GRB241209D

This page lists all entries on GRB241209D in GRBweb

Summary Fermi GBM IPN Swift GCN 38488 GCN 38489 GCN 38491 GCN 38498 GCN 38503 GCN 38505 GCN 38507 GCN 38508 GCN 38518 GCN 38526 GCN 38527 GCN 38569 GCN 38589

Summary table
Variable Value Source
GRB_name_Fermi GRB241209458
T0 10:59:44 UTC GCN_circulars,Fermi GBM final loc
ra 190.1119° Swift
decl -2.8916° Swift
pos_error 3.62e-04° Swift
T90 44.545 s Fermi_GBM
T90_error 1.145 s Fermi_GBM
T90_start 10:59:45.629 UTC Fermi_GBM
fluence 1.10e-05 erg/cm² Fermi_GBM
fluence_error 7.13e-08 erg/cm² Fermi_GBM
T100 46.174 s
GBM_located False
mjd 60653.45814814815 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB241209458
trigger_name bn241209458
ra 190.1129°
decl -2.8903°
pos_error 2.74e+00°
datum 2024-12-09
t_trigger 10:59:44.093 UTC
T90 44.545 s
T90_error 1.145 s
T90_start 10:59:45.629 UTC
fluence 1.10e-05 erg/cm²
fluence_error 7.13e-08 erg/cm²
flux_1024 4.39e+00 erg/cm²/s
flux_1024_error 3.26e-01 erg/cm²/s
flux_1024_time 5.89e+00 erg/cm²/s
flux_64 6.92e+00 erg/cm²/s
flux_64_error 1.42e+00 erg/cm²/s
IPN table
GRB_name GRB241209D
ra 190.1125°
decl -2.8833°
pos_error 5.00e-02°
Swift table
GRB_name GRB241209D
t_trigger 10:59:46 UTC
ra 190.1119°
decl -2.8916°
pos_error 3.62e-04°
GCN 38488 table
GRB_name GRB241209D
GCN_number 38488
Detection_method Fermi GBM final loc
t_trigger 10:59:44 UTC
ra 191.7000°
decl -2.2000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38488 SUBJECT: GRB 241209D: Fermi GBM Final Real-time Localization DATE: 24/12/09 11:10:17 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 10:59:44 UT on 9 Dec 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241209D (trigger 755434789.093062 / 241209458). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 191.7, Dec = -2.2 (J2000 degrees, equivalent to J2000 12h 46m, -2d 12'), with a statistical uncertainty of 1.9 degrees. The angle from the Fermi LAT boresight is 80.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241209458/quicklook/glg_skymap_all_bn241209458.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/bn241209458/quicklook/glg_healpix_all_bn241209458.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241209458/quicklook/glg_lc_medres34_bn241209458.gif
GCN 38489 table
GRB_name GRB241209D
GCN_number 38489
Detection_method Swift Det
t_trigger 10:59:46 UTC
ra 190.1110°
decl -2.8790°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38489 SUBJECT: GRB 241209D: Swift detection of a burst DATE: 24/12/09 11:23:24 GMT FROM: K.L. Page at U Leicester T. M. Parsotan (GSFC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC & INAF-OAR), J. J. DeLaunay (PSU), P. A. Evans (U Leicester), R. A. J. Eyles-Ferris (U Leicester) and A. Melandri (INAF-OAR) report on behalf of the Neil Gehrels Swift Observatory Team: At 10:59:46 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 241209D (trigger=1273106). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 190.111, -2.879 which is RA(J2000) = 12h 40m 27s Dec(J2000) = -02d 52' 42" 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 150 sec. The peak count rate was ~3200 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 11:01:20.0 UT, 93.6 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 190.1129, -2.8901 which is equivalent to: RA(J2000) = 12h 40m 27.09s Dec(J2000) = -02d 53' 24.5" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 41 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial visibility window of the GRB was very short and no prompt UVOT data were generated. We await the full dataset to search for any UV/optical afterglow. Burst Advocate for this burst is T. M. Parsotan (tyler.parsotan 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 38491 table
GRB_name GRB241209D
GCN_number 38491
Detection_method Swift-XRT Det
ra 190.1119°
