GRB 110112A
GCN Circular 11619
Subject
GRB110112A: EVLA Observations
Date
2011-01-31T17:26:28Z (16 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
A. Zauderer, E. Berger, and W. Fong (Harvard) report:
We observed the position of the short GRB 110112A (GCN #11553) with the
EVLA for 1 hour at 5 GHz starting on 2011 January 14.05 UT (1.87 days
after the burst). No radio source is detected within the XRT error
circle (GCN #11556) to a 3-sigma limit of 75 microJy.
We acknowledge the EVLA staff for their support of these observations.
GCN Circular 11589
Subject
GRB 110112A: optical upper limit
Date
2011-01-20T21:37:07Z (16 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
K. Grankin, V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of
larger GRB follow-up collaboration:
We observed the field of the Swift GRB 110112A (Stamatikos et al., GCN
11553) with AZT-11 telescope of CrAO starting on Jan. 12 (UT) 16:35. In the
enhanced Swift-XRT position (Evanset al., GCN 11556) we do not detect
optical afterglow (Xin et al., GCN 11554) up to R=20.6. The photometry is
based on the
USNO B1.0 star 1164-0563915 (21 59 45.42 +26 27 18.3) assuming R=15.64.
T0+ Filter, Exposure, mag.
(mid, d) (s)
0.52955 R 13x180 R >20.6
GCN Circular 11566
Subject
GRB 110112A: MITSuME Akeno and Okayama optical upper limits
Date
2011-01-14T09:21:44Z (16 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
H. Nakajima (Tokyo Tech), D. Kuroda, K. Yanagisawa, Y. Shimizu,
H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto), Y. Yatsu, T. Enomoto, K. Kawakami, K. Tokoyoda,
T. Ohkawa and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 110112A (Stamatikos et al.,GCN 11553)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Akeno Observatory and Okayama
Astrophysical Observatory.
We did not find any new point source within the enhanced XRT error
circle (Evans et al., GCN 11556) in all the three bands. We could
not detect the previously reported afterglow (Xin et al., GCN 11554).
Three sigma upper limits of the OT are listed below. We used GSC2.3
catalog for flux calibration.
Akeno Observatory:
The observation started on 2011-01-12 09:07:48 UT (~5 h after the
trigger).
T0+[day] MID-UT T-EXP[sec] g' Rc Ic
------------------------------------------------------
0.21513 09:22:06 1200.0 >20.2 >20.0 >19.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
Okayama Astrophysical Observatory:
The observation started on 2011-01-12 09:15:35 UT (~5.1 h after
the trigger).
T0+[day] MID-UT T-EXP[sec] g' Rc Ic
------------------------------------------------------
0.23603 09:52:11 3840.0 >19.9 >19.8 >19.3
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11561
Subject
GRB 110112A: Swift-XRT refined Analysis
Date
2011-01-12T23:05:48Z (16 years ago)
From
Andy Beardmore at U Leicester <apb@star.le.ac.uk>
A. P. Beardmore (U. Leicester) and M. Stamatikos (OSU/NASA/GSFC) report
on behalf of the Swift-XRT team:
We have analysed 23 ks of XRT data for GRB 110112A (Stamatikos et al.
GCN Circ. 11553), from 82 s to 52.8 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 11556).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.95 +/- 0.05.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.4, -0.3). The
best-fitting absorption column is 1.4 (+0.8, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 5.5 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 3.4 x 10^-11 (5.4 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.4 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 5.5 x 10^20 cm^-2
Excess significance: 3.0 sigma
Photon index: 2.3 (+0.4, -0.3)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00442039.
This circular is an official product of the Swift-XRT team.
GCN Circular 11560
Subject
GRB 110112A: Swift/UVOT upper limits
Date
2011-01-12T22:53:06Z (16 years ago)
From
Alice Breeveld at MSSL-UCL <aab@mssl.ucl.ac.uk>
A. A. Breeveld (MSSL/UCL) and M. Stamatikos (OSU/NASA/GSFC) report on
behalf
of the Swift/UVOT team:
Swift UVOT started observing the field of GRB 110112A with the white
filter 85s after the trigger (Stamatikos et al., GCN Circ. 11553).
No optical afterglow consistent with the TNT or XRT positions (Xin et
al., CGN Circ. 11554 and Evans et al., GCN Circ. 11556) is detected in
individual or merged UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) are:
Filter T_start T_stop Exp(s) Mag (Upper limits)
---------------------------------------------------------------------------
white 85 235 147 >20.4
white 4499 6134 393 >21.3
v 4909 6544 393 >19.6
b 4294 5929 393 >20.3
u 287 5724 639 >20.2
uvw1 5319 5519 19.7 >18.8
uvm2 5079 6634 280 >18.9
uvw2 4705 6339 393 >19.2
----------------------------------------------------------------------------
The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.06 mag (Schlegel et al., 1998, ApJS, 500, 525).
GCN Circular 11559
Subject
GRB 110112A: WHT candidate afterglow/host galaxy
Date
2011-01-12T22:52:49Z (16 years ago)
From
Andrew Levan at U.of Leicester <A.J.Levan@warwick.ac.uk>
A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester),
D. Baker (U. Leicester/U. Hertfordshire) report for a larger collaboration:
"We observed the field of the short GRB 110112A (Stamatikos et al.
