Gamma-ray Burst 241017A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

none

Results of Observations

GCN Circular #37799
FROM: St=C3=A9phane Schanne at CEA Paris-Saclay/IRFU
SVOM/ECLAIRs Commissioning Team: Herv=C3=A9 Le Provost, St=C3=A9phane Scha= nne, Fr=C3=A9d=C3=A9ric Chateau, Nicolas Dagoneau (CEA), Jean-Luc Atteia, L= aurent Bouchet, Sebastien Guillot, Juliette Alaux (IRAP), Wenjin Xie (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 soft transient, labelled GRB 241017A (sb24101702) at 2024-10-17T0= 3:57:04 UT (Tb).
The burst was detected by the Image Trigger (IMT), which sent 1 Alert, with= a signal-to-noise ratio of 6.9 in the 5-8 keV energy band over a time wind= ow of 40.96 s starting at Tb. The excess was confirmed after reception of the full dataset on ground.
The localization of the burst is RA, Dec =3D 356.28, 15.72 (J2000).
The statistical uncertainty on this position is 12.4 arcminutes, to which w= e recommend adding 10 arcminutes of systematic uncertainty in quadrature.
The significance of the detection was too low to request an automatic slew = of SVOM to the burst position.
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: s.schanne AT cea.fr
GCN Circular #37800
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the SVOM/ECLAIRs GRB 241017A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021723
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 #37805
Viraj Karambelkar (Caltech), Benjamin Schneider (MIT), Geoffrey Mo (MIT), Robert Stein (Caltech), Tomas Ahumada (Caltech), Nathan Lourie (MIT), Danielle Frostig (CFA), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report:
We observed the field of the SVOM/ECLAIRs GRB 241017A (Le Provost et al, GCN 37799) 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 2024-10-17T07:40:52 UTC (~3.7 hours 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 95% of the 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 ~ 19.3 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 #37807
SVOM/MXT Commissioning Team: D. G=C3=B6tz (CEA Irfu/DAp), A. Fort, J. Joube= rt, K. Mercier, S. Crepaldi (CNES), F. Robinet, N. Leroy (IJCLab), P. Ferra= ndo, H. Goto, A. Meuris, M. Moita, C. Plasse, A. Sauvageon (CEA), P. Maggi,= L. Michel (ObAS)=20
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), Shaolin Xiong (IHE= P), Bing Zhang (UNLV)
Report on behalf of the SVOM team:
MXT observed the field of GRB241017A (Le Provost et al., GCN 37799) as a To= O from 2024 October 17th at 18:05 UTC for about 4ks, about 14 hours after = T0.
Our preliminary analysis shows no obvious X-ray conterpart in the entire EC= LAIRs error region down to a limit of about 1e-12 erg/cmsq/s in the 0.5-10 = keV energy band.
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. MXT was developed jointly by CEA, CNES, University of Leicester, IJ= CLab and MPE.
GCN Circular #37808
T. Mohan, A.P. Saikia, R. Kumar, V. Swain, V. Bhalerao (IITB), G.C. Anupama, S. Barway (IIA) and K. Angail (IAO) report on behalf of the GIT team:
We observed the field of the GRB 241017A (SVOM/ECLAIRs team, GCN 37799) with the 0.7m GROWTH-India Telescope (GIT). With the current GIT camera with a field of view of 11' x 7', observed 12 tiles to cover the area for the statistical and systematic uncertainity regions mentioned in GCN 37799.
Obserations started at 2024-10-17 19:02:04 UT, about 15.1 hours after the SVOM/ECLAIRs trigger. Each tile had image of 360s in r' filter. We did not detect any new source in our images. In particular, we do not find any source in the error circle of uncatalogued source at 356.1750d, +15.6574d reported in the automated Swift follow-up (GCN #37800, https://gcn.gsfc.nasa.gov/other/21723.counterpart). Due to the proximity to the bright moon (~28 deg), the images were shallower than usual.
