# GCN_circulars

GRB_name: GRB120219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12987
SUBJECT: GRB 120219A, the review of the sky area in plate archives
DATE:    12/02/24 22:02:58 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120219A (M.R. Goad et al. GCN Circ.12967) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19830312/185937 GUA040C000131A 11.7 15.3 1350-07433967
19840128/215634 GUA040C000295A 13.5 15.3 1350-07433967
19840128/221630 GUA040C000296 13.5 15.3 1350-07433967
19900105/000440 GUA040C001552A 18.0 15.3 1350-07433967
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C  M=103"/mm) of the Ukrainian NAS Main Astro obs.
         (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 20 minutes area around 
       the location given in M.R. Goad et al. GCN Circ.12967: 
       RA(J2000)= 08h 39m 09.66s, Dec(J2000)= +51d 01'54.2"
Star USNOA2 - Comparison star.
  The preview images of 4 areas together with  
the 20x14 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120219A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120224A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12988
SUBJECT: GRB 120224A: GROND detection of the afterglow candidate
DATE:    12/02/27 01:33:33 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.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 GRB120224A (Swift trigger 515976; Saxton et al.,
GCN #12980) 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).

First observations started at 00:14 UT on 25 February 2012, 19.58 hrs
after the GRB trigger. They were perfomed at an average seeing of 1".27
and at an average airmass of 1.4.

After an exposure time of 4.72 min in g'r'i'z' and 8 min JHK, no source was
detected.

Second observations started at 00:48 UT on 26 February 2012, 1.84 days
after the GRB trigger. They were performed at an average seeing of 0".96
and at an average airmass of 2.0.

We find a single point source within the 1".8 refined Swift-XRT error circle
reported by Osborne et al. (GCN #12981) at

RA (J2000) = 02:43:46.15 = 40.94230

Dec. (J2000) = -17:45:42.0 = -17.76169

with an uncertainty of 0".5 in each coordinate.

Based on total exposures of 36 min in JHK, we estimate preliminary
magnitude (AB) of,

J = 20.9 +/- 0.2

The given magnitude is calibrated against 2MASS field stars and is not
corrected for the expected Galactic foreground extinction corresponding to
a reddening of E(B-V)=0.04 in the direction of the burst (Schlegel et al.
1998).


GRB_name: GRB120226A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12989
SUBJECT: GRB 120226A: Fermi-LAT detection of a burst
DATE:    12/02/27 13:53:07 GMT
FROM:    Vlasios Vasileiou at LUPM/Fermi-LAT  <Vlasios.Vasileiou@lupm.in2p3.fr>

V. Vasileiou (CNRS/IN2P3/LUPM) and J. L. Racusin (NASA/GSFC) report on behalf of
the Fermi-LAT team:

Fermi-LAT has detected high energy emission from GRB 120226A in ground analysis.
The GRB was triggered on by Fermi-GBM at 20:54:17.03 on Febuary 26, 2012
(trigger 351982459).

The GRB was significantly detected during the prompt phase only using a
non-standard LAT data selection most sensitive in the tens-of-MeV energy range,
with which over ~50 counts above background were detected within a 60 s interval
coinciding with the time of the GBM emission. This data selection has
insufficient spatial resolution to provide a reliable LAT localization.

However, the GRB became detectable with the standard LAT analysis techniques
only after data of longer time scales were accumulated. A preliminary
maximum-likelihood analysis of the E>100MeV P7SOURCE_V6 LAT data generated
during the first 1.9 ks after the GBM trigger (until the GRB became occulted by
the Earth) revealed a source with a ~4 sigma statistical significance,
corresponding to ~14 excess events. The source spectrum is best fit with a power
law of index -1.6+-0.3. Using this analysis, we obtained the best LAT on-ground
localization of:
RA(J2000) = 305.30 deg
Dec(J2000) = 40.75 deg
with an error radius 0.36 deg (90% containment, statistical error only), which
is 4 deg from the best GBM localization and ~37 deg with respect to the LAT
boresight at the time of the trigger. The GRB triggered an autonomous repoint of
the Fermi spacecraft bringing our best localization to ~12 deg from the LAT
boresight for 1.9 ks after the trigger. The burst position is close to the
Galactic plane at (l,b) = 78.5, 2.3 deg.

A Swift TOO has been requested.

The Fermi LAT point of contact for this burst is Vlasios Vasileiou
(vlasios.vasileiou@lupm.in2p3.fr).

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


GRB_name: GRB120224A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12990
SUBJECT: GRB 120224A: optical observation in Mondy observatory
DATE:    12/02/27 19:44:55 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 120224A (Saxton  et al., GCN 12980) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Feb. 24 between (UT) 
12:49:39 - 13:22:16  (mean time 8.44 hrs after burst trigger) in R filter 
under mean FWHM of 4.5" and at high airmass of  ~ 4 . In a combined image we 
do not detect the afterglow candidate (Elliott  et al., GCN 12988).  A 
photometry is based on the USNO-B1.0 star  USNO-B1.0 0722-0043384 
(02:43:36.48 -17:47:18.1) assuming R = 18.57:
:

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

0.3518    R     37 x 60         n/d        20.3


GRB_name: GRB120224A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12991
SUBJECT: GRB 120224A: VLT/X-shooter observations
DATE:    12/02/27 21:45:20 GMT
FROM:    Klaas Wiersema at U Leicester  <kw113@leicester.ac.uk>

K. Wiersema (Leicester), P. Goldoni (APC/Univ. Paris 7 and SAp/CEA), J. P.
U. Fynbo (DARK/NBI), N. R. Tanvir (U. Leicester), D. Malesani (DARK/NBI),
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), S. D. Vergani (INAF/OAB), S.
Covino (INAF/OAB), H. Flores (Obs. Paris) report on behalf of the
X-shooter GTO GRB collaboration:

We observed the position of the afterglow of GRB 120224A (Saxton et al.,
GCN 12980) using the X-shooter spectrograph mounted on the VLT.
Observations started on 00:30 UT on 25 February 2012, i.e. 19.83 hours
after burst.
In the acquisition images, 5 x 150 seconds in R filter, we find a faint
source, consistent with the candidate afterglow reported by Elliott et al
(GCN 12988). We find a preliminary magnitude of R=22.3 using the USNO-B
star 0722-0043411 (R=16.65). The detection of the afterglow in the R band
places a limit on the redshift of approximately z < 5.

We performed spectroscopy of this source, under poor seeing and high
airmass. We detect a faint continuum in the near-infrared arm over the
whole wavelength range, at low signal to noise.
In the visual arm data we detect a very faint continuum at the red end of
the wavelength range. No emission lines are detected. Because of the low
signal to noise we are not able to identify absorption features. The non-
detection of continuum emission below ~600 nm may be indicative of a
moderately high redshift for this burst, though alternatives, such as a
reddened spectrum (note that the X-ray afterglow shows considerable
absorption; Osborne et al. GCN 12986), can not be excluded at present.

We are grateful for the excellent support from the Paranal Observatory
staff, in particular Myriam Rodrigues and Ivo Saviane.


GRB_name: GRB120227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12992
SUBJECT: GRB 120227A: RAPTOR Limit During the Gamma-Ray Emitting Interval
DATE:    12/02/27 22:06:54 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR wide-field optical monitor located in Maui was observing the
location of GRB 120227A which occured at 09:22:46 UT (Fermi GBM trigger
352027367, INTEGRAL SPI-ACS trigger 6478).  Our system covered the entire
6.33 degree radius statistical error region specified in the Fermi-GBM
Final Position GCN notice.  The image that was coincident with the trigger
started at 09:22:40.6 UT with an exposure duration of 10 seconds.  This
unfiltered image has a 3-sigma limiting magnitude of approximately 10.3
when compared to the Tycho-2 V-band.  A visual inspection of this image
when differenced with one taken 17 minutes later does not show any candidate
optical counterparts within the specified error region.


GRB_name: GRB120226A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12993
SUBJECT: IPN Triangulation of GRB 120226A
DATE:    12/02/28 18:19:34 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,

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,

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

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

The long-duration, bright GRB 120226A was observed by Fermi (GBM: 
trigger 351982459), INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER (GRNS), 
Mars Odyssey (HEND), Swift (BAT), RHESSI, and Suzaku (WAM) at about 
75257 s UT (20:54:17). 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:
   302.930 (20h 11m 43s) +48.665 (+48d 39' 55")
  Corners:
   300.395 (20h 01m 35s) +46.181 (+46d 10' 53")
   303.595 (20h 14m 23s) +49.580 (+49d 34' 48")
   305.877 (20h 23m 30s) +51.105 (+51d 06' 19")
   302.306 (20h 09m 13s) +47.751 (+47d 45' 04")
  ---------------------------------------------

The error box area is 1.2  sq. deg, and its maximum
dimension is 6.1 deg.

This box can be improved.

The center of the LAT position reported by Vasileiou & Racusin (GCN 
12989) is 9.1 deg from the center of the error box (6.5 deg from the 
nearest corner).
Further analysis of the LAT data will be presented in a forthcoming GCN 
Circular.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120226_T75259/IPN/


GRB_name: GRB120226A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12994
SUBJECT: GRB 120226A: Fermi-LAT data analysis
DATE:    12/02/28 19:12:33 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 the high energy LAT data of GRB 120226A (Vasileiou and
Racusin, GCN 12989) using the matched filter technique (Akerlof et al,
2010, ApJ, 725, L15; 2011 ApJ, 726, 22; Zheng et al. 2012, ApJ 745,72,
GCN 12822). We only selected the photons with energy above 100 MeV in
our pipeline analysis. Our localization result gives the coordinate of
Ra = 300.05, Dec=48.81 (J2000) with uncertainty ~0.5 degree. This
location is about 7 degrees away from GBM trigger (Ra = 304.29,Dec =
42.1) and about 9 degrees away from the LAT location (Ra = 305.30, Dec =
40.75) given in GCN 12989. Our localization is much closer to the center
of IPN location (Ra = 302.930, Dec = 48.665, K. Hurley et al. GCN
12993), about 2 degrees away.

The LAT data signal is weak, too low to claim a firm detection. Only
four photons were identified near the estimated coordinate within a 50s
time window following the GBM trigger but by extending the duration to
250s, the number of photons increases to about 10. We encourage X-ray
follow-up observations of the new location.

All the pipeline results including the skymap can be found at the
following link:
http://www.rotse.net/LAT/GBMTriggers/351982459/351982459_res.html


GRB_name: GRB120226A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12995
SUBJECT: GRB 120226A: Fermi-GBM and Fermi-LAT detections; LAT position retraction  
DATE:    12/02/28 23:49:20 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

N. Omodei (SU), V. Pelassa (UAH), V. Vasileiou (CNRS/IN2P3/LUPM) and J. L. Racusin (NASA/GSFC) report on behalf of the Fermi LAT and GBM teams:

"At 20:54:17.03 UT on February 26, GRB 120226A triggered Fermi-GBM (trigger 351982459 / 120226871) and was detected by the Fermi-LAT during the prompt phase using a non-standard LAT data selection technique, as reported by Vasileiou and Racusin (GCN Circular 12989). It was also triangulated by the IPN (Hurley et al, GCN 12993).

The GBM light curve consists of several peaks with a duration (T90) of 57 +/- 2s (50-300 keV). The time-averaged spectrum for the GBM observation, from T0+0.004 s to T0+75.778 s, is well fit by a Band function with Epeak = 296.70 +/- 13.60 keV, alpha = -1.00 +/- 0.02 , and beta = -2.28 +/- 0.10 (Castor stat 742.54 for 487 d.o.f.).
The event fluence (10-1000 keV) in this time interval is (6.125 +/- 0.064)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+17.216 s in the 10-1000 keV band is 12.0 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog.

The significance of this burst in the LAT at low energies (above 20 MeV) is above 6 sigma using a class of non-standard events. The structure of the light curve is consistent with the GBM observation.
However, the re-analysis of P7SOURCE_V6 events shows that the temporally extended emission reported by Vasileiou and Racusin (GCN Circular 12989) is likely due to the bright pulsar PSR J2021+4026 in the field-of-view. This source is 0.31 degrees away from the position reported in GCN Circular 12989, and the measured flux (>100 MeV) of (1.32+/-0.02)E-06 ph/s/cm^2 (Nolan et al. 2012, in press. http://arxiv.org/abs/1108.1435) is also compatible with the observed number of gamma rays.

The IPN localization reported by Hurley et al. (RA=302.930, Dec=48.665; GCN Circular 12993) is not compatible with the original LAT localization and suggests that the analysis of GRB 120226A by Vasileiou and Racusin (GCN Circular 12989) was affected by the bright foreground pulsar. 

GRB 120226A is not detected at high energy by the LAT and therefore any localization using Fermi LAT data should be regarded with caution.

The Fermi LAT point of contact for this burst is Nicola Omodei (nicola.omodei@stanford.edu).

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


GRB_name: GRB120226A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12996
SUBJECT: Konus-Wind observation of GRB 120226A
DATE:    12/02/29 09:07:45 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 120226A (GBM trigger 351982459;
IPN localization: Hurley at al., GCN 12993;
Fermi/LAT & Fermi/GBM detection: Omodei et al., GCN 12995)
triggered Konus-Wind at T0=75259.724s UT (20:54:19.724)

The light curve shows multiple partly overlapped pulses.
A total duration of the burst is ~80 s.
The emission is seen up to ~4 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120226_T75259/

As observed by Konus-Wind the burst
had a fluence of 7.5(-1.2,+0.9)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+25.600 s,
of 2.5(-0.3,+0.3)x10-6 erg/cm2/s
(both in the 20 keV - 5 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 - 5 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.01 (-0.07, +0.07),
the high energy photon index beta = -2.5 (-0.9, +0.2),
the peak energy Ep = 279(-28, +39) keV,
chi2 = 88.6/75 dof.


The spectrum at the maximum count rate
(measured from T0+20.992 to T0+28.928 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.96 (-0.09, +0.10),
and Ep = 317(-42, +54) keV,
chi2 = 79.0/76 dof.

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


GRB_name: GRB120229A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12997
SUBJECT: GRB 120229A: Swift detection of a short burst
DATE:    12/02/29 14:57:25 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), B. Gendre (ASDC),
C. Guidorzi (U Ferrara), S. T. Holland (STScI), J. A. Kennea (PSU),
A. Y. Lien (NASA/GSFC/ORAU), O. M. Littlejohns (U Leicester),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), P. T. O\'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU),
C. A. Swenson (PSU), G. Tagliaferri (INAF-OAB) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 14:35:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120229A (trigger=516571).  Swift could not slew to the burst
due to a sun constraint. 
The BAT on-board calculated location is 
RA, Dec 20.035, -35.807 which is 
   RA(J2000) = 01h 20m 08s
   Dec(J2000) = -35d 48' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single short peak
structure with a duration of about 0.5 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 19:46 UT on 2012 April 17. There will thus be no XRT or
UVOT data for this trigger before this time. 

We note that this location is 5 arc minutes from the relatively
nearby (z=0.03) galaxy 6dFGSgJ012000.6-355307 . 

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: GRB120229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12998
SUBJECT: GRB 120229A, Swift-BAT refined analysis
DATE:    12/02/29 21:43:52 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@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), V. Mangano (INAF-IASFPA), 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 the recent telemetry downlink,
we report further analysis of BAT GRB 120229A (trigger #516571)
(Mangano, et al., GCN Circ. 12997).  The BAT ground-calculated position is
RA, Dec = 20.033, -35.796 deg which is
    RA(J2000)  =  01h 20m 07.9s
    Dec(J2000) = -35d 47' 44.0"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows two peaks, the first about 0.08 seconds
long peaking at T+0.03 and the second about 0.14 seconds long peaking at
T+0.21 seconds.  T90 (15-350 keV) is 0.22 +- 0.03 sec (estimated error
including systematics).

The time-averaged spectrum from T+0.01 to T+0.27 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.29 +- 0.24.  The fluence in the 15-150 keV band is 4.1 +- 0.7 x 10^-08 erg/cm2.
The 1-sec peak photon flux measured from T-0.36 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/516571/BA/


GRB_name: GRB120229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12999
SUBJECT: GRB 120229A: Spectral lag analysis
DATE:    12/02/29 22:11:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Norris (BSU), S.D. Barthelmy (GSFC) for the BAT Team:

We report the spectral lag analysis for GRB 120229A (GCN Circ. 12997)
based on the BAT data.  Using 4-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 0.8 +-8 msec, and 3.6 +5/-7 msec
for the 25-50 keV to 100-350 keV bands for both peaks combined.
These lag values place this burst in the short burst category.


GRB_name: GRB120302A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13000
SUBJECT: GRB 120302A found in ground analysis of BAT data
DATE:    12/03/02 17:13:23 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

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

Automated BAT ground analysis found a burst that occurred at 01:55:39 UT 
with a significance of 8.2 sigma (15-200 keV) from the event data.  
The event is temporally coincident with the Fermi GBM 352346136.  The best 
BAT location is RA, Dec = 122.4506, +29.6598 deg, which is

  RA(J2000)  =  08h 09m 48.14s 
  Dec(J2000) = +29d 39' 35.3" 

with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).

Swift ToO has been requested.  


GRB_name: GRB111222A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13001
SUBJECT: GRB 111222A: Swift observation on 2012 February 06/07 
DATE:    12/03/02 18:08:01 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

D. Grupe and M. Siegel (PSU) report on behalf of the Swift team:

Swift re-observed the field of the IPN burst GRB 111222A (Hurley et 
al., GCN circ. 12714) on 2012-02-06/07 for 5.1 ks. We do not 
detect the  X-ray source reported by Grupe (GCN circ. 12716) in a 
2.5 ks observation 27 hours after the burst. The 3-sigma upper 
limit at the position of the afterglow is 1.4e-3 counts/s in the 
Swift XRT. This observation confirms our findings from a 5 ks Swift
observation obtained on 2011-12-31 (Grupe & Siegel, GCN circ.
12805) that the source has faded. We therefore conclude that the 
X-ray source reported by Grupe (GCN circ. 12716) is the afterglow 
of GRB 111222A.

UVOT observations show that the source reported in Grupe & Siegel 
(GCN circ. 12805) has remained at constant white magnitude of 
19.88 since fading by 0.48 magnitudes between the first and 
second Swift/UVOT observations.  Multi-color photometry confirms 
that the source is very red (B-V=1.26), with only upper limits in 
UV passbands).  Its relation to the burst is still unknown.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.

This circular is an official product of the Swift team.


GRB_name: GRB120302A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13002
SUBJECT: GRB 120302A, Swift-BAT refined analysis
DATE:    12/03/02 21:11:23 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

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

Using the event data from T-220 to T+30 sec (T is the trigger time of the 
ground code which is 01:55:30.8 UT), we report further analysis of GRB 120302A  
(Sakamoto, et al., GCN Circ. 13000).  

The mask-weighted light curve created from the event data shows at least 
two peaks, the first starting and also peaking at ~T sec.  The second starts 
at ~T+10 sec, peaks at ~T+13 sec, and ends at ~T+20 sec.  Although there might 
be another weak episode starting at ~T+20 sec, it is hard to say conclusively 
because the event data ends at T+30 sec.  From the BAT raw light curve, the 
duration of the event is 35-40 sec long.  

The spectrum extracted from T to T+30 sec is best fit by a simple 
power-law model.  The power law index of the spectrum is 1.4 +- 0.3 
(90% confidence).  The fluence measured in this interval is 6.6 +- 
1.3 x 10^-7 erg/cm2 (15-150 keV) and 1-sec peak flux measured from 
T sec in the 15-150 keV band is 0.6 +- 0.3 ph/cm2/s.  All the quoted 
erros are at the 90% confidence level.  

Swift ToO has been approved and the observation is on-going.


GRB_name: GRB120302A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13003
SUBJECT: GRB 120302A: GROND detection of an afterglow candidate
DATE:    12/03/05 18:26:32 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

J. Elliott, J. Greiner, F. Olivares E., A. Rau (all MPE Garching),
T. Kruehler (DARK) report on behalf of the GROND team:

We observed the field of GRB 120302A (Sakamoto et al., GCN #13000)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP,
120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla
Observatory (Chile). Observations centered on the BAT position started
on March 3, 2012, at 00:33 UT, 22.6 h after the GRB trigger. They were
performed at an average seeing of 1.4", and average airmass of 2.

A second epoch of GROND observations was taken starting March 4, 2012, at
01:47 UT, only 15 deg from the Moon. The pointing had been slightly shifted 
to the south-west to cover the X-ray source in the Swift ToO observation
also in the optical channels. Our images reveal no source within the formal
4.7" XRT error circle centered at RA (2000.0) = 08 09 35.96, 
Decl. (2000.0) = 29 37 43.8. 

Slightly outside the XRT error circle, we find a source at
RA (2000.0) = 08 09 35.58
Decl. (2000.0) = 29 37 40.7
(+-0.2 arcsec). This source has been constant between our two epochs in JHK. 
In the second epoch, we measure for this object (all in the AB system)

g' = 22.5 +/- 0.3
r' = 21.9 +/- 0.2
i' = 21.9 +/- 0.3
z' = 21.4 +/- 0.1
J  = 20.9 +/- 0.4
H  = 20.3 +/- 0.3
K  = 19.7 +/- 0.4

where the optical bands have been calibrated against SDSS, and the NIR bands
against 2MASS. This object is not visible on SDSS images, suggesting a
transient nature. The above magnitudes, after correcting for the small reddening 
of E(B-V)=0.04 mag (Schlegel et al. 1998), are well fitted with a power law 
of slope 1.4, typical for GRB afterglows. We therefore propose this 
source as the candidate afterglow of GRB 120302A. The constant flux during
our two epochs might be the result of a plateau or re-brightening event.

Note, that there is a nearby SDSS source, SDSS J080935.14+293739.8, which based 
on our astrometry is definitely a different source, though it is not 
detected in our images due to the high background of the nearby Moon. 
A finding chart will be placed at http://www.mpe.mpg.de/~jcg/grb120302A.html.
We note that the colors of SDSS J080935.14+293739.8 are not consistent with
an AGN or star. If SDSS J080935.14+293739.8 is a galaxy, the large r'-i'
color might indicate a redshift of about 0.7-0.8. This could potentially 
be the host galaxy of GRB 120302A.

A deep observation is suggested in a few days time, when the Moon does not 
disturb so much anymore.


GRB_name: GRB120305A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13004
SUBJECT: GRB 120305A: Swift detection of a short burst
DATE:    12/03/05 20:03:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

G. Stratta (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), B. Gendre (ASDC),
C. Guidorzi (U Ferrara), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL),
B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU),
G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/ORAU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 19:37:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120305A (trigger=516997).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 47.546, +28.493 which is 
   RA(J2000)  =  03h 10m 11s
   Dec(J2000) = +28d 29' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 200 msec.  The peak count rate
was ~32000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Using promptly downlinked data we find a bright, fading, uncatalogued
X-ray source with an enhanced position: RA, Dec 47.5368, 28.4915 which
is equivalent to:
   RA(J2000)  = 03h 10m 08.84s
   Dec(J2000) = +28d 29' 29.3"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 29 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.13 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4
(+3.38/-2.63) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.03e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 71 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
0.43. 

We note quasi-periodic variability in the BAT lightcurve before and after the
burst.  We believe it is unrelated to the GRB and could be coming from a
different source, but will further examine the data to determine the origin. 

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


GRB_name: GRB120305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13005
SUBJECT: GRB 120305A: MASTER-NET  early optical observations
DATE:    12/03/05 20:39:03 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
Sternberg Astronomical Institute, Moscow State University

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

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

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

V.Krushinski, I.Zalozhnich,  A. Popov
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 short  GRB120305A 32 sec   after 
notice time and 57 sec after GRB time at 2012-03-05 19:38:26.385 UT  in 
two polarizations. 
On  our first (10s exposure) set we haven't found optical transient 
within  SWIFT error-box (ra=03 10 11 dec=+28 29 21 r=0.050000).
The 5-sigma upper limit has been about 16.0 mag.
The message may be cited.


GRB_name: GRB120305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13006
SUBJECT: GRB 120305A - Liverpool Telescope Observations
DATE:    12/03/05 21:43:15 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F. J. Virgili (Liverpool, JMU), C. Guidorzi (U. Ferrara), A. Melandri 
(INAF-OAB), C.G. Mundell (Liverpool, JMU) report:

"The 2-m Liverpool Telescope robotically followed up GRB 120305A
(SWIFT trigger 516997; Stratta et al., GCN Circ 13004) 14.00 min after 
the GRB trigger time.

No optical counterpart is detected within the XRT error circle to the
following conservative limits:

r' > 21.3 mag (vs USNOB1)
i' > 21.0 mag (vs USNOB1).


GRB_name: GRB120305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13007
SUBJECT: GRB 120305A: Swift-BAT refined analysis
DATE:    12/03/06 00:10:00 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
G. Stratta (ASDC), 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 120305A (trigger #516997)
(Stratta, et al., GCN Circ. 13004).  The BAT ground-calculated position is
RA, Dec = 47.549, 28.495 deg which is 
   RA(J2000)  =  03h 10m 11.8s 
   Dec(J2000) = +28d 29' 41.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
 
The mask-weighted light curve shows a single FRED-like spike starting
at ~T+0.00 sec, peaking at ~T+0.02 sec, and returning to baseline
at ~T+0.20 sec.  At the ~2-sigma level, there is possible emission out to ~T+20 sec.
T90 (15-350 keV) is 0.10 +- 0.02 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.00 to T+0.136 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.00 +- 0.09.  The fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.43 sec in the 15-150 keV band
is 2.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/516997/BA/


GRB_name: GRB120305A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13008
SUBJECT: GRB 120305A: Enhanced Swift-XRT position
DATE:    12/03/06 00:24:59 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 448 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120305A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 47.53639, +28.49191 which is equivalent
to:

RA (J2000): 03h 10m 8.73s
Dec (J2000): +28d 29' 30.9"

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: GRB120305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13009
SUBJECT: GRB 120305A: Swift-XRT refined Analysis
DATE:    12/03/06 08:03:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 8.2 ks of XRT data for GRB 120305A (Stratta  et al.
GCN Circ. 13004), from 69 s to 24.9 ks after the  BAT trigger. The data
comprise 85 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 13008).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.66 (+0.22, -0.19).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+0.21, -0.20). The
best-fitting absorption column is  4.7 (+1.1, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 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 4.5 x 10^-11 (7.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      4.7 (+1.1, -0.9) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 6.4 sigma
Photon index:      1.94 (+0.21, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00516997.

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


GRB_name: GRB120305A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13010
SUBJECT: GRB 120305A: EVLA deep limit on a radio counterpart
DATE:    12/03/06 15:38:02 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

B. A. Zauderer, W. Fong and E. Berger (Harvard) report:

"We observed the location of the short-duration GRB 120305A (GCN 13004)
with the EVLA starting on 2012 March 05.98 UT (3.9 hours post-burst). We
obtained two hours of observations at a mean frequency of 5.8 GHz. We do
not detect any radio source within the latest enhanced XRT position
(improved from GCN 13008 with RA = 03:10:08.76, Dec = +28:29:30.2 (J2000),
1.9" uncertainty; http://www.swift.ac.uk/xrt_positions/00516997/) to a
3-sigma limit of ~18 microJy."


GRB_name: GRB120305A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13011
SUBJECT: GRB 120305A: Swift/UVOT Upper Limits
DATE:    12/03/06 17:55:47 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and G. Stratta (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120305A
72 s after the BAT trigger (Stratta et al., GCN Circ. 13004).
No optical afterglow consistent with the enhanced XRT position
(Beardmore et al., GCN Circular 13008)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial
finding chart (FC) exposures and subsequent exposures are:

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

white (FC)          72          221          147         >20.1
u (FC)             284          534          246         >20.4
white               72         6382          363         >21.1
v                 5158        11729         1082         >19.7
b                  540        18740          428         >20.4
u                  284        24898         1918         >21.2
w1                5567        24288         1968         >20.7
m2               11734        23381         1740         >21.0
w2                6388         6584          193         >20.4

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: GRB120302A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13012
SUBJECT: GRB 120302A: Swift-BAT refined position and a possible XRT and UVOT counterpart
DATE:    12/03/06 18:59:28 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), V. Mangano (INAF-IASF/Palermo),
A. Maselli (INAF-IASF/Palermo), M. H. Siegel (PSU), 
M. J. R. Cummings (GSFC/UMBC), P.A. Evans (U. Leicester), 
F. E. Marshall (NASA/GSFC), K.L. Page (U. Leicester) and 
B. Sbarufatti (INAF-OAB/IASFPA) on behalf of the Swift team:

We report further analysis of BAT ground detected GRB 120302A
(Sakamoto, et al., GCN Circ. 13000).  By carefully examining the BAT image,
we found a position with a higher significance (9.2 sigma in the 14-200 keV image)
than that originally reported (Sakamoto, et al., GCN Circ. 13000).  The best
BAT position is RA, Dec = 122.426, +29.642 deg which is
   RA(J2000)  =  08h 09m 42.2s
   Dec(J2000) = +29d 38' 31.2"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The center of this position differs by 1.6 arcmin from the position reported
on the initial circular (Sakamoto, et al., GCN Circ. 13000).

A 5 ksec Swift ToO observation was performed on 18:17 UT on March 2
(~16.4 hr after the burst).  The XRT observation was performed in PC mode.
Using 666 s of XRT Photon Counting mode data and 1 UVOT image, we find an
astrometrically corrected X-ray position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue; Evans et al. 2009):
RA, Dec = 122.39761, 29.62781 which is equivalent to:
   RA(J2000)  =  08h 09m 35.43s
   Dec(J2000) = +29d 37' 40.1"
with an uncertainty of 3.2 arcsec (radius, 90% confidence).  This XRT
refined position is consistent with an afterglow candidate reported by
GROND (Elliott et al., GCN Circ. 13003).

The X-ray light curve shows a roughly constant count rate at the average
level of 1.2e-2 counts s^-1.  A fit with a power-law model cannot constrain
the slope.  A spectrum formed from the PC mode data can be fitted with an
absorbed power-law with a photon spectral index of 1.29 (+0.68, -0.35).  The best-fitting
absorption column is less than 1.9 x 10^21 cm^-2, in excess of the Galactic value
of 3.77 x 10^20 cm^-2 (Kalberla et al. 2005).  The observed (unabsorbed) 0.3-10 keV
flux is 6.1 (-2.1,+2.2) x 10^-13 (6.1 (-1.7, +2.3) x 10^-13) erg cm^-2 s^-1.
All the quoted erros are at the 90% confidence level.

The Swift/UVOT data were taken entirely in the u filter.  Using the first u 
data (T0+58.9 ksec, 1391 s exposure), we find a candidate optical afterglow at: 
RA, Dec = 122.39810, 29.62807 which is equivalent to:
    RA(J2000)  =  08h 09m 35.54s 
    DEC(J2000) = +29d 37' 41.1"  
with a 90%-confidence error radius of about 0.6".  The source has a u magnitude of
20.25+/-0.14 (1 sigma) on the system of Breeveld et al. 2011, AIP Conf. Proc. 1358, 373.
This position is consistent with the GROND position.  The magnitude is 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).

The 2nd epoch observation of Swift ToO has been approved.  This observation
will be scheduled on March 8.  


GRB_name: GRB120302A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13013
SUBJECT: GRB 120302A: Fermi GBM Observation
DATE:    12/03/07 08:19:13 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 01:55:34.00 UT on March 02 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120302A (trigger 352346136 / 120302080),
which was also found in the ground analysis of the Swift/BAT data
(Sakamoto et al. 2012, GCN 13000). The Swift position is within
the 3 sigma statistical error contour of the GBM on-ground location.

The GBM light curve shows a short peak starting at about T-1.5s,
followed by a plateau of about 20s and a weaker emission tail.
The duration (T90) is of about 70 s (50-300 keV), which is
consistent with the light curve observed by Swift considering
the Swift/BAT data stops at T+30s (Sakamoto et al, GCN 13002).

The time-averaged spectrum from T0-2 s to T0+67 s is
well fit by a simple power law function with index -1.62 +/- 0.06
(Castor stat 453.64 for 367 d.o.f.), which is consistent with the
results reported by Sakamoto et al (GCN 13002).

