GRB240112C

This page lists all entries on GRB240112C in GRBweb

Summary Fermi GBM IPN Swift GCN 35522 GCN 35525 GCN 35530 GCN 35531 GCN 35533 GCN 35534 GCN 35545 GCN 35546

Summary table
Variable Value Source
GRB_name_Fermi GRB240112734
T0 17:37:24 UTC GCN_circulars,Swift Det
ra 270.6441° Swift
decl 24.4892° Swift
pos_error 9.71e-05° Swift
T90 5.312 s Fermi_GBM
T90_error 0.405 s Fermi_GBM
T90_start 17:37:25.052 UTC Fermi_GBM
fluence 4.52e-06 erg/cm² Fermi_GBM
fluence_error 2.01e-08 erg/cm² Fermi_GBM
T100 6.364 s
GBM_located False
mjd 60321.734305555554 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB240112734
trigger_name bn240112734
ra 262.4900°
decl 29.1500°
pos_error 3.13e+00°
datum 2024-01-12
t_trigger 17:37:25.116 UTC
T90 5.312 s
T90_error 0.405 s
T90_start 17:37:25.052 UTC
fluence 4.52e-06 erg/cm²
fluence_error 2.01e-08 erg/cm²
flux_1024 2.02e+01 erg/cm²/s
flux_1024_error 4.23e-01 erg/cm²/s
flux_1024_time -6.40e-02 erg/cm²/s
flux_64 2.92e+01 erg/cm²/s
flux_64_error 1.91e+00 erg/cm²/s
IPN table
GRB_name GRB240112C
ra 270.6458°
decl 24.4833°
pos_error 5.00e-02°
Swift table
GRB_name GRB240112C
t_trigger 17:37:24 UTC
ra 270.6441°
decl 24.4892°
pos_error 9.71e-05°
GCN 35522 table
GRB_name GRB240112C
GCN_number 35522
Detection_method Swift Det
t_trigger 17:37:24 UTC
ra 270.6440°
decl 24.4870°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35522 SUBJECT: GRB 240112C: Swift detection of a burst with an optical counterpart DATE: 24/01/12 17:51:21 GMT FROM: David Palmer at LANL R. A. J. Eyles-Ferris (U Leicester), J.D. Gropp (PSU), S. Laha (GSFC/UMBC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 17:37:24 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240112C (trigger=1208389). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 270.644, +24.487 which is RA(J2000) = 18h 02m 35s Dec(J2000) = +24d 29' 12" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). Due to a telemetry gap, the BAT lightcurve is not immediately available. The XRT began observing the field at 17:39:18.9 UT, 114.0 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 270.64225, 24.48830 which is equivalent to: RA(J2000) = 18h 02m 34.14s Dec(J2000) = +24d 29' 17.9" with an uncertainty of 4.7 arcseconds (radius, 90% containment). This location is 7.4 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. We cannot determine whether the source is fading at the present time. No spectrum from the promptly downlinked event data is yet available to determine the column density. UVOT took a finding chart exposure of 115 seconds with the White filter starting 120 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 18:02:34.59 = 270.64414 DEC(J2000) = +24:29:21.2 = 24.48923 with a 90%-confidence error radius of about 0.75 arc sec. This position is 7.4 arc sec. from the center of the XRT error circle. The estimated magnitude is 16.73 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.108. Burst Advocate for this burst is R. A. J. Eyles-Ferris (raje1 AT leicester.ac.uk). 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 35525 table
GRB_name GRB240112C
GCN_number 35525
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35525 SUBJECT: Swift GRB 240112C: Global MASTER-Net observations report DATE: 24/01/12 20:15:12 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko, G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gress, N.M. Budnev, O.Ershova (Irkutsk State University, API), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich (Blagoveschensk Educational State University) MASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB 240112C ( R. A. J. Eyles-Ferris et al., GCN 35522) errorbox 8981 sec after notice time and 9002 sec after trigger time at 2024-01-12 20:07:27 UT, with upper limit up to 15.4 mag. The observations began at zenith distance = 85 deg. The sun altitude is -45.5 deg. The galactic latitude b = 21 deg., longitude l = 51 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2354458 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 9040 | MASTER-Tunka | C | 75 | 12.4 | 9124 | MASTER-Tunka | C | 70 | 15.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 35530 table
GRB_name GRB240112C
GCN_number 35530
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35530 SUBJECT: GRB 240112C: SAO RAS optical observations DATE: 24/01/13 04:58:59 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin and O. A. Maslennikova (SAO RAS) report on behalf of the GRB follow-up team. We observed the field of Swift GRB 240112C (Eyles-Ferris et al., GCN #35522) with the 1-m telescope of SAO RAS equipped with the CCD photometer. We obtained 21 x 60 sec. images in Rc band on January 13, 03:00:16--03:34:31 UT (t_mid - T0 = 0.40277 days) under mediocre weather conditions. We did not detect any significant source at the OT position down to the limiting magnitude R_lim = 21.1 (based on R2 magnitudes of nearby USNO-B1 stars).
GCN 35531 table
GRB_name GRB240112C
GCN_number 35531
Detection_method Swift-XRT Other
ra 270.6440°
