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GRB 251016A

GCN Circular 42601

Subject
GRB 251016A: TERI Gamma-ray detection of a short burst
Date
2025-11-06T15:50:38Z (a month ago)
From
Daniel Shy <danielshy@danielshy.com>
Via
Web form
Daniel Shy (a), C.C. Cheung (a), Bernard Phlips (a), Michael Streicher (b), James Mason (b), Douglas M. Groves (b), Feng Zhang (b), and Willy Kaye (b)  

(a) U.S. Naval Research Laboratory, 4555 Overlook Ave SW, Washington, DC 20375  
(b) H3D, Inc., 812 Avis Dr., Ann Arbor, MI 48108, USA 

The cadmium zinc TElluride Radiation Imager (TERI) gamma-ray telescope [1], operating on the International Space Station, reports the detection of GRB 251016A, which was also detected by SVOM/ECLAIRs (GCN 42308, 42374), Fermi/GBM (GCN 42309, 42365), Glowbug (GCN 42313), CALET (GCN 42321), AstroSat/CZTI (GCN 42327), Insight-HXMT/HE (GCN 42359), and Konus-Wind (GCN 42473). 

Using 1 Hz binning, at 2025-10-16T14:59:20.0 we observe a single peak with an excess count rate of roughly 34 counts per second (cps) above the 32 cps baseline rate observed in nearby off-source intervals.  

The analysis results presented here are preliminary and currently lack a detailed response function. 

TERI is an Office of Naval Research funded technology demonstrator for large-volume pixelated CdZnTe detectors developed, built, and operated by the U.S. Naval Research Laboratory (NRL) in conjunction with H3D, Inc. The pixelated CdZnTe detectors have an energy range of 40 keV to 3 MeV per pixel. It was launched on 2025 April 21 aboard the Department of Defense Space Test Program’s STP-H10 to the ISS. On the ISS, it is located on the SOX external payload facility on the Columbus module. Analysis of TERI data at NRL is supported under contract with NASA as correlative science for the Fermi Gamma-ray Space Telescope. 

[1] Shy, Daniel, et al. "Development of the cadmium zinc TElluride Radiation Imager." Journal of Astronomical Telescopes, Instruments, and Systems 10.4 (2024): 044009-044009 (arXiv:2408.04559). 
  
Distribution Statement A: Approved for public release.  Distribution is unlimited.

GCN Circular 42473

Subject
Konus-Wind detection of GRB 251016A (short/hard)
Date
2025-10-27T12:47:24Z (a month ago)
From
Valentina Panteleeva at Ioffe Institute <panteleevav228@gmail.com>
Via
Web form
V. Panteleeva, D. Frederiks, A. Lysenko, A. Ridnaia, D. Svinkin,
A. Tsvetkova,  M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:

The short-duration GRB 251016A
(SVOM/ECLAIRs detection: Basa et al., GCN 42308;
Brunet et al., GCN 42374;
Fermi-GBM detection: The Fermi GBM team, GCN 42309;
Smith and Meegan, GCN 42365;
Glowbug detection: Woolf et al., GCN 42313;
CALET-GBM detection: Kawakubo et al., GCN 42321;
AstroSat-CZTI detection: Arya et al., GCN 42327;
Insight-HXMT/HE detection: Zao et al., GCN 42359)
triggered Konus-Wind at T0=53956.564 s UT (14:59:16.564).

The burst light curve shows a single pulse
which starts at ~T0-0.2 s and has a total duration of ~0.5 s.
The emission is seen up to ~3 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB251016_T53956/

As observed by Konus-Wind, the burst
had the total fluence of 6.32(-0.91,+1.04)x10^-6 erg/cm2,
and the 16-ms peak flux, measured from T0+0.018 s,
of 2.46(-0.52,+0.58)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.44(-0.20,+0.35),
the high energy photon index beta = -2.14(-0.72,+0.34),
the peak energy Ep = 825(-282,+293) keV
(chi2 = 30/25 dof).