The event fluence (10-1000 keV) in this time interval is
(3.84 +/- 0.08)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-1.536 s in the 10-1000 keV band
is 1.5 +/- 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: GRB120302A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13014
SUBJECT: GRB 120302A, the review of the sky area in plate archives
DATE:    12/03/07 09:54:22 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120302A (T. Sakamoto et al. GCN Circ.13000) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19810224/200500 GUA040C001870B 60.2 14.5 1125-05523340
19810224/200504 GUA040D001871 60.2 14.5 1125-05523340
19900222/193842 GUA040C001572 16.0 16.3 1125-05523532
19900224/194049 GUA040C001590 16.0 15.0 1125-05523428
19900303/191807 GUA040C001624 16.0 15.0 1125-05523428
19920226/201021 GUA040C001952 18.0 15.0 1125-05523428
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C,  M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D   (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 20 minutes area around 
      the location given in T. Sakamoto et al. GCN Circ.13000: 
      RA(J2000)= 08h 09m 48.14s, Dec(J2000)= +29d 39'35.3"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 25x25 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120302A/index.html


GRB_name: GRB120305A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13015
SUBJECT: GRB 120305A: Swift spectral lag analysis
DATE:    12/03/07 13:15:04 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Norris (BSU), S.D. Barthelmy (GSFC) for the BAT Team:

We report the spectral lag analysis for GRB 120305A (GCN Circ. 13004)
based on the BAT data.  Using 1-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 2.0 +0.6/-0.9 msec, and
-2.6 +0.6/-0.4 msec for the 25-50 keV to 100-350 keV bands
for both peaks combined.  These lag values place this burst
in the short burst category.


GRB_name: GRB120305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13016
SUBJECT: GRB 120305A: D50 optical limits
DATE:    12/03/07 15:37:04 GMT
FROM:    Jan Strobl at AI AS CR,Ondrejov  <jan@strobl.cz>

Jan Strobl (1), Martin Jelinek (2), Cyril Polasek (1), Martin Nekola (1),
Martin Blazek (1), Petr Kubanek (3) and Rene Hudec (1)
(1. ASU AVCR Ondrejov, 2. IAA-CSIC Granada, 3. FZU AVCR)

We observed the field of Swift GRB 120305A (Stratta et al., GCNC 13004) 
with the 0.5m telescope D50 in Ondrejov (Czech Republic), starting at 
19:39:12.6UT i.e. 102.6s after the trigger. A sequence of 20s unfiltered 
images was obtained. We do not detect any new source in individual (limit 
Rc~17.5) nor coadded images (limit Rc~19.2).

This message can be cited.


GRB_name: GRB120308A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13017
SUBJECT: GRB 120308A: Swift detection of a burst
DATE:    12/03/08 06:29:58 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
M. M. Chester (PSU), V. D'Elia (ASDC), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 06:13:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120308A (trigger=517234).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 219.078, +79.703 which is 
   RA(J2000) = 14h 36m 19s
   Dec(J2000) = +79d 42' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a broad peak
structure with a duration of about ~30 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 06:15:11.3 UT, 92.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 219.08492, 79.68629 which
is equivalent to:
   RA(J2000)  = 14h 36m 20.38s
   Dec(J2000) = +79d 41' 10.6"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 60 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.89
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.17e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
157 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The list of sources is typically complete to about 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 

Burst Advocate for this burst is 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: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13018
SUBJECT: GRB 120308A: Liverpool Telescope optical afterglow candidate
DATE:    12/03/08 07:16:52 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

F. Virgili (LJMU), J. Japelj, (U. Ljubljana), C. Guidorzi (U. Ferrara)
on behalf of a larger collaboration report:

"The 2-m Liverpool Telescope robotically followed up GRB 120308A
(SWIFT trigger 517234) 15.5 min after the GRB trigger time.
The automatic "detection mode" procedure detected an uncatalogued
afterglow candidate within the XRT error circle at:

14:36:19.97   +79:41:12.4   (J2000)

with magnitude r' = 17.2 mag (vs USNOB1) 18.6 min after the burst.

Observations and analysis are ongoing.


GRB_name: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13019
SUBJECT: GRB 120308A: confirmation of the optical afterglow
DATE:    12/03/08 08:06:37 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:

The 0.45-m telescope of  ISON-NM observatory robotically followed up the 
field of the Swift GRB 120308A  (Baumgartner  et al.,  GCN 13017 )  on March 
8, 06:16:55, i.e. 3.3 minutes after burst trigger. In the first frame of 30 
s exposure we do not detect the optical afterglow (Virgili et al.,  GCN 
13018 ) up to R~16m.  However in a stacked several first images of 1800 s 
exposure we clearly detect new source in coordinates 14 36 19.95 +79 41 12.3 
which are coincide with coordinates of the optical afterglow (Virgili et 
al.,  GCN 13018 ). The magnitude of the source at (UT) 06:38:10 (middle 
time) is  R~17.30m. All images are unfiltered and calibrated against 
USNO-B1.0 R2 field stars.

All results are preliminary. Observation is continuing. 


GRB_name: GRB120308A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13020
SUBJECT: GRB 120308A: PAIRITEL NIR observations
DATE:    12/03/08 08:46:02 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

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

We observed the field of GRB 120308A (Baumgartner et al., GCN 13017)
with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations
began at 2012-Mar-08 07h14m27s UT, ~1.0 hours after the Swift Trigger,
under moderate airmass (~1.7).  In  mosaics (effective exposure time
of 0.39 hours) taken simultaneously in the J, H, and Ks filters, we
detect the afterglow (Virgili et al., GCN 13018, Elenin et al., GCN
13019) at the Liverpool position (Virgili et al., GCN 13018).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
1.44       0.39     J     17.71  0.21
1.44       0.39     H     16.74  0.22
1.44       0.39     Ks    16.06  0.25

Observations are ongoing. 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: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13021
SUBJECT: GRB 120308A: IAC80 I-band observations
DATE:    12/03/08 09:31:39 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC) and R. Gimeno (IAC), report on behalf of a larger collaboration:

"We observed the field of GRB 120308A (Baumgartner et al., GCNC 13017) with the 82cm IAC80 telescope at the Observatorio del Teide, Tenerife, Spain. The observations were carried in the I-band on March 8.27260--8.28075 UT  (18.91-30.65 minutes post burst) with a total exposure time of 5x120s. A preliminary analysis of the individual and combined images detect clearly the optical/NIR afterglow (Virgili et al. GCN 13018, Elenin et al. GCN 13019, Morgan et al. GCN 13020) with a magnitude of I~16.8 with respect to the USNO B1.0 catalogue."


GRB_name: GRB120308A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13022
SUBJECT: GRB 120308A: Swift-BAT refined analysis
DATE:    12/03/08 13:50:31 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120308A (trigger #517234)
(Baumgartner, et al., GCN Circ. 13017).  The BAT ground-calculated position is
RA, Dec = 219.123, 79.674 deg, which is 
   RA(J2000)  =  14h 36m 29.5s 
   Dec(J2000) = +79d 40' 25.7" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows a mostly smooth peak starting at ~T-30 sec,
peaking at ~T+1 sec, and ending at ~T+70 sec.  T90 (15-350 keV) is
60.6 +- 17.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-24.15 to T+58.20 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.71 +- 0.13.  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+0.62 sec in the 15-150 keV band
is 0.6 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/517234/BA/


GRB_name: GRB120308A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13023
SUBJECT: GRB 120308A: Enhanced Swift-XRT position
DATE:    12/03/08 14:45:03 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 1980 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120308A, 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 = 219.08506, +79.68651 which is equivalent
to:

RA (J2000): 14h 36m 20.41s
Dec (J2000): +79d 41' 11.4"

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: GRB120308A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13024
SUBJECT: GRB 120308A: Swift-XRT refined Analysis
DATE:    12/03/08 18:30:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 12 ks of XRT data for GRB 120308A (Baumgartner  et al.
GCN Circ. 13017), from 82 s to 30.0 ks after the  BAT trigger. The data
comprise 190 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 Evans et
al. (GCN. Circ 13023).

The late-time light curve (from T0+5.8 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.29 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.17 (+0.10, -0.09). The
best-fitting absorption column is  1.90 (+0.16, -0.15) x 10^21 cm^-2,
in excess of the Galactic value of 2.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.61 (+0.09, -0.08)
and a best-fitting absorption column of 4.8 (+2.1, -1.9) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.3 x 10^-11 (4.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+2.1, -1.9) x 10^20 cm^-2
Galactic foreground: 2.9 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.61 (+0.09, -0.08)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00517234.

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


GRB_name: GRB120308A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13025
SUBJECT: GRB 120308A: Swift/UVOT Detection
DATE:    12/03/08 19:32:24 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (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 120308A
158 s after the BAT trigger (Baumgartner et al., GCN Circ. 13017).
A source consistent with the optical position reported by Virgili et al.
(GCN Circ. 13018) is detected in the initial UVOT exposures, but only
in the v and b band. In u there is no evidence for a source, which
suggests that the source is at a redshift of z < 4, and in case there
is no contamination of dust, z ~ 3.2.

The best UVOT position is

   RA(J2000)  = 14h 36m 20.05s
   Dec(J2000) = 79d 41' 12.2"

with an uncertainty of 0.55" (90% confidence).

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

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

v                  463          483           20         17.02 +/- 0.17
b                  413          432           19         17.65 +/- 0.13
u                  158         7690         1020        >20.9
w1                 512        13962         1165        >21.3
m2                 636        13409         1415        >21.3
w2                 438         8103          646        >21.5
b                  711          730           19         18.40 +/- 0.25
v                  761         1082           39         18.14 +/- 0.29

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


GRB_name: GRB120308A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13026
SUBJECT: GRB120308A: MITSuME Ishigakijima Optical Upper Limits
DATE:    12/03/09 07:46:33 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 120308A (Baumgartner et al., GCNC 13017)
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 012-03-08 12:48:40 UT, (~6.6 h after the burst).
We did not find any new point source within the enhanced XRT error
circle (Evans et al., GCNC 13023) in all the three bands.
We could not detect the previously reported afterglow (Virgili et al., GCNC 13018).


Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc    Ic
-----------------------------------------------------
0.30659    13:35:07    2220.0   >19.4  >19.4  >19.0
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120308A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13027
SUBJECT: GRB 120308A: Further PAIRITEL NIR Observations
DATE:    12/03/09 23:18:17 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, and J. S. Bloom (UC Berkeley) report:

We continued to observe the field of GRB 120308A (Baumgartner et al.,
GCN 13017) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona.
The source faded significantly since our first epoch (Morgan et al.,
GCN 13020), suggesting a temporal decay index of approximately 1.0
during our observations.

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
1.55       0.50     J     17.70  0.18
1.55       0.50     H     16.81  0.21
1.55       0.50     Ks    16.00  0.21
5.08       2.09     J     18.92  0.25
5.08       2.09     H     >18.2  3sigUL
5.08       2.09     Ks    >17.3  3sigUL

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


GRB_name: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13028
SUBJECT: GRB 120308A: 1.23m CAHA I-band observations
DATE:    12/03/10 03:25:36 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), P. Kubanek (FZU, Praha), M. Jelinek (IAA-CSIC), report on behalf of a larger collaboration:

"We imaged the field of the Swift GRB 120308A (Baumgartner et al., GCN Circ. 13017)
with the 1.23m Calar Alto telescope. The observations were carried out in the I-band
on March 8.93056--9.18766 UT (16.1--22.3 hours post burst).  No optical source brighter
than I=20.8 was found consistent with the optical afterglow coordinates (Virgili et al.,
GCN Circ. 13018; Kuin et al., GCN Circ. 13025)."


GRB_name: GRB120302A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13029
SUBJECT: GRB 120302A: RTT150 optical observations
DATE:    12/03/10 07:48:26 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

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

report:

The field of GRB 120302A (Sakamoto et al., GCN 13000) was observed
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK
National Observatory, Turkey) on March 02, 2012, during UT
19:20--20:05, approximately 18 hours after the burst. A serie of 7
exposures by 300 sec each in Rc filter was obtained at moderate
weather conditions and seeing of 1.7 arcsec.

We clearly detected optical source at the position of XRT, UVOT and
GROND OT candidate (Elliott et al., GCN 13003, Sakamoto et al., GCN
13012). In our combined image we estimated brightness of OT as Rc =
21.14+/-0.08, calibrated against USBO-B1.0 star (R2=17.31 mag) at
R.A. (2000.0) = 08:09:36.74, Dec. (2000.0) = +29:37:54.9

We also made a serie of 300 sec exposures on March 08, 2012, UT (mean)
= 21:05. OT is not seen at the limit of combined image of R ~ 22.4


GRB_name: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13030
SUBJECT: GRB 120308A: RTT150 optical observations
DATE:    12/03/10 08:39:23 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

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

report:

The field of GRB 120308A (Baumgartner et al., GCN 13017) was observed
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK
National Observatory, Turkey) on March 08, 2012, UT(mean)= 22:35,
approximately 16 hours after the burst. A serie of exposures by 300
sec each in Rc filter was obtained at moderate weather conditions.

We marginaly detected optical source at the position of OT (Virgili et
al., GCN 13018) and estimated its Rc ~ 22.5 mag in our combined image.


GRB_name: GRB120308A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13031
SUBJECT: GRB 120308A : LOAO optical observation
DATE:    12/03/10 15:26:15 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

Jang, M., Im, M. (SNU), & Urata, Y. (NCU)

We observed GRB 120308A (Baumgartner et al., GCN 13017)
in R, I-bands with a 1 m telescope at Mt. Lemmon, Arizona, U.S.
The obsevation started at 10:51:23 2012-03-08 UT, ~ 4.6 hours
after the burst alert.

We alternatively took 6 frames for each filter with the exposure time, 300s.
We found a optical afterglow candidate in the stacked I image
with a preliminary magnitude, I ~ 18.7 +/- 0.12 mag
at mid-point time, 17274 sec after the burst alert
on the enhanced XRT position (Evans et al., GCN13023).
However, no afterglow candidate was found in the stacked R image.

We thank the LOAO operator, J. Yoon for this observation. 


GRB_name: GRB120311A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13032
SUBJECT: GRB 120311A: Swift detection of a burst
DATE:    12/03/11 05:42:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. B. Markwardt (NASA/GSFC), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), M. H. Siegel (PSU) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team:

At 05:33:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120311A (trigger=517469).  Swift did not slew because of 
the Earth limb observing constraint. 
The BAT on-board calculated location is 
RA, Dec 273.087, +14.275, which is 
   RA(J2000)  =  18h 12m 21s
   Dec(J2000) = +14d 16' 32"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
structure with a duration of about 6 sec.  The peak count rate
was ~5100 counts/sec (15-350 keV), at ~0 sec after the trigger. 

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

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


GRB_name: GRB120311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13033
SUBJECT: GRB 120311A: Liverpool Telescope optical candidate
DATE:    12/03/11 06:49:39 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), C. Guidorzi (U. Ferrara), F. Virgili (LJMU),  
on behalf of a larger collaboration report:

"The 2-m Liverpool Telescope robotically followed up GRB 120311A  
(SWIFT trigger 517469, Markwardt et al., GCN 13032) 14.4 min after the  
GRB trigger time. The automatic "detection mode" procedure detected an  
uncatalogued afterglow candidate close to the XRT error circle (7  
arcsec from its centroid) at:

18:12:22.166   +14:17:46.3   (J2000)

with magnitude R = 19.1 mag (vs USNOB1) 16 min after the burst.

Observations and analysis are ongoing.


GRB_name: GRB120311A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13034
SUBJECT: GRB 120311A: Swift-XRT observations
DATE:    12/03/11 07:29:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

The XRT began observing the field of GRB 120311A at 06:26:19.9 UT,
3161.6 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 273.08966,
14.29709 which is equivalent to:
   RA(J2000)  = 18h 12m 21.52s
   Dec(J2000) = +14d 17' 49.5"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 80 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 (1.03 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.5
(+2.12/-1.86) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB120311A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13035
SUBJECT: GRB 120311A: Enhanced Swift-XRT position
DATE:    12/03/11 12:15:15 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 762 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120311A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 273.09198, +14.29643 which is equivalent
to:

RA (J2000): 18h 12m 22.08s
Dec (J2000): +14d 17' 47.2"

with an uncertainty of 2.6 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB120311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13036
SUBJECT: GRB 120311A: CAHA 1.23m I-band early observations
DATE:    12/03/11 13:58:08 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

P. Kubanek, M. Jelinek, J. Gorosabel (IAA-CSIC), report on behalf of a larger collaboration:

"The 1.23m CAHA telescope responded automatically to GRB 120311A (trigger=517469, Markwardt et al. GCN 13032) starting optical observations on March 11.23381 UT (~3.05 minutes after the trigger). The optical afterglow (Melandri et al. GCNC 13033) is clearly detected in two I-band frames taken before dawn at I ~ 17.3." 


GRB_name: GRB120311A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13037
SUBJECT: GRB 120311A: Swift/UVOT Upper Limits
DATE:    12/03/11 15:16:25 GMT
FROM:    Patricia Schady at MPE/Swift  <msslba@googlemail.com>

S. R. Oates (MSSL-UCL) and C. B. Markwardt (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120311A
3164 s after the BAT trigger (Markwardt et al., GCN Circ. 13032).
No optical afterglow, consistent with the refined XRT position
(Goad et al .,GCN Circ 13035) or optical position reported by the
Liverpool Telescope (Melandri et al., GCN Circ 13033), is detected within
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          3164         3314          147         >16.4
white             3164        16486         2114         >16.5
v                 3321        20754         1454         >15.8
b                 4141        15574         1224         >16.4
u                 3936         5571          393         >16.3
w1                3731         5366          393         >17.7
m2                3526         5161          393         >19.0
w2                4552        17272         1850         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.13 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120311B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13038
SUBJECT: GRB 120311B: Swift detection of a burst
DATE:    12/03/11 15:17:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
P. D'Avanzo (INAF-OAB), C. Guidorzi (U Ferrara),
A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 15:08:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120311B (trigger=517489).  Swift did not slew immediately
because of the Earth limb observing constraint. 
The BAT on-board calculated location is 
RA, Dec 258.501, -13.060 which is 
   RA(J2000)  =  17h 14m 00s
   Dec(J2000) = -13d 03' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peaks
structure with a duration of about 20 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~10 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+49.0
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB120311A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13039
SUBJECT: GRB 120311A, Swift-BAT refined analysis
DATE:    12/03/11 16:07:19 GMT
FROM:    Craig Markwardt at NASA/GSFC  <craigm@milkyway.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)
(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 120311A (trigger #517469)
(Markwardt, et al., GCN Circ. 13032).  The BAT ground-calculated position is
RA, Dec = 273.075, 14.297 deg which is
    RA(J2000)  =  18h 12m 18.1s
    Dec(J2000) = +14d 17' 49.0" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.

The mask-weighted light curve shows a single gradual-rise exponential-decay
peak.  T90 (15-350 keV) is 3.5 +- 0.8 sec (estimated error including systematics).

The time-averaged spectrum from T-1.38 to T+3.22 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.30 +- 0.15.  The fluence in the 15-150 keV band is 3.0 +- 0.3 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.07 sec in the 15-150 keV band
is 3.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/517469/BA/


GRB_name: GRB120311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13040
SUBJECT: GRB 120311B: Swift-XRT observations
DATE:    12/03/11 17:07:00 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne (U. Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU), G.
Tagliaferri (INAF-OAB), S. Campana (INAF-OAB) and P.A. Evans (U.
Leicester) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 120311B at 15:59:18.5 UT,
3067.7 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 258.56101,
-13.05235 which is equivalent to:
   RA(J2000)  = 17h 14m 14.64s
   Dec(J2000) = -13d 03' 08.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 212 arcseconds from the BAT onboard position. This position
may be improved as more data are received; the latest position is
available at http://www.swift.ac.uk/sper. This position is more than
2-sigma away from the BAT position, and so possibly unrelated to the
trigger. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.64
x 10^21 cm^-2 (Kalberla et al. 2005). 


GRB_name: GRB120311B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13041
SUBJECT: GRB 120311B: Swift-BAT refined analysis
DATE:    12/03/11 21:31:25 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+258 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120311B (trigger #517489)
(Marshall, et al., GCN Circ. 13038).  The BAT ground-calculated position is
RA, Dec = 258.551, -13.068 deg, which is 
   RA(J2000)  =  17h 14m 12.2s 
   Dec(J2000) = -13d 04' 05.0" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 62%.
 
The mask-weighted light curve shows two nearly separated peaks, the first
starting at ~T-15 sec, peaking at ~T_0,  and the minimum between the two
peaks is at ~T+5 sec. The second peak peaks at ~T+10 sec, and
returns to baseline at ~T+22 sec.  T90 (15-350 keV) is 28.2 +- 5.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-13.88 to T+21.63 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.96 +- 0.14.  The fluence in the 15-150 keV band is 1.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+9.04 sec in the 15-150 keV band
is 1.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/517489/BA/


GRB_name: GRB120311B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13042
SUBJECT: GRB 120311B: Enhanced Swift-XRT position
DATE:    12/03/11 21:54:08 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 4834 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 120311B, 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 = 258.56208, -13.05144 which is equivalent
to:

RA (J2000): 17h 14m 14.90s
Dec (J2000): -13d 03' 05.2"

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: GRB120311A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13043
SUBJECT: GRB 120311A: Swift-XRT refined Analysis
DATE:    12/03/11 22:58:04 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF/OAB), P. D'Avanzo (INAF/OAB) and C. B. Markwardt
(NASA/GSFC) report on behalf of the Swift-XRT team:

We have analysed 15 ks of XRT data for GRB 120311A (Markwardt  et al.
GCN Circ. 13032), from 3.2 ks to 34.5 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN. Circ 13035). 

The late-time light curve (from T0+3.2 ks) can be modelled with a
single power-law decay with a decay index of alpha=1.09 (+0.13,-0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.03 (+0.27, -0.25). The
best-fitting absorption column is  2.6 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.0 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (6.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.6 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 1.0 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.03 (+0.27, -0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00517469.

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


GRB_name: GRB120311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13044
SUBJECT: GRB 120311B: Swift-XRT refined Analysis
DATE:    12/03/12 08:11:59 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB) and F. E. Marshall (NASA/GSFC) report on behalf
of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 120311B (Marshall  et al.
GCN Circ. 13038), from 3.1 ks to 22.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN. Circ 13042).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.69 (+/-0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.22, -0.21). The
best-fitting absorption column is  3.6 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.2 x 10^-11 (7.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.6 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: 3.9 sigma
Photon index:      2.01 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00517489.

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


GRB_name: GRB120311B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13045
SUBJECT: GRB 120311B: Faulkes Telescope North observations
DATE:    12/03/12 08:58:55 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB), F. Virgili (LJMU),
J. Japeli (U. Ljubljana)  on behalf of a larger collaboration report:

"The 2-m Faulkes Telescope North robotically followed up GRB 120311B
(Swift trigger 517489, Marshall et al., GCN Circ 13038) 200 sec after
the GRB trigger time. Within the enhanced XRT error circle (Osborne et
al., GCN Circ. 13042) we do not detect any object in R and i' filters
down to the following limits:

Mid time from       Exposure        Filter       Magnitude
GRB (hr)            (s)
----------------------------------------------------------
0.29                240             R > 20.5
0.39                220             i' > 20.3
----------------------------------------------------------

Values are calibrated against nearby USNOB-1 field stars.


GRB_name: GRB120311B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13046
SUBJECT: GRB 120311B: MITSuME Okayama Optical upper limits
DATE:    12/03/12 09:14:49 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 120311B (Marshall et al., GCNC 13038)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-03-11 16:48:04 UT (~1.7 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 13042) in all the three bands.


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

T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.09146    17:19:52    4380.0   >18.7  >18.8  >18.3
0.15451    18:50:40    4740.0   >19.6  >19.6  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120311B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13047
SUBJECT: GRB 120311B: Swift/UVOT Upper Limits
DATE:    12/03/12 12:15:09 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120311B
3072 s after the BAT trigger (Marshall et al., GCN Circ. 13038).
No optical afterglow consistent with the XRT position (Osborne et al., 
GCN Circ. 13042) 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          3072         3222          147         >21.4
white             3072        16503         2114         >22.8
v                 3228        21300         2013         >20.3
b                 4048        15591         1233         >20.7
u                 3843         5479          393         >19.7
w1                3638        22969         1136         >20.9
m2                3433        22206         1082         >20.8
w2                4460        17192         1754         >21.9

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.52 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB120311A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13048
SUBJECT: GROND observations of GRB 120311A
DATE:    12/03/12 15:19:16 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120311A (Markwardt et al., GCN #13032) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP, 120, 405) 
mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile). 
Observations centered on the BAT position started on March 11, 2012, at 
08:02 UT, 2.5h after the GRB trigger. They were performed at an average 
seeing of 1.0", and average airmass of 1.8.

Based on a 20 minute exposure centered at 09:09 UT, the afterglow candidate 
reported by Melandri et al. (GCN 13033) is measured as follows (all in the AB 
system and calibrated against GROND zeropoints (g'r'i'z') and 2MASS (JHK)):
g' = 22.9 +/- 0.3 
r' = 22.5 +/- 0.1 
i' = 22.4 +/- 0.1 
z' = 22.0 +/- 0.1 
J  > 20.5 
H  > 19.6 
K  > 18.0
These above magnitudes have not been corrected for the Galactic extinction of 
E(B-V) = 0.13 towards the direction of the burst (Schlegel et al. 1998).

These magnitudes imply a fading of more than two magnitudes relative to the 
observations reported by Melandri et al. (GCN 13033), and thus confirm
the afterglow nature of this object.


GRB_name: GRB120312A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13049
SUBJECT: GRB 120312A: Swift detection of a burst
DATE:    12/03/12 16:33:53 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. Stamatikos (OSU/NASA/GSFC), S. Campana (INAF-OAB),
M. M. Chester (PSU), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
S. T. Holland (STScI), J. A. Kennea (PSU), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), J. P. Osborne (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), M. C. Stroh (PSU), C. A. Swenson (PSU),
G. Tagliaferri (INAF-OAB) and B.-B. Zhang (PSU) report on behalf of
the Swift Team:

At 16:06:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120312A (trigger=517566).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 251.764, +23.857 which is 
   RA(J2000) = 16h 47m 03s
   Dec(J2000) = +23d 51' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked FRED
structure with a duration of 12 about sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Using promptly downlinked data we find an uncatalogued X-ray source
with an enhanced position: RA, Dec 251.7885, 23.8586 which is
equivalent to:
   RA(J2000)  = 16h 47m 09.23s
   Dec(J2000) = +23d 51' 30.8"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
position may be improved as more data are received; the latest position
is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.08 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.7
(+1.51/-1.34) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 112 s 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 M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120311B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13050
SUBJECT: GRB 120311B: C88 optical limits
DATE:    12/03/12 18:32:49 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

Simone Leonini and Paolo Rosi (Montarrenti Observatory, Siena, Italy) report:

We observed the field of GRB 120311B (Swift trigger 517489, Marshall et al.,
GCN Circ 13038) with 0.53m RC telescope + U47 detector at Montarrenti Observatory
(Siena, Italy, IAU code C88).

The first session of observations was started at 2012-03-12 03:59:24 UT
and stopped at 2012-03-12 04:00:07 UT.  The second session started at 04:11:47 UT
and stopped at 04.12.26 UT (~13 hours after the trigger).

Four unfiltered images of 40s exposure was obtained.  We do not detect
any new point source in the coadded images (limit R~18.9, USNO-B1 catalogue)
within the enhanced XRT error circle (Osborne et al., GCN Circ. 13042).
Target was very low on the horizon.

[GCN OPS NOTE(12mar12): Distribution was delayed by ~3 hrs until an account
could be created.]


GRB_name: GRB120311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13051
SUBJECT: GRB 120311A: VLT/X-shooter observations
DATE:    12/03/12 19:24:15 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paolo D'Avanzo (INAF/OAB), Bo Milvang-Jensen (DARK/NBI), Paul
Vreeswijk (U. Iceland), Nial Tanvir (U. Leicester), Daniele Malesani
(DARK/NBI), Paolo Goldoni (APC/U. Paris 7 and SAp/CEA), Lex Kaper
(U. Amsterdam), Stefano Covino (INAF/OAB) and Johan Fynbo (DARK/NBI)
report on behalf of a larger collaboration:

The optical afterglow (Melandri et al., GCN 13033) of the Swift GRB
120311A (Markwardt et al., GCN 13032; Evans et al., GCN 13034) was
observed spectroscopically with VLT/X-shooter, starting on 2012 March
11.384 UT (3.65 hours after the GRB trigger). An exposure of 2400
seconds was secured, which ran well into morning twilight. The
approximate X-shooter wavelength range is 0.3-2.5 micron. The seeing
during the observations was about 0.8" in the optical, and the
spectrum has a resulting resolving power of 5000 in the ultraviolet
and near-infrared arms, and around 9000 in the optical.

The reduced spectrum shows a very weak continuum in all three
arms. The very low signal-to-noise ratio prevents us from identifying
any significant absorption or emission lines.  From the detection of
continuum flux down to roughly 3700 Angstrom we set an upper limit to 
the GRB 120311A redshift of approximately z < 3.

Using acquisition images preceding the spectrum, with a mid-exposure
time of March 11.373 UT (3.40 hours after the GRB), we measure R =
21.57 +- 0.05 for the afterglow, assuming R=18.30 for the USNO-B1.0
star 1042-0333539 at RA = 18:12:21.82, Dec = +14:17:24.6.

We are grateful for the support of the ESO staff at Paranal, in
particular that of Gabriel Brammer and Stan Stefl.


GRB_name: GRB120312A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13052
SUBJECT: GRB 120312A: Swift-BAT refined analysis
DATE:    12/03/12 22:24:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+736 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120312A (trigger #517566)
(Stamatikos, et al., GCN Circ. 13049).  The BAT ground-calculated position is
RA, Dec = 251.812, 23.881 deg, which is 
   RA(J2000)  =  16h 47m 14.8s 
   Dec(J2000) = +23d 52' 50.3" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve shows a single slightly symmetric peak
starting at ~T-10 sec, peaking at ~T+0.5 sec, and ending at ~T+35 sec.
T90 (15-350 keV) is 14.2 +- 3.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.42 to T+15.87 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.72 +- 0.23.  The fluence in the 15-150 keV band is 5.7 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.95 sec in the 15-150 keV band
is 1.3 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/517566/BA/


GRB_name: GRB120312A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13053
SUBJECT: GRB 120312A: Swift-XRT refined Analysis
DATE:    12/03/13 04:34:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

V. Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), 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) and M. Stamatikos report on behalf of the
Swift-XRT team:

We have analysed 9.9 ks of XRT data for GRB 120312A (Stamatikos  et al.
GCN Circ. 13049), from 112 s to 19.6 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 2188 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 = 251.78816, +23.85817 which is equivalent to:

RA (J2000): 16h 47m 09.16s
Dec(J2000): +23d 51' 29.4"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.28 (+0.14, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.54 (+0.26, -0.25). The
best-fitting absorption column is  1.4 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 4.1 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 4.9 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.4 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index:      1.54 (+0.26, -0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00517566.

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


GRB_name: GRB120312A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13054
SUBJECT: GRB 120312A: NOT observations
DATE:    12/03/13 04:42:24 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paul Vreeswijk (U. Iceland), Dong Xu (WIS), John Telting, Gintaras
Barisevicius (NOT), Daniele Malesani (DARK/NBI), Pll Jakobsson
(U. Iceland) report on behalf of a larger collaboration:

Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained
r'- (3 x 300 s) and z'-band (6 x 300 s) imaging of the field of the Swift
GRB 120312A (Stamatikos et al., GCN 13049; Barthelmy et al., GCN
12052), starting on 2012 March 13.085 UT (9.93 hr after the GRB). The
seeing during the observations was around 1".

We do not detect any object within the enhanced Swift-XRT error circle
(Mangano et al., GCN 13053) down to approximate limiting magnitudes of
r'>23.5 and z'>22.2 (calibrated against the SDSS catalog).


GRB_name: GRB120312A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13055
SUBJECT: GRB 120312A: WHT candidate afterglow
DATE:    12/03/13 07:36:16 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), O. Hartoog (U. Amsterdam), and
T. Schrabback (U. Bonn) report on behalf of a larger collaboration:

We imaged the field of GRB120312A (Stamatikos et al. GCN13049) using the
WHT/ACAM beginning 05:15 UT on March 13th (approximately 13 hours post-burst).
A 24 minute integration was obtained in the z-band.
 
