GRB260104A

This page lists all entries on GRB260104A in GRBweb

Summary IPN Swift GCN 43315 GCN 43319 GCN 43320 GCN 43322 GCN 43325 GCN 43355

Summary table
Variable Value Source
T0 5:37:02 UTC GCN_circulars,Swift Det
ra 337.3992° Swift
decl -21.2955° Swift
pos_error 2.59e-04° Swift
GBM_located False
mjd 61044.23405092592 GCN_circulars,Swift Det
IPN table
GRB_name GRB260104A
ra 337.4167°
decl -21.2833°
pos_error 5.00e-02°
Swift table
GRB_name GRB260104A
t_trigger 5:37:02 UTC
ra 337.3992°
decl -21.2955°
pos_error 2.59e-04°
GCN 43315 table
GRB_name GRB260104A
GCN_number 43315
Detection_method Swift Det
t_trigger 5:37:02 UTC
ra 337.4150°
decl -21.2800°
Circular_text TITLE: GCN CIRCULAR NUMBER: 43315 SUBJECT: GRB 260104A: Swift detection of a burst DATE: 26/01/04 05:57:24 GMT FROM: K.L. Page at U Leicester R. Caputo (GSFC), J. J. DeLaunay (PSU), K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 05:37:02 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 260104A (trigger=1430212). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 337.415, -21.280 which is RA(J2000) = 22h 29m 40s Dec(J2000) = -21d 16' 48" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 20 sec. The peak count rate was ~2400 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 05:38:28.9 UT, 86.1 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 337.39898, -21.29547 which is equivalent to: RA(J2000) = 22h 29m 35.76s Dec(J2000) = -21d 17' 43.7" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 77 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (3.40 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.8 (+2.48/-2.16) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 90 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers none of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.033. Burst Advocate for this burst is R. Caputo (regina.caputo AT nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/)
GCN 43319 table
GRB_name GRB260104A
GCN_number 43319
Detection_method Swift-XRT Det
ra 337.3992°
decl -21.2955°
Circular_text TITLE: GCN CIRCULAR NUMBER: 43319 SUBJECT: GRB 260104A: Enhanced Swift-XRT position DATE: 26/01/04 14:49:33 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 3264 s of XRT Photon Counting mode data and 6 UVOT images for GRB 260104A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 337.39920, -21.29552 which is equivalent to: RA (J2000): 22h 29m 35.81s Dec (J2000): -21d 17' 43.9" with an uncertainty of 2.0 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at https://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 43320 table
GRB_name GRB260104A
GCN_number 43320
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 43320 SUBJECT: GRB 260104A: Swift-XRT refined Analysis DATE: 26/01/04 14:58:50 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), D.N. Burrows (PSU), S. Lanava (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-OAR), M. Perri (SSDC & INAF-OAR) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.3 ks of XRT data for GRB 260104A, from 101 s to 28.3 ks after the trigger. The data comprise 10 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. The late-time light curve (from T0+5.1 ks) can be modelled with a power-law decay with a decay index of alpha=1.22 (+0.26, -0.23). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.78 (+0.16, -0.10). The best-fitting absorption column is 3.55 (+3.69, -0.15) x 10^20 cm^-2, consistent with the Galactic value of 3.4 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 3.7 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.55 (+3.69, -0.15) x 10^20 cm^-2 Galactic foreground: 3.4 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.78 (+0.16, -0.10) If the light curve continues to decay with a power-law decay index of 1.22, the count rate at T+24 hours will be 4.6 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x 10^-13 (1.8 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at https://www.swift.ac.uk/xrt_products/01430212. This circular is an official product of the Swift-XRT team.
GCN 43322 table
GRB_name GRB260104A
GCN_number 43322
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 43322 SUBJECT: Swift GRB 260104A: Global MASTER-Net observations report DATE: 26/01/04 16:48:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs 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) was pointed to the Swift GRB 260104A ( R. Caputo et al., GCN 43315) errorbox 39152 sec after notice time and 39173 sec after trigger time at 2026-01-04 16:29:55 UT, with upper limit up to 15.0 mag. The observations began at zenith distance = 82 deg. The sun altitude is -28.6 deg. The galactic latitude b = -58 deg., longitude l = 36 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3095622 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 39263 | MASTER-Kislovodsk | C | 180 | 13.5 | 39263 | MASTER-Kislovodsk | C | 180 | 14.3 | 39471 | MASTER-Kislovodsk | C | 180 | 13.5 | 39471 | MASTER-Kislovodsk | C | 180 | 14.1 | 39687 | MASTER-Kislovodsk | C | 180 | 14.2 | 39687 | MASTER-Kislovodsk | C | 180 | 15.0 | 39903 | MASTER-Kislovodsk | C | 180 | 14.7 | 39903 | MASTER-Kislovodsk | C | 180 | 15.0 | 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 43325 table
GRB_name GRB260104A
GCN_number 43325
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 43325 SUBJECT: GRB 260104A: COLIBRÍ optical upper limits DATE: 26/01/05 04:32:13 GMT FROM: globus@astro.unam.mx Noémie Globus (UNAM), Jean-Luc Atteia (IRAP), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Alan M. Watson (UNAM), Dalya Akl (NYUAD), Camila Angulo (UNAM), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Nikos Mandarakas (LAM), 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 GRB 260104A (Caputo et al., GCN Circ. 43315; Evans et al., GCN Circ. 43319; Kennea et al., GCN Circ. 43320), using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-01-05 at 01:46 to 02:44 UTC (from 20.16 to 21.12 hr after the trigger) and obtained 41 minutes of simultaneous exposure in the r and z filters. The data were reduced and coadded with the COLIBRÍ ASU pipeline and analyzed with STDWeb/STDPipe (Karpov 2025). The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and was not corrected for Galactic extinction. In the stacked image, we do not detect any new source at the XRT uncertainty region (Caputo et al., GCN Circ. 43315) down to the following 5-sigma limit: r > 21.90, z > 20.96. 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 43355 table
GRB_name GRB260104A
GCN_number 43355
Detection_method Swift-BAT Det
ra 337.3950°
decl -21.2910°
Circular_text TITLE: GCN CIRCULAR NUMBER: 43355 SUBJECT: GRB 260104A: Swift-BAT refined analysis DATE: 26/01/09 03:01:10 GMT FROM: Tyler Parsotan at NASA GSFC M. J. Moss (GSFC), S. D. Barthelmy (GSFC), R. Caputo (GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 260104A (trigger #1430212) (Caputo, et al., GCN Circ. 43315). The BAT ground-calculated position is RA, Dec = 337.395, -21.291 deg which is RA(J2000) = 22h 29m 34.8s Dec(J2000) = -21d 17' 27.5" with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 99%. The mask-weighted light curve shows two pulses. T90 (15-350 keV) is 13.26 +- 2.65 sec (estimated error including systematics). The time-averaged spectrum from T-10.09 to T+5.22 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.32 +- 1.08, and Epeak of 42.5 +- 8.8 keV (chi squared 67.04 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 3.5 +- 0.5 x 10^-07 erg/cm2 and the 1-sec peak flux measured from T-0.23 sec in the 15-150 keV band is 1.3 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.85 +- 0.16 (chi squared 76.81 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1430212