EP241113b, GRB 241113B
GCN Circular 38196
Subject
GRB 241113B : detection of a long GRB by SVOM/ECLAIRs
Date
2024-11-13T11:49:49Z (7 months ago)
From
Stéphane Schanne at CEA Paris-Saclay/IRFU <s.schanne@cea.fr>
Via
Web form
SVOM/ECLAIRs Commissioning Team: Nicolas Dagoneau, Stéphane Schanne, Frédéric Chateau, Hervé Le Provost (CEA), Jean-Luc Atteia, Laurent 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 (IHEP), Stéphane Basa (LAM), Olivier Godet (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (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 located 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-latency by the SVOM VHF Alert Network.
The burst was detected by both the on-board Count-Rate Trigger (CRT) and Image Trigger (IMT) and 20 alerts were received. The best detection is obtained 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 single peak.
The localization of the best Alert is RA, Dec = 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 led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. 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
Subject
GRB 241113B: Swift ToO observations
Date
2024-11-13T14:50:26Z (7 months ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
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
Subject
GRB 241113B: SVOM/GRM observation
Date
2024-11-14T07:15:06Z (7 months ago)
From
zhengchao_astro@foxmail.com
Via
Web form
SVOM/GRM team: Jia-Cong Liu, Chen-Wei Wang, Shi-Jie Zheng, Yong-Wei Dong, Jiang-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 Tuo, Wen-Long Zhang, Wen-Jun Tan, Yue Wang, Hao-Xi Wang, Jin Wang, Jin-Zhou Wang, 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-Nan Zhang, Yan-Qiu Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao, Jin-Peng Zhang, Chao Zheng (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IRAP), David Corre (CEA), Tais Maiolino (LUPM), Frédéric Piron (LUPM), Stéphane Schanne (CEA), Jingwei Wang (IAP), JeanLuc Attéia (IRAP)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), 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 SVOM team:
During the commissioning phase, the SVOM/GRM was triggered by GRB 241113B(SVOM trigger reference: sb24111301) at 2024-11-13T11:23:05 UT (T0), which was also triggered by SVOM/ECLAIRs (Dagoneau et al, GCN 38196).
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 degrees 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 led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute 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
Subject
EP241113b/GRB 241113B: EP detection of GRB 241113B
Date
2024-11-14T09:01:38Z (7 months ago)
From
EP Team at NAOC/CAS <ep_ta@bao.ac.cn>
Via
Web form
Z. Y. Liu, M. Q. Huang (USTC), C. Y. Dai (NJU), X. P. Xu, M. H. Zhang, W. Yuan (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) mission. The WXT position of EP241113b is R.A.= 110.233 deg, DEC = 46.800 deg (J2000) with an uncertainty of 2.5 arcmin (radius, 90% C.L. statistical and systematic).
The lightcurve of the transient observed by the WXT lasts around 100 seconds. 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) ×10^(21) cm^-2. The derived average flux is estimated to be around 1.5 (+/- 0.4 ) ×10^(-9) erg/s/cm^2 in 0.5-4.0 keV.
EP241113b is spatially and temporally consistent with GRB 241113B (GCN 38196; GCN 38212). The burst started at 2024-11-13T11:22:50 (UTC), which is about 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 the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics).
GCN Circular 38215
Subject
EP241113b: Global MASTER-Net observations report
Date
2024-11-14T09:09:23Z (7 months ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko,
A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin,
V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU),
O.Gress, N.Budnev (ISU),
C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory)
MASTER-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the EP241113b ( EP Team et al., GCN 38214) errorbox 35232 sec after trigger time at 2024-11-13 21:10:02 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 40 deg. The sun altitude is -65.0 deg.
MASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP241113b errorbox 35748 sec after trigger time at 2024-11-13 21:18:38 UT, with upper limit up to 20.8 mag. The observations began at zenith distance = 6 deg. The sun altitude is -28.5 deg.
