GRB 140311A
GCN Circular 15994
Subject
GRB 140311A: Mondy optical limits
Date
2014-03-18T20:40:18Z (12 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 140311A (Racusin et al., GCN 15944) with
AZT-33IK telescope of Mondy observatory on Mar. 12 and Mar. 13. Within
enhanced Swift-XRT error circle (Evans et al., GCN 15959) we do not
detect the optical afterglow (Xu et al., GCN 15947; Klotz et al., GCN
15952). Details of the photometry is following:
date UT start t-T0 Exp. Filter UpperLimit (3sigma)
(mid, days) (s)
2014-03-12 17:35:08 0.87145 25x120 R 21.4
2014-03-13 20:29:49 2.01082 51x120 R 21.6
The photometry is based on reference star SDSS-DR9, (R mag,
transformation by Lupton 2005):
N SDSS_id R(Lupton) err
J135713.39+003942.0 18.447 0.015
GCN Circular 15985
Subject
GRB 140311A: VLA Detection
Date
2014-03-16T03:24:52Z (12 years ago)
From
Tanmoy Laskar at Harvard U <tanmoylaskar@gmail.com>
T. Laskar, A. Zauderer, and E. Berger (Harvard) report:
"We observed the position of GRB 140311A (Racusin et al; GCN 15944) with
the VLA beginning on 2014 March 14.35 UT (2.48 days after the burst). At a mean
frequency of 21.8 GHz, we detect a radio source with a preliminary flux density
of ~ 0.25 mJy at
RA = 13:57:13.2763 +/- 0.0002
Dec = 00:38:31.423 +/- 0.003
consistent with the enhanced Swft/XRT position (Evans et al.; GCN 15959)
and the optical position (Xu et al.; GCN 15947). Follow-up observations are
planned."
GCN Circular 15980
Subject
GRB 140311A: further NOT observations
Date
2014-03-13T10:30:24Z (12 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), P. D'Avanzo (INAF/Brera), Y. F. Martinez Osorio
(NOT and Univ. Uppsala), report on behalf of the CIBO collaboration:
We observed the optical afterglow of GRB 140311A (Racusin et al., GCN
15944; Xu et al., GCN 15947) with the Nordic Optical Telescope equipped
with ALFOSC. A total exposure of 24 min was secured in the SDSS i band.
At a mean epoch of March 13.043 UT (1.16 days after the GRB), the
optical counterpart is well detected with an AB magnitude i = 22.45 +-
0.08, calibrated to several nearby SDSS stars. The position of the
afterglow is (J2000):
RA = 13:57:13.29
Dec = +00:38:31.7
referenced to the USNO-B1 catalog (0.3" error).
Compared to the i-band value reported by Littlejohns et al. (GCN 15978),
our measurement implies a decay index alpha = 0.81 +- 0.10 (Fnu propto
nu^-alpha), consistent with the value reported by these authors.
GCN Circular 15978
Subject
GRB 140311A: RATIR Optical and NIR Detection
Date
2014-03-13T00:11:31Z (12 years ago)
Edited On
2024-11-07T18:56:32Z (a year ago)
From
Owen Littlejohns at Az State U <olittlej@asu.edu>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
Owen Littlejohns (ASU), 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), Antonino Cucchiara (ORAU/GSFC), 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 140311A (Racusin, et al., GCN 15944) 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 12.24 to 2014/03 12.36
UTC (8.75 to 11.51 hours after the BAT trigger), obtaining a total of
2.10 hours exposure in the r and i bands and 0.89 hours exposure in the
Z and Y bands.
For a source within the Swift-XRT error circle (Evans, et al., GCN
15959), in comparison with the SDSS DR9 and 2MASS, we obtain the
following detections:
r 22.33 +/- 0.13
i 21.56 +/- 0.08
Z 20.58 +/- 0.08
Y 20.09 +/- 0.08
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. The source has faded in comparison
to observations from other facilities (D'Avanzo et, al., GCN 15953),
requiring a power-law with a temporal decay index of alpha = -0.83.
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 15976
Subject
GRB 140311A: Montarrenti Observatory optical upper limit
Date
2014-03-12T22:20:45Z (12 years ago)
From
Simone Leonini at Monarrenti Obs <s.leonini@iol.it>
S. Leonini, P. Rosi, M. Conti, G. Guerrini and L.M. Tinjaca Ramirez
(Montarrenti Observatory, Siena, Italy) report:
We observed the field of GRB140311A (Swift trigger 591390, Racusin et al., GCN
Circ. 15944) with the automatic 0.53m RC telescope + U47 detector at
Montarrenti Observatory (Siena, Italy, IAU code C88).