decl -2.8916°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38491 SUBJECT: GRB 241209D: Enhanced Swift-XRT position DATE: 24/12/09 14:11:43 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1140 s of XRT Photon Counting mode data and 4 UVOT images for GRB 241209D, 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 = 190.11190, -2.89162 which is equivalent to: RA (J2000): 12h 40m 26.86s Dec (J2000): -02d 53' 29.8" with an uncertainty of 2.8 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://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 38498 table
GRB_name GRB241209D
GCN_number 38498
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38498 SUBJECT: Swift GRB 241209D: Global MASTER-Net observations report DATE: 24/12/09 20:56:46 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-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 241209D ( T. M. Parsotan et al., GCN 38489) errorbox 33929 sec after notice time and 33951 sec after trigger time at 2024-12-09 20:25:37 UT, with upper limit up to 18.8 mag. The observations began at zenith distance = 75 deg. The sun altitude is -41.5 deg. The galactic latitude b = 60 deg., longitude l = 299 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2701233 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 34041 | MASTER-Tunka | C | 180 | 15.0 | 35265 | MASTER-Tunka | C | 180 | 18.8 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 38503 table
GRB_name GRB241209D
GCN_number 38503
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38503 SUBJECT: Fermi GRB 241209D: Global MASTER-Net observations report DATE: 24/12/09 21:46:04 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-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) started inspect of the Fermi GRB 241209D ( Fermi GBM team, GCN 38488) errorbox 33914 sec after notice time and 33953 sec after trigger time at 2024-12-09 20:25:37 UT, with upper limit up to 19.2 mag. The observations began at zenith distance = 75 deg. The sun altitude is -41.5 deg. The galactic latitude b = 60 deg., longitude l = 302 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2701308 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 34044 | 2024-12-09 20:25:37 | MASTER-Tunka | (12h 40m 42.72s , -02d 49m 30.7s) | C | 180 | 15.0 | 34224 | 2024-12-09 20:25:37 | MASTER-Tunka | (12h 40m 42.76s , -02d 49m 32.4s) | C | 540 | 19.2 | Coadd 35267 | 2024-12-09 20:46:01 | MASTER-Tunka | (12h 40m 48.04s , -02d 50m 25.9s) | C | 180 | 18.8 | 36758 | 2024-12-09 21:10:52 | MASTER-Tunka | (12h 40m 47.42s , -02d 47m 55.6s) | C | 180 | 19.0 | 37967 | 2024-12-09 21:31:01 | MASTER-Tunka | (12h 40m 42.47s , -02d 48m 50.9s) | C | 180 | 19.3 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 38505 table
GRB_name GRB241209D
GCN_number 38505
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 38505 SUBJECT: GRB 241209D: COLIBRÍ detection of the afterglow DATE: 24/12/09 22:12:33 GMT FROM: Damien Dornic J.-G. Ducoin (CPPM), Francesco Magnani (CPPM), Damien Dornic (CPPM), Alan M. Watson (UNAM), Margarita Pereyra (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), S. Antier (OCA), Jean-Luc Atteia (IRAP), Nathaniel R. Butler (ASU), Francis Fortin (IRAP) and Simona Lombardo (LAM), report: We imaged the field of GRB 241209D detected by Swift/BAT and Fermi/GBM (GCN Circ. 38488, 38489, 38491) during the commissioning of the COLIBRÍ (SVOM/F-GFT) telescope at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir in Mexico. The observations started 21 minutes after the GRB trigger. We observed with the engineering test camera in a red filter that approximates SDSS r. The data were reduced using custom software and then analysed and calibrated against the PS1 catalog using the STDWeb service (Karpov et al. 2022). In 4260 seconds of exposure from 2024/12/09 11:20:50 (UT) to 12:59:15, we detect the optical counterpart with: r = 20.04 +/-0.05 (SNR ~21.6) This source is right next to a catalogued galaxy in PAN-STARRs with rmag of ~21.44. Given the significant difference in magnitude and the slight visible offset with the PAN-STARRs object position, we consider this to be the Afterglow of GRB 241209D. We warmly thank the COLIBRI engineering team and the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir.
