GRB250116A

This page lists all entries on GRB250116A in GRBweb

Summary Fermi GBM IPN GCN 38962 GCN 38963 GCN 38965 GCN 38967

Summary table
Variable Value Source
GRB_name_Fermi GRB250116524
T0 12:33:59.530 UTC GCN_circulars,Fermi GBM Det
ra 266.6417° IPN
decl -19.3667° IPN
pos_error 1.30e-01° IPN
T90 15.872 s Fermi_GBM
T90_error 0.362 s Fermi_GBM
T90_start 12:34:01.901 UTC Fermi_GBM
fluence 9.31e-05 erg/cm² Fermi_GBM
fluence_error 1.18e-07 erg/cm² Fermi_GBM
T100 18.243 s
GBM_located False
mjd 60691.5236056713 GCN_circulars,Fermi GBM Det
Fermi GBM table
GRB_name_Fermi GRB250116524
trigger_name bn250116524
ra 269.8000°
decl -18.4800°
pos_error 4.40e+00°
datum 2025-01-16
t_trigger 12:33:59.533 UTC
T90 15.872 s
T90_error 0.362 s
T90_start 12:34:01.901 UTC
fluence 9.31e-05 erg/cm²
fluence_error 1.18e-07 erg/cm²
flux_1024 4.39e+01 erg/cm²/s
flux_1024_error 4.00e-01 erg/cm²/s
flux_1024_time 1.73e+01 erg/cm²/s
flux_64 5.25e+01 erg/cm²/s
flux_64_error 1.74e+00 erg/cm²/s
IPN table
GRB_name GRB250116A
ra 266.6417°
decl -19.3667°
pos_error 1.30e-01°
GCN 38962 table
GRB_name GRB250116A
GCN_number 38962
Detection_method Fermi GBM Det
t_trigger 12:33:59.530 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38962 SUBJECT: GRB 250116A: Fermi GBM Observation of an Extremely Interesting Burst DATE: 25/01/16 20:44:37 GMT FROM: Ava Myers at NASA GSFC E. Bissaldi (Politecnico and INFN Bari), A. Myers (NPP/GSFC), O.J. Roberts (USRA), and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 12:33:59.53 UT on 16 January 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250116A (trigger 758723644/250116524). The angle from the Fermi LAT boresight is 55 degrees. The GBM light curve consists of multiple peaks, with an apparent duration (T90) of 15.9 s (50-300 keV). However, there is low energy emission that extends longer than the T90 out to at least several hundred seconds after the trigger time. The Sun emerges from Earth occultation midway during this burst, and thus due to the spacecraft motion during this time and the localization being relative close to the Sun position, it is currently unknown whether this is part of a long duration C-class Solar Flare or afterglow emission from the Burst. Analysis is ongoing. The time-averaged spectrum from T0+0 to T0+21 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.71 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 462 +/- 6 keV. from T0+0 to T0+21 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.71 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 462 +/- 6 keV. The event fluence (10-1000 keV) in this time interval is (9.97 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+17 s in the 10-1000 keV band is 43.9 +/- 0.4 ph/s/cm^2. Multi-wavelength follow up of this Burst is strongly encouraged. 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 38963 table
GRB_name GRB250116A
GCN_number 38963
Detection_method Fermi LAT Det
t_trigger 12:33:59.530 UTC
ra 266.6400°
decl -19.3600°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38963 SUBJECT: GRB 250116A: Fermi-LAT detection DATE: 25/01/16 20:58:26 GMT FROM: A. Holzmann Airasca at University of Trento and INFN Bari A. Holzmann Airasca (UniTrento and INFN Bari), S. Lopez (CNRS / IN2P3), N. Di Lalla (Stanford University), T. Khalil (Johannesburg Univ) report on behalf of the Fermi-LAT Collaboration: On January 16, 2025, Fermi-LAT detected high-energy emission from GRB 250116A, which was also detected by Fermi-GBM (trigger 758723644/ 250116524, GCN 38962). The best LAT on-ground location is found to be: RA, Dec = 266.64, -19.36 (J2000) with an error radius of 0.13 deg (90 % containment, statistical error only). This was 53 deg from the LAT boresight at the time of the GBM trigger (T0 = 12:33:59.53 UT). The data from the Fermi-LAT shows a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0 - 1500 s after the GBM trigger is (4.0 ± 0.4) E-5 ph/cm2/s. The estimated photon index above 100 MeV is 2.3 ± 0.1. The highest-energy photon is a 3.9 GeV event which is observed 59 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Chiara Bartolini (Chiara.Bartolini@ba.infn.it). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 38965 table
GRB_name GRB250116A
GCN_number 38965
Detection_method INTEGRAL
Circular_text TITLE: GCN CIRCULAR NUMBER: 38965 SUBJECT: GRB 250116A: INTEGRAL/SPI-ACS and PICsIT detection DATE: 25/01/16 22:28:51 GMT FROM: Aishwarya L Thakur at INAF-IAPS, Rome Patrizia Barria(a,b), Giulia Gianfagna(a), James Craig Rodi(a), Aishwarya Linesh Thakur(a), Lorenzo Natalucci(a,b), Luigi Piro(a) report: GRB 250116A was discovered by Fermi/GBM (GCN 38962, seen also by Fermi/LAT GCN 38963) at time 2025-01-16T12:33:59.53 (UTC) with a duration of 16 s. We searched for any corresponding counterpart in the INTEGRAL/SPI-ACS and IBIS/PICsIT data. In a SPI/ACS light curve above 80 keV, we find a pulse temporally coincident with the GBM detection having an approximate duration of ~ 15 sec. This pulse is also seen in the PICsIT lightcurve above 212 keV, with a similar duration. The approximate peak count rate in SPI/ACS is 80,000 cts/s for E>80 keV, over a median background rate of 65,000 cts/s. After the GRB spike, we note that there is a second, stronger pulse in the light curves of both instruments. The association of this pulse to the GRB at this moment is unclear and is under investigation. This work is based on observations with INTEGRAL, an ESA project with instruments and a science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, and Spain), and with the participation of Russia and the USA. The SPI-ACS detector system has been provided by MPE Garching/Germany. ----- (a) INAF/IAPS-Rome (b) ICSC National Research Centre for High-Performance Computing
GCN 38967 table
GRB_name GRB250116A
GCN_number 38967
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38967 SUBJECT: GRB 250116A: GECAM-B detection of a long burst DATE: 25/01/17 09:54:30 GMT FROM: Yue Wang Yue Wang, Shao-Lin Xiong, Chen-Wei Wang, Chao Zheng, Shi-Jie Zheng, Cheng-Kui Li, Wen-Long Zhang, Yan-Qiu Zhang report on behalf of the GECAM team: GECAM-B was triggered in-flight by a long burst, GRB 250116A, at 2025-01-16T12:33:59.550 UTC (T0), which was also observed by Fermi/GBM (GCN # 38962) and Fermi/LAT (GCN # 38963). According to the GECAM-B light curves in about 20-1000 keV, this burst mainly consists of multiple pulses with a duration (T90) of about 15.5（+0.4,-0.6）s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecamgrb250116A.png GECAM location is consistent with the Fermi/LAT position within the error. We notice that the location is close to the Galactic plane and the light curve pattern is somewhat atypical for GRB but more similar to SGR, though the duration is much longer than SGR. We note that these results are based on in-flight trigger data and thus very preliminary. Refined analysis will be reported later. Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two microsatellites (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).