All the quoted errors are at the 68% confidence level.
All the quoted values are preliminary.

GCN Circular 42374

Subject
GRB 251016A: SVOM/ECLAIRs refined analysis
Date
2025-10-21T11:52:34Z (2 months ago)
Edited On
2025-11-03T15:44:39Z (a month ago)
From
SVOM_group <svomgroup@bao.ac.cn>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of SVOM_group <svomgroup@bao.ac.cn>
Via
Web form
M. Brunet, O. Godet, S. Guillot (IRAP), B. Hubert (CEA), S.Basa, S.Boissier (LAM)

Using the event-by-event data downloaded through the X-band ground station, we report further analysis of ECLAIRs observations of GRB 251016A (SVOM burst-id sb25101602, GCN 42308) detected at T0 = 2025-10-16T14:59:20, which was also detected by SVOM/GRM, Fermi/GBM (GCN 42309), CALET/GBM (GCN 42321), Glowbug (GCN 42313), AstroSat/CZTI (GCN 42327) and HXMT/HE (GCN 42359).

The burst that triggered ECLAIRs consists of a single short peak, with a duration of T90 = 0.69 +0.09/-0.19 s in the 4-120 keV energy band.

The time-averaged spectrum from the peak (T0-0.4 s to T0+0.4 s) in the 5-120 keV energy range is well fitted by a power-law model with a photon index of 1.00 +/-0.16, which is consistent with the results found by Smith at al. 2025 (GCN 42365). With this model, the total 4-120 keV fluence is (3.01 +0.27/-0.94) e-07 erg/cm^2 .

All the quoted errors are at the 68% confidence level.

The Space-based multi-band astronomical 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 CNES, CEA-IRFU, CNRS-IRAP, CNRS-APC.
The SVOM/ECLAIRs point of contact for this burst is: Marius Brunet (IRAP) (marius.brunet at irap.omp.eu).

GCN Circular 42365

Subject
GRB 251016A: Fermi GBM Observation
Date
2025-10-18T23:23:26Z (2 months ago)
From
Jacob Smith at Fermi-GBM Team <jrs0118@uah.edu>
Via
Web form
Jacob Smith (UAH) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:

"At 14:59:19.76 UT on 16 October 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 251016A (trigger 782319564/251016625),
which is was detected by SVOM/ECLAIRs (Basa et al., GCN 42308), CALET-GBM (Kawakubo et al., GCN 42321), Glowbug (Woolf et al., GCN 42313) and Astro Sat CZTI (Arya et al., GCN 42327).
The Fermi GBM on-ground location is consistent with the SVOM/ECLAIRs position.

The angle from the Fermi LAT boresight is 42 degrees.

The GBM light curve consists of a single emission episode with a duration (T90)
of about 0.32 s (50-300 keV). The time-averaged spectrum
from T0-0.1 to T0+0.4 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.83 +/- 0.04 and the cutoff energy,
parameterized as Epeak, is 1317 +/- 145 keV.

The event fluence (10-1000 keV) in this time interval is
(3 +/- 0.08)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.13 s in the 10-1000 keV band is 34 +/- 2 ph/s/cm^2.

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 42359

Subject
GRB 251016A: HXMT/HE detection
Date
2025-10-18T16:40:50Z (2 months ago)
From
xueyuan zao <zaoxueyuan@gmail.com>
Via
Web form
Xue-Yuan Zao, Chen-Wei Wang, Zheng-Hang Yu, Cheng-Kui Li, Shao-Lin Xiong, and Chao Zheng report on behalf of the Insight-HXMT team:

At 2025-10-16T14:59:19.750 (T0), Insight-HXMT/HE detected the short burst GRB 251016A, which is also detected by SVOM/ECLAIRs (Basa et al., GCN 42308), FERMI-GBM (Fermi GBM team, GCN 42309), CALET-GBM (Kawakubo et al., GCN 42321), Glowbug (Woolf et al., GCN 42313) and Astro Sat CZTI (Arya et al., GCN 42327). 