```
| MJD mid     | RA      | Dec    | Lim Mag (5-sigma) |
| ----------- | ------- | ------ | ----------------- |
| 60600.79518 | 356.305 | 15.731 | 19.2  |
| 60600.79972 | 356.637 | 15.726 | 19.3  |
| 60600.80424 | 356.238 | 15.725 | 19.2  |
| 60600.81313 | 356.515 | 15.894 | 19.3  |
| 60600.81766 | 356.367 | 15.892 | 19.1  |
| 60600.82209 | 356.382 | 15.563 | 19.5  |
| 60600.82654 | 356.248 | 15.559 | 19.5  |
| 60600.83556 | 356.101 | 15.723 | 19.1  |
| 60600.84000 | 356.511 | 15.561 | 19.4  |
| 60600.84452 | 356.096 | 15.892 | 19.1  |
| 60600.84894 | 356.376 | 15.729 | 19.4  |
| 60600.85339 | 356.513 | 15.734 | 19.6  |
```
The magnitude are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.
The GROWTH India Telescope (GIT, Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.
GCN Circular #37810
A. Bochenek, D. A. Perley (LJMU) report:
We observed the field of GRB241017a (Le Provost et al, GCN 37799) containing all three reported uncatalogued XRT sources from the Swift ToO follow-up (Evans, GCN 37800) using the IO:O optical camera on the 2m robotic Liverpool Telescope. We obtained 6x100s exposures with the SDSS-i filter starting at 2024-10-17 21:52:53 UT, approximately 18 hours after the SVOM trigger.
The images were stacked and a reference image of the field from SDSS DR12 was subtracted using PSF matching with the help of PSFEx. No uncatalogued optical source was detected at any of the three locations, nor in the entire field of view of IO:O. The 3-sigma limiting magnitude on the stacked image is i > 21.21 mag.
GCN Circular #37811
J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAR), D.N. Burrows (PSU), M. A. Williams (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 241017A, collecting 2.9 ks of Photon Counting (PC) mode data between T0+35.9 ks and T0+48.7 ks.
Three uncatalogued X-ray sources have been detected, however none of them is above the RASS limit or shows definitive signs of fading. Therefore, at the present time we cannot identify which, if any, is the afterglow. Details of these sources are given below:
Source 1:
```
  RA (J2000.0):  356.1750  =  23:44:41.99
  Dec (J2000.0): +15.6574  =  +15:39:26.8
  Error: 6.3 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (5.2 [+1.9, -1.6])e-3 ct s^-1   
  Distance: 420 arcsec from SVOM/ECLAIRs position.
  Flux: (1.48 [+0.55, -0.45])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)
```
Source 2:
```
  RA (J2000.0):  356.2126  =  23:44:51.02
  Dec (J2000.0): +15.5360  =  +15:32:09.7
  Error: 6.4 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (7.3 [+2.4, -1.9])e-3 ct s^-1   
  Distance: 696 arcsec from SVOM/ECLAIRs position.
  Flux: (1.21 [+0.39, -0.32])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

  This source is 0.6" from the SIMBAD position of [CBS2017] ALH2L293,
  an AGN candidate.
```
Source 3:
```
  RA (J2000.0):  356.2454  =  23:44:58.90
  Dec (J2000.0): +15.5560  =  +15:33:21.7
  Error: 5.3 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (2.4 [+1.4, -1.0])e-3 ct s^-1   
  Distance: 597 arcsec from SVOM/ECLAIRs position.
```
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/00021723.
This circular is an official product of the Swift-XRT team.
GCN Circular #37820
SVOM/VT commissioning team: Y. L. Qiu, L. P. Xin, H. L. Li, C. Wu, X. H. Ha= n, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. De= ng, 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)
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 of SVOM mission, we observed the GRB 241017A= detected by SVOM/Eclairs (Le Provost et al, GCN 37799) with SVOM/VT telesc= ope in ToO mode. The observation started at 2024-10-17T18:00:17 UT, about 1= 4.0 hours after the burst, with a total exposure time of 4320 seconds. The = VT telescope conducted observations simultaneously in two channels: VT_B (4= 00nm-650nm) and VT_R (650nm-1000nm).
