GRB 140521A
GCN Circular 16311
Subject
GRB 140521A: Swift detection of a burst
Date
2014-05-21T17:51:56Z (11 years ago)
From
Eleonora Troja at GSFC <eleonora.troja@nasa.gov>
E. Troja (NASA/GSFC/UMCP), S. B. Cenko (GSFC),
J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), L. M. Z. Hagen (PSU),
L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:
At 17:34:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140521A (trigger=599546). Swift did not slew to the burst
due to an observing constraint. The BAT on-board calculated location
is RA, Dec 320.013, +67.602 which is
RA(J2000) = 21h 20m 03s
Dec(J2000) = +67d 36' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of about 12 sec. The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0.1 sec after the trigger.
Due to an observing constraint, Swift will not
slew until 00:39UT on May 22. There will be no XRT or UVOT
data until this time.
Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN Circular 16312
Subject
GRB 140521A: MASTER optical observations
Date
2014-05-21T22:28:09Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Vladimirov, P.Balanutsa, E. Gorbovskoy, V. Lipunov, V.Kornilov,
D.Kuvshinov, A.Belinski, N.Tyurina,
N.Shatskiy, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko,
A.Sankovich, A. Krylov, M.Pruzhinskaya
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University
V.Krushinski, I.Zalozhnih, A. Popov
Ural Federal University, Kourovka
Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Vostryakovo (Alexander Krylov Observatory) was pointed to the
GRB140521A 4553 sec after trigger time at 2014-05-21 18:50:11 directly
after sunset. We haven`t found optical transient within SWIFT error-box
(Troja et. al GCN 16311) on single and coadd images.
In table 1 the images upper limits are provided.
Table 1.
-------
T_start Exptime T-T_mead T-T_start T-T_stop Filter mlimit Coadd
2014-05-21 18:50:11 15 4561 4553 4568 C 14.5 1*
2014-05-21 19:10:18 600 6531 5760 7302 C 18.0 10
2014-05-21 19:10:18 1020 7210 5760 8659 C 18.8 17
2014-05-21 19:38:52 600 8067 7474 8659 C 18.7 10
2014-05-21 20:07:53 1200 10390 9215 11566 C 19.4 20
-----------------------------------------------------------------------------------
* First image with stars on bright evening sky.
C is our white (clear) band which is well described by a parity 0.8R+0.2B (USNO B1).
T is a GRB trigger time.
Another two MASTER II robotic telescope located in Kislovodsk and Blagoveschensk
was pointed to the GRB140521A 21 sec after notice time and 36 sec after
trigger time at 2014-05-21 17:34:54 UT. But observations were spoiled due
to bad weather condition. We have a set of images from that observatories
with different exposures from 10 to 180 and formal upper limit from 13 to
16 during first hour after the burst. However bad quality of images (due
to wind and clouds) don't allow to carry out transient search.
The message may be cited.
GCN Circular 16314
Subject
GRB 140521A: MITSuME Okayama upper limits
Date
2014-05-22T07:20:25Z (11 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME and OISTER collaboration:
We observed the field of GRB 140521A (Troja et al., GCNC 16311)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2014-05-21 17:35:25 (~68 sec after the burst).
We did not find any new point source within the BAT circle
(Troja et al., GCNC 16311) in all the three bands.
Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' Rc Ic
-----------------------------------------------------
0.02943 18:16:40 4320.0 >19.5 >19.3 >18.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 16315
Subject
GRB 140521A: AROMA-N Optical Observation
Date
2014-05-22T10:31:49Z (11 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
D. Kawamura, T. Sakamoto, I. Takahashi, A. Yoshida (AGU)
We observed the field of GRB 140521A detected by Swift (trigger #599546;
Troja et al., GCN Circ. 16311) with the 12-inch AGU Robotic Optical
Monitor for Astrophysical object - Narrow (AROMA-N) located at the Sagamihara
campus of Aoyama Gakuin University.
15 images of 60 sec exposures were taken in the R filter starting from
May 21 17:36:17 (UT) about 119 sec after the trigger
(104 sec after the BAT position notice) and stopped on May 21 18:03:04 (UT).
We do not detect the optical afterglow both in the individual images and
the stacked image inside the BAT flight position (Troja, et al., GCN #16311).
The estimated five sigma upper limit of the combined image (total exposure of 900 sec)
is ~17.2 mag using the USNO-B1 catalog.