Within the refined XRT error circle (Mangano et al. GCN13053) we find a source
at position:

RA(2000) = 16 47 09.23
dec(2000)= +23 51 28.9

The source may be slightly extended, although the S/N is too poor to
determine this with confidence.  Its provisional magnitude is
z~23.8 +/- 0.2 calibrated against nearby SDSS DR8 stars.


GRB_name: GRB120312A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13056
SUBJECT: GRB 120312A: MASTER-NET optical observations
DATE:    12/03/13 08:29:29 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

V.Krushinski, I.Zalozhnich,  A. Popov
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 Tunka was pointed to the  GRB120312A 403 s after notice 
time and  512 s after GRB time at 2012-03-12 16:15:01 UT in two 
polarizations. On our  first (180s exposure) set we haven't found optical 
transient  within SWIFT  error-box.
The 5-sigma upper limit has been about 17.6 mag
The object  has been observed in high zenit distance (~80 deg).
The big time delay (in pointing) is caused by a non-standard format of the 
socket messages.
The message may be cited.


GRB_name: GRB120312A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13057
SUBJECT: GRB 120312A: Swift/UVOT Upper Limits
DATE:    12/03/13 11:11:56 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120312A
105 s after the BAT trigger (Stamatikos et al., GCN Circ. 13049).
No optical afterglow consistent with the XRT position 
(Mangano et al., GCN Circ 13053) or the WHT optical candidate 
position (Tanvir et al., GCN Circ 13055) 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           105          255          147         >21.3
u_FC               318          567          246         >20.6
white              105         7764          861         >21.9
v                  647        18848         1378         >20.5
b                  573         7559          568         >20.9
u                  318        13854         1583         >21.3
w1                 696        13039         1434         >21.0
m2                 844        19630         1998         >21.4
w2                 795        17934         1434         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.071 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13058
SUBJECT: GRB 120311A: C88 optical limits
DATE:    12/03/13 12:45:03 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

Simone Leonini and Paolo Rosi (Montarrenti Observatory, Siena, Italy)
report:

We observed the field of GRB 120311A (Swift trigger 517469, Markwardt et al.,
GCN 13032) with 0.53m RC telescope + U47 detector at Montarrenti Observatory
(Siena, Italy, IAU code C88).

The observations were performed in four sessions (~22 hours after the
trigger):

from 2012-03-12 03:22:33 UT to 2012-03-12 03:23:15 UT
from 2012-03-12 04:16:03 UT to 2012-03-12 04:16:46 UT   
from 2012-03-12 04:18:09 UT to 2012-03-12 04:18:52 UT   
from 2012-03-12 04:20:16 UT to 2012-03-12 04:20:59 UT

Eight unfiltered images of 40s exposure were obtained.
We do not detect any new point source in the coadded images (limit R~19.1,
USNO-B1 catalogue) within the refined XRT error circle (Goad et al.,GCN Circ
13035) or in the afterglow candidate position reported by Melandri et al.
(GCN Circ 13033).  Observations were made on the twilight.


GRB_name: GRB120311B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13059
SUBJECT: GRB 120311B: Optical follow-up
DATE:    12/03/13 13:54:28 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Kumar Bhatt, S.B. Pandey (ARIES, Nainital, India, 
on behalf of larger Indian GRB collaboration).

GRB 120311B field (Marshall et al., GCN Circ 13038) was observed 
with the newly installed 1.3m Devasthal Fast Optical Telescope at 
Nainital. Several images in R_c pass-band (300 sec each) were taken 
in two sessions starting at UT 21:11:10, 11-03-2012.

In the initial co-added R_c frame (3x300sec), we did not detect any 
new optical source within the XRT error-box (Osborne et al., 
GCN Circ. 13042) down to a limiting magnitude of ~ 20.5 mag. 
The photometry was done in comparison to nearby USNO- B1 stars.

This massage may be cited.


GRB_name: GRB120311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13060
SUBJECT: GRB 120311A: Optical follow-up
DATE:    12/03/13 14:09:33 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Vijay Kumar Bhatt, Brajesh Kumar and S.B. Pandey (ARIES,
Nainital, India, on behalf of larger Indian GRB collaboration)

We imaged the field of GRB120311A (Swift trigger 517469, Markwardt 
et al., GCN 13032) using 1.04m and 1.3m telescopes at ARIES Nainital 
starting ~16 hours after the burst. Several sets of 300s exposures 
were taken in R_c and I_c pass-bands.

We do not detect the optical afterglow candidate (Melandri et al., 
GCN 13033) in our stacked images to following limits. The photometry 
was performed in comparison to nearby USNO-B1 stars.


Filter   Exposure     Limiting mag
----------------------------------
R_c      5x300s       20.0 mag

I_c      5x300s       19.5 mag
----------------------------------

This massage could be cited.


GRB_name: GRB120311A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13063
SUBJECT: GRB 120311A, the review of the sky area in plate archives
DATE:    12/03/13 20:44:54 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120311A (M.R. Goad et al. GCN Circ.13035) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19840817/191914 GUA040C002619 40.1 14.50 0975-10768885
19840817/191917 GUA040D002620 40.1 14.50 0975-10768885
19860613/221841 GUA040C002948 41.7 16.20 0975-10753116
19860613/221846 GUA040D002949 41.7 15.95 0975-10751623
19870630/215915 GUA040C003102 50.5 16.20 0975-10753116
19900627/221058 GUA040C001669 19.0 16.20 0975-10753116
19900628/215100 GUA040C001976 18.0 16.20 0975-10753116
19910619/224921 GUA040C001815 18.0 14.75 0975-10758776
19910704/210331 GUA040C001818A 25.0 15.95 0975-10751623
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 25 minutes area around 
       the location given in M.R. Goad et al. GCN Circ.13035: 
       RA(J2000)= 18h 12m 22.08s, Dec(J2000)= +14d 17' 47.2"
Star USNOA2 - Comparison star.
  The preview images of 9 areas together with  
the 25x25 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120311A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120312A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13064
SUBJECT: GRB 120312A: Gemini and UKIRT imaging
DATE:    12/03/13 22:57:53 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), D. Perley (Caltech), K. Wiersema (U. Leicester),
A. Cucchiara (UCSC/UCO Lick), K. Roth (Gemini) and J. Ehle (JACH)
report on behalf of a larger collaboration:

We observed the location of GRB 120312A with Gemini-N/GMOS
in the z-band and UKIRT/WFCAM in the J- and K-bands.  All observations
were obtained approximately 23 hours post-burst.

With GMOS we detect the source reported by Tanvir et al. (GCN 13055).
Calibrating against SDSS field stars we find a magnitude z=24.35 +- 0.12,
indicating a fading compared to the WHT epoch, and confirming this
source as the afterglow of the GRB.

From a provisional reduction of the UKIRT data, the afterglow is undetected
to 3-sigma limits of J=21.1 and K=19.5 (calibrated against 2MASS), showing
that it is not extremely red, as might have been expected if its faintness
were due to a very dusty line of sight.


GRB_name: GRB120312A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13065
SUBJECT: GRB 120312A: CrAO optical upper limit
DATE:    12/03/14 21:35:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 120312A (Stamatikos  et al., GCN 13049) with 
AZT-11  telescope of CrAO observatory starting on March 12  (UT) 23:21:13 
under moderate weather conditions and  seeing  of about 2.4 arsces.  Within 
enhanced Swift-XRT position (Mangano et al., GCN 13053) we do not detected 
any optical source, in particular afterglow candidate (Tanvir et al., GCN 
13055). A photometry is based on the  USNO-B1.0 star 1138-0244157 
(16:47:09.53 +23:51:17.4)  assuming R=17.3:

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

23:21:13  0.3291       R     26x180    n/d     20.75 


GRB_name: GRB120312A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13066
SUBJECT: GRB 120312A, the review of the sky area in plate archives 
DATE:    12/03/15 16:45:55 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120312A (V. Mangano et al. GCN Circ.13053) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19810626/221142 GUA040C001973B 34.0 15.00 1125-07810808
19810626/221142 GUA040D001974 34.0 15.00 1125-07810808
19870424/003510 GUA040C001043A 18.0 16.10 1125-07808472
19870424/010141 GUA040C001044 16.0 15.00 1125-07810808
19890601/214206 GUA040C001474 18.0 16.65 1125-07808939
19900621/205220 GUA040C001663A 16.5 15.00 1125-07810808
19910615/211004 GUA040C001806A 22.5 16.10 1125-07808472
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 24 minutes area around 
       the location given in V. Mangano et al. GCN Circ.13053: 
       RA(J2000)= 16h 47m 09.16s, Dec(J2000)= +23d 51' 29.4"
Star USNOA2 - Comparison star.
  The preview images of 7 areas together with  
the 24x24 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120312A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120302A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13067
SUBJECT: GRB 120302A: Swift XRT refined analysis
DATE:    12/03/16 12:08:34 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano, A. Maselli (INAF-IASFPA), and T. Sakamoto (GSFC/UMBC)
report on behalf of the Swift-XRT team:

Swift performed two additional ToO observations of the field of GRB 120302A
on 2012 March 8 (4.3 ks starting at 05:39:10 UT) and on 2012 March 13
(7.4 ks starting at 06:10:37 UT). In both observations the previously 
detected
XRT source (Sakamoto, et al., GCN Circ. 13012) is still visible and is 
detected
with marginal significance of about 2.5 sigma. The 0.3-10 keV XRT 
lightcurve
shows a decay trend, and a fit with a power-law model gives a decay 
slope of
0.76 +/- 0.13.
The source is a possible X-ray afterglow candidate for GRB 120302A.

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


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13069
SUBJECT: GRB 111228A: possible detection of the SN with the TNG
DATE:    12/03/16 13:03:08 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), E. Palazzi (INAF-IASF Bo), S. Campana
(INAF-OAB), M. Della Valle (INAF-OAC), E. Pian (INAF-OATs), R. Salvaterra
(INAF-IASF Mi), G. Tagliaferri (INAF-OAB) report on behalf of the CIBO
collaboration:

We observed the optical counterpart of GRB 111228A (Ukwatta et al., GCN
12737) with the Italian 3.6m TNG telescope on 2012 Feb 1.16 UT (34.5 days
post burst) and March 13.91 UT (76.2 days post burst). Observations were
carried out in the R and I bands. The counterpart is well detected in the
two epochs in both filters, with a magnitude R = 24.3 in the March
observation (calibrated using Landolt standard stars). The late value is
likely dominated by the host galaxy.

Differential photometry reveals that the source faded between the two
epochs by 0.4 +/- 0.2 and 0.9 +/- 0.1 mag in the R and I band,
respectively. The observed fading indicates that a transient component was
present during our February observation. This could be due to residual
afterglow emission, or to the presence of an emerging supernova (SN).

After subtracting the host galaxy flux, the color of the transient on
February 1 is very red, with
R-I ~ 2. This color is not typical of GRB afterglows, and is much redder
than measured at early times for this object (e.g.,  r'-i' = 0.17 AB at t
= 0.57 days: Nicuesa Guelbenzu et al., GCN 12757). Such a red spectrum, on
the contrary, is consistent with that of a type-Ic SN at z=0.72 (e.g.,
Dittman et al., GCN 12759), since the observed R band corresponds to the
rest-frame U, where severe line blanketing suppresses the SN flux.  Also,
the I-band magnitude of the transient is comparable to that of SN 1998bw
close to the peak of luminosity, placed at z=0.72.

Although a more accurate analysis of the afterglow behaviour is necessary,
based on the above arguments, we believe to have detected the emission
from the SN associated with GRB 111228A.


We acknowledge the TNG staff for their support, in particular Luca Di
Fabrizio and Daniele Carosati.


GRB_name: GRB120316A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13070
SUBJECT: GBM trigger 353549464 (GRB 120316A?) : High-energy photon emission in Fermi/LAT data
DATE:    12/03/19 23:56:20 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

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

 

High-energy photon emission in Fermi/LAT data was found to be correlated

with GBM trigger 353549464 (00:11:02 UT on Mar. 16, 2012, probably GRB

120316A) as a follow-up of a routine search in GBM trigger catalogs using

our LAT data processing pipeline. The GBM trigger location (RA = 47.93,

Dec = -63.09) was about 17 degree from the LAT boresight, and the zenith

angle was about 54 degrees. A maximum likelihood analysis gives a TS value

of 32.9 over a time window extending to 160s after the trigger. In that time

span, more than 10 photons above 100 MeV were detected, with the highest

energy of ~1.98 GeV at 27s after the burst. The GRB location estimated by

the likelihood analysis is RA = 57.70, Dec = -56.51 with uncertainty ~0.5

degree. This is ~8 degrees away from the GBM trigger location. Our location

is consistent with the preliminary IPN error box (GCN in preparation, Hurley
& Pal'shin)

 

The photon information can be found in the following link, including the
skymap

and light curve figures:

http://www.rotse.net/LAT/GBMTriggers/353549464/353549464_res.html


GRB_name: GRB120320A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13071
SUBJECT: GRB 120320A: Swift detection of a burst
DATE:    12/03/20 12:12:39 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

C. B. Markwardt (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
S. Campana (INAF-OAB), M. M. Chester (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), B.P. Gompertz (U Leicester),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
J. L. Racusin (NASA/GSFC), P. Romano (INAF-IASFPA),
T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
C. A. Swenson (PSU) and E. Troja (NASA/GSFC/ORAU) report on behalf of
the Swift Team:

At 11:56:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120320A (trigger=518200).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 212.538, +8.685 which is 
   RA(J2000) = 14h 10m 09s
   Dec(J2000) = +08d 41' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed what appears to be
a series of peaks with a total duration of about 40 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:59:07.3 UT, 171.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 212.5177, 8.6969 which
is equivalent to:
   RA(J2000)  = 14h 10m 04.25s
   Dec(J2000) = +08d 41' 49.0"
with an uncertainty of 2.8 arcseconds (radius, 90% containment). This
location is 83 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.02
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 174 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 84% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 

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


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13072
SUBJECT: GRB 120320A: MASTER optical observations 
DATE:    12/03/20 13:09:04 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


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

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


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

V.Krushinski, I.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  GRB120320A (Markwardt et 
al., GCN 13071) 32 sec s after notice time and 156 sec after GRB time
at 2012-03-20 11:58:51.633 UT. On our first (30s exposure) set we haven't
found optical transient  within SWIFT BAT error-box (Markwardt et al., GCN 13071).
The 5-sigma upper limit has been about 15.4 mag .
The low limit is due to high zenit distance (8 degrees up to horizont).

The message may be cited.


GRB_name: GRB120316A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13073
SUBJECT: IPN Triangulation of GRB 120316A
DATE:    12/03/20 14:09:19 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,

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 GRB 120316A was observed by Fermi (GBM: trigger 353549464), 
INTEGRAL (SPI-ACS), Konus-Wind, Mars Odyssey (HEND), Suzaku (WAM), and 
Swift (BAT) (outside the coded field of view) at about 662 s UT (00:11:02).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    57.016 (03h 48m 04s) -56.288 (-56d 17' 15")
  Corners:
    56.269 (03h 45m 05s) -57.541 (-57d 32' 28")
    57.363 (03h 49m 27s) -57.038 (-57d 02' 16")
    57.698 (03h 50m 48s) -55.028 (-55d 01' 42")
    56.676 (03h 46m 42s) -55.538 (-55d 32' 18")
  ---------------------------------------------

The error box area is 1.07 sq. deg, and its maximum
dimension is 2.6 deg.

This box can be improved.

The LAT position reported by Zheng & Akerlof (GCN
13070 ) is consistent with the IPN box (the center of this position is 
outside the box, but the error circle overlaps with the box).

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/GRB120316_T00672/IPN/


GRB_name: GRB120316A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13074
SUBJECT: Konus-Wind observation of GRB 120316A
DATE:    12/03/20 14:18:02 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 120316A (GBM trigger 353549464;
Fermi/LAT detection: Zheng & Akerlof, GCN 13070;
IPN localization: Hurley at al., GCN 13073)
triggered Konus-Wind at T0=00672.966s UT (00:11:12.966)

The light curve shows multiple partly overlapped pulses.
A total duration of the burst is ~32 s.
The emission is seen up to ~8 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120316_T00672/

As observed by Konus-Wind the burst
had a fluence of 2.3(-0.4,+0.5)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+9.216 s,
of 2.5(-0.5,+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+15.872 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.92 (-0.13, +0.15),
and Ep = 539(-109, +167) keV,
chi2 = 92/86 dof.

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


GRB_name: GRB120320A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13075
SUBJECT: GRB 120320A: Enhanced Swift-XRT position
DATE:    12/03/20 14:48:36 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 995 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120320A, 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 = 212.51794, +8.69646 which is equivalent
to:

RA (J2000): 14h 10m 4.31s
Dec (J2000): +08d 41' 47.3"

with an uncertainty of 2.2 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB120320A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13077
SUBJECT: GRB 120320A: Gemini-N and UKIRT observations
DATE:    12/03/20 15:33:26 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

A. J. Levan (U. Warwick), N. R. Tanvir (U. Leicester), T. Wold (JACH) and
R. Mason (Gemini) report on behalf of a larger collaboration:

We obtained observations of the field of GRB 120320A (Markwardt et al.
GCN13071) with both Gemini-N/GMOS in i and z, and UKIRT/WFCAM in J, H
and K. Our first observations began approximately 30 minutes after the burst,
and continued for a further 2 hours.

Within the refined X-ray error circle (Beardmore et al. GCN 13075) we detect a
very faint source in our GMOS imaging at position (accuracy ~0.5"):

RA(2000)=14:10:04.28
dec(2000)=08:41:47.9

The source has i~25.7+/-0.3 and z~25.3+/-0.3. It is undetected in the UKIRT
imaging to preliminary limits of J>21.6, H>20.0 and K>19.5.

This source could therefore be related to either the afterglow or the host galaxy of
GRB 120320A, but at the current time we cannot make any statements about fading.


GRB_name: GRB120320A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13078
SUBJECT: GRB 120320A, Swift-BAT refined analysis
DATE:    12/03/20 16:10:19 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@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), 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+512 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120320A (trigger #518200)
(Markwardt, et al., GCN Circ. 13071).  The BAT ground-calculated position is
RA, Dec = 212.517, 8.682 deg which is
    RA(J2000)  =  14h 10m 04.0s
    Dec(J2000) = +08d 40' 54.9"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.

The mask-weighted light curve shows two overlapping weak peaks.  There is
possible low-level emission out to approximately T+90 sec.  T90
(15-350 keV) is 25.74 +- 3.55 sec (estimated error including systematics).

The time-averaged spectrum from T-0.01 to T+29.86 sec is best fit by a power
law with an exponential cutoff.  This fit gives a photon index 0.31 +- 0.95,
and Epeak of 62.8 +- 23.4 keV (chi squared 57.5 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.9 +- 1.6 x 10^-07 erg/cm2
and the 1-sec peak flux measured from T+24.10 sec in the 15-150 keV band is
0.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.58 +- 0.18 (chi squared 64.7 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/518200/BA/

[GCN OPS NOTE(20mar12):  The subject line was fixed (added the missing 0).
Appreciation goes to D.Fox for pointing out the omission.]


GRB_name: GRB120320A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13079
SUBJECT: GRB 120320A: Swift-XRT refined Analysis
DATE:    12/03/21 00:12:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), 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), G. Stratta
(ASDC) and C.B. Markwardt report on behalf of the Swift-XRT team:

We have analysed 7.5 ks of XRT data for GRB 120320A (Markwardt et al.
GCN Circ. 13071), from 156 s to 24.3 ks after the  BAT trigger. The
data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Beardmore et al. (GCN. Circ
13075).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.36 (+0.13, -0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.5, -0.4). The
best-fitting absorption column is  1.7 (+1.4, -1.1) x 10^21 cm^-2, in
excess of the Galactic value of 2.0 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 3.8 x 10^-11 (5.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+1.4, -1.1) x 10^21 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index:      2.0 (+0.5, -0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00518200.

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


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13080
SUBJECT: GRB 120320A: BOOTES-4 optical upper limit
DATE:    12/03/21 01:05:22 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

J.C. Tello (IAA-CSIC), P. Kubanek (IP AS CR & IAA-CSIC), J. Gorosabel
(IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC), S. Guziy (Nikolaev St. Univ.),
Yufeng Fan, Xiaohong Zhao, Jiming Bai, Chuanjun Wang and Yuxin Xin
(Yunnan National Astronomical Observatory) and Chenzhou Cui
(Beijing National Astronomical Observatory),
report on behalf of a larger collaboration:

"We observed the field of GRB 120320A (Markwardt et al., GCNC 13071),
detected by Swift/BAT, with the 0.6m BOOTES-4/MET telescope at the Lijiang
Astronomical Observatory, China. Unfiltered images were obtained
starting 13:48:44UT at high airmass (2h12m after the burst, limited by the
local horizon). The resulting limiting magnitude (63 x 180s) is 16.3 when
calibrated with the R1Mag value of USNO-B1.0 catalogue stars."

This message may be cited.

[GCN OPS NOTE(21mar12): Per author's request CW & YX were added to the 
author list.]


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13081
SUBJECT: GRB 120320A , optical observations
DATE:    12/03/21 04:49:14 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Kumar Bhatt and S.B. Pandey (ARIES, Nainital, India,
on behalf of larger Indian GRB collaboration)

We observed the field of GRB 120320A (trigger=518200, Markwardt et al., 
GCN 13071) with the 1.04m telescope at ARIES Nainital starting at 
UT 18:39:42 on 20-03-2012. Three images in R_c pass-band (300 sec each)
were obtained.

The photometry of the co-added R_c frame did not reveal any new source
within the XRT error-box (Melandri et al., GCN 13079). The 3-sigma upper
limit of the co-added frame was found to be ~ 19.5 mag. The photometry
was done in comparison to nearby USNO- B1 stars.

This massage may be cited.


GRB_name: GRB120320A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13082
SUBJECT: GRB 120320A: MITSuME Okayama Optical upper limits
DATE:    12/03/21 04:55:08 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 120320A (Markwardt et al., GCNC 13071)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-03-20 14:11:31 UT (~2.3 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Beardmore et al., GCNC 13075) in all the three bands.
We also could not detect the previously reported afterglow (Levan et al.,
GCNC 13077).


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

T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.13565    15:11:36    6360.0   >20.7  >20.7  >20.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120320A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13083
SUBJECT: GRB 120320A: Swift/UVOT Upper Limits 
DATE:    12/03/21 11:49:34 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 120320A
175 s after the BAT trigger (Markwardt et al., GCN Circ 13071).
No optical afterglow consistent with the enhanced XRT position
(Beardmore et al., GCN Circ 13075) or optical candidate reported
by Levan et al. (GCN Circ 13077) 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    175          325        147      >20.9
White       175        11021       1435      >22.1  
v           663         6181        452      >19.8  
b           589         6965        416      >20.4  
u           333         6796        678      >20.6  
uvw1        713         6591        432      >20.4  
uvm2        688         6386        432      >20.4  
uvw2        639        11148        570      >20.9

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


GRB_name: GRB120229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13084
SUBJECT: GRB 120229A: Magellan observations and limit on an optical afterglow
DATE:    12/03/21 13:41:19 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, E. Berger, N. Sanders (Harvard), K. Cooksey, A. Zangari (MIT) and
N. Morrell (LCO) report:

"We observed the location of the short-duration GRB 120229A (GCN 12997)
with the Low Dispersion Survey Spectrograph 3 (LDSS3) mounted on the
Magellan/Clay 6.5-meter telescope. We obtained 3x180-sec
r-band observations on 2012 March 01.01 UT (9.6 hours post-burst) at
high airmass in mediocre seeing conditions (1.3"). To check for the
presence of a fading optical source, we re-observed the field (6x180-sec)
on 2012 March 02.01 UT (33.6 hours post-burst and 24.0 hours after
the first observations) at similar airmass. Digital image subtraction
of the two epochs using the ISIS software package reveals no
residuals within the BAT-refined position (GCN 12998). Therefore,
calculating the zeropoint from a standard star field at similar
airmass based on several stars, we place a 3-sigma limit of r>22.4 mag on
the optical afterglow of GRB 120229A at 9.6 hours after the burst."


GRB_name: GRB120316A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13085
SUBJECT: GRB 120316A: Fermi-GBM and Fermi-LAT Observations
DATE:    12/03/21 21:22:59 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

Giacomo Vianello (CIFS/SLAC), Nicola Omodei (Stanford U.), J. L.
Racusin (NASA/GSFC), P. Jenke (MSFC/NPP) report on behalf of the Fermi
GBM and LAT Teams:

At 00:11:02.56 UT on 16 March 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120316A (trigger 353549464 / 120316008),
which was also detected by Konus-Wind (GCN 13074) and triangulated by
the IPN (GCN 13073). The GBM H.I.T.L. location is found to be RA, Dec
(J2000) = 48.5, -64.3 with a error radius (90% containment,
statistical) of 1.2 degrees.

The GBM light curve shows multiple peaks with a duration of T90 = 27.5
+/- 0.4 seconds, and a signal extending to 500 keV in the NaI's and
850 keV in the BGO's.

The GRB is barely detected by the LAT, with a Test Statistic slightly
below the TS=25 threshold usually adopted for issuing circulars. The
best LAT on-ground location is found to be RA,Dec (J2000) = 57.97,
-56.46 with an error radius of 0.65 deg (90% containment, statistical
error only). This was 9.7 deg from the LAT boresight at the time of
the trigger.

The LAT position is compatible with that found by Zheng et al. (GCN
13070) and by Hurley et al. (GCN 13073), and is ~9 deg away from the
best GBM localization. Modeling of the uncertainties in GBM
localizations, using known reference locations, suggests that whilst
the majority (>90%) are well-represented by a ~3 deg systematic error,
GRB120316A appears to belong to a small tail which has a much larger
systematic uncertainty, centered on ~10 deg (see Connaughton et al.,
in preparation).

The spectrum of this GRB from 10 keV to 300 GeV, integrated over the
time interval 0-32 s from the trigger time, is well described by a
Band function with Epeak = 552 -25 +22 keV, alpha = -0.77 +/- 0.02,
beta = -2.90 +/-0.15. The fluence in the 10 keV - 1 MeV energy range
is 2.57 ( +/- 0.03 (stat) +/- 0.2 (sys) ) x 10^-5 erg/cm2, compatible
with the value found by Golenetskii et al (GCN 13074).

The spectral analysis results presented above are preliminary;

The Fermi LAT point of contact for this burst is Giacomo Vianello
(giacomov@slac.stanford.edu). The GBM point of contact is Peter Jenke
(peter.a.jenke@nasa.gov).

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


GRB_name: GRB120320A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13086
SUBJECT: GRB 120320A, the review of the sky area in plate archives
DATE:    12/03/22 11:43:46 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V. Golovnya, A. Yatsenko, L. Pakuliak (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120320A (A.P. Beardmore et al. GCN Circ.13075) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19820304/012601 GUA040C000022A 22.5 16.30 0975-07400209
19820304/012601 GUA040D000023A 22.5 15.25 0975-07399206
19820513/204316 GUA040C002367 59.8 16.90 0975-07398764
19820513/204322 GUA040D002368 59.7 15.65 0975-07399102
19830510/214749 GUA040C002451 32.5 15.25 0975-07399206
19900223/015615 GUA040C001585A 20.0 15.65 0975-07399102
19900301/014633 GUA040C001620 16.0 15.65 0975-07399102
19910411/231232 GUA040C001778A 22.5 15.65 0975-07399102
19910512/205130 GUA040C001783 18.0 15.25 0975-07399206
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 28 minutes area around 
     the location given in A. Beardmore et al. GCN Circ.13075: 
       RA(J2000)= 14h 10m 04.31s, Dec(J2000)= +08d 41' 47.3"
Star USNOA2 - Comparison star.
  The preview images of 9 areas together with  
the 28x28 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120320A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13087
SUBJECT: GRB 120320A: Zadko optical observations
DATE:    12/03/22 12:16:50 GMT
FROM:    David Coward at U of Western Aus.  <coward@physics.uwa.edu.au>

D. Macpherson (UWA/ICRAR), D. Coward (UWA), A. Klotz (IRAP-CNRS-OMP),
B. Gendre (ASDC/INAF-OAR), M. Todd (Curtin-ICRAR), M. Boer (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA) report:

We imaged the field of GRB 120320A detected by SWIFT
(trigger 518200) with the UWA Zadko robotic telescope (D=100cm)
located at Gingin, Australia.

The observations started 6.8 hr after the GRB trigger.
The elevation of the field was 49 deg and humid= 63%.

9 images have been maded with a duration of 180.0s each.
At the position of the XRT afterglow (Beardmore et al., GCN 13075),
we do not detect any source with a limiting magnitude of
r = 20.7 on the summed images.

The nearest object, which is about 14 arcsec, in our summed image to
the XRT location, is a SDSS galaxy (J141005.65+084149.2 ) with a
photometric z = 0.34 +- 0.167.

This message may be cited.


GRB_name: GRB120316A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13088
SUBJECT: GRB 120316A : Suzaku WAM observation of the prompt emission
DATE:    12/03/23 07:51:49 GMT
FROM:    Yoshitaka Hanabata at Hiroshima U  <hanabata@hep01.hepl.hiroshima-u.ac.jp>

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

The long GRB 120316A (GBM trigger 353549464; Fermi-LAT detection:
Zheng & Akerlof, GCN 13070; IPN localization: Hurley at al., GCN 13073) 
was detected by the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 00:11:02 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0,
ending at T0+28 s with a duration (T90) of about 24 seconds. The
fluence in 100 - 1000 keV was 1.79 (-0.49, +0.07) x 10^-5 erg/cm^2. The
1-s peak flux measured from T0+21 s was 2.75 (-1.02, +0.31)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from 
T0 to T0+28 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -0.44 (-0.61, +0.89),
the high-energy photon index beta: -2.63 (-0.58, +0.31),
and the peak energy Epeak: 530 (-76, +89) keV (chi^2/d.o.f = 12.6/12).

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

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


GRB_name: GRB120324A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13090
SUBJECT: GRB 120324A: Swift detection of a burst
DATE:    12/03/24 06:14:22 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.-B. Zhang (PSU), A. P. Beardmore (U Leicester), D. Grupe (PSU),
C. Guidorzi (U Ferrara), E. A. Hoversten (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 05:59:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120324A (trigger=518507).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 291.084, +24.145 which is 
   RA(J2000) = 19h 24m 20s
   Dec(J2000) = +24d 08' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 90 sec.  The peak count rate
was ~10500 counts/sec (15-350 keV), at ~34 sec after the trigger. 

The XRT began observing the field at 06:00:26.4 UT, 75.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 291.0771, 24.1290 which is equivalent to:
   RA(J2000)  = +19h 24m 18.50s
   Dec(J2000) = +24d 07' 44.4"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 61 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 1.92e-08 erg cm^-2 s^-1 (0.2-10
keV). 

No UVOT data are available at this time. 

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: GRB120324A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13091
SUBJECT: GRB 120324A: UVOT Finding Chart Observation
DATE:    12/03/24 06:32:25 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

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

In response to GRB120324A (Swift/BAT trigger 518507, Zhang et al. GCN Circ. 
13090) at 05:59:11 UT, UVOT took a finding chart exposure of 150 seconds 
with the White filter starting 84 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. 


GRB_name: GRB120324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13092
SUBJECT: GRB 120324A: Liverpool Telescope optical candidate
DATE:    12/03/24 07:10:25 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
report on behalf of the LJMU GRB group:

The 2-m Liverpool Telescope automatically observed
Swift GRB 120324A (Zhang et al. GCN Circ. 13090)
on March 24, from 06:13:42 UT, corresponding to
14.5 minutes after the BAT trigger time.
Within the XRT error circle we detect an uncatalogued
object with 20.3 +- 0.3 mag in the r' band at the
following position

19:24:18.76   +24:07:50.1  (J2000).

At the moment we cannot make any statement about its
possible variability.
Magnitudes are calibrated against nearby USNOB-1 stars.


GRB_name: GRB120324A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13093
SUBJECT: GRB 120324A: Enhanced Swift-XRT position
DATE:    12/03/24 09:08:32 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 1195 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120324A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 291.07873, +24.12958 which is equivalent
to:

RA (J2000): 19h 24m 18.90s
Dec (J2000): +24d 07' 46.5"

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

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

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


GRB_name: GRB120324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13094
SUBJECT: GRB 120324A: TAROT La Silla observatory optical observations
DATE:    12/03/24 11:35:21 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 120324A detected by SWIFT
(trigger 518507) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 1.98h after the GRB trigger
(it was not risen when the GRB occured).
The elevation of the field increased from
11 degrees above horizon and weather conditions
were good.

