GRB 260130A

Jin-Peng Zhang, Chen-Wei Wang, Chao Zheng, and Shao-Lin Xiong (IHEP) report on behalf of the Insight-HXMT team:

At 2026-01-30T13:29:20.800 (T0), Insight-HXMT/HE detected a short GRB 260130A, which is also detected by Fermi/GBM (Fermi GBM Team, GCN #43569
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 ; A. Jameson et al., GCN #43575
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 ).

The Insight-HXMT/HE light curve mainly consists of a bright single pulse with a T90 of 0.08 +/- 0.02 s. The 1 ms peak rate (since this is a bright short burst with duration < 1 s, we check 1 ms peak rate instead of 1 s), measured from T0+0.019 s, is 46000 +/- 5000 cnts/sec. Insight-HXMT/HE detected a total of 1250 +/- 50 counts from this burst.

The Insight-HXMT/HE light curve can be found here:
https://www.bursthub.cn//admin/static/hxmtgrb260130A.png

All measurements above are made with the CsI detectors of Insight-HXMT/HE operating in the regular mode with the energy range of about 60-900 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://hxmten.ihep.ac.cn

Jin-Peng Zhang, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team:

GECAM-B was triggered in-flight by GRB 260130A, at 2026-01-30T13:29:20.850 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43569
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 ; A. Jameson et al., GCN #43575
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 ).

According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of a bright short pulse, with a duration (T90) of 0.083 +/- 0.009 s.

The GECAM-B light curve can be found here:
https://www.bursthub.cn//admin/static/gecambgrb260130A.png

The time-averaged spectrum from T0 - 0.05 to T0 + 0.02 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.52 +0.23/-0.24 and the cutoff energy, parameterized as Epeak, is 860 +190/-140 keV. The event fluence (10-1000 keV) in this time interval is (1.28 +0.11/-0.10)E-06 erg/cm^2.

The 'Amati' relation diagram of GRB 260130A is shown at:
https://www.bursthub.cn//admin/static/gecambgrb260130A_amati.png

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).

A. Jameson (UAH), C. Meegan (UAH), and M. Dafčíková (MUNI) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:

"At 13:29:20.82 UT on 30 January 2026, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 260130A (trigger 791472565/260130562).

The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 48.70, Dec = 64.17 (J2000 degrees, equivalent to
J2000 3h 14m, +64d 10'), with a statistical uncertainty of 1.60 degrees.
(radius, 1-sigma containment, statistical only; there is additionally a
systematic error which we have characterized as a mixture of two Gaussians,
one with a radius of 1.8 degrees (52% contribution) and one with a radius
of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1]).

The angle from the Fermi LAT boresight is 16 degrees.

The GBM light curve consists of a single emission episode with a duration (T90)
of about 0.5 s (50-300 keV). The time-averaged spectrum
from T0-0.07 to T0+0.20 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.41 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 730 +/- 30 keV.

The event fluence (10-1000 keV) in this time interval is
(8.8 +/- 0.4)E-07 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band is 27 +/- 1 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 570 +/- 20 keV, alpha = -0.33 +/- 0.02 and beta = -2 +/- 0.1.


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/"

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 260130A ( Fermi GBM team, GCN 43569
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 ) errorbox  6593 sec after notice time and 6628 sec after trigger time at 2026-01-30 15:19:49 UT, with upper limit up to  15.6 mag. Observations started at twilight.  The observations began at zenith distance = 23 deg. The sun  altitude  is -11.2 deg. 

The galactic latitude b =  6 deg., longitude l = 138 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=3118825

We obtain a following upper limits.  

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

    6659 | 2026-01-30 15:19:49 |   MASTER-Kislovodsk | (03h 14m 10.80s , +65d 46m 26.8s) |   C |    60 | 15.4 |        
    6760 | 2026-01-30 15:21:30 |   MASTER-Kislovodsk | (03h 33m 51.07s , +65d 44m 38.9s) |   C |    60 | 15.3 |        
    6860 | 2026-01-30 15:23:10 |   MASTER-Kislovodsk | (03h 28m 09.77s , +63d 51m 38.5s) |   C |    60 | 15.6 |        
    6964 | 2026-01-30 15:24:54 |   MASTER-Kislovodsk | (03h 46m 28.40s , +63d 52m 21.7s) |   C |    60 | 15.4 |        
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

The Fermi GBM team reports the detection of a likely SHORT GRB

At 13:29:20 UT on 30 Jan 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260130A (trigger 791472565.82111 / 260130562).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 48.7, Dec = 64.2 (J2000 degrees, equivalent to J2000 03h 14m, 64d 12'), with a statistical uncertainty of 1.6 degrees.

The angle from the Fermi LAT boresight is 16.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260130562/quicklook/glg_skymap_all_bn260130562.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/bn260130562/quicklook/glg_healpix_all_bn260130562.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260130562/quicklook/glg_lc_medres34_bn260130562.gif