GRB 260212A
GCN Circular 43772
Subject
Konus-Wind detection of GRB 260212A
Date
2026-02-17T14:55:21Z (7 months ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
Via
email
D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin,
A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The long-duration GRB 260212A (Fermi-GBM detection:
The Fermi GBM team, GCN 43716; Neights and Meegan GCN 43740;
Glowbug detection: Cheung et al., GCN 43719;
SVOM-GRM detection: Zhang et al., GCN 43727;
GECAM-B detection: Zhang et al., GCN 43736;
AstroSat-CZTI detection: Salunke et al., GCN 43741;
IPN triangulation: Kozyrev et al., GCN 43769)
triggered Konus-Wind (KW) at T0=64149.637 s UT (17:49:09.637).
The burst light curve shows multiple emission pulses
in the interval from ~T0-0.5 s to ~T0+11 s.
The emission is seen up to ~2 MeV.
We also note a much weaker emission bump around T0+25 s,
which is visible only below 80 keV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB260212_T64149/
As observed by Konus-Wind, the burst had
the fluence of (6.81 ± 0.55)x10^-6 erg/cm^2 and
the 64-ms peak energy flux, measured from T0 + 0.640 s,
of (4.98 ± 0.40)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum of the burst (measured from T0 to T0+16.640 s)
is best fitted in the 20 keV - 15 MeV range by a power law with exponential
cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.16 (-0.10, + 0.10) and Ep = 115(-7,+9) keV, chi^2 = 97/93 dof.
Fitting this spectrum by a Band GRB function yields the same values
of alpha and Ep, and only an upper limit on the high energy photon
index beta of -2.7
The spectrum near the peak count rate (measured from T0 to T0+8.448 s)
is best fitted in the 20 keV - 15 MeV range by a CPL model
with alpha = -0.86 (-0.11, + 0.12)and Ep = 108(-8,+10) keV, chi^2 = 94/78 dof.
Fitting this spectrum by a Band function yields the same values
of alpha and Ep, and only an upper limit on the high energy photon
index beta of -3.2
All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary
GCN Circular 43769
Subject
IPN triangulation of GRB 260212A
Date
2026-02-17T12:10:47Z (7 months ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
Web form
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the HEND/Mars Odyssey team,
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,
and T. Cline on behalf of the Konus-Wind team,
A. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi-GBM team,
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, A. Tohuvavohu,
and J. DeLaunay on behalf of the Swift-BAT team,
and
W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr,
and A.S. Gardner on on behalf of the GRS-Odyssey GRB team,
report:
The long-duration GRB 260212A
(Ferm-GBM detection: The Fermi GBM team, GCN 43716;
Neights and Meegan GCN 43740;
Glowbug detection: Cheung et al., GCN 43719;
SVOM-GRM detection: Zhang et al., GCN 43727;
GECAM-B detection: Zhang et al., GCN 43736;
AstroSat-CZTI detection: Salunke et al., GCN 43741)
was detected by Fermi (GBM trigger 792611353), Swift (BAT),
Konus-Wind, Glowbug, SVOM (GRM), GECAM-B, Astrosat (CZTI),
and Mars-Odyssey (HEND) at about 64148 s UT (17:49:08)
The burst was outside the coded field of view of the BAT.
We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
224.837 (14h 59m 21s) +74.800 (+74d 47' 59")
Corners:
225.022 (15h 00m 05s) +76.212 (+76d 12' 45")
224.790 (14h 59m 09s) +73.505 (+73d 30' 18")
224.644 (14h 58m 35s) +73.384 (+73d 23' 04")
224.855 (14h 59m 25s) +76.092 (+76d 05' 30")
---------------------------------------------
The error box area is 372 sq. arcmin, and its maximum
dimension is 2.830 deg (the minimum one is 2.3 arcmin).
The Sun distance was 106 deg.
This localization may be improved.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB260212_T64149/IPN/
The HEALPix triangulation map is the multi-order HEALPix in units of
probability density.
The Konus-Wind time history and spectrum will be given
in a forthcoming GCN circular.
