# GCN_circulars

GRB_name: GRB120427A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13272
SUBJECT: Konus-Wind observation of GRB 120427A
DATE:    12/04/28 17:04:53 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

GRB 120427A (IPN localization: Hurley at al., GCN 13271)
triggered Konus-Wind at T0=04651.927s UT (01:17:31.927)

The light curve shows a broad pulse with
a total duration of ~5 s.
The emission is seen up to ~5 MeV.
A spectral lag between the G2(90-300 keV)
and the G1(25-90 keV) instrument's light curves
is estimated to 0.51  0.07 s (1 sigma).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120427_T04651/

As observed by Konus-Wind the burst
had a fluence of (7.8  1.1)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+1.600 s,
of (2.6  0.4)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.77 (-0.20, +0.23),
the high energy photon index beta = -2.9 (-1.1, +0.3),
the peak energy Ep = 133(-14, +7) keV,
chi2 = 97.5/81 dof.

We note a curious resemblance, both in the light curves
and in the spectral properties, between GRB 120427A and
the one-day older GRB 120426A (Golenetskii et al., GCN 13268).
However, a ~126 deg angular distance between their IPN
localization boxes (GCN 13265, GCN 13271) leaves
no chance for a lensed event.

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


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13273
SUBJECT: GRB 120422A: optical observations
DATE:    12/04/29 17:45:14 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 120422A (Troja et al., GCN 13243) with AZT-11 
telescope of CrAO observatory  on April 22  (UT) 18:54:58 - 19:55:14 under 
mean seeing  of  2.8 arcsec and with Shajn telescope of CrAO observatory  on 
April 23  (UT) 18:22:50 - 19:29:02 under mean seeing  of  1.8 arcsec. In 
both epochs we cannot resolve the afterglow (Cucchiara et al., GCN 13245; 
Kuin et al., GCN 13248) from possible host galaxy SDSS J090738.51+140108.3 
and we used aperture photometry of host + afterglow. A preliminary 
photometry is based on the USNO-B1.0 star 1040-0165213  (09 07 37.94 +14 00 
43.0)  assuming R=16.37:

T0+        Filter,  Exposure, OT+host,  uplim (3 sigma)
(mid, d)             (s)

0.5091     R     20x180      20.5   +/-0.3     20.8
1.4891     R      60x60       20.74 +/-0.03   23.9

From the above photometry of the host + afterglow it is evident that in both 
epochs there is apparent admixture of the afterglow in the brightness of the 
galaxy SDSS J090738.51+140108.3 which have a brightness of R ~ 21.0.

We are grateful for CCD PL4240 provided by ISON for Shajn telescope.


GRB_name: GRB120427A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13274
SUBJECT: GRB 120427A: MASTER follow up observations 
DATE:    12/04/30 08:14:04 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  GRB120427A  41h 32min after GRB time at 
2012-04-28 18:49:09 UT. On our  (180s exposure) set robot haven't found optical transient  within IPN 
Triangulation  error-box (Hurley et al., GCN Circ 13271).
The 5-sigma upper limit has been about 20.0 mag

The message may be cited.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13275
SUBJECT: GRB 120422A: i-band re-brightening and possible SN detection
DATE:    12/04/30 23:33:38 GMT
FROM:    Giorgos Leloudas at Dark Cosmology Centre  <giorgos@dark-cosmology.dk>

D. Malesani (DARK/NBI), S. Schulze (Univ. Iceland), T. Kruehler (DARK/NBI),
G. Leloudas (OKC/Stockholm and DARK/NBI), A. de Ugarte Postigo (IAA/CSIC and DARK/NBI),
D. Xu (WIS), J. P. U. Fynbo, J. Hjorth (DARK/NBI), P. Jakobsson (Univ. Iceland),
R. Kotak, D. Wright (Queens University Belfast), G. Barisevicius, S. Geier (NOT),
report on behalf of a larger collaboration:


We have used the NOT equipped with ALFOSC to monitor the optical counterpart of GRB 120422A
(Troja et al., GCN 13243; Cucchiara et al., GCN 13245). 

The source brightened by 0.80 +- 0.15 mag between Apr. 25.86 UT and Apr. 30.90 UT
(3.56 and 8.60 days after the GRB, respectively). On Apr. 25.86 UT the counterpart
had i ~ 22.10, calibrated against stars from the SDSS catalogue. This is consistent
with the measurement by Perley et al. (GCN 13267) at a similar epoch.  On Apr. 30.90 UT,
we measure i = 21.30 +/- 0.15.

We suggest this re-brightening to be due to the emerging supernova.


GRB_name: GRB120422A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13276
SUBJECT: GRB 120422A: Gemini-N detection of a supernova
DATE:    12/05/01 14:30:04 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

K. Wiersema (U. Leicester), A. Cucchiara (UCSC/UCO Lick),
A. J. Levan (U. Warwick), S. Rapoport, B. P. Schmidt (ANU), D. Bersier (LJMU),
D. Perley (Caltech), S. B. Cenko (UC Berkeley), N. R. Tanvir (U. Leicester)
report on behalf of a larger collaboration:

We observed the position of GRB 120422A (Troja et al., GCN 13243) using
the GMOS-N Spectrograph on the Gemini-North telescope. We acquired spectra
starting at 06:36 UT on 1 May 2012. We used the R400 grism, obtaining 4 x 1200
seconds exposure time, covering a wavelength range 4400 - 8670 A.

In addition to many narrow nebular lines from the host galaxy (Tanvir et
al. GCN 13251; Schulze et al. GCN 13257), the spectra show several broad
undulations in the continuum. The restframe positions of these features are
well matched to those seen in spectra of SN 1998bw at early times. We
therefore conclude that the rebrightening reported by Malesani et al. (GCN
13275) is consistent with being caused by a broad-lined type Ib/c supernova.

We thank Kristin Chiboucas for obtaining these observations.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13277
SUBJECT: GRB 120422A: VLT/X-shooter spectroscopic evidence for a SN
DATE:    12/05/01 14:30:06 GMT
FROM:    Bo Milvang-Jensen at Dark Cosmology Centre,NBI,U. Copenhagen  <milvang@astro.ku.dk>

D. Malesani (DARK/NBI), S. Schulze (Univ. Iceland), T. Kruehler, J. P. U.
Fynbo, J. Hjorth, B. Milvang-Jensen, D. Watson (DARK/NBI), A. de Ugarte Postigo
(IAA/CSIC and DARK/NBI), N. R. Tanvir (Univ.  Leicester), G. Tagliaferri
(INAF-OAB), G. Leloudas, J. Sollerman (OKC, Stockholm), D. Xu (WIS, Israel), M.
D. Stritzinger (IFA, Aarhus), A. De Cia (Univ. Iceland) report on behalf of the
X-shooter GRB GTO collaboration:

We observed the re-brightened optical counterpart of GRB 120422A (Troja et al.,
GCN 13243; Cucchiara et al., GCN 13245; Malesani et al., GCN 13275) with the
ESO VLT equipped with the X-shooter spectrograph. Observations started on 2012
May 1.0 UT (8.7 days after the GRB), for a total exposure time of 80 min in
each of the UVB, VIS, and NIR arms, covering the wavelength range 3000-25000
A. The slit was aligned to cover both the galaxy at z = 0.28 present in
the SDSS (Cucchiara et al., GCN 13245; Tanvir et al., GCN 13251) and the
optical counterpart (Cucchiara et al., GCN 13245).

The spectrum exibits a broad emission peak centred at 6300 A similar to the
previous report based on a Keck spectrum taken on April 27 (Perley et al., GCN
13267). Blueward of the peak the spectrum drops steeply down to around 4000 A
and beyond that we do not detect flux. Over the full covered spectral range
the spectrum bears a good resemblance with spectra of SN 1998bw, associated
with GRB 980425, about 6 days before maximum (Patat et al. 2001, ApJ, 555,
900).

We acknowledge the excellent support of the ESO observing staff, in particular
Claudio Melo, Giacomo Beccari, Marcelo Lopez and Ivo Saviane. We also thank
the visiting astronomer Luca Sbordone for allowing us to observe the event.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13278
SUBJECT: GRB 120422A: CARMA 3mm observations
DATE:    12/05/03 02:58:42 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

We observed the position of GRB 120422A (Troja et al., GCN 13243) with 
the Combined Array for Research in Millimeter-Wave Astronomy (CARMA) at 
a frequency of 92.5 GHz (3 mm) between 23:13 on 2012-04-24 and 00:29 on 
2012-04-25 (UT). The mean observation time was 2.6937 days after the GRB 
trigger.

No source is detected at the position of the X-ray (GCN 13243) optical 
(Cucchiara et al., GCN 13245) and radio (Zauderer et al., GCN 13254) 
counterparts.  The 3-sigma limit of the map is 1.15 mJy.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13279
SUBJECT: GRB 120422A: P200 NIR detection
DATE:    12/05/03 03:21:57 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley, T. Jones, and R. Ellis (Caltech) report:

We observed the field of GRB 120422A (Troja et al., GCN 13243) with the 
Wide-field IR Camera (WIRC) on the Palomar 200-inch telescope between 
04:01 and 05:04 UT on 2012-05-02.  15 exposures of 240s each (1 hour of 
observations total) were acquired in the J-band filter.

The optical counterpart to GRB 120422A (at this stage probably a rising 
supernova; GCNs 13275, 13276, 13277) is clearly detected in the combined 
image.  Seeing conditions were good and the transient is resolved from 
its host galaxy, although the background is affected by scattered light 
from the bright star 1 arcmin to the northwest.  Using a 0.8 arcsec 
radius aperture, we measure a magnitude of J = 20.7 +/- 0.2 at a mean 
time of 9.89 days after the burst.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13281
SUBJECT: GRB 120422A: SN identification from GTC
DATE:    12/05/07 18:55:42 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

R. Sanchez-Ramirez (IAA-CSIC), G. Leloudas (OKC, Stockholm), 
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), 
J. Gorosabel (IAA-CSIC), D. Malesani (DARK/NBI), S. Schulze (Univ. Iceland), 
J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (Univ. Leicester), J. Hjorth (DARK/NBI), 
D. Xu (WIS) report on behalf of a larger collaboration:

We have obtained spectroscopy of the optical counterpart of GRB 120422A 
(Troja et al. GCN 13243, Cucchiara et al. GCN 13245) and its host galaxy, at 
a redshift of 0.283 (Tanvir et al. GCN 13251, Schulze et al. GCN 13257) in two 
epochs, 3.6 and 14.6 days after the burst. Both spectra were obtained with a 
resolution of ~500 and cover the range between 4800 and 10000 AA. 

The first epoch is close to the minimum of the light  curve, before the detection 
of the SN component (Malesani et al. GCN 13275), the spectrum is blue, 
flattening at ~5000 AA. It shows nebular emissions but no clear characteristic 
broad features of a SN spectrum. 

In the second spectrum, we clearly detect SN features, as reported by Wiersema 
(GCN 13276) and Malesani (GCN 13277). These features are now prominent 
and give an excellent match with those of broad-lined Ic SNe close to maximum, 
using SNID (Blondin & Tonry 2007, ApJ, 666, 1024).

In our spectra we included an object located 5" East of the host galaxy, which has 
emission lines at the same redshift as the host and a projected distance at 
z=0.283 of 22 kpc. This could indicate the existence of an interacting system.

We acknowledge the excellent support of the GTC staff, in particular Jose Miguel 
Gonzalez Perez, Daniel Reverte Paya, Antonio Cabrera Lavers and Rene Rutten.


GRB_name: GRB120510A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13282
SUBJECT: GRB 120510A: MAXI/GSC detection of a burst
DATE:    12/05/10 13:45:36 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

N. Serita, H. Negoro, M. Nakajima, M. Asada, H. Sakakibara (Nihon U.), 
M. Serino, T. Mihara, M. Sugizaki, T. Yamamoto, M. Matsuoka (RIKEN), 
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa (JAXA),
N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech),
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka 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.), 
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

During a scan transit centered at UT 2012-05-10T08:47:44,
MAXI/GSC detected a short X-ray transient lasting about 27 seconds 
within the 42 seconds triangular transit response of MAXI/GSC.
Judging from its hardness ratio, 
this transient is probably a gamma-ray burst.

Assuming that the source flux was constant over the transit, 
we obtain the source position at

(R.A., Dec) = (+44.285 deg, +72.850deg) = ( 02 57 08.60, +72 51 00.8 )(J2000)

which has a statistical uncertainty of 10 arcmin at the 90% confidence limit 
and an additional systematic uncertainty of 6 arcmin (90% containment radius).
Due to a short burst duration, the uncertainty for the scan direction is possibly larger than this estimation.
Without assuming a constant flux of the source,
a rectangular sky region of 90% confidence
is 0.4 degrees by 1.4 degrees with the following corners:

(R.A., Dec) = (+41.76 deg, +72.60 deg) = (02 47  2, +72 36 12)(J2000)
(R.A., Dec) = (+41.77 deg, +73.02 deg) = (02 47  4, +73 01 20)(J2000)
(R.A., Dec) = (+46.50 deg, +72.97 deg) = (03 06  0, +72 58  4)(J2000)
(R.A., Dec) = (+46.40 deg, +72.55 deg) = (03 05 36, +72 32 59)(J2000).

The preliminary flux estimate (4-10 keV) of the source was 330+-40 mCrab.

There was no significant detection at the transit location in the
previous and the following orbits (92 min before and after the detection) 
with an upper limit of 20 mCrab.

Follow-up observations are encouraged.


GRB_name: GRB120510A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13283
SUBJECT: GRB 120510A: MASTER follow up observations 
DATE:    12/05/11 08:42:15 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

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

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  120510A 24146 sec after 
GRB time at 2012-05-10 15:30:10.64 UT. On our first (180s exposure) set we 
haven't found optical transient  within MAXI/GSC error-box (Serita 
et al., GCN Circ 13282).
The 5-sigma upper limit has been about 18.6 mag

  The message may be cited.


GRB_name: GRB120510A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13284
SUBJECT: GRB 120510A: Swift XRT and UVOT observations
DATE:    12/05/11 14:39:44 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), K. L. Page, P. A. Evans (U
Leicester), M. Perri (ASDC), S. T. Holland (NASA/GSFC) report on behalf of
the Swift team:

The Swift XRT and UVOT instruments observed the centre of the error circle
for the MAXI-detected GRB 120510A (Serita et al., GCN Circ. 13282) from
21.4 to 33.0 ks after the trigger.

The XRT data comprise 2.0 ks of Photon Counting (PC) mode data. A faint
source is detected RA, Dec = 44.04666, +72.88692 which is equivalent to:

RA (J2000):        02h 56m 11.20s
Dec (J2000):        +72d 53' 12.9"

with an uncertainty of 4.8 arcsec (radius, 90% confidence). The observed
count rate is (3.3 +/- 1.3) x 10^-3 cts/s. This corresponds to an observed
0.3-10 keV flux of (1.4 +/- 0.5) 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 (2.3 x 10^21 cm^-2; Kalberla et al. 2005)
this corresponds to an unabsorbed flux of (2.0 +/- 0.8) x 10^-12
erg/cm2/s. Given the limited statistics, it is not possible to determine
whether the source is fading. We note that the XRT position lies 15.6
arcsec from the ROSAT source 1RXS J025613.2+725300 (RA(J2000), Dec(J2000)=
02h 56m 13.2s, +72d 52' 59", with an error radius of 11 arcsec). We also
note that the XRT field of view covers only about 69% of the reported 16
arcmin radius error circle GRB 120510A (Serita et al., GCN Circ. 13282).

The XRT coordinates correspond to the bright, catalogued ultraviolet
source HD 17785 with a magnitude of uvw2 = 11.85 +/- 0.02 mag.  There is
very weak evidence in the UVOT data that the source may have increased in
brightness by about 0.2 mag between 28 ks and 33 ks after the burst.


GRB_name: GRB120510B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13285
SUBJECT: GRB 120510B/Fermi Trigger 358364818: MASTER possible OT candidate
DATE:    12/05/11 17:37:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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 Fermi Trigger 
358364818/GRB120510B 36 sec after GRB 
time at 2012-05-10 17:47:32.938 UT. On our Very Wide Field Camera 
(400 square degrees, 1 pix = 22 arcsec) set of images we 
have found optical transient within FERMI error-box with ~10 mag 
(unfiltered).

The OT position is:
Ra  =  12h 51m 37.9s
Dec = +00d 05m 35s
with the error box (one sigma) radius equal to 10".

We have reference image without OT on 2012-04-21 20:11:39 UT with 
unfiltered magnitude limit 12.5 m. 
In the follow up MASTER II Amur observations on 2012-05-11 at 15:12:29 UT 
there is no OT brighter than 17.2 m.
There are  two SDSS galaxies  inside one sigma error box:
SDSS J125138.22+000534.5 (rmag=19.83) and
SDSS J125138.45+000534.7 (rmag=21.98)
The data reduction is continuing.


  The message may be cited.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13288
SUBJECT: GRB 120422A: Konkoly optical observations
DATE:    12/05/12 21:25:09 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program
at the Konkoly Observatory.

Starting on the evening of 11/05/2012 we observed the field of GRB 120422A
(Troja et al., GCN 13243) 19.448 days after the burst, using a 50 cm
Cassegrain telescope located at the Mountain Station of the Konkoly
Observatory equipped with an Andor iXon + 888 EMCCD camera through R and I
filters. On the coadded R images (exp.time 600 sec) we could not detect the OT
associated SN (Giorgos Leloudas GCN 13275)and the nearby galaxy (SDSS
J090738.51+140108.3)(A. Cucchiara GCN 13245). Based on a nearby star
(USNO-A2.0 0975-06157109) we provide 19.07 +/- 0.26 magnitude in the R band as
an upper limit.


GRB_name: GRB120514A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13289
SUBJECT: GRB 120514A: Swift detection of a burst
DATE:    12/05/14 01:32:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU)
and B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 01:12:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120514A (trigger=522197).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 282.991, -4.252 which is 
   RA(J2000) = 18h 51m 58s
   Dec(J2000) = -04d 15' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure consisting of two overlapping peaks with a duration of 
about 80 sec and an additional weaker peak at ~T+150 sec coincident 
with a peak observed by the XRT.   The peak count rate was ~2500 
counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:14:31.2 UT, 101.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 282.99969,
-4.26375 which is equivalent to:
   RA(J2000)  = 18h 51m 59.93s
   Dec(J2000) = -04d 15' 49.5"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.09 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.4
(+1.29/-0.95) x 10^22 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 3.94e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 110 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. Because of the density of catalogued stars, further
analysis is required to report an upper limit for any afterglow in the
sub-image. The 8'x8' region for the list of sources generated on-board covers
100% of the 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. 

We note that this source is 2 degrees from the Galactic plane. 
Although the BAT lightcurve and energy distribution is
typical for a GRB, the possibility of this being a Galactic
source will have to be assessed from further observations. 

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


GRB_name: GRB120514A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13290
SUBJECT: GRB 120514A: TAROT Calern observatory optical observations
DATE:    12/05/14 01:55:14 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

GRB 120514A: TAROT Calern observatory optical observations
----------------------------------------------------------------------
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 120514A detected by SWIFT
(trigger 522197) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 534s after the GRB trigger.
The elevation of the field increased from
37 degrees above horizon and weather conditions
were good.

We co-added a series of exposures.
We do not detect any OT in the XRT error box
with a limiting magnitude of:
t0+534s to t0+909s : R > 18.1

Galactic coordinates are lon= 29.2060 lat= -2.0542
and the galactic extinction in R band is 4.3 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

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

This message may be cited.


GRB_name: GRB120514A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13291
SUBJECT: GRB 120514A: Swift-BAT refined analysis
DATE:    12/05/14 04:22:25 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),
V. Mangano (INAF-IASFPA), 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+721 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120514A (trigger #522197)
(Mangano, et al., GCN Circ. 13289).  The BAT ground-calculated position is
RA, Dec = 283.002, -4.258 deg which is 
   RA(J2000)  =  18h 52m 00.4s 
   Dec(J2000) = -04d 15' 28.6" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 61%.
 
The mask-weighted light curve shows 3 main peaks.  The first starts at ~T-40 sec,
and peaks at ~T+1 sec.  The second overlaps the tail of the first and peaks at ~T+52
and ends at ~T+115 sec.  The third peak starts at ~T+120 sec, peaks at ~T+150 sec
and ends at ~T+200 sec.  At the 2-sigma level, there is possible precursor emission
from ~T-160 to T-80 sec, and a possible forth peak from ~T+260 to ~T+420 sec.
T90 (15-350 keV) is 164.4 +- 5.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-8.75 to T+165.55 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.10.  The fluence in the 15-150 keV band is 2.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.22 sec in the 15-150 keV band
is 1.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/522197/BA/


GRB_name: GRB120514A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13292
SUBJECT: GRB 120514A: Enhanced Swift-XRT position
DATE:    12/05/14 04:34:05 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 932 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120514A, 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 = 283.00078, -4.26359 which is equivalent
to:

RA (J2000): 18h 52m 0.19s
Dec (J2000): -04d 15' 48.9"

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: GRB120514A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13293
SUBJECT: GRB 120514A: APEX observations of the submm counterpart
DATE:    12/05/14 12:11:51 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. de Breuck,
T. Stanke, C. Agurto (ESO), M. Valencia-S. (U. Koeln), A. Remy 
(CEA-Saclay), F. Montenegro (ESO), J. Gorosabel, 
R. Sanchez-Ramirez (IAA-CSIC), J.P.U. Fynbo (DARK/NBI) 
report on behalf of a larger collaboration:

We have observed the field of GRB 120514A (Mangano et al. 
GCNC 13289) using LABOCA/APEX at Chajnantor (Chile) in the 
870 micrometer band. The weather conditions were good, with 
precipitable water vapour at the time of the observation of ~0.5mm. 
Observations began on May 14 at 4:55 UT (3.7 hr after the burst) 
and were performed using the photometric mode, centred at the 
enhanced X-ray position (Evans et al. GCNC 13292).

On a preliminary analysis of 160 min on source, we detect a flux 
density at the position of the afterglow of 6.2+/-2.3 mJy.

Further observations are foreseen. We encourage follow-up 
observations in other wavelengths.


GRB_name: GRB120514A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13294
SUBJECT: GRB 120514A: Swift-XRT refined Analysis
DATE:    12/05/14 13:32:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

G. Stratta (ASDC), P. D'Avanzo (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), V. D'Elia (ASDC) and V.
Mangano report on behalf of the Swift-XRT team:

We have analysed 6.5 ks of XRT data for GRB 120514A (Mangano  et al.
GCN Circ. 13289), from 90 s to 28.8 ks after the  BAT trigger. The data
comprise 132 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 13292).

The late-time light curve (from T0+4.4 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.22 (+0.29, -0.24).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.90 (+0.12, -0.11). The
best-fitting absorption column is  1.68 (+0.15, -0.14) x 10^22 cm^-2,
in excess of the Galactic value of 6.1 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.2 (+/-0.3) and a
best-fitting absorption column of 2.4 (+0.5, -0.4) x 10^22 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 6.8 x 10^-11 (2.3 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+0.5, -0.4) x 10^22 cm^-2
Galactic foreground: 6.1 x 10^21 cm^-2
Excess significance: 6.6 sigma
Photon index:      2.2 (+/-0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00522197.

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


GRB_name: GRB120510A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13295
SUBJECT: Konus-Wind observation of GRB 120510A
DATE:    12/05/14 15:05:19 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long GRB 120510A localized by MAXI/GSC (Serita et al., GCN
13282) was detected by Konus-Wind in the waiting mode.

The burst light curve shows several pulses with a total duration of ~130 s.

As observed by Konus-Wind, the burst had a fluence of (3.82 +/- 
0.26)x10^-6 erg/cm2 (in the 20 - 1200 keV energy range).

Fitting the K-W 3-channel time-integrated spectrum (from T0(MAXI)+5 s to 
T0(MAXI)+135 s) by a simple power-law model yields a power law index of 
2.05 +/- 0.24.

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB120510A/


GRB_name: GRB120514A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13296
SUBJECT: GRB 120514A: UKIRT IR observations
DATE:    12/05/14 16:38:51 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J Levan (Warwick), N.R. Tanvir, K. Wiersema (Leicester), T. Wold
(JAC) report on behalf of a larger collaboration:

"We obtained K-band observations of GRB 120514A (Mangano et al. GCN
13289) with the United Kingdom Infrared Telescope (UKIRT) on Mauna
Kea, with a midpoint approximately 12 hours after the initial burst
detection. Comparison of a preliminary reduction of these images
with archival images taken as part of the UKIRT Galactic Plane
Survey (GPS; Lucas et al. 2008 MNRAS 391 136) does not reveal any
new sources within the refined XRT position (Evans et al. GCN 13292).
Given the crowded nature of the field we do note there are several
sources whose location is formally consistent with the X-ray position,
but none of these show clear evidence for variability between the
two epochs."


GRB_name: GRB120514A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13297
SUBJECT: GRB 120514A: Swift/UVOT Upper Limits
DATE:    12/05/14 16:42:24 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 120514A
110 s after the BAT trigger (Mangano et al., GCN Circ. 13289).
No optical afterglow consistent with the enhanced XRT position
(Evans et al., GCN Circ. 13292) 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           110          260          147         >20.6
u_FC               324          574          246         >20.5
white              110         1029          295         >20.9
u                  324          574          246         >20.5

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 1.63 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120514A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13298
SUBJECT: GRB 120514A: GROND upper limits
DATE:    12/05/14 16:45:37 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120514A (Mangano et al., GCN #13289) 
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).

Observation started at 03:39 UT, 2.4 h after the trigger and ended at 
11:10 UT.

We detect two sources just outside of the enhanced 1.8" XRT error circle 
at RA,DEC 18:52:00.1, -04:15:50.8 and 18:52:00.2, -04:15:46.8 with a 
positional uncertainty of +/- 0.3". We note that neither source varies 
in r' brightness relative to USNO field stars over a period of 2 hours. 
Additionally, the southern source exhibits a thermal spectrum. 
Therefore, neither of these two sources are likely associated with the GRB.

Based on exposures of 1480 seconds in g'r'i'z' and 1200 seconds in JHK, 
we do not detect a source within the 1.8" XRT error circle of the X-ray 
counterpart candidate (Evans et al., GCN #13292) to the following 
3-sigma upper limits (AB system):

g' > 22.7,
r' > 23.0
i' > 23.0
z' > 23.0
J > 20.5
H > 19.6
K > 18.5

These magnitudes are calibrated against GROND zeropoints (g'r'i'z') and 
2MASS (JHK) and are not corrected for the expected Galactic foreground 
extinction corresponding to a reddening of E_(B-V)=1.7 mag in the 
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120512A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13300
SUBJECT: GRB 120512A: A long GRB detected by INTEGRAL
DATE:    12/05/15 12:23:22 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 40 s has been detected by IBAS in the 
IBIS/ISGRI data at 02:41:40 UT of May 12.

Due to the 7.3 sigma statistical significance of the detection, only an 
Alert Packet of WEAK type was distributed in real time (Packet n. 6550).

With an off-line analysis with the standard OSA software we obtained the 
following GRB coordinates (J2000):

RA:  325.558    [degrees]
DEC:  13.636    [degrees]

with an uncertainty of 1 arcmin (90% c.l.).

These coordinates differ from those derived automatically (Alert Packet 
n.6550) because the extreme off-axis angle of the GRB (15 degrees) caused 
a wrong identification of its position in the real time image.

The burst has a peak flux of 5 counts/cm2/s (20-200 keV, 1-s integration 
time) and a fluence in the same energy range of about 1e-5 erg/cm2,

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


GRB_name: GRB120514A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13301
SUBJECT: GRB 120514A : Suzaku WAM observation of the prompt emission
DATE:    12/05/21 03:08:04 GMT
FROM:    Norisuke Ohmori at Miyazaki U  <ohmori@astro.miyazaki-u.ac.jp>

M. Akiyama, N. Ohmori,  M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, Y. E. Nakagawa (Waseda U.),
W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, 
S. Kobayashi, A. Sakamoto, H. Ueno (Saitama U.), 
Y. Hanabata,  T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, 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 120514A (Swift/BAT trigger #522197 ; Siegel et al., GCN
13289) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 01:12:43.252 UT (=T0).

The observed light curve shows a single peak starting at T0-2 s, ending
at T0+16 s, with a duration (T90) of about 14 seconds. The fluence in 100
- 1000 keV was 1.62(-0.69, +0.50) x 10^-6 erg/cm^2. The 1-s peak flux 
measured from T0 s was 0.71(-0.20, +0.18) photons/cm^2/s in the same 
energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s to
T0+16 s is well fitted by a single power-law with a photon index of 2.30
(-0.54, 0.75) (chi^2/d.o.f = 43.1/32).

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

The light curves for this burst are now available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB120521A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13302
SUBJECT: GRB 120521A: Swift detection of a short burst
DATE:    12/05/21 06:12:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. M. Chester (PSU), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
B. Gendre (ASDC), D. M. Palmer (LANL) and G. Stratta (ASDC) report on
behalf of the Swift Team:

At 05:59:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120521A (trigger=522578).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 148.693, -49.419 which is 
   RA(J2000) = 09h 54m 46s
   Dec(J2000) = -49d 25' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single short FRED
structure with a duration of about 0.7 sec.  The peak count rate
was ~5000 counts/sec (15-350 keV), at ~0.25 sec after the trigger. 

The XRT began observing the field at 06:00:56.6 UT, 73.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 148.72544, -49.41760 which
is equivalent to:
   RA(J2000)  = 09h 54m 54.11s
   Dec(J2000) = -49d 25' 03.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 76 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 2.08
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 77 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain extinction expected. 


GRB_name: GRB120521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13303
SUBJECT: GRB 120521A: TAROT La Silla observatory optical observations
DATE:    12/05/21 06:34:10 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 120521A detected by SWIFT
(trigger 522578) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 35.2s after the GRB trigger
(15.1s after the notice). The elevation of the field decreased from
10 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 in the XRT position (Chester et al.
GCNC 13302) with a limiting magnitude of:
t0+35.2s to t0+95.2s : R > 15.8

The second image is 30.0s exposure in tracking mode:
t0+108.9s to t0+138.9s : R > 16.5

We co-added a series of exposures:
t0+109s to t0+533s : R > 17.4

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


GRB_name: GRB120521A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13304
SUBJECT: GRB 120521A: Enhanced Swift-XRT position
DATE:    12/05/21 09:01:33 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 508 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120521A, 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 = 148.72462, -49.41733 which is equivalent
to:

RA (J2000): 09h 54m 53.91s
Dec (J2000): -49d 25' 02.4"

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

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

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


GRB_name: GRB120521B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13305
SUBJECT: GRB 120521B: Swift detection of a burst
DATE:    12/05/21 09:24:51 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
B. Gendre (ASDC), D. M. Palmer (LANL),
E. Sonbas (NASA/GSFC/Adiyaman Univ.) and G. Stratta (ASDC) report on
behalf of the Swift Team:

At 09:07:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120521B (trigger=522586).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 197.014, -52.746 which is 
   RA(J2000)  =  13h 08m 03s
   Dec(J2000) = -52d 44' 45"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple overlapping peaks
with a duration of about 40 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 09:09:47.6 UT, 118.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
197.0100, -52.7548 which is equivalent to:
   RA(J2000)  = 13h 08m 02.41s
   Dec(J2000) = -52d 45' 17.4"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 32 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.27 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.2
(+1.94/-1.36) x 10^22 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.42e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 127 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
0.45. 

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


GRB_name: GRB120521B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13306
SUBJECT: GRB 120521B: TAROT La Silla observatory optical observations
DATE:    12/05/21 10:00:12 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

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

We imaged the field of GRB 120521B detected by SWIFT
(trigger 522586) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 88.8s after the GRB trigger
(25.6s after the notice). The elevation of the field decreased from
12 degrees above horizon and weather conditions
were poor.

In a clean exposure, taken between T0 + 473.1s and T0 + 563.1s,
we do not detect any afterglow with a limiting magnitude of R > 17.2.


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

N.B. Galactic coordinates are lon=305.4846 lat=+10.0434
and the galactic extinction in R band is 1.2 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.

----------------------------------------------------------------
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GRB_name: GRB120521B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13307
SUBJECT: GRB120521B: Faulkes Telescope South observations
DATE:    12/05/21 10:35:22 GMT
FROM:    David Bersier at Liverpool John Moores U  <dfb@astro.livjm.ac.uk>

D Bersier, C. Guidorzi, A. Melandri, J. Jalpelj report:

The Faulkes Telescope South robotically observed GRB120521B (Swift trigger 
522586, Cumming et al, GCN 13305). The first exposure started approximately 240 
seconds after the trigger time.
Digital image subtraction does not reveal any variable source inside the XRT 
error circle. We find upper limits in R ~ 22.0 (40 minutes after the burst).

[GCN OPS NOTE(21may12): Corrected per Circular 13308.]