decl 24.4889°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35531 SUBJECT: GRB 240112C: Swift-XRT refined Analysis DATE: 24/01/13 10:19:51 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.3 ks of XRT data for GRB 240112C, from 97 s to 45.8 ks after the BAT trigger. The data comprise 39 s in Windowed Timing (WT) mode (the first 10 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. Using 2660 s of PC mode data and 6 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 270.64402, +24.48893 which is equivalent to: RA (J2000): 18h 02m 34.56s Dec(J2000): +24d 29' 20.2" with an uncertainty of 2.0 arcsec (radius, 90% confidence). The light curve can be modelled with an initial power-law decay with an index of alpha=0.61 (+0.04, -0.48), followed by a break at T+5970 s to an alpha of 1.30 (+0.18, -0.20). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.92 (+0.14, -0.13). The best-fitting absorption column is 2.0 (+0.5, -0.4) x 10^21 cm^-2, in excess of the Galactic value of 1.3 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.0 (+0.5, -0.4) x 10^21 cm^-2 Galactic foreground: 1.3 x 10^21 cm^-2 Excess significance: 2.5 sigma Photon index: 1.92 (+0.14, -0.13) If the light curve continues to decay with a power-law decay index of 1.30, the count rate at T+24 hours will be 0.015 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.3 x 10^-13 (7.0 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01208389. This circular is an official product of the Swift-XRT team.
GCN 35533 table
GRB_name GRB240112C
GCN_number 35533
Detection_method Fermi GBM Det
t_trigger 17:37:25.120 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35533 SUBJECT: GRB 240112C: Fermi GBM Detection DATE: 24/01/13 16:09:48 GMT FROM: Peter Veres at University of Alabama in Huntsville P. Veres (UAH), R. Hamburg (CNRS/IN2P3), A. Myers (NPP/GSFC) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 17:37:25.12 UT on 12 January 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240112C (trigger 726773850/240112734). GRB 240112C was also localized by Swift BAT and XRT (Eyles-Ferris et al., GCN #35522). The Fermi GBM on-ground Localization is consistent with the Swift position. The angle from the Fermi LAT boresight is 43 degrees. The GBM light curve consists of two pulses with a duration (T90) of about 5.3 s (50-300 keV). The time-averaged spectrum from T0-0.6 to T0+6.3 s is best fit by a Band function with with Epeak= 71 +/- 6 keV, alpha = -1.26 +/- 0.08 and beta = -2.34 +/- 0.10. The event fluence (10-1000 keV) in this time interval is (4.8 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.064 s in the 10-1000 keV band is 20.2 +/- 0.4 ph/s/cm^2. 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 35534 table
GRB_name GRB240112C
GCN_number 35534
Detection_method Swift-UVOT Det
ra 270.6441°
decl 24.4892°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35534 SUBJECT: GRB 240112C: Swift/UVOT Detection DATE: 24/01/14 18:22:22 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and Eyles-Ferris (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240112C 121 s after the BAT trigger (Eyles-Ferris et al., GCN Circ. 35522). A source consistent with the XRT position is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 18:02:34.58 = 270.64410 (deg.) Dec (J2000) = +24:29:21.3 = 24.48925 (deg.) with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 121 236 113 16.98 +/- 0.04 v 4955 5126 169 >18.6 b 4340 4539 197 19.35 +/- 0.16 u 4134 4334 197 19.11 +/- 0.18 w1 3930 4129 197 19.13 +/- 0.24 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.108 in the direction of the burst (Schlegel et al. 1998).
GCN 35545 table
GRB_name GRB240112C
GCN_number 35545
Detection_method Fermi GBM Det
t_trigger 17:37:27 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35545 SUBJECT: GRB 240112C: VZLUSAT-2 detection DATE: 24/01/16 16:05:00 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration. The long-duration GRB 240112C (Swift/BAT detection: GCN 35522; Fermi/GBM detection: GCN 35533; GRBAlpha detection: GCN 35536; Konus/Wind detection: GCN 35539; INTEGRAL/SPI-ACS detection: trigger no. 10466) was detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/). The data acquisition was performed by the GRB detector unit no. 1. The detection was confirmed at the peak time 2024-01-12 17:37:27 UTC. The T90 duration is 3 s and the significance during T90 reaches 14 sigma. The light curve obtained by VZLUSAT-2 is available here: https://vzlusat2.konkoly.hu/static/share/GRB240112C_GCN_VZLUSAT2.pdf All VZLUSAT-2 detections are listed at: https://monoceros.physics.muni.cz/hea/VZLUSAT-2/ The GRB detectors on VZLUSAT-2 are a demonstration payload for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13 from Cape Canaveral.
GCN 35546 table
GRB_name GRB240112C
GCN_number 35546
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 35546 SUBJECT: GRB 240112C: Glowbug gamma-ray detection DATE: 24/01/16 17:32:02 GMT FROM: C.C. Cheung at Naval Research Lab C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240112C, which was also detected by Swift/BAT, Fermi/GBM, GRBAlpha, Konus-Wind, VZLUSAT-2 (GCN #35522, #35533, #35536, #35539, #35545), and INTEGRAL/SPI-ACS (Trigger no. 10466). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-01-12 17:37:23.592 with a duration of 4.10 s and a total significance of about 20.1 sigma. The light curve comprises two primary peaks. Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=1.6 and a cutoff energy ("Epeak") of 185 keV. The modeled 10-10000 keV fluence is 7.5e-07 erg/cm^2. 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 telescopes 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. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV. [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] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006 Distribution Statement A: Approved for public release. Distribution is unlimited.