GRB 241029A
GCN Circular 37932
Subject
GRB 241029A: Fermi GBM Final Real-time Localization
Date
2024-10-29T02:30:36Z (7 months ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
Via
email
The Fermi GBM team reports the detection of a likely LONG GRB
At 02:19:59 UT on 29 Oct 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241029A (trigger 751861204.86578 / 241029097).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 324.4, Dec = 6.6 (J2000 degrees, equivalent to J2000 21h 37m, 6d 35'), with a statistical uncertainty of 1.2 degrees.
The angle from the Fermi LAT boresight is 81.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241029097/quicklook/glg_skymap_all_bn241029097.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241029097/quicklook/glg_healpix_all_bn241029097.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241029097/quicklook/glg_lc_medres34_bn241029097.gif
GCN Circular 37934
Subject
GRB 241029A : Detection and localization of a bright long GRB by SVOM/ECLAIRs
Date
2024-10-29T07:47:35Z (7 months ago)
From
Stéphane Schanne at CEA Paris-Saclay/IRFU <s.schanne@cea.fr>
Via
Web form
SVOM/ECLAIRs Commissioning Team: Stéphane Schanne, Nicolas Dagoneau, Hervé Le Provost, Frédéric Chateau (CEA), Wenjin Xie, Donghua Zhao (NAOC), Jean-Luc Atteia, Laurent Bouchet, Sebastien Guillot, Juliette Alaux, Hui Yang (IRAP), Tais Maiolino (LUPM), Floriane Cangemi (APC), 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 detected and localized a bright long duration GRB 241029A at 2024-10-29T02:19:53 UTC (Tb), previously detected by Fermi (Fermi GBM team, GCN circular 37932), and by SVOM/GRM (SVOM reference: sb241002901).
The onboard trigger was not in operations, the following information was obtained by reprocessing on ground the data in the flight trigger algorithms. The burst was detected by the Count-Rate Trigger (CRT) and Image Trigger (IMT) which produced 22 Alert messages. The best Alert was obtained by CRT in the 8-120 keV energy band with a signal-to-noise ratio of 67.1 in a time window of 20.48 s starting at Tb.
The event location is RA, Dec = 325.327, Dec: 5.086 (J2000).
The statistical uncertainty on this position is 1.5 arcminutes to which we recommend adding 2 arcminutes of systematic uncertainty in quadrature.
SVOM did not slew to the burst since automated slewing was not enabled.
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: b.cordier AT cea.fr.
GCN Circular 37935
Subject
GRB 241029A: SVOM/GRM observation
Date
2024-10-29T10:14:31Z (7 months ago)
From
Chenwei Wang at IHEP <cwwang@ihep.ac.cn>
Via
Web form
SVOM/GRM team: 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, 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, 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 in-flight by GRB 241029A at 2024-10-29T02:19:58 UT (T0), which was also observed by Fermi/GBM (Fermi GBM Team, GCN 37932) and SVOM/ECLAIRs (Schanne et al. GCN 37934).
The real-time alert data and light curves of SVOM/GRM were downlinked to the ground through the VHF system with low latency. With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a T90 of 14.6 +0.6/-0.3 s.
The GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb241029A.png
This burst is located at about 29 degrees from the SVOM optical axis.
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: Chen-Wei Wang (IHEP)(cwwang@ihep.ac.cn)
GCN Circular 37936
Subject
GRB 241029A: Swift ToO observations
Date
2024-10-29T10:20:38Z (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 241029A.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021726
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 37937
Subject
GRB 241029A: TRT optical afterglow candidate detection
Date
2024-10-29T10:59:47Z (7 months ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Via
Web form
S.Q. Jiang, S.Y. Fu (NAOC), S. Tinyanont, R. Anutarawiramkul, P. Butpan (NARIT), J. An, X. Liu, Z.P. Zhu, Z. Fan, W.X. Li, N.C. Sun, Y.N. Wang, D. Xu (NAOC) report on behalf of a large collaboration:
We observed the field of GRB 241029A detected by Fermi/GBM (Fermi GBM team, GCN 37932), SVOM/ECLAIRs & SVOM/GRM (Schanne et al., GCN 37934; Wang et al., GCN 37935), using the 0.7-m telescope of the Thai Robotic Telescope network (TRT), located at Springbrook Observatory, New South Wales, Australia. Observations started at 09:49:01.281 UTC on 2024-10-29, i.e., 7.486 hrs after the SVOM/ECLAIRs trigger, and a series of 360 s frames were obtained in R-band.
