GRB 251106A
GCN Circular 42635
Subject
GRB 251106A: Swift/UVOT Upper Limits
Date
2025-11-10T15:56:36Z (2 months ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
Via
Web form
M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 251106A 4.1 ks after the SVOM/ECLAIRs trigger (Antier et al., GCN Circ. 42605). We do not detect any afterglow consistent with the XRT position (D'Ai et al., GCN Circ. 42611) or optical position (Angulo et al., GCN Circ. 42607).
Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
u 4066 9896 1987 >20.56
u 199146 273340 4837 >21.08
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.016 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 42613
Subject
GRB 251106A: SVOM/COLIBRÍ (FM-GFT) fading of the optical counterpart
Date
2025-11-07T14:32:43Z (2 months ago)
From
F. Fortin at IRAP <ffortin.sci.edu@gmail.com>
Via
Web form
Francis Fortin (IRAP), Camila Angulo (UNAM), Jean-Luc Atteia (IRAP), Benjamin Schneider (LAM), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Dalya Akl (NYUAD), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Kin Ocelotl López (UNAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), and Antonio de Ugarte Postigo (LAM) report:
We imaged the field of the SVOM GRB 251106A (Antier et al., GCN Circ. 42605) using the DDRAGO wide-field imager on the SVOM/COLIBRÍ (FM-GFT) telescope. We observed a second epoch from 2025-11-07 12:34 to 12:50 UTC (from 16.63 to 16.89 hours after the trigger) and obtained an additional 16 minutes of exposure in the r filter at high airmass (3 to 3.5).
The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and is not corrected for Galactic extinction.
We detect the optical counterpart we previously reported (Angulo et al, GCN Circ. 42607) at the following preliminary magnitude:
r = 21.85 +/- 0.13
Our photometry shows clear fading with respect to our earlier epoch, confirming that this is the optical counterpart of the GRB.
We note that the position of the afterglow optical counterpart is coincident with a faint source in the Legacy Survey (Dey et al. 2019) at r = 22.56 +/- 0.17, which could be the host galaxy of the GRB.
We thank the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams.
COLIBRÍ is an astronomical observatory developed and operated jointly by France (AMU, CNES and CNRS) and Mexico (UNAM and SECIHTI). It is located at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, Baja California, Mexico.
GCN Circular 42611
Subject
GRB 251106A: Swift-XRT afterglow detection
Date
2025-11-07T10:12:12Z (2 months ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
A. D'Ai (INAF-IASFPA), S. Campana (INAF-OAB), J.A. Kennea (PSU), D.N.
Burrows (PSU), S. Lanava (PSU), A.P. Beardmore (U. Leicester), J.P.
Osborne (U. Leicester), A. Melandri (INAF-OAR) and P.A. Evans (U.
Leicester) reports on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of GRB 251106A. We
searched for X-ray sources in 2.0 ks of Photon Counting (PC) mode
data. The total exposure at the position of the afterglow (see below)
is 2.0 ks, obtained between T0+4.0 ks and T0+9.9 ks.
Three uncatalogued X-ray sources are detected, of which one ("Source
1") is above the RASS 3-sigma upper limit at this position, and is
therefore likely the GRB afterglow. Using 2020 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 = 234.46260, +63.36779 which is equivalent to:
RA (J2000): 15h 37m 51.02s
Dec(J2000): +63d 22' 04.0"
with an uncertainty of 2.6 arcsec (radius, 90% confidence). This
position is consistent with the optical afterglow candidate identified
by Angulo et al. (GCN 42607).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.87 (+0.33, -0.29).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.96 (+0.23, -0.22). The
best-fitting absorption column is 1.1 (+0.6, -0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.7 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.2 x 10^-11 (3.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.1 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index: 1.96 (+0.23, -0.22)
If the light curve continues to decay with a power-law decay index of
0.87, the count rate at T+24 hours will be 0.038 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-12 (1.5 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
https://www.swift.ac.uk/xrt_products/03000182.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/SVOM/SVOM_FIELD00048.
This circular is an official product of the Swift-XRT team.