We co-added a long series of exposures. We do not
detect any OT in the XRT enhanced position (Evans et al.
GCNC 13093):

      start      end    magnitude
tgrb+1.98h tgrb+3.23h  R > 19.7

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

N.B. Galactic coordinates are lon= 58.0588 lat= +4.0337
and the galactic extinction in R band is about 3 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120324A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13095
SUBJECT: GRB 120324A: Swift/UVOT Upper Limits
DATE:    12/03/24 12:36:49 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120324A
84 s after the BAT trigger (Zhang et al., GCN Circ. 13090).
No optical afterglow, consistent with the XRT position
(Evans et al., GCN Circ. 13093) or the uncatalogued 
object reported by the Liverpool Telescope (Guidorzi et al., GCN Circ. 13092),
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            84          234          147         >21.2
u_FC               297          547          246         >20.2
white               84         4917          569         >22.1
v                  627         5329          294         >19.9
b                  553         1510           89         >19.6
u                  297         1493          324         >20.2
w1                 676         5615          171         >19.9
m2                 652         5534          216         >20.0
w2                 603         5124          274         >20.8

The magnitudes in the table are not corrected for the significant Galactic extinction
due to the reddening of E(B-V) = 1.12 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120324A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13096
SUBJECT: GRB 120324A: Swift-BAT refined analysis
DATE:    12/03/24 14:25:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU), B.-B. Zhang (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120324A (trigger #518507)
(Zhang, et al., GCN Circ. 13090).  The BAT ground-calculated position is
RA, Dec = 291.081, 24.140 deg, which is 
   RA(J2000)  =  19h 24m 19.5s 
   Dec(J2000) = +24d 08' 23.6" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.
 
The mask-weighted light curve shows many overlapping peaks starting
at ~T-190 sec with a weak precursor peak, the main peak at ~T+33 sec, and
ending at ~T+180 sec (and possible as long as ~T+330 sec at the 2-sigma level).
T90 (15-350 keV) is 118 +- 10 sec (estimated error including systematics).
 
The time-averaged spectrum from T-150.5 to T+142.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.04.  The fluence in the 15-150 keV band is 1.01 +- 0.03 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+33.68 sec in the 15-150 keV band
is 5.9 +- 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/518507/BA/


GRB_name: GRB120324A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13097
SUBJECT: GRB 120324A: CQUEAN rizY Observation
DATE:    12/03/24 15:47:25 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Jae-Woo Kim, and Duho Kim (CEOU/Seoul National Univ.)

We observed GRB 120324A (Zhang et al., GCN 13090) in
r,i,z,Y filters using CQUEAN camera on the 2.1m Otto-Struve
telescope at McDonald Observatory, Texas, US.

The observation started at 2012-03-24 10:31:44 UT,
or about 4.5 hours after the BAT alert.
We find a faint object in i,z,Y images at the edge of
the error circle of the enhanced XRT position
(Evans et al. GCN 13093).

The coordinate of the object is

   RA=19:24:18.78, Dec=24:07:47.3 (J2000)

with an error of 0.7".

Due to high stellar density in this field, it is not clear
if this object is the optical counterpart of the GRB
Further observations are planned to check the variability
of this source. The finding chart of the object is available at
http://astro.snu.ac.kr/~mim/grb120324a/grb120324a_cquean_i.gif

We note that an optical candidate reported by
Guidorzi et al. (GCN 13092) is clearly seen in both a POSS2 image
retrieved from the Digitized Sky Survey and our CQUEAN images,
making it less likely that the object is a GRB afterglow.

We thank Karl Gebhardt and his observing team for their help
with the observation.


GRB_name: GRB120324A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13098
SUBJECT: GRB 120324A: GROND observations
DATE:    12/03/24 15:53:34 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 120324A (Swift trigger 518507; Zhang et al., 
GCN #13090) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 09:04 UT, approx. 3 hrs after the GRB trigger and 
lasted for approx. 35 min. They were performed at an average seeing of 
1.0" and at high airmass.

The source reported by Guidorzi et al. (GCN #13092) is clearly detected at 
a constant brightness of r' = 20.3 +/- 0.2. The lack of fading and 
location outside the enhanced XRT error circle argue against an 
association with the GRB.

In addition, we detect a single source at the border of the XRT error 
circle at coordinates

RA (J2000):   19h 24m 18.80s
Dec (J2000): +24d 07' 47.4" (+/- 0.5")

at a brightness of r' ~ 22.6 mag. This source has an extended morphology 
and could be the host galaxy (see also Im et al., GCN 13097).

Magnitudes have been calibrated against GROND zeropoints. We note that 
there is a significant Galactic foreground reddening of E(B-V) ~ 1.2 mag 
(Schlegel et al. 1998).


GRB_name: GRB120323A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13099
SUBJECT: GRB 120323A: Fermi GBM detection
DATE:    12/03/24 16:02:47 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

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

"At 12:10:19.72 UT on 23 March 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120323A (trigger 354197421 / 120323507).

The on-ground calculated location, using the GBM trigger
data, is RA = 346.8, DEC = 27.2 (J2000 degrees,
equivalent to 23 h 07 m, 27 d 12 '), 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).
(This location has been updated from an earlier GCN notice).

The angle from the Fermi LAT boresight is 43 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 very bright, double-peaked FRED-like pulse
with a duration (T90) of about 0.446 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.512 s is
best fit by a Band function with Epeak = 64.8 +/- 3.8 keV,
alpha = -0.82 +/- 0.07, and beta = -2.01 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(1.080 +/- 0.002)E-05 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 574.7 +/- 7.8 ph/s/cm^2. 
This peak flux is the highest of the mission to date.

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


GRB_name: GRB120324A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13100
SUBJECT: Konus-Wind observation of GRB 120324A
DATE:    12/03/24 17:02:59 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 120324A (Swift-BAT trigger #518507:
Zhang et al., GCN 13090; Cummings et al., GCN 13096)
triggered Konus-Wind at T0=21550.757s UT (05:59:10.757)

The light curve shows multiple peaks
with a total burst duration of ~65 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/GRB120324_T21550/

As observed by Konus-Wind the burst
had a fluence of (4.5  1.2)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+0.768 s,
of (3.7  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+41.216 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, +0.11),
the high energy photon index beta = -2.3 (-1.0, +0.3),
the peak energy Ep = 445(-80, +117) keV,
chi2 = 82.3/86 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+8.448 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 = -0.87 (-0.12, +0.15),
the high energy photon index beta = -2.6 (<-2.1),
the peak energy Ep = 504(-103, +135) keV,
chi2 = 90.9/86 dof.

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


GRB_name: GRB120324A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13101
SUBJECT: GRB 120324A: Swift-XRT refined Analysis
DATE:    12/03/24 18:14:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), 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), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB) and B.-B. Zhang report on behalf of the Swift-XRT team:

We have analysed 8.3 ks of XRT data for GRB 120324A (-B. Zhang et al.
GCN Circ. 13090), from 81 s to 29.5 ks after the  BAT trigger. The data
comprise 160 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 13093).

The late-time light curve (from T0+4.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.04 (+/-0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.12 (+/-0.10). The
best-fitting absorption column is  1.10 (+0.09, -0.08) x 10^22 cm^-2,
in excess of the Galactic value of 4.5 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.07 (+/-0.14) and a
best-fitting absorption column of 1.18 (+0.13, -0.12) x 10^22 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.7 x 10^-11 (1.3 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.18 (+0.13, -0.12) x 10^22 cm^-2
Galactic foreground: 4.5 x 10^21 cm^-2
Excess significance: 9.9 sigma
Photon index:      2.07 (+/-0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00518507.

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


GRB_name: GRB120323A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13102
SUBJECT: IPN Triangulation of GRB 120323A (short/very intense)
DATE:    12/03/25 09:13:33 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,

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

A. von Kienlin, X. Zhang, V. Savchencko, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team, report:

The short-duration, very intense GRB 120323A has been observed by 
INTEGRAL (SPI-ACS), Fermi (GBM trigger 354197421: Gruber & Connaughton, 
GCN 13099), Konus-Wind, MESSENGER (GRNS), and Swift (BAT) so far, at 
about 43820 s UT (12:10:20). 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:
   340.407 (22h 41m 38s) +29.717 (+29d 43' 03")
  Corners:
   340.592 (22h 42m 22s) +30.058 (+30d 03' 29")
   340.405 (22h 41m 37s) +29.942 (+29d 56' 30")
   340.226 (22h 40m 54s) +29.374 (+29d 22' 27")
   340.410 (22h 41m 38s) +29.493 (+29d 29' 35")
  ---------------------------------------------
The error box area is 262 sq. arcmin, and its maximum
dimension is 45 arcmin.

This box may be improved.

The center of the GBM location (Gruber & Connaughton, GCN 13099) is 6.2 
deg from the center of the IPN box.


GRB_name: GRB120323A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13103
SUBJECT: Konus-Wind observation of GRB 120323A
DATE:    12/03/25 12:28:28 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 very intense GRB 120323A
(Fermi/GBM detection: Gruber & Connaughton, GCN 13099;
IPN localization: Golenetskii at al., GCN 13102)
triggered Konus-Wind at T0=43815.970s UT (12:10:15.970)

The light curve shows a double-headed FRED-like structure.
A total duration of the burst is ~0.5 s.
The emission is seen up to ~8 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120323_T43815/

A spectral lag between hard G3(300-1400 keV) and soft G1(22-80 keV)
instrument's light curves is estimated to (-0.002 +/- 0.004) s.

As observed by Konus-Wind the burst
had a fluence of 1.03(-0.07,+0.07)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.016 s,
of 7.2(-0.9,+0.9)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 = -1.57 (-0.07, +0.07),
and Ep = 331(-50, +64) keV,
chi2 = 45.8/42 dof.
Fitting this spectrum with the GRB (Band) function
gives an equally good result with the following model parameters:
the low-energy photon index alpha = -1.56 (-0.07, +0.09),
the high energy photon index beta = -2.9 (<-2.4),
the peak energy Ep = 317(-76, +68) keV,
chi2 = 44.3/41 dof.

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


GRB_name: GRB120323A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13104
SUBJECT: GRB 120323A: Fermi LAT observations
DATE:    12/03/25 17:28:31 GMT
FROM:    Thomas P.H. Tam at Nat.Tsing Hua U.  <grbtom@gmail.com>

P.H.T. Tam and A.K.H. Kong (NTHU) report:

We report on the Fermi/LAT observations of the short (~0.5s) and very
bright GRB 120323A
that triggered Fermi/GBM (Gruber & Connaughton, GCN 13099), Konus-Wind and
a few other detectors (Golenetskii at al., GCN 13102). Using the 10-degree
radius data centered on the IPN Triangulation position (GCN 13102), we did
not find any significant emission above 60 MeV from this circular region
during the prompt emission nor between 0.5 and 100 seconds after the
Konus-Wind
trigger time (T0).

Extrapolating the high-energy photon index, beta, which is 2.9, in the
best-fit
Band function (GCN 13103) to the LAT energy range, we derived 90% C.L.
upper
limits (0.1-10 GeV) for the following periods as tabulated below
(calculated
using Feldman & Cousins, 1998 formulation):

Epoch U.L. (ph/cm2-s)
T0 to T0+0.5s 3.5e-3
T0+0.5s to T0+1.0s 3.5e-3
T0+1.0s to T0+3.0s 8.7e-4
T0+3.0s to T0+10s 2.5e-5
T0+10s to T0+100s 1.3e-5


GRB_name: GRB120326A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13105
SUBJECT: GRB 120326A: Swift detection of a burst
DATE:    12/03/26 01:32:31 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), D. Grupe (PSU), E. A. Hoversten (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 01:20:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120326A (trigger=518626).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 273.925, +69.278 which is 
   RA(J2000) = 18h 15m 42s
   Dec(J2000) = +69d 16' 41"
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 40 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 01:21:28.8 UT, 59.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 273.90195,
69.26028 which is equivalent to:
   RA(J2000)  = 18h 15m 36.47s
   Dec(J2000) = +69d 15' 37.0"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 70 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 5.24
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 2.01e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 67 seconds after the BAT trigger. No credible
afterglow candidate has  been found in the initial data products. No
afterglow is seen in the 2.7'x2.7' sub-image. 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 M. H. Siegel (siegel AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB120326A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13106
SUBJECT: GRB 120326A: ROTSE-III Optical Limits
DATE:    12/03/26 01:47:12 GMT
FROM:    Wiphu Rujopakarn at U AZ/Steward  <rujopakarn@gmail.com>

W. Rujopakarn (Steward) and H. Flewelling (IfA/Hawaii) report on
behalf of the ROTSE collaboration:

ROTSE-IIId, located at the Turkish National Observatory at
Bakirlitepe, Turkey, responded to GRB 120326A (Swift trigger 518626;
Siegel et al., GCN 13105), producing images beginning 9.9 s after the
GCN notice time. An automated response took the first image at
01:20:51.9 UT, 22.6 s after the burst, under fair conditions. We took
10 5-sec, 10 20-sec and 10 60-sec exposures. These unfiltered images
are calibrated relative to USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or the XRT error circle, for both
single images and coadding into sets of 10. Individual images have
limiting magnitudes ranging from 14.7-16.7; we set the following
specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
01:20:51.9   01:20:56.9         5     14.7           22.6       N
01:20:51.9   01:22:59.9       128     16.3           22.6       Y


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13107
SUBJECT: GRB 120326A: TAROT Calern observatory afterglow optical detection
DATE:    12/03/26 01:54:39 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 120326A detected by SWIFT
(trigger 518626) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 133.1s after the GRB trigger
(119.3s after the notice). The elevation of the field increased from
49 degrees above horizon and weather conditions
were good.

We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart at the XRT position
mentioned by Siegel et al. (GCNC 13105)
at the following position (+/- 2 arcsec):

RA(J2000) = 18h 15m 37.06s
DEC(J2000) = +69d 15' 35.3"

OT was R~18.2 at 163s after GRB.

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

As the afterglow was not detected by UVOT, we suggest
a high redshift (but z<7) for this burst.

N.B. Galactic coordinates are lon= 99.5219 lat=+28.3852
and the galactic extinction in R band is about 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13108
SUBJECT: GRB 120326A: TAROT Calern observatory afterglow optical decay
DATE:    12/03/26 02:35:17 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:

The TAROT observations are continuing after the optical
detection mentioned in the GCNC (13107):

start  end   Rmag
(min) (min)
  2.22  3.21  18.2
24.91 40.66  19.1

That suggests a slow decay (alpha~0.35) of the optical
afterglow.


GRB_name: GRB120326A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13109
SUBJECT: Skynet/Dolomiti Observations of GRB120326A
DATE:    12/03/26 03:02:32 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, J. Haislip, K. Ivarsen, M. Maturi, 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 Swift/XRT localization of GRB 120326A (Swift trigger 
#518626) with the Dolomites Astronomical Observatory located at the Carlo 
Magno Hotel Spa Resort in Italy. Observations in SDSS g',r',i' and z' began 
93 seconds after the trigger (113 seconds after the burst). We detect an 
optical transit at the position reported by Klotz et. al. (GCN 13107). 
Stacking images and calibrating to USNO B1.0 stars yields the following:

Mean Time
Since triger Tel Exposures Filter Magnitude
37.23 m  DAO 3 x 160 s     g 20.770
39.90 m  DAO 4 x 160 s r 19.868
51.48 m  DAO 5 x 160 s i 19.236


GRB_name: GRB120326A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13110
SUBJECT: GRB 120326A: Enhanced Swift-XRT position
DATE:    12/03/26 05:12:08 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 1040 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 120326A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 273.90451, +69.25998 which is equivalent
to:

RA (J2000): 18h 15m 37.08s
Dec (J2000): +69d 15' 35.9"

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: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13111
SUBJECT: GRB 120326A: Liverpool Telescope observations
DATE:    12/03/26 06:50:26 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara) reports on behalf of
the LJMU GRB group:

The 2-m Liverpool Telescope automatically observed
Swift GRB 120326A (Siegel et al. GCN Circ. 13105)
on March 26, from 01:34:07 UT, corresponding to
13.6 minutes after the BAT trigger time.
Within the XRT error circle we clearly detect the
optical afterglow (Klotz et al. GCN Circ. 13107,
13108; LaCluyze et al. GCN Circ 13109) with the
SDSS riz filters at the following position

18:15:37.13   +69:15:35.7   (J2000)

uncertainty of 0.3". We estimate the magnitude
of the afterglow as follows:

Mid time from    Exp     Filter    Magnitude
GRB (min)        (s)
---------------------------------------------
14.1             3x10    r        19.1 +- 0.2
44.8             120     r        19.6 +- 0.1
---------------------------------------------

Magnitudes are calibrated against nearby USNOB-1
stars.


GRB_name: GRB120326A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13112
SUBJECT: GRB120326A: IAC80 observations
DATE:    12/03/26 07:29:53 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

Walker, C., Court J., Duffy, R., Edwards T., Herath, M., Kirk, J.,  
Patel, S., Prajs, S., Tunbridge, B., Williams, D., Wood, R., Wright,  
P., Munoz-Darias, T., Knigge, C., Coriat, M. (University of  
Southampton), Gimeno, R. (IAC, Tenerife), Gorosabel, J. (IAA-CSIC,  
Granada), report:

We observed the Swift/XRT location of the GRB 120326A (Goad et al.,  
GCNC 13110) using the IAC80 82cm telescope at Tenerife (Canary  
Islands, Spain).   We took a set
of VRI-band images from 02:23:20 UT to 05:47:06 UT. The optical  
transient (Klotz et al., GCNC 13108) is clearly detected. After a  
calibration using the USNO B1 catalogue, we detected an important  
rebrightening from R=19.4 to R=18.4.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13113
SUBJECT: GRB 120326A: Optical observations at Crni Vrh
DATE:    12/03/26 13:17:23 GMT
FROM:    Bojan Dintinjana at OCV  <bojan.dintinjana@fmf.uni-lj.si>

B. Dintinjana and B. Mikuz on behalf of PIKA observing program at Crni 
Vrh Observatory:

We observed the afterglow of GRB 120326A (Siegel et al., GCN 13105) with 
60 cm Cichocki robotic telescope at Crni Vrh Observatory, Slovenia. The 
series of twenty 60 second exposures with R filter started at 1:27:50UT, 
440 seconds after the burst. We confirm optical afterglow at coordinates 
by C. Guidorzi (GCN 13111).

Photometry results are given in table below. The table contains the time 
since the Swift GRB detection to the middle of exposure in seconds, R 
magnitude and photometric error. The magnitudes are derived using 
comparison stars from the USNO-B1 catalogue. The 3-sigma limiting 
magnitude in R filter is around magnitude 20.5  0.3


Time [s] R Mag   Err.
----------------------------
  440    18.51    0.2
  507    19.07    0.2
  574    19.21    0.3
  641    19.75    0.4
  708    19.63    0.6
  775    19.10    0.2
  842    19.48    0.3
  909    19.19    0.2
  976    19.77    0.4
1043    19.01    0.2
1110    19.11    0.2
1177    19.18    0.2
1244    19.62    0.3
1311    20.02    0.5
1379    19.35    0.3
1446    19.79    0.4
1513    19.38    0.3
1580    18.97    0.2
1647    19.42    0.3
1714    19.82    0.4
----------------------------


GRB_name: GRB120326A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13114
SUBJECT: GRB 120326A: Swift/UVOT Detection
DATE:    12/03/26 13:21:22 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL), S. Holland (STScI), and M. H. Siegel (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120326A
67 s after the BAT trigger (Siegel et al., GCN Circ. 13105).
A source consistent with the XRT position (Goad et al., GCN Circ. 13110
is detected in the initial UVOT exposures at position: RA (J2000)
= 18:15:37.13, Dec (J2000) = +69:15:35.36 or, in decimal degrees:
273.90471, 69.259822 with an uncertainty of 0.5" (90 % confidence).

The transient was initially increasing in brightness, and after a small
decay rebrightened around 10ks after the trigger. There is also some
indication of colour dependence of the time of rebrightening.

The detection in the UVOT uvw2 filter gives an upper limit for the
redshift of about z < 1.6 for this burst.

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            67          217          147        >20.0
white             3903         4103          197         20.16 +/- 0.12
v                 4314         5949          393        >19.3
b                 3697         5334          393         20.23 +/- 0.16
u                 4929         5128          197         19.66 +/- 0.20
m2                4518        16222         1228        >21.2
w2                4109         5744          393        >21.0
w1                9527        10427          886         20.21 +/- 0.18
v                21959        22259          295         18.67 +/- 0.12
w2               21052        21952          886         21.26 +/- 0.32

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: GRB120326A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13115
SUBJECT: GRB 120326A: Swift-XRT refined Analysis
DATE:    12/03/26 13:32:06 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), G.
Stratta (ASDC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) and M.H.
Siegel report on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 120326A (Siegel  et al. GCN
Circ. 13105), from 65 s to 34.6 ks after the  BAT trigger. The data
comprise 100 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 13110).

The late-time light curve (from T0+3.7 ks) can be modelled with an
initial power-law decay with an index of alpha=0.20 (+0.15, -0.11),
followed by a break at T+16.6 ks to an alpha of -1.47 (+0.76, -0.03).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 4.4 (+0.4, -0.3). The
best-fitting absorption column is  3.4 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 5.2 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.89 (+/-0.10) and a
best-fitting absorption column of 9.1 (+2.3, -2.2) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (4.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.1 (+2.3, -2.2) x 10^20 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: 2.9 sigma
Photon index:      1.89 (+/-0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00518626.

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


GRB_name: GRB120323A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13116
SUBJECT: GRB 120323A: MASTER follow up observations
DATE:    12/03/26 14:12:14 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
Sternberg Astronomical Institute, Moscow State University

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

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

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

V.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 Tunka was pointed to the  GRB100423A  ~56.8 hours after GRB 
time at 2012-03-25 21:00:59 UT.
On our coad image (total exposure is 1620 s )  we haven't found 
optical transient   within IPN error-box (Golenetskii et al., GCN No 13102)
The 5-sigma upper limit has been about 19.6 mag

The image is available at 
http://observ.pereplet.ru/images/GRB120323A/GRB120323A.jpg

The list of the known galaxies in IPN error box is:


   pgc   |        objname         | objtype |  mag   |   gal coord
---------+------------------------+---------+-------+-------+-------+---------+------------------------------------------------
  3967112 | 2MASXJ22410968+2946262 | g      | 17.38 | <(22h 41m 09.7s , +29d 46m 26s) , 00d 00m 04s>
  3967215 | 2MASXJ22412549+2942234 | g      | 18.73 | <(22h 41m 25.5s , +29d 42m 23s) , 00d 00m 04s>
  3967227 | 2MASXJ22412751+2958424 | g      | 17.09 | <(22h 41m 27.5s , +29d 58m 42s) , 00d 00m 04s>
  3967373 | 2MASXJ22415652+2929572 | g      | 16.18 | <(22h 41m 56.5s , +29d 29m 57s) , 00d 00m 04s>
  1869472 | PGC1869472             | G      |  17.2 | <(22h 42m 19.7s , +29d 32m 14s) , 00d 00m 33s>
  1873303 | PGC1873303             | G      | 16.44 | <(22h 41m 08.5s , +29d 39m 07s) , 00d 00m 54s>
  1881060 | PGC1881060             | G      | 17.24 | <(22h 41m 35.2s , +29d 51m 52s) , 00d 00m 35s>
  1884891 | PGC1884891             | G      | 16.69 | <(22h 42m 13.5s , +29d 57m 54s) , 00d 00m 37s>
  1888138 | PGC1888138             | G      | 17.61 | <(22h 41m 46.0s , +30d 02m 53s) , 00d 00m 30s>


The message may be cited.


GRB_name: GRB120326A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13117
SUBJECT: GRB 120326A: CQUEAN grizY Observation
DATE:    12/03/26 15:13:20 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Jae-Woo Kim, and Duho Kim (CEOU/Seoul National Univ.)

We observed GRB 120326A (Siegel et al., GCN 13105) in
g,r,i,z,Y filters using CQUEAN camera on the 2.1m Otto-Struve 
telescope at McDonald Observatory, Texas, US.

The observation started at 2012-03-26 10:09:22 UT, 
or about 8.8 hours after the BAT alert. 
In all of the g,r,i,z,Y-band images with 300 sec
exposure time each, we clearly detect the afterglow
reported earlier (Klotz et al. GCN 13107, 
Guidorzi et al. GCN 13111, Walker et al. GCN 13112, 
Dintinjana et al. GCN 13113, Kuin et al. GCN 13114),

We thank Karl Gebhardt and Alysha Shugart for allowing us
to observe this object during their observing run.
We plan to perform additional observations.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13118
SUBJECT: GRB 120326A: GTC redshift
DATE:    12/03/26 15:39:01 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

J. C. Tello, R. Snchez-Ramrez, J. Gorosabel, A. J. Castro-Tirado (IAA-CSIC Granada), M. A. Rivero, G. Gmez-Velarde (GTC La Palma) and A. Klotz (IRAP-CNRS-OMP), on behalf of a larger collaboration, report:

"Following the detection of the optical afterglow to GRB 120326A (Siegel et al. GCNC 13105, Klotz et al. GCNC 13107), we have taken four spectra (600s each) with the 10.4m GTC (+ OSIRIS) at the Spanish Observatorio del Roque de los Muchachos (La Palma). The spectra, covering the range 4000-10000 A were taken starting 1.8 hr post burst, and reveal several absorption features, including CIV 1548-1550, Fe II 2344, Fe II 2383, Mg II 2796-2804 at a common redshift of 1.798. We therefore suggest this to be the redshift of GRB 120326A."

This message can be quoted.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13119
SUBJECT: GRB 120326A: T17 optical observations
DATE:    12/03/26 17:43:42 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

T17 (AstroCamp Observatory, Nerpio, Spain) CDK17 17 inch (0.43 m)
f/6.8 and FLI ProLine CCD camera were used to detect GRB 120326A
optical afterglow 1.7 hours after the burst trigger. The observations were
started at 2012-03-26 02:54:48 (UT) and stopped at 2012-03-26 
03:10:24 (UT). Six unfiltered observations with 120s exposure time were
made. The afterglow was detected at following position RA 18:15:37.13
and DEC +69:15:35.6.

The following magnitude was obtained from the observations using 
NOMAD1 1592-0145660 (R = 17.740) as the comparison:

Tmid(sec)+T0    Filter            Exp (sec)     Mag      Mag err    Limit
6125                 unfiltered      6x120          19.0      0.2           20.0

A jpg image of the observation is available at the following URL link:
http://cutenews.kassiopeia.net/data/upimages/GRB120326A.png


GRB_name: GRB120326A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13120
SUBJECT: GRB 120326A: Swift-BAT refined analysis
DATE:    12/03/26 18:04:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), C. B. Markwardt (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),
G. Sato (ISAS), M. H. Siegel (PSU), 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 120326A (trigger #518626)
(Siegel, et al., GCN Circ. 13105).  The BAT ground-calculated position is
RA, Dec = 273.906, 69.248 deg, which is 
   RA(J2000)  =  18h 15m 37.3s 
   Dec(J2000) = +69d 14' 54.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 91%.
 
The mask-weighted light curve shows a possible (2-sigma) precursor peak
at ~T-105 sec, and two definite precursor peaks (~30 sec wide each) at ~T-60 sec
and ~T-25 sec.  The main FRED peak starts T_0, peaks at ~T+4 sec, and
returns to background at ~T+20 sec.  T90 (15-350 keV) is 69.6 +- 8.3 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-67.90 to T+22.56 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.41 +- 0.34, 
and Epeak of 41.1 +- 6.9 keV (chi squared 55.8 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.6 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+3.59 sec in the 15-150 keV band is
4.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.06 +- 0.07 (chi squared 68.4 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/518626/BA/


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13121
SUBJECT: GRB 120326A : LOT optical observation
DATE:    12/03/27 00:34:38 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Y. Urata (NCU) and K.Y. Huang (ASIAA) on behalf of EAFON

We observed the field of GRB 120326A (GCN 13105) in g, r, i, and z-bands 
with the Lulin 1m telescope operated by IANCU. The observation was
started at 17.2 hrs after the GRB. The optical afterglow (GCN 13107,
13109, 13111) is clearly detected in all of the g,r,i,z-bands. The
afterglow is still keeping the brightness around r = 19.0 (at 18.7 hrs
after the GRB).


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13122
SUBJECT: GRB 120326A: optical observation of GMG
DATE:    12/03/27 02:51:58 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

X.-H. Zhao (YNAO), J. Mao (KASI/YNAO), D. Xu (WIS/NAOC), J.-M. Bai
(YNAO) report on behalf of a larger collaboration:

We observed the afterglow of GRB 120326A (Siegel et al., GCN 13105) with
the 2.4m Gao-Mei-Gu (GMG) telescope. Observations started at 19:03:32
UT on 2012-3-26  (i.e., ~17.7 hrs after the burst) . We found the
following magnitudes:

Start time post-burst (hr)             Exp. (s)       Filter       Magnitude (err)
          17.7                                   300            R            18.7 (0.1)
          17.8                                   300            V            18.7 (0.1)
          17.9                                   300            B            19.4 (0.1)
          18.0                                   300            R            18.8 (0.1)
          18.1                                   300            V            18.8 (0.1)
          18.2                                   300            B            19.5 (0.1)

 The magnitudes were calibrated with the NOMAD1 stars. Further
observations are planned.

We thank the GMG staff, especially W.-M. Yi, H. -Y. Gao and D. -Q.
Wang for performing these observations.


2012-03-27 



zhaoxiaohong78 


GRB_name: GRB120327A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13123
SUBJECT: GRB 120327A: Swift detection of a burst with an optical counterpart
DATE:    12/03/27 03:17:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. Sbarufatti (INAF-OAB/PSU), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
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 02:55:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120327A (trigger=518731).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 246.828, -29.415, which is 
   RA(J2000)  =  16h 27m 19s
   Dec(J2000) = -29d 24' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows 3 main peaks
with a total duration of about 60 sec.  The peak count rate
was ~6500 counts/sec (15-350 keV), at ~38 sec after the trigger. 

The XRT began observing the field at 02:56:32.2 UT, 75.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 246.86308, -29.41514 which
is equivalent to:
   RA(J2000)  = 16h 27m 27.14s
   Dec(J2000) = -29d 24' 54.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 110 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 (1.40 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.9
(+1.51/-1.37) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 5.41e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
140 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 16:27:27.47 = 246.86445
  DEC(J2000) = -29:24:53.8  = -29.41494
with a 90%-confidence error radius of about 0.64 arc sec. This position is 3.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.92 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.34. 

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


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13124
SUBJECT: GRB 120327A: TAROT La Silla observatory optical detection
DATE:    12/03/27 04:03:13 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 120327A detected by SWIFT
(trigger 518731) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 32.40min after the GRB trigger.
The elevation of the field increased from
21 degrees above horizon and weather conditions
were good. Observations cannot begin earlier because
of the presence of the ESO 3.6 meter telescope that
hid the field of view!

We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart mentioned by Sbarufatti
et al. (GCNC 13123).

OT is still at R=17.5 at 45 min after GRB.

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

This message may be cited.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13125
SUBJECT: GRB 120327A: Liverpool Telescope Observations
DATE:    12/03/27 04:16:30 GMT
FROM:    James Smith at ARI,Liverpool John Moors U  <rjs@astro.livjm.ac.uk>

R.J. Smith, Francisco Virgili (Liverpool JMU) report on behalf of the LJMU GRB group:

The 2-m Liverpool Telescope automatically observed Swift GRB 120327A (Sbarufatti et al., GCN Circ. 13123) on March 27, from 03:22:59.1 UT, corresponding to 27.7 minutes after the BAT trigger time. Within the XRT error circle we clearly detect an fading optical source at

  16:27:27.46 , -29:24:54.00 J2000

with an uncertainty of 0.6 arcsec, confirming the observations of Klotz et al (GCN 13124). We estimate the magnitude of the afterglow as follows:

Mid time from    Exp     Filter    Magnitude
GRB (min)        (s)
---------------------------------------------
34.9             10    R        16.1 +/- 0.3
64.5             60    R        17.0 +/- 0.3
---------------------------------------------

Magnitudes are calibrated against nearby USNOB-1 stars.

