GRB241120A

This page lists all entries on GRB241120A in GRBweb

Summary Fermi GBM IPN GCN 38279 GCN 38280 GCN 38285 GCN 38291 GCN 38295 GCN 38297 GCN 38307

Summary table
Variable Value Source
GRB_name_Fermi GRB241120246
T0 5:53:58 UTC GCN_circulars,Fermi GBM final loc
ra 194.2917° IPN
decl 52.1500° IPN
pos_error 1.67e-02° IPN
T90 3.2 s Fermi_GBM
T90_error 0.202 s Fermi_GBM
T90_start 5:53:58.416 UTC Fermi_GBM
fluence 3.37e-06 erg/cm² Fermi_GBM
fluence_error 1.25e-08 erg/cm² Fermi_GBM
T100 3.616 s
GBM_located False
mjd 60634.24581018519 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB241120246
trigger_name bn241120246
ra 194.2908°
decl 52.1503°
pos_error 2.76e+00°
datum 2024-11-20
t_trigger 5:53:58.544 UTC
T90 3.2 s
T90_error 0.202 s
T90_start 5:53:58.416 UTC
fluence 3.37e-06 erg/cm²
fluence_error 1.25e-08 erg/cm²
flux_1024 1.23e+01 erg/cm²/s
flux_1024_error 2.64e-01 erg/cm²/s
flux_1024_time 1.66e+00 erg/cm²/s
flux_64 1.94e+01 erg/cm²/s
flux_64_error 1.21e+00 erg/cm²/s
IPN table
GRB_name GRB241120A
ra 194.2917°
decl 52.1500°
pos_error 1.67e-02°
GCN 38279 table
GRB_name GRB241120A
GCN_number 38279
Detection_method Fermi GBM final loc
t_trigger 5:53:58 UTC
ra 192.5000°
decl 49.7000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38279 SUBJECT: GRB 241120A: Fermi GBM Final Real-time Localization DATE: 24/11/20 06:04:29 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 05:53:58 UT on 20 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241120A (trigger 753774843.543556 / 241120246). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 192.5, Dec = 49.7 (J2000 degrees, equivalent to J2000 12h 50m, 49d 42'), with a statistical uncertainty of 1.2 degrees. The angle from the Fermi LAT boresight is 36.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241120246/quicklook/glg_skymap_all_bn241120246.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241120246/quicklook/glg_healpix_all_bn241120246.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241120246/quicklook/glg_lc_medres34_bn241120246.gif
GCN 38280 table
GRB_name GRB241120A
GCN_number 38280
Detection_method INTEGRAL
t_trigger 5:53:58 UTC
ra 194.2908°
decl 52.1504°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38280 SUBJECT: GRB241120A: a long GRB detected by INTEGRAL DATE: 24/11/20 07:01:13 GMT FROM: Diego Gotz at CEA D.Gotz (CEA, Saclay), S.Mereghetti (INAF, IASF-Milano), C.Ferrigno, E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC, Versoix) and J.Borkowski (CAMK, Torun) report: a gamma ray burst lasting about 4 s has been detected by IBAS in the IBIS/ISGRI data at 05:53:58 UT of 2024 November 20. The refined coordinates (J2000) are: R.A.= 194.2908 deg, DEC.= 52.1504 deg with an uncertainty of 1 arcmin (90% c.l.). A preliminary analysis gives a peak flux of about 2 ph/cm2/s (20-200 keV, 1-s integration time) and a fluence in the same energy range of about 1.3e-06 erg/cmsq. This burst has also been detected by Fermi/GBM (GCN 38279), and its position is at 2.7° from the Fermi reported position. A plot of the light curve will be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html
GCN 38285 table
GRB_name GRB241120A
GCN_number 38285
Detection_method Fermi GBM Det
t_trigger 5:53:58.540 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38285 SUBJECT: GRB 241120A: Fermi GBM Observation DATE: 24/11/20 20:31:12 GMT FROM: rhamburg@usra.edu R. Hamburg (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 05:53:58.54 UT on 20 November 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241120A (trigger 753774843/241120246), which was also detected by INTEGRAL/IBAS (Gotz et al. 2024, GCN 38280). The Fermi GBM on-ground location is consistent with the INTEGRAL position. The angle from the Fermi LAT boresight is about 39 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 3.2 s (50-300 keV). The time-averaged spectrum from T0-0.5 to T0+3.3 s is best fit by a Band function with Epeak = 181 +/- 13, alpha = -0.3 +/- 0.1, and beta = -2.4 +/- 0.2. The event fluence (10-1000 keV) in this time interval is (3.6 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+1.7 s in the 10-1000 keV band is 12.3 +/- 0.3 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 38291 table
GRB_name GRB241120A
GCN_number 38291
Detection_method Optical
ra 194.2679°