An uncatalogued source is clearly detected in our stacked image within the SVOM/ECLAIRs error circle (Schanne et al., GCN 37934) at coordinates:
R.A. (J2000) = 21:41:20.16
Dec. (J2000) = +05:04:53.31
with an uncertainty of ~ 0.5 arcsec. The source has R = 20.06 +/- 0.08, calibrated with nearby PanSTARRS stars and not corrected for Galactic extinction. NEO can be ruled at this position at the observational time by checking MPC. No other credible candidate is found within the SVOM/ECLAIRs error circle.
We conclude that the source is likely the optical afterglow of the burst.
GCN Circular 37939
Subject
GRB 241029A: Mephisto observations
Date
2024-10-29T14:28:59Z (7 months ago)
From
Brajesh Kumar at SWIFAR, YNU <brajesh@ynu.edu.cn>
Via
Web form
Weikang Lin (SWIFAR, YNU), Guowang Du (SWIFAR, YNU), Brajesh Kumar (SWIFAR, YNU), Yangwei Zhang (SWIFAR, YNU), Tao Wang (SWIFAR, YNU), Xian-ao Wang (SWIFAR, YNU), Yaosong Yu (SWIFAR, YNU), Yu Pan (SWIFAR, YNU), Xingzhu Zou (SWIFAR, YNU), Xinlei Chen (SWIFAR, YNU), Jinghua Zhang (SWIFAR, YNU), Yuanpei Yang (SWIFAR, YNU), Yuan Fang (SWIFAR, YNU), Yehao Cheng (SWIFAR, YNU), Chenxu Liu (SWIFAR, YNU), Xuhui Han (NAOC), Pinpin Zhang (NAOC), Liping Xin (NAOC), Chao Wu (NAOC), Xiangkun Liu (SWIFAR, YNU), Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team:
The 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory was triggered to observe the field of GRB 241029A detected by Fermi/GBM (Fermi GBM team, GCN 37932), SVOM/ECLAIRs and SVOM/GRM (Schanne et al., GCN 37934; Wang et al., GCN 37935). Several uvgriz-band images were acquired starting from 11:47:29 2024-10-29 UT. We clearly detect the uncatalogued source reported by Jiang et al. (GCN 37937) in 300s of r band images and the preliminary estimated magnitude is 20.47+- 0.11 (r-band, 12:19:27 2024-10-29 UT). Further analysis is in progress.
--------------------------------------------------------------------------
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.
--------------------------------------------------------------------------
GCN Circular 37940
Subject
GRB 241029A: Xinglong-2.16m optical afterglow confirmation
Date
2024-10-29T14:45:50Z (7 months ago)
Edited On
2024-10-29T14:49:23Z (7 months ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Edited By
Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov> on behalf of Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Via
Web form
S.Q. Jiang, Z.P. Zhu, S.Y. Fu, J. An, X. Liu, L.P. Xin, X.H. Han, J. Wang, D. Xu, C. Wu, J.Y. Wei (NAOC) report:
We observed the field of GRB 241029A detected by Fermi/GBM (Fermi GBM team, GCN 37932), SVOM/ECLAIRs & SVOM/GRM (Schanne et al., GCN 37934; Wang et al., GCN 37935) using the 2.16m telescope located at Xinglong, Hebei, China, equipped with the BFOSC camera. Observations started at 13:17:07 UT on 2024-10-29, i.e., 10.95 hr after the SVOM/ECLAIRs trigger, and a series of 360 s frames were obtained in R-band.
The previously reproted optical source (Jiang et al., GCN 37937; Lin et al., GCN 37939) is clearly detected in the stacked image, and it has decayed to R = 20.52 +/- 0.04 at 11.21 hr after the SVOM/ECLAIRs trigger, calibrated with nearby PanSTARRS stars and not corrected for Galactic extinction. We thus think the source is the optical afterglow of the burst.