GCN Circular 43741
Subject
GRB 260212A: AstroSat CZTI detection
Date
2026-02-14T21:38:15Z (7 months ago)
Edited On
2026-02-15T01:37:49Z (7 months ago)
From
Anuraag Arya at IIT Bombay <aryaanuraag910@gmail.com>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Anuraag Arya at IIT Bombay <aryaanuraag910@gmail.com>
Via
Web form
S. Salunke (IUCAA), Harsha K. H. (IUCAA), M. Tembhurnikar (IUCAA), U. Pathak (IITB), A. Arya (IITB), A. Goyal (IITB), 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 long GRB 260212A which was also detected by Fermi GBM (Fermi GBM Team, GCN Circ. 43716), and Glowbug (Cheung et. al., GCN Circ. 43719).
The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-12 17:49:08.04 UTC. The measured peak count rate associated with the burst is 641 (+72, -52) counts/s above the background in the combined data of all quadrants, with a total of 1727 (+302, -376) counts. The local mean background count rate was 1247 (+6, -7) counts/s. We measure a T90 of 9.7 (+1.9, -0.5) s from the cumulative Veto light curve.
The source was also faintly detected in the CZT detectors in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-12 17:49:08.50 UTC. The measured peak count rate associated with the burst is 44 (+28, -5) counts/s above the background in the combined data of two quadrants (out of four), with a total of 144 (+111, -95) counts. The local mean background count rate was 130 (+1, -2) counts/s. Due to poor statistics, we cannot reliably estimate the 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 43740
Subject
GRB 260212A: Fermi GBM Observation
Date
2026-02-14T20:29:37Z (7 months ago)
From
eliza.neights@gmail.com
Via
Web form
Eliza Neights (GWU, NASA GSFC) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 17:49:08.21 UT on 12 February 2026, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 260212A (trigger 792611353/260212742),
which was also detected by Glowbug (Cheung et al. 2026, GCN 43719),
SVOM/GRM (Zhang et al. 2026, GCN 43727), and GECAM-B (Zhang et al. 2026, GCN 43736).
The angle from the Fermi LAT boresight is 127 degrees.
The GBM light curve consists of multiple emission episodes with a duration (T90)
of about 9.7 s (50-300 keV). The time-averaged spectrum
from T0-1.5 to T0+14.5 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.66 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 107 +/- 1 keV.
The event fluence (10-1000 keV) in this time interval is
(7.1 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+8.7 s in the 10-1000 keV band is 16.2 +/- 0.6 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 90 +/- 1 keV, alpha = -0.43 +/- 0.02 and beta = -2.52 +/- 0.04.
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 43736
Subject
GRB 260212A: GECAM-B observation
Date
2026-02-14T13:54:35Z (7 months ago)
From
zhangjinpeng@ihep.ac.cn
Via
Web form
Jin-Peng Zhang, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team:
GECAM-B was triggered in-flight by GRB 260212A, at 2026-02-12T17:49:07.800 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43716), Glowbug (C.C. Cheung et al., GCN #43719) and SVOM/GRM (Jin-Peng Zhang et al., GCN #43727).
According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of multiple pulses, with a duration (T90) of 24 +/- 7 s.
The GECAM-B light curve can be found here:
https://www.bursthub.cn//admin/static/gecambgrb260212A.png
The time-averaged spectrum from T0 - 1.0 to T0 + 11.0 s (photon energy > 70 keV) is fitted by a power law function. The power law index is -2.53 +0.14/-0.15. The event fluence (10-1000 keV) in this time interval is (1.07 +0.09/-0.13)E-05 erg/cm^2.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS).
GCN Circular 43727
Subject
GRB 260212A: SVOM/GRM observation of a long burst
Date
2026-02-14T01:04:56Z (7 months ago)
From
zhangjinpeng@ihep.ac.cn
Via
Web form
SVOM/GRM team: Jin-Peng Zhang, Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP)
SVOM/ECLAIRs team: Frédéric Daigne (IAP), Olivier GODET (IRAP)
Report on behalf of the SVOM team:
SVOM/GRM was triggered in-flight by GRB 260212A at 2026-02-12T17:49:08.000 (T0), which is also detected by Fermi/GBM (Fermi GBM Team, GCN #43716) and Glowbug (C.C. Cheung et al., GCN #43719).
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 23.6 +1.4/-1.4 s in the 15-5000 keV band.
The SVOM/GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb260212A.png
In addition, the position of this burst, according to Fermi/GBM localization (RA = 228.9, Dec = 74.1, Fermi GBM Team, GCN #43716), is located at about 53 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. ECLAIRs was not collecting data at the time of this burst.