The Insight-HXMT/HE light curve mainly consists of a single pulse with a T90 of 0.34 +/-0.06 s. The total counts from this burst is 2297 counts.  

The HXMT/HE light curve can be found here: 
https://www.bursthub.cn//admin/static/hxmtgrb251016A.png  

All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 30-1000 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope.   

Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org.

GCN Circular 42356

Subject
GRB 251016A: Swift-XRT afterglow detection
Date
2025-10-18T13:49:20Z (2 months ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi 
(INAF-IASFPA) , S. Lanava (PSU), S. Dichiara (PSU), J.A. Kennea (PSU),
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore
(U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of GRB 251016A. We
searched for X-ray sources in  3.5 ks of Photon Counting (PC) mode
data. The total exposure at the position of the afterglow (see below)
is 5.6 ks, obtained between T0+6.6 ks and T0+107.3 ks.

Thirty-two uncatalogued X-ray sources are detected, of which one
("Source 1") is fading with >3-sigma significance, and is therefore
likely the GRB afterglow. Using 1190 s of PC mode data and 2 UVOT
images, we find an enhanced XRT position (using the XRT-UVOT alignment
and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
266.30279, -39.56008 which is equivalent to:

RA (J2000): 17h 45m 12.67s
Dec(J2000): -39d 33' 36.3"

with an uncertainty of 3.2 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=4.53 (+0.08, -3.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.4 (+1.0, -0.6). The
best-fitting absorption column is  4.8 (+8.8, -0.9) x 10^21 cm^-2,
consistent with the Galactic value of 3.9 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 6.4 x 10^-11 (8.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     4.8 (+8.8, -0.9) x 10^21 cm^-2
Galactic foreground: 3.9 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:	     1.4 (+1.0, -0.6)

The results of the XRT-team automatic analysis are available at
https://www.swift.ac.uk/xrt_products/03000141.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/SVOM/SVOM_FIELD00042.

This circular is an official product of the Swift-XRT team.

GCN Circular 42354

Subject
GRB 251016A: Swift/UVOT Detection
Date
2025-10-18T12:05:09Z (2 months ago)
From
s.shilling@lancaster.ac.uk
Via
Web form
S.P.R. Shilling (Lancaster U.) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 251016A,
detected by SVOM/ECLAIRs (Basa et al., GCN Circ. 42308) and Fermi/GBM
(Fermi GBM team, GCN Circ. 42309), 6.66 ks after the SVOM/ECLAIRs trigger.

A source is detected in the optical by the Swift/UVOT at a position that is
consistent with the likely X-ray counterpart detected by the Swift/XRT
(Source 1: Evans et al., GCN Circ. 42311). 

Preliminary detections and upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the images are:

Filter         T_start(ks)   T_stop(ks)      Exp(s)            Mag

u	       6.66	     12.6	     491.7	       19.13 +/- 0.26
b	       6.91	     12.7	     296.0	       18.70 +/- 0.18
v	       7.42	     7.67	     245.8	       17.52 +/- 0.15
w1	       12.1	     12.4	     245.8	       >18.93
w2	       7.17	     7.42	     245.8	       >19.05
m2	       7.68	     7.85	     168.3	       >18.66

The magnitudes reported here are not corrected for Galactic extinction.