We thank the great support of the Xinglong-2.16m staff, in particular Yinan Zhu and Jie Zheng.
GCN Circular 37941
Subject
GRB 241029A: MASTER early optical counterpart detection
Date
2024-10-29T16:02:37Z (7 months ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
V.Lipunov, E.Gorbovskoy, N.Tiurina, D.Vlasenko, I.Panchenko, A.Kuznetsov (Lomonosov MSU),
P.Balanutsa, G.Antipov, N.Tiurina, A.Sankovich, A.Sosnovskij, M.Gulyaev, Ya.Kechin, V.Senik (Lomonosov MSU),
O.Gress, N.Budnev(ISU),
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
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 Global robotic net (http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L)
started observation of Fermi GRB 241029A (GCN 37932, Ttrigger=02:19:59 UT) at MASTER-OAFA (Lipunov et al. GCN 37933, cover map https://master.sai.msu.ru/site/master2/observ.php?id=2652352 )
66 sec after notice time (101 sec after trigger time) at 2024-10-29 02:21:41 UT.
At first images (20s expositions) MASTER auto-detection system detected
optical transient MASTER OT J214120.16+050453.4
at (RA, Dec) = 21h 41m 20.16s +05d 04m 53.4s on 2024-10-29.09839 UT.
The OT magnitude (unfiltered) is ~13.4m (mlim=16.8). OT automatic light curve http://observ.pereplet.ru/GRB/MASTERGRB241029A_LC.jpg
The OT is seen in 6 images. There is no minor planet at this place.
We have reference image on 2017-05-29.35167 UT with unfiltered 18.3m.
This OT was first publishied by Jiang et al. (GCN 37937, started at 09:49:01 UTC with m_OT=20.0 in R ) and continued by Weikang Lin et al. (GCN 37939), Jiang et al. GCN 37940.
Observations in MASTER-Tunka and other MASTER Global Robotic Net telescopess will be continued.
GCN Circular 37943
Subject
GRB 241029A: GOTO optical afterglow detection
Date
2024-10-29T17:15:04Z (7 months ago)
From
kendall.ackley@warwick.ac.uk
Via
Web form
K. Ackley, B. P. Gompertz, A. Kumar, D. O'Neill, R. Starling, M. J. Dyer, J. Lyman, K. Ulaczyk, F. Jimenez-Ibarra, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Palle and D. Pollacco report on behalf of the GOTO collaboration:
We report on observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022, Dyer et al. 2024) in response to GRB 241029A, detected by Fermi/GBM (Fermi GBM team, GCN 37932), SVOM/ECLAIRs (Schanne et al., GCN 37934) and SVOM/GRM (Wang et al., GCN 37935). Observations were performed by GOTO-S between 09:46:21 and 12:06:59 UT on 2024-10-29 (starting 7.34 hours after trigger). Each observation consisted of 4x90s exposures in the GOTO L-band (400-700 nm).
Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using deeper template observations of the same pointings. We detect the reported optical afterglow, originally discovered by TRT (Jiang et al., GCN 37937) and confirmed by Mephisto (Lin et al., GCN 37939), Xinglong-2.16m (Jiang et al., GCN 37940) and MASTER (Francile et al., GCN 37941). We obtained the following 3-sigma detections and limits of the optical counterpart:
Date | T-T0 (d) | Filter | Mag
-----------------------------------------------------------------------
2024-10-29 09:49:05 | 0.312 | L | 20.59 ± 0.3
2024-10-29 10:55:41 | 0.358 | L | 20.62 ± 0.4
2024-10-29 12:03:21 | 0.405 | L | >20.43
Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.
Observations are ongoing.
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 37944
Subject
GRB 241029A: AKO Optical Afterglow Detection
Date
2024-10-29T17:24:39Z (7 months ago)
From
Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>
Via
legacy email
Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE), and Nidhal Guessoum (American
University of Sharjah, UAE), report:
We observed the field of GRB 241029A detected by Fermi/GBM (Fermi GBM team,
GCN 37932), SVOM/ECLAIRs & SVOM/GRM (Schanne et al., GCN 37934; Wang et
al., GCN 37935), with our 0.36m f/7.7 robotic telescope. The observation
started on 29 October 2024 at 15:36 (UT), 13.3 hours from the trigger.