GCN Circular 42610
Subject
GRB 251106A: Kilonova-Catcher optical upper limit
Date
2025-11-07T08:48:49Z (2 months ago)
Edited On
2025-11-07T18:15:45Z (2 months ago)
From
Damien Turpin at CEA-Saclay <dturpin-astro@hotmail.com>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Damien Turpin at CEA-Saclay <dturpin-astro@hotmail.com>
Via
Web form
M. Freeberg (KNC), D. Turpin (CEA-Saclay/Irfu), C. Andrade(UMN), S. Antier (OCA/IJCLab), M. Coughlin (UMN), S. Karpov (FZU), P. Hello (IJCLAB), M. Pillas (IAP) on behalf of the GRANDMA/Kilonova-Catcher collaboration:
We observed the field of GRB 251106A detected by SVOM (Antier et al., GCN 42605), Swift/BAT-GUANO (Delaunay et al., GCN 42608) and Fermi/GBM subthreshold (Godwin et al., GCN 42608) with the GRANDMA citizen science project Kilonova-catcher (KNC). Our observations were performed with a TEC160FL telescope operated by M. Freeberg. Our observations started at TGRB+5.4hr and were taken with sdss gr filters.
In our stacked frames, subtracted from the PanSTARRS DR2 template image, we do not detect the optical counterpart reported by the SVOM/COLIBRI (FM-GFT) (Angulo et al., GCN 42607).
We report our follow-up results in the table below:
+---------------+-----------+---------+----------------+-------------+
| Tmid-TGRB (hr)| Exp (s) | Filter | Magnitude | Instrument |
+===============+===========+=========+================+=============+
| 5.77 | 15 x 180s | r (AB) | 19.7 (5 sigma) | TEC160FL |
| 6.58 | 15 x 180s | g (AB) | 20.0 (5 sigma) | TEC160FL |
+---------------+-----------+---------+----------------+-------------+
All the data have been reduced by a single data processing pipeline, STDPipe (Karpov et al., 2022). Images obtained with the sloan filters were calibrated using the PanSTARRS DR1 catalog.
We use the SkyPortal application (skyportal.io) to monitor our observational campaign (Coughlin et al. 2023).
GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).
GCN Circular 42609
Subject
Fermi GBM Sub-Threshold Detection of GRB 251106A
Date
2025-11-07T03:05:39Z (2 months ago)
Edited On
2025-11-07T05:48:33Z (2 months ago)
From
Matt Godwin <msg0028@uah.edu>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Matt Godwin <msg0028@uah.edu>
Via
Web form
M. Godwin (UAH) and R. Hamburg (USRA) report on behalf of the Fermi-GBM Team:
SVOM/ECLAIRs detected GRB 251106A on 2025-11-06 at 19:56:37 UTC (Antier et al. 2025, GCN 42605). There was no Fermi-GBM onboard trigger around this event time.
An automated, blind search for gamma-ray bursts below the onboard triggering threshold in Fermi-GBM identified a roughly spatially-consistent candidate at 19:58:18.89 UTC.
The GBM Targeted Search [1], the most sensitive coherent search for GRB-like signals in GBM, also identified a transient spatially consistent with GRB 251106A approximately 10 s before the SVOM trigger time. It is detected most significantly ~133 s after the SVOM trigger time on a 4.096 s timescale with a false alarm rate of 3.8e-5 Hz. The event was best-fit using a "normal" GRB spectrum (Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3). The Targeted Search localization is consistent with the SVOM/ECLAIRs location.
[1] Goldstein et al. 2019 arXiv:1903.12597
GCN Circular 42608
Subject
GRB 251106A: Swift/BAT arcminute localization of a burst
Date
2025-11-07T02:59:54Z (2 months ago)
From
Jimmy DeLaunay at Penn State <delauj2@gmail.com>
Via
Web form
James DeLaunay (PSU), Samuele Ronchini (GSSI), Aaron Tohuvavohu (Cosmic Frontier), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report:
Swift/BAT did not localize GRB 251106A onboard (T0: 2025-11-06T19:56:37 UTC, SVOM/ECLAIRS GCN 42605).
In a ground search of a 10 s event file, available due to a subthreshold trigger onboard. The GRB was detected at a S/N of 7.0 in a single 10 s, 15-150 keV image starting at ~T0 + 129 s.
