TITLE: GCN CIRCULAR NUMBER: 43341 SUBJECT: GRB 260105B: SVOM/GRM observation DATE: 26/01/06 07:25:39 GMT FROM: Yue Wang <m18509381757@163.com> SVOM/GRM team: Yue Wang, Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Sebastien Guillot (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260105B (SVOM trigger reference: sb26010502) at 2026-01-05T23:21:37.000 (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43336). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of a single pulse with a T90 of 6.8 +1.8/-1.4 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260105B.png In addition, the position of this burst, as determined by Fermi/GBM (RA = 259.7, Dec = 1.7, Error = 2.0, GCN #43336), is located at about 91 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. With this localization, the time-averaged spectrum from T0-1 to T0+7 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.61 +0.12/-0.13 and the cutoff energy, parameterized as Epeak, is 177 +15/-13 keV. The event fluence (10-1000 keV) in this time interval is (9.34+0.47/-0.44)E-06 erg/cm^2. The 1s peak spectrum, measured from T0-1.5 to T0+2.5 s, if fitted by a power law function with an exponential high-energy cutoff, the power law index is -0.81 +0.15/-0.17 and the cutoff energy, parameterized as Epeak, is 242 +45/-33 keV. The flux (10-1000 keV) in this time interval is (2.53 +0.22/-0.20)E-06 erg/cm^2/s. The localization of GRB 260105B in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260105B_amati.png The localization of GRB 260105B in the 'Yonetoku' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260105B_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: Yue Wang (IHEP) (yuewang@ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43341. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0LW...