The observations were started at 2014-03-12 00:20:19 UT (approximately 3 hours
post-burst) stacking 5 unfiltered CCD exposures of 60s each.
We have not found optical transient within the error-box given by Swift.
Mag. upper limit R = 20.02+/-0.16
Magnitudes were obtained using Astrometrica software using USNO-B1 catalogue
and are not corrected for galactic extinction.
The message may be cited.
GCN Circular 15974
Subject
GRB 140311A: Kottamia I-band observation
Date
2014-03-12T19:43:56Z (12 years ago)
From
Michitoshi Yoshida at HASC,Hiroshima U <yoshidam@hiroshima-u.ac.jp>
M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)
We report the I-band photometry of GRB 140311A. The observation
was performed with the Newtonian camera of the 188cm telescope
at Kottamia observatory just before the R-band observation
reported by Yoshida et al. (GCN 15954; 15957). We started the
I-band observation at 21:57:30 UT on Marth 11 2014; 0.8706 hours
after the trigger.
Photometric result of the source is shown below. We used the
nearby star NOMAD1 0906-0229809 for flux calibration.
MID-UT T-EXP[sec] I[mag] err[mag]
---------------------------------------------------
2014-03-11 22:02:45 300.0 x 2 19.0 +- 0.1
---------------------------------------------------
GCN Circular 15973
Subject
GRB 140311A: Swift/UVOT Upper Limits
Date
2014-03-12T19:27:01Z (12 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
140311A 9540 s after the BAT trigger (Racusin et al. 2014, GCNC
15944). We do not detect any new source consistent with the Nansan
afterglow position (Xu et al. 2014, GCNC 15947) 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 summed exposures are presented below.
---------------------------------------------------
Filter TSTART TSTOP Exposure Mag
---------------------------------------------------
v 11,358 11,533 171 >19.0
b 37,852 38,759 885 >21.3
uvw1 40,124 40,366 238 >19.8
uvw2 10,542 11,352 886 >21.2
white 9540 10,446 885 >22.0
---------------------------------------------------
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) = 0.03 mag (Schlafly et al. 2011, ApJS, 737,
103). The non-detection in the UVOT data is consistent with a redshift
of z = 4.95 (Tanvir et al, 2014, GCNC 15961).
GCN Circular 15969
Subject
GRB 140311A: Bassano Bresciano Observatory optical upper limit
Date
2014-03-12T17:12:37Z (12 years ago)
From
Ulisse Quadri at Bassano Bresciano Obs <oabb@ulisse.bs.it>
U.Quadri, L.Strabla and R.Girelli report:
We imaged the field of GRB 140311A detected by SWIFT(trigger 591390)
with the robotic telescope of (IAU station 565) Bassano Bresciano
Observatory, Italy (member of ISSP:Italian Supernovae Search Project)
The observations started 1.89 hour after the GRB trigger,
with our Newton telescope D=250 mm F/D=5.
Weather conditions were good.
We co-added 15 exposures of 120 sec each.
We did not found any optical counterpart
in the error box of the XRTcandidate.
(J. L. Racusin (NASA/GSFC) et al, GCN 15944)
Start T0+ End T0+ R.Lim
1.89 hour 2.37 hour 18.5
Magnitudes were estimated with the USNO-B1.0 cat.
and are not corrected for galactic dust extinction.
The message may be cited.
GCN Circular 15968
Subject
GRB 140311A: Swift-XRT refined Analysis
Date
2014-03-12T17:02:28Z (12 years ago)
From
Luca Izzo at ICRA <Luca.Izzo@ICRA.it>
L. Izzo (URoma/ICRA), V. D'Elia (ASDC) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift-XRT team:
We have analysed 6.2 ks of XRT data for GRB 140311A (Racusin et al.