GRB_name: GRB120521B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13308
SUBJECT: Correction to GCN 13307  (GRB120521B)
DATE:    12/05/21 10:47:47 GMT
FROM:    David Bersier at Liverpool John Moores U  <dfb@astro.livjm.ac.uk>

D. Bersier wishes to apologise for any confusion related to the wrong title of 
GCN  13307. The GCN Circular reports observations of GRB120521B, not GRB120521A. 
The title should read: "GRB120521B: Faulkes Telescope South observations".

I thank C. Guidorzi for drawing my attention to this mistake.


GRB_name: GRB120521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13310
SUBJECT: GRB 120521A: Swift-BAT refined analysis
DATE:    12/05/21 11:37:22 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),
M. M. Chester (PSU), 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+363 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120521A (trigger #522578)
(Chester, et al., GCN Circ. 13302).  The BAT ground-calculated position is
RA, Dec = 148.692, -49.422 deg, which is 
   RA(J2000)  =  09h 54m 46.1s 
   Dec(J2000) = -49d 25' 17.8" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows FRED pulse starting at ~T+0.0, peaking
at ~T+0.1, and ending at ~T+1.0 sec.  T90 (15-350 keV) is 0.45 +- 0.08 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+0.02 to T+0.56 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.98 +- 0.22.  The fluence in the 15-150 keV band is 7.8 +- 1.1 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.21 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/522578/BA/


GRB_name: GRB120521B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13311
SUBJECT: GRB 120521B: Enhanced Swift-XRT position
DATE:    12/05/21 12:07:59 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 809 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120521B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 197.00990, -52.75479 which is equivalent
to:

RA (J2000): 13h 08m 2.38s
Dec (J2000): -52d 45' 17.2"

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: GRB120521A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13312
SUBJECT: GRB 120521A: Swift/UVOT Upper Limits
DATE:    12/05/21 14:05:01 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120521A
77 s after the BAT trigger (Chester et al., GCN Circ. 13302).
No optical afterglow consistent with the XRT position
(Goad et al., GCN Circ. 13304) 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            77          227          147         >21.4
u_FC               289          539          246         >20.9
white               77         5491          363         >21.9
v                 4266         5901          393         >19.7
b                  545        11343          766         >21.9
u                  289        10775         1386         >21.6
w1                4676         6312          393         >20.4
m2                4470         6106          393         >20.6
w2                4061         5697          393         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.43 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120519A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13313
SUBJECT: IPN Triangulation of GRB 120519A (short/hard)
DATE:    12/05/21 15:23:28 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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,

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,

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

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

The short-duration, hard GRB 120519A has been observed by Fermi (GBM 
trigger 359140696), Konus-Wind, Swift (BAT),  MESSENGER (GRNS), INTEGRAL 
(SPI-ACS), Suzaku (WAM), and AGILE (MCAL), so far, at about 62295 s UT 
(17:18:15). The burst was outside the coded field of
view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   178.366 (11h 53m 28s) +22.407 (+22d 24' 24")
  Corners:
   179.899 (11h 59m 36s) +24.184 (+24d 11' 02")
   178.690 (11h 54m 46s) +23.008 (+23d 00' 31")
   176.909 (11h 47m 38s) +20.581 (+20d 34' 53")
   178.049 (11h 52m 12s) +21.803 (+21d 48' 09")
  ---------------------------------------------
The error box area is 0.60 sq. deg, and its maximum
dimension is 4.5 deg.

This box may be improved.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120519_T62298/IPN/


GRB_name: GRB120519A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13315
SUBJECT: Konus-Wind observation of GRB 120519A
DATE:    12/05/21 16:04:56 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 GRB 120519A
(IPN localization: Golenetskii at al., GCN 13313)
triggered Konus-Wind at T0=62298.004s UT (17:18:18.004)

The light curve shows a series of overlapping pulses
with a total duration of ~1.2 s.
The emission is seen up to ~7.5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120519_T62298/

As observed by Konus-Wind the burst
had a fluence of 3.7(-1.1,+1.5)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0,
of 1.3(-0.4,+0.5)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 well fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.5 (-0.3, +0.3),
and Ep = 740(-240, +450) keV,
chi2 = 22.9/22 dof.

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


GRB_name: GRB120521B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13316
SUBJECT: GRB 120521B: Swift-XRT refined Analysis
DATE:    12/05/21 21:25:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. D'Avanzo (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), V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA)
and J.R. Cummings report on behalf of the Swift-XRT team:

We have analysed 9.1 ks of XRT data for GRB 120521B (Cummings  et al.
GCN Circ. 13305), from 125 s to 19.4 ks after the  BAT trigger. The
data comprise 28 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 13311).

The light curve can be modelled with an initial power-law decay with an
index of alpha=5.0 (+0.7, -0.6), followed by a break at T+267 s to an
alpha of 0.69 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.4, -0.3). The
best-fitting absorption column is  1.5 (+0.4, -0.3) x 10^22 cm^-2, in
excess of the Galactic value of 2.3 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 6.6 x 10^-11 (1.4 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+0.4, -0.3) x 10^22 cm^-2
Galactic foreground: 2.3 x 10^21 cm^-2
Excess significance: 6.2 sigma
Photon index:      1.9 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00522586.

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


GRB_name: GRB120521B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13317
SUBJECT: GRB 120521B: Swift-BAT refined analysis
DATE:    12/05/21 22:48:55 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)
(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 120521B (trigger #522586)
(Cummngs, et al., GCN Circ. 13305).  The BAT ground-calculated position is
RA, Dec = 197.016, -52.742 deg, which is 
   RA(J2000)  =  13h 08m 03.9s 
   Dec(J2000) = -52d 44' 31.9" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-1 sec, with equal-amplitude maximum peaks at ~T+6 and ~T+32 sec,
and ending at around T+180 sec.  There is a possibility (at the 2-sigma level)
that emission continues out past the T+243sec end of the downlinked data.
T90 (15-350 keV) is 31.4 +- 4.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.39 to T+35.58 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.97 +- 0.15.  The fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+31.04 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/522586/BA/


GRB_name: GRB120521C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13318
SUBJECT: GRB 120521C: Swift detection of a burst
DATE:    12/05/21 23:46:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
V. D'Elia (ASDC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and G. Stratta (ASDC)
report on behalf of the Swift Team:

At 23:22:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120521C (trigger=522656).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 214.290, +42.123 which is 
   RA(J2000) = 14h 17m 09s
   Dec(J2000) = +42d 07' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single FRED
structure with a duration of about 20 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 23:23:16.8 UT, 69.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 214.28671, 42.14311 which
is equivalent to:
   RA(J2000)  = 14h 17m 08.81s
   Dec(J2000) = +42d 08' 35.2"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 72 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.05
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 7.43e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 76 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 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. 
Results from the list of sources generated on-board are not available at this
time. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.01. 

Burst Advocate for this burst is W. H. Baumgartner (wayne 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: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13319
SUBJECT: GRB 120521C: TAROT Calern observatory optical observations
DATE:    12/05/22 00:18:05 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 120521C detected by SWIFT
(trigger 522656) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 23 min after the GRB trigger.
The elevation of the field decreased from
68 degrees above horizon but humidity was higher
than 93% until 23 min after the trigger preventing
the record of the beginning of the event.

We co-added a series of exposures.
No OT was found in the XRT error box (Baumgartner
et al. GCNC 13318).

start   stop
23min   37min   R > 19.4

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

This message may be cited.


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13320
SUBJECT: GRB120521C: Liverpool Telescope observations
DATE:    12/05/22 00:45:25 GMT
FROM:    David Bersier at Liverpool John Moores U  <dfb@astro.livjm.ac.uk>

David Bersier (LJMU) reports on behalf of the Liverpol GRB collaboration:

The Liverpool Telescope responded automatically to Swift trigger 522656
(Baumgartner et al, GCN 13318) 11 minutes after the trigger.

We do not detect any variable source inside the XRT error circle. A
representative upper limit is R=21.5 at 35 minutes after the burst,
calibrated with respect to USNO-B.


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13321
SUBJECT: GRB 120521C - NOT optical limits
DATE:    12/05/22 00:56:05 GMT
FROM:    Annalisa De Cia at U of Iceland  <annalisa@raunvis.hi.is>

A. De Cia (U. of Iceland), A. Sandberg (Oskar Klein Centre), J.Hjorth (DARK), N.R. Tanvir (U. of Leicester) and P. Jakobsson (U. of Iceland) report:

We observed the field of GRB 120521C (Baumgartner et al., GCN 13318) with the NOT equipped with MOSCA in the Sloan r and i filters for 10 minutes, starting at 0:09 UT (47 min after the GRB trigger).

No significant source was detected at the burst position, down to r > 23.6 mag, calibrated against SDSS stars.


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13322
SUBJECT: GRB 120521C: WHT optical observations
DATE:    12/05/22 01:20:38 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester), M. Hrudkova (ING) report for a larger collaboration:

"We obtained observations of GRB 120521C (Baumgartner et al. GCN 13318) with the William Herschel Telescope equipped with ACAM in the r and z-bands. Our observations started at 00:01UT, 39 minutes after the burst trigger. We do not detect any afterglow candidates within the XRT error circle. Provisional limits, calibrated against SDSS suggest r>24.0, z>22.5"


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13323
SUBJECT: GRB 120521C: BOOTES-1 optical observations
DATE:    12/05/22 01:53:37 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

M. Jelinek (IAA-CSIC), P. Kubanek (IP AS CR), A.J. Castro-Tirado
(IAA-CSIC), J. Gorosabel (IAA-CSIC), report on behalf of a larger
collaboration:

"The 0.3-m robotic telescope at the BOOTES-1 station in south Spain
(INTA-CEDEA) responded automatically to GRB 120521C (Baumgartner et al.,
GCN Circ. 13318), performing clear-band observations on May 21.98180 --
21.98863 UT (11.7 -- 21.5 minutes post burst). No object is detected
within the XRT circle down to R~20.5"


GRB_name: GRB120521C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13324
SUBJECT: GRB 120521C: Enhanced Swift-XRT position
DATE:    12/05/22 05:33:54 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 2020 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120521C, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 214.28648, +42.14467 which is equivalent
to:

RA (J2000): 14h 17m 8.76s
Dec (J2000): +42d 08' 40.8"

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: GRB120521C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13325
SUBJECT: GRB 120521C: PAIRITEL NIR Upper Limits
DATE:    12/05/22 05:44:37 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 120521C (Baumgartner et al., GCN 13318)
with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations
began at 2012-May-22 03h52m27s UT, ~4.5 hours after the Swift trigger.
 In  mosaics (effective exposure time of 1568 s) taken simultaneously
in the J, H, and Ks filters, we do not detect any source within the
enhanced XRT error circle (Beardmore et al. GCN 13324).

post burst
t_mid (hr) exp.(hr) filt  U. Limit (3 sig)
4.99      0.44     J     > 18.5
4.99      0.44     H     > 17.6
4.99      0.44     Ks    > 16.0

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


GRB_name: GRB120521A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13326
SUBJECT: GRB 120521A: Swift-XRT refined Analysis
DATE:    12/05/22 07:15:00 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), V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA), V. Mangano
(INAF-IASFPA) and M.M. Chester report on behalf of the Swift-XRT team:

We have analysed 4.3 ks of XRT data for GRB 120521A (Chester  et al.
GCN Circ. 13302), from 83 s to 11.3 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN. Circ 13304).

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

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.36, -0.29). The
best-fitting absorption column is  2.6 (+1.4, -0.5) x 10^21 cm^-2,
consistent with the Galactic value of 2.1 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.6 x 10^-11 (6.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.6 (+1.4, -0.5) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.81 (+0.36, -0.29)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00522578.

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


GRB_name: GRB120521A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13327
SUBJECT: GRB 120521A: XRT light curve (Correction to GCN 13326)
DATE:    12/05/22 07:22:33 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:

There was an error in GCN 13326: the light curve decay slope was
reported as infinity.

The XRT light curve in fact shows a plateau (alpha=0.2 +/-0.4) until
T0+270 seconds. After this it undergoes an extremely sharp decay
(alpha~10) and is not detected in X-rays after T0+1ks.


GRB_name: GRB120521B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13328
SUBJECT: GRB 120521B: GROND Upper limits
DATE:    12/05/22 08:24:45 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

A. Rossi (TLS Tautenburg), M. Nardini (Universita'degli Studi 
Milano-Bicocca), S. Klose (TLS Tautenburg), and J. Greiner (MPE Garching) 
report on behalf of the GROND team:

We observed the field of GRB 120521B (Swift trigger 522586; Cummings et 
al., GCN 13305) 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 00:35 UT on 2012-05-22, 15.3 h after the GRB 
trigger, and lasted for 140 minutes. They were performed with good sky 
conditions at an average seeing of 0.8" and at an average airmass of 1.05. 
(At the time of the GRB trigger the field was already too close to the 
telescope's horizon distance limit in order to observe it with GROND.)

Based on an exposure of 37 minutes in the optical and 30 minutes in the 
NIR we do not detect any source within the Swift-XRT error circle reported 
by Osborne et al. (GCN 13311). Preliminary observed upper limits (AB mags) 
are:

  g' > 24.5
  r' > 24.2
  i' > 23.9
  z' > 23.9
  J  > 21.3
  H  > 20.3
  Ks > 19.3.

These limits are derived based on GROND zeropoints (g'r'i'z') and 2MASS 
stars (JHK). We note that the Galactic reddening along the line of sight 
is E_(B-V)= 0.45 mag (Schlegel et al. 1998).


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13329
SUBJECT: GRB 120521C: MASTER optical limit 
DATE:    12/05/22 09:26:17 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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  GRB120521C  60 sec  after notice 
time and 715 sec after GRB time at 2012-05-21 23:34:03 UT in two 
polarizations. We haven't found optical 
transient  within Swift BAT error-box (Baumgartner et al., GCN 13318) .
  The 5-sigma upper limit has been about 20.0 mag for mean time after 
trigger 1492s (total exposition 1370s).

The direct copy from MASTER DataBase is:

Pro.type   Date      time      Exp.time Limit  Filt. Tube.

Alert  2012-05-21 23:34:03 130 17.7 P| EAST
Alert  2012-05-21 23:34:03 130 18.2 P- WEST
Alert  2012-05-21 23:34:03 130 18.2 P- WEST
Alert  2012-05-21 23:36:45 160 18.6 P- WEST
Alert  2012-05-21 23:36:45 160 18.1 P| EAST
Alert  2012-05-21 23:39:48 180 18.9 P- WEST
Alert  2012-05-21 23:39:48 180 18.4 P| EAST
Alert  2012-05-21 23:43:13 180 18.4 P| EAST
Alert  2012-05-21 23:43:13 180 19.0 P- WEST
Alert  2012-05-21 23:46:37 180 18.3 P| EAST
Alert  2012-05-21 23:46:38 180 18.4 P- WEST
Alert  2012-05-21 23:50:02 180 18.4 P| EAST
Alert  2012-05-21 23:50:02 180 19.1 P- WEST
Alert  2012-05-21 23:53:27 180 18.4 P| EAST
Alert  2012-05-21 23:53:27 180 19.1 P- WEST
Alert  2012-05-21 23:56:57 180 18.4 P| EAST
Alert  2012-05-21 23:56:57 180 19.0 P- WEST 
AddWest 2012-05-21 23:34:03    1370     20.0    P-      WEST

The message may be cited.


GRB_name: GRB120521B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13330
SUBJECT: GRB 120521B: Swift/UVOT Upper Limits
DATE:    12/05/22 10:59:58 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120521B
127 s after the BAT trigger (Cummings et al., GCN Circ. 13305).
No optical afterglow consistent with the XRT position (Osborne et al., GCN Circ. 13311)
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           127          277          147         >19.4
u_FC               286          535          246         >19.4
white              127        30912         2930         >19.8
v                  615        23584         2045         >18.7
b                  541        36686         2819         >19.7
u                  286        36128         2526         >20.2
w1                 665        35215         2046         >20.7
m2                5582        24489         1279         >21.0
w2                 765        19363         1746         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.45 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120521C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13331
SUBJECT: GRB 120521C: Swift/UVOT Upper Limits
DATE:    12/05/22 11:01:12 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and W. H. Baumgartner (GSFC/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120521C
77 s after the BAT trigger (Baumgartner et al., GCN Circ. 13318).
No optical afterglow consistent with the XRT position
(Beardmore et al., GCN Circ. 13324)
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            77          227          147         >20.9
u_FC               289          539          246         >20.4
white               77         2226          470         >21.7
v                  621         2276          194         >19.8
b                  546         2201          156         >20.4
u                  289         2177          343         >20.7
w1                 670         2325          194         >20.4
m2                 645         2128          136         >19.9
w2                 596         2251          156         >20.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120521C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13332
SUBJECT: GRB 120521C: Keck Observations 
DATE:    12/05/22 12:59:03 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), O. Yaron (Weizmann), Y. Cao, and S. R. Kulkarni
(Caltech) report:

We observed the position of GRB 120521C (Baumgartner et al., GCN 13318)
with the Keck I 10m telescope (+LRIS) starting at 10:39 UT on 2012-05-22.
We acquired a total of 1200s of imaging in I-band and 1360s in g-band.
Seeing conditions were relatively poor (1.5").

At the position of the enhanced XRT error circle (Beardmore et al., GCN
13324) we clearly identify a extended source in both the g-band and I-band
images.  It appears to consist of at least two components; a red source at
the southern edge of the XRT error circle and a bluer source at the
western edge of the error circle.  The relation of these sources to each
other and to GRB 120521C is not yet clear, but they could represent a
host-galaxy merger system, an afterglow superposed on a host, or two
unrelated galaxies at different redshifts.

The early nondetections of an afterglow (e.g. Klotz et al., GCN 13319;
Bersier et al., GCN 13320; De Cia et al., GCN 13321;
Levan et al., GCN 13322; Jelinek et al., GCN 13323; Morgan et al.,
GCN 13325; Gorbovskoy et al., GCN 13329; Oates et al., GCN 13331) are
characteristic of a dark burst.  Further observations of this event (in
particular in the NIR) are encouraged.

An image of the field is posted to:
http://www.astro.caltech.edu/~dperley/gcn/120521c/120521c.png 


GRB_name: GRB120521C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13333
SUBJECT: GRB 120521C: Swift-BAT refined analysis
DATE:    12/05/22 13:27:34 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)
(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 120521C (trigger #522656)
(Baumgartner, et al., GCN Circ. 13318).  The BAT ground-calculated position is
RA, Dec = 214.288, 42.144 deg, which is 
   RA(J2000)  =  14h 17m 09.1s 
   Dec(J2000) = +42d 08' 39.8" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.
 
The mask-weighted light curves shows a FRED peak starting at ~T-2 sec,
peaking at ~T+1 sec, abd ending at ~T+40 sec.  T90 (15-350 keV) is
26.7 +- 4.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.03 to T+31.84 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.73 +- 0.11.  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-0.02 sec in the 15-150 keV band
is 1.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/522656/BA/


GRB_name: GRB120521C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13334
SUBJECT: GRB 120521C: Swift-XRT refined Analysis
DATE:    12/05/22 13:46:05 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), A. Maselli 
(INAF-IASFPA), V. Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), J.A.
Kennea (PSU) and W.H. Baumgartner report on behalf of the Swift-XRT
team:

We have analysed 7.2 ks of XRT data for GRB 120521C (Baumgartner  et
al. GCN Circ. 13318), from 59 s to 29.2 ks after the  BAT trigger. The
data comprise 101 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
Beardmore et al. (GCN. Circ 13324).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.78 (+0.19, -0.17), followed by a break at T+489 s to
an alpha of 0.51 (+0.11, -0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+0.25, -0.16). The
best-fitting absorption column is  consistent with the Galactic value
of 1.0 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 3.9 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+4.2, -0) x 10^20 cm^-2
Galactic foreground: 1.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.78 (+0.25, -0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00522656.

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


GRB_name: GRB120521A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13335
SUBJECT: GRB 120521A: GROND Upper limits
DATE:    12/05/22 17:11:33 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

A. Rossi (TLS Tautenburg), M. Nardini (Universita' degli Studi
Milano-Bicocca), S. Klose (TLS Tautenburg), and J. Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 120521A (Swift trigger 522578; Chester
et al., GCN 13302) 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 22:53 UT on 2012-05-21, 16.9 h after the GRB
  trigger, and lasted for 100 minutes.  They were performed under good
  sky conditions at an average seeing of 0.9 and at an average airmass
  of 1.1.

Using an exposure of 50 minutes in the optical and 40 minutes in the
NIR we do not detect any source within the Swift-XRT error circle
reported by Goad et al. (GCN 13304).  Preliminary observed upper
limits (AB mags) are:

g' > 25.5
r' > 25.0
i' > 24.0
z' > 23.7
J > 20.9
H > 20.3
K > 19.1

The given limits are derived based on calibrating the images against
GROND zeropoints (g'r'i'z') and 2MASS stars (JHK).  We note that the
Galactic reddening along the line of sight is E_(B-V)= 0.43 mag
(Schlegel et al. 1998).


GRB_name: GRB120521C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13336
SUBJECT: GRB 120521C: EVLA 22 GHz Upper Limit
DATE:    12/05/22 21:57:19 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

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

"We observed the position of GRB 120521C (GCN 13318) beginning 2012 May
22.12 (3.6 hours after the burst) with the EVLA.  At a mean frequency of 
21.8 GHz, we find no significant radio emission within the refined 
Swift-XRT error circle (GCN 13324) to a 3-sigma limit of ~50 uJy."


GRB_name: GRB120521C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13337
SUBJECT: GRB 120521C: Early Tautenburg limits
DATE:    12/05/22 22:17:24 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, B. Stecklum and U. Laux (TLS Tautenburg) report:

We observed to position of Swift GRB 120521C (Trigger 522656, Baumgartner
et al., GCN 13318) with the TLS 1.34m Schmidt telescope. Conditions were
mediocre, with good seeing but bad transparency. Observations were
triggered manually and began 28 minutes after the trigger (17 minutes
after the alert). We obtained 5 x 60 s images in Rc, 4 x 180 s images also
in Rc, and 1 x 600 s each in Z and Ic. The Ic image is affected in depth
by passing clouds.

At the position of the enhanced X-ray afterglow (Beardmore et al., GCN
13324), we do not detect any source, in agreement with earlier results
(Klotz et al., GCN 13319; Bersier et al., GCN 13320; De Cia et al., GCN
13321; Levan et al., GCN 13322; Jelinek et al., GCN 13323; Morgan et al.,
GCN 13325; Gorbovskoy et al., GCN 13329; Oates et al., GCN 13331). The
possible host galaxy (Perley et al., GCN 13332) is not detected.

We us the SDSS star at RA, Dec. (J2000) = 14:17:02.836, +42:6:07.62
(214.26181759, 42.10211787, catalog ID 1237661874023500000) as a
comparison star. Using the transformations of Lupton (2005), we find Rc =
18.33, Ic = 17.93 and Z = 17.78 for this star.

We find the following 2 sigma limiting magnitudes:

Time (days) Exposure (s) Filter UL
0.019827 1 x 60  Rc 21.0
0.022275 5 x 60  Rc 21.8
0.027171 1 x 180  Rc 21.5
0.030760 4 x 180  Rc 22.5
0.040247 1 x 600  Z 20.2
0.048757 1 x 600  Ic 19.3

We note that while the non-detections we as well as other telescopes have
found point to this being a dark GRB, the X-ray absorption seen by Swift
is small. The Keck detection of a possible host galaxy in g' band likely
rules out a high-z interpretation, though.

No further observations are planned.

This message may be cited.


GRB_name: GRB120521A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13338
SUBJECT: GRB 120521A: ATCA 34GHz upper limit
DATE:    12/05/23 01:44:01 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 (Dark Cosmology / IAA)

We observed GRB120521A (GCN13302) with the Australia Telescope Compact 
Array at 34GHz for 112 mins centered on 07:55UT May 22 2012 (T0+1.08days).

We detect no radio source at the location of the GRB (GCN13304) and 
place a 3sigma upper limit of 95uJy on the flux of an afterglow.

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: GRB120521B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13339
SUBJECT: GRB 120521B: Fermi GBM observation
DATE:    12/05/23 09:16:58 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team:

"At 09:07:52.39 UT on 21 May 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120521B (trigger 359284074 / 120521380).
which was also detected by the Swift/BAT
(Krimm et al. 2012, GCN 13317)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 84 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 91 s (50-300 keV).
The time-averaged spectrum from T0-5 s to T0+29 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.34 +/- 0.20 and
the cutoff energy, parameterized as Epeak, is 213 +/- 29 keV

The event fluence (10-1000 keV) over the T90 time interval is
(3.11 +/- 0.07)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.4 s in the 10-1000 keV band
is 1.55 +/- 0.23 ph/s/cm^2.

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


GRB_name: GRB120522A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13340
SUBJECT: IPN triangulation of GRB 120522A (long/intense)
DATE:    12/05/23 14:09:17 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, report:

The long-duration, bright GRB 120522A has been observed by Konus-Wind, 
MESSENGER (GRNS), and Mars Odyssey (HEND), so far, at about 11467 s UT 
(03:11:07).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   165.996 (11h 03m 59s) -62.094 (-62d 05' 37")
  Corners:
   165.772 (11h 03m 05s) -61.976 (-61d 58' 35")
   165.879 (11h 03m 31s) -62.218 (-62d 13' 06")
   166.222 (11h 04m 53s) -62.211 (-62d 12' 38")
   166.112 (11h 04m 27s) -61.969 (-61d 58' 08")
  ---------------------------------------------
The error box area is 141 sq. arcmin, and its maximum
dimension is 19 arcmin. The Sun distance is ~116 deg.

This box may be improved.

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


GRB_name: GRB120522A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13341
SUBJECT: Konus-Wind observation of GRB 120522A
DATE:    12/05/23 14:14:54 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 GRB 120522A (IPN localization: Hurley at al., GCN 13340)
triggered Konus-Wind at T0=11467.377s UT (03:11:07.377)

The light curve shows multiple partly overlapped pulses.
A total duration of the burst is ~13 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/GRB120522_T11467/

As observed by Konus-Wind the burst
had a fluence of 2.5(-0.2,+0.2)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+6.528 s,
of 9.3(-0.9,+0.9)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+78.086 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.88 (-0.05, +0.05),
and Ep = 381(-33, +40) keV,
chi2 = 100.1/84 dof.

The spectrum at the maximum count rate
(measured from T0+0.256 to T0+7.168 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.79 (-0.05, +0.05),
and Ep = 379(-32, +37) keV,
chi2 = 89.5/84 dof.

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


GRB_name: GRB120521B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13342
SUBJECT: GRB120521B: SSO 2.3m upper limits
DATE:    12/05/24 09:31:38 GMT
FROM:    Sharon Rapoport at The ANU  <rapoport@mso.anu.edu.au>

S. Rapoport, S. Sweet, J. Scharwachter, B. Schmidt, M. Childress

report observations of GRB120521B taken on 2012-05-21.42 UTC (2.7
hours post-alert) using the Wide Field Spectrograph (WiFeS) on the ANU
2.3m, obtaining 3x900s integration at resolution R=3000.  

Spectral summation of the sky-subtracted data cube in a 3" radius centered at
the GRB location shows no detectable optical counterpart to the GRB
and no detectable host galaxy. Based on measurement of a nearby field
star in the data cube (m_B=18.4, m_R=17.2 -- USNO) we estimate a
non-detection upper limit of m_R=20.5 and m_B=20.0 at 5 sigma for the
GRB or its host galaxy.


GRB_name: GRB120521C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13343
SUBJECT: GRB 120521C: EVLA 22 GHz Detection
DATE:    12/05/25 15:16:06 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

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

"We re-observed the position of GRB 120521C (GCN 13318) on 2012 May 
23.12 UT (1.15 d after the burst) with the EVLA at 21.8 GHz.   Within 
the enhanced Swift-XRT error circle (GCN 13324) we detect a brightening 
radio source with a flux density that is about a factor of two above our 
early 3-sigma limit of 50 uJy (GCN 13336).  We conclude that this is the 
radio afterglow of GRB 120521C.  Follow-up observations at multiple 
frequencies are in progress."


GRB_name: GRB120521C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13344
SUBJECT: GRB 120521C: EVLA Localization of Afterglow
DATE:    12/05/25 21:39:06 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger and T. Laskar (Harvard) report on behalf of a 
larger collaboration:

"Further to GCN 13343, we note that the EVLA 21.8 GHz brightening source 
within the XRT enhanced error circle of GRB 120521C (GCNs 13318, 13324) 
is located at (J2000):

RA:   14:17:08.802 (+/- 0.002)
Dec: +42:08:41.22  (+/- 0.02).

This position appears to be offset from the two galaxies at the edge of 
the Swift-XRT error circle based on the image provided by Perley et al. 
in GCN 13332."


GRB_name: GRB120512A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13345
SUBJECT: GRB 120512A: Suzaku WAM observation of the prompt emission
DATE:    12/05/29 01:37:55 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

A. Sakamoto, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara,
M. Asahina, S. Kobayashi, H. Ueno (Saitama U.),
M. Akiyama, N. Ohmori,  M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, Y. E. Nakagawa (Waseda U.),
Y. Hanabata,  T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, 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 120512A (INTEGRAL/IBIS; Mereghetti et al., GCN 13300)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an 
energy range of 50 keV - 5 MeV at 02:41:43.783 UT (=T0).
The observed light curve shows  a multi-peaked structure starting at 
T0+4 s, ending at T0+24 s,  with a duration (T90) of about 20 seconds. 
The fluence in 100 - 1000 keV was 9.33(-1.13 +0.27) x 10^-6 erg/cm^2. 
The 1-s peak flux measured from T0+9.5s was 2.81(-0.56 +0.26) 
photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from T0+4s to 
T0+24s is well fitted by a power-law with exponential cutoff model:
   dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha       1.05(-0.47 +0.39), and
   Epeak       508.5(-72.2 +114.3) keV (chi^2/d.o.f. = 13.74/24).
We also shows the results with the same spectrum fitted by a GRB Band
model fixing beta of 2.5,ã€€the low-energy photon index alpha: 
-1.03(-0.47 +0.78),ã€€and the peak energy Epeak: 470.5(-85.4 +136.2) keV 
(chi^2/d.o.f = 17.86/24).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
The light curves for this burst are available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB120528B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13346
SUBJECT: GRB 120528B: MAXI/GSC detection
DATE:    12/05/29 01:41:48 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

M. Morii, N. Kawai, R. Usui, K. Ishikawa (Tokyo Tech),
M. Serino, T. Mihara, M. Sugizaki, T. Yamamoto,
M. Matsuoka (RIKEN),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa (JAXA),
H. Negoro, M. Nakajima, N. Serita, M. Asada, H. Sakakibara (Nihon U.),
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka 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.),
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

MAXI/GSC triggered at 2012-05-28T18:12:08 UT on a bright uncatalogued
X-ray transient source.
The transient emission lasted at least for 20.0 seconds
within the 40.0 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 120528B.

Assuming that the source flux was constant over the transit,
we obtain the source position at

(R.A., Dec) = (+77.59 deg, -37.80 deg) = (05 10 21, -37 47 50)(J2000)

with a rectangular statistical error box (90%C.L.) of the following corners:

(R.A., Dec) = (+77.23 deg, -37.92 deg) = (05 08 56, -37 54 60)(J2000)
(R.A., Dec) = (+77.56 deg, -38.12 deg) = (05 10 16, -38 07 15)(J2000)
(R.A., Dec) = (+77.96 deg, -37.71 deg) = (05 11 51, -37 42 47)(J2000)
(R.A., Dec) = (+77.63 deg, -37.51 deg) = (05 10 31, -37 30 36)(J2000)

There is an additional systematic uncertainty of 0.1 deg (90%
containment radius).

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

(R.A., Dec) = (+76.80 deg, -37.54 deg) = (05 07 12, -37 32 34)(J2000)
(R.A., Dec) = (+77.09 deg, -37.25 deg) = (05 08 21, -37 15 0)(J2000)
(R.A., Dec) = (+78.38 deg, -38.05 deg) = (05 13 31, -38 02 57)(J2000)
(R.A., Dec) = (+78.09 deg, -38.35 deg) = (05 12 22, -38 20 42)(J2000)

The X-ray flux averaged over the scan was 285 +65/-58 mCrab (4-10 keV,
1 sigma error).

Follow-up observations are encouraged.


GRB_name: GRB120521C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13348
SUBJECT: GRB 120521C redshift estimate
DATE:    12/05/29 22:22:31 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir, K. Wiersema (U. Leicester), A. J. Levan (U. Warwick),
A. Cucchiara (UCSC/UCO Lick), D. Perley (Caltech), P. Hirst (Gemini),
T. Carroll, T. Kerr, W. Varricatt (JACH), C. Farina, M. Hrudkova (ING), 
L. Ker (Edinburgh) report on behalf of a larger collaboration:

We have combined observations of GRB 120521C (Baumgartner et al. GCN
13318) made using the WHT (Levan et al., GCN 13322), Keck (Perley et al. GCN
13332), UKIRT and Gemini-N telescopes across the optical-IR region in r,i,z,J,H,K.

