GRB 140114A
GCN Circular 15756
Subject
GRB 140114A: optical upper limit
Date
2014-01-21T08:34:59Z (12 years ago)
From
Alina Volnova at SAI MSU <alinusss@gmail.com>
A. Volnova (IKI), R. Inasaridze (AAO), Yu. Krugly (IA KhNU), I. Slyusarev
(IA KhNU), G. Inasaridze (AAO), V. Zhuzhunadze (AAO), I. Slyusarev (IA
KhNU), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:
We observed the field of Swift GRB 140114A (Troja et al., GCN 15728) on
Jan., 15 with AS-32 (0.7m) telescope of Abastumani Observatory, and AZT-8
(0.7m) telescope of Institute of Astronomy, Kharkiv National University. We
obtained several unfiltered frames with exposures of 120 s (AS-32), and
several frames with filter R with exposure of 120 s (AZT-8). Within the
enhanced XRT circle (Beardmore et al., GCN 15733) we did not detect the
afterglow reported by Butler et al. (GCN 15732).
The details of the photometry are the following:
Telescope t_start, UT t-T0, mid, days Exptime,s Filter Uplim, 3 sigma
AS-32 00:07:23 0.54452 40*120
None 20.6
AZT-8 00:29:00 0.54720 32*120 R
20.8
The photometry is based on SDSS stars, R mag (R mag obtained using ugriz
transformations in BVRI (Lupton, 2005):
SDSS id R
J123415.64+275948.8 16.079 J123342.40+275950.2 15.120
GCN Circular 15743
Subject
GRB 140114A: NOT afterglow observations
Date
2014-01-15T16:25:02Z (12 years ago)
From
Zach Cano at U of Iceland <zcano@mail.com>
Z. Cano (U. Iceland), D. Xu, D. Malesani (DARK/NBI), P. Jakobsson (U Iceland), T. Pursimo (NOT) report on behalf of a larger collaboration:
We observed the field of GRB 140114A (Troja et al., GCN Circ. 15728) with the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC starting at 03:19 UT on 15-Jan-2014. We obtained 12x300 s frames in SDSS-i at a mean time of 15.93 hr after the burst.
The afterglow is clearly detected in the stacked image at coordinates:
RA: 12:34:05.1
Dec: +27:57:02.6
with an uncertainty of 0.5''. This position is 1.4'' from the enhanced XRT position (Beardmore et al., GCN Circ. 15733), and falls within the enhanced XRT error circle. This is presumably the source detected by Butler et al. (GCN Circ. 15732). The afterglow has m(i)=23.19+/-0.16 AB at 15.93 hr post-burst, calibrated with the nearby SDSS stars and not corrected for foreground extinction.
GCN Circular 15742
Subject
GRB 140114A: Continued RATIR Optical and NIR Observations
Date
2014-01-15T15:20:07Z (12 years ago)
Edited On
2024-11-07T19:44:54Z (a year ago)
From
Nat Butler at Az State U <natbutler@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>
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), Owen Littlejohns (ASU), 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 140114A (Troja et al., GCN 15728) 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 2014/01 15.32 to 2014/01 15.55 UTC (19.72 to
25.20 hours after the BAT trigger), obtaining a total of 3.36 hours
exposure in the r and i bands and 1.48 hours exposure in the Z, Y, J, and H
bands.
The optical/NIR source detected by RATIR last night (Butler et al., GCN
15732) has now faded below our detection limit. In comparison with the
SDSS DR9 and 2MASS, we obtain the following upper limits (3-sigma):
r > 23.67
i > 23.52
Z > 22.56
Y > 21.98
J > 21.87
H > 21.33
These magnitudes are in the AB system and are not corrected for
Galactic extinction in the direction of the GRB.
GCN Circular 15741
Subject
GRB 140114A: MITSuME Okayama upper limits
Date
2014-01-15T04:41:49Z (12 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 collaboration:
We observed the field of GRB 140114A (Troja et al., GCNC 15728)
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 2014-01-14 14:12:05 UT (~2.2 h after the burst).