Observations are continuing.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13126
SUBJECT: GRB 120326A: Maisoncelles Observatory optical observations
DATE:    12/03/27 04:40:33 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Soulier J.-F. (Observatoire de Maisoncelles) reports
the observation of the afterglow of GRB 120326A
19.7 hours after the GRB using a 30cm F/4 telescope
at the Observatoire de Maisoncelles, France (IAU
observatory code is C10).

A CCD camera ST7XME and no filter were
used. A stack of images shows clearly the
presence of the afterglow that confirms the
rebrightening mentioned by Gorosabel et al.
(GCNC 13112):

Tgrb +
start end    Rmag    error
19.7h 20.7h  18.6    0.1

We used the star NOMAD1 1593-0145121
(ra,dec)=(273.9707306,+69.3063278)
as reference R=15.32. Magnitudes are not
corrected for galactic dust extinction.


GRB_name: GRB120327A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13127
SUBJECT: Skynet/PROMPT observations of GRB120327A
DATE:    12/03/27 05:17:36 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 GRB120327A (Sbarufatti et al., GCN 13123) with 
the PROMPT telescopes located at CTIO in Chile beginning ~11 minutes after 
the burst in BVRI. Observations were delayed due to horizon limits. We 
detect a bright, fading afterglow at the location reported by Klotz et al. 
(GCN 13124) in all filters. A preliminary light curve, calibrated to 
nearby USNO B1.0 stars, can be found at:

http://skynet.unc.edu/grb/grb120327a.png

Further observations are ongoing.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13128
SUBJECT: GRB 120327A: REM NIR and optical observations
DATE:    12/03/27 05:28:57 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

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


We imaged the field of GRB120327A (Sbarufatti et al., GCN 13123) with  
the recently
re-aluminized REM telescope located at La Silla.

The optical counterpart also reported in GCN 13124 (Klotz et al.), GCN  
13125 (Smith et al.)
and GCN 13126 (LaCluyze et al.) is well detected both in the optical  
and in the NIR.

The source is detected from about 10 min from the GRB time and  
observations are still in progress.
At 10min after the burst the source was approximately at H=12.69 +-  
0.03, calibrated to 2MASS field stars.


GRB_name: GRB120327A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13129
SUBJECT: GROND observations of GRB 120327A
DATE:    12/03/27 05:31:26 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

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

We observed the field of GRB 120327A (Swift trigger 518731; Sbarufatti et al., GCN #13123) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile).

Observations started at 03:34 UT, 39 minutes min after the GRB trigger, and are continuing. They were performed at an average seeing of 1.6" and at an average airmass of 2.3.

We found a single point source consistent with both the UVOT (Sbarufatti et al, GCN #13123) and Liverpool telescope (Smith et al., GCN #13125) afterglow position.

Based on the second of two 2.4 min of exposures in g'r'i'z' and 4 min in JHK, we estimate preliminary magnitudes (all in AB) at an observations midpoint 03:44 UT of

g' = 18.6 +- 0.1 mag,
r' = 17.5 +- 0.1 mag,
i' = 17.2 +- 0.1 mag,
z' = 17.0 +- 0.1 mag,
J  = 16.3 +- 0.1 mag, and
H  = 15.9 +- 0.1 mag

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.34 mag in the direction of the burst (Schlegel et al. 1998). If this value is correct for the line-of-sight to this GRB, then the substantially reduced g-band flux suggests a redshift around 3.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13130
SUBJECT: GRB 120327A: IAC80 I-band observations
DATE:    12/03/27 06:09:30 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel, A. J. Castro-Tirado (IAA-CSIC, Granada), C. Walker, J. Court, R. Duffy, T. Edwards, M. Herath, J. Kirk, S. Patel, S. Prajs, B. Tunbridge, D. Williams,  R. Wood,  P. Wright, T. Munoz-Darias, C. Knigge, M. Coriat (University of  Southampton) and R. Gimeno (IAC, Tenerife), report:

"We observed the optical counterpart of GRB 120327A (Sbarufatti et al., GCNC 13123) with the 82cm IAC80 telescope at the Observatorio del Teide, Tenerife, Spain. The observations were carried out in the I-band on 04:06 - 05:33 UT (starting 1.12 hours post burst) with a total exposure time of 14x300s. A preliminary  photometry, against the USNO B1.0 catalogue, shows a clear decay from R~18 to R~19.2".


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13131
SUBJECT: GRB120326A: TNT optical observation
DATE:    12/03/27 06:52:51 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 GRB120326A (Siegel et al., GCN Circ. 13105)
with Xinglong TNT telescope in R-band at 20:47:11.734 (UT),  19.45 hours after 
the burst. The optical counterpart (e.g. Klotz et al. GCN Cir 13107) 
was clearly detected with a brightness of 18.56 mag relatively to USNO B1.0 R2 mag 

Further observations are planed.

This message may be cited.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org:8080/grb/index.html

We thank Liang Ma for performing these observations.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13132
SUBJECT: GRB 120327A: TAROT La Silla observatory optical decay
DATE:    12/03/27 07:04:56 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We continue observations of GRB 120327A (trigger 518731)
with the TAROT robotic telescope (D=25cm) located at the
European Southern Observatory, La Silla observatory, Chile.

An optical decay alpha=1.3 (+/- 0.3) is deduced from the
following observations:

No filter:
start  end     Rmag  dmag filter
(sec)  (sec)
1944.2 2234.6  16.96 0.17 CR
2387.2 3159.2  17.31 0.19 CR
3169.5 3938.0  17.81 0.09 CR
4156.0 4916.2  18.03 0.17 CR
4926.5 6102.7  18.84 0.13 CR

R filter:
start   end     Rmag  dmag filter
(sec)   (sec)
2767.6  3539.5  17.65 0.09 R
3948.0  4716.3  18.34 0.32 R
5116.5  7072.8  18.56 0.17 R
7472.9 10018.6  18.84 0.09 R

Photometry is relative to the star NOMAD1 0605-0398765:
(ra,dec) J2000 = (246.8438328,-29.4187269) R=14.930.
Magnitudes are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB120327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13133
SUBJECT: GRB 120327A: Gemini-South redshift
DATE:    12/03/27 07:35:33 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and N. R. Tanvir (U. Leicester) report on behalf 
of a larger collaboration:

On March 27 starting at 06:01 UT (186 minutes after the BAT trigger) we 
began spectroscopic observations of the optical afterglow of GRB 120327A 
(Sbarufatti et al., GCN 13123) using GMOS-South on the Gemini-South 8-m 
telescope.  We acquired four exposures of 800s each using the B600 
grating, with wavelength coverage between 3865-6680 Angstroms.

In the reduced spectrum we identify a strong damped Lyman-alpha system 
at z=2.81 as well as numerous narrow absorption lines corresponding to 
(among others) CIV, CII, OI, SiII at the same redshift, as well as 
possible Lyman-beta.   We therefore identify this as the redshift of the 
GRB.

We thank German Gimeno and the Gemini staff for prompt execution of the 
observations.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13134
SUBJECT: GRB 120327A: X-shooter redshift 
DATE:    12/03/27 07:38:40 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler, J. P. U Fynbo, B. Milvang-Jensen (all DARK), N. Tanvir (U. Leicester) and P. Jakobsson (U. Iceland) report on behalf of a larger collaboration.

We observed the optical/NIR afterglow (e.g., Sbarufatti et al., GCN# 13123, Klotz et al., GCN#13124, Smith et al., GCN#13125) of the Swift GRB 120327A (Sbarufatti et al., GCN# 13123) with the VLT/UT2 equipped with the X-shooter spectrograph. Observations started around 05:03 UT on 2012-03-27, which is roughly 2.13 hrs after the trigger. Four exposures in a nodding pattern with an integration time of 600 s each were obtained. The spectrum covers an approximate wavelength range between 3100 and 23000 AA. The slit width was set to 1" in the ultra-violet/blue arm, and 0.9" in the visual and near-infrared arm, resulting in a resolving power range of approximately 4500-7500.

Preliminary reduction of the spectrum shows a well detected continuum with several absorption features, that we identify with Ly-limit and Ly-alpha as well as absorption lines of CII/CII*, SiII/SiII*, AlI, FeII and MgII at a redshift of 2.813. This is confirms previous reports based on spectroscopy (Perley & Tanvir, GCN #13133) and photometry (Sudilovsky et al. GCN #13129).

We are grateful for the excellent support from the Paranal Observatory staff, in particular Dimitri Gadotti. We acknowledge private communication with the GROND team, in particular Vlad Sudilovsky.


GRB_name: GRB120327A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13135
SUBJECT: GRB 120327A: Enhanced Swift-XRT position
DATE:    12/03/27 08:14:58 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 1105 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120327A, 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 = 246.86448, -29.41491 which is equivalent
to:

RA (J2000): 16h 27m 27.47s
Dec (J2000): -29d 24' 53.7"

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: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13136
SUBJECT: GRB 120326A : SMA submm observation
DATE:    12/03/27 10:37:17 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Y. Urata (NCU), K.Y. Huang, S. Takahashi (ASIAA), G. Petitpas (SMA)
on behalf of EAFON

We observed the field of GRB120326A(GCN 13105) using Sub-Millimeter
Array (SMA). The observation in 219 GHz was started at 2012 Mar 26,
10:15 and ended at 21:10 (UT).  Our preliminary analysis shows a radio
counterpart at the position of optical afterglow(GCN 13107, 13109, 13111). 
The averaged flux density during the observation is 3.1 +/- 0.5 mJy.

Further detail analysis and monitoring are ongoing.


GRB_name: GRB120327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13137
SUBJECT: GRB 120327A: Swift-BAT refined analysis
DATE:    12/03/27 12:22:18 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), B. Sbarufatti (INAF-OAB/PSU),
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 120327A (trigger #518731)
(Sbarufatti, et al., GCN Circ. 12123).  The BAT ground-calculated position is
RA, Dec = 246.854, -29.415 deg, which is 
   RA(J2000)  =  16h 27m 25.0s 
   Dec(J2000) = -29d 24' 55.5" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.
 
The mask-weighted light curve shows 3 main peaks (two weak peaks, then the
main peak).  The first starts at ~T-25 sec, peaks at ~T+2 sec;  and the second
peaks at ~T+18 sec.  The main peak starts at ~T+30 sec, peaks at ~T+37 sec,
and returns to baseline at ~T+180 sec.  T90 (15-350 keV) is 62.9 +- 7.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-15.79 to T+74.58 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.06.  The fluence in the 15-150 keV band is 3.6 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+37.09 sec in the 15-150 keV band
is 3.9 +- 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/518731/BA/


GRB_name: GRB120327A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13138
SUBJECT: GRB 120327A: Swift/UVOT further analysis
DATE:    12/03/27 12:50:38 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and B. Sbarufatti (INAF-OAB/PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120327A
141 s after the BAT trigger (Sbarufatti et al., GCN Circ. 13123).
A source consistent with the enhanced XRT position (Osborne et al.
GCN Circ. 13135) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  16:27:27.48  = 246.864500 (deg.)
   Dec (J2000) = -29:24:53.74  = -29.414928 (deg.)
with an estimated uncertainty of 0.48 arc sec. (radius, 90% confidence).

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

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

v                  448          468           20         15.68 +/- 0.10
b                  396          416           20         16.97 +/- 0.11
u                  141          391          246         18.02 +/- 0.08
w1                 497         1295           97        >19.0
m2                 622         1271           78        >19.2
w2                 424         1222           97        >19.6

The absence of detection in uvw1, uvm2, and uvw2 is consistent with the
reported redshift of 2.81 (Perley & Tanvir, GCN Circ 13133, and
Krueler et al, GCN Circ. 13134).

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.34 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13139
SUBJECT: GRB 120326A: LOAO R-band Observations
DATE:    12/03/27 13:20:38 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

M. Jang, M. Im, (SNU), & Y. Urata (NCU) on behalf of EAFON

We observed GRB 120326A (120326A et al., GCN 13105)
in R-band with a 1 m telescope at Mt. Lemmon, Arizona, U.S.
The obsevation started at 09:06:33 2012-03-26 UT, ~ 8 hours
after the burst alert.

We totally took 6 frames with 300 sec of exposure time and found
a bright optical afterglow in each frame (Im et al. GCN 13117,
Klotz et al. GCN 13107, Guidorzi et al. GCN 13111, Walker et al. GCN 13112,
Dintinjana et al. GCN 13113, Kuin et al. GCN 13114).
Preliminary photometry values are shown below. The R magnitudes were calibrated
with three nearby USNO B1.0 stars, USNO-B1.0 1592-0143334, 1592-0143322,
and 1592-0143349

Mid-time[sec] R-mag   Err
================================
27639    17.63   0.06
27964    17.53   0.04
28282    17.61   0.04
28601    17.84   0.03
28915    17.90   0.03
29239    18.08   0.03

We thank the LOAO operator, I. Baek for her assistance with this observation.


GRB_name: GRB120327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13140
SUBJECT: GRB 120327A: CQUEAN grizY Observation
DATE:    12/03/27 14:11:30 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Jae-Woo Kim, and Duho Kim (CEOU/Seoul National Univ.)

We observed GRB 120327A (Sbarufatti et al., GCN 13123) in
g,r,i,z,Y filters using CQUEAN camera on the 2.1m Otto-Struve
telescope at McDonald Observatory, Texas, US.

The observation started at 2012-03-27 11:00:08 UT,
or about 8 hours after the BAT alert.
In all of the g,r,i,z,Y-band images taken with 300 sec
exposure each, we identify the afterglow (r ~ 20 AB mag)
which was reported earlier by several groups
(Klotz et al. GCN 13124, Smith et al. GCN 13125,
Soulier et al. GCN 13126, LaCluyze et al. GCN 13127,
Covino et al. GCN 13128,Sudilovsky et al. GCN 13129,
Grosabel et al. GCN 13130).

Further observations are planned.


GRB_name: GRB120327A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13141
SUBJECT: GRB 120327A: Swift-XRT refined Analysis
DATE:    12/03/27 16:17:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 7.3 ks of XRT data for GRB 120327A (Sbarufatti  et al.
GCN Circ. 13123), from 66 s to 0 s after the  BAT trigger. The data
comprise 267 s in Windowed Timing (WT) mode (the first 7 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 13135).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.95 (+0.10, -0.11). At T+217 s  the decay
flattens to an alpha of 0.62 (+0.09, -0.13) before breaking again at
T+2540 s to a final decay with index alpha=1.42 (+0.13, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.98 (+/-0.08). The
best-fitting absorption column is  1.5 (+0.5, -0.4) x 10^22 cm^-2, at a
redshift of 2.81, in addition to the Galactic value of 1.4 x 10^21
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 1.79 (+0.11, -0.10) and a best-fitting absorption column of 1.5
(+0.8, -0.7) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum  is 4.4 x 10^-11
(5.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.4 x 10^21 cm^-2
Intrinsic column:    1.5 (+0.8, -0.7) x 10^22 cm^-2 at z=2.81
Photon index:      1.79 (+0.11, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00518731.

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


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13142
SUBJECT: Subject:GRB 120326A: Bassano Bresciano Observatory optical observations
DATE:    12/03/27 17:05:07 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

We imaged the field of GRB 120326A detected by SWIFT
(trigger 518626) Goad et al (GCNC 13110), with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory (member of ISSP), Italy.

The observations had started 19h 58m and ended 26h 08m  after the 
GRB trigger,with our schmidt telescope D=320 mm F/D=3.1.

Weather conditions were good.

We co-added some series of 20 exposures of 120s takings for the 
whole night between 26 and 27 March 2012.

We detected clearly the presence of the optical couterpart 
(e.g. Klotz et al. GCNC 13107) that confirms the rebrightening 
mentioned by Gorosabel et al.(GCNC 13112), 
at the following position: 

RA (J2000) =  18 15 37.19 
DEC(J2000) = +69 15 35.5

The CCD unfiltered magnitude during all through the 
observations has been 18.7 (+/- 0.2)
The magnitude has nearly been constant during 
this period.

Magnitudes were estimated with the UCAC-3 
catalog and are not corrected for galactic 
dust extinction.

Lightcurve analisis is in progress, 
further observations are planed.

This message may be cited.


GRB_name: GRB120326A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13143
SUBJECT: GRB 120326A: PAIRITEL NIR Observations
DATE:    12/03/27 18:22:24 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 120326A (Siegel et al., GCN 13105) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2012-03-27 09:25:19 UT, ~32.1 hours after the Swift Trigger.  In  mosaics
(effective exposure time of 1.31 hours) taken simultaneously in the J, H,
and Ks filters, we detect a source at the optical afterglow location (Klotz
et al., GCN 13107; LaCluyze et al., GCN 13109; Guidorzi et al., GCN 13111;
Walker et al., GCN 13112; Kuin et al., GCN 13114; Im et al., GCN 13117;
Hentunen et al., GCN 13119; Urata et al., GCN 13121; Zhao et al., GCN
13122; Soulier, GCN 13126; Jang et al., GCN 13139; Quadri et al., GCN
13142).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
33.58      1.31     J     17.5   0.1
33.58      1.31     H     16.7   0.1
33.58      1.31     Ks    16.0   0.2

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


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13144
SUBJECT: GRB 120327A afterglow detection
DATE:    12/03/27 20:48:42 GMT
FROM:    Petr Kubanek at AIO  <pkubanek@gmail.com>

S. Meehan, L. Hanlon, M. Topinka (UCD Dublin), P. Kubanek (FZU AV CR
Prague), report on behalf of a large collaboration:

We imaged the field of GRB 120327A detected by SWIFT (trigger 518731)
with the Watcher robotic telescope (D=40cm) located at Boyden
Observatory, Bloemfontein, South Africa.

Our first good observation was 14.4 min after the GRB trigger, 3 min
after receipt of the GCN notice. The source was close to the zenith
with an airmass of 1.01. 

We detect a fading source in the error box given by SWIFT, which
coincides with candidate counterpart mentioned by Sbarufatti et al.
(GCN 13123).

The optical transient was measured at 15.5 +/- 0.1 mag @ 14.4 minutes
after the trigger in the clear filter.  

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

Analysis of the remaining images is on-going.


GRB_name: GRB120326A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13145
SUBJECT: GRB 120326A: Fermi GBM Observation
DATE:    12/03/27 21:47:34 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 01:20:31.51 UT on March 26, 2012, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 120326A (trigger 354417633 / 120326056) which was
triggered and detected by Swift (Siegel et al., GCN 13105).
The on-ground calculated location, using the Fermi GBM trigger data,
is consistent with the locations seen by Swift.

The GBM light curve shows a single FRED-like event with a 
duration (T90) of about 12 s (50-300 keV). 
The time-averaged spectrum from T0-3.584 to T0+13.824 s
is fit equally well by a Band and Comptonized Power Law function.

For the Band function, the parameters are: 
Epeak = 46.45 +/- 3.67 keV, alpha = -0.98 +/- 0.14, and beta = -2.53 +/- 0.15.
This results in a 1-s peak flux of 3.10 +/- 0.05 ph/s-cm^2 and a
yields a fluence (10-1000 keV) in this time interval 
of (3.539 +/- 0.174)E-06 erg/cm^2.  The C-Stat for this fit is
653.15 over 489 degrees of freedom.

For the Comptonized function, the parameters are: 
Epeak = 55.46 +/- 2.61 keV, and alpha = -1.21 +/- 0.08.
This results in a 1-s peak flux of 3.08 +/- 0.05 ph/s-cm^2.
Which yields a fluence (10-1000 kev) in this time interval of
(3.027 +/- 0.091)E-06 erg/s-cm^2.  The C-Stat for this fit is
654.83 over 490 degrees of freedom.

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


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13146
SUBJECT: GRB 120327A: GTC redshift confirmation
DATE:    12/03/27 21:59:50 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

R. Snchez-Ramrez, J. Gorosabel, A. J. Castro-Tirado (IAA-CSIC Granada),
M. A. Rivero and G. Gmez-Velarde (GTC La Palma), on behalf of a larger
collaboration, report:

"Following the detection of the optical afterglow to GRB 120327A
(Sbarufatti et al. GCNC 13123), we have taken three spectra (400s each)
with the 10.4m GTC (+ OSIRIS) at the Spanish Observatorio del Roque de los
Muchachos (La Palma). The spectra, covering the range 3800-7800 A were
taken starting 2.33 hr post burst, and reveal a strong damped Ly-alpha
system besides several absorption features, including SiIV, SiII, CIV,
FeII, AlII (and others) at a common redshift of 2.813, consistent with the
value reported by Perley and Tanvir (GCNC 13133) and Kruehler et al.
(GCNC 13134)."

This message can be quoted.


GRB_name: GRB120328A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13147
SUBJECT: GRB 120328A: Swift detection of a burst
DATE:    12/03/28 03:19:16 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. Pagani (U Leicester), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
A. Y. Lien (NASA/GSFC/ORAU), O. M. Littlejohns (U Leicester),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), M. Stamatikos (OSU/NASA/GSFC),
C. A. Swenson (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report
on behalf of the Swift Team:

At 03:06:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120328A (trigger=518792).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 241.550, -39.340 which is 
   RA(J2000) = 16h 06m 12s
   Dec(J2000) = -39d 20' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with broad peak preceding a shorter spike for a 
total duration of about 20 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 03:07:27.2 UT, 68.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 241.61294,
-39.33664 which is equivalent to:
   RA(J2000)  = 16h 06m 27.11s
   Dec(J2000) = -39d 20' 11.9"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 175 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 (1.61 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.5
(+0.62/-0.52) x 10^22 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.53e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 78 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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
0.73. 

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: GRB120328A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13148
SUBJECT: Skynet/PROMPT observations of GRB120328A
DATE:    12/03/28 03:39:28 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

J. Haislip, A. LaCluyze, K. Ivarsen, D. Reichart, J. Moore, H. T. 
Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. 
Speckhard, A.Trotter, and J. A. Crain report:

Skynet observed the field of GRB120328A (Pagani et al., GCN 13147, Swift 
trigger #518792) with the PROMPT telescopes located at CTIO in Chile 
beginning 4.1 minutes after the burst. We do not detect any uncatalogued 
sources in our earliest images (mean time 4.43 minutes after the burst) 
down to 3-sigma limiting magnitudes of V=17.92, R=18.73, I=18.15. 
Stacking all data taken up to 17.2 minutes after the burst yields 3-sigma 
limiting magnitudes of B=19.19, V=19.75, R=20.26, I=19.38. Limits were 
calibrated to nearby USNO-B1.0 stars for B,R,I, and nearby NOMAD stars for 
V.


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13149
SUBJECT: GRB 120326A: Xinglong TNT further optical observation
DATE:    12/03/28 04:52:23 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 reobserve GRB120326A (Siegel et al., GCN Circ. 13105)
with Xinglong TNT telescope in R-band at 20:30:50.7 (UT), Mar. 28th 2012.  
43.7 hours after  the burst.  The optical counterpart (e.g. Klotz et al. GCN Cir 13107) 
was still clearly detected with a brightness of R=19.32 mag, relatively to  USNO B1.0 R2 mag. 
Comparing to the observation last time (Xin et al. GCN Cir. 13131),
the brightness decayed by a magnitude of 0.76 mag during these two epoch.

Further observations are planed.

This message may be cited.

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.




xlp@bao.ac.cn


GRB_name: GRB120326A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13150
SUBJECT: GRB 120326A: Xinglong TNT further optical observationcorrection for GCN Cir 13149)
DATE:    12/03/28 05:00:57 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 reobserve GRB120326A (Siegel et al., GCN Circ. 13105)
with Xinglong TNT telescope in R-band at 20:30:50.7 (UT), Mar. 27th 2012.  
43.7 hours after  the burst.  The optical counterpart (e.g. Klotz et al. GCN Cir 13107) 
was still clearly detected with a brightness of R=19.32 mag, relatively to  USNO B1.0 R2 mag. 
Comparing to the observation last time (Xin et al. GCN Cir. 13131),
the brightness decayed by a magnitude of 0.76 mag during these two epoch.

Further observations are planed.

This message may be cited.

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: GRB120328A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13151
SUBJECT: GRB 120328A: TAROT La Silla observatory optical observations
DATE:    12/03/28 05:19:00 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 120328A detected by SWIFT
(trigger 518792) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 345.7s after the GRB trigger.
The elevation of the field increased from
26 degrees above horizon and weather conditions
were good.

Images are unfiltered. We do not detect any OT with
a limiting magnitude of:

t0+345.7s to t0+405.7s : R > 18.5

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=339.0212 lat= +9.5155
and the galactic extinction in R band is ~2 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13152
SUBJECT: GRB 120327A: NOT optical observations
DATE:    12/03/28 05:38:24 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI), Johan P. U. Fynbo (DARK/NBI), Pall 
Jakobsson (Univ. Iceland), Jens Jessen-Hansen (NOT and Univ. Aarhus), 
Jyri Lehtinen (NOT and Univ. Helsinki), report:

We observed the optical afterglow of GRB 120327A (Sbarufatti et al., GCN 
13123) with the NOT equipped with ALFOSC in imaging mode. Observations 
were carried out in the R band, for a total exposure time of 30 min, 
with a seeing of 1.2".

The optical afterglow is well detected in our images taken at a mean 
epoch of March 28.164 UT (1.05 days after the GRB), with a magnitude R = 
21.8+-0.16 calibrated against nearby USNO-B1 stars (R1 magnitudes).

This value is in fair agreement with the extrapolation of the R-band 
data reported in the literature (LaCluyze et al., GCN 13127; Klotz et 
al., GCNs 13124, 13132; Sudilovsky et al., GCN 13129; Gorosabel et al., 
GCN 13130; Im et al., GCN 13140; Meehan et al., GCN 13144). The 
afterglow has faded following a single power-law decay with slope alpha 
= 1.3 between 12 min and 1 day after the GRB, though small-scale 
variability may be present (see also LaCluyze et al., GCN 13127).


GRB_name: GRB120328A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13153
SUBJECT: GRB 120328A: Enhanced Swift-XRT position
DATE:    12/03/28 06:12:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 763 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120328A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 241.61376, -39.33565 which is equivalent
to:

RA (J2000): 16h 06m 27.30s
Dec (J2000): -39d 20' 08.3"

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: GRB120328A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13154
SUBJECT: GRB 120328A: Swift-BAT refined analysis
DATE:    12/03/28 12:17:01 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), C. Pagani (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120328A (trigger #518792)
(Pagani, et al., GCN Circ. 13147).  The BAT ground-calculated position is
RA, Dec = 241.607, -39.322 deg, which is 
   RA(J2000)  =  16h 06m 25.8s 
   Dec(J2000) = -39d 19' 20.8" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows two overlapping peaks.  The first starts
at ~T-20 sec, peaks at ~T+0; the second peaks at ~T+8 sec and ends at ~T+20 sec.
T90 (15-350 keV) is 24.2 +- 6.7 sec (estimated error including systematics).
 
The time-averaged spectrum from T-17.27 to T+20.61 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.87 +- 0.20.  The fluence in the 15-150 keV band is 4.7 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.11 sec in the 15-150 keV band
is 0.7 +- 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/518792/BA/


GRB_name: GRB120326A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13155
SUBJECT: GRB 120326A: MITSuME Ishigakijima Optical Observation
DATE:    12/03/28 14:19:34 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 120326A (Siegel et al., GCNC 13105)
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 2012-03-27 16:59:18 UT (~1.65 days after the
burst). We detected the previously reported afterglow (Klotz et al.,
GCNC 13107; Guidorzi, GCNC 13111) in g' and Rc bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err  Rc  Rc_err   Ic
----------------------------------------------------------------------
1.68494    17:46:48    960.0     20.3  0.2   19.9  0.2   >18.93
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120327A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13156
SUBJECT: GRB 120327A: MITSuME Ishigakijima Optical Observation
DATE:    12/03/28 14:21:01 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 120327A (Sbarufatti et al., GCNC 13123)
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 2012-03-27 19:19:59 UT (~16.4 h after the
burst). We detected the previously reported afterglow (Klotz et al.,
GCNC 13124; Smith et al., GCNC 13125) in Rc and Ic bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'    Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.70335    19:48:05   2640.0    >21.3  20.3  0.1    19.7  0.3
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120328B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13157
SUBJECT: IPN Triangulation of GRB 120328B (long/intense)
DATE:    12/03/28 15:05:38 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

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

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

The long-duration, intense GRB 120328B has been observed by Fermi (GBM: 
trigger 354608782), Konus-Wind, MESSENGER (GRNS), INTEGRAL (SPI-ACS), 
Swift (BAT), and AGILE (MCAL), so far, at about 23181 s UT (06:26:21). 
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:
   229.038 (15h 16m 09s) +25.299 (+25d 17' 58")
  Corners:
   227.666 (15h 10m 40s) +28.399 (+28d 23' 55")
   228.177 (15h 12m 43s) +28.152 (+28d 09' 05")
   230.230 (15h 20m 55s) +22.104 (+22d 06' 15")
   229.765 (15h 19m 04s) +22.401 (+22d 24' 05")
  ---------------------------------------------
The error box area is 2.15  sq. deg, and its maximum
dimension is 6.7 deg.

This box can be improved.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120328_T23186/IPN/


GRB_name: GRB120328B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13158
SUBJECT: Konus-Wind observation of GRB 120328B
DATE:    12/03/28 15:07:31 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 120328B
(IPN localization: Hurley at al., GCN 13157)
triggered Konus-Wind at T0=23186.645s UT (06:26:26.645)

The light curve shows two main overlapping pulses
which peaks are separated by ~15 s.
A total burst duration of the burst ~50 s.
The emission is seen up to ~8 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120328_T23186/

As observed by Konus-Wind the burst
had a fluence of (1.2  0.1)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+4.352 s,
of (1.5  0.2)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+50.176 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.08 (-0.07, +0.07),
the high energy photon index beta = -2.2 (-0.2, +0.1),
the peak energy Ep = 267(-30, +36) keV,
chi2 = 111/86 dof.

The spectrum at the maximum count rate
(measured from T0+0.256s to T0+4.864 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 = -0.59 (-0.11, +0.09),
the high energy photon index beta = -2.2 (-0.2, +0.1),
the peak energy Ep = 430(-54, +66) keV,
chi2 = 90.4/82 dof.

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


GRB_name: GRB120328A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13159
SUBJECT: GRB 120328A: Swift-XRT refined Analysis
DATE:    12/03/28 15:19:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 9.0 ks of XRT data for GRB 120328A (Pagani  et al. GCN
Circ. 13147), from 62 s to 34.2 ks after the  BAT trigger. The data
comprise 139 s in Windowed Timing (WT) mode (the first 5 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 13153).

The late-time light curve (from T0+4.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.98 (+0.22, -0.20).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+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 1.6 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 3.0 (+0.5, -0.4) and
a best-fitting absorption column of 1.9 (+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 4.7 x 10^-11 (3.9 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+0.5, -0.4) x 10^22 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: 6.9 sigma
Photon index:      3.0 (+0.5, -0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00518792.

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


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13160
SUBJECT: GRB 120326A: Bassano Bresciano Observatory further optical observations
DATE:    12/03/28 15:32:32 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

We reobserved GRB120326A (see GCNC 13142)
with the robotic telescope of (IAU station 565) Bassano Bresciano 
Observatory (member of ISSP), Italy. 

We began on 2012/03/27.988 - 46.4 hours after  the burst.  
and finished on 2012/03/28.117 - 49.5 hours after  the burst.

We co-added a series of 80 exposures (120s each) takings for
whole night between 27 and 28 March 2012.

The afterglow was still detected. Unfiltered magnitude was decreasing 
from  19.1 (+/-0.1) to 19.7 (+/-0.1) during this period.

Weather conditions were good.

Magnitudes were estimated with the UCAC-3 
catalog and are not corrected for galactic 
dust extinction.

Lightcurve analisis is in progress, 
further observations are planed.

This message may be cited.


