Gamma-ray Burst 241113B
(All information courtesy of the instrument teams.)
Previous IAU Circulars
Results of Observations
- GCN Circular #38196
SVOM/ECLAIRs Commissioning Team: Nicolas Dagoneau, St=C3=A9phane Schanne, F=
r=C3=A9d=C3=A9ric Chateau, Herv=C3=A9 Le Provost (CEA), Jean-Luc Atteia, La=
urent Bouchet, Marius Brunet, Sebastien Guillot, Juliette Alaux, Hui Yang (=
IRAP), Wenjin Xie, Donghua Zhao (NAOC), Alexis Coleiro (APC), Tais Maiolino=
(LUPM), Karine Mercier, Marie-Claire Charmeau, Stefano Crepaldi (CNES)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Olivier Godet (IRAP), Arnaud Claret (CEA), =
Zi-Gao Dai (USTC), Fr=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), A=
ndrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lacha=
ud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris=
), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Bing Zhang (UNLV)
Report on behalf of the SVOM team:
During the commissioning phase, the SVOM/ECLAIRs telescope triggered and lo=
cated the long duration GRB 241113B (sb24111301) at 2024-11-13T11:23:05 UT =
(Tb) which was also detected by SVOM/GRM.
The following trigger information was received on the ground with low-laten=
cy by the SVOM VHF Alert Network.
The burst was detected by both the on-board Count-Rate Trigger (CRT) and Im=
age Trigger (IMT) and 20 alerts were received. The best detection is obtain=
ed by CRT with a signal-to-noise ratio of 22.4 in the 8-50 keV energy band =
over a time window of 20.48 s starting at Tb. The light curve shows a singl=
e peak.
The localization of the best Alert is RA, Dec =3D 110.230, 46.804 (J2000).
The statistical uncertainty on this position is 3.8 arcminutes, to which we=
recommend adding 2 arcminutes of systematic uncertainty in quadrature.
SVOM did not slew on this burst.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA), French Space Agency=
(CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to o=
bserving gamma-ray bursts and other transient phenomena in the energetic un=
iverse. ECLAIRs was developed jointly by APC, CEA, CNES, and IRAP.
The SVOM point of contact for this burst is: stephane.schanne AT cea.fr
- GCN Circular #38202
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the SVOM/ECLAIRs GRB 241113B.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021731
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the SVOM/ECLAIRs event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a
GCN Circular after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
- GCN Circular #38212
SVOM/GRM team: Jia-Cong Liu, Chen-Wei Wang, Shi-Jie Zheng, Yong-Wei Dong, J=
iang-Tao Liu, Jian-Chao Sun, Yue Huang, Jiang He, Min Gao, Hao-Xuan Guo, Lu=
Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li Tu=
o, Wen-Long Zhang, Wen-Jun Tan, Yue Wang, Hao-Xi Wang, Jin Wang, Jin-Zhou W=
ang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-Bing Wu, Shao-Lin Xiong, Jian-=
Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang, Shuang-Na=
n Zhang, Yan-Qiu Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao, Jin-Pe=
ng Zhang, Chao Zheng (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laure=
nt Bouchet (IRAP), David Corre (CEA), Tais Maiolino (LUPM), Fr=C3=A9d=C3=A9=
ric Piron (LUPM), St=C3=A9phane Schanne (CEA), Jingwei Wang (IAP), JeanLuc =
Att=C3=A9ia (IRAP)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (I=
HEP), St=C3=A9phane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Fr=
=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), =
Andrea Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lac=
haud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Par=
is), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong =
(IHEP), Bing Zhang (UNLV)
report on behalf of the SVOM team:
During the commissioning phase, the SVOM/GRM was triggered by GRB 241113B(S=
VOM trigger reference: sb24111301) at 2024-11-13T11:23:05 UT (T0), which wa=
s also triggered by SVOM/ECLAIRs (Dagoneau et al, GCN=C2=A038196).
With the event-by-event data downloaded through the X-band ground station, =
the GRM light curve shows that this burst consists of one pulse, with a T90=
of 11.7 +1.9/-3.0 s (15-550 keV). This burst is located at about 23.8 degr=
ees from the SVOM optical axis.
The GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb241113B.png
The Space Variable Objects Monitor (SVOM) is a China-France joint mission l=
ed by the Chinese National Space Administration (CNSA, China), National Cen=
ter for Space Studies (CNES, France) and the Chinese Academy of Sciences (C=
AS, China), which is dedicated to observing gamma-ray bursts and other tran=
sient phenomena in the energetic universe. GRM is developed by the Institut=
e of High Energy Physics (IHEP) of CAS.
The SVOM point of contact for this burst is: Jia-Cong Liu (IHEP)(liujiacong=
@ihep.ac.cn)
- GCN Circular #38214
TITLE: GCN CIRCULAR
NUMBER: 38214
SUBJECT: EP241113b/GRB 241113B: EP detection of GRB 241113B
DATE: 24/11/14 09:01:38 GMT
FROM: EP Team at NAOC/CAS
Z. Y. Liu, M. Q. Huang (USTC), C. Y. Dai (NJU), X. P. Xu, M. H. Zhang, W. Y=
uan (NAO, CAS) report on behalf of the Einstein Probe team:
We report on the detection of an X-ray transient, designated EP241113b, by =
the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) missi=
on. The WXT position of EP241113b is R.A.=3D 110.233 deg, DEC =3D 46.800 de=
g (J2000) with an uncertainty of 2.5 arcmin (radius, 90% C.L. statistical a=
nd systematic).
