GRB 241204A
GCN Circular 38436
Subject
GRB 241204A: Fermi-LAT detection
Date
2024-12-04T09:26:19Z (6 months ago)
From
Elisabetta Bissaldi at Politecnico and INFN Bari <elisabetta.bissaldi@ba.infn.it>
Via
Web form
E. Bissaldi (Politecnico and INFN Bari), A. Holzmann Airasca (UniTrento and INFN Bari)
and T. Khalil (Johannesburg Univ) report on behalf of the Fermi-LAT Collaboration:
On Dec 4, 2024, Fermi-LAT detected high-energy emission from GRB 241204A,
which was also detected by Fermi-GBM (trigger 754976367 / 241204.152).
The best LAT on-ground location is found to be:
RA, Dec = 316.50, 6.55 (J2000),
with an error radius of 0.5 deg (90 % containment, statistical error only).
This was 26 deg from the LAT boresight at the time of the GBM trigger (T0 = 03:39:22.51 UT).
The data from the Fermi-LAT show a significant increase in the event rate
that is spatially and temporally correlated with the GBM emission
with high significance.
The photon flux above 100 MeV in the time interval 0 - 350 s after the GBM trigger
is (1.7 +/- 0.4) E-5 ph/cm2/s.
The estimated photon index above 100 MeV is 2.8 +/- 0.4.
The highest-energy photon is a 260 MeV event which is observed ~16 seconds after the GBM trigger.
The Fermi-LAT point of contact for this burst is Tamador Khalil (tamtam2030@gmail.com).
The Fermi-LAT is a pair conversion telescope designed to cover
the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.
GCN Circular 38440
Subject
Fermi GRB 241204A: Global MASTER-Net observations report
Date
2024-12-04T16:30:42Z (6 months ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 241204A ( E. Bissaldi et al., GCN 38436) errorbox 39000 sec after notice time and 40326 sec after trigger time at 2024-12-04 14:51:28 UT, with upper limit up to 19.8 mag. Observations started at twilight. The observations began at zenith distance = 41 deg. The sun altitude is -13.4 deg.
The galactic latitude b = -26 deg., longitude l = 53 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2695247
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
40356 | 2024-12-04 14:51:28 | MASTER-Kislovodsk | (21h 05m 11.61s , +06d 39m 14.6s) | C | 60 | 17.3 |
40617 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.85s , +06d 36m 35.4s) | C | 60 | 17.7 |
40677 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.85s , +06d 36m 35.3s) | C | 180 | 18.4 | Coadd
41157 | 2024-12-04 14:55:49 | MASTER-Kislovodsk | (21h 05m 10.84s , +06d 36m 35.4s) | C | 1140 | 19.8 | Coadd
40697 | 2024-12-04 14:57:09 | MASTER-Kislovodsk | (21h 05m 17.71s , +06d 36m 52.8s) | C | 60 | 17.8 |
40776 | 2024-12-04 14:58:28 | MASTER-Kislovodsk | (21h 05m 13.79s , +06d 38m 06.3s) | C | 60 | 17.7 |
40856 | 2024-12-04 14:59:48 | MASTER-Kislovodsk | (21h 05m 14.85s , +06d 36m 37.2s) | C | 60 | 17.8 |
40976 | 2024-12-04 14:59:48 | MASTER-Kislovodsk | (21h 05m 14.85s , +06d 36m 37.1s) | C | 300 | 19.0 | Coadd
40966 | 2024-12-04 15:01:08 | MASTER-Kislovodsk | (21h 05m 17.13s , +06d 38m 07.3s) | C | 120 | 18.4 |
