GRB241229B

This page lists all entries on GRB241229B in GRBweb

Summary Fermi GBM IPN Swift GCN 38698 GCN 38699 GCN 38706 GCN 38708 GCN 38710 GCN 38712 GCN 38717 GCN 38721 GCN 38729 GCN 38732 GCN 38734 GCN 38738 GCN 38746

Summary table
Variable Value Source
GRB_name_Fermi GRB241229067
T0 1:36:12.992 UTC Fermi_GBM
ra 274.1761° Swift
decl 74.6833° Swift
pos_error 8.80e-04° Swift
T90 5.888 s Fermi_GBM
T90_error 1.864 s Fermi_GBM
T90_start 1:36:12.992 UTC Fermi_GBM
fluence 1.30e-06 erg/cm² Fermi_GBM
fluence_error 2.04e-08 erg/cm² Fermi_GBM
T100 5.888 s
GBM_located False
mjd 60673.06681703703 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB241229067
trigger_name bn241229067
ra 274.1492°
decl 74.7139°
pos_error 4.68e+00°
datum 2024-12-29
t_trigger 1:36:16.064 UTC
T90 5.888 s
T90_error 1.864 s
T90_start 1:36:12.992 UTC
fluence 1.30e-06 erg/cm²
fluence_error 2.04e-08 erg/cm²
flux_1024 6.17e+00 erg/cm²/s
flux_1024_error 2.66e-01 erg/cm²/s
flux_1024_time 6.40e-02 erg/cm²/s
flux_64 7.86e+00 erg/cm²/s
flux_64_error 1.19e+00 erg/cm²/s
IPN table
GRB_name GRB241229B
ra 274.1500°
decl 74.7167°
pos_error 5.00e-02°
Swift table
GRB_name GRB241229B
t_trigger 4:13:05 UTC
ra 274.1761°
decl 74.6833°
pos_error 8.80e-04°
T90 5.05 s
fluence 7.00e-07 erg/cm²
GCN 38698 table
GRB_name GRB241229B
GCN_number 38698
Detection_method Fermi GBM final loc
t_trigger 1:36:16 UTC
ra 275.0000°
decl 62.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38698 SUBJECT: GRB 241229B: Fermi GBM Final Real-time Localization DATE: 24/12/29 01:46:54 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 01:36:16 UT on 29 Dec 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241229B (trigger 757128981.063788 / 241229067). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 275.0, Dec = 62.4 (J2000 degrees, equivalent to J2000 18h 19m, 62d 23'), with a statistical uncertainty of 6.1 degrees. The angle from the Fermi LAT boresight is 27.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241229067/quicklook/glg_skymap_all_bn241229067.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/bn241229067/quicklook/glg_healpix_all_bn241229067.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241229067/quicklook/glg_lc_medres34_bn241229067.gif
GCN 38699 table
GRB_name GRB241229B
GCN_number 38699
Detection_method Swift Det
t_trigger 1:36:15 UTC
ra 274.1490°
decl 74.7140°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38699 SUBJECT: GRB 241229B: Swift detection of a burst DATE: 24/12/29 01:52:48 GMT FROM: Amy A. D'Ai (INAF-IASFPA), S. Dichiara (PSU), R. Gupta (NASA GSFC), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), A. Y. Lien (U Tampa) and T. M. Parsotan (GSFC) report on behalf of the Neil Gehrels Swift Observatory Team: At 01:36:15 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 241229B (trigger=1277428). Swift did not slew immediately to the burst. The BAT on-board calculated location is RA, Dec 274.149, +74.714 which is RA(J2000) = 18h 16m 36s Dec(J2000) = +74d 42' 50" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 10 sec. The peak count rate was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to an observing constraint, Swift cannot slew to the BAT position. There will thus be no XRT or UVOT data for this trigger. Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it). 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 38706 table
GRB_name GRB241229B
GCN_number 38706
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38706 SUBJECT: Swift GRB 241229B: Global MASTER-Net observations report DATE: 24/12/29 11:26:26 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 241229B ( A. D'Ai et al., GCN 38699) errorbox 34817 sec after notice time and 34851 sec after trigger time at 2024-12-29 11:17:07 UT, with upper limit up to 19.3 mag. The observations began at zenith distance = 43 deg. The sun altitude is -19.1 deg. The galactic latitude b = 28 deg., longitude l = 106 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2725189 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 34941 | MASTER-Tunka | C | 180 | 19.3 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 38708 table
GRB_name GRB241229B
GCN_number 38708
Detection_method Swift-XRT Other
ra 274.1761°
decl 74.6833°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38708 SUBJECT: GRB 241229B: Swift-XRT refined Analysis DATE: 24/12/29 14:06:47 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: We have analysed 2.7 ks of XRT data for GRB 241229B, from 23.5 ks to 34.3 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 274.1761, +74.6833 which is equivalent to: RA (J2000): 18 16 42.26 Dec(J2000): +74 40 60.0 with an uncertainty of 6.8 arcsec (radius, 90% confidence). The source has a mean count rate of 1.4e-02 ct/sec; we cannot determine at the present time whether it is fading. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01277428. This circular is an official product of the Swift-XRT team.