GCN Circular 16316
Subject
GRB 140521A: Swift-BAT refined analysis
Date
2014-05-22T13:27:00Z (11 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140521A (trigger #599546)
(Troja, et al., GCN Circ. 16311). The BAT ground-calculated position is
RA, Dec = 320.177, 67.587 deg, which is
RA(J2000) = 21h 20m 42.6s
Dec(J2000) = +67d 35' 12.7"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 55%.
The mask-weighted light curve shows a single peak starting at ~T-2 sec,
peaking at ~T+1 sec, and ending at ~T+11 sec with a tail out to ~T+50 sec.
T90 (15-350 keV) is 9.88 +- 1.09 sec (estimated error including systematics).
The time-averaged spectrum from T+0.15 to T+11.44 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.42 +- 0.11. The fluence in the 15-150 keV band is 9.5 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.64 sec in the 15-150 keV band
is 1.9 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/599546/BA/
GCN Circular 16317
Subject
GRB 140521A: AAO optical observations
Date
2014-05-22T13:59:41Z (11 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed a field of the Swift GRB 140521A(Troja et al., GCN 16311)
with AS-32 (0.7m) telescope of Abastumani Observatory starting on May,
21 (UT) 18:12:00. We obtained several unfiltered frames with exposure
of 120 s. Within the BAT ground-calculated position (Barthelmy et al.,
GCN 16316) we do not detect evident variable source. Since our stacked
image is somewhat deeper than USNO-B1.0 we need one more epoch of
observation.
The details of the photometry are the following:
UT start t-T0 Filter Exp. Uplim
(mid, days) (s) (3 sigma)
2014-05-21 18:12:00 0.05746 None 28*120 21.2
and based on USNO-B1.0 star 1575-0248114 (21:20:10.32 +67:35:37.5)
assuming R=15.70.
GCN Circular 16319
Subject
GRB 140521A: Fermi GBM Detection
Date
2014-05-22T19:18:56Z (11 years ago)
From
Matthew Stanbro at UAH/Fermi <mcs0001@uah.edu>
Matthew Stanbro (UAH) reports on behalf of the Fermi GBM Team:
"At 17:34:18.73 UT on 21 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140521A (trigger 422386461 / 140521732)
which was also detected by Swift (E. Troja et al. 2014, GCN 16311).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.
The GBM light curve consists of one main episode with a total
duration (T90) of about 11.5 s (50-300keV). The time-averaged
spectrum from T0-0.864 s to T0+10.400 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.04 +/- 0.08 and the cutoff energy,
parameterized as Epeak, is 273 +/- 44 keV.
The event fluence (10-1000 keV) in this time interval is
(2.99 +/- 0.21)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-0.10 s in the 10-1000 keV band is 3.9 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 16320
Subject
GRB 140521A : Xinglong TNT upper limit
Date
2014-05-23T07:50:38Z (11 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
L. P. Xin, X. F. Wang, J. Y. Wei, Y. L. Qiu, J. S. Deng,
J. Wang, X. H. Han and C. Wu on behalf of EAFON report:
We began to observe GRB 140521A (Troja et al., GCN 16311)
with Xinglong 0.8-m TNT telescope at 15:35:50 (UT) ,
92 sec after the burst.
No any optical transient was detected in our single or stacked image.
The 3-sigma upper limit magnitude is about 18.4 mag at the mean time of
7.3 min , calibrated by nearby USNO B1.0 R2 mag.
The message may be cited.
GCN Circular 16372
Subject
GRB 140521A: AAO optical upper limit
Date
2014-06-09T19:46:36Z (11 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed second epoch of the field of the Swift GRB 140521A (Troja et
al., GCN 16311) with AS-32 (0.7m) telescope of Abastumani Observatory
starting on May, 22 (UT) 21:34:30. We obtained several unfiltered
frames with exposure of 120 s. In comparison with our first epoch
observation (Volnova et al., GCN 16317) we do not detect any variable
source within the BAT ground-calculated position (Barthelmy et al., GCN
16316).
A photometry is based on the same reference star used in first epoch
(see GCN 16311):
UT start t-T0 Filter Exp. Uplim
(mid, days) (s) (3 sigma)
2014-05-22 21:34:30 1.12809 None 38*120 21.5