GRB 140311B
GCN Circular 15945
Subject
GRB 140311B: Swift detection of a burst
Date
2014-03-11T21:36:02Z (11 years ago)
From
Judith Racusin at GSFC <judith.racusin@nasa.gov>
J. L. Racusin (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC),
B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:
At 21:14:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140311B (trigger=591392). Swift could not immediately
slew to the burst due to the Earth limb constraint.
The BAT on-board calculated location is
RA, Dec 252.291, +52.747 which is
RA(J2000) = 16h 49m 10s
Dec(J2000) = +52d 44' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). We are awaiting information on the BAT
light curve.
Due to an observing constraint, Swift will not slew until T0+55
minutes. There will be no XRT or UVOT data until this time.
The observation of this burst will delay the observation of GRB 140311A.
Burst Advocate for this burst is J. L. Racusin (judith.racusin AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN Circular 15948
Subject
GRB 140311B: MASTER early optical observations
Date
2014-03-11T22:02:51Z (11 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, M. Pruzhinskaya, D.Denisenko, V.Kornilov,
N.Tyurina,
P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov
Lomonosov Moscow 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.Zalozhnih, A. Popov
Ural Federal University, Kourovka
Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the GRB140311B 29 sec after notice time
and 107 sec after trigger time at 2014-03-11 21:16:16 UT in two
polarizations. On our first (20s exposure) set we haven`t found optical
transient within SWIFT error-box (Racusin et. al. GCN 15945). The 5-sigma
upper limit has been about 17.0 mag. The observations is proceed.
MASTER II robotic telescope located in Blagoveschensk was pointed to the
GRB140311B 9 sec after notice time and 85 sec after trigger time at
2014-03-11 21:15:54 UT in two polarizations. On our first (20s exposure)
set we haven`t found optical transient within SWIFT error-box.
The 5-sigma upper limit has been about 14.0 mag. The observations on this
place made on the bright morning sky.
The message may be cited.
[GCN OPS NOTE(12mar14): Per author's request, the Subject was changed
from "MASTER OT light curve (fwd)" to "MASTER early optical observations".]
GCN Circular 15949
Subject
GRB 140311B: Nanshan afterglow detection
Date
2014-03-11T22:52:01Z (11 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), C.-H. Bai, X. Zhang, A. Esamdin, L. Ma (XAO) report:
We observed the field of GRB 140311B (Racusin et al., GCN 15945)
using the 1m telescope located in Nanshan, Xinjiang, China.
Observations started at 21:41:05 UT on 2014-03-11 and some 300s/600s
R-band frames were obtained.
The afterglow is detected in each image within the XRT error circle
(http://www.swift.ac.uk/sper/) at coordinates
R.A. (J2000) = 16:49:17.97
Dec. (J2000) = +52:43:26.41
Uncertainty radius: ~1.5 aecsec
The first 300s image reveals that the afterglow has m(R)=20.6 at 29.1
min post-burst, calibrated with nearby two SDSS stars.
Observations are ongoing.
GCN Circular 15950
Subject
GRB 140311B: Swift-XRT observations
Date
2014-03-11T23:07:34Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.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 140311B at 22:11:04.3 UT,
3394.7 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 252.32458,
52.72393 which is equivalent to:
RA(J2000) = 16h 49m 17.90s
Dec(J2000) = +52d 43' 26.1"
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 consistent with the Galactic value of 3.03
x 10^20 cm^-2 (Kalberla et al. 2005).
GCN Circular 15951
Subject
GRB140311B: Swift/XRT position
Date
2014-03-11T23:08:55Z (11 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
V. D'Elia (ASDC), L. Izzo (URoma/ICRA) and J. Racusin (NASA/GSFC) report:
XRT began observing GRB140311B (Racusin et al. GCN 15945) 55 minutes
after the trigger.
Using promptly downlinked data we find a bright uncatalogued X ray
source located at RA,Dec = 252.3242, 52.7240 which is equivalent to:
RA� (J2000.0) =� 16 49 17.81
DEC (J2000.0) =� +52 43 26.4
with an uncertainty of 3.6 arcsec (radius, 90% containment). This
location is 109.6 arcsec from the BAT position, inside the BAT error
circle.
This is an official product of the Swift/XRT team.
----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.
GCN Circular 15955
Subject
GRB 140311B: TAROT Calern observatory optical observations
Date
2014-03-12T00:42:49Z (11 years ago)
From
Alain Klotz at IRAP-CNRS-OMP <Alain.Klotz@free.fr>
Klotz A., Turpin D. (IRAP-CNRS-OMP), Gendre B.,
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:
We imaged the field of GRB 140311B detected by SWIFT
(trigger 513505) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.
