GRB 110119A
GCN Circular 11592
Subject
GRB 110119A: Fermi GBM detection
Date
2011-01-21T16:33:25Z (15 years ago)
From
Adam Goldstein at Fermi-GBM/UAH <adam.m.goldstein@msfc.nasa.gov>
A. Goldstein (UAH) reports on behalf of the Fermi GBM Team:
"At 22:21:00.17 UT on 19 January 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110119A (trigger 317168462 / 110119931)which was
also detected by the Swift/BAT (E. Troja et al. 2011, GCN 11581). The GBM
on-ground location is consistent with the Swift position. The angle from
the Fermi LAT boresight is 71 degrees.
The GBM light curve consists of ~100 s of variable outburst followed
by a small bump ~175 s after T0. The entire burst has a duration (T90)
of about 219 s (50-300 keV). The time-averaged spectrum from T0-16.4 s
to T0+62.5 s is best fit by a Band function with Epeak = 126.3 +/- 16.8 keV,
alpha = -0.60 +/- 0.13, and beta = -1.95 +/- 0.09
(C-Stat 1348 for 357 d.o.f.).
The event fluence (10-1000 keV) in this time interval is
(1.36 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+31.4 s in the 10-1000 keV band is 4.5 +/- 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 11590
Subject
GRB 110119A: Suzaku WAM observation of the prompt emission
Date
2011-01-21T16:13:25Z (15 years ago)
From
Satoshi Sugita at Aoyama Gakuin U. <sugita@phys.aoyama.ac.jp>
S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Serino, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report:
The long GRB 110119A (Swift/BAT trigger #442978 ; Troja et al., GCN 11581
; Goad et al., GCN 11582, Baumgartner et al., GCN 11584 ; D'Elia et al., GCN 11586)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 22:20:58.220 UT (=T0).
The observed light curve shows a multi-peaked structure
starting at T0-7.5s, ending at T0+217.5s with a duration (T90) of 206 (+/- 10) seconds.
The fluence in 100 - 1000 keV was 1.21 (+/- 0.14) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+34s was 1.60 (+/- 0.16) photons/cm^2/s in the same
energy range.
Preliminary result shows that the time-averaged spectrum from T0-7.5s to
T0+217.5s is well fitted by a single power-law with a photon index
of 1.97 (+0.20, -0.18) (chi^2/d.o.f = 27.14/25).
All the quoted errors are at statistical 90% confidence level,
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN Circular 11586
Subject
GRB 110119A: Swift-XRT refined Analysis
Date
2011-01-20T14:46:32Z (15 years ago)
From
Valerio D'Elia at ASDC <delia@asdc.asi.it>
V. D'Elia, G. Stratta (ASDC), E. Troja (NASA/GSFC/ORAU) report on
behalf of the Swift-XRT team:
We have analysed 18 ks of XRT data for GRB 110119A (Troja et al. GCN
Circ. 11581), from 48 s to 45.5 ks after the BAT trigger. The data
comprise 358 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 11582).
The late-time light curve (from T0+4.9 ks) can be modelled with a
power-law decay with a decay index of alpha=1.64 (+/-0.10).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+/-0.03). The
best-fitting absorption column is 1.80 (+/-0.11) x 10^21 cm^-2, in
excess of the Galactic value of 6.4 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.23 (+0.12, -0.11)
and a best-fitting absorption column of 1.29 (+0.26, -0.14) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.5 x 10^-11 (5.2 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.29 (+0.26, -0.14) x 10^21 cm^-2
Galactic foreground: 6.4 x 10^20 cm^-2
Excess significance: 15.3 sigma
Photon index: 2.23 (+0.12, -0.11)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00442978.
This circular is an official product of the Swift-XRT team.
GCN Circular 11585
Subject
GRB110119A: MITSuME Okayama optical upper limits
Date
2011-01-20T12:50:29Z (15 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 the MITSuME collaboration:
We observed the field of GRB 110119A (Troja et al., GCN 11581)
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 2011-01-20 10:11:12 UT (~11.8 hours
after the burst). We did not find any new point source within the
enhanced XRT error circle (Goad et al., GCNC 11582) and could not
detect the previously reported afterglow (Morgan et al., GCN 11583)
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
------------------------------------------------------
0.50235 10:24:21 1200.0 >18.9 >18.9 >18.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11584
Subject
GRB 110119A: Swift-BAT refined analysis
Date
2011-01-20T04:33:59Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
E. Troja (NASA/GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+713 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110119A (trigger #442978)
(Troja, et al., GCN Circ. 11581). The BAT ground-calculated position is
RA, Dec = 348.589, 5.982 deg, which is
RA(J2000) = 23h 14m 21.3s
Dec(J2000) = +05d 58' 54.3"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows a cluster of 4 or 5 overlapping peaks
starting at ~T-90 sec and ending at ~T+90 sec, then a second cluster
of 2 or 3 peaks starting at ~T+110 sec and ending at ~T+260 sec.
T90 (15-350 keV) is 208 +- 13 sec (estimated error including systematics).
The time-averaged spectrum from T-86.4 to T+215.5 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.44 +- 0.05. The fluence in the 15-150 keV band is 7.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+33.16 sec in the 15-150 keV band
is 2.2 +- 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/442978/BA/
GCN Circular 11583
Subject
GRB 110119A: PAIRITEL NIR Afterglow Detection
Date
2011-01-20T03:43:24Z (15 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan, C. R. Klein, and J. S. Bloom (UC Berkeley) report:
We observed the field of GRB 110119A (Troja et al., GCN 11581) with the 1.3m
PAIRITEL located at Mt. Hopkins, Arizona. Observations began at 2011-Jan-20
01h24m08s UT, ~3.1 hours after the Swift Trigger, under high airmass (~1.9),
and continued until the source set beyond telescope limits. In mosaics
(effective exposure time of 0.64 hours) taken simultaneously in the J, H,
and Ks filters, we detect a source at the UVOT position (Troja et al., GCN
11581).
The preliminary photometry yields:
post burst
t_mid (hr) exp.(hr) filt mag m_err
3.78 0.64 J 17.9 0.2
3.78 0.64 H 17.0 0.2
3.78 0.64 Ks 16.2 0.2
All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values.
GCN Circular 11582
Subject
GRB 110119A: Enhanced Swift-XRT position
Date
2011-01-20T03:06:52Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1831 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 110119A, 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 = 348.58574, +5.98598 which is equivalent
to:
RA (J2000): 23h 14m 20.58s
Dec (J2000): +05d 59' 09.5"
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 11581
Subject
GRB 110119A: Swift detection of a burst with an optical detection
Date
2011-01-19T22:31:42Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
E. Troja (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester) and G. Stratta (ASDC) report on behalf
of the Swift Team:
At 22:20:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110119A (trigger=442978). Swift slewed immediately to the burst.
The BAT on-board calculated location is RA, Dec 348.558, +5.985 which is
RA(J2000) = 23h 14m 14s
Dec(J2000) = +05d 59' 05"
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 about 95 sec. The peak count rate
was ~4500 counts/sec (15-350 keV), at ~35 sec after the trigger.
The XRT began observing the field at 22:21:56.0 UT, 57.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 348.5881, +5.9874 which is equivalent to:
RA(J2000) = 23h 14m 21.14s
Dec(J2000) = +05d 59' 14.6"
with an uncertainty of 6.2 arcseconds (radius, 90% containment). This
location is 108 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 67 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 23:14:20.61 = 348.58587
DEC(J2000) = +05:59:10.5 = 5.98626
with a 90%-confidence error radius of about 0.61 arc sec. This position is 9.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.48 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.12.
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.)