We obtained multiple 180-sec exposures in Ic filter. We barely detected the
optical afterglow at:
R.A. (J2000): 21:41:20.11
Dec. (J2000): +05:04:53.2
Our detection is consistent with the results of (Jiang et al., GCN 37937;
Lin et al., GCN 37939; Jiang et al., GCN 37940; Francile et al., GCN 37941;
Ackley et al., GCN 37943).
The following observation was calculated using Atlas catalogue as a
reference:
----------------------------------------------------------------------------
-
ObsTime (mid), Exposure (sec), Filter, Mag
----------------------------------------------------------------------------
-
2024-10-29T16:18:15Z, 28 x 180s (stacked), Ic, 19.9 +/- 0.32
----------------------------------------------------------------------------
-
The magnitude is not corrected for galactic extinction.
GCN Circular 37945
Subject
GRB 241029A: Fermi GBM Observation
Date
2024-10-29T18:20:11Z (7 months ago)
From
Ava Myers at NASA GSFC <ava.myers@nasa.gov>
Via
Web form
A. Myers (NPP/GSFC), M. Godwin (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team:
At 02:19:59.87 UT on 29 October 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 241029A (trigger 751861204/241029097).
which was also detected by SVOM/ECLAIRs (S. Schanne et al., GCN [37934](https://gcn.nasa.gov/circulars/37934)).
The Fermi GBM on-ground location is consistent with the SVOM position.
The angle from the Fermi LAT boresight is 76 degrees.
The GBM light curve consists of multiple peaks with a duration (T90)
of about 13.3 s (50-300 keV). The time-averaged spectrum
from T0 to T0+13.152 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.01 +/- 0.04 and the cutoff energy,
parameterized as Epeak, is 220 +/- 10 keV.
The event fluence (10-1000 keV) in this time interval is
(9.2 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band is 9.6 +/- 0.4 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 190 +/- 20 keV, alpha = -0.96 +/- 0.05 and beta = -2.5 +/- 0.3.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/
GCN Circular 37946
Subject
GRB 241029A: Swift-XRT observations
Date
2024-10-29T18:39:18Z (7 months ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , D.N. Burrows
(PSU), M. A. Williams (PSU), S. Dichiara (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), M. Capalbi (INAF-IASFPA) 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 241029A, collecting 747 s of Photon
Counting (PC) mode data between T0+29.1 ks and T0+30.0 ks.
One uncatalogued X-ray source has been detected consistent with being
within 434 arcsec of the SVOM/ECLAIRs position, it is below the RASS
limit and shows no definitive signs of fading. The X-ray position is
consistent with the optical transient reported by Jiang et al. (GCN
37937), Lin et al., (GCN 37939), Jiang et al. (GCN 37940), Francile et
al. (GCN 37941), Ackley et al. (GCN 37943), Odeh et al. (GCN 37944).
Source 1:
RA (J2000.0): 325.3343 = 21:41:20.23
Dec (J2000.0): +5.0814 = +05:04:53.0
Error: 3.4 arcsec (radius, 90% conf. [Enhanced position])
Count-rate: 0.080 +/- 0.012 ct s^-1
Distance: 87 arcsec from SVOM/ECLAIRs position.
Flux: (2.60 +/- 0.39)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)
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/00021726.
This circular is an official product of the Swift-XRT team.