GCN 11553) with ACAM mounted on the William Herschel Telescope (WHT)
on La Palma. Observations began 15.5 hours after the GRB. Within
the XRT localization (Evan et al. GCN 11556) we detect a faint,
possibly extended source at a position of
RA(J2000) 21:59:43.84
DEC(J2000) 26:27:24.0
with an error of ~0.5" in each axis The source has a magnitude of
i~22, calibrated against nearby stars from the USNO B1 catalog.
This magnitude is fainter than that inferred for a candidate afterglow
of Xin et al. (GCN 11554), suggestive of fading between the two
epochs. We note that the positions of the two objects are only
marginally consistent with each other, and suggest that the source
observed in our WHT observations is a candidate host galaxy for GRB
110112A, although with a single epoch we cannot constrain any
possible afterglow contribution at this time."
GCN Circular 11558
Subject
GRB 110112A: MASTER optical observations
Date
2011-01-12T18:20:16Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University
V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the GRB110112.18 48131 sec s after
notice time and 48156 sec after GRB time at 2011-01-12 17:34:54.665 UT. On
our first (180s exposure) set we haven`t found optical transient within
SWIFT error-box (ra=21 59 45 dec=+26 29 24 r=0.050000).
The 5-sigma upper limit has been about 18.3 mag (V) and 19.0 (R).
The message generated automaticaly.
cited.
mailto: lipunov@sai.msu.ru
GCN Circular 11557
Subject
GRB 110112A: Swift-BAT refined analysis
Date
2011-01-12T16:32:56Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU)
(on behalf of the Swift-BAT team):
Using the data set from T-60 to T+123 sec from the recent telemetry downlink,
we report further analysis of BAT short GRB 110112A (trigger #442039)
(Stamatikos, et al., GCN Circ. 11553). The BAT ground-calculated position is
RA, Dec = 329.936, 26.470 deg, which is
RA(J2000) = 21h 59m 44.6s
Dec(J2000) = +26d 28' 10.6"
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.
The mask-weighted light curve shows a single spike starting at ~T-0.1 sec
and ending at ~T+0.5 sec. T90 (15-350 keV) is 0.5 +- 0.1 sec
(estimated error including systematics).
The time-averaged spectrum from T-0.1 to T+0.5 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.14 +- 0.46. The fluence in the 15-150 keV band is 3.0 +- 0.9 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.28 sec in the 15-150 keV band
is 0.5 +- 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/442039/BA/
GCN Circular 11556
Subject
GRB 110112A: Enhanced Swift-XRT position
Date
2011-01-12T16:00:11Z (16 years ago)
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 1127 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 110112A, 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 = 329.93240, +26.45636 which is equivalent
to:
RA (J2000): 21h 59m 43.77s
Dec (J2000): +26d 27' 22.9"
with an uncertainty of 3.2 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.
GCN Circular 11554
Subject
GRB110112A: TNT optical afterglow candidate
Date
2011-01-12T13:17:22Z (16 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
L.P. Xin, T. M. Zhang, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng,
C. Wu, X. H. Han on behalf of EAFON report:
We began to observe GRB110112A (stamatikos et al., GCN 11553 )
with Xinglong TNT telescope at 10:08:35.375 (UT), 6 hours after
the burst. 16 images in R-band were obtained with an exposure
time of 300 sec for each frame.
After combining all these images, a new marginal source was
found within the errorbox of X-ray counterpart
( stamatikos et al., GCN 11553).
Its coordinates ( RA and Dec ) are 21:59:43.8 26:27:25.9 (J2000)
with an uncertainty of about 1 arcsecond.
The brightness of the source is estimated to be about
19.6 +/- 0.3 mag which is derived from USNO B1.0 R2 mag
at the mean time of 6.5 hour after the burst.
Further observations and confirmation 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/grb/
GCN Circular 11553
Subject
GRB 110112A: Swift detection of a possible short burst
Date
2011-01-12T04:26:58Z (16 years ago)
From
Michael Stamatikos at OSU/GSFC <michael.stamatikos-1@nasa.gov>
M. Stamatikos (OSU/NASA/GSFC), A. P. Beardmore (U Leicester),
J. R. Cummings (NASA/UMBC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
O. M. Littlejohns (U Leicester), K. L. Page (U Leicester),
J. L. Racusin (NASA/GSFC), T. Sakamoto (NASA/UMBC),
M. H. Siegel (PSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:
At 04:12:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110112 A (trigger=442039). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 329.941, +26.489 which is
RA(J2000) = 21h 59m 46s
Dec(J2000) = +26d 29' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single peak
with a duration of about 2 sec. The peak count rate
was ~1700 counts/sec (15-350 keV), at the trigger time.
The XRT began observing the field at 04:13:33.9 UT, 75.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 329.9330, 26.4564 which
is equivalent to:
RA(J2000) = 21h 59m 43.91s
Dec(J2000) = +26d 27' 23.0"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 119 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 5.54
x 10^20 cm^-2 (Kalberla et al. 2005).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 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 none of
the XRT error circle. The coverage of the XRT error circle by the 8'x8' region
for the list of sources generated on-board is uncertain because the large
number of sources filled the available telemetry. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.06.
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.)