We could not detect the previously reported afterglow (Butler et al., GCNC
15732) 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
-----------------------------------------------------
0.13037 15:05:24 6000.0 >18.9 >19.3 >18.6
0.29802 19:06:49 6300.0 >20.1 >20.3 >19.4
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 15740
Subject
GRB 140114A: ROTSE-III Optical Limits
Date
2014-01-15T01:07:06Z (12 years ago)
From
Farley V. Ferrante at Southern Methodist U/ROTSE <fferrante@smu.edu>
T. Guver (Istanbul Univ.), F. V. Ferrante (SMU), R. Kehoe (SMU), G. Dhungana
(SMU), and W. Zheng (UC Berkely) report on behalf of the ROTSE GRB team:
ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
140114A (Swift trigger 583861; Troja et al, GCN 14728), producing images
beginning 22.4 s after the GCN notice time. An automated response took the
first image at 11:59:20.4 UT, 98.1 s after the burst, under fair conditions.
We took 10 5-sec, 10 20-sec and 9 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; the field is not crowded.
Individual images have limiting magnitudes ranging from 14.0-15.1; we set
the following specific limits.
start UT end UT t_exp(s) mlim t_start-t_GRB(s) Coadd?
---------------------------------------------------------------------------
11:59:20.4 11:59:25.4 5 14.0 98.1 N
11:59:20.4 11:60:20.4 60 15.0 98.1 N
GCN Circular 15739
Subject
GRB 140114A: Swift-XRT refined Analysis
Date
2014-01-15T00:23:05Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
V. Mangano (PSU), M.C. Stroh (PSU), P.A. Evans (U. Leicester), B.P.
Gompertz (U. Leicester), J.P. Osborne (U. Leicester), B. Sbarufatti
(INAF-OAB/PSU), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D.N. Burrows
(PSU) and E. Troja report on behalf of the Swift-XRT team:
We have analysed 11 ks of XRT data for GRB 140114A (Troja et al. GCN
Circ. 15728), from 118 s to 24.7 ks after the BAT trigger. The data
comprise 449 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 15733).
The late-time light curve (from T0+5.0 ks) can be modelled with a
power-law decay with a decay index of alpha=0.50 (+/-0.15).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.22 (+/-0.03). The
best-fitting absorption column is 1.53 (+/-0.07) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.33 (+0.21, -0.20)
and a best-fitting absorption column of 1.3 (+0.5, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.1 x 10^-11 (4.8 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.3 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 4.5 sigma
Photon index: 2.33 (+0.21, -0.20)
If the light curve continues to decay with a power-law decay index of
0.50, the count rate at T+24 hours will be 0.020 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-13 (9.6 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/00583861.
This circular is an official product of the Swift-XRT team.
GCN Circular 15738
Subject
GRB 140114A: Swift-BAT refined analysis
Date
2014-01-14T22:29:15Z (12 years ago)
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), N. Gehrels (GSFC), 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-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140114A (trigger #583861)
(Troja, et al., GCN Circ. 15728). The BAT ground-calculated position is
RA, Dec = 188.498, 27.942 deg, which is
RA(J2000) = 12h 33m 59.6s
Dec(J2000) = +27d 56' 31.9"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows one roughly symmetrical peak starting
at ~T+10 sec, peaking at ~T+100 sec, and ending at ~T+210 sec. There are a few
small peaks riding on top of the main peak. T90 (15-350 keV) is 139.7 +- 16.4 sec
(estimated error including systematics).
The time-averaged spectrum from T+24.2 to T+202.5 sec (with 2.7 sec missing
in the middle due to data drop outs) is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 2.06 +- 0.09.
The fluence in the 15-150 keV band is 3.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+115.88 sec in the 15-150 keV band
is 0.9 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/583861/BA/
GCN Circular 15737
Subject
GRB 140114A: Swift/UVOT Upper Limits
Date
2014-01-14T22:18:03Z (12 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <m.depasquale@ucl.ac.uk>
M. De Pasquale (UCL-MSSL) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 140114A
120 s after the BAT trigger (Troja et al., GCN Circ. 15728).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 15733) is detected in the initial UVOT
exposures and following summed 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 120 270 147 >20.9
u_FC 278 528 246 >20.2
white 120 1701 411 >21.2
v 608 1404 97 >18.8
b 534 1330 78 >19.6
u 278 528 246 >20.2
w1 658 1626 117 >19.3
m2 633 1429 58 >18.6
w2 1013 1379 39 >18.6
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 15736
Subject
GRB 140114A: KAIT Optical Upper Limit
Date
2014-01-14T21:58:17Z (12 years ago)
From
Weikang Zheng at UC Berkeley <zwk@astro.berkeley.edu>
WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 140114A (Troja et al.,
GCN 15728) starting at 12:01:57 UT, 257 s after the burst.