GRB_name: GRB120328A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13161
SUBJECT: GRB 120328A: Swift/UVOT Upper Limits
DATE:    12/03/28 16:02:39 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (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 120328A
78 s after the BAT trigger (Pagani et al., GCN Circ. 13147).  No optical
afterglow consistent with the enhanced XRT position (Beardmore el al.,
GCN Circ. 13153) 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            78          228          147         >20.6
u_FC               290          540          246         >19.6
white               78          764          186         >20.5
v                  621          813           39         >18.2
b                  547          739           39         >19.1
u                  290          715          265         >19.8
w1                 670          862           39         >18.9
w2                 769          789           20         >18.6

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 0.73 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120328B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13162
SUBJECT: long/intense GRB 120328B: MASTER follow up observations 
DATE:    12/03/28 16:26:33 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 
Tunka was started to survey IPN error box of the long/intense  GRB 120328B 
(Hurley et al., GCN Circ 13157)  6 hours after GRB time at 2012-03-28 13:26:23 UT.
The eroor box was arised. The weather was changed. The better images limit 
was about 18 unfiltered magnitudes.

There is no OT inside IPN error box with 18 mag limit.

MASTER-Tunka auto-detection system discovered faint OT source (4.1 sigma) 
at (RA, Dec) = 15h 06m 01.01s +28d 41m 59.8s on 2012-03-28.59161 UT (~7h45 
min after GRB time)  outside error IPN box (see map 
http://observ.pereplet.ru/images/GRB120328B_IPN_map_MASTER$ 
GRB120328B_IPN_map_MASTER.png ).
The OT unfiltered magnitude is 17.9m (limit 18.0m).

The OT is marginally seen at several images 2 images. There is no minor 
planet at this place.

There is no known source at this place.

We have reference image without OT on 2011-06-04.67172 UT with unfiltered 
magnitude limit 20.1m.

Follow up observations will be continuated.

The discovery and reference images are available at:
http://master.sai.msu.ru/static/OT/150601.01284159.8.png


The message may be cited.


GRB_name: GRB120328B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13163
SUBJECT: GRB 120328B: Fermi GBM detection
DATE:    12/03/28 19:55:22 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (UCD)
reports on behalf of the Fermi GBM Team:

"At 06:26:20.95 UT on 28 March 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120328B (trigger 354608782 / 120328268).
The GBM on-ground location is consistent with the IPN error box
(Hurley at al., GCN 13157).

The angle from the Fermi LAT boresight is 69 degrees.

The GBM light curve consists of two main pulses
with a duration (T90) of about 30.5 s (50-300 keV).
The time-averaged spectrum from T0+3.072 s to T0+34.816 s is
best fit by a Band function with Epeak = 177.90 (+4.35/-4.16) keV,
alpha = -0.75 +/-0.02, and beta = -2.00 +/-0.02
(CSTAT 1669.1 for 721 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(7.74 +/- 0.02)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.95 s in the 10-1000 keV band
is 33.5 +/- 0.4 ph/s/cm^2.


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


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13164
SUBJECT: GRB 120327A: Zadko optical observations
DATE:    12/03/28 21:29:19 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (ASDC/INAF-OAR), M. Boer (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA) report:

We imaged the field of GRB 120327A detected by SWIFT
(trigger 518731) with the Zadko robotic telescope (D=100cm)
located at Gingin observatory, Australia.

The observations started 41 hours after the GRB trigger.
Weather conditions were excellent.

The optical transcient (Sbarufatti et al. GCNC 13123)
is detected very close to the limiting magnitude
of a co addition of images obtained with no filter.

start   end     Rmag  dmag filter
(day) (day)
1.73   1.75     22.0  0.3  CR

Magnitude was estimated with the nearby star
NOMAD1 0605-0398765 (246.8438328 -29.4187269)
using R=14.930.


GRB_name: GRB120328B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13165
SUBJECT: GRB 120328B: Fermi-LAT Observations
DATE:    12/03/28 23:43:31 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G.Vianello (CIFS/SLAC), V. Vasileiou (CNRS/IN2P3/LUPM), D.Kocevski
(Stanford) report on behalf of the Fermi LAT Team:

Fermi-LAT has detected high energy emission from GRB 120328B in ground
analysis. The GRB was triggered on by Fermi-GBM at 06:26:20 on March
28, 2012 (trigger 354608782, GCN 13163), and by Konus-Wind (GCN
13158).

The best available position, provided by the IPN (GCN 13157), is ~66
deg off-axis, outside of the Fermi/LAT nominal field of view for the
standard data analysis. Moreover, the zenith angle is ~105 deg, well
within the region strongly contaminated by gamma-ray emission from the
Earth's limb.

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 during the time interval of the
prompt emission between T0 and ~T0+30 s. The significance of the
excess corresponds to ~8 sigma. This data selection has insufficient
spatial resolution to provide a reliable LAT localization.

The GRB position entered the nominal field of view of the LAT ~2200 s
after the trigger. A standard likelihood analysis on the time interval
T0+2200 s - T0+3500 s does not show any excess at the position of the
GRB.

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


GRB_name: GRB120327A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13169
SUBJECT: GRB 120327A: MITSuME Ishigakijima Optical Upper Limits at 1 day afterthe burst
DATE:    12/03/29 14:06:52 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 120327A (Sbarufatti et al., GCNC 13123)
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 2012-03-28 17:27:54 UT (~1.61 days after the
burst). We could not detect the previously reported afterglow
(Klotz et al., GCNC 13124; Smith et al., GCNC 13125; Kuroda et al.,
GCNC 13156) 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
----------------------------------------------------------------------
1.62756    17:58:57   1500.0    >20.5  >20.2  >19.0
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120326A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13170
SUBJECT: GRB 120326A: MITSuME Ishigakijima Optical Observation at 2 days afterthe burst
DATE:    12/03/29 14:07:35 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 120326A (Siegel et al., GCNC 13105)
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 2012-03-28 15:12:13 UT (~2.58 days after the
burst). We detected the previously reported afterglow (Klotz et al.,
GCNC 13107; Guidorzi, GCNC 13111; Kuroda et al., GCNC 13155) in g' and Rc
bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err  Rc  Rc_err   Ic
----------------------------------------------------------------------
2.61348    16:03:53   1620.0     20.0  0.2   20.1  0.2   >18.9
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120328A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13171
SUBJECT: GRB 120328A: MITSuME Ishigakijima Optical Upper Limits
DATE:    12/03/29 14:08:13 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 120328A (Pagani et al., GCNC 13147)
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 2012-03-28 18:34:18 UT (~15.5 h after the
burst). We did not find any new point source within the enhanced XRT error
circle (Beardmore et al., GCNC 13153) 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
----------------------------------------------------------------------
0.68772    19:36:38   4800.0    >20.1  >20.4  >19.3
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13172
SUBJECT: GRB 120326A: Bassano Bresciano Observatory optical observations
DATE:    12/03/29 15:10:35 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

We imaged the field of GRB 120326A detected by SWIFT
(trigger 518626) Goad et al (GCNC 13110), with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory (member of ISSP), Italy.

The observations had started 19h 58m and ended 26h 08m  after the 
GRB trigger,with our schmidt telescope D=320 mm F/D=3.1.

Weather conditions were good.

We co-added some series of 20 exposures of 120s takings for the 
whole night between 26 and 27 March 2012.

We detected clearly the presence of the optical couterpart 
(e.g. Klotz et al. GCNC 13107) that confirms the rebrightening 
mentioned by Gorosabel et al.(GCNC 13112), 
at the following position: 

RA (J2000) =  18 15 37.19 
DEC(J2000) = +69 15 35.5

The CCD unfiltered magnitude during all through the 
observations has been 18.7 (+/- 0.2)
The magnitude has nearly been constant during 
this period.

Magnitudes were estimated with the UCAC-3 
catalog and are not corrected for galactic 
dust extinction.

Lightcurve analisis is in progress, 
further observations are planed.

This message may be cited.


GRB_name: GRB120324A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13174
SUBJECT: GRB 120324A, the review of the sky area in plate archives
DATE:    12/03/30 18:01:07 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120324A (P.A. Evans et al. GCN Circ.13093) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19880831/190518 GUA040C001326A 16.0 14.55 1125-12506783
19890803/201455 GUA040C001494A 16.0 15.65 1125-12498949
19890803/204023 GUA040C001495 16.0 15.65 1125-12498949
19910807/205429 GUA040C001847 16.0 16.40 1125-12498743
Plates:  the plates archive identifier of DWA (D/F=400/2000, 
GUA040C  M=103"/mm) of the Ukrainian NAS Main Astro obs.
         (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 24 minutes area around 
       the location given in P.A. Evans et al. GCN Circ.13093: 
       RA(J2000)= 19h 24m 18.90s, Dec(J2000)= +24d 07' 46.5"
Star USNOA2 - Comparison star.
  The preview images of 4 areas together with  
the 24x24 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120324A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13175
SUBJECT: GRB 120326A: CARMA 3mm detection
DATE:    12/03/31 01:42:24 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), K. Alatalo (UCB), and A. Horesh (Caltech) report:

We observed the position of GRB 120326A (Siegel et al., GCN 13105) with 
the Combined Array for Research in Millimeter-Wave Astronomy (CARMA) at 
a frequency of 92.5 GHz (3 mm) between 13:33 and 15:19 UT on 2012-03-30. 
  A bright point source is observed consistent with the X-ray and 
optical positions (Goad et al., GCN 13110; Klotz et al., GCN 13107; 
Guidorzi et al., GCN 13111), at (J2000):

18:15:37.14  +69:15:35.07  (+/- 0.4")

We measure a flux density of 3.2 +/- 0.4 mJy at the mean time of t = 
4.55 days after the GRB trigger.


GRB_name: GRB120326A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13176
SUBJECT: GRB 120326A : Suzaku WAM observation of the prompt emission
DATE:    12/03/31 06:18:03 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 120326A (Swift/BAT trigger #518626 ; Siegel et al., GCN
13105) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 01:20:31.907 UT (=T0).

The observed light curve shows a single peak starting at T0-5 s, ending
at T0+10 s, with a duration (T90) of about 9 seconds. The fluence in 100
- 1000 keV was 1.61(+/-0.26) x 10^-6 erg/cm^2. The 1-s peak flux 
measured from T0+3 s was 0.61(-0.44, +0.40) photons/cm^2/s in the same 
energy range.

Preliminary result shows that the time-averaged spectrum from T0-5 s to
T0+10 s is well fitted by a single power-law with a photon index of 2.14
(-0.31, 0.45) (chi2/d.o.f = 11.1/14).

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

The light curves for this burst will be available at:

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


GRB_name: GRB120326A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13177
SUBJECT: GRB 120326A: MITSuME Ishigakijima Optical Observation at 3 days afterthe burst
DATE:    12/03/31 10:23:14 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 120326A (Siegel et al., GCNC 13105)
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 2012-03-29 17:40:10 UT (~3.68 days after the
burst). We detected the previously reported afterglow (Klotz et al.,
GCNC 13107; Guidorzi, GCNC 13111; Kuroda et al., GCNC 13155, 13170)
in all the three bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err  Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
3.71188    18:25:35   4320.0     20.9  0.2   20.8  0.2    19.7  0.3
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13178
SUBJECT: GRB 120326A: Bassano Bresciano Observatory lightcurve analisis
DATE:    12/03/31 10:31:25 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

Photometric optical measurements of GRB 120326A detected by SWIFT  (trigger 518626) 
M. H. Siegel et al (GCNC 13105) have been done using the Schmidt telescope 0.32m F/3.1
and Starlight CCD camera HX-516 applied at direct focus. 120 sec. exposure time and 
2x2 binning were used for all photos. All exposure were unfiltered. 
Every night flat field and dark have been captured and all images were corrected 
with them. In order to capture faint objects 60 shots was added before measurement
MPO  Canopus  version 10.4.0.20 was used to perform differential photometry on 
the reduced images. 

began of period: 2012/03/26.945 - 21.3 hours after  the burst.
end   of period: 2012/03/29.103 - 73.1 hours after  the burst.

-----------------  
GSC1.2 STARS USED  
-----------------  
               
 ID: 0442901998    
 ID: 0442901953    
 ID: 0442902070    
 ID: 0442901970 

The photometric results as follow:

-------------------------
Date UTC             Mag.
-------------------------
2012 03 26.94456    18.75
2012 03 26.96648    18.70
2012 03 26.98842    18.70
                         
2012 03 27.01038    18.80
2012 03 27.03232    18.70
2012 03 27.05427    18.80
2012 03 27.07624    19.85
2012 03 27.10038    19.95
                         
2012 03 28.03167    19.30
2012 03 28.05361    19.48
2012 03 28.05362    19.41
2012 03 28.07558    19.52
                         
2012 03 29.02885    19.77
2012 03 29.04972    19.91
2012 03 29.07231    19.93
2012 03 29.09504    20.00
2012 03 29.10332    19.98
-------------------------

Images and analisis are available at the following address:

http://www.osservatoriobassano.org/archivio/grb/GRB120326A-Trig-518626-2012-03-26.htm

This message may be cited.


GRB_name: GRB120324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13179
SUBJECT: GRB 120324A: CrAO optical upper limit
DATE:    12/03/31 11:30:44 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 120324A (Zhang  et al., GCN  13090) with AZT-11 
telescope of CrAO observatory starting on March 25  (UT) 01:46:17 under 
moderate weather conditions and  seeing  of about 2.7 arsces.  Within 
enhanced Swift-XRT position (Evans et al., GCN 13093) we do not detected 
any optical source up to R=20.7. The source reported in  (Guidorzi et al., 
GCN 13092; Im et al., GCN 13097; Sudilovsky et al., GCN 13098) is clearly 
detected and have a brightness R=20.16 +/-0.25.  A photometry is based on 
the  USNO-B1.0 star 1141-0365943 (19 24 20.29 +24 07 58.2)  assuming 
R=17.07:

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

0.8411       R     16x180      n/d     20.7


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13180
SUBJECT: GRB120327A - ATCA radio afterglow detection at 34GHz
DATE:    12/03/31 21:01:15 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 GRB120327A (GCN13123) with the Australia Telescope Compact 
Array for 40 mins centered on 17:55UT on March 31 2012 (T0+4.625days).

We find an unresolved radio source at ra=16:27:27.4, dec=-29:24:54.0 
with a flux of 0.72+/-0.03 mJy. This position is consistent with the 
optical position of GCN13138.

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: GRB120326A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13181
SUBJECT: GRB 120326A: EVLA Observations
DATE:    12/03/31 23:12:27 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 120326A (GCN 13105) with the EVLA at a
mean frequency of 21.9 GHz starting on 2012 March 31.51 UT (5.45 days after
the burst).  We detect a radio counterpart consistent with the Swift-XRT
position (Goad et al., GCN 13110), the optical position (Klotz et al., GCN
13107; Guidorzi et al., GCN 13111; Kuin et al., GCN 13114), and the CARMA 3
mm position (Perley et al., GCN 13175) with a flux density of 1.36 mJy.
 Further observations are planned."


GRB_name: GRB120401A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13182
SUBJECT: GRB 120401A: Swift detection of a burst
DATE:    12/04/01 05:33:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), W. H. Baumgartner (GSFC/UMBC),
V. D'Elia (ASDC), A. Maselli (INAF-IASFPA),
C. J. Mountford (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester) and B.-B. Zhang (PSU) report on behalf
of the Swift Team:

At 05:24:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120401A (trigger=519043).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 58.068, -17.671 which is 
   RA(J2000) = 03h 52m 16s
   Dec(J2000) = -17d 40' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for an image trigger, no
activity is apparent in the immediately available light curve. 

The XRT began observing the field at 05:26:14.1 UT, 118.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 58.0835, -17.6349 which is equivalent to:
   RA(J2000)  = +03h 52m 20.04s
   Dec(J2000) = -17d 38' 05.6"
with an uncertainty of 5.4 arcseconds (radius, 90% containment). This
location is 140 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 1.35e-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
0.05. 

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


GRB_name: GRB120401A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13183
SUBJECT: GRB 120401A: Prompt enhanced Swift-XRT position
DATE:    12/04/01 06:16:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 120401A, we find an
enhanced XRT position of the afterglow: RA, Dec: 58.0819, -17.6359
which is equivalent to:
   RA (J2000)  = 03 52 19.67
   Dec (J2000) = -17 38 09.2
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/519043.

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

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


GRB_name: GRB120401A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13184
SUBJECT: GRB 120401A: Enhanced Swift-XRT position
DATE:    12/04/01 10:53:59 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 2418 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 120401A, 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 = 58.08251, -17.63577 which is equivalent
to:

RA (J2000): 03h 52m 19.80s
Dec (J2000): -17d 38' 08.8"

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: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13185
SUBJECT: GRB 120326A: HCT optical observations
DATE:    12/04/01 11:06:15 GMT
FROM:    D.K. Sahu at Indian Inst of Astrophysics,Bangalore  <dks@iiap.res.in>

D.K. Sahu, G.C. Anupama (Indian Institute of Astrophysics, Bangalore)
and S.B. Pandey (ARIES, Nainital) report.

The optical afterglow of GRB 120326A  (Siegel  et al., GCN 13105)
was observed in Bessell R  band,  with the 2m. Himalayan Chandra Telescope of
the Indian Astronomical  Observatory, Hanle, India. Observations were made
between 22:36 UT and 23:14 UT on 27/03/2012. The optical afterglow was
detected in our individual frames of 300sec each.
The preliminary R  magnitudes of the optical afterglow
calibrated using  nearby USNO B1.0 stars is as under:
------------------------------------------------------------------
Date           Mid UT       Mid time from   Exp.    R  Magnitude

                             GRB(hrs)      (sec)
------------------------------------------------------------------
23-03-2012     22:55         45.5750       5x300    19.68 +/-0.07
-------------------------------------------------------------------


GRB_name: GRB120401A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13186
SUBJECT: GRB 120401A: Swift-BAT refined analysis
DATE:    12/04/01 15:53:31 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),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
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 120401A (trigger #519043)
(Beardmore, et al., GCN Circ. 13182).  The BAT ground-calculated position is
RA, Dec = 58.057, -17.658 deg, which is 
   RA(J2000)  =  03h 52m 13.8s 
   Dec(J2000) = -17d 39' 29.6" 
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows the burst was occuring when the location
came into the BAT FoV at T-100 sec during a preplanned slew.  There was a decline,
then a increase around T+0, and the a decline again returning to baseline
around T+180 sec.  We are not quoting a T90 because we did not observe
the burst in its entirety.
 
The time-averaged spectrum from T-92.97 to T+52.72 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.66 +- 0.23.  The fluence in the 15-150 keV band is 9.1 +- 1.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-85 sec in the 15-150 keV band
is 0.12 +- 0.04 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/519043/BA/


GRB_name: GRB120401A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13187
SUBJECT: GRB 120401A: Swift-XRT refined Analysis
DATE:    12/04/01 17:34:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 120401A (Beardmore  et al.
GCN Circ. 13182), from 124 s to 24.8 ks after the  BAT trigger. The
data comprise 519 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 13183).

The late-time light curve (from T0+5.0 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.2 (+0.4, -0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.29 (+0.07, -0.06). The
best-fitting absorption column is  1.27 (+0.13, -0.12) x 10^21 cm^-2,
in excess of the Galactic value of 3.2 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.75 (+0.11, -0.10)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+1.5, -0) x 10^20 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.75 (+0.11, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00519043.

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


GRB_name: GRB120327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13188
SUBJECT: GRB 120327A: SMARTS optical/IR afterglow observations
DATE:    12/04/02 04:00:35 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 120327A (GCN 13123,
Sbarufatti et al.) over several epochs, starting ~1.8 hours post-burst.
For each epoch, several dithered images were obtained
with
total summed exposure times of 15 min in V and I and 12 min in J and K.

The fading afterglow of GRB 120327A (e.g. GCN 13123, Sbarufatti et al.; GCN
13124,
Klotz et al.; GCN 13125, Smith et al.) was detected with the following
magnitudes (or
3-sigma limits):

mid-exposure
time              V mag               I mag               J
mag               K mag
 1.8 hrs        18.92+/-0.03     17.73+/-0.04    16.46+/-0.07
14.83+/-0.09
 4.1 hrs        19.97+/-0.03     18.57+/-0.04    17.42+/-0.08
15.73+/-0.09
25.8 hrs       >21.9                >20.9                >19.0
   >17.4

(Optical photometry is calibrated against Landolt standard stars
and IR photometry is calibrated against 2MASS stars in the field.)

Between about 1.8 hrs and 4.1 hrs post-burst, the GRB afterglow fades with
a decay rate of approximately alpha = 1 (where afterglow flux is
proportional to t^-alpha).


GRB_name: GRB120326A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13189
SUBJECT: GRB 120326A: Cima Rest and Bassano Brescia
DATE:    12/04/02 11:44:42 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

M.Tonincelli, G.Arici (Cima Rest obs.)
U.Quadri, L.Strabla, R.Girelli and A.Quadri (Bassano Bresciano Obs.)
 
report:

We imaged the field of GRB 120326A detected by SWIFT
(trigger 518626) Goad et al (GCNC 13110), with the telescope
D=508 mm F/D=5 of Cima Rest Observatory (IAU station B11), Italy
during a collaboration with Bassano Bresciano Observatory 
(IAU station 565), Italy

The observations: 
had started 5d 19h 49m after the burst (2012-03-31 at 21h 08m UTC) 
and ended   6d 00h 33m after the burst (2012-04-01 at 01h 51m UTC)  

We co-added 40 exposures of 300s each.

We detected very faint optical couterpart 
of 21.8 (+/- 0.1) unfiltered CCD magnitude.

at the following coordinates:

RA (J2000) =  18 15 37.03 
DEC(J2000) = +69 15 35.1

Magnitudes were estimated using USNO-B1.0 
catalog and are not corrected for galactic 
dust extinction.

This message may be cited.


GRB_name: GRB120402A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13190
SUBJECT: GRB 120402A: Swift detection of a possible burst or noise
DATE:    12/04/02 23:10:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester),
V. D'Elia (ASDC), S. T. Holland (STScI), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), O. M. Littlejohns (U Leicester),
V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), K. L. Page (U Leicester),
T. Sakamoto (NASA/UMBC), R. L. C. Starling (U Leicester) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 22:49:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120402A (trigger=519207).  Swift slewed immediately to the location. 
The BAT on-board calculated location is 
RA, Dec 314.326, +19.258, which is 
   RA(J2000)  =  20h 57m 18s
   Dec(J2000) = +19d 15' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single pulse
with a duration of about 5 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 22:51:08.6 UT, 105.8 seconds after
the BAT trigger. No source was detected in 451 s of promptly downlinked
data. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.12. 

Given that the BAT image significance is only 6.6 sigma
and that the XRT and UVOT do not detect anything, it is 
unlikely that this is a real GRB.  It is possible that
this is a noisy detector in the BAT array.  We will have 
to wait for the full data set to downlink to resolve
this uncertainty. 


GRB_name: GRB120403A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13191
SUBJECT: GRB 120403A: Swift detection of a burst
DATE:    12/04/03 01:25:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/PSU) and C. A. Swenson (PSU) report on behalf
of the Swift Team:

At 01:05:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120403A (trigger=519211).  Swift did not slew because
of the Sun observering constraint.  The BAT on-board calculated location is 
RA, Dec 42.459, +40.466 which is 
   RA(J2000)  =  02h 49m 50s
   Dec(J2000) = +40d 27' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 2 sec.  The peak count rate
was ~2200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 18:44 UT on 2012 June 25. There will thus be no XRT or
UVOT data for this trigger before this time. 

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


GRB_name: GRB120326A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13192
SUBJECT: GRB 120326A: Bassano Bresciano Observatory - correction for GCN Cir 13178
DATE:    12/04/03 08:49:33 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

Photometric optical measurements of GRB 120326A detected by SWIFT  (trigger 518626) 
M. H. Siegel et al (GCNC 13105) have been done using the Schmidt telescope 0.32m F/3.1
and Starlight CCD camera HX-516 applied at direct focus. 120 sec. exposure time and 
2x2 binning were used for all photos. All exposure were unfiltered. 
Every night flat field and dark have been captured and all images were corrected 
with them. In order to capture faint objects 60 shots was added before measurement
MPO  Canopus  version 10.4.0.20 was used to perform differential photometry on 
the reduced images. 

began of period: 2012/03/26.945 - 21.3 hours after  the burst.
end   of period: 2012/03/29.103 - 73.1 hours after  the burst.

-----------------  
GSC1.2 STARS USED  
-----------------  
               
 ID: 0442901998    
 ID: 0442901953    
 ID: 0442902070    
 ID: 0442901970 

The photometric results as follow:

-------------------------
Date UTC             Mag.
-------------------------
2012 03 26.94456    18.75
2012 03 26.96648    18.70
2012 03 26.98842    18.70
                         
2012 03 27.01038    18.80
2012 03 27.03232    18.70
2012 03 27.05427    18.80
2012 03 27.07624    18.85
2012 03 27.10038    18.95
                         
2012 03 28.03167    19.30
2012 03 28.05361    19.48
2012 03 28.05362    19.41
2012 03 28.07558    19.52
                         
2012 03 29.02885    19.77
2012 03 29.04972    19.91
2012 03 29.07231    19.93
2012 03 29.09504    20.00
2012 03 29.10332    19.98
-------------------------

Images and analisis are available at the following address:

http://www.osservatoriobassano.org/archivio/grb/GRB120326A-Trig-518626-2012-03-26.htm

This message may be cited.


[GCN OPS NOTE(24dec12):  See their correction Circular 13192.]


GRB_name: GRB120328B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13193
SUBJECT: GRB 120328B: Pi of the Sky simultaneous upper limits
DATE:    12/04/03 13:06:43 GMT
FROM:    Lech Wiktor Piotrowski at U Warsaw  <lewhoo@fuw.edu.pl>

T.Batsch,A.Majcher,A.Majczyna,K.Nawrocki,M.Sokolowski,G.Wrochna (NCBJ,
Swierk),
M.Cwiok,L.W.Piotrowski,M.Zaremba,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz (Warsaw University of Technology),
from the "Pi of the Sky" collaboration ( http://grb.fuw.edu.pl ).

The wide field "Pi of the Sky South" telescope, installed in
the private observatory of Alain Maury in San Pedro de Atacama 
(http://grb.fuw.edu.pl/pi/index.html#spda_site.htm) observed coordinates 
of the GRB 120328B prior, during and after the reported IPN flash 
detection. No new source was identified. Following limiting magnitudes 
have been set:

t_start - t0 [s]    t_exp     start (UT)  end (UT)     3-sigma limit

      -15             10s       06:26:06   06:26:16         11.6
      +1              10s       06:26:22   06:26:32         11.6
      +16             10s       06:26:37   06:26:47         11.6
      -165          20x10s      06:23:36   06:28:32         12.2
      +152          20x10s      06:28:53   06:33:54         12.3

where limit is based on the reference star magnitudo in V filter.

We acknowledge support received from Alain Maury at SPdA Observatory.


GRB_name: GRB120402B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13194
SUBJECT: GRB 120402B: Fermi GBM detection
DATE:    12/04/03 14:30:16 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 16:04:00.76 UT on 02 April 2012, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 120402B (trigger 355075442 / 120402.669).
The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 223.7, Dec = -10.4 (J2000 degrees, equivalent to
J2000 14h 55m, -10 24'), with a statistical uncertainty of 2.6 degrees
(radius, 1-sigma containment, statistical only; there is additionally
a systematic error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 106 degrees.

The GBM light curve shows a soft, bright, main pulse with some small sustained
emission with a duration (T90) of about 17.5 s (50-300 keV). The time-averaged
spectrum from T0-7.46 to T0+20.192 s is equally well fit by Comptonized Power
Law and a Band function.  

For the CPL function, the best fit parameters are alpha = -1.35 +/- 0.11 and 
Epeak = 37.2 +/- 2.2. The fluence (10-1000 keV) in this time interval
is (3.4 +/- 0.12)E-06 erg/cm^2.

For the Band function, the best fit parameters are alpha = -0.48 +/- 0.37, 
Epeak = 27.5 +/- 2.45, and beta = -2.44 +/- 0.09.  
The fluence (10-1000 keV) in this time interval
is (4.2 +/- 0.22)E-06 erg/cm^2.

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


GRB_name: GRB120403A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13195
SUBJECT: GRB 120403A, Swift-BAT refined analysis
DATE:    12/04/03 15:30:30 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),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120403A (trigger #519211)
(Beardmore, et al., GCN Circ. 13191).  The BAT ground-calculated position is
RA, Dec = 42.458, 40.489 deg which is 
   RA(J2000)  =  02h 49m 49.8s 
   Dec(J2000) = +40d 29' 21.8" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
 
The mask-weighted light curve shows a single peak, starting at T+0 s, 
peaking at T+0.1 s and ending at T+1.8 s.  T90 (15-350 keV) is 1.25 +- 0.19 sec 
(estimated error including systematics).
 
The time-averaged spectrum from T+0.0 to T+1.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.64 +- 0.30.  The fluence in the 15-150 keV band is 1.0 +- 0.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band
is 1.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/519211/BA/


GRB_name: GRB120402A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13196
SUBJECT: GRB 120402A: MASTER follow up observations 
DATE:    12/04/03 16:29:27 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB120402B 10651 sec s after 
notice time and 10700 sec after GRB time at 2012-04-03 01:47:42.444 UT. On 
our first (180s exposure) set we haven't found optical transient  within 
SWIFT error-box (ra=20 57 19 dec=+19 15 36 ).
The 5-sigma upper limit has been about 17.4mag
The long delay  was due to the weather conditions.

The message may be cited.


GRB_name: GRB120403A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13197
SUBJECT: GRB 120403A: MASTER follow up observations 
DATE:    12/04/03 16:40:05 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  GRB120403A 35321 sec s 
after notice time and 36026 sec after GRB time at 2012-04-03 11:05:49.415 
UT. On our first (180s exposure) set we haven't found optical transient 
within SWIFT error-box (Beardmore et al., GCN Circ 13191).
The 5-sigma upper limit has been about 16.0 mag
The message may be cited.

The long delay  was due to the  Eath rotation.

The message may be cited.


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13198
SUBJECT: GRB 120320A: early optical upper limit
DATE:    12/04/03 18:22:28 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A.Volnova (SAI MSU), E. Sinyakov (ISON), D. Varda (ISON), I. Molotov
(KIAM), A.
Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:

We observed the field of the Swift GRB 120320A (Markwardt et al.,
GCN 13071) with ORI-25 (0.25-m) telescope ofISON-Blagoveschensk
observatory. We took several unfiltered images of 60 s exposure on
Mar.20, starting (UT) 12:06:10, i.e. 10 min after trigger.

Within enhanced XRT position (Beardmore et al., GCN 13075) we do not
detect any source in different combined images. Photometry is based
on nearby USNO-B1.0 stars, R2-values.

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

12:06:10 0.00874  none   10x30    n/d   16.7
12:06:10 0.08435  none  360x30    n/d   19.2


GRB_name: GRB120320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13199
SUBJECT: GRB 120320A: optical upper limit in Mondy observatory
DATE:    12/04/03 18:25:11 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed the field of the Swift GRB 120320A (Markwardt et al.,
GCN 13071) with AZT-33IK telescope of Sayan observatory (Mondy) on
Mar. 20 under mean seeing 2.6 arcsec. We took several images in
R-filter of 60 s exposure on Mar.20, between (UT) 14:45:13 -
15:58:25.

Within enhanced XRT position (Beardmore et al., GCN 13075) we do not
detect any source in a combined image. Photometry is based on nearby
USNO-B1.0 stars, R2-values.

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

14:45:13  0.14275  R    72x60     n/d   21.3


GRB_name: GRB120402A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13200
SUBJECT: GRB 120402A: optical upper limit
DATE:    12/04/03 18:48:49 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed the field of the possible GRB 120402A (Swift
trigger=519207; Barthelmy et al., GCN 13190) with ORI-40 telescope of
Kitab ISON observatory on Apr. 02 starting (UT) 22:55:14, i.e. ~6 min
after burst trigger. We obtained several unfiltered images with
exposure of 60 seconds. Within BAT error circle of 3 arcmin, radius
(Barthelmy et al., GCN 13190) we do not detect apparently new source
in comparison with DSS2-red. The photometry is based on USNO-B1.0
reference star 1092-0548647 (20:57:27.42 +19:17:47.2) assuming R =
14.41.

