GRB 231110A
GCN Circular 34977
Subject
GRB 231110A: Swift detection of a burst
Date
2023-11-10T21:35:09Z (2 years ago)
From
Jamie Kennea at Penn State <jak51@psu.edu>
Via
email
V. D'Elia (SSDC & INAF-OAR), E. Ambrosi (INAF-IASFPA),
A. D'Ai (INAF-IASFPA), S. Dichiara (PSU), J.D. Gropp (PSU),
J. A. Kennea (PSU), A. Melandri (INAF-OAR) and M. A. Williams (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 21:19:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 231110A (trigger=1195733). Swift did not slew immediately
to the burst due to an observing constraint.
The BAT on-board calculated location is
RA, Dec 356.296, +82.621 which is
RA(J2000) = 23h 45m 11s
Dec(J2000) = +82d 37' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of about 20 sec. The peak count rate
was ~2800 counts/sec (15-350 keV), at ~1 sec after the trigger.
Due to an observing constraint, Swift will not slew until T0+50.7
minutes. There will be no XRT or UVOT data until this time.
Burst Advocate for this burst is V. D'Elia (valerio.delia AT ssdc.asi.it).
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/)
GCN Circular 34979
Subject
GRB231110A: WFST Observation and upper limits
Date
2023-11-11T14:16:02Z (2 years ago)
From
Tianrui Sun at Purple Mountain Obs,CAS <trsun@pmo.ac.cn>
Via
legacy email
Tian-Rui Sun, Jin-Jun Geng, and Zhen-Qiang Li report on behalf of the WFST Collaboration:
Following the detection of GRB 231110A by SWIFT (D’Elia et al., GCN 34977) and MASTER (Lipunov et al., GCN 34978), we carried out image observations using the newly deployed Wide Field Survey Telescope (WFST Collaboration; arXiv:2306.07590) at Lenghu Astronomical Observation Base (Qinghai province, China) to search and follow up its afterglow in the BAT error box.
We observed the target position with 13x60s and 27x90s exposure in i-band starting from 10 Nov 2023, UTC 05:59:01, about 39.45 minutes after the burst.
After stacking the individual exposures (5x90s) to enhance observation depth at low altitude, we found two possible candidates:
RA | DEC | i-magnitude |magerr |limit
23:45:02.3407 | +82:38:43.067 | 21.6953 |0.0957 |22.3909
23:45:18.0531 | +82:37:18.403 | 22.0166 |0.1286 |22.3909
We used the PanStarrs DR1 (Flewelling,2020) catalog as the magnitude reference for calibration.
GCN Circular 34986
Subject
GRB 231110A: Swift-XRT afterglow detection
Date
2023-11-11T20:48:23Z (2 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), M. Perri
(SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti
(INAF-OAB), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU), J. D. Gropp
(PSU) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT
team:
Swift-XRT has performed follow-up observations of the
Swift-BAT-detected burst GRB 231110A, collecting 10 ks of Photon
Counting (PC) mode data between T0+8.9 ks and T0+61.1 ks.
Four uncatalogued X-ray sources are detected consistent with being
within 296 arcsec of the Swift-BAT position, of which one ("Source 2")
is believed to be the afterglow. The position of this source is RA,
Dec=356.2752, +82.6447 which is equivalent to:
RA (J2000): 23:45:6.05
Dec(J2000): +82:38:40.9
with an uncertainty of 5.1 arcsec (radius, 90% confidence). This
position is 85 arcsec from the Swift-BAT position. There is evidence
that the source may be fading, however we cannot constrain the decay at
the current time
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01195733.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/01195733.
This circular is an official product of the Swift-XRT team.
GCN Circular 34987
Subject
GRB 231110A: SAO RAS optical observations
Date
2023-11-11T21:59:36Z (2 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin and O. A. Maslennikova (SAO RAS)
report on behalf of the GRB follow-up team.
We observed the field of Swift GRB 231110A (D'Elia et al., GCN #34977)
with the 1-m telescope of SAO RAS equipped with the CCD photometer.
We obtained 8 x 300 sec. images in Rc band on November 10,
22:09:05--22:55:32 UT (t_mid - T0 = 1.21224 hours).
Following the non-detection of OT by MASTER team (Lipunov et al.,
GCN #34978) we also did not detect any significant source within
the probable XRT error circle (Beardmore et al., GCN #34986)
down to the limiting magnitude R_lim = 22.9. We should note
the presence of the first object mentioned by Sun et al. (GCN #34979)
near the XRT error circle. The brightness of this object is
R = 22.50 +/- 0.24.
Preliminary photometry is based on nearby USNO-B1 stars (R2 mag).
Magnitudes are not corrected for MW extinction.