GCN Circ. 15944), from 9.5 ks to 57.1 ks after the BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 2850 s of PC mode
data and 7 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 = 209.30521, +0.64191 which is equivalent to:
RA (J2000): 13h 57m 13.25s
Dec(J2000): +00d 38' 30.9"
with an uncertainty of 1.5 arcsec (radius, 90% confidence).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.13 (+0.16, -0.14).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.61 (+0.17, -0.12). The
best-fitting absorption column is consistent with the Galactic value
of 2.8 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 3.9 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.8 x 10^20 cm^-2
Intrinsic column: 0 (+2.2, -0) x 10^22 cm^-2 at z=4.95
Photon index: 1.61 (+0.17, -0.12)
If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.1 x
10^-13 (5.3 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00591390
This circular is an official product of the Swift-XRT team.
GCN Circular 15966
Subject
GRB 140311A: Gemini-North redshift
Date
2014-03-12T16:33:51Z (12 years ago)
From
Ryan Chornock at Harvard <rchornock@cfa.harvard.edu>
R. Chornock (Harvard), D. B. Fox (Penn State), N. R. Tanvir (U. Leicester), and
E. Berger (Harvard) report:
We obtained 2x900s of spectroscopy of the optical afterglow (Xu et al., GCN
15947) of GRB 140311A (Racusin et al., GCN 15944) using GMOS on the 8-m Gemini-N
telescope beginning at 12:56 UT on March 12. We used the R831 grating to cover
the wavelength range of 6950-9075 Angs at a resolution of approximately 2.8
Angs. Our data exhibit a broad damped Lyman-alpha feature centered near 7250
Angs (redshift~4.95), in agreement with previous reports from Gemini-South
(Tanvir et al., GCN 15961) and NOT (D'Avanzo et al., GCN 15964). In addition,
we detect many metal lines, including C II, C II*, O I, O I*, Si II, Si II*, and
Si IV at a common redshift of 4.954, which we adopt as the redshift of the GRB.
We thank the Gemini staff, particularly Jesse Ball, for their excellent
assistance in obtaining these data.
GCN Circular 15964
Subject
GRB 140311A: NOT redshift confirmation
Date
2014-03-12T13:37:59Z (12 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
P. D'Avanzo (INAF-OAB), V. D'Elia (INAF-OAR/ASI-ASDC), S. Piranomonte
(INAF-OAR), A. Melandri (INAF-OAB), D. Malesani (DARK/NBI), T. Pursimo
(NOT), M. C. Baglio, I. Andreoni (INAF-OAB) report on behalf of the
CIBO collaboration:
Following the detection of the optical afterglow reported in D'Avanzo
et al. (GCN 15953), we carried out optical spectroscopy of GRB 140311A
(Racusin et al. GCN 15944) with the Nordic Optical Telescope (NOT)
equipped with ALFOSC. The observation consisted of two 1800 s
exposures covering the range between 3200 and 9100 A carried out at a
mean t-t0=3.37 hours.
Despite the low SNR and a seeing of ~2, we detect broad absorption
features at lambda ~ 7300 and 6100 AA which we interpret as Ly-alpha
and Ly-beta at z ~ 5.
This is consistent with the redshift reported by Tanvir et al(GCN 15961).
----------------------------------------------------------------
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GCN Circular 15962
Subject
GRB 140311A: Swift-BAT refined analysis
Date
2014-03-12T12:37:56Z (12 years ago)
From
Hans Krimm at NASA-GSFC <hans.krimm@nasa.gov>
H. A. Krimm (GSFC/USRA),S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),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-239 to T+423 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140311A (trigger #591390)
(Racusin, et al., GCN Circ. 15944). The BAT ground-calculated position is
RA, Dec = 209.293, 0.607 deg which is
RA(J2000) = 13h 57m 10.4s
Dec(J2000) = +00d 36' 23.9"
with an uncertainty of 3.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 10%.
The mask-weighted light curve shows two weak peaks, the first from roughly T-5
sec to T+5 sec and the second from approximately T+40 to T+60 sec. T90 (15-350
keV) is 71.4 +- 9.5 sec (estimated error including systematics).
The time-averaged spectrum from -4.456 to 83.736 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.67 +- 0.23. The fluence in the 15-150 keV band is 2.3 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-2.40 sec in the 15-150 keV band
is 1.3 +- 0.5 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/591390/BA/
GCN Circular 15961
Subject
GRB 140311A: Gemini-South redshift
Date
2014-03-12T11:51:40Z (12 years ago)
From
Nial Tanvir at U.Leicester <nrt3@star.le.ac.uk>
N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick),
K. Wiersema (U. Leicester), A. Cucchiara (NASA/GSFC) report:
We observed the afterglow of GRB 140311A (Racusin et al. GCN 15944;
Xu et al. GCN 15947) with Gemini-South using the GMOS-S spectrograph,
beginning March 12 08:24 UT, approximately 11.3 hours post-trigger.