Analysis of further WHT z-band imaging, obtained at 01:54 UT, 2 hours
after our initial epoch (Levan et al. GCN 13322) shows a faint source
within the XRT error circle. This source is also seen at high confidence
in z-band imaging obtained with Gemini-N at 07:03 UT, and photometry 
shows that it brightened by 0.5 magnitudes over this period, suggesting 
it is the afterglow of GRB 120521C. This source is only very weakly visible in
contemporaneous I-band imaging obtained with Keck (Perley et al. GCN
13332), and this indicates a red colour i-z >2.3 . However, the source is not
detected in our initial reductions of the UKIRT WFCAM imaging in JHK,
suggesting that z-K < 1.3 (AB, corresponding to f(nu) ~ nu^-beta with
beta<1.3). This is indicative of a high-redshift, rather than a highly
reddened afterglow. We note that the position of the afterglow candidate
in our data matches the radio position reported by Zauderer et al (GCN 13344)
within our calibration uncertainty of ~0.3 arcseconds.

Gemini-North GMOS spectroscopy was obtained in poor conditions, using the
R400 grating centered at 8000 A, giving a wavelength range of
approximately 5850-10100 A. Observations (2 x 1800 s) started at 12:03 UT
on 23 May 2012. We used the GMOS Nod&Shuffle observing mode to improve
skyline subtraction.

In the resulting spectrum, a weak trace is seen at the expected location,
which is only detected redward of ~8700 A. The absence of any emission
bluewards of this wavelength is suggestive of a high redshift of this
source, z~6.0. The low signal of the trace precludes detection of
absorption lines.

Further analysis of the data is ongoing.


GRB_name: GRB120528C
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13349
SUBJECT: GRB 120528C: MAXI/GSC detection
DATE:    12/05/30 03:54:42 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

M. Morii (Tokyo Tech), H. Negoro (Nihon U.), M. Serino (RIKEN),
S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, K. Ishikawa (Tokyo Tech),
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka U.), 
M. Nakajima, M. Asada, H. Sakakibara, 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.), 
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

MAXI/GSC detected an uncatalogued X-ray transient source at the 4.4
sigma level in the 2-20 keV band. The maximum of the raw count rate in
the 2-20 keV band, before the correction of the triangular transit
response of MAXI/GSC, was observed around 2012-05-28T21:21:58. The
enhancement lasted at least 30 seconds before and after the maximum
within the about 40 seconds transit response.

Assuming that the source flux was constant over the transit, we obtain
the source position at 

(R.A., Dec) = (+12.93 deg, -0.95 deg) = (00 51 44, -00 57 18)(J2000) 

with a statistical 90% C.L. elliptical error region
with long and short radii of 0.8 deg and 0.6 deg, respectively.
The position angle of long axis is 0 deg.
There is an additional systematic uncertainty of 0.1 deg (90%
containment radius).

The preliminary flux of the transient source was 37 +- 16 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. A hard spectrum of the source suggests the
source was a GRB, but another possibility can not be excluded.

Follow-up observations are encouraged.


GRB_name: GRB120519A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13350
SUBJECT: GRB 120519A: Suzaku WAM observation of the prompt emission
DATE:    12/05/30 07:29:10 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

A. Sakamoto, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara,
M. Asahina, S. Kobayashi, H. Ueno (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 short GRB 120519A (IPN; Pal'shin et al., GCN 13313, Konus-Wind;
Golenetskii et al., GCN 13315) triggered the Suzaku Wide-band All-sky 
Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 
17:18:14.64 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-0.2 s, ending at T0+0.6 s, with a duration (T90) of about 0.72 
seconds. The fluence in 100 - 1000 keV was 1.45(-0.28 +0.09) x 10^-6 
erg/cm^2. The 1-s peak flux measured from T0-0.5s was 2.76(-0.33 +0.18) 
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-0.5s to
T0+0.5s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 0.41(-0.41 +0.58), and Epeak 736(-141 +226) keV
(chi^2/d.o.f. = 16.9/24).

In case we fit the same spectrum by a GRB Band model with a fixed
beta of 2.5, the best fit parameters and their errors are,
low-energy photon index alpha: -0.10(-0.92 +1.60),
and the peak energy Epeak: 611(-146 +279) keV (chi^2/d.o.f = 20.0/24).


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

----
The light curves for this burst are available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB120528B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13351
SUBJECT: Konus-Wind observation of GRB 120528B
DATE:    12/05/31 10:25:04 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 120528B (MAXI/GSC detection and localization:
M. Morii et al., GCN 13346) was detected by Konus-Wind
in the waiting mode starting at T0(KW)= 65508 s UT (18:11:48),
~20s before the T0(MAXI).

The burst light curve shows a single pulse with a total duration of ~30s.

As observed by Konus-Wind, the burst had a fluence
of (2.9  0.8)x10-6 erg/cm2 (in the 20 - 1200 keV energy range).

Modelling the K-W 3-channel time-integrated spectrum
(from T0(KW) to T0(KW)+26 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -0.41  1.22, and Ep = 201  112 keV

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB120528B/


GRB_name: GRB120603A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13353
SUBJECT: IPN Triangulation of short GRB 120603A
DATE:    12/06/04 17:59:15 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 NS 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

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 GRB 120603A has been observed by Fermi (GBM: trigger
360412331), INTEGRAL (SPI-ACS), Konus-Wind, Suzaku (WAM), and MESSENGER
(GRNS), so far, at about 37930 s UT (10:32:10).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    198.794 (13h 15m 11s)  +4.326 ( +4d 19' 35")
   Corners:
    197.693 (13h 10m 46s)  +2.527 ( +2d 31' 36")
    199.766 (13h 19m 04s)  +6.230 ( +6d 13' 49")
    199.927 (13h 19m 42s)  +6.103 ( +6d 06' 12")
    197.853 (13h 11m 25s)  +2.399 ( +2d 23' 56")
   ---------------------------------------------

The error box area is 0.857 sq. deg, and its maximum
dimension is 4.280 deg.

This box may be improved.

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


GRB_name: GRB120603A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13354
SUBJECT: Konus-Wind observation of GRB 120603A
DATE:    12/06/05 11:40:54 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 GRB 120603A
(IPN detection and localization: Golenetskii at al., GCN 13353)
triggered Konus-Wind at T0=37934.201s UT (10:32:14.201)

The light curve shows a single pulse with a total duration of ~0.3 s.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120603_T37934/

As observed by Konus-Wind the burst
had a fluence of (1.0  0.1)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.064,
of (6.2  1.1)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Since almost the whole of the emission is seen before the trigger,
no multichannel spectra are available for this burst.
Modelling the 3-channel time-integrated spectrum
(from T0-0.256 to T0) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields
alpha = -0.4  0.2, and Ep = 560  60 keV.

All the quoted errors are estimated at the 1 sigma confidence level.


GRB_name: GRB120603A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13356
SUBJECT: GRB 120603A: Suzaku WAM observation of the prompt emission
DATE:    12/06/06 08:15:54 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

T. Yasuda, M. S. Tashiro, Y. Terada, W. Iwakiri, K. Takahara,
M. Asahina, S. Kobayashi, A. Sakamoto, H. Ueno (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 IPN localized GRB 120603A (IPN; Golenetskii et al., GCN 13353,
Konus-Wind; Golenetskii et al., GCN 13354)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 2012-06-03 10:32:9.80 UT (=T0).

The observed light curve shows a single peak with a duration (T90) of 
about 0.19 seconds.
The fluence in 100 - 1000 keV was 5.49 (+1.15/-4.79) x10^-7 erg/cm^2.
The 1-s peak flux was 1.19 (+0.20/-0.94) photons/cm^2/s in the same
energy range.

Preliminary result shows that the time-averaged spectrum is well fitted 
by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.70 (+0.81/-1.17), and
Epeak       580 (+285/-203) keV (chi^2/d.o.f. = 16/14).

All the quoted errors are at statistical 90% confidence level

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


GRB_name: GRB120612A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13357
SUBJECT: GRB 120612A: Swift detection of a burst
DATE:    12/06/12 02:18:17 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. Pagani (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (NASA/UMBC),
S. T. Holland (STScI), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 02:05:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120612A (trigger=524128).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 126.726, -17.578 which is 
   RA(J2000)  =  08h 26m 54s
   Dec(J2000) = -17d 34' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows s single broad peak
with a duration of about 30 sec.  The peak count rate
was ~1250 counts/sec (15-350 keV), at ~7 sec after the trigger. 

The XRT began observing the field at 02:07:38.1 UT, 138.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 126.72350,
-17.57649 which is equivalent to:
   RA(J2000)  = 08h 26m 53.64s
   Dec(J2000) = -17d 34' 35.4"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 10 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 5.49
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 5.98e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 147 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
0.07. 

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: GRB120612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13358
SUBJECT: GRB 120612A: BOOTES-3 optical upper limit
DATE:    12/06/12 07:36:14 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C. Tello (IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC),  J.
Gorosabel (IAA-CSIC),  W. Allen (Vintage Lane Obs.), Ph. Yock and Kuan-Yu
Lin (Auckland Univ.), P. Kubanek (IP AS CR & IAA-CSIC), report on behalf of
a larger collaboration:

"We observed the field of GRB 120612A (Pagani et al., GCNC 13357), detected
by Swift/BAT, with the 0.6m Yock-Allen robotic telescope (BOOTES-3) located
in Blenheim, New Zealand. Unfiltered images were obtained starting
05:58:29UT (3h53m after the burst, limited by sunset). The first 40 images,
each of 60 seconds, were combined (with the last exposure ending at
06:39:14 UT). This resulted in a limiting magnitude of 18.0 when calibrated
with the R1Mag value of USNO-B1.0 catalogue stars."

This message may be cited.


GRB_name: GRB120612A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13359
SUBJECT: GRB 120612A: Enhanced Swift-XRT position
DATE:    12/06/12 11:30:36 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 1361 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120612A, 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 = 126.72179, -17.57496 which is equivalent
to:

RA (J2000): 08h 26m 53.23s
Dec (J2000): -17d 34' 29.9"

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: GRB120612A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13360
SUBJECT: GRB 120612A: Swift-BAT refined analysis
DATE:    12/06/12 12:28:06 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), C. Pagani (U Leicester),
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 120612A (trigger #524128)
(Pagani, et al., GCN Circ. 13357).  The BAT ground-calculated position is
RA, Dec = 126.723, -17.598 deg which is 
   RA(J2000)  =  08h 26m 53.5s 
   Dec(J2000) = -17d 35' 52.9" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.
 
The mask-weighted light curve shows a broad peak starting at ~T+15 sec,
peaking at roughtly T+35 sec, and ending around T+150 sec with a long
low-level tail out to about T+380 sec.  T90 (15-350 keV) is 90 +- 14 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+16.9 to T+125.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.16.  The fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+30.20 sec in the 15-150 keV band
is 0.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/524128/BA/


GRB_name: GRB120612A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13361
SUBJECT: GRB 120612A: Swift-XRT refined Analysis
DATE:    12/06/12 14:18:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 13 ks of XRT data for GRB 120612A (Pagani  et al. GCN
Circ. 13357), from 144 s to 30.4 ks after the  BAT trigger. The data
comprise 91 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 13359).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.27 (+0.26, -0.22), followed by a break at T+485 s to
an alpha of 0.90 (+0.11, -0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.20 (+0.23, -0.22). The
best-fitting absorption column is  1.9 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 5.5 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 (5.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 5.5 x 10^20 cm^-2
Excess significance: 3.9 sigma
Photon index:      2.20 (+0.23, -0.22)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00524128.

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


GRB_name: GRB120612A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13362
SUBJECT: GRB 120612A: Swift/UVOT observations
DATE:    12/06/12 18:08:11 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C.A. Swenson (PSU) and C. Pagani (U Leicester) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB
120612A 148 s after the BAT trigger (Pagani et al., GCN Circ.
13357).  No new optical afterglow consistent with the XRT posistion
(Evans et al., GCN Circ. 13359) is detected in the initial UVOT
exposures.

We note that there is a DSS source, which complicates the UVOT
analysis, located at RA, DEC = 126.72113, -17.57439.  This source
lies 3.05 arcsec from the XRT position and may or may not be related
to GRB 120612A, though we see no sign of variability in the source
in the first 1500 s of UVOT observations.  The source is also listed
in the USNOB catalog with a color of (B-R) = 0.728, corrected for
Galactic reddening.

Follow-up observations are encouraged to determine a redshift for
the DSS source to determine whether this is potentially the host galaxy.


GRB_name: GRB120612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13363
SUBJECT: GRB 120612A: optical observations
DATE:    12/06/13 00:32:25 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI), R. 
Sanchez-Ramirez (IAA-CSIC and DARK/NBI), J. P. U. Fynbo (DARK/NBI), 
report on behalf of the X-shooter GRB GTO collaboration:

We observed the field of GRB 120612A (Pagani et al., GCN 13357) with the 
ESO VLT equipped with X-shooter. Observations were taken with the 
acquisition camera in the R and z filters, with an exposure time of 45 s 
each. The images were obtained around 23:25 UT (about 21.3 hr after the 
GRB).

Within the revised XRT error circle (Evans et al., GCN 13359), we do not 
detect any object in either filters, down to a limiting magnitude R = 
22.5 (3 sigma). We confirm the presence of a bright star just outside 
the XRT circle (Swenson et al., GCN 13362), which brightness is 
consistent with the value reported in the USNO catalog. This object is 
pointlike (with a seeing of 1.3") and is significantly outside the XRT 
error circle, so it is very likely unrelated to the GRB.

We acknowledge excellent support from the observing staff in Paranal, in 
particular Alain Smette and Claudio Melo.


GRB_name: GRB120614A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13364
SUBJECT: GRB 120614A: MAXI/GSC detection of a burst
DATE:    12/06/14 08:16:59 GMT
FROM:    Satoshi Nakahira at JAXA/MAXI  <nakahira.satoshi@jaxa.jp>

J. Sugimoto, T. Yamamoto (RIKEN), M. Morii (Tokyo Tech),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa (JAXA),
T. Mihara, M. Serino, M. Sugizaki, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, K. Ishikawa (Tokyo Tech),
H. Negoro, M. Nakajima, N. Serita, M. Asada, H. Sakakibara (Nihon U.),
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka 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.),
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

MAXI/GSC triggered at 2012-06-14T05:49:10 UT on a bright uncatalogued
X-ray transient source.
The transient emission lasted at least for 45 seconds
within the 56 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 120614A.

There was no violent variability within the scan transit.
Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (+312.73 deg, +65.16 deg) = (20 50 56, +65 09 53)(J2000)

with a 90% C.L. statistical error of 0.17 deg and an additional
systematic uncertainty of 0.1 deg (90% containment radius).
The source flux was 317 +- 36 (mCrab) in 4 - 10 keV.

There was no flux in the previous transit at 04:17 UT and in the next
transit at 07:21 UT with an upper limit of 20 mCrab for each.

Follow-up observations are encouraged.


GRB_name: GRB120602A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13365
SUBJECT: IPN Triangulation of GRB 120602A (long/very bright)
DATE:    12/06/14 17:25:50 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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,

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

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, very bright GRB 120602A was observed by INTEGRAL 
(SPI-ACS), Swift (BAT), Konus-Wind, Suzaku (WAM), MESSENGER (GRNS), and 
Mars Odyssey (HEND) on June 2 at about 18001 s UT (05:00:01). The burst 
was outside of the coded field of view of the BAT.

We have triangulated it to a 3 sigma error box whose
coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    87.922 (05h 51m 41s) -39.354 (-39d 21' 16")
  Corners:
    87.761 (05h 51m 03s) -39.306 (-39d 18' 22")
    87.798 (05h 51m 12s) -39.441 (-39d 26' 28")
    88.084 (05h 52m 20s) -39.402 (-39d 24' 08")
    88.046 (05h 52m 11s) -39.267 (-39d 16' 02")
  ---------------------------------------------
The error box area is 111 sq. arcmin, and its maximum
dimension is 16 arcmin.

This box may be further improved.

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


GRB_name: GRB120602A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13366
SUBJECT: Konus-Wind observation of GRB 120602A
DATE:    12/06/15 09:28:27 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 intense GRB 120602A
(IPN localization: Hurley at al., GCN 13365)
triggered Konus-Wind at T0=18000.228s UT (05:00:00.228)

The light curve shows a bright pulse at ~T0+55 s,
preceded by several weaker overlapping pulses.
A total burst duration of the burst is ~70 s.
The emission is seen up to ~9 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120602_T18000/

As observed by Konus-Wind the burst
had a fluence of (3.6  0.1)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+54.912 s,
of (3.9  0.5)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+60.416 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.77 (-0.03, +0.03),
the high energy photon index beta = -2.8 (-0.1, +0.1),
the peak energy Ep = 300(-10, +10) keV,
chi2 = 104.3/80 dof.

The spectrum at the maximum count rate
(measured from T0+54.784s to T0+55.040 s) is best fitted
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.85 (-0.10, +0.12),
the high energy photon index beta = -2.9 (<-2.5),
the peak energy Ep = 530(-90, +90) keV,
chi2 = 39.2/45 dof.

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


GRB_name: GRB120617A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13370
SUBJECT: IPN Triangulation of GRB 120617A (short/intense)
DATE:    12/06/18 20:28:42 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,

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 bright, short-duration GRB 120617A has been observed by INTEGRAL 
(SPI-ACS), Konus-Wind, and MESSENGER (GRNS), so far, at about 54171 s UT 
(15:02:51).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
      22.309 (01h 29m 14s) +33.804 (+33d 48' 14")
    Corners:
      22.485 (01h 29m 57s) +33.057 (+33d 03' 25")
      22.035 (01h 28m 08s) +34.123 (+34d 07' 23")
      22.140 (01h 28m 34s) +34.534 (+34d 32' 02")
      22.583 (01h 30m 20s) +33.482 (+33d 28' 55")
    ---------------------------------------------
The error box area is 881 sq. arcmin, and its maximum
dimension is 90 arcmin (the minimum one is 25 arcmin).

This box may be improved.

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


GRB_name: GRB120617A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13371
SUBJECT: Konus-Wind observation of GRB 120617A
DATE:    12/06/19 12:24:29 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 intense GRB 120617A
(IPN localization: Golenetskii at al., GCN 13370)
triggered Konus-Wind at T0=54167.025s UT (15:02:47.025)

The light curve shows two pulses,
a total duration of the burst is ~0.5 s.
The emission is seen up to ~4 MeV.
A spectral lag between G2(80-300 keV) and G1(20-80 keV)
instrument's light curves is estimated to 28 +/- 4 ms (1 sigma).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120617_T54167/

As observed by Konus-Wind the burst
had a fluence of 2.1(-0.2,+0.2)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.256 s,
of 1.5(-0.3,+0.4)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 well fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.95 (-0.4, +0.5),
and Ep = 180(-40, +70) keV,
chi2 = 12.6/22 dof.

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


GRB_name: GRB120602A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13372
SUBJECT: GRB 120602A: Suzaku WAM observation of the prompt emission
DATE:    12/06/20 11:48:02 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

S. Kobayashi, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara,
M. Asahina, A. Sakamoto, H. Ueno (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 120602A (IPN; Hurley and Goldsten et al., GCN 13365, 
Konus-Wind; Golenetskii et al., GCN 13366)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an 
energy range of 50 keV - 5 MeV at 05:00:0.83 UT (=T0).

The observed light curve shows a multi-peaked structure starting at 
T0+5.8 s, ending at T0+59.8 s,  with a duration (T90) of about 54 
seconds. The fluence in 100 - 1000 keV was
1.97 (-0.03, +0.07) x 10^-4 erg/cm^2. The 1-s peak flux measured from
T0+56.4s was 40.0 (+/-1.3) photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from T0s to
T0+70s is well fitted by a power-law with exponential cutoff model:
   dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha       1.49(-0.13, +0.12), and
   Epeak       305 (-51, +40) keV (chi^2/d.o.f. = 67.7/48).

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

----
The light curves with 1-second time resolution for this burst are 
available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB120622A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13374
SUBJECT: GRB 120622A: MAXI/GSC detection
DATE:    12/06/22 05:17:01 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

N. Serita , H. Negoro (Nihon U.), M. Serino (RIKEN), M. Morii (Tokyo Tech),
S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto,  J. Sugimoto, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, K. Ishikawa (Tokyo Tech),
M. Nakajima, M. Asada, H. Sakakibara (Nihon U.),
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka 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.),
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered at 2012-06-22T03:21:46 UT on an 
uncatalogued soft X-ray transient source.
The transient emission lasted at least for 39 sec
within the 65 sec long triangular transit response of
MAXI/GSC. We identify this event as GRB 120622A.

Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (+205.43 deg, -1.71 deg) = (13 41 43, -01 42 36)(J2000)

with a 90% C.L. statistical error of 20 arcmin and an additional
systematic uncertainty of 0.1 deg (90% containment radius).

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

 (R.A., Dec) = (+204.33 deg, -1.49 deg) = (13 37 18, -01 29 35)(J2000)
 (R.A., Dec) = (+204.50 deg, -1.02 deg) = (13 37 59, -01 01 12)(J2000)
 (R.A., Dec) = (+206.52 deg, -1.84 deg) = (13 46  6, -01 50 40)(J2000)
 (R.A., Dec) = (+206.33 deg, -2.31 deg) = (13 45 20, -02 18 35)(J2000)

The source flux was about 60 mCrab in the 2 - 4 keV band, 
and about 90 mCrab  in the 4-10 keV band.

There was no flux in the previous transit at 01:48 UT and 
in the nexttransit at 04:53 UT with an upper limit of 20 mCrab for each.

Follow-up observations are encouraged.


GRB_name: GRB120624A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13376
SUBJECT: IPN Triangulation of GRB 120624A (short/intense)
DATE:    12/06/24 23:00:23 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:

The bright, short-duration GRB 120624A has been observed by Fermi (GBM
trigger 362215467), INTEGRAL (SPI-ACS), Konus-Wind, Swift (BAT), and
MESSENGER (GRNS), so far, at about 26665 s UT (07:24:25). The burst was
outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
       4.773 (00h 19m 05s)  +7.167 ( +7d 10' 00")
    Corners:
       5.349 (00h 21m 24s)  +5.841 ( +5d 50' 28")
       5.463 (00h 21m 51s)  +5.941 ( +5d 56' 27")
       4.182 (00h 16m 44s)  +8.484 ( +8d 29' 02")
       4.068 (00h 16m 16s)  +8.384 ( +8d 23' 01")
    ---------------------------------------------
The error box area is 0.42 sq. deg, and its maximum dimension is 2.9 deg
(the minimum one is 0.2 deg).

This box may be improved.

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


GRB_name: GRB120624B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13377
SUBJECT: GRB 120624B: Fermi GBM detection
DATE:    12/06/25 09:39:54 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

D. Gruber (MPE), J. M. Burgess (UAH) and V. Connaughton (UAH)
report on behalf of the Fermi GBM Team:

"At 22:23:54.92 UT on 24 June 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120624B (trigger 362269436 / 120624933).

The on-ground calculated location, using the GBM trigger
data, is RA = 172.9, DEC = 6.5 (J2000 degrees,
equivalent to 11 h 31 m 36 s, 06 d 30 '), with an uncertainty
of 1 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 71 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.

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

The GBM light curve consists of 3 bright, highly variable pulses
starting ~ 250 s prior to the GBM trigger. The first pulse
lasted ~100 s, the second pulse lasted ~120 s and the final pulse,
which triggered GBM, lasted ~50 s.
The event duration (T90) is about 271 s (50-300 keV).
GBM triggered on the third episode because the first and second
episode occurred during the brief part of the Fermi orbit at high 
geomagnetic latitude where triggering is currently disabled 
owing to particle activity and ensuing false triggers.

The time-averaged spectrum from T0-270 s to T0+22.5 s is
best fit by a Band function with Epeak = 566 +/- 20 keV,
alpha = -0.85 +/- 0.01, and beta = -2.36 +/- 0.08.

The event fluence (10-1000 keV) in this time interval is
(8.980 +/- 0.007)E-03 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+11.4 s in the 10-1000 keV band
is 846 +/- 17 ph/s/cm^2.

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


GRB_name: GRB120624A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13378
SUBJECT: Konus-Wind observation of GRB 120624A
DATE:    12/06/25 09:50:57 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 intense GRB 120624A
(IPN localization: Golenetskii at al., GCN 13376)
triggered Konus-Wind at T0=26662.982s UT (07:24:22.982)

The light curve shows a single pulse,
a total duration of the burst is ~0.3 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120624_T26662/

As observed by Konus-Wind the burst
had a fluence of 3.3(-0.3,+0.3)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.048 s,
of 2.0(-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+0.256 s)
is well fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.70 (-0.1, +0.1),
and Ep = 3350(-460, +550) keV,
chi2 = 49.4/50 dof.

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


GRB_name: GRB120624B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13379
SUBJECT: GRB 120624B: Fermi-LAT Detection
DATE:    12/06/25 10:18:47 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

Giacomo Vianello (CIFS/SLAC), Daniel Kocevski (Stanford Univ.) report
on behalf of the Fermi LAT Team:

Fermi-LAT has detected high energy emission from the long, hard and
bright GRB 120624B in ground analysis. The GRB was triggered on by the
GBM on June 24, 2012 at 22:23:54.93 UTC, although the emission started
~250 seconds earlier (trigger 362269436, GCN 13377).

The best GBM position was \~70 deg off-axis for the whole duration of
the prompt emission (~270 seconds), outside of the Fermi/LAT nominal
field of view for the standard data analysis.

Using a non-standard data selection most sensitive in the tens-of-MeV
energy range and with a broader acceptance, we significantly detected
the burst between ~T0-250s and ~T0+20 s. The significance of the
excess corresponds to 10 sigma. The light curve shows 3 peaks, with a
total duration of \~270 s.

This burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver, starting 100 s after the GBM
trigger. Thus, the GBM position entered the LAT field of view at
\~T0+100 s.

A preliminary maximum-likelihood analysis of the E>100MeV
P7TRANSIENT_V6 LAT data generated during the interval T0+100, T0+1.3
ks (until the GRB became occulted by the Earth) revealed a very
significant transient source, with a spectrum well described by a
power law of index -2.4 +/- 0.1 (68% c.l. statistical only). Using
this analysis, we obtained the best LAT on-ground localization of:

RA(J2000) = 170.73 deg
Dec(J2000) = 9.48 deg

with an error radius 0.45 deg (90% containment, statistical error
only), which is 3.6 deg from the best GBM localization.

The Zenith angle for this source was ~30 deg at the time of the
trigger, thus very far from the Earth Limb.

A Swift/ToO request has been submitted.

The Fermi-LAT point of contact for this burst is Daniel Kocevski
(kocevski@stanford.edu)


GRB_name: GRB120624A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13380
SUBJECT: GRB 120624A: Fermi GBM observation
DATE:    12/06/25 14:24:49 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 07:24:25.34  UT on 24 June 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120624A (trigger 362215467 / 120624309).
The burst was also detected by the 3rd Interplanetary Network (Golenetskii
et al. 
2011, GCN 13376). The angle from the Fermi LAT boresight is 90.2 degrees.

The GBM light curve consists of a single FRED-like pulse 
with a duration (T90) of about 0.7 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.448 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.83 (+0.02/-0.02) and
the cutoff energy, parameterized as Epeak, is 3800 (+200/-180) keV.

The event fluence (10-1000 keV) in this time interval is
(6.5 +/- 0.1)E-06 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0+0.064 s in the 10-1000 keV band
is 78.245 +/- 2.4 ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak = 3700 (+200/-220)
keV, 
alpha = -0.83 (+0.02/-0.02) and beta = -3.4 (+0.4/-0.8).

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


GRB_name: GRB120624B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13381
SUBJECT: GRB 120624B: Swift detection of a burst
DATE:    12/06/25 15:35:04 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. Kennea (PSU), J. Racusin (GSFC)
report on behalf of the Swift Team:

At 22:19:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120624B (trigger=525068) (also detected by Fermi-GBM, Circ 13377
and Fermi-LAT, Circ 13379).  There were no real-time notices
for this event because it occurred during a TDRSS outage (22:07 to 22:46),
so none of the normal sequence of real-time notices were available.
There was no automated slew to this BAT trigger because of a Moon constraint.
The BAT on-board calculated location is RA, Dec 170.94, 8.93 (J2000),
with an uncertainty of 3 arcmin (radius, 90% containment,
including systematic uncertainty).  We are in the process of getting
the full data set downlinked,  and will produce the nomal "refined"
circular when it becomes available.

[GCN OPS NOTE905jul12): Per author's request, the Trigger Time has been
changed from 22:19:51 to 22:19:33.66 UT.  We apologize for the mistake.
We thank Frank Marshall for bring the mistake to our attention.]


GRB_name: GRB120624B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13382
SUBJECT: Konus-Wind observation of GRB 120624B
DATE:    12/06/25 17:39:20 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 long intense hard GRB 120624B
(GBM trigger 362269436: Gruber et al., GCN 13377;
Fermi/LAT detection: Vianello & Kocevski, GCN 13379)
triggered Konus-Wind at T0=80406.904s UT (22:20:06.904)

The light curve shows multiple pulses grouped to three main episodes.
A total duration of the burst is ~300 s.

We note a quasi-periodic light curve structure (with T~3.6s)
which is observed during the second bursting episode
(from ~T0+120s to ~T0+150s).

The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120624_T80406/

As observed by Konus-Wind the burst
had a fluence of 2.75(-0.1,+0.1)x10-4 erg/cm2,
and a 2.944-ms peak flux, measured from T0+235.28 s,
of 3.0(-0.6,+0.7)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+253.952 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.02 (-0.10, +0.12),
the high energy photon index beta = -2.6 (-2.0, +0.4),
the peak energy Ep = 530(-80, +90) keV,
chi2 = 82.7/86 dof.

The spectrum at the maximum count rate
(measured from T0+229.634 to T0+237.824 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.12 (-0.13, +0.21),
the high energy photon index beta = -2.3 (<-1.8),
the peak energy Ep = 1000(-450, +620) keV,
chi2 = 77.8/86 dof.

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


GRB_name: GRB120624B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13383
SUBJECT: GRB 120624B: Fermi GBM fluence and peak photon flux correction
DATE:    12/06/25 19:38:51 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

D. Gruber (MPE) reports on behalf of the Fermi GBM Team:

"The peak flux and fluence values reported for GRB 120624B
in GCN 13380 were erroneously calculated.

The correct numbers are as follows:
The fluence in the 10-1000 keV energy range 
is (1.916 +/- 0.002)E-04 erg/cm^2.
This is consistent with the values reported 
by Konus-Wind (Golenetskii et al. GCN 13382).

The 1-sec peak photon flux measured
in the 10-1000 keV band is 17.7 +/- 0.3 ph/s/cm^2.

We apologize for any inconvenience this has caused."


GRB_name: GRB120624B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13384
SUBJECT: GRB 120624B, Swift-BAT refined analysis
DATE:    12/06/25 20:53:53 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
A. M. Parsons (GSFC), 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-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120624B (trigger #525068)
(Vianello, et al., GCN Circ. 13379; Barthelmy, et al., GCN Circ. 13381).  
The BAT ground-calculated position is RA, Dec = 170.886, 8.933 deg which is 

   RA(J2000)  =  11h 23m 32.6s 
   Dec(J2000) = +08d 56' 00.4" 

with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 86%.
 
The mask-weighted light curve shows multiple overlapping episodes starting 
from T-25 sec.  There are two main episodes going from T-10 to T+70 sec with a
peak around T+35 sec, and the second episode starts T+120 sec and appears to 
end around T+200 sec, with peaks at T+140 sec and T+170 sec.  But the data ends 
due to observing constraint and slewing to a pre-planned target.  T90 (15-350 keV) 
is greater than 192 sec due to the end of the mask-weighted light curve when 
the source location left the field of view.  

The time-averaged spectrum from T-15.1 to T+192.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.17 +- 0.03.  The fluence in the 15-150 keV band is 2.83 +- 0.04 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+138.06 sec in the 15-150 keV band
is 5.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/525068/BA/


GRB_name: GRB120624B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13385
SUBJECT: GRB 120624B: optical observations
DATE:    12/06/25 22:47:56 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. Snchez-Caso (Gualba Observatory, Barcelona) and A. J. Castro-Tirado
(IAA-CSIC Granada), on behalf of a larger collaboration, report:

Following the detection of GRB 120624B by Fermi/GBM, Fermi/LAT,
Konus/Wind and Swift/BAT (GCNC 13377, 13378, 13379 and 13381
respectively), we have imaged the field with the 0.36m f/7 telescope at
Gualba Observatory in Barcelona (Spain) starting on June 25 at 20:30 UT
(i.e. about 22 hr post-burst). Within the Swift/BAT 3 radius error box no
optical afterglow candidate is identified for GRB 120624B. The limiting
magnitude in the 300-s unfiltered image (with the crescent moon only 9 deg
away) is 18.5.