The galactic latitude b = 25 deg., longitude l = 171 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2669806
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
35262 | 2024-11-13 21:10:02 | MASTER-Kislovodsk | (07h 19m 25.31s , +46d 57m 34.8s) | C | 60 | 17.3 |
35322 | 2024-11-13 21:10:02 | MASTER-Kislovodsk | (07h 19m 25.31s , +46d 57m 34.8s) | C | 180 | 18.0 | Coadd
35554 | 2024-11-13 21:14:54 | MASTER-Kislovodsk | (07h 19m 28.89s , +46d 59m 28.3s) | C | 60 | 17.3 |
35636 | 2024-11-13 21:16:15 | MASTER-Kislovodsk | (07h 19m 28.71s , +46d 58m 01.3s) | C | 60 | 17.2 |
35718 | 2024-11-13 21:17:38 | MASTER-Kislovodsk | (07h 19m 30.58s , +46d 59m 35.6s) | C | 60 | 17.3 |
35778 | 2024-11-13 21:17:38 | MASTER-Kislovodsk | (07h 19m 30.58s , +46d 59m 35.7s) | C | 180 | 17.9 | Coadd
35778 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.94s , +46d 54m 47.8s) | C | 60 | 18.5 |
35838 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.95s , +46d 54m 47.9s) | C | 180 | 19.3 | Coadd
36378 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.94s , +46d 54m 47.8s) | C | 1260 | 20.6 | Coadd
35800 | 2024-11-13 21:19:00 | MASTER-Kislovodsk | (07h 19m 25.38s , +46d 58m 45.1s) | C | 60 | 17.2 |
35854 | 2024-11-13 21:19:53 | MASTER-Tunka | (07h 20m 31.76s , +46d 53m 50.6s) | C | 60 | 18.5 |
35881 | 2024-11-13 21:20:21 | MASTER-Kislovodsk | (07h 19m 24.23s , +46d 59m 43.9s) | C | 60 | 17.3 |
35926 | 2024-11-13 21:21:05 | MASTER-Tunka | (07h 20m 39.09s , +46d 54m 14.9s) | C | 60 | 18.4 |
36001 | 2024-11-13 21:22:20 | MASTER-Tunka | (07h 20m 35.07s , +46d 55m 53.4s) | C | 60 | 18.5 |
36061 | 2024-11-13 21:22:20 | MASTER-Tunka | (07h 20m 35.07s , +46d 55m 53.4s) | C | 180 | 19.4 | Coadd
36072 | 2024-11-13 21:23:32 | MASTER-Tunka | (07h 20m 35.00s , +46d 54m 17.8s) | C | 60 | 18.4 |
36146 | 2024-11-13 21:24:46 | MASTER-Tunka | (07h 20m 38.35s , +46d 55m 52.1s) | C | 60 | 18.6 |
36223 | 2024-11-13 21:26:03 | MASTER-Tunka | (07h 20m 31.31s , +46d 55m 04.5s) | C | 60 | 18.6 |
36283 | 2024-11-13 21:26:03 | MASTER-Tunka | (07h 20m 31.30s , +46d 55m 04.4s) | C | 180 | 19.4 | Coadd
36296 | 2024-11-13 21:27:16 | MASTER-Tunka | (07h 20m 31.90s , +46d 56m 07.3s) | C | 60 | 18.5 |
36367 | 2024-11-13 21:27:56 | MASTER-Kislovodsk | (07h 19m 26.72s , +46d 59m 40.3s) | C | 120 | 17.3 |
36380 | 2024-11-13 21:28:40 | MASTER-Tunka | (07h 20m 38.02s , +46d 55m 10.0s) | C | 60 | 18.6 |
36509 | 2024-11-13 21:30:18 | MASTER-Kislovodsk | (07h 19m 27.33s , +46d 58m 31.5s) | C | 120 | 17.3 |
36862 | 2024-11-13 21:36:11 | MASTER-Kislovodsk | (07h 19m 22.82s , +46d 59m 19.5s) | C | 120 | 16.8 |
37004 | 2024-11-13 21:38:33 | MASTER-Kislovodsk | (07h 19m 24.47s , +47d 00m 18.7s) | C | 120 | 16.8 |
38196 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.59s , +46d 56m 15.4s) | C | 60 | 19.6 |
38256 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.60s , +46d 56m 15.5s) | C | 180 | 20.2 | Coadd
38466 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.59s , +46d 56m 15.5s) | C | 600 | 20.8 | Coadd
38270 | 2024-11-13 22:00:09 | MASTER-Tunka | (07h 20m 28.15s , +46d 55m 17.7s) | C | 60 | 19.6 |
38348 | 2024-11-13 22:01:27 | MASTER-Tunka | (07h 20m 35.52s , +46d 55m 42.3s) | C | 60 | 19.5 |
38420 | 2024-11-13 22:02:40 | MASTER-Tunka | (07h 20m 31.85s , +46d 57m 17.0s) | C | 60 | 19.6 |
38480 | 2024-11-13 22:02:40 | MASTER-Tunka | (07h 20m 31.85s , +46d 57m 17.0s) | C | 180 | 20.1 | Coadd
38492 | 2024-11-13 22:03:52 | MASTER-Tunka | (07h 20m 31.77s , +46d 55m 25.9s) | C | 60 | 19.4 |
38564 | 2024-11-13 22:05:04 | MASTER-Tunka | (07h 20m 34.94s , +46d 56m 58.6s) | C | 60 | 19.4 |
38636 | 2024-11-13 22:06:16 | MASTER-Tunka | (07h 20m 28.92s , +46d 56m 29.0s) | C | 60 | 19.5 |
38696 | 2024-11-13 22:06:16 | MASTER-Tunka | (07h 20m 28.92s , +46d 56m 29.0s) | C | 180 | 20.2 | Coadd
38708 | 2024-11-13 22:07:28 | MASTER-Tunka | (07h 20m 28.35s , +46d 57m 31.3s) | C | 60 | 19.6 |
38782 | 2024-11-13 22:08:42 | MASTER-Tunka | (07h 20m 34.36s , +46d 56m 33.4s) | C | 60 | 19.6 |
