a power-law decay slope of ~1.0 and 
no evidence for a jet break, consistent with Berger et al. (arXiv:1209:5423).  

We thank Dan Schwartz  and the entire Chandra staff for 
rapidly executing this observation.


GRB_name: GRB120927A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13842
SUBJECT: GRB 120927A: optical upper limit
DATE:    12/10/05 18:23:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed field of the Swift  GRB 120927A  (Maselli et al. GCN  13822) 
with Zeiss-600 telescope of Mt.Terskol observatory starting on Sep. 28 (UT) 
01:31:05. Several unfiltered images were taken under favorable weather 
conditions. We do not detect any sources in the enhanced XRT error circle 
(Beardmore et al. GCN  13824). Photometry is based on nearby USNO-B1.0 (R2) 
stars:

  T0+,     Filter      Exposure,  OT,     UL (3 sigma)
  mid, d                (s)

0.1292    none      30x60         n/d     22.0 


GRB_name: GRB121011A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13845
SUBJECT: GRB 121011A: Swift detection of a burst with optical afterglow
DATE:    12/10/11 11:36:05 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), D. N. Burrows (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
B.P. Gompertz (U Leicester), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), C. Pagani (U Leicester),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 11:15:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121011A (trigger=535764).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 260.200, +41.137 which is 
   RA(J2000) = 17h 20m 48s
   Dec(J2000) = +41d 08' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 11:17:07.9 UT, 97.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 260.21504,
41.11179 which is equivalent to:
   RA(J2000)  = 17h 20m 51.61s
   Dec(J2000) = +41d 06' 42.4"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 99 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.34
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 6.36e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 108 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 17:20:51.22 = 260.21340
  DEC(J2000) = +41:06:36.9  =  41.11024
with a 90%-confidence error radius of about 0.63 arc sec. This position is 9.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.76 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 

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: GRB121011A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13846
SUBJECT: GRB 121011A: MITSuME Okayama Optical Observation
DATE:    12/10/11 12:11:41 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 collaboration:

We observed the field of GRB 121011A (Racusin et al., GCNC 13845)
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 2012-10-11 11:17:00 UT, (~90 sec after the burst)
We detected the previously reported afterglow (Racusin et al., GCNC 13845)
in  all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'   g'_err Rc    Rc_err Ic    Ic_err
-----------------------------------------------------------------------
0.00449    11:21:58    540.0     17.23 0.09   16.81 0.05   16.11 0.05
0.01159    11:32:11    540.0     17.36 0.10   16.65 0.04   16.10 0.04
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13847
SUBJECT: GRB121011A : Xinglong TNT optical observation
DATE:    12/10/11 12:35:21 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB121011A ( Racusin  et al., GCN 13845 ) 
with Xinglong TNT telescope at  11:17:24(UT), about 2 min after 
the burst. A series of white and R-band images were obtained. 
The OT reported by (Racusin  et al., GCN 13845; Kuroda et al. 13845 ) 
was detected in all images.  The brightness of this OT was about 
R=16.8 mag at  10 min after the burst, calibrated by USNO B1.0 R2 mag.
The brightness is consistent with the report by Kuroda et al. 13845.

This message may be cited.


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13848
SUBJECT: GRB 121011A: MASTER-Net early OT light curve
DATE:    12/10/11 13:10:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

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

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

V.Krushinski, I.Zalozhnich,  A. Popov, A. Bourdanov, A. Punanova
Ural Federal University

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  GRB121011.47 10 sec s after
notice time and 51 sec after GRB time at 2012-10-11 11:16:21.301 UT in
two polarizations.
The 5-sigma upper limit  of the first (10s exposure) set  has been about
17.0 mag

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB 121011A   65 sec s after notice 
time and 106 sec after GRB time at 2012-10-11 11:17:14 UT in two 
polarizations. On our first 
(10s exposure) set we haven't found optical transient  within SWIFT 
error box. The weather conditions were not very good.

The first individual image on which we see the OT was taken on 2012-10-11 
at 11:19:20, i.e 230 sec. after the GRB time. The maximum brightness
(calibrated to 0.8*R+0.2*B from USNO-B1.0) was 16.1.

The preliminary light curve is available here:
http://master.sai.msu.ru/static/GRB/GRB121011_pre_lc.png

We note that nothing is visible at the position of the OT on the Palomar 
DSS plates and on color-combined SDSS image, implying the host galaxy is 
fainter than 22.5 m.

The reduction of the whole data set is continuing.

This message can be cited.