GCN 38507 table
GRB_name GRB241209D
GCN_number 38507
Detection_method Fermi GBM Det
t_trigger 10:59:44.090 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38507 SUBJECT: GRB 241209D: Fermi GBM Observation DATE: 24/12/09 22:50:55 GMT FROM: Christian Malacaria at INAF-OAR C. Malacaria (INAF-OAR) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 10:59:44.09 UT on 09 December 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241209D (trigger 755434789/241209458). which was also detected by Swift BAT (T. M. Parsotan et al. 2024, GCN 38489, M.R. Goad et al. 2024, GCN 38491). The Fermi GBM on-ground location is consistent with the Swift BAT position. The angle from the Fermi LAT boresight is 82 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 45 s (50-300 keV). The time-averaged spectrum from T0-0.8 to T0+44.3 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.40 +/- 0.07 and the cutoff energy, parameterized as Epeak, is 110 +/- 3 keV. The event fluence (10-1000 keV) in this time interval is (9.5 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+5.9 s in the 10-1000 keV band is 4.4 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 107 +/- 4 keV, alpha = -0.35 +/- 0.08 and beta = -3.4 +/- 0.6. 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 38508 table
GRB_name GRB241209D
GCN_number 38508
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38508 SUBJECT: GRB 241209D: Swift-XRT refined Analysis DATE: 24/12/10 00:31:53 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.4 ks of XRT data for GRB 241209D, from 260 s to 37.7 ks after the BAT trigger. The data comprise 22 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The light curve can be modelled with an initial power-law decay with an index of alpha=4.3 (+3.4, -2.5), followed by a break at T+626 s to an alpha of 0.66 (+/-0.13). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.89 (+0.29, -0.26). The best-fitting absorption column is 5.9 (+6.9, -3.6) x 10^20 cm^-2, consistent with the Galactic value of 2.3 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 3.5 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.9 (+6.9, -3.6) x 10^20 cm^-2 Galactic foreground: 2.3 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.89 (+0.29, -0.26) If the light curve continues to decay with a power-law decay index of 0.66, the count rate at T+24 hours will be 0.014 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.1 x 10^-13 (5.8 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/01273106. This circular is an official product of the Swift-XRT team.
GCN 38518 table
GRB_name GRB241209D
GCN_number 38518
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 38518 SUBJECT: GRB 241209D: AstroSat CZTI detection DATE: 24/12/10 09:10:32 GMT FROM: Gaurav Waratkar at IIT Bombay M. Tembhurnikar (IUCAA), G. Waratkar (IITB), A. Dasgupta (BITS Pilani, Hyderabad), J. Joshi (IUCAA), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 241209D which was also detected by Fermi/GBM (Fermi-GBM Team, GCN Circ. 38507), and Swift/BAT (Page et al., GCN Circ. 38508). The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-12-09 10:59:47.1 UTC. The measured peak count rate associated with the burst is 739 (+62, -67) counts/s above the background in the combined data of all quadrants, with a total of 9569 (+1176, -1291) counts. The local mean background count rate was 6618 (+7, -8) counts/s. We measure a T90 of 26 (+5, -6) s from the cumulative Veto light curve. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project. CZTI GRB detections are reported regularly on the payload site at: http://astrosat.iucaa.in/czti/?q=grb
GCN 38526 table
GRB_name GRB241209D
GCN_number 38526
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 38526 SUBJECT: Konus-Wind detection of GRB 241209D DATE: 24/12/10 14:55:58 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 241209D (Fermi-GBM detection: Fermi GBM team, GCN 38488; Malacaria & Meegan, GCN 38507; Swift-BAT detection: Parsotan et al., GCN 38489; AstroSat CZTI detection: Tembhurnikar et al., GCN 38518) was detected by Konus-Wind (KW) in the waiting mode. A Bayesian block analysis of the KW waiting mode data in the 20-300 keV band reveals a >13 sigma count rate increase in the interval from T0-2.0 s to T0+42.160 s where T0 = T0(BAT) = 10:59:45.649 UT. The KW light curve of this burst is available at http://www.ioffe.ru/LEA/GRBs/GRB241209D/ Modeling a time-integrated spectrum of the burst (from T0-2.0 s to T0+42.160 s) by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep): yields alpha = -1.16 (-0.37, +4.03) and Ep = 90(-12,+14) keV. The total burst fluence is 8.79(-0.87,+1.74)x10^-6 erg/cm^2, and the 2.944 s peak energy flux, measured from T0-2.0 s, is 5.86(-0.75,+1.25)x10^-7 erg/cm^2. (both in the 20 keV - 10 MeV energy range). All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary.