GCN Circular 42349

Subject
GRB 251016A: VLT/FORS2 Optical Observation
Date
2025-10-18T09:53:25Z (2 months ago)
From
Roberto Ricci at INAF-IRA <ricci@ira.inaf.it>
Via
Web form
Roberto Ricci (U Rome), Niccolo Passaleva ( U Rome) and Eleonora Troja (U Rome) report:

We observed the field of the short duration GRB 251016A detected by SVOM/ECLAIRs (Basa et al., GCN 42308), FERMI-GBM (Fermi GBM team, GCN 42309), CALET-GBM (Kawakubo et al., GCN 42321), Glowbug (Woolf et al., GCN 42313) and Astro Sat CZTI (Arya et al., GCN 42327) with the FORS2 imager on the ESO VLT UT1 (Antu). Observations started on Oct 16th, 2025 at 23:45 UT (~9 hours after the SVOM trigger) and were carried out in the I_BESS filter with an average airmass of ~1.3. 

The GRB lies within a very crowded region at low Galactic latitude. Several optical sources are detected within the localization of Swift/XRT Source #1 (Evans et al., GCN 42311).  Objects brighter than 24 AB mag have counterparts in the GAIA DR3 catalogue (Babusiaux et al., 2023), however several fainter (>24 AB mag) sources remain unmatched. 

Further observations are planned  to determine variability.           

We thank the staff at the VLT for the rapid execution of these observations.

GCN Circular 42327

Subject
GRB 251016A: AstroSat CZTI detection of a short burst
Date
2025-10-17T13:05:35Z (2 months ago)
From
Anuraag Arya at IIT Bombay <aryaanuraag910@gmail.com>
Via
Web form
A. Goyal (IITB), A. Arya (IITB), S. Salunke (IUCAA), M. Tembhurnikar (IUCAA), Harsha K. H. (IUCAA), G. Waratkar (Caltech/IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a short-duration GRB 251016A which was also detected by SVOM/ECLAIRs (Basa et al., GCN Circ. 42308), Fermi GBM (Fermi GBM Team, GCN Circ. 42309), Glowbug (Woolf et al., GCN Circ. 42313) and CALET GBM (Kawakubo et al., GCN Circ. 42321).

The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2025-10-16 14:59:16.90 UTC. The measured peak count rate associated with the burst is 1142 (+782, -64) counts/s above the background in the combined data of all four quadrants, with a total of 140 (+39, -30) counts. The local mean background count rate was 264 (+14, -45) counts/s. Using cumulative rates, we measure a T90 of 0.31 (+0.04, -0.08) s. 

The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2025-10-16 14:59:16.68 UTC. The measured peak count rate associated with the burst is 1099 (+76, -82) counts/s above the background in the combined data of all quadrants, with a total of 1056 (+117, -126) counts. The local mean background count rate was 1232 (+9, -10) counts/s. Due to the intrinsic 1 s binning of veto data, we cannot reliably estimate a T90 from it.

CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.

CZTI GRB detections are reported regularly on the payload site at:
http://astrosat.iucaa.in/czti/?q=grb

GCN Circular 42321

Subject
GRB 251016A: CALET Gamma-Ray Burst Monitor detection
Date
2025-10-17T07:26:43Z (2 months ago)
From
Yuta Kawakubo at Aoyama Gakuin University <kawakubo@phys.aoyama.ac.jp>
Via
Web form
Y. Kawakubo , A. Yoshida, T. Sakamoto, S. Sugita (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii,
Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The short GRB 251016A (SVOM detection: Basa et al., GCN Circ. 42308;
Fermi GBM Final Localization: Fermi GBM team, GCN Circ. 42309; Glowbug
gamma-ray detection: Woolf et al., GCN Circ. 42313) triggered the 
CALET Gamma-ray Burst Monitor (CGBM) at 14:59:19.37 UTC on 16 October 2025
(https://cgbm.calet.jp/cgbm_trigger/flight/1444661491/index.html).
The burst signal was seen by all CGBM detectors. 

The burst light curve shows a short pulse that starts
at T+0.32 sec, peaks at T+0.51 sec, and ends at T+0.69 sec.
The T90 and T50 durations measured by the SGM data are 0.29 +/- 0.05 sec
and 0.10+/- 0.03 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

https://cgbm.calet.jp/cgbm_trigger/ground/1444661491/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at Waseda University.