GCN Circular 37948
Subject
MISTRAL@OHP photometric and spectroscopic observations of GRB 241029A
Date
2024-10-29T22:13:27Z (7 months ago)
From
Christophe Adami at LAM <christophe.adami@lam.fr>
Via
Web form
C. Adami, S. Basa (LAM/Pytheas/AMU), E. Le Floc'h, D. Turpin, F. Schussler (CEA Paris-Saclay),
J. Palmerio (GEPI, Obs. de Paris), B. Schneider (MIT), A. Saccardi (GEPI/Obs. de Paris & CEA
Paris-Saclay), report on behalf of the MISTRAL GRB collaboration:
We first performed imaging of the field of GRB 241029A (Fermi GBM team, GCN 37932; Schanne et al.,
GCN 37934; Chenwei Wang et al., GCN 37935; Evans et al., GCN 37936; Jiang et al., GCN 37937;
Weikang Lin et al., GCN 37939; Jiang et al., GCN 37940; Francile et al., GCN 37941; Ackley et al.,
GCN 37943; Odeh et al., GCN 37944; Myers et al., GCN 37945; Bernardini et al., GCN 37946) with
MISTRAL mounted on the 1.93 m telescope at Observatoire du Haut Provence (OHP, France).
The observations consisted of 300s + 600s exposures in r-band plus 2x600s in g-band. We have
very clear detections of the transient object both in g and r-band images: using as reference
field stars from the Pan-STARRS catalogue, we determine preliminar magnitudes of r(AB) =
21.6 +/- 0.1 mag and g(AB) = 21.4 +/- 0.1 mag at a mean date of 2024-10-29T18:12:00 UT, ~16
hours after the burst.
We immediately after took a spectrum of the object using the MISTRAL blue grism (end of data
collection at 2024-10-29T19:45:21UT, ~17h30 after ther burst). Our spectrum cover the wavelength
range 4200-8000 AA and consist of one exposure of 1500 seconds. We detect a weak but significant
continuum between ~5700/5900 and ~6500AA and this suggests an upper limit of 3.7/3.9 for the
redshift.
We acknowledge the excellent support from Observatoire de Haute-Provence and in particular
Yoann Degot-Longhi for the MISTRAL observations and Thomas Baycroft.
GCN Circular 37950
Subject
GRB 241029A: GTC/OSIRIS+ spectroscopic redshift z=1.072
Date
2024-10-29T23:35:55Z (7 months ago)
From
Antonio Martin-Carrillo at UCD,Space Science Group <antonio.martin-carrillo@ucd.ie>
Via
Web form
J. F. Agui Fernandez (CAHA), A. de Ugarte Postigo (LAM/OCA, CNRS), D. B. Malesani (DAWN/NBI and Radboud Univ.), A. Martin-Carrillo (UCD), G. Lombardi (GTC), C. C. Thoene (ASU-CAS, AbAO), N. R. Tanvir (U. Leicester), L. Izzo (INAF-OACn & DARK/NBI), S. Geier (GTC), D. Perez Valladares (GTC) report:
We observed the afterglow of GRB 241029A (Fermi GBM team, GCN 37932; Schanne et al., GCN 37934; Chenwei Wang et al., GCN 37935; Evans et al., GCN 37936; Jiang et al., GCN 37937; Weikang Lin et al., GCN 37939; Jiang et al., GCN 37940; Francile et al., GCN 37941; Ackley et al., GCN 37943; Odeh et al., GCN 37944; Myers et al., GCN 37945; Bernardini et al., GCN 37946, Adami et al., GCN 37948) using OSIRIS+ on the 10.4 m GTC telescope, at the Roque de los Muchachos Observatory (La Palma, Spain). The observation consisted of 4 acquisition images in r-band, followed by a 4x1200 s spectrum. The spectrum was obtained with grism R1000B, covering the spectral range between 3650 and 7800 AA at a resolving power of 600.
The acquisition image, obtained at 2024-10-29T21:32:51 UT, 19.21 hr since the Fermi trigger, shows the afterglow at r(AB) = 21.40 +/- 0.04 mag, as compared to SDSS field stars. The spectrum has a strong continuum throughout the complete range with absorption features due Fe II, FeII*, Mn II, Mg II, Mg I and the [O II] doublet at z = 1.072, which we propose as the redshift of GRB 241029A.
GCN Circular 37954
Subject
GRB 241029A: SAO RAS optical observations
Date
2024-10-30T02:10:46Z (7 months ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin and O. I. Spiridonova (SAO RAS), report
on behalf of the GRB follow-up team.