The spectrograph was configured to cover wavelength range from
about 4000 AA to 6700 AA.
The optical trace of the afterglow is clearly detected, with many
absorption lines suggesting we are only seeing the region
blueward of Ly-alpha in the rest frame. Based on several strong
absorption features and a break, which would correspond to Ly-beta,
Ly-gamma, Ly-delta and the Ly-limit at approximately z=4.95, we
conclude this is likely to be the redshift of the GRB. Further
analysis of the spectrum is ongoing.
We thank the observatory staff, particularly Peter Pessev,
for excellent support in obtaining these observations.
GCN Circular 15959
Subject
GRB 140311A: Enhanced Swift-XRT position
Date
2014-03-12T09:56:51Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the
Swift-XRT team:
Using 1977 s of XRT Photon Counting mode data and 4 UVOT
images, we find an astrometrically corrected X-ray position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec =
209.30516, 0.64193 which is equivalent to:
RA (J2000): 13 57 13.24
Dec (J2000): +00 38 31.0
with an uncertainty of 1.8 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This position is 0.5 arc sec from the optical counterpart reported by
Xu et al (GCN Circ. 15947), thus we believe this is the X-ray afterglow.
This circular is an official product of the Swift-XRT team.
GCN Circular 15957
Subject
GRB 140311A: Recalibration of photometry of OT detected with Kottamia 188cm telescope
Date
2014-03-12T01:06:41Z (12 years ago)
From
Michitoshi Yoshida at HASC,Hiroshima U <yoshidam@hiroshima-u.ac.jp>
M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)
We performed recalibration of the photometry of the OT of GRB 140311A
(Racusin et al. GCN 15944), and found that the R-band magnitude we
previously reported (Yoshida et al. GCN 15954) is about 1 magnitude
fainter than the newly calibrated value. The recalibration result is
as follows:
MID-UT T-EXP[sec] R[mag] err[mag]
----------------------------------------
23:19:29 1800.0 20.9 +- 0.3
----------------------------------------
GCN Circular 15956
Subject
GRB 140311A: Nanshan afterglow decay
Date
2014-03-12T00:51:27Z (12 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:
The previously reported afterglow candidate (Xu et al., GCN 15947) has
been decaying throughout our R-band observations. Part of the
photometry are listed below
Tmid (hr) Mag(R) MagErr(R)
2.06778 21.06 0.10
1.53056 20.80 0.10
0.49306 19.96 0.10
All magnitude are calibrated with the following three SDSS stars using
Lupton (2005) transformation:
SDSS J135709.54+003731.9 m(r)=16.81, m(i)=16.30
SDSS J135716.45+003657.3 m(r)=16.41, m(i)=16.10
SDSS J135713.38+003942.0 m(r)=18.57, m(i)=18.47
Together with measurements in Klotz et al. (GCN 15952) and D'Avanzo et
al. (GCN 15953), it shows that the optical afterglow peaks at ~0.23 hr
post-burst and is decaying roughly as F(t) ~ t^-0.75 since ~0.5 hr
post-burst.
GCN Circular 15954
Subject
GRB 140311A: Optical follow-up observation with Kottamia 188cm telescope
Date
2014-03-12T00:41:43Z (12 years ago)
From
Michitoshi Yoshida at HASC,Hiroshima U <yoshidam@hiroshima-u.ac.jp>
M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)
We made an optical follow-up observation of GRB 140311A (Racusin
et al. GCN 15944) with the Newtonian CCD camera attached to the
188cm telescope at Kottamia astronomical observatory of NRIAG in
Egypt. We started the observation at 22:08:26 UT on Marth 11 2014;
1.053 hours after the trigger. We combined six 300 sec exposure
R-band frames and detected a faint point source at the position
of the optical transient reported by Xu et al. (GCN 15947).
Rough photometric result of the source is shown below. We used the
nearby star NOMAD1 0906-022793 (Klotz et al. GCN 15952) for flux
calibration.