GCN Circular 42314

Subject
GRB 251016A: BOOTES-6/DPRT optical upper limit
Date
2025-10-16T21:13:12Z (2 months ago)
From
I. Perez-Garcia at Institute of Astrophysics of Andalusia <ipg@iaa.es>
Via
Web form

I. Perez-Garcia, E. Fernandez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez, S.-Y. Wu, S. Guziy and A. J. Castro-Tirado (IAA-CSIC, Granada), P. J. Meintjes and H. J. van Heerden (UFS, South Africa), A. Martin-Carrillo and L. Hanlon (UCD, Ireland), M. Gritsevich (Univ. of Helsinki), M. Jelinek (ASU-CAS), A. Kumar (ARIES) and C. J. Perez del Pulgar (UMA, Malaga), on behalf of a larger collaboration, report:

Following the detection of GRB 251016A by Fermi/GBM (Smith et al., GCN 42309

Loading...
 
 
) and SVOM/ECLAIRs (Basa et al., GCN 42308), the BOOTES-6/DPRT 0.6m robotic telescope at Boyden Observatory in Maselspoort (South Africa) responded to this event starting on Oct 16, 17:35 UT (~ 2.6 h after trigger) with 60s images. No new source is detected within the Swift/XRT X-ray afterglow Source 1 position (Evans et al., GCN 42311) up to magnitude 17.14 using Gaia DR3 Gmag magnitude as reference on our first image. Further images were gathered and using ATLAS REFCAT2 as reference (Tonry et al. 2018) we get an upper limit of:

UT mid exposureMag limitFilterExp time (sec)
2025-10-16 18:05:0719.3clear60x7
2025-10-16 18:37:0717.6Z60x4
2025-10-16 18:43:0219.1g60x4
2025-10-16 19:05:3018.7r60x3
2025-10-16 19:10:3818.3i60x4

We thank the staff at Boyden Observatory for their excellent support.

GCN Circular 42313

Subject
GRB 251016A: Glowbug gamma-ray detection of a short burst
Date
2025-10-16T21:06:59Z (2 months ago)
From
richard.s.woolf.civ@us.navy.mil
Via
Web form
R. Woolf,  C.C. Cheung, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:
 
The Glowbug gamma-ray telescope [1,2,3], operating on the International Space Station, reports the detection of GRB 251016A, which was also detected by SVOM/ECLAIRs (GCN 42308), Fermi/GBM (GCN 42309), and CALET (Trigger 1444661491).
 
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2025-10-16 14:59:18.560 with a duration of 0.64 s and a total significance of about 76 sigma. The light curve comprises a single peak.
 
The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.
 
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC.  It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS, and operated until 2024 April when it was put in safe storage on orbit. Glowbug was removed from storage and resumed operation on 2025 September 12.
 
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Woolf, R.S. et al. 2024, Proc. SPIE, 13151, id. 1315108
 
Distribution Statement A: Approved for public release.  Distribution is unlimited.

GCN Circular 42310

Subject
Fermi GRB 251016A: Global MASTER-Net observations report
Date
2025-10-16T19:00:45Z (2 months ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
email
V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, 
G.Antipov,  A.Sankovich, Yu.Tselik, 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.Sosnovskij (CrAO),
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-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 251016A ( Fermi GBM team, GCN 42309) errorbox  9753 sec after notice time and 9784 sec after trigger time at 2025-10-16 17:42:24 UT, with upper limit up to  16.8 mag. Observations started at twilight.  The observations began at zenith distance = 38 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = -12 deg., longitude l = 344 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=3016116

We obtain a following upper limits.  

Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________

    9814 | 2025-10-16 17:42:24 |         MASTER-SAAO | (17h 41m 59.48s , -48d 04m 09.1s) |   C |    60 | 14.4 |        
    9814 | 2025-10-16 17:42:24 |         MASTER-SAAO | (17h 44m 44.95s , -48d 19m 26.1s) |   C |    60 | 16.5 |        
    9909 | 2025-10-16 17:43:58 |         MASTER-SAAO | (17h 39m 01.22s , -50d 11m 14.5s) |   C |    60 | 16.8 |        
    9909 | 2025-10-16 17:43:58 |         MASTER-SAAO | (17h 36m 07.40s , -49d 55m 40.2s) |   C |    60 | 15.2 |        
   10004 | 2025-10-16 17:45:33 |         MASTER-SAAO | (17h 48m 32.79s , -46d 10m 37.6s) |   C |    60 | 14.6 |        
   10004 | 2025-10-16 17:45:33 |         MASTER-SAAO | (17h 51m 12.71s , -46d 25m 54.6s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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GCN Circular 42309

Subject
GRB 251016A: Fermi GBM Final Localization
Date
2025-10-16T15:46:56Z (2 months ago)
From
Jacob Smith at Fermi-GBM Team <jrs0118@uah.edu>
Via
Web form
The Fermi GBM team reports the detection of a likely SHORT GRB

"At 14:59:19.76 UT on 16 October 2025, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 251016A (trigger 782319564/251016625).

The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 268.93, Dec = -48.82 (J2000 degrees, equivalent to J2000 17h 55m, -48d 49'),
with a statistical uncertainty of 3.55 degrees.

The angle from the Fermi LAT boresight is 33 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251016625/quicklook/glg_skymap_all_bn251016625.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251016625/quicklook/glg_healpix_all_bn251016625.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251016625/quicklook/glg_lc_medres34_bn251016625.gif"

GCN Circular 42308

Subject
GRB 251016A: SVOM detection of a short burst
Date
2025-10-16T15:30:00Z (2 months ago)
From
SVOM_group <svomgroup@bao.ac.cn>
Via
Web form
S. Basa, S. Boissier (LAM), O. Godet, S. Guillot (IRAP), D. Turpin (CEA)

At 2025-10-16T14:59:20 UTC (T0), SVOM/ECLAIRs triggered and located the gamma-ray burst GRB 251016A (SVOM burst-id sb25101602).

The following trigger information was received on the ground with low latency by the SVOM VHF Alert Network.

The burst was only detected by the Count-Rate Trigger (CRT), which produced a sequence of 5 alerts. CRT provided the alert with the best signal-to-noise-ratio in the image (SNR) of 8.16 in the [8-120] keV energy band over a time window of 0.60 seconds starting at 2025-10-16T14:59:19.

The localization of the best alert is R.A., Dec. 266.207, -39.577 degrees:
R.A. (J2000) = 17h44m49.58s
Dec. (J2000) = -39d34m35.95s
 with a 90% confidence level (C.L.) radius of 9.64 arcmin (including systematic error of 2 arcmin added in quadrature).

The SVOM/ECLAIRs light curve showed a single and narrow peak.

This burst also triggered SVOM/GRM at 2025-10-16T14:59:19 on a timescale of 0.10 seconds with an SNR of 37.30.

This burst seems to have been detected by Fermi, but with a declination of about 10 degrees offset.

The satellite did not slew due to Sun constraint. No X-ray observation could be performed by SVOM/MXT for the time being. No optical observation could be performed by SVOM/VT for the time being.

The Space-based multi-band astronomical 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. SVOM/ECLAIRs was developed jointly by CNES, CEA-IRFU, CNRS-IRAP, CNRS-APC. SVOM/GRM was developed by the Institute of High Energy Physics (IHEP) of CAS. SVOM/MXT was developed jointly by CNES, CEA-IRFU, CNRS-IJCLab, University of Leicester, MPE.

The Burst Advocate (BA) on shift for this alert is Stephane Basa: stephane.basa@lam.fr.
Please contact the BA by email if you require additional information.
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