We observed the field of GRB 241029A (Fermi GBM team, GCN 37932;
Schanne et al., GCN 37934; Wang et al., GCN 37935; Myers and Godwin,
GCN 37945; Bernardini et al., GCN 37946) with the 1-m telescope
of SAO RAS equipped with the CCD-photometer. We obtained 6 x 300 sec.
images in Rc band on October 29, 18:39:32--19:13:23 UT (16.6079 hours
after the burst).
The OT (Jiang et al., GCNs 37937, 37940; Lin et al., GCN 37939;
Francile et al., GCN 37941; Ackley et al., 37943; Odeh and Guessoum,
GCN 37944; Adami et al., GCN 37948; Fernandez et al., GCN 37950)
is clearly detected in our stacked
frame with the brightness of R = 20.98 +/- 0.05 (R_lim = 23.0).
This preliminary photometry is based on nearby SDSS stars (magnitudes
converted with Lupton 2005 equations) and not corrected for the Galaxy
extinction.
GCN Circular 37961
Subject
GRB 241029A: GROWTH-India Telescope optical follow up
Date
2024-10-30T10:03:34Z (7 months ago)
Edited On
2024-10-30T15:33:33Z (7 months ago)
From
vishwajeet.s@iitb.ac.in
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of V. Swain at IIT Bombay <vishwajeet.s@iitb.ac.in>
Via
Web form
A.P. Saikia, T. Mohan, V. Swain, R. Kumar, 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 GRB 241029A by Fermi/GBM (Fermi GBM team, GCN 37932), SVOM/ECLAIRs & SVOM/GRM (Schanne et al., GCN 37934; Wang et al., GCN 37935) with 0.7m GROWTH-India Telescope (GIT). We started the observation at 2024-10-29 14:08:55 UT, i.e., 11.8 hours after the Fermi GBM trigger. We obtained multiple exposures of 360 seconds in r' filter. We clearly detected the afterglow in our stacked image at the positions given by TRT (Jiang et. al., GCN 37937). The photometry result follows as:
---------------------------------------------------------------------------------
| JD (mid) | t-t0 (hours) | Filter | Total Exposure (s) | Magnitude (AB) |
| ----------------- | ----------- |------- | ------------------ | -------------- |
| 2460613.16666 | 13.6 | r' | 6x360 | 20.97 +/- 0.10 |
---------------------------------------------------------------------------------
Our result is consistent with Jiang et al., (GCN 37937), Lin et al., (GCN 37939), Jiang et al., (GCN 37940), Francile et al., (GCN 37941), Ackley et al., (GCN 37943), Odeh et al., (GCN 37944), Moskvitin et al., (GCN 37954).
The measurement is 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 37994
Subject
GRB 241029A: SVOM/VT optical afterglow observations
Date
2024-10-31T00:13:56Z (7 months ago)
From
SVOM_group <svomgroup@bao.ac.cn>
Via
Web form
SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, C. Wu, L. P. Xin, 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), S. L. Xiong(IHEP)
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:
VT started to observe the field of GRB 241029A triggered by Fermi/GBM (Fermi GBM team, GCN 37932) and SVOM/ECLAIRs & SVOM/GRM (Schanne et al., GCN 37934; Wang et al., GCN 37935) via ToO observations started at 2024-10-29T21:41:18.43, about 19.2 hours after the burst. The VT conducted observations simultaneously in two channels: VT_B (400nm-650nm) and VT_R (650nm-1000nm).
The counterpart (Jiang et. al. GCNa 37937; Lin et al., GCN 37939; Jiang et al., GCN 37940; Francile et al., GCN 37941; Ackley et al., GCN 37943; Odeh et al., GCN 37944; Moskvitin et al., GCN 37954; Saikia et al.,GCN 37961) was detected in both bands with VT_B=23.3+/-0.3 mag and VT_R=21.8+/-0.12 mag with a 2.2 ks exposed time of VT.