This message can be quoted.


GRB_name: GRB120624B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13387
SUBJECT: GRB 120624B: NOT optical upper limit
DATE:    12/06/25 23:32:09 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Malesani
(DARK/NBI), D. Gandolfi (ESTEC/ESA), G. Leloudas (OKC, Stockholm)
report on behalf of a larger collaboration:

We observed the Swift/BAT field of GRB 120624B (Gruber et al., GCN
13377; Vianello&  Kocevski, GCN 13379; Sakamoto et al., GCN 13384)
using the 2.5m Nordic Optical Telescope (NOT) equipped with the ALFOSC
camera, at La Palma, Canary Islands. Observations started at 21:26 UT
on 2012-06-25 (i.e., 23.05 hr after the Fermi trigger) and a series of
SDSS r-band frames with a total exposure time of 1250s were obtained,
but were affected by the dusty calima from the Sahara desert.

No new optical source was detected within the refined BAT error circle
down to a 3-sigma limit of r(AB)~21.0.


GRB_name: GRB120624B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13389
SUBJECT: GRB 120624B: Discussion of Fermi and Swift measurements and future Swift observations
DATE:    12/06/26 01:42:50 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (UNLV), D. Gruber (MPE), J. M. Burgess (UAH), J. McEnery 
(NASA/GSFC), S. T. Holland (STSCI), S. Razzaque (GMU/NRL) and J. L. 
Racusin (NASA/GSFC), on behalf of the Swift, Fermi-GBM, and the Fermi-LAT 
teams:

GRB 120624B, detected by Fermi-GBM (GCN 13377), Fermi-LAT (GCN 13379), 
Swift-BAT (GCN 13381), and Konus-Wind (GCN 13382) has very high fluence 
(1.9e-04 erg cm-2) and peak flux. The fluence of GRB 120624B in among the 
top 1.5% of bursts detected by Swift-BAT and the top 0.55% detected by 
Fermi-GBM.

The GRB position is unfortunately within the Swift Moon constraint. 
Swift-XRT/-UVOT follow-up observations are planned when if comes out of 
Moon constraint on June 27.4.

The refined BAT localization (GCN 13384) has an error radius of 1 arcmin 
(90% containment). There are 13 SDSS galaxies with r>24 within the BAT 
error circle. Analysis of the prompt emission suggests that the redshift 
of this event is z > ~0.3 if this burst obeys the Amati relation, with 
E_iso > ~4e+52 erg.

We strongly encourage follow-up observations of GRB 120624B.


GRB_name: GRB120624B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13391
SUBJECT: GRB 120624B: NIR counterpart candidate from HAWKI
DATE:    12/06/27 19:33:15 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

P. D'Avanzo (OaB/INAF), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), S. Campana (OaB/INAF), J. Gorosabel (IAA-CSIC), S. Covino (OaB/INAF), J.P.U. Fynbo (DARK/NBI), and C.C. Thoene (IAA-CSIC) report on behalf of a larger collaboration,

We observed the field of the very intense GRB 120426B detected by Fermi, Swift and Konus-Wind (Gruber et al., GCN 13377, Barthelmy et al. GCN 13381, Golenetskii et al. GCN 13382) with HAWKI at ESO's VLT (Paranal, Chile). Observations consisted of two epochs of 600s of integration in K-band covering the entire BAT error box (Sakamoto et al. GCN 13384). In the first epoch obtained 24.7 hr after the burst, we detect a faint source with a preliminary photometry K~20.8 compared to the 2MASS catalogue. This source is no longer visible in a second epoch 48.7 hr after the burst, where we estimate a 3-sigma limiting magnitude of K~21.6. The coordinates of the candidate nIR counterpart are (J2000 +/- 0.3"):

R.A.: 11:23:29.67
Dec.: +08:55:28.7

We note that this source falls North East of a galaxy at a projected distance of ~1.7" from the center of the galaxy.

We acknowledge excellent support from the Paranal staff, in particular Emanuela Pompei.


GRB_name: GRB120624B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13393
SUBJECT: GRB 120624B: GROND upper limits
DATE:    12/06/28 09:14:58 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady (MPE Garching), A. Nicuesa Guelbenzu, S. Klose, D. A. Kann  
(TLS Tautenburg), M. Nardini (Universita' degli Studi Milano-Bicocca),  
and J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of the bright GRB 120624B (Fermi/GBM trigger  
362269436/120624933, Gruber et al., GCN 13377, 13383; Konus-Wind  
detection, Golenetskii et al., GCN 13382; Swift trigger 525068,  
Sakamoto et al., GCN 13384) 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 23:17 UT on 2012-06-25, about 23 hrs after the  
GRB trigger and lasted for about 2 hrs. At the time of our  
observations, the angular distance of the source position to the Moon  
(last quarter) was just 10 degrees, significantly increasing the  
background in our optical images.

In stacked images of the first 20min in the g'-band, of the first hour  
in r', i' and z'  and the whole  2 hr period of J, H and K  
observations, we do not detect any new source at the position of the  
NIR afterglow candidate (D'Avanzo et al., GCN 13391), nor within the  
BAT error circle (Sakamoto et al., GCN 13384). The 3sigma limiting AB  
magnitudes  are as follows

g' > 23.3
r' > 24.0
i' > 23.5
z' > 23.4
J > 21.7
H > 21.1
K > 20.0

The galaxy close to the NIR afterglow candidate position mentioned in  
D'Avanzo et al. (GCN 13391) is clearly detected in our J and H-band  
images, with AB magnitudes J=20.9+/-0.2 and H=20.4+/-0.2.

The above limits are derived based on calibrating the optical and NIR  
images against GROND zeropoints and 2MASS field stars respectively,  
and are not corrected for the Galactic foreground extinction  
corresponding to a reddening of E(B-V)=0.06 mag in the direction of  
the burst (Schlegel et al. 1998).


GRB_name: GRB120624B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13394
SUBJECT: GRB 120624B: Swift-XRT observations
DATE:    12/06/28 10:24:28 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O.M. Littlejohns, P.A. Evans, K.L. Page (U. Leicester), A. Melandri, P.
D'Avanzo (INAF-OAB) and J.Racusin (GSFC) reports on behalf of the
Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 120624B (Barthelmy  et al.
GCN Circ. 13381), from 218.7 ks to 260.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Inside the BAT refined
error circle (Sakamoto et al. GCN Circ. 13384) we find an uncatalogued
X-ray source (S1) at RA, Dec = 170.8845, +8.9283 which is equivalent
to:

RA (J2000): 11 23 32.28
Dec(J2000): +08 55 42.0

with an uncertainty of 4.3 arcsec (radius, 90% confidence). This source
lies 40 arcsec from the NIR object reported by D'Avanzo et al. (GCN
Circ. 13391). We cannot determine at the present time whether the
source is fading, the count-rate is approximately 2e-3 ct/sec in XRT.

There is a second source (S2) at RA, Dec = 170.8670, +8.9319 which is
equivalent to:

RA (J2000): 11 23 28.07
Dec(J2000): +08 55 54.8

with an uncertainty of 4.2 arcsec (radius, 90% confidence). This source
is 70 arcsec away from the BAT refined position, just outside the error
circle. This source is 35 arcsec from the NIR counterpart. This source
has a count-rate of approximately 1e-3 ct/sec, and again we cannot
measure variability at this time. 

An image of the XRT field, with the two XRT sources, BAT error circle
and NIR source marked, is available at
http://www.swift.ac.uk/products/GRB120624B.png

Further observations are planned.

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


GRB_name: GRB120624B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13395
SUBJECT: GRB 120624B: Further analysis of the HAWKI observations
DATE:    12/06/28 10:50:37 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), P. D'Avanzo (OaB/INAF), 
S. Campana (OaB/INAF), J. Gorosabel (IAA-CSIC), S. Covino (OaB/INAF), 
J.P.U. Fynbo (DARK/NBI), and C.C. Thoene (IAA-CSIC) report on behalf of 
a larger collaboration,

In light of the recent XRT observation (Littlejohns et al., GCN13394) we 
have performed further analysis of the HAWKI data reported by D'Avanzo 
et al. (GCN 13391). Within the error circle of the XRT source  we detect a 
point-like source and a galaxy at the following coordinates (J2000 +/- 0.3"):

Galaxy 1A (RA, Dec): 11:23:32.08, +08:55:44.7
Point-like 1B (RA, Dec): 11:23:32.30, +08:55:42.5

We have performed image subtraction between our two K-band observations 
and we detect no variability of any of these sources between the two epochs.

We also note that the galaxy is well detected in the SDSS with r=21.46 and a 
has a photometric redshift of 0.57+/-0.07.

Our observations also cover the second XRT source that lies slightly outside 
the BAT error circle. Within this region we detect 2 extended sources, with 
coordinates (J2000 +/- 0.3"):

Galaxy 2 (RA, Dec): 11:23:28.17, +08:55:57.6
Galaxy 3 (RA, Dec): 11:23:28.07, +08:55:56.8

Again, no variability is found within the second XRT position. These are detected 
as a single source in SDSS at r=21.55 and a photometric redshift of 0.43+/-0.07.

[GCN OPS NOTE(28jun12): Per author's request, the "120426B" in the Subject-line
was changed to "120624B:.]


GRB_name: GRB120624B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13397
SUBJECT: GRB 120624B: Swift/UVOT Upper Limits
DATE:    12/06/28 13:17:00 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL/UCL), F. E. Marshall (NASA/GSFC) and J.Racusin 
(GSFC) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120624B
60hours 45mins after the BAT trigger (Barthelmy et al., GCN Circ. 13381).
No optical afterglow is found at either of the XRT positions 
(Littlejohns et al. GCN 13394) nor the HAWKI position reported by 
D'Avanzo et al. (GCN 13391) 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 summed exposures are:

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

white_FC        218726       218864          136         >20.9
white           218865       260947         7027         >23.1

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


GRB_name: GRB120624B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13398
SUBJECT: GRB 120624B Further Swift-XRT analysis
DATE:    12/06/28 20:30:51 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O.M. Littlejohns, P.T. O'Brien, P.A. Evans, K. Page (UL) and J.Racusin (GSFC) reports on behalf of the Swift-XRT team:

Following the XRT observations of the BAT error circle for GRB 120624B reported in Littlejohns et al. (GCN Circ. 13394), we have compared the measured XRT flux of source S1 at 240 ks to that of bursts with similar or greater measured BAT fluence. Measurements of the XRT flux at approximately 240 ks for these bursts show that GRB 120624B lies at the faint end of the distribution of such bursts, should S1 prove to be the X-ray counterpart to GRB 120624B.

Further XRT observations are planned for Tuesday the 3rd July (2012), with a total exposure time of 10 ks, to check if either source S1 or S2 has faded.

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


GRB_name: GRB120624B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13400
SUBJECT: GRB120624B: Chandra observations and afterglow detection
DATE:    12/07/01 19:04:24 GMT
FROM:    Sergio Campana at INAF-OAB  <sergio.campana@brera.inaf.it>

S. Campana (INAF-OAB), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI),
A. J. Levan (U. Warwick) on behalf of a larger collaboration report:

we imaged for 10 ks the field of GRB 120624B (Gruber et al. 2012, GCN
13377) with the Chandra ACIS-S starting on June 30, 2012 8:56:22 UT.
Within the Swift/BAT 1 arcmin error circle (Barthelmy et al. 2012, GCN 13381)
we detect two sources, already reported by Swift/XRT (Littlejohns et al.  2012,
GCN 13394).

S1 source is detected with wavdetect at a (preliminary) position:
RA(J2000):  11 23 32.31
Dec(J2000):+08 55 42.8
The nominal positional error (90% c.l.) is 0.3 arcsec
(not including any statistical error).
The source is detected with 25 counts.

S2 source is detected with wavdetect at a (preliminary) position:
RA(J2000):  11 23 28.09
Dec(J2000):+08 55 57.0
The nominal positional error (90% c.l.) is 0.2 arcsec
(not including any statistical error).
The source is detected with 49 counts.

We do not detect any X-ray source at the position of
the NIR afterglow candidate (D'Avanzo et al. 2012, GCN13391).

We note that S1 is brighter than S2 in Swift/XRT observations.
The contrary occurs in the Chandra observation.

We extrapolate the Swift XRT rates based on the Swift/XRT spectrum
(Galactic column density of 3.6e20 cm-2, intrinsic column density of
2.4e21 cm-2 at redshift zero and a power law photon index of 2.52).
Assuming this spectrum for both sources, we predict
78 counts for S1 and 59 counts for S2, with large uncertainties due to
spectral modeling and statistics.

Despite this, the disagreement between Swift/XRT predictions (78 counts)
and Chandra observation (25 counts), likely indicate that S1 is the 
afterglow of GRB120624B.

We thank Chandra director (H. Tananbaum) for granting this observation
under the DDT program.


GRB_name: GRB120630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13403
SUBJECT: GRB 120630A: NOT optical source within the XRT error circle
DATE:    12/07/02 09:24:21 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), L.-P. Xin (NAOC), D. Malesani, J. P. U. Fynbo (DARK/NBI),
S. Geier (NOT) report on behalf of a larger collaboration,

Using the 2.5m Nordic Optical Telescope (NOT) equipped with StanCam,
we observed GRB 120630A (distributed by Swift PI: Neil Gehrels) whose
initial XRT localization/position was determined as

RA(J2000) =    23h 29m 10.6s
Dec(J2000) =   42d 33m 14.1s

with an uncertainty of 10 arcsec radius. Observations started at
03:06:20 UT on 2012-07-02 (i.e., 27.8 hr since the BAT trigger) and
5x360s R-band frames were obtained.

Within the XRT error circle, an optical source is clearly detected in
the stacked image at coordinates

RA(J2000) =    23h 29m 10.23s
Dec(J2000) =   42d 33m 13.0s

with an uncertainty of 0.5 arcsec radius. The source had R=22.53 +/-
0.15 mag, calibrated with nearby USNO stars with R2 magnitudes.


GRB_name: GRB120701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13404
SUBJECT: GRB 120701A: Swift-BAT refined analysis
DATE:    12/07/03 03:41:43 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), E. Sonbas (GSFC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report analysis of BAT GRB 120701A (trigger #525477).
There was no initial set of GCN Notices nor a rapid-response circular
because of the power outage at GSFC when this burst occurred.
The BAT ground-calculated position is
RA, Dec = 80.338, -58.531 deg which is 
   RA(J2000)  =  05h 21m 21.0s 
   Dec(J2000) = -58d 31' 52.3" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-2 sec and ending at ~T-20 sec.  T90 (15-350 keV) is 13.8 +- 0.7 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.0 to T+15.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.05 +- 0.10.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+10.36 sec in the 15-150 keV band
is 1.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/525477/BA/

[GCN OPS NOTE(03jul12):  Per author's request: "It should be noted that the
trigger_time for trigger 525477 is 07:50:41.57 UT on 01 July 2012."]


GRB_name: GRB120630A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13405
SUBJECT: GRB 120630A: Swift-BAT/-XRT/-UVOT refined analysis
DATE:    12/07/03 11:32:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), Gehrels (GSFC),
E. Sonbaas (GSFC)   (for the Swift-BAT team);
O. Littlejohns (U. Leicester)  (for the Swift-XRT team);
S. R. Oates (MSSL-UCL) (of the Swift-UVOT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120630A (trigger #525451).
There was no initial set of GCN Notices nor a rapid-response circular
because of the power outage at GSFC when this burst occurred.
Swift slewed immediately to the burst location.

The BAT ground-calculated position is RA, Dec = 352.300, 42.495 deg, which is 
   RA(J2000)  =  23h 29m 12.0s 
   Dec(J2000) = +42d 29' 41.5" 
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 65%.
 
The mask-weighted light curve shows a single spike starting at ~T-0.05 sec
and ending at ~T+0.65 sec.  T90 (15-350 keV) is 0.6 +- 0.2 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.1 to T+0.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.04 +- 0.43.  The fluence in the 15-150 keV band is 6.1 +- 1.4 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.25 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence level. 

Given the short duration and the hard spectrum of this burst,
it is very likely a short GRB.
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/525451/BA/ .


We have analysed 1.4 ks of XRT data for GRB 120630A from 97 s to 1.5 ks
after the BAT trigger.  The data are entirely in Photon Counting (PC) mode.
The refined XRT position is RA, Dec = 352.29481, 42.55483 which is equivalent to:
   RA (J2000): 23 29 10.75
   Dec(J2000): +42 33 17.4
with an uncertainty of 3.9 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay index
of alpha=1.7 (+/-0.5).

A spectrum formed from the PC 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 consistent with the Galactic value of 8.8 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 (4.9 x 10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
   Total column:        0 (+2.2, -0) x 10^21 cm^-2
   Galactic foreground: 8.8 x 10^20 cm^-2
   Excess significance: <1.6 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/00525451 .


The Swift/UVOT began settled observations of the field of GRB 120630A
150 s after the BAT trigger (trigger #525451).  No optical afterglow
consistent with the refined XRT position nor with the candidate optical
afterglow (Xu et al., GCN Circ. 13403) 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
v                  457          1409         117         >19.0
b                  406          1508         156         >20.0
u_FC               150          400          246         >20.2
u                  150          1032         393         >20.3
uvw1               506          1458         117         >19.3
uvm2               481          1434          97         >19.0
uvw2               432          1530         131         >19.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.106 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13406
SUBJECT: GRB 120701A: Swift-XRT afterglow detection and analysis
DATE:    12/07/03 12:20:14 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 analysed 19 ks of XRT data for GRB 120701A (Barthelmy et al. et
al. GCN Circ. 13404), from 61 s to 58.8 ks after the  BAT trigger. The
data comprise 69 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. We find an uncatatalogued, fading X-ray source inside the
BAT error circle. Using 7344 s of PC mode data and 5 UVOT images, we
find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
80.34740, -58.54973 which is equivalent to:

RA (J2000): 05h 21m 23.38s
Dec(J2000): -58d 32' 59.0"

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=1.078 (+0.031, -0.030).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.06 (+0.22, -0.21). The
best-fitting absorption column is  1.6 (+0.6, -0.5) x 10^21 cm^-2, in
excess of the Galactic value of 2.5 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 3.7 x 10^-11 (5.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 2.5 x 10^20 cm^-2
Excess significance: 4.0 sigma
Photon index:      2.06 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00525477.

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


GRB_name: GRB120703A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13408
SUBJECT: GRB 120703A: Swift detection of a bright burst with an optical afterglow
DATE:    12/07/03 17:34:05 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.-B. Zhang (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC), D. Grupe (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 17:25:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120703A (trigger=525671).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 339.357, -29.736 which is 
   RA(J2000) = 22h 37m 26s
   Dec(J2000) = -29d 44' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiply-peaked
structure with a duration of about 50 sec.  The peak count rate
was ~14000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 17:26:48.9 UT, 86.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 339.35607, -29.72444 which is
equivalent to:
   RA(J2000)  = 22h 37m 25.46s
   Dec(J2000) = -29d 43' 28.0"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 41 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.21 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.5
(+1.97/-1.72) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 91 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 22:37:25.71 = 339.35711
  DEC(J2000) = -29:43:23.5  = -29.72320
with a 90%-confidence error radius of about 1.10 arc sec. This position is 5.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.51. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

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: GRB120701A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13409
SUBJECT: GRB 120701A: GROND detection of the afterglow
DATE:    12/07/03 18:15:59 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 120701A (Swift trigger 525477; Barthelmy et 
al., GCN #13404) 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 09:11 UT on 2012-07-01, 1.34 hr after the GRB 
trigger. They were performed at an average seeing of 1.6 arcsec and at an 
average airmass of 2.5. A second epoch observation was performed 25.3 hr 
after the the trigger.

Inside the 1.8 arcsec XRT error circle (Evans et al., GCN #13406) we 
detect a fading object in all bands at coordinates RA(J2000) = 
05:21:23.52, DEC(J2000) = -58:32:58.3 (+/- 0.3 arcsec).

During the first night we obtained exposures of 3120s in JHK and 2550s in 
g'r'i'z'. At a mid time of 2.08 hrs after the trigger we measure the 
following preliminary magnitudes (all in the AB system)

  g' = 21.7 +- 0.1,
  r' = 21.3 +- 0.1,
  i' = 20.8 +- 0.1,
  z' = 20.8 +- 0.1,
  J  = 20.3 +- 0.1,
  H  = 20.5 +- 0.2,
  K  = 20.1 +- 0.3.

The object faded in r' by about 1.0 mag between the first and the second 
epoch. We therefore propose this source to be the afterglow of GRB 
120701A.

All magnitudes are derived based on calibrating the images against GROND 
zeropoints and 2MASS field stars. The Galactic reddening along the line of 
sight is E(B-V) =0.02 mag (Schlegel et al. 1998).


GRB_name: GRB120701A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13410
SUBJECT: GRB 120701A: Swift/UVOT Detection
DATE:    12/07/03 21:34:12 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and T. N. Ukwatta(MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120701A
89 s after the BAT trigger (Barthelmy et al. GCN Circ. 13404).
A fading source consistent with the XRT and GROND positions (Evans et 
al., GCN Circ. 13406 and Elliott et al., GCN Circ. 13409) is detected in 
the initial UVOT exposures in white and U.

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 and summed exposures are:

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

white_FC            89         239           147         18.27  0.06
white              880        1030           147         20.01  0.36
v                 6603        6809           197        >18.8
b                 5994       18439           494        >20.3
u_FC               303         553           245         19.16  0.23
u                 5788        5988           197        >19.9
w1               11812       12668           842        >20.6
m2                6815       22538           969        >20.7
w2                6405        6605           197        >19.8

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


GRB_name: GRB120703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13411
SUBJECT: GRB 120703A: NOT optical observation
DATE:    12/07/04 07:56:33 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), D. Malesani, J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (U.
Leicester), K. Karhunen (U. Turku) report on behalf of a larger
collaboration,

We observed the field of GRB 120703A (Zhang et al., GCN 13408) using
the 2.5m Nordic Optical Telescope (NOT) equipped with StanCam.
Observations started at 04:02:42 UT on 2012-07-04 (i.e., 10.62 hr
after the BAT trigger) and 6x300s R-band frames were obtained.

An optical source was marginally detected in the stacked image at coordinates

RA (J2000)  = 22:37:25.61
Dec (J2000) = -29:43:23.7

with an uncertainty of ~0.5 arcsec radius, being consistent, but
slightly offset, with the UVOT position. The source had R~21.7
calibrated against nearby USNO star.


GRB_name: GRB120703A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13412
SUBJECT: Konus-Wind observation of GRB 120703A
DATE:    12/07/04 07:58:07 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 120703A (Swift-BAT trigger #525671:
B.-B. Zhang et al., GCN 13408)
triggered Konus-Wind at T0=62723.578s UT (17:25:23.578)

The burst light curve shows a single peak
with a total duration of ~12.5 s.
The emission is seen up to ~7 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120703_T62723/

As observed by Konus-Wind the burst
had a fluence of (7.7  1.0)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.960 s,
of (5.4  1.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+8.448 s)
is well fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which:
alpha = -0.81 (-0.25, +0.30),
and Ep = 295(-56, +88) keV,
chi2 = 96.8/84 dof.
Fitting this spectrum with the GRB (Band) function yields
the following model parameters:
the low-energy photon index alpha = -0.67 (-0.37, +0.54),
the high energy photon index beta = -2.7 (<-2.3),
the peak energy Ep = 256(-75, +100) keV,
chi2 = 96.4/83 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+0.256 s) is best fitted
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which:
alpha = -0.50 (-0.37, +0.46),
and Ep = 410(-90, +150) keV,
chi2 = 21.5/22 dof.

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


GRB_name: GRB120624B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13413
SUBJECT: GRB 120624B Suzaku WAM observation of the prompt emission
DATE:    12/07/04 08:26:22 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

A. Sakamoto, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara,
M. Asahina, S. Kobayashi, H. Ueno (Saitama U.),
M. Akiyama, N. Ohmori,  M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, Y. E. Nakagawa (Waseda U.),
Y. Hanabata,  T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), M. Kokubun,
T. Takahashi (ISAS/JAXA),ã€€Y. Urata, P. Tsai (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo),ã€€on behalf of the Suzaku WAM team, report:

The long GRB 120624B (Fermi/GRM; Gruber et al., GCN 13377,Fermi/LAT;
Vianello et al., GCN 13379,Konus-Wind; Golenetskii et al., GCN
13382,Swift/BAT; Sakamoto et al., GCN 13384)ã€€was detected by the Suzaku
Wide-band  All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 22:19:30.985 UT (=T0).

The observed light curve shows  a multi-peaked structure starting at
T0+5 s, ending at T0+279 s, with a duration (T90) of about 274 seconds.
The fluence inã€€100 - 1000 keV was 1.22(-0.06 +0.02) x 10^-4 erg/cm^2.
The 1-s peak flux measured from T0+274.5s was
6.88(-2.11 +0.27) photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from T0-20s to
T0+285s is well fitted by a GRB Band model:
the low-energy photon index alpha: -1.03(-0.16 +0.20),
                      beta        : -2.61 (-0.33, +0.20)
and the peak energy Epeak: 628(-73 +84) keV (chi^2/d.o.f = 72.1/50).

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

----
The light curves for this burst will be available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB120703A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13414
SUBJECT: GRB 120703A: Swift-BAT refined analysis
DATE:    12/07/04 13:10:16 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),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), J. Tueller (GSFC),
T. N. Ukwatta (MSU), B.-B. Zhang (PSU) (i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120703A (trigger #525671)
(Zhang, et al., GCN Circ. 13408).  The BAT ground-calculated position is
RA, Dec = 339.353, -29.726 deg, which is 
   RA(J2000)  =  22h 37m 24.7s 
   Dec(J2000) = -29d 43' 34.9" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
 
The mask-weighted light curve shows the burst started at ~T-45 sec with a weak
pulse with a width of about 20 sec.  The burst continues with a moderate increase
to a strong central pulse from T-0.2 to T+1.0 sec, and then a decay back
to baseline at ~T+45 sec.  T90 (15-350 keV) is 25.2 +- 4.3 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-7.27 to T+32.60 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.51 +- 0.06.  The fluence in the 15-150 keV band is 3.5 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band
is 10.5 +- 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/525671/BA/


GRB_name: GRB120703A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13415
SUBJECT: GRB 120703A: Enhanced Swift-XRT position
DATE:    12/07/04 23:24:19 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 7867 s of XRT Photon Counting mode data and 16 UVOT
images for GRB 120703A, 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 = 339.35690, -29.72350 which is equivalent
to:

RA (J2000): 22h 37m 25.66s
Dec (J2000): -29d 43' 24.6"

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: GRB120703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13416
SUBJECT: GRB 120703A: Swift-XRT refined Analysis
DATE:    12/07/04 23:34:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 12 ks of XRT data for GRB 120703A (-B. Zhang  et al.
GCN Circ. 13408), from 70 s to 68.9 ks after the  BAT trigger. The data
comprise 374 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 13415).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.69 (+0.04, -0.06), followed by a break at T+4130 s to
an alpha of 1.04 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.13, -0.12). The
best-fitting absorption column is  1.4 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 1.2 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (5.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.4 (+/-0.3) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: 7.0 sigma
Photon index:      2.00 (+0.13, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00525671.

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


GRB_name: GRB120703A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13417
SUBJECT: GRB 120703A: Fermi GBM detection
DATE:    12/07/05 02:29:05 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

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

"At 17:25:17 UT on 03 July 2012, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 120703A (trigger 363029120 / 
120703.726). This burst was also detected by Swift/BAT (Zhang, B.-B. 
et al., GCN 13408).  The GBM on-ground position is consistent with 
the Swift location.  The burst was also detected by Konus-Wind 
(Golenetskii, R. et al., GCN 13412).

The burst triggered an ARR (Automatic Repointing Request), causing 
Fermi to slew so the LAT would point to the source.

The GBM light curve is similiar to the Swift detection. We observe a
strong central pulse with fainter wings, the total pulse having a 
width of ~20s. We measure the duration (T90) of about 9.216s 
(50-300 keV). The time-averaged spectrum from T0-2.048 to T0+14.336 s 
is best fit by a Comptonized power-law function, with Epeak = 
305.6 +/- 21.1 keV and alpha = -1.06 +/- 0.03.  The fluence 
(10-1000 keV) in this time interval is (9.154 +/- 0.246)E-06 erg/cm^2.

The burst is also fit well with a Band function with Epeak = 
238.5 +/- 26.5, keV alpha = -0.98 +/- 0.05, and beta = -2.08 +/- 0.12.

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


GRB_name: GRB120703A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13418
SUBJECT: GRB 120703A:  Swift/UVOT Detection
DATE:    12/07/05 14:00:15 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and B.-B. Zhang (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120703A
90 s after the BAT trigger (Zhang et al., GCN Circ. 13408).
A source consistent with the XRT position (Goad et al., GCN Circ.
13415) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  22:37:25.67 = 339.35694 (deg.)
     Dec (J2000) = -29:43:23.8  = -29.72327 (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               90          240          147         18.48  0.06
v                 4299         4499          197        >19.5
b                 3684         5249          325        >20.9
u                  304          416          110         18.07  0.13
w1                4710         4909          197        >19.5
m2                4504         4704          197        >21.4
w2                4095         4294          197        >21.4

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


GRB_name: GRB120703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13420
SUBJECT: GRB 120703A: SMARTS optical/IR observations
DATE:    12/07/05 20:54:45 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU) reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 120703A
(GCN 13408, Zhang et al.) with a mid-exposure time of 13.7 hours
post-burst (2012-07-04 07:07 UT).  Total summed exposure
times amounted to 15 minutes in I and V and 12 minutes in J and K.

No source is detected at the position of the optical
afterglow (e.g. GCN 13411, Xu et al.; GCN 13418, Swenson
et al.) to approximate limiting magnitudes of I > 20.5, J > 18.5
and K > 17.4.  Magnitudes are calibrated using USNO-B1.0 stars in I,
and 2MASS stars in J and K.


GRB_name: GRB120624B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13421
SUBJECT: GRB 120624B: mm detection at PdBI
DATE:    12/07/06 06:34:59 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Bremer, J. M. Winters, S. Knig (IRAM Grenoble), A. de Ugarte Postigo 
and A. J. Castro-Tirado (IAA-CSIC Granada) on behalf of a larger 
collaboration, report:

"Following the detection of the intense GRB 120624B by different 
spacecraft (GCNC 13379, 13381,13382), we have conducted follow-up 
observations at 3 mm with the PdBI on June 28 and July 2. Consistent 
with the position of the proposed X-ray afterglow (GCNC 13394, 13400) we 
detect a 1 mJy source (6 sigma). Observations are ongoing".

This message can be quoted.


GRB_name: GRB120707A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13422
SUBJECT: GRB 120707A: Fermi GBM Detection of a Bright Burst
DATE:    12/07/08 05:55:26 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (NASA/USRA), report on behalf of the Fermi GBM Team:

"At 19:12:17.42 UT on 07 July 2012, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 120707A (trigger 363381140 / 120707.800).
The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 291.06, Dec = -34.44 (J2000 degrees, equivalent to
J2000 19h 24m, -34d 26'), with a statistical uncertainty of 1.0 degrees
(radius, 1-sigma containment, statistical only; there is additionally
a systematic error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 159 degrees.

The burst triggered an ARR (Automatic Repointing Request), causing 
Fermi to slew so the LAT would point to the source.  Because the burst 
was close to the Earth's limb, this maneuver was delayed, placing the 
GRB position near the LAT boresight starting about 1000 s after the GBM trigger time.

The GBM light curve shows a strong central  pulse with fainter wings
with a duration (T90) of about 50 s (50-300 keV). The time-averaged
spectrum from T0-3 to T0+57 s is best fit by a Band function with Epeak = 
174 +/- 7 keV, alpha = -1.17 +/- 0.03, and beta = -2.31 +/- 0.03.

The fluence (10-1000 keV) in this time interval is (1.1 +/- 0.007)E-4 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+29.1 s in the 10-1000 keV band
is 62 +/- 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: GRB120709A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13423
SUBJECT: GRB 120709A: Fermi-LAT Detection
DATE:    12/07/10 08:05:30 GMT
FROM:    Daniel Kocevski at SLAC  <dankocevski@gmail.com>

Daniel Kocevski (Stanford Univ.), Giacomo Vianello (CIFS/SLAC), and James Chiang (KIPAC/SLAC) report on behalf of the Fermi LAT Team:

Fermi-LAT has detected high energy emission from the long, hard and bright GRB 120709A in ground analysis. The GRB was triggered on by the GBM on July 9th, 2012 at 21:11:41 UTC (trigger 363561103).

