GRB 190110A
GCN Circular 23670
Subject
GRB 190110A: Swift detection of a burst
Date
2019-01-10T17:34:23Z (6 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
B. Sbarufatti (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU),
M. J. Moss (George Washington University), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report
on behalf of the Neil Gehrels Swift Observatory Team:
At 17:24:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190110A (trigger=883012). Swift did not slew due to an observing
constraint. The BAT on-board calculated location is
RA, Dec 276.882, -53.676, which is
RA(J2000) = 18h 27m 32s
Dec(J2000) = -53d 40' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows several peaks
with a total duration of about 15 sec. The peak count rate
was ~7000 counts/sec (15-350 keV), at ~5 sec after the trigger.
Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 16:10 UT on 2019 February 01. There will thus be no XRT
or UVOT data for this trigger before this time.
Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu).
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 23671
Subject
GRB 190110A: Fermi GBM detection
Date
2019-01-11T05:34:52Z (6 years ago)
From
Suraj Poolakkil at UAH <sp0076@uah.edu>
S.Poolakkil(UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:
"At 17:24:49.21 UT on 10 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190110A(trigger 568833894/ 190110726),
which was also detected by the Swift/BAT (Sbarufatti et al. 2019, GCN
23670).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight
at the GBM trigger time is 50 degrees.
The GBM light curve consists of a single bright peak
with a duration (T90) of about 9 s (50-300 keV).
The time-averaged spectrum from T0-2.04 s to T0+10.24 s is
best fit by a Band function with Epeak = 73 +/- 8 keV,
alpha = -0.44 +/- 0.20 and beta = -2.12 +/- 0.08.
The event fluence (10-1000 keV) in this time interval is
(5.331 +/- 0.209)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+3.71 s in the 10-1000 keV band
is 14.7 +/- 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 23674
Subject
GRB 190110A, Swift-BAT refined analysis
Date
2019-01-11T20:23:05Z (6 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (PSU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+180 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190110A (trigger #883012)
(Sbarufatti et al., GCN Circ. 23670). The BAT ground-calculated position is
RA, Dec = 276.939, -53.643 deg which is
RA(J2000) = 18h 27m 45.3s
Dec(J2000) = -53d 38' 34.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.
The mask-weighted light curve shows several overlapping peaks that starts at
~ T-1 s and ends at ~ T+11 s. The main peak occurs at ~T+5 s. T90 (15-350 keV)
is 9.3 +- 0.8 sec (estimated error including systematics).
The time-averaged spectrum from T-0.8 to T+11.0 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.66 +- 0.07. The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.66 sec in the 15-150 keV band
is 9.0 +- 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/883012/BA/
GCN Circular 23675
Subject
Konus-Wind observation of GRB 190110A
Date
2019-01-12T21:29:13Z (6 years ago)
From
Anna Kozlova at Ioffe Institute <ann_kozlova@mail.ioffe.ru>
A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 190110A
(Swift-BAT detection and analysis: Sbarufatti et al., GCN Circ. 23670;
Ukwatta et al., GCN Circ. 23674;
Fermi-GBM detection: Poolakkil & Meegan, GCN Circ. 23671)
triggered Konus-Wind at T0=62689.767 s UT (17:24:49.767).
The burst light curve shows a single pulse
started at ~T0-3.5 s with a total duration of ~5 s.
The emission is seen up to ~8 MeV.
As observed by Konus-Wind, the burst
had a fluence of 3.39(-0.51,+0.88)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.158 s,
of 2.21(-0.93,+1.71)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.44(-0.46,+0.58)
and Ep = 132(-60,+111) keV (chi2 = 62/81 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 62/80 dof).
The spectrum near the maximum count rate
(measured from T0+0.128 to T0+0.256 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model
with alpha = -0.87(-0.82,+1.27)
and Ep = 165(-53,+382) keV (chi2 = 12/18 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 = 12/17 dof).
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190110_T62689/
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 23676
Subject
GRB 190110A：Insight-HXMT/HE detection
Date
2019-01-13T09:52:26Z (6 years ago)
From
Qi Luo at IHEP <luoqi@ihep.ac.cn>
Q. Luo, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu, J. L. Zhao,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
At 2019-01-10T17:24:48.30 (T0), the Insight-HXMT/HE detected
GRB 190110A(trigger ID: HEB190110725) in a routine search of the data,
which was also triggered by the Swift/BAT (Sbarufatti et al. 2019, GCN
23670),Fermi/GBM(S.Poolakkil et al. ,GCN 23671) and Konus-Wind(A. Kozlova
et al. ,GCN 23675).
The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 7.19 s measured from T0-0.18 s.
The 1-s peak rate, measured from T0+4.45 s, is 1630.6 cnts/sec.
The total counts from this burst is 3920.2 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190110725_lc.jpg
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (record energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the telescope.
The analysis results presented above are preliminary,
final results will be published elsewhere.
Insight-HXMT is the first Chinese space X-ray telescope, which was
fundedjointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://www.hxmt.org.