The BAT position is
RA, Dec = 234.4744, +63.3387 deg which is
RA(J2000) = 15h 37m 53.9s
Dec(J2000) = +63d 20′ 19.3″
with an estimated uncertainty of 3 arcmin radius.
GCN Circular 42607
Subject
GRB 251106A: SVOM/COLIBRÍ (FM-GFT) detection of a likely optical counterpart
Date
2025-11-07T02:38:53Z (2 months ago)
From
Camila Angulo Valdez at UNAM <camiangulo@astro.unam.mx>
Via
Web form
Camila Angulo (UNAM), Francis Fortin (IRAP), Jean-Luc Atteia (IRAP), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Dalya Akl (NYUAD), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Kin Ocelotl López (UNAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), Benjamin Schneider (LAM), and Antonio de Ugarte Postigo (LAM) report:
We imaged the field of the SVOM GRB 251106A (Antier et al., GCN Circ. 42605) using the DDRAGO wide-field imager on the SVOM/COLIBRÍ (FM-GFT) telescope. We observed from 2025-11-07 01:46 to 01:52 UTC (from 5.82 to 5.93 hours after the trigger) and obtained 360 seconds of simultaneous exposure in the r and z filters.
The data were analyzed with STDWeb/STDPipe (Karpov 2025). The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and is not corrected for Galactic extinction.
We detect an uncatalogued source (revealed by image subtraction using PanSTARRS as template) consistent with the XRT 2.6 arcsec error circle (https://www.swift.ac.uk/SVOM/SVOM_FIELD00048/) at RA, DEC = 234.462239, 63.367568 (J2000) and with preliminary magnitudes of:
r = 21.49 +/- 0.10
z = 20.77 +/- 0.13
We suggest this is likely to be the optical counterpart of the GRB.
Further observations are ongoing.
We thank the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams.
COLIBRÍ is an astronomical observatory developed and operated jointly by France (AMU, CNES and CNRS) and Mexico (UNAM and SECIHTI). It is located at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, Baja California, Mexico.
GCN Circular 42606
Subject
GRB 251106A: MASTER optical observations
Date
2025-11-06T22:11:56Z (2 months ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
email
V.A. Senik, V.M. Lipunov, A.Kuznetsov, E.Gorbovskoy, G.Antipov, 1P.Balanutsa, I.Panchenko, N. Tiurina, K.Zhirkov, Ya.Kechin, A.Chasovnikov, V.Topolev, D.Vlasenko, Yu. Tselik(Lomonosov MSU, SAI, Moscow),
R. Podesta, C.Francile, F. Podesta, E. Gonzalez (OAFA, San Juan Uni.,Argentina);
D. Buckley (SAAO, South Africa),
O. Gress, N.Budnev, O.Ershova (Irkutsk State University),
A. Sosnovskij (CrAO RAS),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity),
V.M.Pillet, R.Rebolo Lopez (The Instituto de Astrofisica de Canarias, Spain),L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez,J.Martinez,A.R.Corella,L.H.Rodriguez (INAOE, Guillermo Haro Astrophysic Observatory, Mexico)
MASTER-Kislovodsk robotic telescope (Global MASTER-Net [1-4], http://observ.pereplet.ru)
located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
started inspect of SVOM GRB 251106A (Antier et al. GCN 42605, Ttrigger= 2025-11-06T19:56:37, Tnotice=2025-11-06 20:21:29.84UT) error-box observations 1550 sec after trigger time at 2025-11-06 20:22:27 UT, with upper limit up to 17.9 mag. The observations began 17deg altitude.
The sun altitude was -62.3 deg.