The lightcurve of the transient observed by the WXT lasts around 100 second=
s. The 0.5-4.0 keV spectrum can be fitted using an absorbed power law with =
a photon index of 1.5 +/- 0.7, and a column density of 2.7 (+/- 1.8) =C3=97=
10^(21) cm^-2. The derived average flux is estimated to be around 1.5 (+/- =
0.4 ) =C3=9710^(-9) erg/s/cm^2 in 0.5-4.0 keV.
EP241113b is spatially and temporally consistent with GRB 241113B (GCN 3819=
6; GCN 38212). The burst started at 2024-11-13T11:22:50 (UTC), which is abo=
ut 15 seconds before the SVOM/ECLAIRs trigger time (2024-11-13T11:23:05).
Launched on January 9, 2024, EP is a space X-ray observatory to monitor th=
e soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handboo=
k of X-ray and Gamma-ray Astrophysics).
- GCN Circular #38219
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), C. Salvaggio
(INAF-OAB), M. Ferro (INAF-OAB), R. Brivio (INAF-OAB), S. Dichiara
(PSU), J.A. Kennea (PSU), D.N. Burrows (PSU) and P.A. Evans (U.
Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
SVOM/ECLAIRs-detected burst GRB 241113B, collecting 1.5 ks of Photon
Counting (PC) mode data between T0+10.3 ks and T0+16.1 ks.
No X-ray sources have been detected consistent with being within 572
arcsec of the SVOM/ECLAIRs position. The 3-sigma upper limit in the
field ranges from ~0.006 to ~0.007 ct s^-1, corresponding to a 0.3-10
keV observed flux of 2.4e-13 to 2.8e-13 erg cm^-2 s^-1 (assuming a
typical GRB spectrum).
The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021731.
This circular is an official product of the Swift-XRT team.
- GCN Circular #38223
Benjamin Schneider (MIT), Geoffrey Mo (MIT), Tomas Ahumada (Caltech), Viraj Karambelkar (Caltech), Robert Stein (UMD), Nathan Lourie (MIT), Danielle Frostig (CFA), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report:
We observed the field of the GRB 241113B (Dagoneau et al, GCN 38196; Liu et al., GCN 38212; Liu et al., GCN 38214) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1-square degree WINTER camera (Lourie et al. 2020, Frostig et al. 2024).
Our observations began at 2024-11-13T12:14:04.71 UTC (51 mins after the GRB trigger) and consisted of 30x120s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.10888436), with image subtraction performed relative to J-band images from the UKIRT Hemisphere survey (Dye et al., 2017).
Our observations covered the entire SVOM/ECLAIRs statistical error circle. In the stacked and subtracted images, we do not detect any new source down to a 5-sigma depth of J ~ 19.1 mag (AB).
WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research.
- GCN Circular #38232
WeiKang Zheng and Alexei V. Filippenko (UCB),
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang
(IHEP), St=C3=A9phane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC),
Fr=C3=A9d=C3=A9ric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP)=
, Andrea
Goldwurm (APC), Diego G=C3=B6tz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (AP=
C),
En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing
Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (IHEP),
Bing Zhang (UNLV)
report on behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick
Observatory, automatically responded to GRB 241113B (SVOM/ECLAIRs, Dagoneau
et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN
38214) starting at 11:24:48 UT, 103s after ECLAIRs trigger. Observations
were performed in 3x3 tiling mode and lasted for about 2 hours, a set of
clear (roughly R) filter images were obtained. We detected a bright
uncataloged optical afterglow candidate at J2000 position of (error ~0.5"):
RA: 07:20:57.72
Dec: +46:47:12.3
Its brightness decayed from 16.7 mag at ~250s to 20.5 mag (Vega) at ~1.37
hours, we therefor suggest this to be the optical afterglow of GRB 241113B.
- GCN Circular #38252
Guowang Du, Brajesh Kumar, Weikang Lin, Yaosong Yu, Yehao Cheng, Yu Pan, Xinlei Chen, Xingzhu Zou, Jinghua Zhang, Yuanpei Yang, Yuan Fang (all SWIFAR, YNU), Xuhui Han, Pinpin Zhang, Liping Xin, Chao Wu (all NAOC), Xiangkun Liu, Xiaowei Liu (all SWIFAR, YNU) report on behalf of the Mephisto Team:
The field of GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN 38214) was observed with the 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory starting from 16:17:01 UT 2024-11-13 (~4.9 hr after the trigger). Six simultaneous frames in vrz bands were taken with 300s each exposure. The optical afterglow candidate reported by Zheng et al. (GCN 38232) is not visible in our stacked images. The 3-sigma upper limits are below.
Start_Time(UT) Band Exp(s) Lim-mag(AB)
2024-11-13T16:17:01 v 300*6 >22.18
2024-11-13T16:17:01 r 300*6 >22.79
2024-11-13T16:17:01 z 300*6 >21.07
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Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21.
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