The best GBM position was ~22 deg off-axis for the duration of the prompt emission (~35 seconds), and remained within the Fermi/LAT nominal field of view for an additional ~650 seconds.

Using a non-standard data selection most sensitive in the tens-of-MeV energy range and with a broader acceptance, we significantly detected the burst between ~T0 and ~T0+5 s. The significance of the excess corresponds to ~7 sigma. The light curve also shows a secondary peaks at ~11s of lesser significance, but coincident with the second of three peaks seen in the GBM light curve.

A preliminary maximum-likelihood analysis of the E>75MeV P7SOURCE_V6 LAT data generated during the interval T0, T0+100s revealed a significant transient source, with a spectrum well described by a power law of index -2.0 +/- 0.3 (68% C.L. statistical only). Integrating over a duration covering T0 to T0+200s, we obtained the best LAT on-ground localization of:

RA(J2000) = 318.41 deg
Dec(J2000) = -50.03 deg

with an error radius of 0.35 deg (90% containment, statistical error only), which is 6.3 deg from the best GBM localization.

The zenith angle for this source was ~42.3 deg at the time of the trigger, thus very far from the Earth limb.

A Swift/ToO request has been submitted.

The Fermi-LAT point of contact for this burst is Daniel Kocevski (kocevski@stanford.edu)


GRB_name: GRB120707A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13424
SUBJECT: IPN Triangulation of GRB 120707A
DATE:    12/07/10 17:52:25 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,

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 long-duration, intense GRB 120707A (Younes, GCN 13422) has been 
observed by Fermi (GBM: trigger 363381140), Konus-Wind, INTEGRAL 
(SPI-ACS), Swift (BAT), Mars Odyssey (HEND), and Suzaku (WAM), so far, 
at about 69140 s UT (19:12:20). The burst was outside the coded field of 
view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   291.874 (19h 27m 30s) -32.770 (-32d 46' 12")
  Corners:
   293.104 (19h 32m 25s) -36.566 (-36d 33' 56")
   292.808 (19h 31m 14s) -37.093 (-37d 05' 36")
   290.585 (19h 22m 20s) -27.663 (-27d 39' 48")
   290.769 (19h 23m 05s) -26.473 (-26d 28' 23")
  ---------------------------------------------

The error box area is 3.50 sq. deg, and its maximum dimension is 10.8 deg.
This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120707_T69146/IPN/


GRB_name: GRB120707A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13425
SUBJECT: Konus-Wind observation of GRB 120707A
DATE:    12/07/10 18:02:26 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 intense GRB 120707A
(GBM trigger 363381140: Younes, GCN 13422;
IPN localization: Hurley at al., GCN 13424)
triggered Konus-Wind at T0=69146.810s UT (19:12:26.810)

The light curve shows a strong pulse peaked at ~T0+24 s.
A total duration of the burst is ~95 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120707_T69146/

As observed by Konus-Wind the burst
had a fluence of 1.35(-0.15,+0.15)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+24.064 s,
of 1.05(-0.15,+0.15)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+57.600 s)
is best fit in the 30 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.54 (-0.09, +0.12),
the high energy photon index beta = -2.22 (-0.24, +0.14),
the peak energy Ep = 190(-37, +41) keV,
chi2 = 74.9/82 dof.

The spectrum at the maximum count rate
(measured from T0+20.224 to T0+26.368 s)
is best fit in the 30 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.30 (-0.12, +0.16),
the high energy photon index beta = -2.3 (-0.38, +0.16),
the peak energy Ep = 213(-41, +53) keV,
chi2 = 86.4/82 dof.

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


GRB_name: GRB120709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13426
SUBJECT: GRB 120709A: optical afterglow limits
DATE:    12/07/10 19:42:25 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

J. Elliott, J. Greiner (both MPE Garching), A. Nicuesa Guelbenzu, S. Schmidl, 
S. Klose (all TLS Tautenburg) report on behalf of the GROND team:
 
We observed the field of GRB 120709A (Kocevski et al., GCN #13423) with the 
Wide-Field Imager (WFI; 33 arcmin field-of-view) at the 2.2 m MPG/ESO 
telescope at La Silla Observatory (Chile). In order to cover the 0.35 deg 
radius error circle, a mosaic of 2*2 pointings was performed. The sequence 
of exposures started at 07:42 UT, 10.5 hrs after the GRB, with 10 min 
exposure per tile. The observations were performed at an average airmass 
of 1.13, mean seeing of 1 arcsec, and a Moon distance of 80 deg.

We compared our R-band images with the DSS2-R plates, but find no new object
brighter than R~19 mag within the 0.35 deg radius error circle.


GRB_name: GRB120709A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13427
SUBJECT: GRB 120709A: Matched filter analysis of Fermi-LAT data
DATE:    12/07/10 20:51:49 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

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

We analyzed Fermi/LAT data of GRB 120709A (Kocevski et al., GCN 13423)
as a follow-up of routine search in GBM trigger catalogs in our LAT data
processing pipeline using 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).
We use a standard data selection method (with Energy range of 100 MeV <
E < 300 GeV). About 10 photons associated with GRB are detected above
100 MeV in 47.5s duration, with the highest energy of ~3.07 GeV at 2.04s
after the burst. The GRB location estimated by the matched filter
technique is RA = 320.23, Dec = -51.13 with uncertainty ~0.5 degree,
consistent with the location given in GCN 13423.

The photon information can be found in the following link including the
skymap:
http://www.rotse.net/LAT/GBMTriggers/363561103/


GRB_name: GRB120709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13428
SUBJECT: GRB 120709A: Swift-XRT observations
DATE:    12/07/10 21:36:13 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe and Craig Swenson (PSU) report on behalf of the Swift-XRT
team:

We have analysed 4.0 ks of XRT data for the Fermi/LAT-detected burst:
GRB 120709A (Kocevski et al. GCN Circ. 13423), from 60.2 ks to 67.4 ks
after the  Fermi/LAT trigger. The data are entirely in Photon Counting
(PC) mode.  An uncatalogues X-ray source is detected within the
Fermi/LAT error circle. Using 1389 s of PC mode data and 1 UVOT images,
we find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
318.17277, -49.97297 which is equivalent to:

RA (J2000): 21h 12m 41.47s
Dec(J2000): -49d 58' 22.7"

with an uncertainty of 3.5 arcsec (radius, 90% confidence). This
position is 11.25 arcmin from the Fermi/LAT position.  The source has a
mean count rate of 8.8e-03 ct/sec; we cannot determine at the present
time whether it is fading.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.7 (+0.7, -0.6). The
best-fitting absorption column is  consistent with 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 2.3 x 10^-11 (2.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+7.5, -0) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.7 (+0.7, -0.6)

Note that the XRT only covered the center of the FERMI/LAT error circle
(about 40%) given in Kocevski et al. (GCN Circ. 12423). There are two
additional X-ray sources in the XRT image which are known sources. 


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020222.

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


GRB_name: GRB120709A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13429
SUBJECT: GRB 120709A: Fermi GBM detection
DATE:    12/07/10 23:19:36 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

Sylvain Guiriec (GSFC), Valerie Connaughton (UAH)
and Michael Briggs (UAH)
report on behalf of the Fermi GBM Team:

"At 21:11:40.37 UT on 09 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120709A (trigger 120709883 / 120709.883).

The on-ground calculated location, using the GBM trigger
data, is RA = 320.02, DEC = -47.87 (J2000 degrees,
equivalent to 21h20m04, -47d52'12), with an uncertainty
of  1.70 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 22 degrees.
The burst was also seen by the LAT (Kocevski et al., GCN 13423)

The GBM light curve consists of 3 intense peaks
with a duration (T90) of about 30 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+41s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.22 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 449 +/- 55 keV

The event fluence (10-1000 keV) in this time interval is
(1.43 +/- 0.04)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+11.65 s in the 10-1000 keV band
is 11.4897 +/- 0.2869 ph/s/cm^2.

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


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13430
SUBJECT: Skynet/PROMPT Observations of GRB120711A
DATE:    12/07/11 03:23:16 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. Lacluyze, J. Haislip, 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 GRB12711 (INTEGRAL trigger 6599) in B, V, and 
R starting 37 seconds after the burst.  Although no afterglow was detected 
in the initial exposures, a transient source was detected at 06:18:42.839 
-70:59:56.78 (J2000).  The source rapidly brightened, peaking at roughly 
112 seconds after the trigger.  Preliminary peak magnitudes, calibrated to 
~5 UNSO B1.0 stars are as follows:

Time Tel Filt Mag 1sigERR
112 P4 R 12.117 0.008 
113 P1 V 12.593 0.014
116 P3 B 14.061 0.014

The post-peak temporal index is estimated to be -2.1, suggesting a reverse 
shock.

Further observations are ongoing.


GRB_name: GRB120711B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13431
SUBJECT: Swift detection of GRB 120711B or a new Galactic transient
DATE:    12/07/11 03:40:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. J. Page (UCL-MSSL), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
F. E. Marshall (NASA/GSFC), S. R. Oates (UCL-MSSL),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:

At 03:11:02.58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located what may be GRB 120711B (trigger=526270).  Swift slewed immediately
to the position. The BAT on-board calculated location is 
RA, Dec 331.668, +60.020 which is 
   RA(J2000) = 22h 06m 40s
   Dec(J2000) = 60d 01' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve does not show any obvious
variation, which is typical for an image trigger (64 second duration). 

The XRT began observing the field at 03:13:05.6 UT, 123.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 331.69037, 60.02173 which
is equivalent to:
   RA(J2000)  = 22h 06m 45.69s
   Dec(J2000) = +60d 01' 18.2"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 40 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 does not constrain the column density. 

The initial flux in the 2.5 s image was 8.75e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 260 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain extinction expected. 

Due to the proximity of the source to the Galactic plane (3.46 degrees),
the fact that this source was detected in the first image following
the SAA, and the relative constancy of the XRT light curve, we
believe that this is more likely to be a previously-unknown
Galactic source rather than a GRB.  However we will need the 
complete downlinked data to determine the nature of the source. 

Burst Advocate for this burst is M. J. Page (mjp 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: GRB120711A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13432
SUBJECT: GRB 120711A: ROTSE-III confirm of Optical Counterpart 
DATE:    12/07/11 03:43:34 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich), report on behalf of the ROTSE collaboration: 

ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia, responded
to GRB 120711A (Integral trigger 6599). The first image was at 02:45:54.4
UT, 59.1 s after the burst (5.4 s after the GCN notice time). We also
detected the suggested optical afterglow found by Skynet/PROMPT (Lacluyze et
al., GCN 13430). The afterglow is detected in our first co-add image with
Mag ~14.2 (mean time of ~60s) and decayed fainter than 15.8 mag in the
second co-add (mean time of 460s). The unfiltered images are calibrated
relative to USNO A2.0. 

Continuing observations are in progress.

 


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13433
SUBJECT: Continued Skynet/PROMPT observations of GRB120711A
DATE:    12/07/11 04:14:24 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. Lacluyze, J. Haislip, 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 continued to observe the field of GRB120711A (INTEGRAL trigger 6599, 
GCN 13430 and 13432.)  A preliminary light curve in B, V, and R, calibrated 
to ~5 USNO B1.0 stars can be found at:

http://skynet.unc.edu/grb/grb120711a.png


GRB_name: GRB120711A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13434
SUBJECT: GRB 120711A: an bright long GRB detected with INTEGRAL
DATE:    12/07/11 04:28:05 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

a long and bright GRB has been detected by IBAS in the IBIS/ISGRI data at 02:44:48 UT on July 11th 2012. The GRB lasts approximately 135 s and its refined coordinates are

RA: 94.703 [degrees]
DEC: -71.001 [degrees]

with an uncertainty of 1.1 arc min (90% c.l.).

A preliminary spectral analysis yields a fluence of 1.6e-5 erg/cmsq in the 20-200 keV energy band and a peak flux over 1 s of 10 photons/cmsq/s in the same energy band. Please note that due to telemetry saturation at satellite levels there values are only lower limits. 
We note that our position is consistent with the optical transient reported by Lacluyze et al. (CGN 13430).
A plot of the light curve has been posted at 
http://ibas.iasf-milano.inaf.it/IBAS_Results.html
This message can be cited.


GRB_name: GRB120711A
Detection_method: IBAS
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13435
SUBJECT: GRB 120711A: a possible X-ray transient
DATE:    12/07/11 09:59:40 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

A refined analysis of a larger IBIS/ISGRI dataset corresponding to the GRB120711A (GCN 13434), revealed a faint emission, lasting for at least ~1000s, after the main outburst.
Being this duration unusual for a GRB, we are at present unable to rule out a different nature for this event (e.g. a bright transient in the direction of the LMC).

The event has been detected also using the SPI Anti Coincidence System (ACS) on board of INTEGRAL which is not saturated and shows a highly structured light-curve at the peak http://www.isdc.unige.ch/~bozzo/lightcurve.dat .

Further observations are encouraged.

[GCN OPS NOTE(11jul12): Per author's request, the 13432 reference was changed to 13434.]


GRB_name: GRB120711A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13436
SUBJECT: GRB 120711A: MAXI/GSC detection
DATE:    12/07/11 10:14:08 GMT
FROM:    Mikio Morii at Tokyo Inst Tech  <morii@hp.phys.titech.ac.jp>

M. Serino (RIKEN), M. Morii(Tokyo Tech), S. Nakahira (JAXA),
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto, J. Sugimoto, M. Matsuoka (RIKEN), 
A. Yoshida (AGU),
H. Tsunemi, M. Kimura (Osaka U.), 
H. Negoro, M. Nakajima, M. Asada, H. Sakakibara, 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.), 
K. Yamaoka (Waseda U.)
report on behalf of the MAXI team:

MAXI/GSC triggered at 2012-07-11T02:45:12 UT on a bright uncatalogued X-ray transient source.
The transient emission lasted at least 50 seconds
within the 67 second long triangular transit response of
MAXI/GSC.

Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (94.04 deg, -71.09 deg) = (06 16 10,$B!!(B-71 05 37)(J2000)

with a 90% C.L. statistical error of 12 arcmin and an additional systematic uncertainty of 0.1 deg (90% containment radius).

Without assuming the source constancy, we obtain a rectangular 
error box (90%C.L.) with the following corners: 

(R.A., Dec) = (+94.86 deg, -70.99 deg) = (06 19 29, -70 59 26)(J2000)
(R.A., Dec) = (+94.93 deg, -71.21 deg) = (06 19 44, -71 12 23)(J2000)
(R.A., Dec) = (+91.53 deg, -71.22 deg) = (06 06 06, -71 13 27)(J2000)
(R.A., Dec) = (+91.52 deg, -71.01 deg) = (06 06 05, -71 00 26)(J2000)

This error region includes the position of GRB 120711A 
reported by Lacluyze et al. (GCN #13430) and Gotz et al. (GCN #13434).

Fixing the source position to that of GRB 120711A,
we obtained the light curve corrected with the transit response
within the GSC scan.
It was variable within the scan, and
the peak flux was  610 +- 130 (mCrab, 2-20 keV) on 2012-07-11 02:44:54 UT.


GRB_name: GRB120711A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13437
SUBJECT: GRB 120711A: Fermi GBM observation
DATE:    12/07/11 10:18:39 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) and Vronique Pelassa (UAH)
report on behalf of the Fermi GBM Team:

"At 02:44:53.29 UT on 11 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120711A (trigger 363667496 / 120711115).
which was also detected by the INTEGRAL/IBAS
(Gotz et al. 2012, GCN 13434).
The GBM on-ground location is consistent with the INTEGRAL position.

The angle from the Fermi LAT boresight is 140 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.

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

The GBM light curve consists of a precursor which is
followed by a hard, main emission after ~ 50 s, lasting for
another ~ 50 s. The T90 is about 44 s (50-300 keV).
The time-averaged spectrum from T0-1 s to T0+131 s is
best fit by a Band function with Epeak = 973 +/- 35 keV,
alpha = -0.94 +/- 0.01, and beta = -2.40 +/- 0.04.
This spectrum is typical of a bright, hard GRB, and would be 
highly unusual for an X-ray transient (Bozzo et al. 2012, GCN 13435).

The event fluence (10-1000 keV) in this time interval is
(1.942 +/- 0.002)E-04 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+95 s in the 10-1000 keV band
is 26.7 +/- 0.6 ph/s/cm^2.

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


GRB_name: GRB120711A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13438
SUBJECT: GRB 120711A: GROND photometric redshift 
DATE:    12/07/11 11:11:49 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 120711A (INTEGRAL trigger 6599: Gotz et al., 
GCN 13434; Bozzo et al., GCN 13435; MAXI/GSC detection: Serino et al., GCN 
13436; Fermi/GBM trigger 363667496 / 120711115: Gruber & Pelassa, GCN 
13427) 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 on July 11, 08:34 UT, 5.8 hrs after the trigger as 
soon the location became visible at La Silla. The afterglow (Lacluyze et 
al., GCN 13430, 13433; Zheng, GCN 13432) is clearly detected in all bands.

For an exposure of 8 min in JHK and 7.66 min in g'r'i'z', at an average 
airmass of 2.5 and an average seeing of 2".0, we measure the following 
preliminary AB magnitudes

    g' = 20.9  +/- 0.1
    r' = 20.2  +/- 0.1
    i' = 19.6  +/- 0.1
    z' = 19.4  +/- 0.1
    J  = 18.6  +/- 0.1
    H  = 18.2  +/- 0.1
    K  = 18.0  +/- 0.1

The SED, after correction for Galactic reddening along the line of sight 
(E(B-V)=0.09 mag; Schlegel et al. 1998), can be described by a power law 
(beta ~ 1.4) with a reduced flux in the g-band, suggesting a photometric 
redshift of about 3. We note that also the PROMPT afterglow light curve 
(http://skynet.unc.edu/grb/grb120711a.png) supports a drop-out in the blue 
bands.

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


GRB_name: GRB120711A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13439
SUBJECT: GRB 120711A: REM NIR early time detection
DATE:    12/07/11 11:31:46 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

D. Fugazza, S. Covino, A. Rossi on behalf of the REM team report:


We imaged the field of GRB120711A (Gotz et al., GCN 13434 and Bozzo et al., GCN 13435) with the NIR camera (the optical camera is at present under maintenance) of the REM 60cm telescope located at La Silla. 

The bright optical counterpart reported in GCN 13430 (Lacluyze et al.), GCN 13432 (Zheng et al.) and GCN 13438 (Elliot et al.) is well detected in the NIR at a peak magnitude of H = 11.90 + 0.05 between 2-4 minutes after the burst. The source was then fading rapidly remaining approximately at the same magnitude, H~13, for several more minutes.

Data have been calibrated by isolated not-saturated 2MASS stars in the field.


GRB_name: GRB120709A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13440
SUBJECT: Konus-Wind observation of GRB 120709A
DATE:    12/07/11 11:55:36 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 GRB 120709A
(GBM trigger 120709883: Guiriec et al., GCN 13429;
Fermi/LAT detection: Kocevski et al., GCN 13423)
triggered Konus-Wind at T0=76303.609s UT (21:11:43.609)

The light curve shows multiple pulses grouped to three main episodes.
A total duration of the burst is ~25 s.

The emission is seen up to ~7 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120709_T76303/

As observed by Konus-Wind the burst
had a fluence of 1.8(-0.9,+1.0)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+11.968 s,
of 6.4(-1.6,+2.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+24.832 s)
is well fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which:
alpha = -0.86 (-0.25, +0.31),
and Ep = 414(-117, +233) keV,
chi2 = 75.8/84 dof.
This spectrum is equally well fit by the GRB (Band) function
with the following model parameters:
the low-energy photon index alpha = -0.68 (-0.45, +0.56),
the high energy photon index beta = -2.0 (<-1.7),
the peak energy Ep = 296(-100, +356) keV,
chi2 = 75.4/83 dof.

The spectrum at the maximum count rate
(measured from T0+8.848 to T0+16.640 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which:
alpha = -0.94 (-0.23, +0.28),
and Ep = 643(-216, +470) keV,
chi2 = 81.6/84 dof.

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


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13441
SUBJECT: GRB 120711A Gemini-S likely redshift 
DATE:    12/07/11 12:46:35 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir, K. Wiersema (U. Leicester), A. J. Levan (U. Warwick),
D. Fox (Penn State), A. Fruchter (STScI) and D. Krogsrud (Gemini)
report on behalf of a larger collaboration:

We observed the afterglow of GRB 120711A (Gotz et al. GCN 12434;
Lacluyze et al. GCN 12430) using the GMOS-S spectrograph on Gemini-South.

Observations began at 2012-7-11 10:08 UT, about 7.5 hr post-burst.
The data were obtained at high air-mass and on the boundary of twilight,
so the signal-to-noise is rather poor.  Nevertheless,
in the spectrum we identify lines of MgII (2797/2804A) and
FeII (2374/2383/2587/2600A) at a common redshift of z=1.405.

This therefore provides a robust lower-limit to the redshift of the GRB.
Furthermore, given the lack of other absorption features, in particular
any matching a redshift z~3 (Elliott et al. GCN 13438), we tentatively
identify z=1.405 as the most likely GRB redshift.


GRB_name: GRB120711A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13442
SUBJECT: GRB 120711A: Swift-XRT observations
DATE:    12/07/11 13:00:00 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

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

We have analysed 657 s of XRT data for the INTEGRAL-detected burst: GRB
120711A (Gotz et al. GCN Circ. 13434), from 8.3 ks to 20.0 ks after the
 INTEGRAL trigger. The data comprise 269 s in Windowed Timing (WT) mode
with the remainder in Photon Counting (PC) mode.  An X-ray source is
detected within the INTEGRAL error circle. Using 336 s of PC mode data
and 1 UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 94.67830, -70.99905 which is equivalent to:

RA (J2000): 06h 18m 42.79s
Dec(J2000): -70d 59' 56.6"

with an uncertainty of 1.7 arcsec (radius, 90% confidence). This
position is 29 arcsec from the INTEGRAL position and 0.3 arcsec from
the Skynet/PROMPT position (LaCluyze et al. GCN Circ. 13430). 

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.59 (+0.16, -0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.15 (+/-0.11). The
best-fitting absorption column is  3.6 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 7.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.80 (+0.25, -0.23)
and a best-fitting absorption column of 2.4 (+0.9, -0.8) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.5 x 10^-11 (6.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 7.9 x 10^20 cm^-2
Excess significance: 3.2 sigma
Photon index:      1.80 (+0.25, -0.23)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020223.

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


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13443
SUBJECT: GRB 120711A: MASTER  early OT detection
DATE:    12/07/11 15:51:48 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)

D. Denisenko, A. Kuznetsov, V. Lipunov, E. Gorbovskoy, V. Kornilov, 
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
INTEGRAL TRIGGER_NUM 6599 = Fermi TRIGGER_NUM: 363667496
60 sec after INTEGRAL trigger Time (Gotz et al., GCN 13434, Gruber 
and Pelassa, GCN 13437) on 2012-07-11 at 02:45:54.107 UT.

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

On our first unfiltered image (5 sec exposure) we have not found any OT.
We see OT (Lacluyze et al., GCN 13430, Zheng et al., GCN 13432, Elliot et 
al., GCN 13438, Fugazza et al., GCN 13439 and Tanvir et al., GCN 13441)
on the sum of 4 images obtained between T0+121s and T0+141s with the
unfiltered magnitude 12.5. Nothing is visible at the OT position on 
the individual (m_lim = 12.0) and combined (m_lim=13.0) images obtained 
before T0+121s and after T0+141s.

This message can be cited.


GRB_name: GRB120711A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13444
SUBJECT: GRB 120711A: Fermi LAT detection
DATE:    12/07/11 17:29:37 GMT
FROM:    Thomas P.H. Tam at Nat.Tsing Hua U.  <grbtom@gmail.com>

P.H.T. Tam, K.L. Li and A.K.H. Kong (NTHU) report:

We report on the Fermi Large Area Telescope (LAT) detection of >100 MeV
gamma-ray emission from the direction of the bright GRB 120711A, which
triggered INTEGRAL (Gotz et al., GCN 13434), MAXI/GSC (Serino et al., GCN
13436), and Fermi/GBM (Gruber et al., GCN 13437). The GRB position was
outside the LAT field of view at the GRB onset (c.f. GCN 13437). However,
gamma-ray emission up to around 2 GeV was detected from the GRB direction
from 0.8 ks to ~7 ks after the burst. Such duration is one of the longest
ever observed for a GRB in GeV domain.

Using the data obtained from the above period, an unbinned likelihood
analysis resulted in a detection significance of ~7 sigma, and a photon
spectral index of -1.8+-0.3. We localized the LAT emission to be at RA, DEC
(J2000 deg) = 94.58, -70.93, with a statistical error of ~0.17 deg (68%
CL), which is compatible with the Swift/XRT position (Beardmore et al., GCN
13442).


GRB_name: GRB120707A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13445
SUBJECT: Konus-Wind observation of GRB 120707A
DATE:    12/07/11 18:30:58 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 hard intense GRB 120711A
(detected by the INTEGRAL/IBAS Gotz et al., GCN 13434;
MAXI/GSC detection: Serino et al., GCN 13436;
Fermi/GBM trigger 363667496/120711115: Gruber & Palassa, GCN 13437;
Fermi/LAT detection: Tam, Li & Kong, GCN 13444)
triggered Konus-Wind at T0=09955.810s UT (02:45:55.810)

The light curve starts with a precursor at ~T0-65s followed by
a strong hard double pulse lasting from ~T0-3 s to ~T0+50 s.
Several short (100 - 200 ms) bright spikes are well detected
over the general burst light curve in the ~T0+30 s to ~T0+40 s
time interval.
A a weak decaying emission tail in the soft energy channel
G1(25-90 keV) is detectable till at least ~T0+400s.
The emission during the main phase of the event is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120711_T09955/

As observed by Konus-Wind the burst
had a fluence of 3.8(-0.2,+0.2)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+32.576 s,
of 3.6(-0.4,+0.4)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+46.336 s)
is best fit in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.97 (-0.02, +0.02),
the high energy photon index beta = -2.7 (-0.3, +0.2),
the peak energy Ep = 1060(-60, +60) keV,
chi2 = 95.7/87 dof.

The spectrum at the maximum count rate
(measured from T0+30.208 to T0+34.560 s)
is best fit in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.93 (-0.04, +0.04),
the high energy photon index beta = -2.5 (-0.5, +0.3),
the peak energy Ep = 1400(-160, +170) keV,
chi2 = 85.5/87 dof.

Assuming the likely GRB redshift of z=1.405 (Tanvir et al., GCN 13441)
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 (1.95  0.1)x10^54 erg,
the isotropic peak luminosity L_iso_max is (4.5  0.5)x10^53 erg/s,
and Ep_rest is (2550  150) keV.

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


GRB_name: GRB120711A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13446
SUBJECT: Konus-Wind observation of GRB 120711A
DATE:    12/07/11 18:35:12 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 hard intense GRB 120711A
(detected by the INTEGRAL/IBAS Gotz et al., GCN 13434;
MAXI/GSC detection: Serino et al., GCN 13436;
Fermi/GBM trigger 363667496/120711115: Gruber & Palassa, GCN 13437;
Fermi/LAT detection: Tam, Li & Kong, GCN 13444)
triggered Konus-Wind at T0=09955.810s UT (02:45:55.810)

The light curve starts with a precursor at ~T0-65s followed by
a strong hard double pulse lasting from ~T0-3 s to ~T0+50 s.
Several short (100 - 200 ms) bright spikes are well detected
over the general burst light curve in the ~T0+30 s to ~T0+40 s
time interval.
A a weak decaying emission tail in the soft energy channel
G1(25-90 keV) is detectable till at least ~T0+400s.
The emission during the main phase of the event is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120711_T09955/

As observed by Konus-Wind the burst
had a fluence of 3.8(-0.2,+0.2)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+32.576 s,
of 3.6(-0.4,+0.4)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+46.336 s)
is best fit in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.97 (-0.02, +0.02),
the high energy photon index beta = -2.7 (-0.3, +0.2),
the peak energy Ep = 1060(-60, +60) keV,
chi2 = 95.7/87 dof.

The spectrum at the maximum count rate
(measured from T0+30.208 to T0+34.560 s)
is best fit in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.93 (-0.04, +0.04),
the high energy photon index beta = -2.5 (-0.5, +0.3),
the peak energy Ep = 1400(-160, +170) keV,
chi2 = 85.5/87 dof.

Assuming the likely GRB redshift of z=1.405 (Tanvir et al., GCN 13441)
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 (1.95  0.1)x10^54 erg,
the isotropic peak luminosity L_iso_max is (4.5  0.5)x10^53 erg/s,
and Ep_rest is (2550  150) keV.

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


GRB_name: GRB120709A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13447
SUBJECT: GRB 120709A: Swift/UVOT Observations
DATE:    12/07/11 20:20:12 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

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

Swift/UVOT began observations of GRB 120709A (Kocevski et al.
GCN Circ. 13423) 16.7 hours after the trigger.
Observations covered the central 16'x16' region of
the 0.35 deg. radius LAT error circle with the 
White, U, and V filters. No credible afterglow candidate
was seen in any of the exposures.

The candidate X-ray afterglow from observations with 
Swift/XRT (Grupe and Swenson GCN Circ. 13428) is too
near the edge of the UVOT images to do accurate
photometry except for the 568-second white exposure
starting 66.8 ks after the trigger and the 802-second
U exposure starting 66.0 ks after the trigger.
The catalogued optical source at the edge
of the XRT error circle is clearly detected with
UVOT, but there is no indication of any other source
consistent with the XRT position. Preliminary magnitudes
for the catalogued source and 3-sigma upper limits for
positions well removed from the catalogued source
using the UVOT photometric system (Breeveld et al. 2011,
AIP Conf. Proc. 1358, 373) are given below.

Filter   T_Start    Exposure   Source Mag   Upper Limit
           (ks)        (s)
white      66.8       568      19.3 +/- 0.1   21.8
u          66.0       802      19.0 +/- 0.1   21.1


GRB_name: GRB120711A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13448
SUBJECT: GRB 120711A: Swift/UVOT Observations
DATE:    12/07/11 21:55:34 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120711A
8216 s after the INTEGRAL trigger (Gotz et al., GCN Circ. 13434).
No significant optical afterglow consistent with the position given in 
Lacluyze et al. (GCN_Circ. 13430) is detected in the initial UVOT 
exposures. However, in the U filter, the source may be detected at this 
position with a significance of 2 sigma. The possible detection is 
included in the table.
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

b                 8464         8480           16         >18.7
u                 8380         8459           79         >19.4
w1                8216         8375          157         >19.8

u                 8380         8459           79        19.6  0.5 (2sig)


The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.08 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB120711B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13449
SUBJECT: GRB 120711B: Swift/UVOT Upper Limits
DATE:    12/07/11 21:56:05 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120711B
260 s after the BAT trigger (Page et al., GCN Circ. 13431).
No optical afterglow consistent with the XRT position (Page et al., GCN 
Circ. 13431) 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           260          410          147         >21.7
white              260          734          186         >21.8
v                  417          784           58         >18.9
b                  516          710           39         >19.8
u                  491          858           58         >19.5
w1                 466          833           58         >18.9
m2                 441          809           58         >19.3
w2                 566         6472          208         >20.2

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 1.13 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB120711B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13450
SUBJECT: GRB 120711B: Swift-BAT refined analysis
DATE:    12/07/11 22:05:20 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), M. J. Page (UCL-MSSL), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-141 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120711B (trigger #526270)
(Page, et al., GCN Circ. 13431).  The BAT ground-calculated position is
RA, Dec = 331.710, 59.996 deg, which is 
   RA(J2000)  =  22h 06m 50.5s 
   Dec(J2000) = +59d 59' 46.0" 
with an uncertainty of 3.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
 
The mask-weighted light curve shows the emission starting ~T-100 sec, 
peaking at ~T+20 sec, and slowly decaying out to T+875 sec.
T90 (15-350 keV) is 60 +- 19 sec (estimated error including systematics).
 
The time-averaged spectrum from T-12.1 to T+51.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.75 +- 0.32.  The fluence in the 15-150 keV band is 5.6 +- 1.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+13.11 sec in the 15-150 keV band
is 0.4 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

Contrary to our GCN 13431, we now think that this trigger is very likely GRB,
and not a new Galactic source.
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/526270/BA/


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13451
SUBJECT: GRB 120711A: ATCA 34GHz upper limit
DATE:    12/07/12 01:53:15 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 (Dark Cosmology / IAA)

We observed GRB120711A (GCN 13434) with the Australia Telescope
Compact Array at 34GHz for 26 minutes centered on 21:37UT Jul 11 2012
(T0+18.9hours) in stormy weather.

We detect no radio source at the location of the GRB (GCN 13430) and
place an upper limit of 3.6mJy on the flux of an afterglow.

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.