GCN 38710 table
GRB_name GRB241229B
GCN_number 38710
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 38710 SUBJECT: GRB 241229B: NUTTelA-TAO / BSTI Optical Limits DATE: 24/12/29 16:53:38 GMT FROM: Toktarkhan Komesh at Nazarbayev University T. Komesh (NU), Z. Abdullayev (NU), Z. Maksut (NU), B. Grossan (UCB, NU), D. Berdikhan (NU), M. Krugov (FAI) and E. Abdikamalov (NU) report on behalf of the Energetic Cosmos Laboratory: The Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) pointed at GRB 241229B on receipt of an automated GCN / BAT position alert, observing in Sloan g' and r' bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14). We started observations at 01:37:16 UT on 2024-12-29, 61 s after the BAT trigger. Observations were made in partly cloudy conditions. No source consistent with the XRT (P.A. Evans et al., GCN Circ. 38708) was detected. We report the following results: start time t-t0(s) end time UL g' UL r' exposure_time (s) -------------------------------------------------------------- 01:37:16 61 1:37:41 - 16.67 25 01:38:25 135 1:40:25 16.21 17.35 120 The start and end time is in UT. t is the middle time, t0 is the BAT trigger time, t-t0 is given in seconds. UL gives the 5 sigma upper limit sensitivity in magnitudes, for images co-added to the given exposure time. The first row in the table corresponds to co-adds of an initial short exposure image sequence of 1 s (these sub-second exposures are read-noise suppressed by our EMCCD cameras, with high gain electron multiplication active; other images are taken in conventional CCD operation mode) for r'. The second row corresponds to co-adds from a continuing series of 15 s exposures for g' and r’. Calibration was done with 3 Pan-STARRS catalog stars on our images. No color or other corrections were applied to the values above. ---------------------------------- NU = Nazarbayev University, Astana, Kazakhstan UCB = University of California, Berkeley, USA FAI = Fesenkov Astrophysical Institute, Kazakhstan This research has been funded by the Science Committee of the Ministry of Science and Higher Education of the Republic of Kazakhstan (Grant No. AP14870504). The NUTTelA-TAO Team acknowledges the support of the staff of the Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazkhstan.
GCN 38712 table
GRB_name GRB241229B
GCN_number 38712
Detection_method Fermi GBM Det
t_trigger 1:36:16.060 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38712 SUBJECT: GRB 241229B: Fermi GBM Observation DATE: 24/12/29 18:21:40 GMT FROM: Peter Veres at University of Alabama in Huntsville Peter Veres (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 01:36:16.06 UT on 29 December 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241229B (trigger 757128981/241229067). which was also detected by Swift BAT (H. A. Krimm et al. 2024, GCN 38699). The Fermi GBM on-ground location is consistent with the Swift BAT position. The angle from the Fermi LAT boresight is 39 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 6 s (50-300 keV). The time-averaged spectrum from T0-5.1 to T0+4.1 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.7 +/- 0.2 and the cutoff energy, parameterized as Epeak, is 76 +/- 5 keV. The event fluence (10-1000 keV) in this time interval is (1.24 +/- 0.06)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 6.1 +/- 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 38717 table
GRB_name GRB241229B
GCN_number 38717
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 38717 SUBJECT: GRB241229B: UVOT upper limits DATE: 24/12/29 23:57:41 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and A. D'Ai (INAF-IASFPA SSDC) report on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the field of GRB 241229B 6.5 hours after the BAT trigger due to an observing constraint (D'Elia et al., GCN Circ. 38699). No optical afterglow consistent with the XRT position (Evans, GCN Circ. no 38708) was detected with UVOT. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag b 23500 39885 1686 >21.5 uvw1 27820 45505 1800 >21.0 u 28727 45738 404 >20.3 uvw2 33481 51179 1800 >21.2 v 34386 51381 376 >20.0 white 39890 40021 132 >20.9 b 55868 56383 254 >20.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.06 in the direction of the burst (Schlegel et al. 1998).