The observations started 5 minutes after the GRB trigger
The elevation of the field increased from
20 degrees above horizon and weather conditions
were good.
The first image is 60.0s exposure in tracking mode.
We do not detect the OT discovered by Xu et al.
(GCNC 15949) with a limiting magnitude of:
t0+246s to t0+306s : Rlim = 17.3
We co-added a series of exposures:
We do not detect the OT with limiting magnitudes of:
t0+246s to t0+511s : Rlim = 17.8
t0+541s to t0+1568s : Rlim = 18.4
Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.
N.B. Galactic coordinates are lon= 80.3934 lat=+39.5637
and the galactic extinction in R band is about 0.2 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.
This message may be cited.
GCN Circular 15958
Subject
GRB 140311B: Enhanced Swift-XRT position
Date
2014-03-12T02:30:17Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2577 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 140311B, 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 = 252.32518, +52.72426 which is equivalent
to:
RA (J2000): 16h 49m 18.04s
Dec (J2000): +52d 43' 27.3"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 15960
Subject
GRB 140311B: final MASTER OT light curve
Date
2014-03-12T10:53:33Z (11 years ago)
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, M. Pruzhinskaya, D.Denisenko, V.Kornilov, N.Tyurina,
P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute
V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinski, I.Zalozhnih, A. Popov
Ural Federal University, Kourovka
Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)
MASTER-II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the GRB140311B (Racusin et al., GCN
15945) 29 sec after notice time and 107 sec after trigger time (Gorbovskoy
et. al GCN 15948 ) and made observations during ~ 1.5 h before sunrise.
We see OT (Xu et. al. GCN 15949) only on several coadditional images. On
all of them the object is close to limit and has s/n from 3 to 6.
Our preliminary ligth curve available in table below and on image here
http://master.sai.msu.ru/static/GRB/grb140311B.png.
T_start T_t-T_m Exptime Mag. Coadd
[s] [s] [m]
21:17:12 326 220 19.4 4
21:18:18 432 300 19.0 4
21:16:16 557 650 19.4 8
21:19:44 557 380 18.7 4
21:19:44 661 550 18.9 5
21:21:19 708 490 18.9 4
21:18:18 834 960 19.4 8
21:25:40 1485 1380 19.8 8
21:25:40 1702 1740 20.0 10
T_t is GRB trigger time, T_m is middle time of our exposure.
Our unfiltered magnitude is well described by a parity 0.8R + 0.2B (USNO
B1)
The power low index alpha from 380 to 1740 seconds after the trigger is
1.07+-0.10 (F ~ t-apha).
We also apologize for an error in the title of our previous telegram (GCN
15948) if it misled somebody.
The message may be cited.
GCN Circular 15963
Subject
GRB 140311B: Swift-XRT refined Analysis
Date
2014-03-12T13:20:17Z (11 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
V. D'Elia (ASDC), L. Izzo (URoma/ICRA) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift-XRT team:
We have analysed 7.8 ks of XRT data for GRB 140311B (Racusin et al.
GCN Circ. 15945), from 3.4 ks to 46.3 ks after the BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 15958).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.66 (+0.18, -0.15).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.68 (+0.25, -0.23). The
best-fitting absorption column is 1.6 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 3.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.1 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.6 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: 2.7 sigma
Photon index: 1.68 (+0.25, -0.23)
If the light curve continues to decay with a power-law decay index of
1.66, the count rate at T+24 hours will be 9.6 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.0 x
10^-14 (4.8 x 10^-14) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00591392.
This circular is an official product of the Swift-XRT team.
GCN Circular 15970
Subject
GRB 140311B: RATIR Optical and NIR Observations
Date
2014-03-12T17:17:37Z (11 years ago)
Edited On
2024-11-07T19:51:21Z (7 months ago)
From
Owen Littlejohns at Az State U <olittlej@asu.edu>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
Owen Littlejohns (ASU), Antonino Cucchiara (ORAU/GSFC), Nat
Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein
(UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Eleonora Troja (GSFC), Enrico Ramirez-Ruiz (UCSC),
José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González
(UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:
We observed the field of GRB 140311B (Racusin, et al., GCN 15945)
with the Reionization and Transients Infrared Camera
(RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the
Observatorio Astronómico Nacional on Sierra San Pedro Mártir from
2014/03 12.37 to 2014/03 12.52 UTC (11.52 to 15.25 hours after the
BAT trigger), obtaining a total of 2.84 hours exposure in the r and
i bands and 1.19 hours exposure in the Z and Y bands.
For a source within the Swift-XRT error circle, in comparison with
the SDSS DR9 and 2MASS, we obtain the following upper limits (3-sigma):
r > 23.99
i > 23.82
Z > 22.85
Y > 22.26
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the earlier
detection of the optical afterglow (Xu, et al., GCN 15949) the GRB has
faded. A power-law temporal decay with an index of alpha = -0.94 or
steeper is required for our r-band upper limit to be consistent with the
earlier detection.