GRB_name: GRB120711A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13452
SUBJECT: GRB 120711A: Fermi LAT Detection
DATE:    12/07/12 02:03:05 GMT
FROM:    Daniel Kocevski at SLAC  <dankocevski@gmail.com>

Daniel Kocevski (Stanford Univ.) and Giacomo Vianello (CIFS/SLAC), Nicola Omodei (Stanford Univ.), and Seth Digel (SLAC) report on behalf of the Fermi LAT Team:

Fermi-LAT has detected high energy emission from the bright GRB 120711A in ground analysis. The GRB triggered the Fermi-GBM on July 11th, 2012 at 02:44:53.29 UTC (trigger 363667496/120711115, Gruber et al. GCN 13437) and was bright enough to result in a spacecraft autonomous repoint.

At the time of the GBM trigger, the angle between the GRB position and the LAT bore-sight was 134.4 degrees for the duration of the prompt emission, and remained outside the Fermi-LAT nominal field of view for an additional ~600 seconds.

A preliminary maximum-likelihood analysis of the E>75MeV P7TRANSIENT_V6 LAT data centered on the XRT position reported by Beardmore et al. (GCN 13442) generated for the interval T0+600s to T0+1100s revealed a significant transient source, with a spectrum well described by a power law of index -2.0 +/ 0.3 (68% C.L. statistical only). These results are in agreement with those found by Tam et al. (GCN 13444).  Using the data covering T0+600s to T0+1100s, we obtained the best LAT on-ground localization of:

RA(J2000) = 94.7 deg
Dec(J2000) = -70.9 deg

with an error radius of 0.16 deg (90% containment, statistical error only), which is 0.09 deg from the XRT position, and 0.07 deg from the position reported by Tam et al. (GCN 13444).

We note that this position is ~1.4 degrees away from the known variable gamma-ray source 2FGL J0601.1-7037, which has been associated with the blazar PKS 0601-70. In order to understand if the observed excess can be due to a brightening of the blazar we considered two nested models for our data, one including just the blazar, and one including both the blazar and a new source (the GRB). Our data favor the latter model, with the fit converging to a solution with a negligible contribution from the blazar, as expected from the mean flux reported in the Fermi 2FGL catalog (Nolan et al., 2012). An analysis using E>75MeV P7TRANSIENT_V6 data covering an interval before the burst (T0-6000s to T0-2000 s) shows no significant emission at the location of the blazar. Thus, 2FGL J0601.1-7037 is unlikely to be the source of the excess.

We caution against the use of data after ~T0+2600 s, because of a large Zenith angle of the GRB, potentially resulting in a strong contamination from terrestrial gamma-rays originating from charged particle interactions with Earth's atmosphere.

The Fermi-LAT point of contact for this burst is Daniel Kocevski
(kocevski@stanford.edu)


GRB_name: GRB120711B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13453
SUBJECT: GRB 120711B: Swift-XRT refined Analysis
DATE:    12/07/12 05:58:14 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

We have analysed 4.5 ks of XRT data for GRB 120711B (Page  et al. GCN
Circ. 13431), from 208 s to 47.2 ks after the  BAT trigger. The data
comprise 106 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. Using 551 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 =
331.69137, +60.02267 which is equivalent to:

RA (J2000): 22h 06m 45.93s
Dec(J2000): +60d 01' 21.6"

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=1.69 (+0.22, -0.17).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.5, -0.4). The
best-fitting absorption column is  2.4 (+0.9, -0.8) x 10^22 cm^-2, in
excess of the Galactic value of 7.2 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.5 (+0.4, -0.3) and
a best-fitting absorption column of 2.9 (+0.7, -0.6) x 10^22 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 9.9 x 10^-11 (1.7 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.9 (+0.7, -0.6) x 10^22 cm^-2
Galactic foreground: 7.2 x 10^21 cm^-2
Excess significance: 5.6 sigma
Photon index:      1.5 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00526270.

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


GRB_name: GRB120712A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13454
SUBJECT: GRB 120712A: Swift detection of a burst with optical afterglow
DATE:    12/07/12 13:52:34 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. J. Page (UCL-MSSL), A. A. Breeveld (UCL-MSSL), D. N. Burrows (PSU),
V. D'Elia (ASDC), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
N. P. M. Kuin (UCL-MSSL), O. M. Littlejohns (U Leicester),
F. E. Marshall (NASA/GSFC), S. R. Oates (UCL-MSSL),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
V. N. Yershov (UCL-MSSL) report on behalf of the Swift Team:

At 13:42:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120712A (trigger=526351).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 169.605, -20.061 which is 
   RA(J2000)  =  11h 18m 25s
   Dec(J2000) = -20d 03' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a couple of overlapping
peaks with a total duration of about 25 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~8 sec after the trigger. 

The XRT began observing the field at 13:43:58.2 UT, 90.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 169.59034, -20.03336 which is
equivalent to:
   RA(J2000)  = 11h 18m 21.68s
   Dec(J2000) = -20d 02' 00.1"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 111 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.60 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3
(+2.23/-1.94) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 95 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 11:18:21.23 = 169.58847
  DEC(J2000) = -20:02:01.8  = -20.03383
with a 90%-confidence error radius of about 1.10 arc sec. This position is 6.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.10. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.04. 

Burst Advocate for this burst is M. J. Page (mjp 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: GRB120712A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13455
SUBJECT: GRB 120712A: Swift-BAT refined analysis
DATE:    12/07/12 20:14:07 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),
M. J. Page (UCL-MSSL), 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-120 to T+254 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120712A (trigger #526351)
(Page, et al., GCN Circ. 13454).  The BAT ground-calculated position is
RA, Dec = 169.598, -20.051 deg, which is 
   RA(J2000)  =  11h 18m 23.6s 
   Dec(J2000) = -20d 03' 02.9" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 55%.
 
The mask-weighted light curve shows two main overlapping peaks starting 
at ~T-5 sec, peaking at ~T+0 and ~T+8 sec, and ending at ~T+20 sec.
T90 (15-350 keV) is 14.7 +- 3.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-4.57 to T+16.53 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.08.  The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+7.51 sec in the 15-150 keV band
is 2.4 +- 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/526351/BA/


GRB_name: GRB120712A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13456
SUBJECT: GRB 120712A: Enhanced Swift-XRT position
DATE:    12/07/12 22:28:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 5145 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 120712A, 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 = 169.58851, -20.03397 which is equivalent
to:

RA (J2000): 11h 18m 21.24s
Dec (J2000): -20d 02' 02.3"

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

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

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


GRB_name: GRB120712A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13457
SUBJECT: GRB 120712A: GROND Detection of the Optical/NIR Afterglow  Candidate and photo-z
DATE:    12/07/13 01:17:11 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott, P. Schady (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 120712A (Swift trigger 526351; Page et al.,
GCN #13454) 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 22:57 UT on 2012-07-12, 9.24 hours after the GRB
trigger, and are continuing. They were performed at an average seeing of
1".12 and at an average airmass of 1.27.

We found a single point source within the 1".5 enhanced Swift-XRT error
circle reported by Osborne et al. (GCN #13456) at

RA (J2000) = 11:18:21.24

DEC (J2000) = -20:02:01.4

with an uncertainty of 0".5 in each coordinate.

Based on images of 7.66 min of total exposures in g'r'i'z' and 8 min in
JHK, 9.5 hours post-burst, we estimate preliminary magnitudes (all in AB)
of

g' = 23.1 +/- 0.1,

r' = 21.3 +/- 0.1,

i' = 20.6 +/- 0.1,

z' = 20.5 +/- 0.1,

J  = 20.0 +/- 0.1,

H  = 19.8 +/- 0.2 and,

K  > 19.1.

Assuming no dust the SED is well fit with a spectral index of beta=1.1 +/-
0.1 at a redshift of z=4.0 +/- 0.2. Including host galaxy dust decreases
the redshift, although both solutions remain consistent within 1-sigma.

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)=0.04 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120712A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13458
SUBJECT: GRB 120712A Gemini-S redshift 
DATE:    12/07/13 01:17:34 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick) and D. Krogsrud (Gemini)
report on behalf of a larger collaboration:

We observed the afterglow of GRB 120712A (Page et al. GCN 12454;
using the GMOS-S spectrograph on Gemini-South in good conditions.

Observations began at 2012-7-12 23:43 UT, about 10 hr post-burst.
The spectrum reveals a clear Ly-a break, and many other absorption
features.  A provisional reduction gives a redshift of z=4.15, although
this figure will be refined with better calibration.


GRB_name: GRB120712A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13459
SUBJECT: GRB 120712A: Swift-XRT refined Analysis
DATE:    12/07/13 01:52:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 6.2 ks of XRT data for GRB 120712A (Page  et al. GCN
Circ. 13454), from 94 s to 12.9 ks after the  BAT trigger. The data
comprise 90 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 13456).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.87 (+/-0.06), followed by a break at T+3706 s to an
alpha of 1.80 (+0.33, -0.29).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.16 (+0.17, -0.14). The
best-fitting absorption column is  5.0 (+3.1, -1.4) x 10^20 cm^-2,
consistent with the Galactic value of 3.6 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 3.3 x 10^-11 (4.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.0 (+3.1, -1.4) x 10^20 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.16 (+0.17, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00526351.

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


GRB_name: GRB120712A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13460
SUBJECT: GRB 120712A: VLT/Xshooter redshift
DATE:    12/07/13 03:07:57 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), J. P. U. Fynbo (DARK/NBI), V. D'Elia (ASDC, INAF), N. R.
Tanvir (U. Leicester) report on behalf of the X-shooter GRB GTO
collaboration:

We observed the field of GRB 120712A (Page et al., GCN 13454) with the
ESO VLT equipped with the X-shooter spectrograph. Observations started
at 00:06 UT on 2012-07-13 (10.4 hr after the BAT trigger), for a total
exposure time of ~60 min in each of the UVB, VIS, and NIR arms,
covering the wavelength range 3000-25000A.

The spectrum exhibits a relatively broad trough (centered at ~6292A)
which we interpreted as Lyman-alpha break. Redward of this feature the
spectrum shows metals lines such as Mg II, Si II, and  Fe II, all at a
common redshift z=4.1745. We also measured the HI column density,
logN(HI)~20.3, from the Lyman-alpha feature.

We acknowledge the excellent support of the ESO observing staff, in
particular Fernando J. Selman.


GRB_name: GRB120712A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13461
SUBJECT: GRB 120712A: Swift/UVOT Detection
DATE:    12/07/13 12:15:47 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120712A
95 s after the BAT trigger (Page et al., GCN Circ. 13454).
A source consistent with the XRT position (Osborne et al., GCN Circ. 13456) 
and the optical position reported by GROND (Elliott et al., GCN Circ. 13457) 
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  11:18:21.25 = 169.58854 (deg.)
  Dec (J2000) = -20:02:01.7  = -20.03380 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

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

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

white (FC)         95           245          147        16.95 +/- 0.03
white              861         1010          150        18.93 +/- 0.09
v                  637          657           19        16.79 +/- 0.15
b                  563        18691         1160        >21.8
u                  308        35517         2569        >22.1
w1                 686        35216         3108        >22.0
m2                4818        41481         3296        >22.1
w2                 613        40167         2931        >22.1

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


GRB_name: GRB120709A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13462
SUBJECT: IPN Triangulation of GRB 120709A
DATE:    12/07/13 17:02:49 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

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,

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:

GRB 120709A has been observed by Fermi GBM and LAT (GCN 13423, 13427,
13429), INTEGRAL (SPI-ACS), Konus-Wind (GCN 13440), and MESSENGER
(GRNS), so far, at about 76300 s UT (21:11:40).  A Swift XRT
observation of part of the LAT error circle in GCN 13423 revealed an
uncataloged X-ray source at RA, Dec = 318.17277, -49.97297 (GCN
13428).  We have triangulated this burst  to a preliminary, 3 sigma
error box whose coordinates are:

    RA(2000)                         DEC(2000)
 21 h 15 m 22.14 s=318.842 o   -50 o 17 '  56.07 " =-50.290 o (CENTER)
 21 h 20 m 51.20 s=320.213 o   -50 o 16 '  14.33 " =-50.271 o (CORNER)
 21 h 09 m 08.08 s=317.284 o   -50 o 32 '  41.99 " =-50.545 o (CORNER)
 21 h 21 m 34.21 s=320.393 o   -50 o 00 '  17.46 " =-50.005 o (CORNER)
 21 h 09 m 55.60 s=317.482 o   -50 o 17 '  28.57 " =-50.291 o (CORNER)


The error box area is 0.46 sq. deg., and its maximum and minimum
dimensions are ~ 1.9 and 0.12 degrees, respectively.  This box may be
improved.  As the XRT source lies outside the IPN error box, at least
0.26 degrees from its closest side, it is veryy unlikely to be
associated with the GRB.  A map has been posted at
ssl.berkeley.edu/ipn3/120709.  On this map, "LAT1" is from GCN 13423,
and "LAT2" is from GCN 13427.


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13463
SUBJECT: GRB 120711A: ATCA 34GHz further observations (upper limit)
DATE:    12/07/14 01:29:01 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 GRB120711A (GCN 13434) with the Australia Telescope
Compact Array at 34GHz for 60 minutes centered on 23:18UT Jul 13 2012
(T0+2.85days).

We detect no radio source at the location of the GRB (GCN 13430) and
place a 3sigma upper limit of 230uJy on the flux of an afterglow.

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.


GRB_name: GRB120714A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13464
SUBJECT: GRB 120714A: Swift detection of a burst
DATE:    12/07/14 07:57:26 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. J. Saxton (UCL-MSSL), V. D'Elia (ASDC), S. R. Oates (UCL-MSSL),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 07:46:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120714A (trigger=526593).  Swift could not immediately
slew to the location due to the Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec 167.970, -30.632 which is 
   RA(J2000) = 11h 11m 53s
   Dec(J2000) = -30d 37' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+51
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is C. J. Saxton (cjs2 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: GRB120711B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13465
SUBJECT: GRB120711B: MITSuME Ishigakijima upper limits
DATE:    12/07/14 08:16:23 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 120711B (Page et al., GCNC 13431)
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 2012-07-11 14:35:55 UT (~11.4 h after the burst).
We did not find any new point source within the XRT error
circle (Page et al., GCNC 13431) 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
----------------------------------------------------------------------
0.49154    14:58:51   4200.0    >22.1   >21.7  >20.5
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120714A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13466
SUBJECT: GRB 120714A: Swift-XRT observations
DATE:    12/07/14 09:44:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

The XRT began observing the field of GRB 120714A at 08:41:02.2 UT,
3255.5 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 167.98413,
-30.62769 which is equivalent to:
   RA(J2000)  = 11h 11m 56.19s
   Dec(J2000) = -30d 37' 39.7"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 46 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 6.09
x 10^20 cm^-2 (Kalberla et al. 2005). 


GRB_name: GRB120714A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13467
SUBJECT: GRB120714A: UVOT non-detection
DATE:    12/07/14 09:57:51 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin, S.R. Oates, and C.J. Saxton (UCL/MSSL) report on behalf
of the UVOT Team.

Swift UVOT took a finding chart exposure of GRB120714A (Saxton et al.,
GCN Circ. 13464) of 150 seconds with the White filter starting 3259
seconds after the BAT trigger. No credible afterglow candidate is
found in the initial data products. At the XRT position (Burrows et al.,
GCN Circ. 13466) a 3-sigma upper limit of 20.4 mag. is found.

No correction has been made for the expected extinction corresponding to
E(B-V) of 0.06.


GRB_name: GRB120711A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13468
SUBJECT: GRB 120711A: INTEGRAL/SPI observations
DATE:    12/07/14 12:08:26 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

L. Hanlon (UCD), A. Martin-Carrillo (UCD), X.-L. Zhang (MPE) and A. von Kienlin
(MPE) report:

"The bright and long GRB detected by IBAS in the INTEGRAL IBIS/ISGRI data
at 02:44:48 UT on July 11th 2012 (Gotz et al., GCN 13434 ) was also observed
by the Spectrometer SPI onboard INTEGRAL, in addition to the detection by
its anticoincidence shield (SPI-ACS). The event was located in the field
of view of SPI, which allows spectral analysis of this event.

The light curve from SPI events starts with a precursor at 02:44:50 UT followed 
by a bright double peaked main emission phase at 02:45:55 UT with a duration 
of about 50 sec. The emission during the main peak is seen up to ~3 MeV. 
We searched for the faint and soft emission after the main outburst reported by 
E. Bozzo et al. (GCN 13435) and S. Golenetskii et al. (GCN 13446). 
We find a weak tail in the 20 to 100 keV energy range, lasting for about 800 s 
after the main emission phase .

The time-integrated spectrum of the main emission phase is well fitted (in
the 20 keV - 3 MeV range) by an exponential cutoff powerlaw model, with
photon index = 1.00+/-0.03 and an high energy cutoff at 1200 +/- 200 keV.
The fluence during the 50 seconds main emission phase in the 20-1000 keV 
range is (2.26 +/- 0.04)E-4 erg/cm^2.

The spectral analysis results presented above are preliminary."


GRB_name: GRB120712A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13469
SUBJECT: GRB 120712A: Fermi GBM observation
DATE:    12/07/14 17:45:22 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team:

"At 13:42:25.61 UT on 12 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120712A (trigger 363793348 / 120712571).
which was also detected by the Swift/BAT (Page et al. 2012, GCN 13454).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 42 degrees.

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

The GBM light curve consists of two overlapping peaks
with a duration (T90) of about 23 s (50-300 keV).
The time-averaged spectrum from T0-3 s to T0+16 s is
well fit by a Band function with Epeak = 124 +/- 26 keV, 
alpha = -0.6 +/- 0.2, and beta = -1.80 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(4.43 +/- 0.05)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+9.3 s in the 10-1000 keV band
is 3.5 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB120714A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13470
SUBJECT: GRB 120714A: Enhanced Swift-XRT position
DATE:    12/07/14 20:45:15 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 2408 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 120714A, 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 = 167.98288, -30.62740 which is equivalent
to:

RA (J2000): 11h 11m 55.89s
Dec (J2000): -30d 37' 38.6"

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

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

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


GRB_name: GRB120714B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13471
SUBJECT: GRB 120714B: Swift detection of a burst
DATE:    12/07/14 21:34:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. J. Saxton (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), S. R. Oates (UCL-MSSL),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 21:18:46.57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120714B (trigger=526642).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 355.433, -46.186 deg, which is 
   RA(J2000)  =  23h 41m 44s
   Dec(J2000) = -46d 11' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for image triggers (64 sec),
the realtime TDRSS lightcurve does not show anything significant. 

The XRT began observing the field at 21:20:46.6 UT, 120.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 355.3993, -46.1764 which is equivalent to:
   RA(J2000)  = +23h 41m 35.83s
   Dec(J2000) = -46d 10' 35.0"
with an uncertainty of 5.2 arcseconds (radius, 90% containment). This
location is 90 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 1.59e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT results will not be available until further data are processed. 

Burst Advocate for this burst is C. J. Saxton (cjs2 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: GRB120714A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13472
SUBJECT: GRB 120714A: Swift-BAT refined analysis
DATE:    12/07/14 21:56:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), C. J. Saxton (UCL-MSSL), 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 120714A (trigger #526593)
(Saxton, et al., GCN Circ. 13464).  The BAT ground-calculated position is
RA, Dec = 167.975, -30.625 deg, which is 
   RA(J2000)  =  11h 11m 54.1s 
   Dec(J2000) = -30d 37' 29.8" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 40%.
 
The mask-weighted light curve shows a single FRED-like pulse starting at
~T-1 sec, peaking at ~T+4 sec, and ending at ~T90 sec.
T90 (15-350 keV) is 16.2 +- 4.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.74 to T+17.78 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.16.  The fluence in the 15-150 keV band is 8.2 +- 0.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.58 sec in the 15-150 keV band
is 1.5 +- 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/526593/BA/


GRB_name: GRB120714B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13473
SUBJECT: GRB 120714B: Position Correction and Candidate Optical Afterglow
DATE:    12/07/15 00:06:32 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and C. J. Saxton (UCL-MSSL)
report on behalf of the Swift team:

The positions reported for GRB 120714B in GCN Circular 13471
are incorrect because of an unusally large attitude error
on the spacecraft. Using the initial UVOT exposure, we find
the corrected XRT position is:
  RA  (J2000) =  23h 41m 38.35s
  DEC (J2000) = -46d 11' 07"

There is a candidate afterglow in the initial UVOT exposure
of 36 seconds starting 129 seconds after the trigger.
The source has a mag of 18.6 in the white filter and is
located at the following position:
  RA  (J2000) =  23h 41m 38.05s
  DEC (J2000) = -46d 11' 03"


GRB_name: GRB120624B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13474
SUBJECT: GRB 120624B: VLA Observations
DATE:    12/07/15 03:50:18 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

C. Bathurst (U. South Florida), D. A. Frail (NRAO) and S. B. Cenko (UC
Berkeley) report on behalf of a larger collaboration:

We have observed the field of the potential X-ray afterglow (GCN 13400,
13394) of the Fermi GBM (GCN 13377) and LAT (GCN 13379) GRB 120624B with
the VLA. In observations taken on 2012 July 10.00 UT, at center
frequencies of 5 GHz and 14 GHz, we find an unresolved radio source
coincident with the position of the claimed X-ray afterglow (GCN 13400).
The radio source is detected at 5-6 sigma significance and it has a
rising spectrum consistent with the extrapolation of the 3mm PdBI
detection (GCN 14321). Further 5 GHz observations were also made on June
26, June 29 and July 11. The 5 GHz flux density of the radio source shows
no evidence for variability through these 4 epochs.

Further observations are planned.


GRB_name: GRB120714A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13476
SUBJECT: GRB 120714A: Swift-XRT refined Analysis
DATE:    12/07/15 05:26:49 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

We have analysed 16 ks of XRT data for GRB 120714A (Saxton  et al. GCN
Circ. 13464), from 3.3 ks to 46.3 ks after the BAT trigger. The data
comprise 1.2 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN. Circ 13470).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.77 (+0.18, -0.17).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.9 (+0.5, -0.4). The
best-fitting absorption column is  4.1 (+1.4, -1.5) x 10^21 cm^-2, in
excess of the Galactic value of 6.1 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 3.0 x 10^-11 (1.0 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.1 (+1.4, -1.5) x 10^21 cm^-2
Galactic foreground: 6.1 x 10^20 cm^-2
Excess significance: 3.9 sigma
Photon index:      2.9 (+0.5, -0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00526593.

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


GRB_name: GRB120714B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13477
SUBJECT: GRB 120714B: Redshift from VLT/X-shooter
DATE:    12/07/15 08:22:43 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

J.P.U. Fynbo (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), 
V. D'Elia (ASDC, INAF), D. Xu (WIS), and D. Malesani (DARK/NBI) report 
on behalf of the X-shooter GRB GTO collaboration:

We observed the field of GRB 120714B (Saxton et. al GCN 13471, Marshall & 
Saxton GCN 13473) with X-shooter at VLT (Paranal, Chile). Observations started 
on 15 July at 5:06 UT (7.8 hr after the burst) and consisted of a total observing 
time of 4800 s in each of the UVB, VIS and NIR arms, covering the range 
between 3000 and 18000 A.

The spectrum shows a faint continuum where we detect MgII absorption as well 
as emission lines of [OII], H-beta, [OIII] and H-alpha at a common redshift of 
z=0.3984.

We acknowledge excellent support from the ESO staff, in particular Dimitri 
Gadotti.


GRB_name: GRB120714B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13478
SUBJECT: GRB 120714B: GROND confirmation of fading afterglow
DATE:    12/07/15 08:26:41 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), and J. Greiner (MPE 
Garching) report on behalf of the GROND team:

We observed the field of GRB 120714B (Swift trigger 526642; Saxton et al., 
GCN 13471) 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 3:01 UT on 2012-07-15, about 6 hrs after the GRB 
trigger, at a airmass of 2.2, and a mean seeing of 2.4". Based on an exposure 
of 460 seconds in the optical and 480 seconds in the NIR, at a mean time 
of 03:27 UT we detect the UVOT afterglow candidate (Marshall et al., GCN 13473) 
with preliminary AB magnitudes

  g' = 22.3 +/- 0.2
  r' = 22.1 +/- 0.2
  i' = 21.5 +/- 0.2
  z' = 20.5 +/- 0.2
  J  > 20.7
  H  > 20.1
  Ks > 19.2.

This suggests a fading relative to the white light magnitude of 18.6 mag as
reported by Marshall et al. (GCN 13473), suggesting this to be the 
afterglow of GRB 120714B. Observations are ongoing.

The magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS 
stars (JHK). We note that the Galactic reddening along the line of sight 
is E_(B-V)= 0.01 mag (Schlegel et al. 1998).


GRB_name: GRB120714A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13479
SUBJECT: GRB 120714A: GROND upper limits
DATE:    12/07/15 08:55:35 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), and J. Greiner (MPE 
Garching) report on behalf of the GROND team:

We observed the field of GRB 120714A (Swift trigger 526593; Saxton et al., 
GCN 13464) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 23:12 UT on 2012-07-14, 15.5 hrs after the GRB 
trigger, at a airmass of 1.3, and a mean seeing of 1.6". We do not find
any source in the XRT error circle (Burrows et al., GCN 13466). Based on 
an exposure of 1500 seconds in the optical and 1200 seconds in the NIR, 
at a mean time of 00:00 UT we derive the following upper limits (all AB 
magnitudes):

  g' > 23.9 
  r' > 23.9 
  i' > 23.1 
  z' > 23.1 
  J  > 20.9
  H  > 20.2
  Ks > 19.2.

The magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS 
stars (JHK). We note that the Galactic reddening along the line of sight 
is E_(B-V)= 0.06 mag (Schlegel et al. 1998).


GRB_name: GRB120714B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13481
SUBJECT: GRB 120714B: Swift-BAT refined analysis
DATE:    12/07/15 17:34:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), C. J. Saxton (UCL-MSSL),
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 120714B (trigger #526642)
(Saxton, et al., GCN Circ. 13471).  The BAT ground-calculated position is
RA, Dec = 355.412, -46.196 deg, which is 
   RA(J2000)  =  23h 41m 38.9s 
   Dec(J2000) = -46d 11' 47.3" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
 
The mask-weighted light curve shows a broad peak starting at ~T-35 sec,
peaking around T+0 sec, and ending at ~T+55 sec with a tail out to ~T+150 sec.
T90 (15-350 keV) is 159 +- 34 sec (estimated error including systematics).
 
The time-averaged spectrum from T-23.0 to T+154.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.17.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-21.71 sec in the 15-150 keV band
is 0.4 +- 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/526642/BA/


GRB_name: GRB120714A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13482
SUBJECT: GRB120714A: Swift/UVOT upper limits
DATE:    12/07/15 19:44:42 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 120714A
3259 s after the BAT trigger (Saxton et al., GCN Circ. 13464).

No optical afterglow consistent with the XRT position (Beardmore etal.,
GCN Circ. No. 13470) 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          3259         3409          147         >19.9
white             3259        28944         2696         >21.8
v                 3416        21584         2027         >20.4
b                 4237        28344         2135         >21.1
u                 4031        27431         1278         >20.7
w1                3826        23171         1058         >21.0
m2                3621        22489         1279         >21.0
w2                4648        17394         1667         >21.5

A possible source was marginally present in the u band during the first two
images, but not seen later, nor in any of the other bands.

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


GRB_name: GRB120714B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13483
SUBJECT: GRB 120714B: Swift-XRT refined Analysis
DATE:    12/07/16 09:17:01 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O. M. Littlejohns, K. Page (U. Leicester) & C. J. Saxton (UCL-MSSL)
reports on behalf of the Swift-XRT team:

We have analysed 2.4 ks of XRT data for GRB 120714B (Saxton  et al. GCN
Circ. 13471), from 110 s to 75.0 ks after the  BAT trigger. The data
comprise 9 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode.

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.87 (+0.13, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.9, -0.6). The
best-fitting absorption column is  1 (+11, -0) x 10^20 cm^-2,
consistent with the Galactic value of 1.2 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.4 x 10^-11 (3.6 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1 (+11, -0) x 10^20 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.0 (+0.9, -0.6)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00526642.

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


GRB_name: GRB120714B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13484
SUBJECT: GRB 120714B: Swift/UVOT Detection
DATE:    12/07/16 17:33:51 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL), F. Marshall (NASA/GSFC), and C. J. Saxton (UCL-MSSL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120714B
129 s after the BAT trigger (Saxton et al., GCN Circ. 13471).
The UVOT source candidate reported by Marshall and Saxton
(GCN Circ. No.  13473) is found to decay.

The preliminary UVOT position is RA, Dec (J2000) = (355.40864,-46.18387),
or in sexagesimal coordinates:

RA = 23h41m38.1s
Dec = -46d11'02"

with 90% confidence error radius of 0.58".

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              129          165           35         18.40 +/- 0.20
white            10034        10184          147        >20.8
b                10195        11102          885        >21.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13485
SUBJECT: GRB 120711A: ATCA 34GHz final observations (upper limit)
DATE:    12/07/17 01:19:37 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 GRB120711A (GCN 13434) with the Australia Telescope
Compact Array at 34GHz for 64 minutes centered on 21:42UT Jul 16 2012
(T0+3.78days) in clear weather.

We detect no radio source at the location of the GRB (GCN 13430) and
place a 3sigma upper limit of 96uJy on the flux of an afterglow.

No 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.


GRB_name: GRB120716A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13487
SUBJECT: IPN Triangulation of unusual GRB 120716A
DATE:    12/07/17 20:16:23 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

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

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 GRB 120716A has been observed by Fermi (GBM: trigger
364151106), Konus-Wind, INTEGRAL (SPI-ACS), Suzaku (WAM), and MESSENGER
(GRNS), so far, at about 61504 s UT (17:05:04).

The burst light curve shows a short initial pulse followed in ~170 s
period of quiescence by two long pulses with a total duration of ~60 s.

We have triangulated both emission episodes and have revealed that they
came from the same direction.

We have localized the burst to a preliminary, 3 sigma error box whose
coordinates are:
    ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    313.089 (20h 52m 21s)  +9.558 ( +9d 33' 28")
   Corners:
    311.595 (20h 46m 23s)  +9.913 ( +9d 54' 46")
    313.791 (20h 55m 10s) +10.049 (+10d 02' 56")
    314.615 (20h 58m 28s)  +9.110 ( +9d 06' 36")
    312.407 (20h 49m 38s)  +9.046 ( +9d 02' 45")
   ---------------------------------------------
The error box area is 2.04 sq. deg, and its maximum dimension is 3.1 deg.

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120716_T61507/IPN/

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


GRB_name: GRB120716A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13488
SUBJECT: Konus-Wind observation of GRB 120716A
DATE:    12/07/18 10:21:17 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 unusual GRB 120716A
(IPN detection and localization: Hurley at al., GCN 13487)
triggered Konus-Wind at T0=61507.357s UT (17:05:07.357)

The light curve started with a short (~0.9 s) pulse followed,
after ~170 s, by a double-peaked structure lasting for ~60 s.
The total duration of the burst is ~230 s.

This GRB is similar to GRB 041219A, GRB 050820A, and GRB 060124,
which display a rather short precursor, a ~200 s long period
of quiescence, and the main episode of emission. For this burst,
the precursor is relatively short and bright and the main part
is shorter and dimmer.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120716_T61507/

As observed by Konus-Wind:
   - the precursor had a fluence of 1.4(-0.3,+1.0)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.064 s,
of 3.3(-0.8,+2.7)x10-6 erg/cm2/s;
   - the main part of the burst
had a fluence of 1.3(-0.3,+0.3)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+181.760 s,
of 8.8(-0.15,+0.15)x10-7 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The 3-channel spectrum of the precursor (from T0-0.256 to T0+0.512 s)
can be modeled  (in the 20-1200 keV range) by a power law
with exponential cutoff model with alpha = -1.3  0.1
and Ep = 380  50 keV (one-sigma errors are given for this fit).

The time-integrated spectrum of the main emission episode
(measured from T0+172.288 to T0+213.248 s)
is well fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which:
alpha = -1.50 (-0.2, +0.2),
and Ep = 190(-44, +110) keV,
chi2 = 59.2/75 dof.
Fitting this spectrum with the GRB (Band) function yields
the following model parameters:
the low-energy photon index alpha = -1.5 (-0.2, +0.3),
the high energy photon index beta = -2.4 (<-2.0),
the peak energy Ep = 175(-73, +96) keV,
chi2 = 58.2/74 dof.

The spectrum at the maximum count rate
(measured from T0+180.480 to T0+188.672 s) is best fitted
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which:
alpha = -1.1 (-0.3, +0.3),
and Ep = 180(-37, +68) keV,
chi2 = 66.5/75 dof.