GCN 38721 table
GRB_name GRB241229B
GCN_number 38721
Detection_method Swift-BAT Det
ra 274.1400°
decl 74.6940°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38721 SUBJECT: GRB 241229B: Swift-BAT refined analysis DATE: 24/12/30 05:50:24 GMT FROM: Amy S. D. Barthelmy (GSFC), D'Ai (INAF-IASFPA), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (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 241229B (trigger #1277428) (D'Ai et al., GCN Circ. 38699). The BAT ground-calculated position is RA, Dec = 274.140, 74.694 deg which is RA(J2000) = 18h 16m 33.5s Dec(J2000) = +74d 41' 39.5" with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 39%. The mask-weighted light curve shows several overlapping pulses that start at ~T-3 s and end at ~T+3 s. The main peak occurs at ~T+0.5 s, T90 (15-350 keV) is 5.05 +- 0.65 sec (estimated error including systematics). The time-averaged spectrum from T-2.62 to T+3.38 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.93 +- 0.50, and Epeak of 68.3 +- 22.6 keV (chi squared 47.78 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 7.0 +- 0.6 x 10^-07 erg/cm2 and the 1-sec peak flux measured from T-0.06 sec in the 15-150 keV band is 4.0 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.70 +- 0.11 (chi squared 55.86 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/1277428
GCN 38729 table
GRB_name GRB241229B
GCN_number 38729
Detection_method Optical
ra 274.1803°
decl 74.6851°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38729 SUBJECT: GRB 241229B: SVOM/VT optical candidate DATE: 24/12/30 16:15:59 GMT FROM: SVOM_group SVOM/VT commissioning team: Y. L. Qiu, H. L. Li (NAOC), A. Li (BNU), Y. F. Liang (PMOC), L. P. Xin, C. Wu, X. H. Han, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. Deng, L. Lan, X. M. Lu, R. S. Zhang, Z. H. Yao (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (IHEP), Bing Zhang (UNLV) report on behalf of the SVOM team: The SVOM/VT conducted a ToO follow-up observations of the Fermi (GCN 38698) and Swift triggered GRB 241229B (GCN 38699) in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously, from 12.09 hours to 15.5 hours after the burst. A new optical source was detected within the errorbox of XRT (GCN 38708) in VT_R stacked image, compared to the PanSTARRS catalog. The brightness of the source was estimated to be 21.8 ± 0.1 mag in AB magnitude in VT_R image at the mid time of 13.8 hours post the burst, with a total exposure time of 34*60 seconds. The source was not detected in VT_B stacked image with 3 sigma upper limit of ~23.2 mag in AB magnitude. The source is located at RA, Dec = 274.1803, 74.6851 deg, which is equivalent to: RA (J2000) : 18:16:43.271 Dec (J2000): +74:41:06.04 with an uncertainty of 0.5 arcsec. We do not confirm the fading of the source, but which might be the candidate for the gamma-ray burst. More deep follow-ups are encouraged for the nature of the source. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC),CAS.