The galactic latitude b = 45 deg., longitude l = 98 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=3034637
There is no optical counterpart withthe following MASTER upper limits upper limits:
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
1610 | 2025-11-06 20:22:27 | MASTER-Kislovodsk | (15h 37m 28.85s,+63d 06m 03.4s) | P- | 120 | 15.6 |
1750 | 2025-11-06 20:24:47 | MASTER-Kislovodsk | (15h 37m 29.81s,+63d 05m 56.6s) | P- | 120 | 15.6 |
1750 | 2025-11-06 20:24:47 | MASTER-Kislovodsk | (15h 37m 42.69s,+63d 28m 24.2s) | P| | 120 | 17.2 |
1890 | 2025-11-06 20:27:07 | MASTER-Kislovodsk | (15h 37m 30.71s,+63d 05m 51.6s) | P- | 120 | 15.5 |
1890 | 2025-11-06 20:27:07 | MASTER-Kislovodsk | (15h 37m 43.57s,+63d 28m 18.7s) | P| | 120 | 17.3 |
2030 | 2025-11-06 20:29:27 | MASTER-Kislovodsk | (15h 37m 31.56s,+63d 05m 46.7s) | P- | 120 | 15.6 |
2030 | 2025-11-06 20:29:27 | MASTER-Kislovodsk | (15h 37m 44.37s,+63d 28m 13.8s) | P| | 120 | 17.2 |
2140 | 2025-11-06 20:31:47 | MASTER-Kislovodsk | (15h 37m 25.48s,+63d 04m 04.1s) | C | 60 | 17.0 |
2260 | 2025-11-06 20:31:47 | MASTER-Kislovodsk | (15h 37m 25.50s,+63d 04m 04.1s) | C | 300 | 17.5 | Coadd
2140 | 2025-11-06 20:31:47 | MASTER-Kislovodsk | (15h 37m 38.06s,+63d 26m 36.1s) | C | 60 | 17.4 |
2858 | 2025-11-06 20:43:45 | MASTER-Kislovodsk | (15h 36m 59.84s,+63d 06m 24.9s) | C | 60 | 17.0 |
2918 | 2025-11-06 20:43:45 | MASTER-Kislovodsk | (15h 36m 59.83s,+63d 06m 24.9s) | C | 180 | 17.8 | Coadd
2858 | 2025-11-06 20:43:45 | MASTER-Kislovodsk | (15h 37m 12.09s,+63d 29m 02.0s) | C | 60 | 17.4 |
2938 | 2025-11-06 20:45:05 | MASTER-Kislovodsk | (15h 37m 04.06s,+63d 05m 20.5s) | C | 60 | 17.1 |
2938 | 2025-11-06 20:45:05 | MASTER-Kislovodsk | (15h 37m 16.46s,+63d 27m 56.8s) | C | 60 | 17.5 |
3018 | 2025-11-06 20:46:25 | MASTER-Kislovodsk | (15h 36m 58.81s,+63d 04m 17.3s) | C | 60 | 17.0 |
3018 | 2025-11-06 20:46:25 | MASTER-Kislovodsk | (15h 37m 11.34s,+63d 26m 52.9s) | C | 60 | 17.4 |
3128 | 2025-11-06 20:47:45 | MASTER-Kislovodsk | (15h 37m 04.62s,+63d 04m 30.1s) | C | 120 | 17.3 |
3128 | 2025-11-06 20:47:45 | MASTER-Kislovodsk | (15h 37m 17.42s,+63d 27m 05.1s) | C | 120 | 17.4 |
3289 | 2025-11-06 20:50:26 | MASTER-Kislovodsk | (15h 37m 04.51s,+63d 05m 55.6s) | C | 120 | 17.3 |
3289 | 2025-11-06 20:50:26 | MASTER-Kislovodsk | (15h 37m 17.54s,+63d 28m 30.4s) | C | 120 | 17.5 |
3429 | 2025-11-06 20:52:46 | MASTER-Kislovodsk | (15h 37m 05.48s,+63d 04m 10.8s) | C | 120 | 17.2 |
3549 | 2025-11-06 20:52:46 | MASTER-Kislovodsk | (15h 37m 05.48s,+63d 04m 10.8s) | C | 360 | 17.9 | Coadd
3429 | 2025-11-06 20:52:46 | MASTER-Kislovodsk | (15h 37m 18.70s,+63d 26m 45.1s) | C | 120 | 17.5 |
3569 | 2025-11-06 20:55:05 | MASTER-Kislovodsk | (15h 37m 07.60s,+63d 05m 54.6s) | C | 120 | 17.2 |
3569 | 2025-11-06 20:55:05 | MASTER-Kislovodsk | (15h 37m 20.97s,+63d 28m 28.6s) | C | 120 | 17.4 |