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


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13489
SUBJECT: GRB 120716A: Candidate Optical Afterglow from PTF
DATE:    12/07/19 00:01:37 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), E. O. Ofek (Weizmann Institute of Science), and
P. E. Nugent (Lawrence Berkeley National Laboratory / UC Berkeley) report
on behalf of a larger collaboration:

We have imaged the location of the IPN GRB 120716A (Hurley et al., GCN
13487) with the Palomar 48 inch Oschin Schmidt telescope as part of the
Palomar Transient Factory (PTF).  Images were obtained in the r' filter
beginning at 4:25 UT on 18 July 2012 (~ 1.5 d after the IPN trigger).

Within the IPN localization, we identify a new point source with
coordinates:

 RA: 20:52:12.10   Dec: +09:35:53.7  (J2000)

Using several nearby stars from the Sloan Digital Sky Survey for
reference, we measure a magnitude of r' ~ 20.4 at this time.

Nothing is detected at this location in previous PTF imaging of this
field, with images beginning in June 2011.  Furthermore, no source is
detected in archival SDSS imaging of this location (a faint nearby object
in the SDSS database, SDSS J205212.01+093551.9, appears to be of very low
significance).  However, our most recent epoch of PTF imaging was obtained
in March 2012, so we cannot currently rule out the chance alignment of an
unassociated foreground or background transient.

Further observations of this candidate optical afterglow are planned.


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13490
SUBJECT: GRB 120716A: Optical decay from NOT
DATE:    12/07/19 05:52:35 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), N. Groeneboom, K. Mikkelsen (U. Oslo) report on behalf of
a larger collaboration:

We observed the field of the candidate optical afterglow (Cenko et
al., GCN 13489) of GRB 120716A (Hurley et al., GCN 13487), using the
2.5m Nordic Optical Telescope (NOT) equipped with ALFOSC. Observations
started 04:03 UT on 2012-07-19 (i.e., 2.455 days after the IPN
trigger) and 5x300s SDSS r'-band images were obtained in a seeing of
~0.7".

The optical source reported in GCN 13489 is well detected in each NOT
image at coordinates

RA(J2000)=20:52:12.17
Dec(J2000)=+09:35:53.9

with an uncertainty of ~0.1 arcsec radius, being consistent with the
PTF position.

The source had r(AB)=20.10+/-0.04, calibrated with nearby SDSS stars.
The decay between the PTF and NOT epochs indicates that the source may
be the optical afterglow of GRB 120716A.


GRB_name: GRB120716A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13491
SUBJECT: GRB 120716A: Typo correction in GCN 13490
DATE:    12/07/19 06:10:16 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS) reports

The magnitude in GCN 13490 should be r'(AB)=21.00 rather than
r'(AB)=20.10. Otherwise there would be no decay compared with the
previous PTF magnitude of r'~20.4. Thanks to Brad Cenko for pointing
out this.


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13492
SUBJECT: GRB 120716A: GROND confirmation of the optical/NIR afterglow
DATE:    12/07/19 06:26:31 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady (MPE Garching), M. Nardini (Universita degli studi di
Milano-Bicocca ) and J. Greiner (MPE Garching) report on behalf of the
GROND team:

We observed the field of GRB 120716A (Hurley et al., GCN #13487) at the
position of the afterglow candidate (Cenko et al., GCN #13489)
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 05:07 UT on 2012-07-19, 2.5 days after the GRB
trigger. They were performed at an average seeing of 1.4" and at an
average airmass of 1.3.

We found a single point source at a position consistent the afterglow
candidate reported in Cenko et al. (GCN #13489) and Xu et al. (GCN
#13490). Based on the first 460s of total exposures in g'r'i'z' and 480 s
in JHK, we estimate preliminary magnitudes (all in AB system) of

g' = 21.8 +- 0.1 mag,

r' = 20.9 +- 0.1 mag,

i' = 20.5 +- 0.1 mag,

z' = 20.3 +- 0.1 mag,

J = 19.9 +- 0.2 mag,

H = 19.6 +- 0.2 mag and

K = 18.8 +- 0.5 mag

The optical/NIR SED is well fit by a power-law with a spectral slope of
~1.3, typical for GRB afterglows, confirming this to be the afterglow of
GRB120716A.

Given magnitudes are calibrated against SDSS 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)=0.07 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120716A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13493
SUBJECT: VLT/FORS2 redshift of GRB120716A
DATE:    12/07/19 08:40:51 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Jochen Greiner, Arne Rau, Patricia Schady (all MPE), Ivo Saviane (ESO), 
and Brad Cenko ( UC Berkeley) report on behalf of a larger collaboration.

We observed the afterglow candidate of GRB 120716A (Hurley et al., GCN 
13454; Cenko et al. GCN 13489; Xu et al, GCN 13490; Schady et al. CGN 
13492) with the ESO VLT equipped with the FORS2 spectrograph. 
Observations with the 600B grism, covering a spectral range of 
350-610nm) started at ~06:54 UT on July 19th 2012 (~58.2 hr after the 
gamma-ray trigger) and lasted for ~ 1.5hr.

The spectrum shows a prominent, broad absorption trough centered at 
~4250A, interpreted as Lyman-alpha, together with numerous metal lines 
(SiII, OI, SiIV, CIV) at longer wavelength. We find a common redshift of 
these features of z=2.48.


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13494
SUBJECT: GRB 120716A: Redshift confirmation from VLT/X-shooter
DATE:    12/07/19 16:56:53 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC/INAF-OAR), P. Goldoni (APC,CEA/Irfu),
D. Xu (WIS), T. Kruehler, J. P. U. Fynbo, D. Malesani (DARK/NBI), O.E.  
Hartoog (UvA, Netherland), N. R. Tanvir (U. of Leicester) 
report on behalf of the X-shooter GRB GTO collaboration:

We observed the GRB 120716A (Hurley et. al GCN 13487) optical counterpart
(Cenko et al. GCN 13489, Xu et al. GCN 13490, Schady et al. GCN 13492) with
X-shooter at the VLT (Paranal, Chile). Observations started on 19 July  
at 8:40 UT
(2.6 days after the burst) and consisted of a total observing
time of 3600 s in each of the UVB, VIS and NIR arms, covering the range
between 3000 and 18000 A.

The spectrum shows a broad absorption trough at ~4250A which we interpret
as due to Lyman-alpha. At the same redshift z=2.486 we detect plenty of metal
absorption lines, such as (CII, SiII, OI, FeII, CIV, SiIV), fine  
structure (CII*, SiII* FeII*) and metastable (NiII) lines.
We thus confirm the redshift reported by Greiner et al. (GCN 13493).


We acknowledge excellent support from the ESO staff, in particular Dimitri
Gadotti, Lorena Faundez, Fernando Selman and Jonathan Smoker.

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GRB_name: GRB120716A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13495
SUBJECT: GRB 120716A: Swift/XRT position consistent with that of the optical counterpart
DATE:    12/07/19 18:22:19 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS) reports on behalf of a larger collaboration:

The Swift satellite observed the field of the decaying optical
transient (Cenko et al. GCN 13489; Xu et al. GCN 13490; Schady et al.
GCN 13492), which is very likely the optical afterglow of GRB 120716A
(Hurley et al., GCN 13487). Initial observation started at 12:47 UT
and ended at 13:12 UT on 2012-07-19 (i.e., a median time of 2.83 d
after the IPN trigger), and consisted of a total observing time of
1470s for Swift/XRT.

Preliminary XRT data reduction reveals a S/N~2 source at coordinates

RA(J2000)  =  20:52:12.4
Dec(J2000) = +09:35:51.1

with an uncertainty of 7.7 arcsec radius, being consistent with the
position of the optical source. Currently we don't know whether the
X-ray source is decaying or not.

We thank the Swift team for carrying out a quick ToO observation.


GRB_name: GRB120716A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13496
SUBJECT: GRB 120716A: Swift-XRT detection
DATE:    12/07/19 19:15:34 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), J. Gelbord and J. Kennea (PSU)  report on behalf of  
the Swift-XRT team:

Swift began a target of opportunity observation of GRB120716A on July
19, 2012 at 14:22 UT, approximately 2.9 days after the discovery  
(Hurley et al. GCN 13487). Swift data for these observations utilize  
Target ID 20225.

Preliminary analysis of the 1.5 ks downlinked XRT data finds an  
uncatalogued X-ray source at RA, Dec = 313.05050, 9.59850 which is  
equivalent
to:

RA(J2000) = 20h 52m 12.12s
Dec(J2000)= +09d 35m 54.6s,

with an error radius of 3.4 arcsecs (position enhanced by UVOT field  
astrometry).
The above position is consistent with the optical afterglow detection  
reported by Cenko et al. (GCN 13489), Xu et al. (GCN 13490), Schady et  
al. (GCN 13492). In addition, no known X-ray object is present at the  
XRT coordinates, so this is likely the X-ray afterglow of GRB120716A.  
The count rate of the XRT source is 8.32E-03+/-2.9E-03 cts/s. We  
cannot determine at the present time whether the
source is fading.

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


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GRB_name: GRB120716A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13497
SUBJECT: GRB 120716A:  EVLA Detection
DATE:    12/07/19 22:26:20 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, T. Laskar, A. Soderberg and E. Berger (Harvard) report on 
behalf of a larger collaboration:

"We observed the position of GRB 120716A (Hurley et al.; GCN 13487) with 
the EVLA beginning 2012 July 19.26 (dt ~ 2.5 d).  At a mean frequency of 
6 and 22 GHz, we detect a radio source (10 and 6 sigma, respectively) 
consistent with optical candidates (e.g. Cenko et al.; GCN 13489) and 
the Swift-XRT detection (D'Elia et al.; GCN 13496).

Followup observations are planned."


GRB_name: GRB120716A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13498
SUBJECT: GRB 120716A: Fermi GBM observation
DATE:    12/07/20 11:21:05 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) and Adam Goldstein (UAH)
report on behalf of the Fermi GBM Team:

"At 17:05:03.91 UT on 16 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120716A (trigger 364151106 / 120716712).

This burst was localized by the IPN (Hurley et al., GCN 13487).
The GBM on-ground calculated location is consistent with the
IPN location.

The angle from the Fermi LAT boresight is 63 degrees.

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

The GBM light curve consists of a bright precursor, followed
by a double-peaked main emission after ~ 160 s.
The duration (T90) is about 234 s (50-300 keV).
The time-averaged spectrum of the precursor is best fit by
a power law function with an exponential
high-energy cutoff.  The power law index is -0.84 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 173 +/- 18 keV.
A Band function fits the spectrum equally well
with Epeak= 115 +/- 19 keV, alpha = -0.48 +/- 0.22 and beta = -2.19 +/- 0.17.
The time-averaged spectrum of the main emission is best fit by 
a Band function with Epeak= 114 +/- 12 keV, alpha = -1.00 +/- 0.08
and beta= -2.08 +/- 0.07.

The event fluence (10-1000 keV) is (1.47 +/- 0.01)E-05 erg/cm^2. 
The 1-sec peak photon flux measured starting from T0-0.13 s 
in the 10-1000 keV band is 8.37 +/- 0.32 ph/s/cm^2.

Using the redshift of 2.48 (Greiner et al., GCN 13493; D'Elia et al., GCN 13494) 
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, 
Omega_Lambda = 0.73, this corresponds to an isotropic 
energy release of ~ 3E+53 erg. 

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


GRB_name: GRB120722A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13499
SUBJECT: GRB 120722A: Swift detection of a burst
DATE:    12/07/22 13:05:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU) and
E. Sonbas (NASA/GSFC/Adiyaman Univ.) report on behalf of the Swift
Team:

At 12:53:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120722A (trigger=528195).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 230.491, +13.250 which is 
   RA(J2000)  =  15h 21m 58s
   Dec(J2000) = +13d 15' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a peak with a total
duration of about 25 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 12:55:59.4 UT, 153.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 230.49665, 13.25112 which is equivalent
to:
   RA(J2000)  = 15h 21m 59.20s
   Dec(J2000) = +13d 15' 04.0"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 20 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 does not constrain the column density. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 156 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
0.05. 

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


GRB_name: GRB120722A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13500
SUBJECT: GRB 120722A: Xinglong TNT optical afterglow candidate
DATE:    12/07/22 14:18:45 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 120722A  (Melandri et al. GCN 13499)
with Xinglong TNT telescope in R-band at 12:56:53 (UT),  
3.5 min  after the burst.  An optical counterpart was detected 
 in our combined image  within the errorbox of X-ray afterglow location
 (Melandri et al. GCN 13499)   with a brightness of about 20.8 mag in R band,  
calibrated against the USNO B1.0 R2mag.

The coordinates and magnitude of the reference star we used 
are 15:21:54.116  +13:15:50.70, J2000 and R2=16.91 mag in USNO B1.0.

This message may be cited.

Further observations are encouraged.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org:8080/grb/index.html

We thank Chunlan Lu for performing these observations.


GRB_name: GRB120722A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13501
SUBJECT: GRB 120722A:  Correction for GCN circ.13500
DATE:    12/07/22 16:43:59 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We apologize for the wrong result reported in GCN circ. 13500 . 

Caused by a wrong astronomical calibration,
the optical candidate of GRB 120722A reported in GCN circ. 13500 
should be a known object in the USNO B1.0 

Therefore, no any new source within the location of 
XRT counterpart was detected by TNT.  The 3 sigma upper limit
of 21 mag was derived relatively to USNO B1.0 R2 mag. 


GRB_name: GRB120722A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13502
SUBJECT: GRB 120722A: Enhanced Swift-XRT position
DATE:    12/07/22 17:58:21 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 1220 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120722A, 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 = 230.49656, +13.25109 which is equivalent
to:

RA (J2000): 15h 21m 59.17s
Dec (J2000): +13d 15' 03.9"

with an uncertainty of 2.1 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: GRB120722A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13503
SUBJECT: GRB 120722A: Swift-BAT refined analysis
DATE:    12/07/22 22:40:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120722A (trigger #528195)
(Melandri, et al., GCN Circ. 13499).  The BAT ground-calculated position is
RA, Dec = 230.489, 13.249 deg, which is 
   RA(J2000)  =  15h 21m 57.4s 
   Dec(J2000) = +13d 14' 56.8" 
with an uncertainty of 3.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.
 
The mask-weighted light curve shows a couple overlapping peaks starting
at ~T-10 sec, peaking at ~T+23 sec, and ending at ~T+50 sec.
T90 (15-350 keV) is 42.4 +- 10.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.3 to T+47.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.90 +- 0.25.  The fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+24.02 sec in the 15-150 keV band
is 1.0 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/528195/BA/


GRB_name: GRB120722A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13504
SUBJECT: GRB 120722A: Swift-XRT refined Analysis
DATE:    12/07/23 01:05:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 8.4 ks of XRT data for GRB 120722A (Melandri  et al.
GCN Circ. 13499), from 161 s to 27.7 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN. Circ 13502).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.85 (+0.12, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.6 (+0.8, -0.7). The
best-fitting absorption column is  5.1 (+1.8, -1.5) x 10^22 cm^-2, in
excess of the Galactic value of 3.1 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 8.4 x 10^-11 (5.7 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.1 (+1.8, -1.5) x 10^22 cm^-2
Galactic foreground: 3.1 x 10^20 cm^-2
Excess significance: 5.6 sigma
Photon index:      2.6 (+0.8, -0.7)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00528195.

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


GRB_name: GRB120722A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13505
SUBJECT: GRB 120722A: 1.5m OSN I-band observations
DATE:    12/07/23 02:37:11 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

F. Aceituno (OSN, IAA-CSIC),  R. Sanchez-Ramirez (IAA-CSIC), A. de Ugarte
Postigo (IAA-CSIC, DARK), J. Gorosabel (IAA-CSIC), A.J. Castro-Tirado
(IAA-CSIC), report on behalf of a larger collaboration:

"We observed the field of the GRB 120722A XRT error circle (Melandri et
al., GCN 13499; Evans et al., GCN 13502) with the 1.5m telescope at the
Observatorio de Sierra Nevada, Granada, Spain. The observations were
conducted in the I-band with a total exposure time of 16x300s on July
22.86617-22.92716 UT (7.9--9.4 hours post GRB). No object is detected
inside the XRT error circle down to I~21 (Vega mag, calibrated against
USNO-B1.0). We note the presence of a faint object close to the XRT error
circle border located at RA(J2000)=15:21:59.19, Dec(J2000)=+13:15:05.0
(+/-0.9") which seems also present at the SDSS."


GRB_name: GRB120722A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13506
SUBJECT: GRB 120722A: GROND detection of the afterglow
DATE:    12/07/23 02:43:22 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 120722A (Swift trigger 528195; Melandri et
al., GCN #13499) 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 23:20 UT on 2012-07-22, 10.5 hrs after the GRB
trigger. They were performed at an average seeing of 1.1" arcsec and at an
average airmass of 1.4.

Inside the 2.1 arcsecond XRT error circle (Evans et al., GCN #13502), we
detect a fading source in g'r'i'z' at coordinates RA,DEC (J2000) =
230.4966, 13.2513 = 15:21:59.184, +13:15:04.68 (+/- 0.3 arcsec).

Based on exposures of 1600 seconds in g'r'i'z' and 1200 seconds in JHK,
we measure the following preliminary magnitudes (all in the AB system)

   g' = 23.8 +- 0.1,
   r' = 23.6 +- 0.1,
   i' = 22.8 +- 0.1,
   z' = 22.6 +- 0.1,
   J  > 21.8,
   H  > 21.2,
   K  > 19.8.

The power-law like SED and fading nature of this source confirm that it 
is the afterglow of GRB 120722A.

All magnitudes are calibrated against SDSS (g'r'i'z') and 2MASS field 
stars.
The magnitudes have not been corrected for the Galactic reddening of 
E(B-V)=0.05 mag along the line of
sight towards the source (Schlegel et al. 1998).


GRB_name: GRB120722A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13507
SUBJECT: GRB 120722A: VLT/X-shooter redshift of the host galaxy
DATE:    12/07/23 07:24:14 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC/INAF-OAR), D. Xu (WIS), A. de Ugarte Postigo (IAA-CSIC, DARK), 
D. Malesani (DARK/NBI), , J. P. U. Fynbo (DARK/NBI), P. Goldoni (APC,CEA/Irfu), 
N. R. Tanvir (U. of Leicester) and T. Kruehler (DARK/NBI) 
report on behalf of the GRB/X-shooter collaboration 


We imaged the field of GRB 120722A (Melandri et al., GCN 
13499) with the ESO VLT equipped with the 
X-shooter spectrograph. Observations started on 2012 July 22 at 23:08 UT 
(10 hr after the GRB), for a total exposure time of 80 min in each of 
the UVB, VIS, and NIR arms, covering the wavelength range 3000-25000 AA. 
Within the XRT error circle we noted a SDSS object, which is coincident
with the position of the afterglow reported by Sudilovsky et al. (GCN 13506).
The slit was positioned on this object. The object reported by Sudilovsky et al. (GCN 13506) 
is faintly detected in a combined stack of the ugriz SDSS data, suggesting a significant host contribution. 
The object is also well detected in our R-band acquisition images.

The spectrum is dominated by several nebular emission lines from the candidate host galaxy, 
including [O II], [O III] and Balmer lines (Halpha, Hbeta and Hgamma), 
at a common redshift z = 0.9586. Given the superposition with
the optical afterglow reported by Sudilovsky et al. (GCN 13506), this is likely the
host galaxy of GRB120722A.

We acknowledge excellent support from the ESO staff, in particular Lorenzo Monaco, 
Lorena Faundez and Emanuela Pompei.


GRB_name: GRB120722A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13508
SUBJECT: GRB 120722A: Swift/UVOT Upper Limits
DATE:    12/07/23 16:33:17 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. A. Pritchard (PSU) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120722A
157 s after the BAT trigger (Melandri et al., GCN Circ. 13499).
No optical afterglow consistent with the Enhanced Swift-XRT position
(Evans et al., GCN Circ. 13502)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           157          307          147         >20.9
u_FC               315          565          246         >20.2
white              157         7159          685         >21.7
v                  646        11696         1356         >20.5
b                  570        18708          758         >21.4
u                  315        18411         1583         >21.6
w1                 696        16188          820         >21.3
m2                4785        12602         1279         >21.1
w2                1028         6012          216         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120709A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13509
SUBJECT: GRB 120709A: Swift re-observation of the field of the X-ray counterpart candidate.
DATE:    12/07/23 20:23:09 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe and Craig Swenson (PSU) report on behalf of the Swift-XRT
team:

Swift re-observed the field of the X-ray afterglow counterpart
candidate of GRB 120709A (Kocevski et al. GCN Circ. 13423) on 2012
July 20  for 4.8 ks. In an initial observation on July 10 Swift
found an uncatalogued X-ray source within the FERMI/LAT error circle
(Grupe & Swenson, GCN Circ. 13428). In the new Swift observation
this source is still detected at a level of (5.1+/-1.1)e-3 counts/s.
This is a factor of roughly 2 lower than we had reported previously
in GCN Circular #13428 for this source. Assuming a normal decay
slope of an X-ray afterglow we would not expected to detect a source
so late after the burst. We conclude that the X-ray source reported
in GCN circular 13428 is not the X-ray afterglow of GRB 120709A.
Note that this result confirms the findings by Hurley et al. (GCN
Circ 13462) from IPN triangulations that the X-ray source reported
by Grupe & Swenson lies significantly outside the IPN error box of
GRB 120709A.


GRB_name: GRB120724A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13510
SUBJECT: GRB 120724A: Swift detection of a burst
DATE:    12/07/24 06:50:25 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), W. H. Baumgartner (GSFC/UMBC),
V. D'Elia (ASDC), H. A. Krimm (CRESST/GSFC/USRA),
B. Sbarufatti (INAF-OAB/PSU) and M. Stamatikos (OSU/NASA/GSFC) report
on behalf of the Swift Team:

At 06:39:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120724A (trigger=528443).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 245.190, +3.509 which is 
   RA(J2000) = 16h 20m 46s
   Dec(J2000) = +03d 30' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 06:40:52.0 UT, 109.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 245.18192, 3.50750 which
is equivalent to:
   RA(J2000)  = 16h 20m 43.66s
   Dec(J2000) = +03d 30' 27.0"
with an uncertainty of 4.0 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.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.29
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 5.14e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 117 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
0.05. 

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


GRB_name: GRB120724A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13511
SUBJECT: GRB 120724A: FTN optical afterglow candidate
DATE:    12/07/24 07:58:29 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
J. Japelj (U. Ljubljana) on behalf of a large
collaboration report:

The 2-m Faulkes Telescope North automatically began observing
GRB 120724A (D'Avanzo et al. GCN Circ. 13510) on July 24 2012,
06:42:31 UT corresponding to 209 seconds post burst trigger
with BVRi' filters. Within the XRT error circle we found the
following uncatalogued fading source,

R.A. = 16:20:43.21
Dec = +03:30:29.3   (J2000)

with an uncertainty of about 1" with a magnitude of
20.5 +/- 0.3 in the i band at 13.8 minutes, calibrated
against nearby USNOB-1 stars. The source is also visible
in stacked R-band frames.


GRB_name: GRB120724A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13512
SUBJECT: GRB 120724A: Gemini-N tentative redshift
DATE:    12/07/24 09:51:40 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), N.R. Tanvir (U. Leicester), 
D. Perley (Caltech), and A. J. Levan (U. Warwick) report 
on behalf of a larger collaboration:

We observed the afterglow of GRB 120724A (Guidorzi et al. 
GCN 13511; D'Avanzo et al. GCN 13510) using the GMOS-N 
spectrograph on the Gemini-North telescope under very good 
seeing conditions (0.5").

Observations began at 2012-7-24 08:31 UT, about 2 hr post-burst.
Two spectra of 900s each were acquired, covering the
6000-10000 Angstrom wavelength range.

A preliminary analysis of some of the absorption features
identified suggests that the GRB redshift is z = 1.48, 
based on identification of MgII2796,2803 doublet, 
MnII2606, FeII2600, and MnII2594.

We thank the Gemini staff, in particular J. Holt and 
J. Kemp, for making these observations possible.


GRB_name: GRB120711A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13513
SUBJECT: GRB120711A: Planned XMM-Newton observation
DATE:    12/07/24 15:22:35 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB120711A at location
(RA=06h 18m 42.79s, DEC=-70d 59' 56.6", J2000),
starting at 20:01:44 UT, on July 28, 2012,
for an exposure of 28000 seconds.

XMM-Newton SOC

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GRB_name: GRB120724A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13514
SUBJECT: GRB 120724A: Swift-XRT refined Analysis
DATE:    12/07/24 18:50:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 6.4 ks of XRT data for GRB 120724A (D'Avanzo  et al.
GCN Circ. 13510), from 115 s to 13.0 ks after the  BAT trigger. The
data comprise 40 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The best available XRT position  (using the
promptly downlinked event data, the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue) is RA, Dec = 245.1800,
3.5081 which is equivalent to:

RA (J2000): 16 20 43.19
Dec(J2000): +03 30 29.0

with an uncertainty of 2.2 arcsec (radius, 90% confidence).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.78 (+/-0.22), followed by a break at T+851 s to an
alpha of 0.48 (+0.18, -0.79).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+0.20, -0.09). The
best-fitting absorption column is  consistent with the Galactic value
of 4.3 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.7 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 4.3 x 10^20 cm^-2
Intrinsic column:    0 (+9.3, -0) x 10^20 cm^-2 at z=1.48
Photon index:      1.88 (+0.20, -0.09)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00528443.

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


GRB_name: GRB120724A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13515
SUBJECT: GRB 120724A: Enhanced Swift-XRT position
DATE:    12/07/24 19:24:49 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 2299 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 120724A, 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 = 245.18020, +3.50793 which is equivalent
to:

RA (J2000): 16h 20m 43.25s
Dec (J2000): +03d 30' 28.6"

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

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

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


GRB_name: GRB120724A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13516
SUBJECT: GRB 120724A: Swift/UVOT Detection of the Optical Afterglow
DATE:    12/07/25 13:11:42 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:

    The Swift/UVOT observed the field of GRB 120724A starting 99 s
after the BAT trigger (D'Avanzo et al., 2012, GCNC 13510).  Settled
observations started at 120 s.  We detect a faint source with preliminary
coordinates

    RA (J2000)  16:20:43.35  =  245.18062 (deg)
   Dec (J2000) +03:30:27.8   =   +3.50772 (deg)

and an estimated uncertainty of 0.77 arcsec (radius, 90% confidence,
statistical + systematic).  This position is consistent with the
optical source discovered by Guidorzi et al. (2012, GCNC 13511) and is
slightly outside the UVOT-enhanced XRT position (D'Avanzo et al.,
2012, GCNC 13514).  Preliminary magnitiudes for this source, and
3-sigma upper limits for the finding charts (FC) and the co-added
images, are

Filter       TSTART       TSTOP  EXPOSURE       Mag   Err  Sigma
----------------------------------------------------------------
white (FC)      117         267       147     >21.3
   u (FC)      330         580       246     >20.5
white (FC)      609         629        20     >19.8
----------------------------------------------------------------
  v            832        1404        72     >19.2
  b            585        1331        58      20.01 0.41    2.7
  u            330        1461       288      20.50 0.37    3.0
uvw1           1088        1453        59     >19.2
uvm2           1237        1429        39     >18.4
uvw2            635        1380        78     >19.5
white           117        1355       199      21.54 0.45    2.5
----------------------------------------------------------------

   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} = 0.05 mag (Schlafly et al. 2011, ApJS, 737, 103).


GRB_name: GRB120724A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13517
SUBJECT: GRB 120724A, Swift-BAT refined analysis
DATE:    12/07/25 18:14:34 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P. D'Avanzo (INAF-OAB), 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)
(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 120724A (trigger #528443)
(D'Avanzo, et al., GCN Circ. 13510).  The BAT ground-calculated position is
RA, Dec = 245.193, 3.535 deg which is
     RA(J2000)  =  16h 20m 46.3s
     Dec(J2000) = +03d 32' 07.2"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.

The mask-weighted light curve shows a single broad peak starting at roughly
T0-30 seconds, peaking at T0 and extending until T0+100 seconds.
T90 (15-350 keV) is 72.8 +- 16.4 sec (estimated error including systematics).

The time-averaged spectrum from -21.3 to 64.5 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.53 +- 1.53,
and Epeak of 27.6 +- 7.5 keV (chi squared 43.55 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.8 +- 1.1 x 10^-07 erg/cm2
and the 1-sec peak flux measured from T+7.51 sec in the 15-150 keV band is
0.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.45 +- 0.26 (chi squared 50.75 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/528443/BA/


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13518
SUBJECT: GRB 120716A: optical observation in CrAO
DATE:    12/07/25 19:24:53 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 region of  optical afterglow (Cenko et al., GCN 13489)  of
IPN localized GRB 120716A (Hurley et al., GCN 13487)  with AZT-11 telescope
of CrAO observatory starting on July 19  (UT) 18:51 under seeing  of about
3.3 arsces.   We do not detected  optical afterglow  up to R=20.8. The
photometry is based on the  USNO-B1.0 star 0996-0576906 (20 52 01.46 +09 36
17.8)  assuming R=15.97:

T0+        Filter,  Exposure, OT,  uplim (3 sigma)
(mid, d)             (s)

 2.0972       R     22x180      n/d     20.8


GRB_name: GRB120724A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13519
SUBJECT: GRB 120724A: JCMT SCUBA-2 sub-mm observation
DATE:    12/07/25 20:30:50 GMT
FROM:    Ian Smith at Rice U  <ian@spacsun.rice.edu>

I.A. Smith (Rice U.), R.P.J. Tilanus (JAC), N.R. Tanvir (U. of Leicester),
D.A. Frail (NRAO) report:

We observed the location of GRB 120724A (D'Avanzo et al., GCN Circ.
13510) using the SCUBA-2 sub-millimeter continuum camera on the James
Clerk Maxwell Telescope.  The observation started at 07:48 UT on
2012-07-24, corresponding to 69 minutes after the burst trigger.
Exposures totaling 1.7 hours were made in reasonable weather conditions.
No source was detected, with a preliminary RMS of 3.3 mJy/beam at 
850 microns.

We thank Jeff Cox and Antonio Chrysostomou for their prompt support of 
these observations.


GRB_name: GRB120724A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13520
SUBJECT: GRB 120724A: optical observation in Maidanak observatory
DATE:    12/07/26 19:48:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Sergeev (Institute of Radio Astronomy of NASU), A. 
Volnova (SAI MSU), O. Burhonov (UBAI), I. Molotov (KIAM) report on behalf 
GRB follow-up collaboration:

We observed  the field of Swift  GRB 120724A (D'Avanzo et al., GCN 13510) 
with AZT-22 telescope of Maidanak observatory starting on Jul. 24 (UT) 
15:55:51 under mean seeing (FWHM) of about 1.1 arcsec. Totally we obtained 4 
images of 600 s exposure in R  filter. At the edge of the enhanced XRT 
position (Goad et al., GCN 13515) we detected the object with coordinates 
(J2000) 16 20 43.28  +03 30 27.1 (uncertainty of  0.12 arcsec in both 
coordinates), which is slightly apart from coordinates of the OT reported 
earlier (Guidorzi  et al., GCN 13511; Holland et al., GCN 13516).  Since the 
object is also visible in stacked DSS images (R+I) we suggest it is a 
possible host galaxy of GRB 120724A.

A preliminary photometry of the object is based on USNO-B1.0 nearby stars:

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

 0.42252       R    3x600        20.97 +/- 0.09

A finding chart can be found at 
http://grb.rssi.ru/GRB120724A/GRB120724A_AZT22&DSS.png


GRB_name: GRB120722A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13521
SUBJECT: GRB 120722A: optical upper limit
DATE:    12/07/27 15:28:21 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed the field of the Swift GRB 120422A (Troja et al., GCN
13243) with 20-inch telescope C40 of Kuban State University
Astrophysical Observatory on April 22 between (UT) 18:51:21 - 21:54:56
under mean FWHM of about 3.5 arcsec. We took two series of 30 s and 60
s exposures using R filter. In a stacked image we do not detect any
source in the enhanced XRT error circle (Evans et al., GCN 13502). A
preliminary photometry is based on the nearby USNO-B1.0 stars:

T0+         Filter, Exposure,              OT,   uplim (3 sigma)

(mid, d)             (s)
0.28316   R       60*30s + 31*60s     n/d   21.2


GRB_name: GRB120716A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13523
SUBJECT: GRB 120716A: optical observation in Maidanak observatory
DATE:    12/07/28 14:43:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Sergeev (Institute of Radio Astronomy NASU), A. 
Volnova (SAI MSU), O. Burhonov (UBAI), I. Molotov (KIAM) report on behalf of 
larger GRB follow-up collaboration:

We observed the region of the optical afterglow (Cenko et al., GCN 13489) 
of IPN localized GRB 120716A (Hurley et al., GCN 13487) with AZT-22 
telescope  of Maidanak observatory on Jul. 19 (UT) 17:57:06  and Jul. 21 
(UT) 18:46:16 under mean seeing  of about 0.6 arcsec.  Totally we obtained 8 
images of 600 s exposure in R  filter. In each particular image we clearly 
see the optical afterglow (Cenko et al., GCN 13489; Xu  et al., GCN 13490; 
Schady  et al., GCN 13492) in coordinates (J2000) 20:52:12.15 +09:35:54.2 
(uncertainty of 0.13 arcsec in both coordinates).