Observations were performed with an automatic sequence in the
I and clear (roughly R) filters, and the exposure time was
20 s per image. Within the enhanced XRT error circle (Beardmore
et al., GCN 15733), we do not detect the afterglow reported by
Butler et al. (GCN 15732) in our single images, nor in a co-added
image from the first 5 images. The typical limiting magnitude of
our single clear image is about 19.4. The co-added image limiting
magnitude is 20.6 at a mean time of about 490 s after the burst.
GCN Circular 15733
Subject
GRB 140114A: Enhanced Swift-XRT position
Date
2014-01-14T18:56:03Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.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 2514 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140114A, 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 = 188.52173, +27.95080 which is equivalent
to:
RA (J2000): 12h 34m 5.22s
Dec (J2000): +27d 57' 02.9"
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.
GCN Circular 15732
Subject
GRB 140114A: RATIR Optical and NIR Afterglow Detection
Date
2014-01-14T17:26:26Z (12 years ago)
Edited On
2024-11-07T19:58:42Z (a year ago)
From
Nat Butler at UC berkeley <natxbutler@gmail.com>
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>
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), Owen Littlejohns (ASU), 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 140114A (Troja et al., GCN 15728) 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 2014/01 14.50 to 2014/01 14.56 UTC (9.6 to
90.6 minutes after the BAT trigger), obtaining a total of 0.98 hours
exposure in the r and i bands and 0.43 hours exposure in the Z, Y, J, and H
bands.
For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS, we obtain the following detections:
r 21.92 +/- 0.10
i 21.31 +/- 0.07
Z 21.14 +/- 0.12
Y 20.75 +/- 0.15
J 20.56 +/- 0.12
H 20.28 +/- 0.15
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 15729
Subject
GRB 140114A: P60 Observations
Date
2014-01-14T13:18:09Z (12 years ago)
From
S. Bradley Cenko at NASA/GSFC <brad.cenko@nasa.gov>
S. B. Cenko (NASA/GSFC) reports on behalf of a larger collaboration:
We imaged the location of GRB140114A (Troja et al., GCN 15728) with the robotic Palomar 60 inch telescope. Observations were obtained in the r', i', and z' filter beginning at 12:01 UT on 2014 January 14 (~ 3 minutes after the Swift trigger). The seeing was relatively poor throughout the observations (~ 3").
We do not detect any emission at the location of the XRT counterpart. Using several nearby point sources from SDSS for reference, we calculate the following upper limits in coadded images:
i' > 20.8 mag at a mean epoch of dt ~ 14 min
r' > 21.2 mag at a mean epoch of dt ~ 15 min
z' > 20.0 mag at a mean epoch of dt ~ 16 min
GCN Circular 15728
Subject
GRB 140114A: Swift detection of a burst
Date
2014-01-14T12:23:14Z (12 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
E. Troja (NASA/GSFC/UMCP), A. P. Beardmore (U Leicester),
M. G. Bernardini (INAF-OAB), D. N. Burrows (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:
At 11:57:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140114A (trigger=583861). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 188.482, +27.926 which is
RA(J2000) = 12h 33m 56s
Dec(J2000) = +27d 55' 35"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of at least 300 sec. The peak count rate
was ~1000 counts/sec (15-350 keV), at ~118 sec after the trigger.
The XRT began observing the field at 11:59:46.0 UT, 126 seconds after
the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued
X-ray source with an enhanced position: RA, Dec 188.5214, 27.9514 which
is equivalent to:
RA(J2000) = 12h 34m 05.13s
Dec(J2000) = +27d 57' 05.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 155 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 (1.55 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.1
(+3.20/-2.63) x 10^21 cm^-2 (90% confidence).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 120 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
0.02.
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.)