MID-UT T-EXP[sec] R[mag] err[mag]
----------------------------------------
23:19:29 1800.0 21.9 +- 0.3
----------------------------------------
GCN Circular 15953
Subject
GRB 140311A: NOT observations of the optical afterglow
Date
2014-03-12T00:36:08Z (12 years ago)
From
Paolo D'Avanzo at INAF-OAB <paolo.davanzo@brera.inaf.it>
P. D'Avanzo, A. Melandri (INAF-OAB), D. Malesani (Dark/NBI), T. Pursimo (NOT), M. C. Baglio, I. Andreoni (INAF-OAB) report on behalf of the CIBO collaboration:
We observed the field of GRB 140311A (Racusin et al. GCN 15944) with the Nordic Optical Telescope (NOT) equipped with ALFOSC.
The optical afterglow reported by Xu et al. (GCN 15947) and Klotz et al. (GCN 15952) is detected in the R band at 21.1 +/- 0.2 mag (calibrated against the USNOB1 catalogue) at t-t0=2.6 hours.
GCN Circular 15952
Subject
GRB 140311A: Zadko observatory - Gingin optical observations
Date
2014-03-12T00:10:54Z (12 years ago)
From
Alain Klotz at IRAP-CNRS-OMP <Alain.Klotz@free.fr>
A. Klotz, D. Turpin (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D.
Coward (UWA),
M. Boer, B. Gendre, K. Siellez, H. Dereli, O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA)
report:
We imaged the field of GRB 140311A detected by SWIFT
(trigger 591390) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.
The observations started 119.5s after the GRB trigger
(46.9s after the notice). The elevation of the field was at
45 degrees above horizon and weather conditions
were good.
The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect the OT discovered by Xu et al. GCNC 15947
with a limiting magnitude of:
t0+119.5s to t0+179.5s : Rlim = 19.5
The second image is 30.0s exposure in tracking mode
We detect the OT discovered by Xu et al. GCNC 15947:
t0+208s to t0+238s : R = 19.6 +/- 0.5
Follow-up was performed until the dawn which arrived
18 minutes after the trigger.
We co-added a series of exposures:
t0+208s to t0+325s : R = 19.9 +/- 0.3
t0+338s to t0+515s : R = 19.2 +/- 0.3
t0+530s to t0+1111s : R = 18.5 +/- 0.3
Conclusions, the afterglow brightness increases
slowly during the first 18 minutes after the trigger.
Magnitudes were estimated with the nearby star
NOMAD1 0906-0229793 (R=16.44) and are not corrected
for galactic dust extinction.
GCN Circular 15947
Subject
GRB 140311A: Nanshan OT detection
Date
2014-03-11T21:56:00Z (12 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 BAT error circle of GRB 140311A (Racusin et al., GCN
15944) using the 1m telescope located in Nanshan, Xinjiang, China.
Observations started at 21:26:44 UT on 2014-03-11 and some R-band
frames were obtained.
A seemingly varying optical source is clearly detected in each image
at coordinates
R.A. (J2000) = 13:57:13.27
Dec. (J2000) = +00:38:31.07
Uncertainty radius: ~1 aecsec
This object is not present in both SDSS and DSS. We thus suggest it
may be the afterglow of the burst.
Observations are ongoing.
GCN Circular 15946
Subject
GRB 140311A: MASTER early optical observations
Date
2014-03-11T21:53:51Z (12 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 GRB140311A 27 sec after trigger time
and 127 sec after trigger
time at 2014-03-11 21:07:23 UT in two polarizations. On our first (30s
exposure) set we haven`t found optical transient within SWIFT error-box
(Racusin et. al GCN 15944).
The 5-sigma upper limit has been about 16.27mag
MASTER II robotic telescope located in Blagoveschensk was pointed to the GRB140311A 10 sec after
notice time and 89 sec after trigger time at 2014-03-11 21:06:45 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 14mag. The observations made on the
morning sky.
The message may be cited.
GCN Circular 15944
Subject
GRB 140311A: Swift detection of a probable burst
Date
2014-03-11T21:20:47Z (12 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
J. L. Racusin (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:
At 21:05:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140311A (trigger=591390). Swift could not immediately
slew to the burst due to the Earth limb constraint.
The BAT on-board calculated location is
RA, Dec 209.301, +0.612 which is
RA(J2000) = 13h 57m 12s
Dec(J2000) = +00d 36' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). This is an image trigger and we cannot
say much about the light curve.
Due to an observing constraint, Swift will not slew until T0+50.6
minutes. There will be no XRT or UVOT data until this time.
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.)