Analysis shows that, no any uncatalogued source was detected within the err= or circles of any of the three X-ray sources (Kennea et al., GCN 37811) wit= h the 3 sigma limit magnitudes of about 23.9 mag for VT_B and 23.6 mag for = VT_R in AB magnitude system, after stacking the images for both bands separ= ately.
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. VT was jointly developed by Xi'a= n Institute of Optics and Precision Mechanics (XIOPM), CAS and National ast= ronomical observatories (NAOC),CAS.
GCN Circular #37829
Xiangkun Liu (SWIFAR, YNU), Brajesh Kumar (SWIFAR, YNU), Guowang Du (SWIFAR= , YNU), Kaushik Chatterjee (SWIFAR, YNU), Fanchuan Kong (SWIFAR, YNU), Yaos= ong Yu (SWIFAR, YNU), Xingzhu Zou (SWIFAR, YNU), Yu Pan (SWIFAR, YNU), Xinl= ei Chen (SWIFAR, YNU), Yuanpei Yang (SWIFAR, YNU), Yehao Cheng (SWIFAR, YNU= ), Jinghua Zhang (SWIFAR, YNU), Yuan Fang (SWIFAR, YNU), Xuhui Han (NAOC), = Pinpin Zhang (NAOC), Liping Xin (NAOC), Chao Wu (NAOC), Xiaowei Liu (SWIFAR= , YNU) report on behalf of the Mephisto Team: We performed simultaneous multi-band photometric observations of GRB 241017= A/sb24101702 (Le Provost et al., GCN 37799) with the 1.6m Multi-channel Pho= tometric Survey Telescope (Mephisto) of Yunnan University located at Lijian= g Observatory. The observations were initiated at 15:35:30 2024-10-17 UT (~= 11.6 hrs after SVOM/Eclairs trigger) and several frames were taken in uvgri= z bands (although affected with high background due to the moon light). We = did not find any uncatalogued source in the stacked images which is consist= ent with the results reported by Mohan et al. (GCN 37808), Bochenek et al. = (GCN 37810) and Qiu et al. (GCN 37820). The 3-sigma limiting magnitudes are= below:
```
Mid-Time (UT)          Band  Total-Exp (s)  Lim-mag (AB)
2024-10-17T15:53:31    u       180s x 4       >21.07
2024-10-17T15:52:06    v       180s x 4       >21.70
2024-10-17T15:52:58    g        50s x 10      >19.89
2024-10-17T15:51:33    r        50s x 10      >22.14
2024-10-17T15:53:05    i=C2=A0       79s x 7       >20.09
2024-10-17T15:51:40    z=C2=A0       79s x 7       >19.48
```
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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 ima= ging the same field of view in three optical bands simultaneously. It provi= des real-time, high-quality colors of stellar objects. The on-site telescop= e assemblage and commissioning were carried out in September 2022. The firs= t light in all three channels was achieved on 2023 December 21.
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GCN Circular #37838
Anshika Gupta, Amit K. Ror, Arjun Dawn, Kuntal Mishra and Shashi B. Pandey (ARIES) report:
We observed the field of GRB 241017A detected by SVOM (SVOM Team, GCN 37799), with the 1.3m Devasthal Fast Optical Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2024-10-18 at 15:57:20 UT, nearly 1.5 days after the SVOM trigger. We took multiple frames with an exposure time of 300 s in the R filter. We did not detect any optical afterglow in the stacked image within the error box of the burst position by the SVOM team (GCN 37799). We obtain the following preliminary 3-sigma upper limit in the stacked image:
Date Start_UT T_start-T0 (days) Filter Exp time (s) Limiting magnitude
================================================================
2024-10-18 15:57:20 ~1.5 R 300*12 > 22.0
Our non-detection is consistent with Karambelkar et al. 2024 (GCN 37805); Mohan et al. 2024 (GCN 37808); Bochenek et al. 2024 (GCN 37810); and SVOM Team (GCN 37820).
The magnitude is not corrected for the Galactic extinction in the direction of the burst. Photometric calibration is performed using the standard stars from the USNO-B1.0 catalog. This circular may be cited.

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