Preliminary photometry of the afterglow is based on USNO-B1.0 nearby stars:

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

date            t_start (UT)    filter   exp,s    OT

2012-07-19  17:57:06      R      4*600  20.71+/-0.04
2012-07-21  18:46:16      R      4*600  21.01+/-0.04 


GRB_name: GRB120728A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13525
SUBJECT: GRB 120728A: Swift detection of a burst
DATE:    12/07/28 22:37:55 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), C. B. Markwardt (NASA/GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL), M. H. Siegel (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 22:25:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120728A (trigger=529021).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 137.100, -54.437, which is 
   RA(J2000)  =  09h 08m 24s
   Dec(J2000) = -54d 26' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a peak with structure
with a total duration of about 20 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 22:27:38.8 UT, 147.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 137.09412, -54.43783 which
is equivalent to:
   RA(J2000)  = 09h 08m 22.59s
   Dec(J2000) = -54d 26' 16.2"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 12 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 5.18
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
148 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. Because of the density of catalogued stars, further analysis
is required to report an upper limit for any afterglow in the sub-image. The
8'x8' region for the list of sources generated on-board covers 100% of the 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 J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120728A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13526
SUBJECT: GRB 120728A: GROND observations
DATE:    12/07/29 02:20:44 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of GRB 120728A (Swift trigger 529021; Cummings et
al., GCN 13525) 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 23:05 UT on 2012-07-28, 41 minutes after the GRB
trigger. Observations were obtained in twilight, at high (2.5) airmass and
bad seeing (2".7 in the r' band).

Based on an exposure of 9.4 minutes in the optical and 16 minutes in the
NIR we do not detect any source within the Swift/XRT error circle at
coordinates RA, Dec(J2000)= 09:08:22.69, -54:26:17.7, error 3".6. (SPER
data)

At the edge of the error circle, we find two sources. One, at RA (J2000)
= 09:08:23.20, Dec. (J2000) = -54:26:18.8, is a star also visible in the
DSS. The other may be marginally detected in the DSS, and likely consists
of two sources, centered at (+/- 0".5) RA (J2000) = 09:08:22.82, Dec.
(J2000) = -54:26:13.1 and RA (J2000) = 09:08:22.55, Dec. (J2000) =
-54:26:14.2. We are unable to make any statements about the variability
of these objects at this time, but given the crowded field this close to
the Galactic plane, it is likely neither is associated with the GRB.

Preliminary limiting magnitudes (AB mags) are:

  g' > 21.6
  r' > 21.9
  i' > 21.3
  z' > 21.1
  J  > 19.5
  H  > 19.9
  Ks > 19.3.

Magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS
stars (JHKs). No correction for the high Galactic reddening along the
line of sight (E(B-V)=0.57 mag; Schlegel et al. 1998) has been applied.


GRB_name: GRB120728A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13528
SUBJECT: GRB 120728A: Enhanced Swift-XRT position
DATE:    12/07/29 09:02:12 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 4986 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 120728A, 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 = 137.09469, -54.43760 which is equivalent
to:

RA (J2000): 09h 08m 22.73s
Dec (J2000): -54d 26' 15.4"

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: GRB120728A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13529
SUBJECT: GRB 120728A: Swift-XRT refined Analysis
DATE:    12/07/29 10:38:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 120728A (Cummings  et al.
GCN Circ. 13525), from 161 s to 24.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN. Circ 13528).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.98 (+/-0.25).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.67 (+0.25, -0.10). The
best-fitting absorption column is  consistent with the Galactic value
of 5.2 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.4 x 10^-11 (1.1 x 10^-10) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+2.2, -0) x 10^20 cm^-2
Galactic foreground: 5.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.67 (+0.25, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00529021.

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


GRB_name: GRB120729A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13530
SUBJECT: GRB 120729A: Swift detection of a burst with an optical afterglow
DATE:    12/07/29 11:17:04 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

T. N. Ukwatta (MSU), D. N. Burrows (PSU), M. M. Chester (PSU),
S. T. Holland (STScI), H. A. Krimm (CRESST/GSFC/USRA),
V. Mangano (INAF-IASFPA), A. Maselli (INAF-IASFPA),
E. Sonbas (NASA/GSFC/Adiyaman Univ.) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift Team:

At 10:56:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120729A (trigger=529095).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 13.056, +49.940 which is 
   RA(J2000) = 00h 52m 13s
   Dec(J2000) = +49d 56' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-shaped
structure with a total duration of about 25 sec.  The peak count rate
was ~5700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 10:57:22.2 UT, 68.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
13.0745, 49.9401 which is equivalent to:
   RA(J2000)  = 00h 52m 17.88s
   Dec(J2000) = +49d 56' 24.5"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 43 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.42 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.1
(+1.91/-1.68) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.75e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 77 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 00:52:17.84 =  13.07433
  DEC(J2000) = +49:56:23.1  =  49.93974
with a 90%-confidence error radius of about 0.61 arc sec. This position is 1.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.26 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.16. 

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


GRB_name: GRB120729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13531
SUBJECT: GRB120729A - Faulkes Telescope North Optical Afterglow Candidate
DATE:    12/07/29 11:40:07 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F.J. Virgili (LJMU), J. Japelj (U. Ljubljana), C.G. Mundell (LJMU), A. Melandri (INAF-OAB) report:

"The 2-m Faulkes Telescope North robotically followed up GRB120729A
(SWIFT trigger 529095, Ukwatta et al. GCN 15530 ) 4.60 min after the GRB trigger time.
The automatic "detection mode" procedure LT-TRAP (Guidorzi et al. 2006) detected a variable uncatalogued afterglow
candidate consistent with the UVOT detection and within the XRT/UVOT and error circles at:

RA 00 52 17.82
DEC 49 56 23    (J2000)

with magnitude R = 16.4 mag (vs USNOB1) 4.60 min after the burst.

Observations are ongoing.


GRB_name: GRB120729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13532
SUBJECT: GRB 120729A Gemini-N redshift 
DATE:    12/07/29 13:16:08 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester) and J. Ball (Gemini) report on behalf of a 
larger collaboration:

We observed the afterglow of GRB 120729A (Ukwatta et al. GCN 13530)
using the GMOS-N spectrograph on Gemini-North.

Observations began at 2012-7-29 12:11 UT, about 75 mins post-burst.
The spectrum reveals strong absorption lines of MgI, MgII, FeII, MnII.  
A provisional reduction gives a redshift of z=0.80, which we believe is most 
likely the redshift of this burst.


GRB_name: GRB120728A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13533
SUBJECT: GRB 120728A: Swift/UVOT Upper Limits
DATE:    12/07/29 13:31:20 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120728A
148 s after the BAT trigger (Cummings et al., GCN Circ. 13525).
No optical afterglow consistent with the XRT position
(Osborne et al., GCN Circ.13528) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

u_FC               148          398          246         >19.5
v                  456        17454         1356         >20.6
b                  404        24174         2261         >22.3
u                  148        23261         2438         >21.0
w1                 505        19107         1200         >20.8
m2                 480        18359         1357         >21.0
w2                 430        24878         1735         >21.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.53 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120729A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13534
SUBJECT: GRB 120729A: Enhanced Swift-XRT position
DATE:    12/07/29 15:41:52 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 1033 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120729A, 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 = 13.07446, +49.93967 which is equivalent
to:

RA (J2000): 00h 52m 17.87s
Dec (J2000): +49d 56' 22.8"

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: GRB120728A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13535
SUBJECT: GRB 120728A, Swift-BAT refined analysis
DATE:    12/07/29 16:13:33 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@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) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120728A (trigger #529021)
(Cummings, et al., GCN Circ. 13525).  The BAT ground-calculated position is
RA, Dec = 137.085, -54.437 deg which is
    RA(J2000)  =  09h 08m 20.3s
    Dec(J2000) = -54d 26' 12.4"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 13%.

The mask-weighted light curve shows a broad FRED-like peak of total duration
~25 seconds with three subsidiary peaks superimposed.  The
T90 (15-350 keV) is 22.06 +- 2.59 sec (estimated error including systematics).

The time-averaged spectrum from T+0.56 to T+26.46 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.79 +- 0.13.  The fluence in the 15-150 keV band is 2.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+12.12 sec in the 15-150 keV band
is 2.4 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/529021/BA/


GRB_name: GRB120729A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13536
SUBJECT: GRB 120729A, Swift-BAT refined analysis
DATE:    12/07/29 16:17:26 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA),C. B. Markwardt (GSFC), 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-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120729A (trigger #529095)
(Ukwatta, et al., GCN Circ. 13530).  The BAT ground-calculated position is
RA, Dec = 13.078, 49.936 deg which is
    RA(J2000)  =  00h 52m 18.8s
    Dec(J2000) = +49d 56' 08.5"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.

The mask-weighted light curve shows a single FRED peak with a rise of ~20 secs
and a fall of ~100 seconds.  There are no significant subsidiary peaks.
T90 (15-350 keV) is 71.5 +- 17.5 sec (estimated error including systematics).

The time-averaged spectrum from T-3.08 to T+101.94 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.08.  The fluence in the 15-150 keV band is 2.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.03 sec in the 15-150 keV band
is 2.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/529095/BA/


GRB_name: GRB120729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13537
SUBJECT: GRB 120729A: Xinglong TNT optical upper limit
DATE:    12/07/29 17:51:13 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 120729A (Ukwatta et al. GCN Circ. 13530 ) 
with Xinglong TNT telescope at 15:23:22.671 (UT), 4.45 hour after 
the burst. A series of R-band images were obtained. 
Preliminary analysis shows that no any source was found 
at the location of optical counterpart (Ukwatta et al. GCN Circ. 13530;
Virgili et al. GCN 13531), down to 3 sigma upper limit of R~19.5 mag,
relatively to the USNO B1.0 R2 mag, at the mean time of 4.8 hour after
the burst.

This message may be cited.

Thanks to the help of TNT observation assistant for this work. 

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


GRB_name: GRB120729A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13539
SUBJECT: GRB 120729A: Swift/UVOT Detection
DATE:    12/07/29 18:39:35 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and T. N. Ukwatta (MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120729A
77 s after the BAT trigger (Ukwatta et al., GCN Circ. 13530).
A source consistent with the XRT position (Beardmore et al., GCN Circ. 13534)
and the optical position reported by FTN (Virgili et al., GCN Circ. 13531) is 
detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  00:52:17.83 =  13.07431 (deg.)
  Dec (J2000) = +49:56:23.1  =  49.93974 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

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

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

white               77          227          147         15.33 +/- 0.02
v                  620          640           20         15.92 +/- 0.15
b                  545          564           20         16.56 +/- 0.12
u                  289          539          246         15.78 +/- 0.04
w1                4113         4313          197         18.49 +/- 0.16
m2                3908         4108          197         18.91 +/- 0.25
w2                 595          615           20         17.57 +/- 0.32

The magnitudes in the table are 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: GRB120729A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13541
SUBJECT: GRB 120729A: Swift-XRT refined Analysis
DATE:    12/07/29 23:17:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 13 ks of XRT data for GRB 120729A (Ukwatta  et al. GCN
Circ. 13530), from 74 s to 29.5 ks after the  BAT trigger. The data
comprise 170 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN. Circ 13534).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.115 (+0.023, -0.022), followed by a break at T+8203 s
to an alpha of 2.9 (+/-0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+/-0.10). The
best-fitting absorption column is  1.9 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 1.4 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.87 (+0.15, -0.14)
and a best-fitting absorption column of 2.1 (+0.5, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.2 x 10^-11 (5.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.1 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^21 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.87 (+0.15, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00529095.

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


GRB_name: GRB120728A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13542
SUBJECT: GRB 120728A: GROND Afterglow discovery
DATE:    12/07/30 10:09:43 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed again the field of GRB 120728A (Swift trigger 529021; Cummings
et al., GCN 13525) 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).

Compared to our first epoch (Kann et al., GCN 13526), seeing conditions
significantly improved to 1".5 in the r' band. We obtained 7 minutes of
optical observations and 12 minutes of NIR observations centered 1.035 days
after the GRB. We achieve limiting magnitudes which are 0.5 mag deeper in
all optical bands compared to our first epoch, but shallower in the NIR.

The enhanced Swift-XRT position (Osborne et al., GCN 13528) does not include
the bright DSS source in the south-east anymore, but still overlaps with the
two northern sources (Kann et al., GCN 13526). Upon close inspection, the
eastern source is also detected in the DSS, whereas the western source is
not. This source is furthermore not present anymore in our second epoch,
which we confirm by image subtraction.

We therefore propose this source to be the optical afterglow of GRB 120728A,
and derive a position:

RA  (J2000) =  09:08:22.62,
DEC (J2000) = -54:26:14.5

with an error of 0".8.

The preliminary magnitude is r' = 20.80 +/- 0.16 (statistical) +/- 0.27
(systematic) against the USNO-B1.0 catalog in the first epoch, 0.0377 days
after the GRB.


GRB_name: GRB120729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13543
SUBJECT: T100 observations of GRB 120729A
DATE:    12/07/30 10:54:36 GMT
FROM:    Tolga Guver at UA  <tolga@physics.arizona.edu>

Guver, T. (Sabanci Univ.), Sonbas, E. (GSFC, Adiyaman Univ.), S.  
Kaynar (Akdeniz Univ.), O. Onal (Istanbul Univ.), S. Tuncel Guctekin  
(Istanbul Univ.),
Gogus, E. (Sabanci Univ.), S. Ak (Istanbul Univ.), Z. Eker (TUG) on  
behalf of a larger collaboration.

We observed the field of GRB 120729A (Ukwatta et al., GCN #13530)
with the 1.0 meter T100 telescope (TUBITAK National Observatory,
Antalya - Turkey), starting at 2012-07-29, 19:43:07 UT ( ~9 hours
after the trigger). We obtained 4 x 300 s exposures with R filter under poor
weather conditions (seeing 2.4").

Similar to the report by Xin et al. (GCN #13537) we do not detect an
optical afterglow at the UVOT error circle reported by Ukwatta et al.
(GCN #13530) in the combined R band image. We determine the 4-sigma
detection limit of our R band image to be 20.04 mag, (calibrated to R2
of USNO-B1).

We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their technical support.

----------------------------------------------------------------
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GRB_name: GRB120729A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13544
SUBJECT: GRB 120729A: UKIRT Observation
DATE:    12/07/30 14:05:05 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im and Jueun Hong (CEOU/Seoul National Univ.) on behalf of 
a larger collaboration.

We observed GRB 120729A (Ukwatta et al., GCN 13530) in
ZYJHK using WFCAM on UKIRT.

The observation started at 2012-07-29 13:01:41 UT, 
or about 2.09 hours after the BAT alert. 
In all of the ZYJHK images, we identify the afterglow
(H ~ 18.0 AB mag) which was reported earlier by several groups 
(Virgili et al. GCN 13531; Oates et al. GCN 13539).
We also confirm fading of the object from another set of
WFCAM data we took about 3 hours later.

Further observations are planned.


GRB_name: GRB120729A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13545
SUBJECT: GRB 120729A: Early RAPTOR Observations
DATE:    12/07/30 21:15:47 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes responded to Swift trigger
529095 (Ukwatta et al., GCN 13530).  Observations began at 10:56:42.0 UT,
27.9 s after the initial Swift trigger and before the end of the gamma-ray
emitting interval.  Our observations were performed under clear skies with
morning twilight just beginning.  We clearly detect the optical counterpart
(Ukwatta et al., GCN 13530, and Virgili et al., GCN 13531).  We initially
detect the counterpart at a magnitude of 13.2, and at about T+50 s
it begins to fade steadily at a power law index of about 0.9 for the next
1000 seconds.  Our unfiltered magnitudes are calibrated against the USNO-B1
R-band.  The following table gives a sample of some of our observations.
The image mid-points are given relative to the initial BAT trigger time.

t-mid(s)  exp(s)  mag     error
--------------------------------------
30.4      5       13.21   0.01
39.8      5       13.28   0.01
49.2      5       13.35   0.01
118.4     10      14.18   0.01
248.8     10      14.97   0.02
391.8     30      15.36   0.02
817.0     30      16.11   0.06
1071.4    30      16.46   0.11


GRB_name: GRB120729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13546
SUBJECT: Virtual Telescope  observations of GRB 120729A
DATE:    12/07/30 21:58:10 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy) report:

On July 29.9496 2012 UT, we imaged the field around the position provided
by Ukwatta et al. (GCN 13530) with the 0.43m-f/6.8 unit part of the Virtual
Telescope robotic facility in Italy.

4, 300 seconds unfiltered CCD images were coadded and compared with a R plate
from the DSS2: they do NOT show any obvious afterglow, down to R = 20.0 (based
on USNO B1.0). The position of the afterglow mentioned on GCN 13530 is close to
a R=19.2 source (with end figures 18.28s and 23.2", J2000).


GRB_name: GRB120729A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13547
SUBJECT: GRB 120729A: EVLA Observations
DATE:    12/07/31 02:39:04 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 120729A (Ukwatta et al. GCN 13530) with
the EVLA beginning 2012 July 30.3 UT (0.84 days after the burst). No
significant radio emission is detected at the enhanced Swift-XRT position
(Beardmore et al. GCN 13534), the UVOT position (Oates et al. GCN 13539) or
optical position (Virgili et al. GCN 13531) to three-sigma upper limits
of 39 uJy and 58 uJy, at 5.8 and 21.8 GHz, respectively."


GRB_name: GRB120729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13548
SUBJECT: GRB 120729A: RTT150 optical observations
DATE:    12/07/31 10:28:25 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

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

report:

We observed the field of the Swift-BAT GRB 120729A (Ukwatta et al. GCN
15530 ) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe,
TUBITAK National Observatory, Turkey), starting at 30 Jul, 01:26 UT,
i.e. approximately 14.5 hours after the burst, using TFOSC instrument.

We made 6x300s exposures in R-band under good atmospheric conditions
(1.4 arcsec seeing) at the beginning of morning twilight without
moonlight. We do not detect any new source on combined image at the
position of OT (Virgili et al., GCN13531; Oates and Ukwatta,
GCN13539). Using USNO-B1 stars we estimated the limiting magnitude of
combined image as m_R =~ 23.5.

A small field around of the OT position can be found at:

http://hea.iki.rssi.ru/grb/120729a/indexeng.html


GRB_name: GRB120728B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13549
SUBJECT: IPN Triangulation of GRB 120728B (long/intense)
DATE:    12/07/31 10:36:31 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,

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

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

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

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

The long-duration, intense GRB 120728B was observed by Konus-Wind, Fermi 
(GBM: trigger 365163927), INTEGRAL (SPI-ACS), Mars Odyssey (HEND), and 
RHESSI at about 37524 s UT (10:25:24).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   103.772 (06h 55m 05s) -45.893 (-45d 53' 36")
  Corners:
   103.695 (06h 54m 47s) -44.477 (-44d 28' 37")
   103.463 (06h 53m 51s) -47.210 (-47d 12' 37")
   103.857 (06h 55m 26s) -47.308 (-47d 18' 29")
   104.069 (06h 56m 17s) -44.576 (-44d 34' 33")
  ---------------------------------------------
The error box area is 0.745 sq. deg, and its maximum
dimension is 2.8 deg.

This box can be improved.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120728_T37534/IPN/


GRB_name: GRB120729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13550
SUBJECT: GRB 120729A: Optical observations from OSN, BOOTES1/2 and IAC80 
DATE:    12/07/31 10:53:25 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), M. Jelinek (IAA-CSIC), Ch. Wang (Yunnan
Observatory, China), C. Zurita (IAC), A. Sota (OSN, IAA-CSIC), J.C. Tello
(IAA-CSIC), R. Sanchez-Ramirez (IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC),
report on behalf of a larger collaboration:

"We carried out BRI-band observations of the GRB 120729A (Ukwatta et al.
GCN Circ. 13530) optical afterglow (Virgili et al. GCN Circ. 13531; Oates
et al. GCN Circ. 13539) as follows:

Telescope Obs.Date(UT) Time post GRB(hr) Exp.Time(s) Mag.(Vega)
------------------------------------------------------------------------
0.3m Bootes-1B  29.879537-30.022106     10.17-13.58     326x30  R > 19.0
0.6m Bootes-2 30.007951-30.042095     13.25-14.07     50x60   R > 19.4
1.5m OSN 30.077613-30.163785     14.93-16.99     18x300  R > 22.1
1.5m OSN 30.096195-30.099667     15.37-15.45     1x300   B > 21.5
0.82m IAC80 30.120174-30.205093     15.95-17.98     22x300  I = 21.9+/-0.3

The calibration was based on the USNO B1.0 catalogue."


GRB_name: GRB120729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13551
SUBJECT: GRB 120729A: break in the optical light curve
DATE:    12/07/31 11:06:32 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), I. Steele, C.G. Mundell (LJMU),  
E. Palazzi (INAF-IASFBo) report, on behalf of larger collaborations:

We observed the optical counterpart of GRB 120729A (Ukwatta et al.,  
GCN 13530; Virgili et al., GCN 13531; Oates et al., GCN 13539; Wren et  
al., GCN 13545) with the 2-m Faulkes Telescope North (FTN), the 2-m  
Liverpool Telescope (LT) and with the Italian 3.6m Telescopio  
Nazionale Galileo (TNG). Early time observations were carried out from  
4.6 min to 2.1 hours after the burst with the FTN, while a later  
observation epoch was taken at a mid time of about 14.5 hours after  
the burst with the LT and the TNG.

 From a preliminary analysis the overall R-band light curve can be  
described by an initial power-law decay with an index of alpha1=1.0  
that breaks around t-t0=6000 s to a steeper decay with alpha2=1.8. The  
early time decay is consistent with the report of Wren et al. (GCN  
13545).

The last detection was obtained with the TNG at a level of R ~ 23.3  
mag (15.1 hours post burst) consistent with the marginal detections  
obtained with LT SDSS-r filter (image acquired ~13.6 hours after the  
burst). These late time values fall slightly below the best broken  
power-law fit described above, suggesting that the post-break decay  
index might be steeper than 2.

We note that the reported X-ray afterglow decay (Maselli et al., GCN  
13541) shows a similar behaviour and that this may be indicative of an  
achromatic break in the afterglow light curve.

We thank the TNG staff for performing the ToO observations, in  
particular Massimo Cecconi.


GRB_name: GRB120728B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13552
SUBJECT: Konus-Wind observation of GRB 120728B
DATE:    12/07/31 14:19:25 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 120728B
(IPN detection and localization: Hurley at al., GCN 13549)
triggered Konus-Wind at T0=37534.985s UT (10:25:34.985)

The light curve shows multiple pulses in at least
three main bursting episodes.
The total duration of the burst is ~250 s,
the emission is seen up to 5 Mev.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120728_T37534/

As observed by Konus-Wind, the burst
had a fluence of 1.20(-0.15,+0.15)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+57.472 s,
of 3.8(-0.4,+0.4)x10-6 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+192.256 s)
is best fit in the 20 keV - 5 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.3 (-0.1, +0.1),
the high energy photon index beta = -2.9 (-1.0, +0.3),
the peak energy Ep = 77(-5, +4) keV,
chi2 = 86.9/75 dof.

The spectrum at the maximum count rate
(measured from T0+55.552 to T0+64.256 s) is best fitted
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model, for which:
alpha = -1.0 (-0.1, +0.1),
and Ep = 95(-4, +4) keV,
chi2 = 67.8/57 dof.


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


GRB_name: GRB120728B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13553
SUBJECT: GRB 120728B: Fermi GBM detection
DATE:    12/07/31 20:59:26 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

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

"At 10:25:24.24 UT on 28 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120728B (trigger 365163927 / 120728434)
which was also detected by Konus-Wind
(Golenetskii et al., GCN 13552).
This burst was localized by the IPN (Hurley et al., GCN 13549).
The GBM on-ground calculated location is consistent with the
IPN location.

The angle from the Fermi LAT boresight is 117 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous repoint request (ARR) maneuver.

The GBM light curve consists of multiple pulses
with a duration (T90) of about 105 s (50-300 keV).
The time-averaged spectrum from T0+8.7 s to T0+113.2 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.31 +/-0.01 and
the cutoff energy, parameterized as Epeak, is
94.86 (+1.04/-1.01) keV.

The event fluence (10-1000 keV) in this time interval is
(1.27 +/- 0.02)E-4 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+69.6 s in the 10-1000 keV band
is 42.8 +/- 0.6 ph/s/cm^2.


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


GRB_name: GRB120729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13554
SUBJECT: GRB 120729A: JCMT SCUBA-2 sub-mm observation
DATE:    12/07/31 22:33:41 GMT
FROM:    Ian Smith at Rice U  <ian@spacsun.rice.edu>

I.A. Smith (Rice U.), R.P.J. Tilanus (JAC), N.R. Tanvir (U. of Leicester),
D.A. Frail (NRAO) report:

We observed the location of GRB 120729A (Ukwatta et al., GCN Circ.
13530) using the SCUBA-2 sub-millimeter continuum camera on the James
Clerk Maxwell Telescope.  The observation started at 12:14 UT on
2012-07-29, corresponding to 78 minutes after the burst trigger.
Exposures totaling 3.1 hours were made in reasonable weather conditions.
No source was detected, with a preliminary RMS of 1.8 mJy/beam at 
850 microns.

We thank Jeff Cox and Ruud Visser for their prompt support of these 
observations.


GRB_name: GRB120802A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13555
SUBJECT: GRB 120802A: Swift detection of a burst
DATE:    12/08/02 08:14:00 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

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

At 08:00:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120802A (trigger=529486).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 44.849, +13.757 which is 
   RA(J2000) = 02h 59m 24s
   Dec(J2000) = +13d 45' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two overlapping FRED 
peaks with a duration of about 20 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~8 sec after the trigger. 

The XRT began observing the field at 08:02:16.3 UT, 84.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 44.84120, 13.76787 which
is equivalent to:
   RA(J2000)  = 02h 59m 21.89s
   Dec(J2000) = +13d 46' 04.3"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 47 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 9.65
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 86 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 S. T. Holland (sholland AT stsci.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120802A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13556
SUBJECT: GRB 120802A: optical uper limit in ISON-NM observatory
DATE:    12/08/02 10:06:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), 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, 
i.e. 12.5 minutes after burst  trigger.  We took  several unfiltered images 
of 30 s exposure.  We do not detect any source within XRT error circle 
(Holland et al., GCN 13555) in any co-added frames.   The preliminary 
photometry of  co-added frames is based  on the USNO-B1.0 (R2)  nearby 
stars:

T_start,     Exposure, OT,  Upper Limit (3sigma)
(UT)           (s)

08:13:18    10x30       n/d    17.5
08:13:18    20x30       n/d    17.7
08:13:18    29x30       n/d    18.1

Observations are continued. 


GRB_name: GRB120802A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13557
SUBJECT: GRB 120802A: MASTER optical observations
DATE:    12/08/02 10:14:46 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 GRB120802A (Holland et al, GCN 13555) 21 s after notice 
time and 43 s after GRB time at 2012-08-02 
08:01:34 UT under full Moon. We haven't found optical transient  within 
SWIFT error-box  our first (5 s exposure) set.
The 5-sigma upper limit has been about 10.6 
mag The 5-sigma upper limit on coadd first 42 images is about 12.0 mag.

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

This message can be cited.


GRB_name: GRB120802A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13558
SUBJECT: GRB 120802A: Enhanced Swift-XRT position
DATE:    12/08/02 11:57:38 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 539 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120802A, 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 = 44.84185, +13.76805 which is equivalent
to:

RA (J2000): 02h 59m 22.04s
Dec (J2000): +13d 46' 05.0"

with an uncertainty of 2.8 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: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13559
SUBJECT: GRB 120802A: Swift-BAT refined analysis
DATE:    12/08/02 12:29:32 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),
S. T. Holland (STScI), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), 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-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120802A (trigger #529486)
(Holland, et al., GCN Circ. 13555).  The BAT ground-calculated position is
RA, Dec = 44.833, 13.762 deg, which is 
   RA(J2000)  =  02h 59m 20.0s 
   Dec(J2000) = +13d 45' 43.1" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.
 
The mask-weighted light curve shows a small precursor peak from ~T-40 to ~T-33 sec,
then a fast rise at ~T-2 sec, peaking at ~T+2 sec and decaying exponentially
with a second peak peaking at ~T+8 sec and ending at ~T+45 sec.
T90 (15-350 keV) is 50 +- 31 sec (estimated error including systematics).
 
The time-averaged spectrum from T-35.68 to T+28.02 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.21 +- 0.47, 
and Epeak of 57.2 +- 19.4 keV (chi squared 52.25 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.9 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+7.94 sec in the 15-150 keV band is
3.0 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.84 +- 0.10 (chi squared 58.45 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/529486/BA/


GRB_name: GRB120729A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13560
SUBJECT: GRB 120729A: Fermi GBM observation
DATE:    12/08/02 12:40:37 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

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

"At 10:56:12.67  UT on 29 July 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120729A (trigger 365252175  / 120729456)
which was also detected by the Swift/BAT (Ukwatta et al. 2012, GCN 13530).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 83 degrees.

The GBM light curve shows a single pulse with a duration (T90) of about 25 s (50-300 keV).
The time-averaged spectrum from T0-3.6 s to T0+17.9 s is
best fit by a simple power law function with index -1.49 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(5.1 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.2 s in the 10-1000 keV band
is 5.2 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB120802A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13561
SUBJECT: GRB 120802A: APEX/LABOCA submm observations
DATE:    12/08/02 14:09:06 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Richard 
(CRAL, U. Lyon), P. Moller (ESO), C. de Breuck (ESO),
C. Agurto (ESO) and F. Azagra (ESO) report on behalf of a 
larger collaboration:

We have observed the field of GRB 120802A (Holland et 
al. GCN 13555) using APEX/LABOCA (Chajnantor, Chile) 
in the 870um band (345 GHz) under poor weather conditions 
(PWV starting at 2.0 mm and going down to 1.4 mm at the end 
of the observation). Data acquisition started at 08:58 UT 
(58 min after the burst) and lasted for 3.5hr (2.7hr on source). 
In a preliminary analysis we do not detect any source at the GRB 
position, where we have an r.m.s. of 4mJy/beam (3-sigma limit of 
12 mJy/beam). 


GRB_name: GRB120802A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13562
SUBJECT: GRB 120802A Gemini-N redshift 
DATE:    12/08/02 19:52:48 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), D. Fox (Penn State), J. Fynbo (DARK) 
and C. Trujllo (Gemini) report on behalf of a larger collaboration:

We observed the afterglow of GRB 120802A (Holland et al. GCN 13555)
using the GMOS-N spectrograph on Gemini-North, covering a spectral 
range of about 5900A to 10000A.

Observations began at 2012-8-2 13:30 UT, about 5:30 hr post-burst.
The spectrum reveals many absorption lines including S II (1250), 
Si II (1260/1304/1526/1808), O I (1304), C II (1334), Si IV (1394/1403), 
C IV (1548/1551), Fe II (1608), Al II (1670) at a common redshift of z=3.796, 
which we believe is most likely the redshift of this burst.  We no clear
evidence of any fine-structure lines.

Note, this redshift is consistent with the absence of a strong Lyman-alpha line or 
Lyman-alpha forest since they would just fall off the blue end of our spectrum.

We also detect an intervening system at z=2.38, based on Fe II and Mg II features.


GRB_name: GRB120802A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13563
SUBJECT: GRB 120802A: Swift-XRT refined Analysis
DATE:    12/08/02 20:14:04 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), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester), V.
Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU) and S.T. Holland report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 120802A (Holland  et al.
GCN Circ. 13555), from 88 s to 17.6 ks after the  BAT trigger. The data
comprise 22 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 13558).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.7 (+/-0.4), followed by a break at T+270 s to an alpha
of 0.35 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 (+0.21, -0.20). The
best-fitting absorption column is  1.5 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 9.6 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 3.6 x 10^-11 (5.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 9.6 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.10 (+0.21, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00529486.

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


GRB_name: GRB120802A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13564
SUBJECT: GRB 120802A: GRT Optical Observation
DATE:    12/08/02 22:24:03 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (GSFC), Y. Urata (NCU)

We observed the field of GRB 120802A detected by Swift
(trigger #529486; Holland et al., GCN Circ. 13555) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

30 images of 60 sec exposures were taken in the R filter starting 
from August 2 08:37:05  (UT) about 36 minues after the trigger and 
stopped on August 2 09:08:49 (UT).  We do not detect the optical 
afterglow both in the individual images and the stacked image, which only 
combined 27 good quality images, inside the enhanced XRT position 
(Evans et al., GCN #13558).  The estimated five sigma upper limit of 
the combined image (total exposure of 1620 sec) is ~17.2 mag using 
the USNO-B1 catalog.