38854 | 2024-11-13 22:09:54 | MASTER-Tunka | (07h 20m 28.04s , +46d 55m 35.5s) | C | 60 | 19.7 |
38914 | 2024-11-13 22:09:54 | MASTER-Tunka | (07h 20m 28.04s , +46d 55m 35.4s) | C | 180 | 20.3 | Coadd
38927 | 2024-11-13 22:11:06 | MASTER-Tunka | (07h 20m 34.43s , +46d 55m 40.2s) | C | 60 | 19.6 |
39000 | 2024-11-13 22:12:20 | MASTER-Tunka | (07h 20m 31.08s , +46d 57m 32.7s) | C | 60 | 19.8 |
39105 | 2024-11-13 22:13:35 | MASTER-Tunka | (07h 20m 30.97s , +46d 55m 53.0s) | C | 120 | 19.9 |
39225 | 2024-11-13 22:13:35 | MASTER-Tunka | (07h 20m 30.97s , +46d 55m 53.0s) | C | 360 | 20.5 | Coadd
39240 | 2024-11-13 22:15:49 | MASTER-Tunka | (07h 20m 32.98s , +46d 57m 37.2s) | C | 120 | 19.9 |
39371 | 2024-11-13 22:18:01 | MASTER-Tunka | (07h 20m 27.32s , +46d 56m 51.7s) | C | 120 | 19.9 |
39426 | 2024-11-13 22:18:56 | MASTER-Kislovodsk | (07h 17m 59.03s , +47d 11m 09.6s) | C | 120 | 16.2 |
39546 | 2024-11-13 22:18:56 | MASTER-Kislovodsk | (07h 17m 58.99s , +47d 11m 09.6s) | C | 360 | 16.4 | Coadd
39505 | 2024-11-13 22:20:14 | MASTER-Tunka | (07h 20m 27.95s , +46d 57m 56.0s) | C | 120 | 19.8 |
39625 | 2024-11-13 22:20:14 | MASTER-Tunka | (07h 20m 27.95s , +46d 57m 56.0s) | C | 360 | 20.4 | Coadd
39568 | 2024-11-13 22:21:17 | MASTER-Kislovodsk | (07h 17m 57.57s , +47d 12m 27.8s) | C | 120 | 16.3 |
39636 | 2024-11-13 22:22:25 | MASTER-Tunka | (07h 20m 32.35s , +46d 56m 60.0s) | C | 120 | 19.8 |
39709 | 2024-11-13 22:23:38 | MASTER-Kislovodsk | (07h 17m 57.13s , +47d 11m 11.1s) | C | 120 | 16.3 |
39768 | 2024-11-13 22:24:37 | MASTER-Tunka | (07h 20m 26.74s , +46d 56m 04.0s) | C | 120 | 19.9 |
40060 | 2024-11-13 22:29:30 | MASTER-Kislovodsk | (07h 17m 53.72s , +47d 12m 05.5s) | C | 120 | 16.6 |
40180 | 2024-11-13 22:29:30 | MASTER-Kislovodsk | (07h 17m 53.72s , +47d 12m 05.6s) | C | 360 | 17.5 | Coadd
40202 | 2024-11-13 22:31:51 | MASTER-Kislovodsk | (07h 17m 52.16s , +47d 13m 05.1s) | C | 120 | 17.0 |
40344 | 2024-11-13 22:34:14 | MASTER-Kislovodsk | (07h 17m 58.71s , +47d 12m 06.8s) | C | 120 | 16.9 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 38219
Subject
GRB 241113B: Swift-XRT observations
Date
2024-11-14T16:03:31Z (7 months ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
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
Subject
GRB 241113B: J-band upper limit from WINTER
Date
2024-11-14T21:18:47Z (7 months ago)
From
Benjamin Schneider at MIT <bschn@mit.edu>
Via
Web form
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
Subject
GRB 241113B: KAIT Optical Afterglow Candidate
Date
2024-11-15T08:40:03Z (7 months ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
Via
email
WeiKang Zheng and Alexei V. Filippenko (UCB),
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang
(IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC),
Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea
Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC),
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
Subject
GRB 241113B: Mephisto upper limits
Date
2024-11-16T14:23:37Z (6 months ago)
From
Brajesh Kumar at SWIFAR, YNU <brajesh@ynu.edu.cn>
Via
Web form
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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GCN Circular 38306
Subject
GRB 241113B: SVOM/VT optical afterglow observations
Date
2024-11-25T12:03:27Z (6 months ago)
From
Huali Li at at NAOC, SVOM <lhl@nao.cas.cn>
Via
Web form
SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, L. P. Xin, C. Wu, X. H. Han, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. Deng, L. Lan, X. M. Lu, R. S. Zhang, (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO), W. K. Zheng (UCB), Z. Q. Wang (GXU)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), 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 SVOM team:
VT started to observe GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN 38214; Du et al., GCN 38252) in ToO mode from 2024-11-13T14:23:24 UT, about 3.0 hours after the burst. The VT conducted observations in VT_B band (400-650nm) and VT_R band (650-1000nm) simultaneously.