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

22:55:14  0.01449  none  2800   n/d   19.8


GRB_name: GRB120326A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13201
SUBJECT: GRB 120326A, the review of the sky area in plate archives
DATE:    12/04/03 19:56:27 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V. Golovnya, L. Kizyun (Main Astronomical Observatory, Kyiv)
   report:
We have undertaken the review of the sky area in vicinity of 
GRB 120326AA (M.R. Goad et al., GCN Circ.13110) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Ex. LimM Star USNOA2 
19860529/234300 GUA040C000924A 18 14.90 1575-03932397
19860531/232820 GUA040C000931 25 15.65 1575-03932513
19860710/175702 TAS040A000019B 45 17.90 1575-03933870
19860710/175706 TAS040B000020 45 17.95 1575-03933903
19860716/205409 GUA040C000960 16 15.85 1575-03934841
19940726/200551 GUA040C002347 18 15.45 1575-03933972
Plates:  
GUA040C the plates archive identifier of DWA (D/F=400/2000, 
         M=103"/mm) of the Ukrainian NAS Main Astro obs.
         (Marsden's number - 83) the plate number [1].
TAS040A,-the plates archive identifier of DAZ (D/F=400/3000,
TAS040B  M=68.8"/mm) of the Tashkent Astro obs.
         (Marsden's number - 186) the plate number [1].
Ex.  - Duration of the maximum exposure (minutes). 
LimM - Limited V mag, derived in the 15 minutes area around 
       the location given in M.R.Goad et al. GCN Circ.13110: 
       RA(J2000): 18h 15m 37.08s, Dec(J2000): +69d 15' 35.9"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 35x15 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120326A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120402A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13202
SUBJECT: BAT trigger 519207 was a burst from Cyg X-1, was not GRB 120402A
DATE:    12/04/03 20:32:51 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), C. B. Markwardt (GSFC), and
T. Sakamoto (NASA/UMBC) on behalf of the Swift-BAT team

The BAT trigger# 519207 (Barthelmy et al, GCN Circ# 13190) has been
identified as due to a flare from Cyg X-1, not a GRB.  The maskweighted
BAT lightcurve for Cyg X-1 shows a single symmetric pulse in the
15-50 keV band, about 4 seconds long at the same time as the BAT
trigger.  The BAT triggered on the Cyg X-1 flare.  While the on-board
processing ignores known bright sources, a portion of the Cyg X-1 flare
appeared in a spatially separate side-lobe, which the BAT did
trigger on.


GRB_name: GRB120403B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13203
SUBJECT: GRB 120403B: Swift detection of a burst
DATE:    12/04/03 21:03:49 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. Campana (INAF-OAB), M. M. Chester (PSU), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), G. Stratta (ASDC),
C. A. Swenson (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report
on behalf of the Swift Team:

At 20:33:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120403B (trigger=519256).  Because of an observing constraint,
the slew to the burst was delayed by 12.9 minutes. 
The BAT on-board calculated location is 
RA, Dec 54.809, -89.037, which is 
   RA(J2000)  =  03h 39m 14s
   Dec(J2000) = -89d 02' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several spikes
with a total duration of about 10 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 20:49:04.0 UT, 907.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 55.33838, -89.00933 which is equivalent
to:
   RA(J2000)  = 03h 41m 21.21s
   Dec(J2000) = -89d 00' 33.6"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 104 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 9.52
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 910 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
0.13. 

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


GRB_name: GRB120403A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13204
SUBJECT: GRB 120403A: Swift/BAT spectral lag analysis
DATE:    12/04/03 23:35:34 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

J. Norris (BSU), T. Sakamoto (GSFC/UMBC), S.D. Barthelmy (GSFC), 
J. R. Cummings (GSFC/UMBC) for the BAT Team:

We report the spectral lag analysis for GRB 120403A (Beardmore, et al., GCN Circ. 13191)
based on the BAT data.  Using 64-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 63 +380/-180 msec.  Because of a relatively
large error in the lag measurement due to a weak nature of the burst, we can not
conclusively say that this burst is in the short burst category.


GRB_name: GRB120403B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13205
SUBJECT: GRB 120403B: Enhanced Swift-XRT position
DATE:    12/04/04 01:09:27 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 1035 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120403B, 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 = 55.27631, -89.00862 which is equivalent
to:

RA (J2000): 03h 41m 6.31s
Dec (J2000): -89d 00' 31.0"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB120403B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13206
SUBJECT: GRB 120403B: Swift/UVOT Upper Limits
DATE:    12/04/04 11:35:55 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 120403B
911s after the BAT trigger (D'Elia et al., GCN Circ. 13203).
No optical afterglow consistent with the XRT position
(Goad et al., GCN Circ. 13205) 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           911         1061          147         >21.7
white             1190         7931          568         >22.0
v                 1068         8342          588         >20.7
b                 1166         7726          568         >21.3
u                 1141        12488          404         >21.1
w1                1117         9020          851         >21.1
m2                1092         8547          568         >20.8
w2                1216         8137          485         >21.0

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.13 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB120403B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13207
SUBJECT: GRB 120403B: Swift-BAT refined analysis
DATE:    12/04/04 12:42:38 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), V. D'Elia (ASDC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+70 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120403B (trigger #519256)
(D'Elia, et al., GCN Circ. 13203).  The BAT ground-calculated position is
RA, Dec = 54.302, -89.029 deg, which is 
   RA(J2000)  =  03h 37m 12.6s 
   Dec(J2000) = -89d 01' 45.1" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 47%.
 
The mask-weighted light curve shows several overlapping peaks starting 
at ~T-5 sec and ending at ~T+10 sec.  T90 (15-350 keV) is 7.3 +- 1.9 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-3.0 to T+5.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.79 +- 0.31.  The fluence in the 15-150 keV band is 2.1 +- 0.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+0.92 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/519256/BA/


GRB_name: GRB120404A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13208
SUBJECT: GRB 120404A: Swift detection of a burst with an optical counterpart
DATE:    12/04/04 13:01:42 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

G. Stratta (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), S. T. Holland (STScI), E. A. Hoversten (PSU),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB),
P. T. O'Brien (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester), P. Romano (INAF-IASFPA),
R. L. C. Starling (U Leicester), M. C. Stroh (PSU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 12:51:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120404A (trigger=519380).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 235.012, +12.882 which is 
   RA(J2000)  =  15h 40m 03s
   Dec(J2000) = +12d 52' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single symmetric peak
with a duration of about 35 sec.  The peak count rate
was ~1800 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 12:53:12.4 UT, 130.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 235.00884, 12.88446 which
is equivalent to:
   RA(J2000)  = 15h 40m 02.12s
   Dec(J2000) = +12d 53' 04.1"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 14 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.42
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 7.34e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 138 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 15:40:02.29 = 235.00956
  DEC(J2000) = +12:53:06.3  =  12.88508
with a 90%-confidence error radius of about 0.65 arc sec. This position is 4.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.37 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.05. 

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


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13209
SUBJECT: GRB 120404A: Faulkes Telescope North afterglow confirmation
DATE:    12/04/04 13:13:33 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 larger collaboration report:

"The 2-m Faulkes Telescope North robotically followed up GRB 120404A
(Stratta et al., GCN Circ. 13208) at 12:55:03 UT, corresponding to 4 min
after the GRB trigger time. We clearly detect the optical afterglow
candidate by Swift-UVOT (GCN 13208) with a magnitude of 18.8 +- 0.3
in the R filter in a 10-s exposure frame, calibrated against nearby
USNOB-1 field stars.


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13210
SUBJECT: GRB 120404A: MASTER early OT limit 
DATE:    12/04/04 13:24:31 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  GRB120404A 24 sec s after 
notice time and 71 sec after GRB time at 2012-04-04 12:52:13.917 UT. On 
our first (10s exposure) set we haven't found optical transient  within 
SWIFT error-box (Stratta et al., GCN 13208).
The GRB was at 15 degrees under horizont.
The 5-sigma upper limit has been about 15.3 mag. 
The message may be cited.


The message may be cited.


GRB_name: GRB120404A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13211
SUBJECT: GRB 120404A: MITSuME Akeno Optical upper limits
DATE:    12/04/04 14:51:25 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

Y. Saito, Y. Aoki, S. Song, M. Hayashi, K. Kawakami, K. Tokoyoda,
R. Usui, Y. Yatsu, and N. Kawai (Tokyo Tech)  report on behalf of
the MITSuME collaboration:

We observed GRB 120404A (Stratta et al., GCN Circular 13208) with the
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.

We started the observation 84 sec after the BAT trigger
from 2012-04-04 12:52:24.8 UT.  And we did not find any new point source
within the XRT error circle in the three bands.
The results of photometry (3sigma upper limits) are listed below.

The photon flux were calibrated against GSC2.3 catalog.

T0+[sec]      MID-UT     T-EXP[sec]       g'              Rc           Ic
----------------------------------------------------------------------------------------------------
   219         12:54:40          270           > 15.4       > 16.1     > 16.7
----------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120403B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13212
SUBJECT: GRB 120403B: AAT nIR observations
DATE:    12/04/04 14:53:57 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

Rhaana Starling, Klaas Wiersema (U. Leicester), Stuart Ryder (AAO), Peter Barnes (U. Florida) and Christopher Stockdale (Marquette Univ.) report:

We began observations of the field of GRB 120403B with IRIS2 on the 4m Anglo-Australian Telescope on 2012-04-04 at 08:34:00 UT, 
12 hours after the BAT trigger (D'Elia et al., GCN Circ. 13203). We performed near-infrared photometry in the Ks, H and J bands, 
totalling 2x9 minutes in each filter. 

We do not detect any source within the UVOT-enhanced XRT error circle (Goad et al., GCN Circ. 13205) down to limiting magnitudes of
Ks > 19.4 mag
H  > 20.0 mag
J  > 20.9 mag.
Calibration was carried out using 8 2MASS field stars. No correction for Galactic extinction has been applied.


These observations were obtained under programme AAT/11B/21.


GRB_name: GRB120404A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13213
SUBJECT: GRB 120404A: Gemini-N Redshift
DATE:    12/04/04 15:17:07 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), on behalf of a larger
collaboration reports:

On April 4.58 UT (~60 minutes after the BAT trigger) 
we observed the field of GRB 120404A (Stratta et al., 
GCN 13208) using GMOS Spectrograph on the Gemini-North 
8-m telescope.  

The optical afterglow is clearly detected in our r-band 
acquisition image. 
We performed 2x900s spectroscopic observations of the 
optical afterglow using the B600 grating centered at 6500 
Angstrom (covering the range 5100-7900 A).
The spectrum reveals several absorption features, including 
FeII2586,2600, MgII2796,2803 at a common redshift of 1.633.
Other features indicate at least one MgII intervening system at
z=1.101

We therefore suggest that the redshift of GRB 120404A is z=1.633.

We thank the Gemini-North staff for their prompt support.


GRB_name: GRB120403B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13214
SUBJECT: Subject: GRB 120403B: Fermi GBM Observation
DATE:    12/04/04 15:35:26 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

George Younes (USRA)
reports on behalf of the Fermi GBM Team:

"At 20:33:58.49 UT on April 03, 2012, the Fermi Gamma-ray Burst
Monitor (GBM) triggered and located GRB 120403B (trigger 355178040 /
120403857) which was triggered and detected by Swift (D'Elia et al.,
GCN 13203). The on-ground calculated location, using the Fermi GBM
trigger data is consistent with the Swift location.

The GBM light curve shows a single event with a duration (T90) of
about 4 s (50-300 keV).

The time-averaged spectrum from T0-1.792 s to T0 is well fit
by a power law with index -1.51 +/- 0.08.
A power law with an exponential high-energy cutoff fits the
spectrum equally well. The power law index is  -0.9 +/- 0.3
and the cutoff energy, parameterized as Epeak, is 182 +/- 74 keV.

The event fluence (10-1000 kev) in this time interval is
(4.6 +/- 0.6)E-07 erg/s-cm^2. The 1-s peak photon flux starting at
T0-0.896 s in the 10-1000 keV range is 1.7 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB120403B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13215
SUBJECT: GRB 120403B: TAROT La Silla observatory optical observations
DATE:    12/04/04 16:39:02 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 120403B detected by SWIFT
(trigger 519256) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 2.8h after the GRB trigger
(the burst occured during the afternoon).
The elevation of the field was 29 degrees above
horizon and weather conditions were good.

We co-added a series of exposures. No optical
counterpart was found. The limiting magnitude
of the image is R=19.5 but the burst occured
close to a R=17.2 star. So we prefer to
publish a conservative value of 18.2 as the
upper limit of the afterglow:

start   stop
2.95h   4.82h   R > 18.2

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

This message may be cited.


GRB_name: GRB120402B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13216
SUBJECT: GRB 120402B: MASTER early OT limit
DATE:    12/04/04 16:56:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

V.Krushinski, I.Zalozhnich,  A. Popov
Ural State University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER robotic Very Wide Field Cameras    (MASTER: http://observ.pereplet.ru) 
located in Tunka was pointed to the  FERMI GRB 120402B (Collazzi, 
GCN 13194) 64 sec after GRB time at 2012-04-02 16:05:04.583 UT.
On our first (10s exposure) set we haven't 
found optical transient  within FERMI error-box (RA = 223.7, Dec = -10.4, 
Rad=9 degrees (3 sigma + 3 deg. of systematic error ) .
The MASTER VWF cameras cover full 1 sigma (+ 3 deg. sys. error) 
error box and ~ 95% 3 sigma  (+ 3 deg. sys. error) error box.
The unfiltered upper limit is 12.0 mag.


The message may be cited.


GRB_name: GRB120404A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13217
SUBJECT: GRB 120404A: Gemini-N Redshift correction
DATE:    12/04/04 18:38:17 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), N.R. Tanvir (U. of Leicester) report
on behalf of a larger collaboration:

We re-analyzed the GMOS spectra of GRB 120404A presented 
in GCN 13213.
Based on further analysis we report a corrected redshift 
for the GRB of z=2.876. 

This new value is based on the identification of SiIV1393,1403,
CIV1550,AlIII1855,1963, CII1335, CII*1335, SiII1527, SiII*1533,
SiII1808.
We note that the CIV1448 line at this redshift is partly covered
by the GMOS chip gap.

At least four different intervening systems are identified at 
the following redshifts:

z1=2.551 (based on CIV1548,1550 doublet)
z2=1.776 (based on MgII2796,2803 doublet)
z3=1.633 (based on MgII2796,2803 doublet)
z4=1.101 (based on MgII2796,2803 doublet)

We encourage further spectroscopic observations and apologize for
any inconvenience the previous redshift determination may have caused.


GRB_name: GRB120404A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13218
SUBJECT: GRB 120404A: Enhanced Swift-XRT position
DATE:    12/04/04 20:47:59 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 852 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120404A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 235.00951, +12.88471 which is equivalent
to:

RA (J2000): 15h 40m 2.28s
Dec (J2000): +12d 53' 04.9"

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: GRB120401A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13219
SUBJECT: GRB 120401A: GROND Detection of an optical/NIR afterglow candidate
DATE:    12/04/04 23:27:18 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

V. Sudilovsky, J. Elliott, J. Greiner (all MPE Garching), T. Kruehler (DARK) and A. Rau (also MPE Garching), report on behalf of the GROND team:

We observed the field of GRB120401A (Swift trigger 519043; Beardmore et al., GCN #13182) 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).

First observations started at 23:32 UT on 2012-04-01, 18.1 hours after the GRB trigger. For an exposure time of 18.76 min in g'r'i'z' and 15 min in JHK performed at an average seeing of 1".8 and at an average airmass of 2.1, we find a single point source within the 1".6 enhanced Swift-XRT error circle reported by Evans et al. (GCN #13184) at

RA (J2000)   = 03:52:19.82 = 58.08258
Dec. (J2000) = -17:38:08.5 = -17.63569

with an uncertainty of 0.3" in each coordinate.

We estimate preliminary magnitudes (all in AB) of

g' > 23,
r' = 22.7 +/- 0.2
i' = 21.5 +/- 0.1
z' = 21.0 +/- 0.1
J  = 20.7 +/- 0.2,
H  > 20.7, and
K  > 18.5

The SED, constructed from the Galactic foreground extinction (E_(B-V)=0.053 mag, Schlegel et al. 1998) corrected magnitudes of the object gives a photometric redshift of z=4.5  0.5, while intrinsic or host galaxy extinction alone cannot account for the r'-i' colour. 

A second observation began at 23:29 UT on 2012-04-02, 1.75 days after the GRB trigger. Due to telescope pointing problems, JHK were the only filters to cover the GRB location. For an exposure time of 38.3 min in JHK at an average seeing of 1".4 and at an average airmass of 2.0, we do not detect the source. With an upper limit of J (AB) > 21.4, it suggests a decay of at least 0.7 mag.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars.


GRB_name: GRB120404A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13220
SUBJECT: GRB 120404A: Swift-BAT refined analysis
DATE:    12/04/05 00:40:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
G. Stratta (ASDC), J. Tueller (GSFC)
(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 120404A (trigger #519380)
(Strata, et al., GCN Circ. 13208).  The BAT ground-calculated position is
RA, Dec = 235.002, 12.883 deg, which is 
   RA(J2000)  =  15h 40m 00.4s 
   Dec(J2000) = +12d 52' 57.3" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 49%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-20 sec, peaking at ~T+4 sec, and ending at ~T+80 sec.
T90 (15-350 keV) is 38.7 +- 4.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-7.31 to T+38.45 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.85 +- 0.13.  The fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+3.29 sec in the 15-150 keV band
is 1.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/519380/BA/


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13221
SUBJECT: GRB 120404A : TNT optical observation 
DATE:    12/04/05 00:44:27 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 120404A (Stratta et al., GCN Circ. 13208)
with Xinglong TNT telescope in R-band at 19:33:05(UT),   6.7 hours after 
the burst. The optical counterpart (Stratta et al., GCN Circ. 13208, Guidorzi et al. GCN Circ. 13209) 
was marginal detected with a brightness of 20.3 +/- 0.2 mag 
calibrated to USNO B1.0 R2 mag, at the mean time of 7.4 hours after the burst.

Combined with the report by Guidorzi et al. ( GCN Circ. 13209 ), the brightness of this burst
decayed by 1.5 magnitude in R-band during 4 min and 7.4 hour after the burst,
corresponding to a shallow decay index of about 0.3 during this phase. 
 
Further observations are encouraged. 

This message may be cited.
 
For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org:8080/grb/index.html
 
We thank Liang Ma for performing these observations.


GRB_name: GRB120404A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13222
SUBJECT: GRB 120404A: Swift-XRT refined Analysis
DATE:    12/04/05 01:02:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 7.7 ks of XRT data for GRB 120404A (Stratta  et al.
GCN Circ. 13208), from 119 s to 23.3 ks after the  BAT trigger. The
data comprise 109 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Osborne et al. (GCN. Circ 13218).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.15 (+0.18, -0.17). At T+544 s  the decay
flattens to an alpha of 0.1 (+0.4, -0.6) before breaking again at
T+2930 s to a final decay with index alpha=1.83 (+0.21, -0.19).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.72 (+0.14, -0.13). The
best-fitting absorption column is  2.3 (+4.7, -2.3) x 10^21 cm^-2, at a
redshift of 2.87, in addition to the Galactic value of 3.4 x 10^20
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 1.90 (+/-0.12) and a best-fitting absorption column of 4.5 (+4.3,
-4.0) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.7 x 10^-11 (4.3
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 3.4 x 10^20 cm^-2
Intrinsic column:    4.5 (+4.3, -4.0) x 10^21 cm^-2 at z=2.87
Photon index:      1.90 (+/-0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00519380.

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


GRB_name: GRB120403B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13223
SUBJECT: GRB 120403B: Swift-XRT refined Analysis
DATE:    12/04/05 09:05:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 4.5 ks of XRT data for GRB 120403B (D'Elia  et al. GCN
Circ. 13203), from 920 s to 8.9 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Goad et al. (GCN. Circ 13205).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.80 (+0.15, -0.14).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+/-0.3). The
best-fitting absorption column is  2.2 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 9.5 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 (5.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 9.5 x 10^20 cm^-2
Excess significance: 2.5 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/00519256.

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


GRB_name: GRB120404A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13224
SUBJECT: GRB 120404A: MITSuME Okayama Optical Observation
DATE:    12/04/05 09:17:14 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 120404A (Stratta et al., GCNC 13208)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on  2012-04-04 17:41:39 UT (~4.8 h after the
burst). We detected the previously reported afterglow (Guidorzi et al.,
GCNC 13209) in Rc and Ic bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc  Rc_err    Ic  Ic_err
----------------------------------------------------------------------
0.24381    18:42:07   5760.0    >20.4   20.2  0.3     19.1  0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120404A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13225
SUBJECT: GRB 120404A: MITSuME Ishigakijima Optical Observation
DATE:    12/04/05 09:17:32 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 120404A (Stratta et al., GCNC 13208)
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 2012-04-04 14:31:32 UT (~1.7 h after the
burst). We detected the previously reported afterglow (Guidorzi et al.,
GCNC 13209) in only Ic band.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc    Ic  Ic_err
----------------------------------------------------------------------
0.09215    15:03:44   1080.0    >18.6  >18.7  17.5  0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120404A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13226
SUBJECT: GRB 120404A: Swift/UVOT Detection
DATE:    12/04/05 11:44:46 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and G. Stratta (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120404A
139 s after the BAT trigger (Stratta et al., GCN Circ. 13208).
A source at the UVOT position given in Stratta et al., GCN Circ. 13208, 
and consistent with the enhanced XRT position (Osborne et al., GCN Circ. 
13218), is detected in the initial UVOT exposures. The source is only 
seen in the optical filters and rises initially and then fades. The fact 
that the source is not detected in the UV filters is consistent with the 
redshift of z=2.876 reported by Cucchiara et al., GCN Circ. 13217.

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              139          288          147         19.43  0.12
v                 4734         4934          197         17.69  0.10
b                  606         1178           58         19.22  0.28
u                  351         1327          304         19.90  0.19
w1                 729         6779          452        >20.3
m2                 704         6574          432        >21.5
w2                 656        11408         1179        >22.1

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: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13227
SUBJECT: GRB 120404A: VLT/X-shooter redshift confirmation
DATE:    12/04/05 14:05:02 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (INAF-OAR and ASI-ASDC), Paolo Goldoni (APC/U. Paris 7 and SAp/CEA), Daniele Malesani (DARK/NBI), Nial R. Tanvir (U. of Leicester), Johan P. U. Fynbo (DARK/NBI) and Andrea Melandri (INAF-OAB) and  report on behalf of a larger collaboration:

We observed the optical/NIR afterglow of the Swift GRB 120404A (Stratta et al., GCN 13208; Guidorzi et al., GCN 13209)  with the VLT/UT2 equipped with the X-shooter spectrograph. Observations started around 04:30 UT on 2012-04-05, which is roughly 16 hr after the trigger. 

In the acquisition frame (taken 15.9 hr after the GRB), the afterglow is detected at low S/N. Comparison with two closeby SDSS stars yields R ~ 21.3 (Vega), with a systematic uncertainty of ~0.3 mag.

Four exposures in a nodding pattern with an integration time of 2400 s each were obtained in poor sky conditions. The spectrum covers an approximate wavelength range between 3000 and 25000 AA. The slit width was set to 1" in the ultra-violet/blue arm, and 0.9" in the visual and near-infrared arms, resulting in a resolving power range of approximately 4500-7500.

Preliminary reduction of the spectrum shows a weak continuum with a trough at ~4720 AA, which we identify as Ly-alpha. We also detect faint absorption lines of OI 1302 and SiIV 1393/1402 at a common redshift of ~2.88. This confirms the redshift determination by Gemini-N (Cucchiara et al., GCN 13217). A second dip matching Lya at z=2.55 is also marginally detected. This is consistent with the CIV intervening absorber reported in Cucchiara et al., GCN 13217.

We are grateful for the excellent support from the Paranal Observatory staff, in particular Claudio Melo. We are in debt to Cristiano Guidorzi for providing us a FTN finding chart.


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13228
SUBJECT: GRB120404A: MOA optical observations of the initial rise afterglow
DATE:    12/04/05 15:09:11 GMT
FROM:    Akihiko Fukui at Nagoya U/MOA  <afukui@stelab.nagoya-u.ac.jp>

P. J. Tristram (MJUO), A. Fukui (NAOJ/OAO) and T. Sako (Nagoya U.) 
report on behalf of the MOA collaboration.

We began prompt observations for the afterglow of GRB120404A (Stratta et al., GCN 13208)
at Apr. 4 12:55:44 UT (4.7 min after the Swift trigger 519380),
using the 61-cm B&C telescope at Mt John University Observatory in New Zealand.
We obtained a series of I and V band images with 60 sec exposure times, followed by some 
120 and 180 sec exposures, until 18:04 UT (5.2 hours after the trigger).

In the first images, we detected marginal objects having I ~ 18.6 and V ~ 19.0 
at the reported coordinate of the afterglow (Osborne et al., GCN13218).
The afterglow was then getting bright, as reported by Breeveld et al. (GCN 13226),
reaching I = 16.6 and V = 17.4 at around 13:40 UT (about 50 min after the trigger).
After the peak, the afterglow had faded out with the rate of +0.7 mag/hour.
The characteristic magnitudes are summarized as bellow.

  UT              I                        V
-------------------------------------------------------
12:56   18.6 +2/-0.6      19.0 +1.2/-0.6
13:40   16.6 +/- 0.1        17.4 +/- 0.1
16.50   18.4 +0.6/-0.4    19.5 +0.6/-0.4
-------------------------------------------------------

All the above magnitudes are measured on 60-sec exposure images,
and calibrated by the GSC2.3 star catalog.
The errors represent 1-sigma statistic uncertainties.


We would like to thank Alberto J Castro-Tirado for giving us useful suggestions.
We acknowledge University of Canterbury for allowing the use of the B&C telescope.


GRB_name: GRB120404A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13229
SUBJECT: GRB120404A: GROND observations show steeply decaying afterglow
DATE:    12/04/05 15:30:10 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

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

We observed the field of GRB120404A (Swift trigger 519380; Stratta et 
al., GCN #13208) 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 2012-04-05 07:01:16 
UT, 18.2 hours after the GRB trigger.

The afterglow (e.g., Stratta et al., GCN #13208; Guidorzi et al., GCN 
#13209) is clearly detected. At mid-time of 19.3 hours post trigger and 
with an exposure of 20 min we measure the following preliminary SDSS 
(g'r'i'z') and 2MASS (JHK) calibrated AB magnitudes:

g' = 23.2  0.3
r' = 22.6  0.1
i' = 22.3  0.1
z' = 22.0  0.1
J = 21.2  0.3
H = 20.6  0.3
K > 20.0

The SED, corrected for the Galactic foreground reddening of E_(B-V)=0.05 
mag (Schlegel et al. 1998) is best fit by a power law with a slope of 
beta~1.4 and no additional rest frame extinction.

The comparison with the MITSuME observation at 4.8 hours post-trigger 
(Kuroda et al., GCN #13224) and TNT measurement at 7.4 hours 
post-trigger (Xin et al., GCN #13221) suggests a significant steepening 
of the afterglow decay. Assuming the decay started around ~7.4 hours 
post-trigger, we estimate the decay slope to be ~2.2.


GRB_name: GRB120404A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13230
SUBJECT: GRB 120404A: MASTER OT observations
DATE:    12/04/06 16:00:51 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,

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  Blagoveschensk was pointed to the  GRB120404A 24 sec  after 
notice time and 71  sec after GRB time at 2012-04-04 12:52:13.917 UT 
(Yurkov et al., GCN  13210).

The observations was  made with a full moon and at high zenith distance.
We see an OT (G. Stratta et. al., GCN  13208) on 3 single and some coadd 
images. First time  the OT seen at coadd of six first images set with 
magnitude about 16.8. After this time the object  was decay below 17.5 
mag for an hour. The OT have a flash to 16.9 mag in our unfiltered  band 
(0.8R+0.2B) ~ 1  h after  trigger time.

The detail imformation about observations in a table 1.

Table 1.

T_mid UT | T-T_grb sec.| Exptime | Coadd  |  Mag | err.mag
---------+-------------+---------+--------+------+--------
12:55:25 |  263        |  180    |  6     | 16.8 |  0.3
13:46:14 | 3311        |  180    |  1     | 17.2 |  0.4
13:49:40 | 3517        |  180    |  1     | 16.9 |  0.4
13:56:33 | 3930        |  180    |  1     | 17.1 |  0.4
14:10:22 | 4760        |  900    |  5     | 17.8 |  0.3
14:36:13 | 6311        | 1800    | 10     | 18.1 |  0.3
15:21:03 | 9001        | 1800    | 10     | 18.2 |  0.3
----------------------------------------------------------

The message may be cited.


GRB_name: GRB120404A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13231
SUBJECT: GRB 120404A:  EVLA Detection
DATE:    12/04/06 20:55:35 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

Ashley Zauderer, Tanmoy Laskar and Edo Berger (Harvard) report:

"We observed the position of GRB 120404A (GCN 13208) with the EVLA at 22 
GHz beginning 2012 Apr 5.27 UT (0.75 d after the burst).  We detect a 
source at 22 GHz consistent with the Swift-XRT (GCN 13218) and the UVOT 
position (GCN 13208) with a flux of 82 uJy (+/- 22 uJy).  The position 
of the radio source is

RA    15:40:02.28 (+/- 0.01)
DEC  +12:53:06.1  (+/- 0.1)

The source was not detected at 6 GHz (3-sigma upper limit of 33 uJy)."


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13232
SUBJECT: GRB 120404A: SMARTS optical/IR observations
DATE:    12/04/06 21:07:50 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 120404A
(GCN 13208, Stratta et al.) with a mid-exposure time of 17.4 hours
post-burst (2012-04-05 06:13 UT).  Total summed exposure
times amounted to 36 minutes in I and 30 minutes in J.

No source is detected at the position of the optical
afterglow (e.g. GCN 13208, Stratta et al.; GCN 13209, Guidorzi
et al.) to approximate limiting magnitudes of I > 21.6 and J > 19.6.
Magnitudes are calibrated using USNO-B1.0 stars in I, and 2MASS
stars in J.


GRB_name: GRB120404A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13233
SUBJECT: GRB 120404A: JCMT SCUBA-2 sub-mm observation
DATE:    12/04/06 21:32:06 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 counterpart to GRB 120404A (Stratta et al., GCN Circ.
13208) using the SCUBA-2 sub-millimeter continuum camera on the James
Clerk Maxwell Telescope.  The observation started at 13:50 UT on
2012-04-04, corresponding to 59 minutes after the burst trigger.
Exposures totaling one hour were made in marginal weather conditions.
No source was detected, with a preliminary RMS of 4.1 mJy at 850 microns.

We thank William Montgomerie for his prompt support of these observations.


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13234
SUBJECT: GRB 120404A, Optical Observations
DATE:    12/04/07 09:01:17 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Kumar Bhatt and S.B. Pandey (ARIES, Nainital,
India, on behalf of larger Indian GRB collaboration)

We started to observe the GRB 120404A field (Swift trigger 519380, Stratta
et al., GCN Circ. 13208) with the 1.04m telescope at ARIES, Nainital
starting 2012-04-04 19:18:43 (UT). Several images in R_c and I_c pass-bands
were obtained.

The optical afterglow  candidate (Stratta et al., GCN Circ. 13208,
Guidorzi et al. GCN Circ. 13209) was clearly detected in our frames.
The preliminary photometry of co-added R_c (300sec x 4) and I_c
(300sec x 3) frames yield the following magnitudes.

...............................................................
Time (MID-UT)     Exp (sec)          Filter        Magnitude
...............................................................
19:39:40           1200                R_c       20.6 +/- 0.14
19:51:22            900                I_c       19.7 +/- 0.12
...............................................................

The nearby USNO stars have been used for calibration.

This massage may be cited.