GCN Circular 34988
Subject
GRB 231110A: GOTO optical upper limits
Date
2023-11-11T22:37:18Z (2 years ago)
From
Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>
Via
email
B. P. Gompertz, R. Starling, A. Kumar, K. Ackley, M. J. Dyer, J. Lyman, K. Ulaczyk, F. Jimenez-Ibarra, D. O'Neill, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Pall'e and D. Pollacco report on behalf of the GOTO collaboration:
The Gravitational-wave Optical Transient Observer (GOTO, Steeghs et al. 2022) performed a targeted observation in response to GRB 231110A (D’Elia et al., GCN 34977) at 22:26:08 UT on 2023-11-10, 66.5 minutes after trigger. The observation consisted of a 4x90s exposure in the GOTO L-band (400-700 nm).
Images were processed immediately after acquisition using the GOTO pipeline. No optical counterpart is detected at the position of the X-ray afterglow (Beardmore et al., GCN 34986) to a 3-sigma limit of L > 19.9 magnitudes (AB).
Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.
GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).
GCN Circular 34989
Subject
GRB 231110A: GECAM detection
Date
2023-11-12T01:01:31Z (2 years ago)
From
Yue Wang <m18509381757@163.com>
Via
Web form
Yue Wang, Shaoli Xiong, Yue Huang report on behalf of the GECAM team:
GECAM-B was triggered in-flight by a long burst, GRB 231110A, at 2023-11-10T21:19:35.100 UTC (T0), which was also observed by Swift/BAT (GCN # 34977).
According to the realtime alert data of GECAM-B, this burst
mainly consists of a long pulse with a duration (T90) of about ~20 sec (20-1000 keV).
The GECAM-B localization is consistent with the Swift/BAT team localization (trigger=1195733) within the error.
The time-averaged spectrum of GECAM-B realtime data shows that it could be
adequately fit by a cut-off power-law with a flux about 1.3E-6 erg/cm^2 in 20-1000 keV.
We note that these results are based on realtime alert data and thus very preliminary.
Refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B)
launched in Dec. 2020. As the third member of GECAM constellation,
GECAM-C was launched onboard SATech-01 experimental satellite in July 2022.
GECAM mission is funded by the Chinese Academy of Sciences (CAS).
GCN Circular 34992
Subject
GRB 231110A: GECAM-B detection (correction)
Date
2023-11-12T02:26:47Z (2 years ago)
From
Yue Wang <m18509381757@163.com>
Via
Web form
Yue Wang, Shao-Lin Xiong, Yue Huang report on behalf of the GECAM team:
GECAM-B was triggered in-flight by a long burst, GRB 231110A, at 2023-11-10T21:19:35.100 UTC (T0), which was also observed by Swift/BAT (GCN #34977).
According to the realtime alert data of GECAM-B, this burst
mainly consists of a long pulse with a duration (T90) of about ~20 sec (20-1000 keV).
The GECAM-B localization is consistent with the Swift/BAT localization (trigger=1195733) within the error.
The time-averaged spectrum of GECAM-B realtime data from about T0 to T0+4 s could be
adequately fit by a cut-off power-law with a flux about 1.3E-6 erg/cm^2/s in 20-1000 keV.
We note that these results are based on realtime alert data and thus very preliminary.
Refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B)
launched in Dec. 2020. As the third member of GECAM constellation,
GECAM-C was launched onboard SATech-01 experimental satellite in July 2022.
GECAM mission is funded by the Chinese Academy of Sciences (CAS).
GCN Circular 34996
Subject
GRB 231110A: Terskol Zeiss-2000 optical upper limit
Date
2023-11-12T10:50:05Z (2 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Via
legacy email
N. Pankov (IKI, HSE), I. Sokolov (INASAN, KIAM), A. Buslaeva (INASAN), A. Pozanenko (IKI), S. Belkin (IKI, HSE) report on behalf of GRB IKI FuN:
We observed the Swift GRB 231110A (D'Elia et al., GCN #34977) with Zeiss-2000 telescope of Terskol observatory starting on 2023-11-10 (UTC) 23:25:16. We do not detect any object within Source #2 of XRT probable afterglow (Beardmore et al., GCN 34986). This is cosnistent with non-detection in other observations (Lipunov et al., GCN 34978; Sun et al., GCN 34979; Sun et al., GCN 34985; Moskvitin et al., GCN 34987; Gompertz et al., GCN 34988). Preliminary photometry of the field is following.
Date UT start t-T0 Filter Exp. OT Err. UL. Telescope
(mid, days) (s)
2023-11-10 23:25:16 0.08729 R 28*120 R n/d n/d 22.4 Zeiss-2000
The photometry is based on the nearby USNO-B1.0 stars.
GCN Circular 35005
Subject
GRB 231110A: AstroSat CZTI detection
Date
2023-11-12T19:05:57Z (2 years ago)
From
Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>
Via
Web form
P. K. Navaneeth (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 231110A which was also detected by Swift-BAT (D'Elia et al., GCN Circ. 34977), and GECAM-B (Wang et al., GCN Circ. 34992).
The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-11-10 21:19:35.25 UTC. The measured peak count rate associated with the burst is 246 (+54, -49) counts/s above the background in the combined data of all quadrants, with a total of 611 (+135, -146) counts. The local mean background count rate was 290 (+4, -5) counts/s. Using cumulative rates, we measure a T90 of 6 (+2, -2) s.