41105 | 2024-12-04 15:03:27 | MASTER-Kislovodsk | (21h 05m 12.10s , +06d 37m 15.1s) | C | 120 | 18.5 |
41245 | 2024-12-04 15:05:47 | MASTER-Kislovodsk | (21h 05m 11.16s , +06d 38m 11.1s) | C | 120 | 18.4 |
41365 | 2024-12-04 15:05:47 | MASTER-Kislovodsk | (21h 05m 11.16s , +06d 38m 11.1s) | C | 360 | 19.2 | Coadd
41385 | 2024-12-04 15:08:07 | MASTER-Kislovodsk | (21h 05m 18.09s , +06d 37m 07.3s) | C | 120 | 18.5 |
41525 | 2024-12-04 15:10:27 | MASTER-Kislovodsk | (21h 05m 11.35s , +06d 36m 04.7s) | C | 120 | 18.5 |
41665 | 2024-12-04 15:12:47 | MASTER-Kislovodsk | (21h 05m 18.32s , +06d 36m 12.3s) | C | 120 | 18.6 |
41725 | 2024-12-04 15:12:47 | MASTER-Kislovodsk | (21h 05m 18.32s , +06d 36m 12.3s) | C | 240 | 19.0 | Coadd
41774 | 2024-12-04 15:15:06 | MASTER-Kislovodsk | (21h 05m 14.44s , +06d 37m 37.2s) | C | 60 | 18.0 |
41854 | 2024-12-04 15:16:26 | MASTER-Kislovodsk | (21h 05m 15.52s , +06d 36m 04.1s) | C | 60 | 18.0 |
41934 | 2024-12-04 15:17:46 | MASTER-Kislovodsk | (21h 05m 18.53s , +06d 37m 41.4s) | C | 60 | 18.0 |
42114 | 2024-12-04 15:17:46 | MASTER-Kislovodsk | (21h 05m 18.51s , +06d 37m 41.2s) | C | 420 | 19.5 | Coadd
42073 | 2024-12-04 15:19:05 | MASTER-Kislovodsk | (21h 05m 12.75s , +06d 36m 52.9s) | C | 180 | 18.8 |
42273 | 2024-12-04 15:22:25 | MASTER-Kislovodsk | (21h 05m 11.88s , +06d 37m 48.3s) | C | 180 | 18.8 |
42473 | 2024-12-04 15:25:45 | MASTER-Kislovodsk | (21h 05m 18.89s , +06d 36m 44.0s) | C | 180 | 18.8 |
43655 | 2024-12-04 15:46:27 | MASTER-Kislovodsk | (20h 46m 30.15s , +05d 04m 06.4s) | C | 60 | 17.7 |
44775 | 2024-12-04 16:05:07 | MASTER-Kislovodsk | (20h 54m 32.68s , +05d 03m 31.1s) | C | 60 | 17.5 |
44855 | 2024-12-04 16:06:27 | MASTER-Kislovodsk | (20h 46m 28.95s , +05d 04m 25.4s) | C | 60 | 17.8 |
44935 | 2024-12-04 16:07:47 | MASTER-Kislovodsk | (20h 54m 29.51s , +05d 02m 58.9s) | C | 60 | 17.7 |
45014 | 2024-12-04 16:09:06 | MASTER-Kislovodsk | (20h 46m 31.91s , +05d 04m 23.6s) | C | 60 | 17.8 |
45154 | 2024-12-04 16:10:26 | MASTER-Kislovodsk | (20h 58m 42.92s , +03d 10m 49.9s) | C | 180 | 18.2 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 38441
Subject
GRB 241204A: Fermi GBM Observation
Date
2024-12-04T21:07:30Z (6 months ago)
From
Matt Godwin <msg0028@uah.edu>
Via
Web form
Matt Godwin (UAH), E. Bissaldi (Politecnico and INFN Bari), and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 03:39:22.51 UT on 04 December 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 241204A (trigger 754976367/241204152).
which was also detected by Fermi-LAT (E. Bissaldi et al. 2024, GCN 38436).
The Fermi GBM on-ground location is consistent with the Fermi-LAT position.
The angle from the Fermi LAT boresight is 26 degrees.
The GBM light curve consists of two peaks with a duration (T90)
of about 0.8 s (50-300 keV). The time-averaged spectrum
from T0-0.4 to T0+1.0 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.31 +/- 0.04 and the cutoff energy,
parameterized as Epeak, is 3453 +/- 1070 keV.