GCN 38732 table
GRB_name GRB241229B
GCN_number 38732
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38732 SUBJECT: GRB 241229B: CrAO ZTSh possible optical counterpart of SVOM/VT confirmation DATE: 24/12/30 20:16:39 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), A. Pozanenko (IKI), V. Rumyantsev (CrAO), N. Pankov (HSE, IKI) report on behalf of GRB-IKI-FuN collaboration: We observed the GRB 241229B (Fermi GBM Team, GCN 38698; D'Ai et al., GCN 38699) with 2.6-meter ZTSh telescope of CrAO. The observations started on 2024-12-29 (UT) 20:22:02, i.e. ~15.4 hours after GBM trigger. We clearly detected SVOM/VT optical candidate (SVOM/VT team, GCN 38729). The preliminary photometry of the the optical candidate is the following: Date UT start T0+ Exp. Filter OT Err. UL(3sigma) (mid, days) (s) 2024-12-29 20:22:02 0.64631 88x120 R 21.91 0.05 24.2 The magnitudes are calibrated using nearby Pan-Starrs PS1 (transformed into R by Lupton's transformations) RA Dec R_Lupton 18:16:50.10 +74:41:42.2 18.928 +- 0.020 18:16:33.99 +74:41:43.6 18.778 +- 0.026 18:16:26.64 +74:41:33.2 17.917 +- 0.014
GCN 38734 table
GRB_name GRB241229B
GCN_number 38734
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38734 SUBJECT: GRB 241229B: SAO RAS optical upper limit DATE: 24/12/30 21:20:15 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin, O. I. Spiridonova (SAO RAS), A. A. Volnova and A. S. Pozanenko (IKI RAS) report on behalf of the GRB follow-up team. We observed the field of GRB 241229B (Fermi GBM Team, GCN 38698; D'Ai et al., GCN 38699) with the 1-m telescope of SAO RAS, Zeiss-1000 equipped with the CCD-photometer on December 30, 14:47:58--16:04:24 UT, t_mid - T0 = 1.5763 days. We obtained 12 x 300 sec. images in Rc band. In the stacked image we did not detected OT discovered by SVOM/VT team (GCN 38729) and confirmed by Volnova et al., (GCN 38732) down to the limiting magnitude of R_lim = 22.3 (based on the same nearby PS1 stars, magnitudes were converted with the Lupton 2005 equations).
GCN 38738 table
GRB_name GRB241229B
GCN_number 38738
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 38738 SUBJECT: GRB 241229B: SVOM/GRM observation DATE: 24/12/31 08:11:34 GMT FROM: Yue Wang SVOM/GRM team: Yue Wang, Chen-Wei Wang, Shi-Jie Zheng, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP), report on behalf of the SVOM team: The SVOM/GRM was triggered in-flight by GRB 241229B (SVOM trigger reference: sb24122902) at 2024-12-29T01:36:17.000 UT (T0), which was also observed by Fermi/GBM (Fermi GBM Team, GCN 38698) and Swift/BAT (A. D'Ai et al, GCN 38699). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of one main pulse with a T90 of 5.45 +0.76/-1.01 s This burst is located (from Swift/BAT) at about 57.10 degrees from the SVOM optical axis, and outside the ECLAIRs field of view. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241229B.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM point of contact for this burst is: Yue Wang (IHEP)(yuewang@ihep.ac.cn)
GCN 38746 table
GRB_name GRB241229B
GCN_number 38746
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38746 SUBJECT: GRB 241229B: Continued CrAO ZTSh observations DATE: 24/12/31 23:03:47 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Volnova (IKI), A. Pozanenko (IKI), V. Rumyantsev (CrAO), report on behalf of the IKI-GRB-FuN collaboration: We observed the field of GRB 241229B (Fermi GBM Team, GCN 38698; D'Ai et al., GCN 38699) with 2.6-meter ZTSh telescope of CrAO. The observations started on 2024-12-30 (UT) 18:30, i.e. ~1.73 days since GBM trigger. The series of 30x120 s images were obtained using the CCD-photometer. The optical counterpart (SVOM/VT team, GCN 38729; Volnova et. al, GCN 38732) has been detected in a stacked image. Preliminary photometry is the following: Date UTstart T-T0 Exp. Filter OT Err. UL(3sigma) (mid, days) (s) 2024-12-30 18:13:33 1.73423 30x120 R 23.40 0.15 24.0 The photometry has been calibrated against nearby PS1 stars (see Volnova et. al, GCN 38732).