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 38006
Subject
GRB 241029A: LCO optical detection
Date
2024-10-31T12:14:05Z (7 months ago)
From
Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>
Via
Web form
L. Izzo (INAF-OACn and DARK/NBI) and D. B. Malesani (DAWN/NBI and Radboud Univ.) report:
We observed the field of the GRB 241029A (Schanne et al., GCN #37934; Wang et al., GCN #37935; Myers & Godwin, GCN 37945) with the Sinistro instrument mounted on the 1-m telescope of the LCO network, located at the Siding Spring Observatory, Australia. Observations started on 2024 October 29 at 09:21:56 UT (7.03 hr after the GRB trigger). We obtained a sequence of 3x180 s images in the SDSS-r filter.
In the stacked r-band image, we clearly detect the optical afterglow previously reported by other facilities (Jiang et al., GCN #37937; Lin et al., GCN #37939; Jiang et al., GCN #37940; Francile et al., GCN #37941; Ackley et al., GCN #37943; Odeh et al., GCN #37944; Adami et al., GCN #37948; Agui Fernandez et al., GCN #37950; Moskvitin & Spiridonova, GCN #37954; Saikia et al., GCN #37961; Qiu et al., GCN #37994) and by Swift-XRT (Bernardini et al., GCN #37946). We measure a preliminary magnitude of r = 20.32 +/- 0.07 mag (AB), calibrated against nearby stars from the Pan-STARRS catalog.
This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No 101004719.
GCN Circular 38009
Subject
GRB 241029A: COLIBRI Detection of the Optical Counterpart
Date
2024-10-31T13:28:54Z (7 months ago)
From
Alan Watson at UNAM <alan@astro.unam.mx>
Via
legacy email
Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM),
D. Akl (AUS), S. Antier (OCA), Jean-Luc Atteia (IRAP), Nathaniel R. Butler
(ASU), Damien Dornic (CPPM), J.-G. Ducoin (CPPM), Francis Fortin (IRAP),
Simona Lombardo (LAM), Francesco Magnani (CPPM), and Margarita Pereyra
(UNAM)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang
(IHEP), Stéphane Basa (LAM), Jean-Luc Atteia (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:
We imaged again the field of GRB 241029A detected by Fermi/GBM,
SVOM/ECLAIRs, and SVOM/GRM (Fermi GBM Team, GCN Circ. 37932; Schanne et
al., GCN Circ. 37956; Wang et al., GCN Circ. 37935) during the
commissioning of the COLIBRÍ (SVOM/F-GFT) telescope at the Observatorio
Astronómico Nacional on the Sierra de San Pedro Mártir in Mexico.
We observed with the engineering test camera in a red filter that
approximates SDSS r. The data were reduced using custom software and then
analysed and calibrated against the PS1 catalog using the STDWeb service
(Karpov et al. 2022).
In 4560 seconds of exposure from 2024-10-30 02:10 to 06:12 UTC (0.99 to
1.16 days after the trigger), we detect the optical counterpart (Jiang et
al, GCN Circ. 37937) with an AB magnitude of:
r = 21.78 +/- 0.15
This magnitude is consistent with the last optical observations reported
(Agui Fernandez et al., GCN Circ. 37950, Moskvitin et al., GCN Circ. 37954;
Qiu et al., GCN Circ. 37994).
We warmly thank the COLIBRI engineering team and the staff of the
Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir
GCN Circular 38048
Subject
GRB 241029A: GRBAlpha detection
Date
2024-11-02T19:24:49Z (7 months ago)
From
Marianna Dafčíková at Masaryk University <500025@mail.muni.cz>
Via
Web form
M. Dafcikova, J. Ripa, M. Kolar (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Duriskova, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.
The long-duration GRB 241029A (Fermi/GBM detection: GCN 37932; SVOM/GRM detection: GCN 37935) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract).
The detection was confirmed at the peak time 2024-10-29 02:19:59.8 UTC. The T90 duration measured by GRBAlpha is 10.5 s and the overall significance during T90 reaches 10.5 sigma.
The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB241029A_GCN.pdf
All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/
GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.