GCN 38527 table
GRB_name GRB241209D
GCN_number 38527
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38527 SUBJECT: GRB 241209D: REM optical/NIR upper limits DATE: 24/12/10 16:46:08 GMT FROM: Riccardo Brivio at INAF-OAB R.Brivio, M. Ferro, P. D’Avanzo, Y.-D. Hu, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team: We observed the field of GRB 241209D detected by Swift/BAT (Parsotan et al., GCN 38489) and Fermi/GBM (Fermi GBM team, GCN 38488) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, J, H, K bands, starting on 2024 December 10 at 06:54:39 UT (i.e. 19.9 hours after the Swift trigger), and lasting for about 1 hour. From preliminary photometry we do not detect the optical counterpart (Ducoin et al., GCN 38505) in the optical and NIR images at the Swift-XRT enhanced position (Goad et al., GCN 38491) down to the following 3sigma magnitude upper limits: r > 20.3 (AB; calibrated against the PanSTARRS catalogue) at a mid-time of t - t0 = 20.4 hr after the trigger, J > 18.1 (Vega; calibrated against the 2MASS catalogue) at a mid-time of t - t0 = 20.5 hr after the trigger.
GCN 38569 table
GRB_name GRB241209D
GCN_number 38569
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 38569 SUBJECT: GRB 241209D: CALET Gamma-Ray Burst Monitor detection DATE: 24/12/14 09:21:25 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University 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), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 241209D (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ 38488; Swift detection of a burst: Parsotan et al., GCN Circ 38489; Fermi GBM Observation: Malacaria et al., GCN Circ 38507; AstroSat CZTI detection: Tembhurnikar et al., GCN Circ 38518; Konus-Wind detection: Ridnaia et al., GCN Circ 38526) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 10:59:46.760 UTC on 9 December 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1417777157/index.html). The burst signal was seen by only the SGM detector. 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 pulse that starts at T-4.0 sec, peaks at T+0.6 sec, and ends at T+6.7 sec. The T90 and T50 durations measured by the SGM data are 9.2 +/- 0.7 sec and 4.6 +/- 0.4 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1417777157/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.
GCN 38589 table
GRB_name GRB241209D
GCN_number 38589
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 38589 SUBJECT: GRB 241209D: GRBAlpha detection DATE: 24/12/17 14:24:14 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa, M. Kolar (Masaryk U.), A. Pal (Konkoly Observatory), 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 241209D (Fermi/GBM detection: GCN 38488; Swift/BAT detection: GCN 38489; AstroSat/CZTI detection: GCN 38518; Konus/Wind detection: GCN 38526; CALET/CGBM detection: GCN 38569) 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 2024-12-09 10:59:45.2 UTC. The T90 duration measured by GRBAlpha is 52 s and the overall significance during T90 reaches 11 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB241209D_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.