decl 52.1461°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38291 SUBJECT: GRB 241120A: Mondy and AbAO optical observations DATE: 24/11/21 16:55:29 GMT FROM: XXXX at IKI N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), R. Ya. Inasaridze (AbAO), V. Aivazyan (AbAO) report on behalf of IKI-GRB-FuN: We observed the field of GRB 241120A detected (The Fermi GBM team, GCN 38279; Gotz et al., GCN 38280) with AZT-33IK telescope of Sayan (Mondy) observatory, and AS-32 telescope of Abastumani observatory (AbAO). The observations started at Mondy on 2024-11-20 at 20:01 UT, i.e. ~0.6 days since trigger. Within the localization circle of INTEGRAL (Gotz et al., GCN 38280) we do not find any evident candidates in comparison with known catalogues. However, there is a source in our observations at the coordinates of (J2000) RA=12:57:04.3 Dec=+52:08:45.8 with uncertainty of 0.2 arcses in both coordinates for which it can be assumed that the source is showing marginal decreasing of brightness. The source is presented at least in PS1, SDSS and DESI. Preliminary photometry of the source is as follows: Date UT_start Exp_time t-T0 Filter OT Err UL (s) (mid, days) (3sigma) 2024-11-20 20:01:27 28*120 0.60798 R 19.85 0.10 22.6 AZT-33IK 2024-11-20 23:12:31 56*60 0.74066 R 20.1 0.3 20.6 AS-32 The magnitudes were calibrated with nearby USNO-B1.0 stars (R2 magnitudes) and not corrected for the Galactic extinction. The source is 53 arcsec from the centre of IBIS/ISGRI localization. The catalogued source is a galaxy with estimated photo-z = 0.36 and brightness of r=20.2 (SDSS DR16), and photo-z = 0.38 (DESI). The source brightness in PS1 is r = 20.69. We may suggest the source is a possible candidate in the afterglow of GRB 241120A.
GCN 38295 table
GRB_name GRB241120A
GCN_number 38295
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 38295 SUBJECT: GRB 241120A: CALET Gamma-Ray Burst Monitor detection DATE: 24/11/22 06:14:13 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University M. L. Cherry (LSU), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 241120A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 38279; a long GRB detected by INTEGRAL: Gotz et al., GCN Circ. 38280; Fermi GBM Observation, Hamburg et al., GCN Circ. 38285) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 05:54:00.493 UTC on 20 November 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1416117245/index.html). The burst signal was seen by all CGBM detectors. Because of a problem with the ground alert processing script, the GCN notice was not distributed automatically for this event. The burst light curve shows a single emission episode that starts at T-3.0 sec, peaks at T+0.1 sec, and ends at T+0.8 sec. The T90 and T50 durations measured by the SGM data are 2.9 ± 0.5 sec and 0.8 ± 0.3 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1416117245/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.
GCN 38297 table
GRB_name GRB241120A
GCN_number 38297
Detection_method Konus-Wind Det
t_trigger 5:54:00.717 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38297 SUBJECT: Konus-Wind detection of GRB 241120A DATE: 24/11/22 14:38:03 GMT FROM: Anna Ridnaia at Ioffe Institute A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration GRB 241120A (Fermi-GBM detection: Fermi GBM team, GCN 38279; Hamburg & Meegan, GCN 38285; INTEGRAL (IBIS/ISGRI) detection: Gotz et al., GCN 38280; CALET (CGBM) detection: Cherry et al., GCN 38295) triggered Konus-Wind at T0=21240.717 s UT (05:54:00.717). The burst light curve shows a single pulse, which starts at ~T0-1.9 s and has a total duration of ~2.9 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB241120_T21240/ As observed by Konus-Wind, the burst had a fluence of 3.55(-0.48,+0.59)x10^-6 erg/cm2, and a 64-ms peak flux, measured from T0+0.372 s, of 4.98(-1.17,+1.30)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.91(-0.29,+0.34) and Ep = 267(-56,+95) keV (chi2 = 80/78 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.6 (chi2 = 80/77 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 38307 table
GRB_name GRB241120A
GCN_number 38307
Detection_method Fermi GBM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 38307 SUBJECT: GRB 241120A: GRBAlpha detection DATE: 24/11/25 12:53:07 GMT FROM: Andras Pal at Konkoly Observatory A. Pal (Konkoly Observatory), M. Dafcikova, J. Ripa, M. Kolar, N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Duriskova, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. The long-duration GRB 241120A (Fermi/GBM detection: GCN 38279; INTEGRAL/SPI-ACS detection: GCN 38280; CALET/CGBM detection: GCN 38295; Konus/Wind detection: GCN 38297) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract). The detection was confirmed at the peak time 2024-11-20 05:54:00.1 UTC. The T90 duration measured by GRBAlpha is 3 s and the overall significance during T90 reaches 8 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB241120A_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.