GCN Circular 38669
Subject
GRB 241029A: AbAO AS-32 optical observations
Date
2024-12-25T07:22:16Z (5 months ago)
From
Nicolai Pankov at HSE, IKI RAS <colinsergesen@gmail.com>
Via
Web form
N. Pankov (HSE, IKI), R. Ya. Inasaridze (AbAO), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN:
We performed optical observations of the field of GRB 241029A (The Fermi GBM team, GCN 37932; Schanne et. al, GCN 37934; Wang et. al, GCN 37935; Evans, GCN 37936; Jiang et. al, GCN 37937; Lin et. al, GCN 37939; Jiang et. al, GCN 37940; C.Francile et. al, GCN 37941; Ackley et. al, GCN 37943; Odeh et. al, GCN 37944; Myers et. al, GCN 37945; Bernardini et. al, GCN 37946; Adami et. al, GCN 37948; Fernandez et. al, GCN 37950; Moskvitin et. al, GCN 37954; Saikia et. al, GCN 37961; Qiu et. al, GCN 37994; Izzo, GCN 38006; Watson et. al, GCN 38009; Dafcikova et. al, GCN 38048) in the R filter with AS-32 of Abastumani observatory (AbAO) equipped with CCD-photometer FLI PL4240. The observations began on 2024-10-29 15:10 UT, i.e. ~0.55 days since trigger. The optical counterpart is marginally detected in the stacked image of 43*60 sec. The preliminary photometry is given below:
Date UT start t-T0 Exp. Filter OT Err. UL(3sigma)
(mid, days) (s)
2024-10-29 15:10:45 0.550185 43*60 R 20.9 0.3 20.9
The magnitudes were calibrated using nearby stars from USNO-B1.0 (R2 magnitudes) and are not corrected for the Galactic extinction.
GCN Circular 38672
Subject
GRB 241029A: LCO optical observation
Date
2024-12-26T14:00:51Z (5 months ago)
From
ankur ghosh at CAPP, University of Johannesburg <ghosh.ankur1994@gmail.com>
Via
Web form
Ankur Ghosh, Soebur Razzaque (CAPP, University of Johannesburg), Navin Dukiya (ARIES), Alexander Moskvitin (SAO RAS), Yulia Sotnikova (SAO RAS) on behalf of a larger collaboration.
We observed the field of the GRB 241029A (The Fermi GBM team, GCN 37932; Schanne et. al, GCN 37934; Wang et. al, GCN 37935; Evans, GCN 37936) using r filter of the 1-meter Sinistro telescope and B filter of the 0.4-m SCICAM QHY600 at the Las Cumbres Observatory Global Telescope (LCOGT) node located at South African Astronomical Observatory (SAAO) Sutherland observatory. The 1-m Sinistro telescope is equipped with a 4K x 4K CCD (FOV: 26 x 26 arcmin, scale: 0.39 arcsec/pixel) and the 0.4 m SCICAM QHY600 is equipped with 9576 x 6388 pixel CCD (FOV: 1.9 x 1.2 degrees, scale: 0.74 arcsec/pixel).
Observations began on October 30 2024, starting from 22.30 hours after the trigger of GRB 241029A. We clearly detect the optical transient (OT) reported by GCNs (Jiang et. al, GCN 37937; Lin et. al, GCN 37939; Jiang et. al, GCN 37940; C.Francile et. al, GCN 37941; Ackley et. al, GCN 37943; Odeh et. al, GCN 37944; Myers et. al, GCN 37945; Bernardini et. al, GCN 37946; Adami et. al, GCN 37948; Fernandez et. al, GCN 37950; Moskvitin et. al, GCN 37954; Saikia et. al, GCN 37961; Qiu et. al, GCN 37994; Izzo, GCN 38006; Watson et. al, GCN 38009; Dafcikova et. al, GCN 38048, Pankov et. al, GCN 38669) in our stacked images. Our detection is well consistent with the observation reported at the similar epoch by Watson et. al, GCN 38009.
dateobs jd t-t0 (hrs) mag dmag telescope filter
2024-10-30 2460613.52658 22.30 21.9422 0.2573 0m4-76 B
2024-10-30 2460613.99240 33.48 22.1959 0.0399 1m0-11 r
The field was calibrated against nearby APASS stars, with magnitudes converted using Lupton (2005) equations, and has not been corrected for Galactic extinction.