3709 | 2025-11-06 20:57:25 | MASTER-Kislovodsk | (15h 37m 04.73s,+63d 05m 01.2s) | C | 120 | 17.2 |
3709 | 2025-11-06 20:57:26 | MASTER-Kislovodsk | (15h 37m 18.15s,+63d 27m 35.0s) | C | 120 | 17.4 |
3849 | 2025-11-06 20:59:45 | MASTER-Kislovodsk | (15h 37m 04.57s,+63d 05m 58.7s) | C | 120 | 17.1 |
3909 | 2025-11-06 20:59:45 | MASTER-Kislovodsk | (15h 37m 04.57s,+63d 05m 58.8s) | C | 240 | 17.5 | Coadd
3849 | 2025-11-06 20:59:45 | MASTER-Kislovodsk | (15h 37m 18.12s,+63d 28m 32.3s) | C | 120 | 17.4 |
3959 | 2025-11-06 21:02:05 | MASTER-Kislovodsk | (15h 37m 10.31s,+63d 04m 57.0s) | C | 60 | 16.8 |
3959 | 2025-11-06 21:02:05 | MASTER-Kislovodsk | (15h 37m 23.89s,+63d 27m 30.6s) | C | 60 | 17.2 |
4039 | 2025-11-06 21:03:25 | MASTER-Kislovodsk | (15h 37m 05.87s,+63d 03m 55.5s) | C | 60 | 16.8 |
4039 | 2025-11-06 21:03:25 | MASTER-Kislovodsk | (15h 37m 19.52s,+63d 26m 29.2s) | C | 60 | 17.2 |
4118 | 2025-11-06 21:04:45 | MASTER-Kislovodsk | (15h 37m 13.13s,+63d 04m 18.9s) | C | 60 | 16.8 |
4178 | 2025-11-06 21:04:45 | MASTER-Kislovodsk | (15h 37m 13.12s,+63d 04m 18.9s) | C | 180 | 17.3 | Coadd
4118 | 2025-11-06 21:04:45 | MASTER-Kislovodsk | (15h 37m 26.81s,+63d 26m 52.7s) | C | 60 | 17.1 |
Observations and data analysis will be continued.
[1] Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L
[2] Lipunov et al. 2022, Universe, Vol. 8(5), id.271
[3] Lipunov et a. 2019, ARep, vol.63, 293
[4] Lipunov V., Kornilov V., Gorbovskoy E., Tiurina N., Kuznetsov A. 2023,
Astronomical Robotic Networks and Operative Multichanel Astrophysics,Lomonosov MSU PRESS, 591pp.
http://www.pereplet.ru/lipunov/625.html#625
GCN Circular 42605
Subject
GRB 251106A: SVOM detection of a burst
Date
2025-11-06T20:37:09Z (2 months ago)
From
SVOM_group <svomgroup@bao.ac.cn>
Via
Web form
S. Antier (IJCLAB), M. Dennefeld (IAP), S. Schanne (CEA/Irfu), F. Lacreu (IAP) report on behalf of the SVOM mission team:
At 2025-11-06T19:56:37 UTC (T0), SVOM/ECLAIRs triggered and located the gamma-ray burst GRB 251106A (SVOM burst-id sb25110604).
The following trigger information was received on the ground with low latency by the SVOM VHF Alert Network.
The burst was detected both by the Count-Rate Trigger (CRT) and the Image Trigger (IMT), which produced a sequence of 16 alerts. IMT provided the alert with the best signal-to-noise-ratio in the image (SNR) of 11.02 in the [8-120] keV energy band over a time window of 163.84 seconds starting at 2025-11-06T19:55:40.
The localization of the best alert is R.A., Dec. 234.6169, 63.3716 degrees:
R.A. (J2000) = 15h38m28.05s
Dec. (J2000) = 63d22m17.83s
with a 90% confidence level (C.L.) radius of 7.27 arcmin (including systematic error of 2 arcmin added in quadrature).
Due to sun constraints, no immediate slew was performed on this burst.
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 Sarah Antier: sarah.antier@ijclab.in2p3.fr.
Please contact the BA by email if you require additional information.