The event fluence (10-1000 keV) in this time interval is
(2.22 +/- 0.09)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.64 s in the 10-1000 keV band is 41 +/- 2 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 Circular 38442
Subject
GRB 241204A: DDOTI Upper Limits on the Afterglow
Date
2024-12-05T11:40:03Z (6 months ago)
From
Rosa L. Becerra at Tor Vergata, Roma <rosa.becerra@roma2.infn.it>
Via
Web form
Rosa L. Becerra (Tor Vergata, Roma), Alan M. Watson (UNAM), Eleonora Troja (Tor Vergata, Roma), Camila Angulo Valdez (UNAM), Nat Butler (ASU), Simone Dichiara (Penn State University), Tsvetelina Dimitrova (ASU), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), Océlotl López (UNAM), and Margarita Pereyra (UNAM) report:
We observed the field of the GRB 241204A detected by Fermi/LAT (Bissaldi et al., GCN [38436](https://gcn.nasa.gov/circulars/38436)) and Fermi/GBM (Godwin et al., GCN 38441) with the DDOTI/OAN wide-field imager at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir (http://ddoti.astroscu.unam.mx) on 2024-12-05 from 02:29 to 03:54 UTC (22.83 to 24.25 hrs after the event), obtaining a total of 48 minutes of exposure in the w filter down to a 10-sigma limiting magnitude of w = 20.6.
Comparing our observations to the USNO-B1 and PanSTARRS PS1 DR2 catalogues, we
detect no uncatalogued sources within the observed field to our 10-sigma limit within the error radius reported by Fermi/LAT (Bissaldi et al., GCN 38436).
We thank the DDOTI technical team and the staff of the Observatorio Astronómico Nacional.
GCN Circular 38445
Subject
GRB 241204A: COLIBRÍ Optical Upper Limit
Date
2024-12-05T21:16:51Z (6 months ago)
From
Dornic Damien <dornicdamien@gmail.com>
Via
Web form
Francesco Magnani (CPPM), J.-G. Ducoin (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), Simona Lombardo (LAM), and report:
We imaged the field of GRB 241204A detected by Fermi/LAT (Bissaldi et al., GCN 38436) and Fermi/GBM (Godwin et al., GCN 38441) 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 23.9 hours after the GRB trigger. We obtained 1200 seconds of exposure with the engineering test camera in a red filter that approximates SDSS r. The observation covers 13 arcmin field of view centered to the LAT coordinates. The data were reduced using custom software and then analysed and calibrated against the PS1 catalog using the STDWeb service (Karpov et al. 2022).
We estimate an upper limit of 20.6 mag (10 sigma). This limiting magnitude is consistent with other optical observations of MASTER (Lipunov et al., GCN Circ. 38440) and DDOTI (Becerra et al., GCN Circ. 38442).
We warmly thank the COLIBRI engineering team and the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir.
GCN Circular 38631
Subject
Konus-Wind detection of GRB 241204A (short/hard)
Date
2024-12-19T08:22:13Z (5 months ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
Web form
V. Panteleeva, D. Frederiks, A. Lysenko, A. Ridnaia,
D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The short-duration GRB 241204A
(Fermi-LAT detection: Bissaldi et al., GCN 38436;
Fermi-GBM detection: Godwin et al., GCN 38441)
triggered Konus-Wind at T0=13159.909 s UT (03:39:19.909).
The burst light curve shows a single pulse
which starts at ~T0 and has a total duration of ~0.1 s.
The emission is seen up to ~7 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB241204_T13159/
As observed by Konus-Wind, the burst
had a fluence of 6.20(-1.01,+1.11)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.004 s,
of 1.45(-0.34,+0.37)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+0.064 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 = -1.22(-0.11,+0.12)
and Ep = 3550(-1308,+4267) keV (pgstat = 62/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.62
(pgstat = 62/72 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.