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 15972
Subject
GRB 140311B: Swift/UVOT Upper Limits
Date
2014-03-12T19:26:59Z (11 years ago)
From
Stephen Holland at STScI <sholland@stsci.edu>
S. T. Holland (STScI) and J. L. Racusin (NASA/GSFC) report on behalf
of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB
140311B 3398 s after the BAT trigger (Racusin et al. 2014, GCNC
15945). We do not detect any new source consistent with the Nansan
afterglow position (Xu et al. 2014, GCNC 15949) in any of the UVOT
exposures. Preliminary 3-sigma upper limits, using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373),
for the finding chart and summed exposures are presented below.
---------------------------------------------------
Filter TSTART TSTOP Exposure Mag
---------------------------------------------------
white (FC) 3398 3548 147 >21.2
---------------------------------------------------
v 3555 5191 393 >20.0
b 4375 5990 372 >20.4
u 4170 5806 393 >20.2
uvw1 3965 5601 393 >20.3
uvm2 3760 5396 393 >20.2
uvw2 4787 4986 197 >20.1
white 4580 4780 197 >21.4
---------------------------------------------------
The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.05 mag (Schlafly et al. 2011, ApJS, 737,
103).
GCN Circular 15975
Subject
GRB 140311B: Fermi GBM Detection
Date
2014-03-12T20:40:40Z (11 years ago)
From
Matthew Stanbro at UAH/Fermi <mcs0001@uah.edu>
M. Stanbro (UAH) reports on behalf of the Fermi GBM Team:
"At 21:14:35.65 UT on 11 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140311B (trigger 416265278/140311885),
which was also detected by Swift (J. L. Racusin et al. 2014, GCN 15945).
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/BAT location.The angle to the
Fermi LAT boresight is 110 deg. from Swift location.
The GBM light curve consists of several overlapping peaks with a
combined duration (T90) of 72 s (50-300 keV).
The time-averaged spectrum from T0-3 s to T0+69 s is
well fit by a power law function with an exponential
high energy cutoff. The power law index is -0.5 +/- 0.1
and the high energy cutoff, parameterized as
Epeak, is 117 +/- 8 keV.
The event fluence (10-1000 keV) in this time interval is
(7.9 +/- 0.4)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+0.6 s in the 10-1000 keV band
is 3.2 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15979
Subject
GRB 140311B: Swift-BAT refined analysis
Date
2014-03-13T03:07:06Z (11 years ago)
From
Jay R. Cummings at NASA/GSFC/Swift <james.r.cummings@nasa.gov>
A. Y. Lien (NASA/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (looking), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-0 to T+3 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140311B (trigger #591392)
(Racusin, et al., GCN Circ. 15945). The BAT ground-calculated position is
RA, Dec = 252.333, +52.733 deg which is
RA(J2000) = 16h 49m 20.0s
Dec(J2000) = +52d 44' 00"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
This trigger followed that of GRB 140311A by only about 9 minutes, which led
to a complication in recording the photon-event data. Only 3 seconds of
photon-event data was recorded, so no mask-weighted lightcurve is available.
T90 (15-350 keV) is estimated to be 70 +- 10 sec. The burst had multiple
peaks. Peak emission occurred about 15 seconds after the trigger time.
The time-averaged spectrum for the limited range of data available (about
5% of T90) from T+0 to T+3 sec is best fit by a simple power-law model. The
power law index of the time-averaged spectrum is 1.12 +- 0.15 (90% confidence).
Because of the lack of event data, the fluence is not available. Based on an
eye-ball estimate comparing the non-maskweighted lightcurve to those of other
bursts with a similar partial coding, the fluence in the 15-150 keV band was on
the order of several times 10^-6 ergs/cm^2
GCN Circular 15995
Subject
GRB 140311B: Mondy optical limit
Date
2014-03-18T20:45:27Z (11 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A.Volnova (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich
(ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:
We observed the field of GRB 140311B (Racusin et al., GCN 15945) with
AZT-33IK telescope of Mondy observatory starting on Mar. 12 (UT)
20:21:16. Within enhanced Swift-XRT eror circle (Evans et al., GCN
15958) we do not detect the optical afterglow (Xu et al., GCN 15949).
Details of the photometry is following:
date UT start t-T0 Exp. Filter UpperLimit (3sigma)
(mid, days) (s)
2014-03-12 20:21:16 0.98389 30x120 R 20.2
The photometry is based on reference star SDSS-DR9, (R mag,
transformation by Lupton 2005):
N SDSS_id R(Lupton) err
J164910.91+524333.6 17.449 0.009