The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2023-11-10 21:19:34.93 UTC. The measured peak count rate associated with the burst is 469 (+67, -71) counts/s above the background in the combined data of all quadrants, with a total of 957 (+229, -242) counts. The local mean background count rate was 1167 (+6, -7) counts/s. We measure a T90 of 5 (+3, -2) s from the cumulative Veto light curve.
CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.
CZTI GRB detections are reported regularly on the payload site at:
http://astrosat.iucaa.in/czti/?q=grb
GCN Circular 35006
Subject
GRB 231110A: Glowbug gamma-ray detection
Date
2023-11-13T02:43:32Z (2 years ago)
From
C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>
Via
Web form
C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (MSFC), and M.S. Briggs (UAH) report:
The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 231110A, which was also detected by Swift/BAT, GECAM-B, and AstroSat/CZTI (GCN 34977, 34992, 35005).
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-11-10 21:19:32.008 with a duration of 8.2 s and a total significance of about 38 sigma. The light curve comprises the single peak observed by Swift/BAT, GECAM-B, and AstroSat/CZTI.
Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=1.2 and a cutoff energy ("Epeak") of 271 keV. The modeled 10-10000 keV fluence is 2.4e-06 erg/cm^2.
The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006
Distribution Statement A: Approved for public release. Distribution is unlimited.
GCN Circular 35011
Subject
GRB 231110A: Swift-UVOT Upper Limits
Date
2023-11-13T15:10:22Z (2 years ago)
From
N. Klingler at NASA-GSFC/UMBC/CRESST II <noelklingler@gmail.com>
Via
Web form
Swift-UVOT has performed follow-up observations of the Swift-BAT-detected burst GRB 231110A (Kennea et al. GCN 34977), collecting 2.8 ks of observations between T0+8.80 ks and T0+27.45 ks. No source was detected in the UVOT data at the position of the X-ray source reported by Evans et al. (GCN 34986).
3-sigma upper limits (AB) using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:
Filter T_start(s) T_stop(s) Exp(s) Mag
V 8893 9216 314.67 >19.55
B 14638 15545 881.77 >21.00
U 26828 27450 604.93 >21.67
W1 25992 26822 885.58 >21.76
white 15545 15695 147.43 >21.68
The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.198 in the direction of the burst (Schlegel et al. 1998).
GCN Circular 35015
Subject
GRB 231110A: Swift-BAT refined analysis
Date
2023-11-13T17:16:36Z (2 years ago)
From
Mike Moss at NASA GSFC <mikejmoss3@gmail.com>
Via
Web form
S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC),
V. D'Elia (SSDC & INAF-OAR), H. A. Krimm (NSF),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
M. J. Moss (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU),
M. Stamatikos (OSU) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 231110A (trigger #1195733)
(D'Elia, et al., GCN Circ. 34977). The BAT ground-calculated position is
RA, Dec = 356.244, 82.630 deg which is
RA(J2000) = 23h 44m 58.7s
Dec(J2000) = +82d 37' 48.6"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 34%.
The BAT light curve shows a single pulse structure with a duration of ~ 11
seconds and peaking ~1.5 seconds after the trigger time.
T90 (15-350 keV) is 11.34 +- 1.56 sec (estimated error including systematics).
The time-averaged spectrum from T-1.60 to T+12.32 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.35 +- 0.11. The fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+0.63 sec in the 15-150 keV band
is 3.4 +- 0.4 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/1195733/BA/
GCN Circular 35020
Subject
GRB 231110A: CALET Gamma-Ray Burst Monitor detection
Date
2023-11-14T03:07:36Z (2 years ago)
From
Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>
Via
Web form
S. Sugita, A. Yoshida, T. Sakamoto (AGU), Y. Kawakubo (LSU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR),
S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu,
T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The long GRB 231110A (Swift detection: D'Elia et al., GCN Circ. 34977;
GECAM-B detection: Wang et al., GCN Circ. 34992; AstroSat CZTI
detection: Navaneeth et al., GCN Circ. 35005; Glowbug gamma-ray
detection: Cheung et al., GCN Circ. 35006; Swift-BAT refined analysis:
Laha et al., GCN Circ. 35015) triggered the CALET Gamma-ray Burst
Monitor (CGBM) at 21:19:35.19 UTC on 10 November 2023
(http://cgbm.calet.jp/cgbm_trigger/flight/1383686313/index.html).
The burst signal was seen by all CGBM detectors. No real-time
CGBM GCN notice was distributed about this trigger because
the real-time communication from the ISS was off (loss of signal).
The burst light curve shows a single pulse that starts
at T-1.0 sec, peaks at T+0.5 sec, and ends at T+1.5 sec.
The T90 and T50 durations measured by the SGM data are 2.1 +/- 0.2 sec
and 1.1 +/- 0.1 sec (40-1000 keV), respectively.
The ground-processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1383686313/index.html
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at Waseda University.