With this localization, the time-averaged spectrum from T0-1.0 to T0+11.0 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.87 +0.07/-0.07 and the cutoff energy, parameterized as Epeak, is 116 +6/-5 keV. The event fluence (10-1000 keV) in this time interval is (7.24 +0.20/-0.19)E-06 erg/cm^2.
The 1s peak spectrum, measured from T0+8.8 to T0+9.8 s, is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.03 +0.09/-0.08 and the cutoff energy, parameterized as Epeak, is 157 +16/-13 keV. The flux (10-1000 keV) in this time interval is (1.88 +0.09/-0.08)E-06 erg/cm^2/s.
The localization of GRB 260212A in the 'Amati' relation diagram is shown at:
https://www.bursthub.cn//admin/static/svgrb260212A_amati.png
And the localization in the 'Yonetoku' relation diagram is shown at:
https://www.bursthub.cn//admin/static/svgrb260212A_yonetoku.png
The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS.
The SVOM/GRM point of contact for this burst is: Jin-Peng Zhang (IHEP) (zhangjinpeng@ihep.ac.cn)
GCN Circular 43719
Subject
GRB 260212A: Glowbug gamma-ray detection
Date
2026-02-13T03:41:12Z (7 months ago)
From
C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>
Via
Web form
C.C. Cheung, R. Woolf, 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 260212A, which was also detected by Fermi/GBM (GCN 43716).
Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-02-12 17:49:06.400 with a duration of 10.5 s and a total significance of about 69 sigma. The light curve comprises two primary peaks at ~T0+1s and +10s.
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 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 43717
Subject
Fermi GRB 260212A: Global MASTER-Net observations report
Date
2026-02-12T19:15:22Z (7 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-Kislovodsk robotic telescope [1] located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 260212A ( Fermi GBM team, GCN 43716) errorbox 552 sec after notice time and 585 sec after trigger time at 2026-02-12 17:58:53 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 59 deg. The sun altitude is -37.1 deg.
The galactic latitude b = 40 deg., longitude l = 111 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=3132416
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
645 | 2026-02-12 17:58:53 | MASTER-Kislovodsk | (15h 16m 06.75s , +73d 36m 46.3s) | C | 120 | 18.0 |
786 | 2026-02-12 18:01:14 | MASTER-Kislovodsk | (15h 16m 08.64s , +73d 36m 52.0s) | C | 120 | 17.5 |
926 | 2026-02-12 18:03:34 | MASTER-Kislovodsk | (15h 16m 10.47s , +73d 36m 57.7s) | C | 120 | 17.6 |
1068 | 2026-02-12 18:05:56 | MASTER-Kislovodsk | (15h 16m 12.12s , +73d 37m 03.6s) | C | 120 | 17.7 |
1209 | 2026-02-12 18:08:16 | MASTER-Kislovodsk | (15h 16m 13.41s , +73d 37m 09.3s) | C | 120 | 17.4 |
1652 | 2026-02-12 18:16:09 | MASTER-Kislovodsk | (15h 10m 30.28s , +72d 55m 28.4s) | C | 60 | 17.0 |
1860 | 2026-02-12 18:19:38 | MASTER-Kislovodsk | (15h 30m 36.29s , +74d 48m 40.5s) | C | 60 | 17.3 |
2274 | 2026-02-12 18:26:31 | MASTER-Kislovodsk | (15h 03m 57.80s , +76d 45m 03.8s) | C | 60 | 17.0 |
2516 | 2026-02-12 18:30:34 | MASTER-Kislovodsk | (15h 52m 21.24s , +72d 54m 23.0s) | C | 60 | 17.3 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
[1] - V.M. Lipunov, V.G. Kornilov, E.S. Gorbovskoy, N.A. Tiurina & A.S.Kuznetsov, 2023, Astronomical Robotic Networks and Operative Multichanel Astrophysics, Lomonosov MSU PRESS, 591pp.
http : // www.pereplet.ru/lipunov/625.html
GCN Circular 43716
Subject
GRB 260212A: Fermi GBM Final Real-time Localization
Date
2026-02-12T17:59:41Z (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 17:49:08 UT on 12 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260212A (trigger 792611353.21224 / 260212742).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 228.9, Dec = 74.1 (J2000 degrees, equivalent to J2000 15h 15m, 74d 05'), with a statistical uncertainty of 1.1 degrees.
The angle from the Fermi LAT boresight is 127.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/quicklook/glg_skymap_all_bn260212742.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/quicklook/glg_healpix_all_bn260212742.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/quicklook/glg_lc_medres34_bn260212742.gif