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13235
SUBJECT: GRB 120404A: optical observations
DATE:    12/04/07 22:40:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU),  D. Varda (ISON), E. Sinyakov (ISON),  E. Litvinenko 
(UBAI), V. Kouprianov (GAO), I. Molotov (KIAM), A. Pozanenko (IKI) on behalf 
of  larger GRB follow up collaboration report:

We observed the field of the Swift GRB 120404A  (Stratta et al., GCN 13208) 
with ORI-25 (0.25-m) telescope of  ISON-Blagoveschensk observatory between 
Apr. 04 (UT) 13:06:10 - 14:43:45 and ORI-40 (0.4-m) telescope of ISON-Kitab 
observatory between Apr. 04 (UT) 17:13:02 - 18:16:58.  Several unfiltered 
images were taken in both observatories. We detected optical afterglow 
(Stratta et al., GCN 13208; Guidorzi et al., GCN 13209) in combined image 
(see below).  Coordinates of the OT are (J2000) 15:40:02.17,  +12:53:06.5 
with unceraininty of 0.75" on both coordinates which is compatible with 
coordinates reported by UVOT team (Stratta et al.,  GCN 13208). A photometry 
is based on nearby USNO-B1.0 stars (R2 magnitude):

t_start,    t-t0 (mid),  filter  exp.,    OT,                UL
(UT)             d                   s

13:06:10 0.01529  none  12x25   n/d                   16.5
13:21:11 0.03700  none  38x25   17.35 +/- 0.25 17.5
14:08:43 0.06611  none  29x25   n/d                   17.9
17:13:02 0.20378  none  60x60   n/d                   18.9

Based on initially non-detection of the OT we can confirm the brightening of 
the afterglow (Breeveld et al., GCN 13226;  Tristram et al., GCN 13228; 
Gorbovskoy  et al., GCN 13230) with a peak between (UT) 13:21 and 14:06 
(i.e. ~ 50 min after burst trigger). 


GRB_name: GRB120404A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13236
SUBJECT: GRB 120404A: optical observations in Mondy observatory
DATE:    12/04/08 14:58:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 120404A  (Stratta et al., GCN 13208) 
with AZT-33IK telescope of Sayan observatory (Mondy). We took several images 
in R-filter of  60 s exposure on Apr. 04, starting (UT) 14:31:21. We clearly 
detected optical afterglow (Stratta et al., GCN 13208; Guidorzi et al., GCN 
13209) in single images. A preliminary photometry of combined images is 
based on nearby USNO-B1.0 stars:

t_start,    t-t0 (mid),  filter exp., OT,    err
(UT)             d               s
 14:31:21     0.07142 R 5x60   18.24  0.05
 14:37:26     0.07564 R 5x60   18.36  0.04
 14:42:30     0.07916 R 5x60   18.40  0.05
 14:47:34     0.08268 R 5x60   18.36  0.07
 14:52:37     0.08619 R 5x60   18.59  0.07
 14:58:42     0.09041 R 5x60   18.59  0.04
 15:03:46     0.09393 R 5x60   18.77  0.12
 15:08:50     0.09920 R 10x60 18.76  0.06
 15:19:58     0.10694 R 10x60 18.95  0.06
 15:30:06     0.11432 R 10x60 18.94  0.08
 15:41:14     0.12171 R 10x60 19.00  0.08
 15:51:21     0.12908 R 10x60 19.30  0.09

Our photometry suggests bumpy light curve of the afterglow during our 
observations.


GRB_name: GRB120419A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13241
SUBJECT: GRB 120419A: A long GRB detected by INTEGRAL
DATE:    12/04/19 14:10:21 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a long gamma ray burst lasting about 20 s has been detected by IBAS in the 
IBIS/ISGRI data at 12:56:25 UT of April 19

Its refined coordinates (J2000) are:
RA: 187.4024 [degrees]
DEC: -63.017 [degrees]

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

A preliminary analysis gives a 20-200 keV fluence of about 2e-7 erg/cm2 
and a peak flux of about 0.4 ph/cm2 s (1 s integration time)

A plot of the light curve will be posted at

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


GRB_name: GRB120419A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13242
SUBJECT: GRB 120419A: Swift-XRT and UVOT observations
DATE:    12/04/20 15:01:09 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, R.L.C. Starling, P.A. Evans (U. Leicester), S.R. Oates
(MSSL-UCL) and T. Sakamoto (GSFC/UMBC) report on behalf of the
Swift-XRT and UVOT teams:

We have analysed 2.0 ks of XRT data for the INTEGRAL-detected burst GRB
120419A (Gotz et al., GCN Circ. 13241), from 25.6 ks to 32.3 ks after
the INTEGRAL trigger. The data are entirely in Photon Counting (PC)
mode. There is a faint source detected within the INTEGRAL error circle
at a position of RA, Dec = 187.38762, -63.00791, which is equivalent to


RA (J2000): 12h 29m 33.03s
Dec(J2000): -63d 00' 28.5"

with an uncertainty of 4.5". This position is 40.7" from the
INTEGRAL position. The source count rate is 0.0079 +/- 0.0033 count
s^-1; we cannot determine whether the source is fading.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020215.

The UVOT began settled observations of the field of GRB 120419A
25.7 ks after the INTEGRAL trigger. No optical afterglow, consistent
with either the INTEGRAL position or with the candidate X-ray position
given above, is detected in the initial UVOT exposures. Preliminary
3-sigma upper limit using the UVOT photometric system (Breeveld et al.
2011, AIP Conf. Proc. 1358, 373) for the initial exposure is:

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

u      25697      26908      1191    >20.5

The magnitude in the table is not corrected for the Galactic extinction
due to the large but uncertain reddening in the direction of the burst
(Schlegel et al. 1998).

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


GRB_name: GRB120422A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13243
SUBJECT: GRB 120422A: Swift detection of a burst
DATE:    12/04/22 07:22:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/ORAU), V. D'Elia (ASDC), C. Guidorzi (U Ferrara),
E. A. Hoversten (PSU), H. A. Krimm (CRESST/GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), O. M. Littlejohns (U Leicester),
A. Melandri (INAF-OAB), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 07:12:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120422A (trigger=520658).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 136.929, +14.006 which is 
   RA(J2000) = 09h 07m 43s
   Dec(J2000) = +14d 00' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single complex peak
structure with a duration of about 10 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 07:13:38.7 UT, 95.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 136.91183, 14.01873 which
is equivalent to:
   RA(J2000)  = 09h 07m 38.84s
   Dec(J2000) = +14d 01' 07.4"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 75 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.71
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 3.12e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 104 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 

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


GRB_name: GRB120422A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13244
SUBJECT: GRB 120422A: Faulkes Telescope North observations
DATE:    12/04/22 08:09:59 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), J. Japelj (U. Ljubljana),
A. Melandri (INAF-OAB) on behalf of a larger collaboration report:

"The 2-m Faulkes Telescope North robotically followed up GRB 120422A
(D'Elia et al., GCN Circ. 13243) at 07:18:38 UT, corresponding to 6.6
min after the GRB trigger time.
In the XRT error circle, in a 3x10s frame we do not find
any source brighter than R=18.4 mag, calibrated against nearby
USNOB-1 field stars.


GRB_name: GRB120422A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13245
SUBJECT: GRB 120422A: Gemini observations
DATE:    12/04/22 10:44:59 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), A. Levan (U Warwick), D. B. Fox (PennState),
N. R. Tanvir (U. Leicester) report on behalf of a larger collaboration reports:

On April 22.33 UT (~50 minutes after the BAT trigger) we observed the field 
of GRB 120422A (Troja et al., GCN 13243) using GMOS Spectrograph on 
the Gemini-North 8-m telescope.  

In our acquisition image of 240s in i' band an optical candidate was identified at:

RA: 09:07:38.38
Dec: +14:01:07.5

with an uncertainty of 0.3" in each direction.
Using three SDSS stars in the field we estimate a magnitude of 

i'=19.03 +- 0.15 

We also noticed just outside the XRT error circle the presence of 
the SDSS (DR8) galaxy SDSS J090738.51+140108.3.

A subsequent spectrum of 2x900s, covering the wavelength range 6000-10000 
does not present evident absorption features. 
If the SDSS galaxy is associated with GRB 120422A then its brightness would 
suggest a moderately low redshift (z<1).
Further analysis is in progress.

We thank the Gemini-North staff for their prompt support.


GRB_name: GRB120422A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13246
SUBJECT: GRB 120422A: Swift-BAT refined analysis
DATE:    12/04/22 13:48:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), E. Troja (NASA/GSFC/ORAU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+224 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120422A (trigger #520658)
(Troja, et al., GCN Circ. 13243).  The BAT ground-calculated position is
RA, Dec = 136.915, 13.974 deg, which is 
   RA(J2000)  =  09h 07m 39.7s 
   Dec(J2000) = +13d 58' 27.1" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 68%.
 
The mask-weighted light curve shows a single peak starting at ~T-3 sec,
peaking at ~T+1, and ending at ~T+20 sec.  There is a low-significance peak
(~3 sigma) at T+45 to T+65.  T90 (15-350 keV) is 5.35 +- 1.4 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.80 to T+6.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.19 +- 0.24.  The fluence in the 15-150 keV band is 2.3 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.86 sec in the 15-150 keV band
is 0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/520658/BA/


GRB_name: GRB120422A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13247
SUBJECT: GRB 120422A: Enhanced Swift-XRT position
DATE:    12/04/22 15:12:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1079 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120422A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 136.91027, +14.01822 which is equivalent
to:

RA (J2000): 09h 07m 38.46s
Dec (J2000): +14d 01' 05.6"

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

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

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


GRB_name: GRB120422A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13248
SUBJECT: GRB 120422A: A Swift/UVOT Detection
DATE:    12/04/22 18:23:37 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and E. Troja (NASA/GSFC/ORAU) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120422A
104 s after the BAT trigger (Troja et al., GCN Circ. 13243). A source
consistent with the XRT position (Beardmore et al., GCN Circ.  13247)
is detected in the summed UVOT exposures at position:

RA  (J2000) = 136.91012  deg. =  09:07:38.4
Dec (J2000) = +14.018782 deg. = +14:01:07.6

with an estimated uncertainty of 1".

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           104          254          147         20.39 +/- 0.27
white              857         1007          147         20.51 +/- 0.29
white             5251         6888          393         20.25 +/- 0.15
v                 5662         5862         1082        >19.4
b                 5047         6683          393        >20.7
u                  262          512          246         19.89 +/- 0.32
u                 4842         6478          393         20.00 +/- 0.31
w1                4637        12807         1039         19.84 +/- 0.18
m2                5867         6067          197         19.21 +/- 0.28
m2               11245        12145          886         19.36 +/- 0.14
w2                5457         7032          332         18.98 +/- 0.16

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


GRB_name: GRB120422A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13249
SUBJECT: GRB 120422A: Swift-XRT refined Analysis
DATE:    12/04/22 19:23:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 13 ks of XRT data for GRB 120422A (Troja  et al. GCN
Circ. 13243), from 101 s to 30.1 ks after the  BAT trigger. The data
comprise 307 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 13247).

The light curve can be modelled with an initial power-law decay with an
index of alpha=6.22 (+0.30, -0.28), followed by a break at T+373 s to
an alpha of 0.30 (+0.11, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 4.5 (+0.4, -0.3). The
best-fitting absorption column is  2.5 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 3.7 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 1.9 x 10^-11 (1.7 x 10^-10) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      2.5 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: 8.5 sigma
Photon index:      4.5 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00520658.

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


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13250
SUBJECT: GRB 120422A: Zadko observatory - Gingin optical observations
DATE:    12/04/22 20:14:59 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (ASDC/INAF-OAR), M. Boer (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA) report:

We imaged the field of GRB 120422A detected by SWIFT
(trigger 520658) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 3.6h and finished 4.8h
after the GRB trigger.

Weather conditions were good but a poor seeing
of 3.5 arcsec does not allow to separate the
GRB afterglow (Cucchiara et al. GCNC 13245) and
the SDSS galaxy J090738.51+140108.3.

We added the r, g, i SDSS images to create an
equivalent of the Zadko unfiltered image.
The star R=16.37 at ra=136.9080750 dec=+14.0119528
J2000 was used as reference. The flux ratio
of the reference star and the galaxy shows that an
additional component at R=21.1 should be present
in the galaxy on the Zadko image.

start   end     Rmag  dmag filter
   (h)   (h)
   3.6   4.8     21.1  0.2  CR


GRB_name: GRB120422A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13251
SUBJECT: GRB 120422A: Gemini redshift of candidate host
DATE:    12/04/22 20:18:05 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), A. Cucchiara (UCSC/UCO Lick) &
D. B. Fox (Penn State) report on behalf of a larger collaboration:

Further analysis of the Gemini/GMOS spectrum of the nearby galaxy reported by
Cucchiara et al. (GCN 13245) revealed emission lines of Ha, OIII(5007/4959) and Hb
at a common redshift of z=0.28.  At this redshift, the impact parameter of the afterglow
is about 8kpc, which would be a rather large offset for a long-GRB, but certainly possible.
If the galaxy is the host, then the absence of absorption lines in the afterglow spectrum
would not be too surprising, given the weakness of expected lines in the observed
wavelength range.  However, it would also make it one of the lowest
redshift GRBs so far detected by Swift, and so an important target for further follow-up.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13252
SUBJECT: GRB 120422A: NOT optical observations
DATE:    12/04/23 01:25:22 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

S. Schulze (U. Iceland), D. Malesani (DARK/NBI), A. de Ugarte Postigo
(IAA-CSIC, DARK/NBI), A. J. Levan (U Warwick), P. Jakobsson (U.
Iceland), E. Wuyts (KIPAC Chicago) report on behalf of a larger
collaboration:

We observed the field of GRB 120422A (Troja et al., GCN 13243) with
the Nordic Opitcal Telescope (NOT) equipped with MOSCA. We obtained 12
x 300 s I-band images. Observations started at 20:54 UT on April 22
(i.e., 13.3 hrs after the burst).

We clearly detected the source reported in Cucchiara et al. (GCN
13245) in all individual images. There was no significant fading
during observations. The source has an I-band brightness of 21.7 mag
(Vega magnitude) in the stacked image. This value is not corrected for
foreground extinction and calibrated with the #1039-0167772 star (I =
18.98 mag) in the USNO B1 catalogue.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13253
SUBJECT: GRB 120422A: Xinglong TNT optical upper limit
DATE:    12/04/23 02:38:19 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 120422A  (Troja et al., GCN 13243)
with Xinglong TNT telescope in R-band at 11:37:41(UT),   
4.45 hours after the burst under the bad weather condition. 
The optical counterpart  ( Cucchiara et al. GCN 13245;  
Kuin et al. GCN 13248; Klotz et al. GCN 13250; Schulze et al. GCN 13252)  
was not detected in our combined image.
The upper limit was estimated about 19.5 mag in R band 
at the mean time of 5.15 hours after 
the burst, calibrated against the USNO B1.0 R2mag.

This message may be cited.
 
For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org:8080/grb/index.html
 
We thank Liang Ma for performing these observations.
 


GRB_name: GRB120422A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13254
SUBJECT: GRB 120422A:  EVLA Detection
DATE:    12/04/23 06:34:07 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

Ashley Zauderer, Edo Berger and Tanmoy Laskar (Harvard) report:

"We observed the position of GRB 120422A (GCN 13243) with the EVLA at 6 
GHz and 22 GHz beginning 2012 Apr 23.09 (0.8 d after the burst).  We 
detect a 5- and 3-sigma source (for 6 and 22 GHz, respectively) 
consistent with the Swift-XRT position (GCN 13247) and the UVOT position 
(GCN 13248).  The position of the radio source is

RA   09:07:38.42  (+/- 0.01)
DEC +14:01:07.1   (+/- 0.2)

Followup observations are planned."


GRB_name: GRB120422A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13255
SUBJECT: GRB 120422A: Super-LOTIS early observations
DATE:    12/04/23 06:49:46 GMT
FROM:    Peter A. Milne at Super-LOTIS  <pmilne511@cox.net>

Adria C. Updike (Dickinson College), Dieter H. Hartmann (Clemson
University), Peter A. Milne (Steward Observatory), and G. Grant Williams
(MMTO) report:

We observed the field of GRB 120422A (Troja et al., GCN 13243) with the
0.6m Super-LOTIS telescope at KPNO beginning 77 seconds after the
trigger under good conditions.  We do not detect the OT (Cucchiara et
al., GCN 13245; Kuin & Troja, GCN 13248) in the R band.  Limiting
magnitudes are given below, compared to the USNO B1.0 catalog.

midtime (s)       stack         limiting mag
----------------------------------------------------
126                  4 x 5s           16.4
233                  5 x 10s         16.9
557                  5 x 60s         19.0


GRB_name: GRB120422A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13256
SUBJECT: GRB 120422A GROND observations
DATE:    12/04/23 07:42:24 GMT
FROM:    Marco Nardini at MPE  <nardini@mpe.mpg.de>

M. Nardini (Uni. Milano-Bicocca), S. Schmidl (TLS Tautenburg),
J.Greiner (MPE Garching), and D.A. Kann  (TLS Tautenburg) report on behalf of the GROND team:

We observed the field of GRB 120422A (Swift trigger 520658, Troja et al.,
GCN #13243) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla
Observatory (Chile).

Observations started on April 22, 2012, at 23:39 UT, 16.5 hr after the GRB
trigger, and continued for 3 hours. They were performed at an average seeing of
1.45" and at an average airmass of 1.45.

Based on 49 min of total exposures  in g'r'i'z' and 100 min in JHK
we found a blue source consistent with the afterglow position
reported by Kuin et al. (GCN #13248) and  Cucchiara et al. (GCN #13245). 

In g'r'i'z'J we measure a separation of about 1.6" from the SDSS (DR8) galaxy
SDSS J090738.51+140108.3 cited by Cucchiara et al., even if we notice that this value is just slightly larger than the measured seeing.


At the position of afterglow candidate we measure the following magnitudes (in the AB system)

g' = 21.68 +- 0.05 AB mag,

r' = 21.59 +- 0.05 AB mag,

i' = 21.3 +- 0.1AB mag

calibrated against SDSS field stars and not corrected for Galactic foreground reddening of E(B-V)=0.035 (Schlegel et al. 1998). 
We note that the i'-band measurement is significantly contaminated by the underlying candidate host galaxy and thus has to be considered preliminary. Nonetheless, a comparison with the earlier observations reported by Cucchiara et al. (GCN #13245) indicate a fading of at least 2 mag and thus confirms the afterglow nature of the source.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13257
SUBJECT: GRB 120422A: VLT/X-shooter spectroscopy of the GRB counterpart
DATE:    12/04/23 09:13:23 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

S. Schulze (Univ. Iceland), A. J. Levan (Univ. Warwick), D. Malesani 
(DARK/NBI), J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (Univ. Leicester), 
B. Milvang-Jensen (DARK/NBI), A. de Ugarte Postigo (IAA/CSIC and 
DARK/NBI), V. D'Elia (ASI/ASDC and INAF/OAR), J. Sollerman (OKC, 
Stockholm), J. Hjorth (DARK/NBI), report on behalf of the X-shooter GRB 
GTO collaboration:

We observed the optical counterpart of GRB 120422A (Troja et al., GCN 
13243; Cucchiara et al., GCN 13245) with the ESO VLT equipped with the 
X-shooter spectrograph. Observations started on 2012 April 22.99 UT 
(16.5 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. 
The slit was aligned so 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 
GRB optical counterpart (Cucchiara et al., GCN 13245).

We detect a plethora of nebular emission lines from the candidate host 
galaxy, including [O II], [O III], Balmer lines up to Hzeta, [N II], [S 
II], at a common redshift z = 0.283, thus confirming the results of 
Tanvir et al. (GCN 13251).

The trace of the GRB counterpart is rather blue (see also Nardini et 
al., GCN 13256), and we detect Mg II at z = 0.283 in absorption. No 
further absorption features are visible. We also note that the spatial 
extent of the brightest emission lines from the SDSS galaxy encompasses 
the position of the GRB counterpart, indicating nebular emission at z = 
0.283 at the GRB position.

While a chance superposition cannot be excluded, we note that the lack 
of absorption features at z > 0.283 would require a very tenuous 
environment at the GRB location. Furthermore, the UVOT detection in all 
the UV filters (Kuin & Troja, GCN 13248) implies a low redshift z <~ 
1.3. Last, we note that the UVOT photometry at t ~ 5 ks after the burst 
reveals a very blue spectrum, which is not typical of GRB afterglows, 
but is reminiscent of the very blue early emission of GRB 060218 
(Campana et al. 2006, Nature, 442, 1008). We thus conclude that the GRB 
is also likely at z = 0.283.

Using the gamma-ray fluence reported by Barthelmy et al. (GCN 13246), at 
z = 0.283 the isotropic-equivalent energy release of GRB 120422A is 
~4.4*10^49 erg, which is typical of local GRBs, often associated with 
supernovae. We encourage photometric and spectroscopic follow-up to 
detect the emergence of a supernova, or lack thereof.

We acknowledge the excellent support of the ESO observing staff in 
Paranal, in particular Henri Boffin and Giovanni Carraro. We thank Nino 
Cucchiara for providing us with a finding chart from the Gemini 
observation (GCN 13245).


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13258
SUBJECT: GRB 120422A: RAPTOR Limits During Gamma-ray Emitting Interval
DATE:    12/04/23 22:37:04 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 520658 (Troja et al., GCN 13243).  The burst location was within
the field of our wide-field monitor located in Maui, HI, which began a 10 s
integration of the location at 07:12:06.81 UT, 3.2 s after the Swift trigger
time and during the gamma-ray emitting interval.  The optical counterpart
(Cucchiara, et al., GCN 13245, and Kuin et al., GCN 13248) was not detected
above our 3-sigma limiting magnitude of 10.3 based on a comparison of our
unfiltered image to the Tycho-2 V-band catalog.  Our narrow-field instruments
in Los Alamos, NM, began imaging at 07:12:55.49 UT, 51.8 s after the Swift
trigger and 5.7 s after receiving the GCN packet.  The initial 5 s exposure
shows no counterpart to a 3-sigma limiting magnitude of 16.6 when compared
to the USNO-B1 R-band.  The following table gives a sample of our
observations.  The start time is given as the seconds between the start of
the exposure and the initial Swift trigger time.

start(s)  exp(s)  mag limit
--------------------------------
-16.8     10.0    >10.3
3.2       10.0    >10.3
22.7      10.0    >10.3
51.8       5.0    >16.6
60.8       5.0    >16.9
149.8     10.0    >17.4
437.2     30.0    >17.9


GRB_name: GRB120422A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13259
SUBJECT: GRB 120422A: JCMT SCUBA-2 sub-mm observation
DATE:    12/04/24 01:16:41 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 counterpart to GRB 120422A (Troja et al., GCN Circ.
13243) using the SCUBA-2 sub-millimeter continuum camera on the James
Clerk Maxwell Telescope.  The observation started at 07:53 UT on
2012-04-22, corresponding to 41 minutes after the burst trigger.
Exposures totaling 1.5 hours were made in moderate weather conditions.
No source was detected, with a preliminary RMS of 2.8 mJy at 850 microns.

We thank William Montgomerie for his prompt support of these observations.


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13260
SUBJECT: GRB 120422A: 272 GHz observations from SMA
DATE:    12/04/24 16:44:53 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

S. Martn (ESO), G. Petitpas (SMA), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI) on behalf of a larger collaboration report:

We have observed the field of GRB 120422A (Troja et al. GCN 13243) with the Submillimeter Array (SMA, Hawaii, U.S.A.). Observations, with mean epoch  23.19 April 2012 (21.4 hours after the burst), were carried out with 8 antennas in very extended configuration at an average frequency of 272 GHz under excellent weather conditions (optical depth at 225 GHz ~0.03, equivalent to PWV~0.5mm). The short 57 minutes integration on source yielded a preliminary r.m.s. of 1.2 mJy. No source is detected at the position of the optical (Cucchiara et al. GCN 13245) and radio (Zauderer et al. GCN 13245) afterglow down to a 3-sigma limit of 3.6 mJy.

Considering the low redshift of 0.283 (Schulze et al. GCN 13257), this limit places GRB 120422A at the faint end of the luminosity distribution of mm/submm GRB afterglows (see Fig. 8 of de Ugarte Postigo et al. 2012, A&A, 538, 44), consistent with what has been seen for other local low-luminosity GRB/SN.

We acknowledge the excellent support of the SMA staff.


GRB_name: GRB120424A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13261
SUBJECT: GRB 120424A: MAXI/GSC detection of a burst
DATE:    12/04/25 12:00:14 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

M. Serino, T. Yamamoto, T. Mihara, M. Sugizaki, M. Matsuoka (RIKEN), 
S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa (JAXA),
N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech),
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:

At the scan transit centered at UT 2012-04-24 16:47:14,
MAXI/GSC detected a short X-ray transient lasting about 34 seconds 
within the 40 seconds triangular transit response of MAXI/GSC.
Judging from its high galactic latitude (-80deg) and spectral 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) = (+23.985deg,-29.879deg) = (01 35 56.40, -29 52 44.0)(J2000)

which has a statistical uncertainty of 16 arcmin at the 90% confidence limit 
and an additional systematic uncertainty of 6 arcmin (90% containment radius).

The preliminary flux (4-10 keV) of the source was 170 +- 30 mCrab.

There was no significant detection at the transit location in the
next orbit (92 min after the detection) with an upper limit of 20 mCrab.
Unfortunately the source position went out of view of the MAXI/GSC sky 
coverage at 2012/04/23 22:20, the upper limit at that time was 20 mCrab.
There is no known bright X-ray source at the detected position. 

Follow-up observations are encouraged.


GRB_name: GRB120422A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13263
SUBJECT: GRB 120422A: MITSuME Ishigakijima upper limit
DATE:    12/04/26 15:20:07 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 120422A (Troja et al., GCNC 13243)
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 2012-04-22 13:03:25 UT (~5.9 h after the
burst). We could not detect the previously reported afterglow
(Cucchiara et al., GCNC 13245) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
----------------------------------------------------------------------
0.27008    13:40:57   2880.0    >21.5   >21.3  >19.5
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120426A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13265
SUBJECT: IPN Triangulation of bright GRB 120426A
DATE:    12/04/27 15:48:46 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,

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,

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

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

The bright GRB 120426A has been observed by Fermi (GBM: trigger 
357098956), INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER (GRNS), and Swift 
(BAT), so far, at about 7754 s UT (02:09:14). 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:
   111.537 (07h 26m 09s) -65.631 (-65d 37' 53")
  Corners:
   111.594 (07h 26m 23s) -66.533 (-66d 31' 58")
   111.041 (07h 24m 10s) -65.195 (-65d 11' 41")
   111.487 (07h 25m 57s) -64.732 (-64d 43' 56")
   112.050 (07h 28m 12s) -66.066 (-66d 03' 59")
  ---------------------------------------------
The error box area is 0.355 sq. deg, and its maximum
dimension is 1.8 deg.

This box may be improved.

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


GRB_name: GRB120422A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13267
SUBJECT: GRB 120422A: Additional Gemini observations and Keck/LRIS spectroscopy
DATE:    12/04/27 16:45:33 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), A. Cucchiara (UCO/Lick), S. B. Cenko (UC 
Berkeley), A. J. Levan (Warwick), S. R. Kulkarni, S. Ben-Ami, and Y. Cao 
(Caltech) report:

We conducted a second epoch of imaging at the position of GRB 120422A 
(Troja et al., GCN 13243) with GMOS-N on Gemini-North starting at 05:42 
UT on 2012-04-26 in each of the griz filters.  Seeing conditions were 
excellent (0.7"), cleanly resolving the transient previously identified 
by Cucchiara et al. (GCN 12345) from its putative host galaxy.  A curved 
bridge of emission connects the transient with the host, suggesting it 
occurred either in a spiral arm (however no counter-arm is visible on 
the far side of the galaxy) or within an interacting companion.  An 
image is posted to:

http://www.astro.caltech.edu/~dperley/gcn/120422a/120422a_gmos.png

The transient has clearly faded since the last observations, and is now 
at r = 22.05 +/- 0.09 mag, i = 22.31 +/- 0.07 mag (using a 0.7" radius 
aperture and calibrating relative to SDSS standards, with the 
uncertainties due almost entirely to the systematics of the color 
comparison).  This would indicate a relatively blue color.  However, the 
(nearly contemporaneous) g-band flux lies approximately 1 magnitude 
below a simple extrapolation of the r-i color, indicating that the SED 
peaks in or near the r-band range.

As previously noted by Schulze et al. (GCN 13257) on the basis of the 
blue UVOT color, this type of SED is very unusual for traditional GRB 
afterglows (which normally are power-laws in the optical band) but 
similar properties have been seen at early times in GRBs 060218 (e.g. 
Campana et al., Nature 442:1008), as well as GRBs 100316D (Starling et 
al. 2011, MNRAS 411:2792), and 101225 (Thne et al. 2011, Nature 
480:72).  We suggest that the apparent color evolution of the peak 
wavelength of the transient from the UV to the optical and NIR is likely 
to continue in subsequent days, and encourage multi-band photometric 
follow-up as well as spectroscopy.

Additionally, on the night of 2012-04-27 UT we acquired 30 minutes of 
spectroscopy using LRIS on the Keck 10m telescope.  A preliminary flux 
calibration of the spectrum shows a similar signature as evident in the 
photometry, with a pronounced, smooth peak around 6500 Angstroms.  No 
obvious absorption or emission features are evident except for the 
narrow emission lines from the underlying host, previously mentioned by 
Tanvir et al. (GCN 13251) and Schulze et al. (GCN 13257).   In 
particular, we do not yet recognize any broad supernova signatures. 
Further observations are planned.


GRB_name: GRB120426A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13268
SUBJECT: Konus-Wind observation of GRB 120426A
DATE:    12/04/27 16:55:33 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 bright GRB 120426A
(IPN localization: Hurley at al., GCN 13265)
triggered Konus-Wind at T0=07755.610s UT (02:09:15.610)

The light curve shows a broad pulse with
a total duration of ~3.2 s.
The emission is seen up to ~8 MeV and displays
a noticeable hard-to-soft spectral evolution.
A spectral lag between the hard G3(1400-300 keV)
and the soft G1(25-90 keV) instrument's light curves
is estimated to 0.57  0.08 s (1 sigma).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120426_T07755/

As observed by Konus-Wind the burst
had a fluence of (1.9  0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.344 s,
of (1.3  0.1)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+2.048 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.61 (-0.10, +0.11),
the high energy photon index beta = -3.2 (-0.4, +0.2),
the peak energy Ep = 140(-8, +7) keV,
chi2 = 84.8/81 dof.

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


GRB_name: GRB120422A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13269
SUBJECT: GRB 120422A, the review of the sky area in plate archives
DATE:    12/04/28 08:26:21 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

We have undertaken the review of the sky area in vicinity of 
GRB 120422A (A.P. Beardmore et al. GCN Circ.13247) on 
astronegatives, collected in Ukrainian NAS Main astronomical 
observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek 
ScanMaker 9800XL TMA and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Ex. LimM Star USNOA2 
19921201/022312 GUA040C002050A 18.0 15.05 0975-06157849
19921201/025107 GUA040C002051 18.0 15.95 1575-06157752
19930114/232017 GUA040C002089A 22.5 15.05 0975-06157849
19930114/235112 GUA040C002090 22.5 15.05 0975-06157849
Plates:  
GUA040C the plates archive identifier of DWA (D/F=400/2000, 
         M=103"/mm) of the Ukrainian NAS Main Astro obs.
         (Marsden's number - 83) the plate number [1].
Ex.  -  Duration of the maximum exposure (minutes). 
LimM -  Limited V mag, derived in the 26 minutes area 
        around the location given in A.P. Beardmore et al. 
        GCN Circ.13247: RA(J2000): 09h 07m 38.46s,
                        Dec(J2000): +14d 01' 05.6"
Star USNOA2 - Comparison star.
  The preview images of 4 areas together with  
the 26x26 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120422A/index.html
The images with full resolution are available via e-mail on 
demand.
References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB120427A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13271
SUBJECT: IPN Triangulation of GRB 120427A
DATE:    12/04/28 16:51:31 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,

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 moderately intense single-pulsed GRB 120427A was observed by Fermi 
(GBM: trigger 357182249), INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER 
(GRNS), Mars Odyssey (HEND), and Suzaku (WAM) at about 4646 s UT (01:17:26).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   224.935 (14h 59m 44s) +29.311 (+29d 18' 39")
  Corners:
   224.688 (14h 58m 45s) +29.951 (+29d 57' 03")
   225.169 (15h 00m 41s) +29.418 (+29d 25' 06")
   225.175 (15h 00m 42s) +28.663 (+28d 39' 47")
   224.701 (14h 58m 48s) +29.203 (+29d 12' 11")
  ---------------------------------------------
The error box area is 1109 sq. arcmin (0.31 sq. deg), and its maximum
dimension is 81 arcmin (the minimum one is 28 arcmin). The Sun distance 
is ~136 deg.

This box may be improved.

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