The afterglow (Zheng et al., GCN 38232) was detected in both bands with the brightness of VT_B = 22.5 +/- 0.1 mag and VT_R = 21.95+/-0.06 mag in AB magnitude at the midtime of 3.87 hours after the burst. The exposure time of images in VT_R and VT_B are 1470 sec and 1620 sec respectively.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS.
GCN Circular 38330
Subject
GRB 241113B: EP-FXT afterglow detection
Date
2024-11-26T17:27:56Z (6 months ago)
From
Damien Turpin at CEA-Saclay <dturpin-astro@hotmail.com>
Via
Web form
D. Turpin (CEA), Y.-H. I. Yin (NJU), T. Y. Lian (NAOC, CAS), Z. Y. Liu, M. Q. Huang (USTC), H. W. Pan, W. Yuan (NAOC, CAS), D. Adrien, C. Plasse (CEA/irfu), J. Guan, C. K. Li, Y . Chen, S. M. Jia, W. W. Cui, D. W. Han, W. Li, C. Z. Liu, F . J. Lu, L. M. Song, J. Wang, J. J. Xu, J. Zhang, S. N. Zhang, H. S. Zhao, X. F . Zhao (IHEP , CAS), Y . Liu, C. C. Jin, C. Zhang, Z. X. Ling, J. Wang, L. P . Xin (NAOC,CAS), E. Kuulkers, A. Santovincenzo (ESA), P . O'Brien (Univ. of Leicester), K. Nandra, A. Rau (MPE), B. Cordier (CEA) on behalf of the SVOM and Einstein Probe teams
We performed a follow-up observation of GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al. GCN 38214) with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. The observation started at 2024-11-13T15:43:11 (T-TGRB ~ 4.3hr) for about 3ks of exposure in total.
An uncatalogued X-ray source is detected by both FXT-A and FXT-B at the position (J2000)
RA, DEC = 110.2396, 46.787 (error=10", 90% C.L.), 1.09 arcminute away from the SVOM/ECLAIRs position (Dagoneau et al., GCN 38196). This position is also consistent with the optical afterglow detected by KAIT (Zheng et al., GCN 38232) and SVOM/VT (Qiu et al., GCN 38306).
A preliminary analysis shows that the spectrum can be fitted with an absorbed power law with nH=0.72*10^21 cm^-2 and the photon index of 2.11. The observed flux in the 0.5-10.0 keV is 1.7(-0.4/+0.4)*10^-13 erg/s/cm^2.
The above observation was made with the EP-FXT instrument. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES.
GCN Circular 38431
Subject
GRB 241113B : RAPAS follow-up observation
Date
2024-12-03T16:29:28Z (6 months ago)
From
Thierry Midavaine at GRANDMA <thierrymidavaine@sfr.fr>
Via
Web form
Thierry Midavaine on behalf of the RAPAS network reports (#2) :
Patrick Martinez, Pascal André, David Bregou, David Fardin, Erik Guthleben [1] observed the Gamma-Ray Burst GRB241113B (N. Dagoneau et al. GCN 38196, D. Turpin et al. GCN 38330) using [1] ADAGIO N 820mm telescope f=3.1m at Belesta Observatory (IAU A05) equiped with a Moravian C3 CMOS camera, 25mn exposure, equiped with RAPAS filter meeting the Gaia G photometric band. The FITS file is reduced with the Gaia photometric catalog in respective G band.
The afterglow is detected RA(J2000) = 07h20m55.30s ; Dec(J2000) = +46°48’13.1” Accy +/- 0.5“ [1]
MJD(mid) Gaia band mag. accy RAPAS station
60642.92014 G 22.25 +/-0.5 [1]
RAPAS ( https://proam-gemini.fr/rapas/ ) is a new ProAm collaboration funded by Paris Observatory, delivering to a network of french amateur observatories a set of 3 filters meeting the Gaia spectral bands. This network is dedicated to deliver data in the Gaia photometric system on selected astrophysical alerts by Astro-COLIBRI ( https://astro-colibri.com/ ) or from Gaia alerts.