GRB240204A

This page lists all entries on GRB240204A in GRBweb

Summary Fermi GBM IPN Swift GCN 35664 GCN 35666 GCN 35668 GCN 35670 GCN 35671 GCN 35673 GCN 35677 GCN 35680 GCN 35688 GCN 35690 GCN 35691 GCN 35692 GCN 35705 GCN 35714 GCN 35922

Summary table
Variable Value Source
GRB_name_Fermi GRB240204630
T0 15:07:38 UTC GCN_circulars,Fermi GBM final loc
ra 104.1815° Swift
decl 1.0267° Swift
pos_error 2.85e-04° Swift
T90 15.872 s Fermi_GBM
T90_error 0.81 s Fermi_GBM
T90_start 15:07:40.213 UTC Fermi_GBM
fluence 1.59e-05 erg/cm² Fermi_GBM
fluence_error 4.31e-08 erg/cm² Fermi_GBM
T100 18.085 s
GBM_located False
mjd 60344.63030092593 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB240204630
trigger_name bn240204630
ra 101.5000°
decl -3.4100°
pos_error 2.65e+00°
datum 2024-02-04
t_trigger 15:07:38.677 UTC
T90 15.872 s
T90_error 0.81 s
T90_start 15:07:40.213 UTC
fluence 1.59e-05 erg/cm²
fluence_error 4.31e-08 erg/cm²
flux_1024 3.29e+01 erg/cm²/s
flux_1024_error 5.13e-01 erg/cm²/s
flux_1024_time 1.21e+01 erg/cm²/s
flux_64 3.68e+01 erg/cm²/s
flux_64_error 2.14e+00 erg/cm²/s
IPN table
GRB_name GRB240204A
ra 104.1833°
decl 1.0333°
pos_error 5.00e-02°
Swift table
GRB_name GRB240204A
t_trigger 15:07:38 UTC
ra 104.1815°
decl 1.0267°
pos_error 2.85e-04°
GCN 35664 table
GRB_name GRB240204A
GCN_number 35664
Detection_method Fermi GBM final loc
t_trigger 15:07:38 UTC
ra 101.5000°
decl -3.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35664 SUBJECT: GRB 240204A: Fermi GBM Final Real-time Localization DATE: 24/02/04 15:18:07 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 15:07:38 UT on 4 Feb 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240204A (trigger 728752063.677018 / 240204630). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 101.5, Dec = -3.4 (J2000 degrees, equivalent to J2000 06h 46m, -3d 23'), with a statistical uncertainty of 1.6 degrees. The angle from the Fermi LAT boresight is 102.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240204630/quicklook/glg_skymap_all_bn240204630.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/bn240204630/quicklook/glg_healpix_all_bn240204630.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240204630/quicklook/glg_lc_medres34_bn240204630.gif
GCN 35666 table
GRB_name GRB240204A
GCN_number 35666
Detection_method Swift Det
t_trigger 15:10:12.200 UTC
ra 104.1819°
decl 1.0277°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35666 SUBJECT: GRB 240204A: Swift detection of a burst DATE: 24/02/04 15:33:54 GMT FROM: K.L. Page at U Leicester S. B. Cenko (GSFC), C. Gronwall (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU) and K. L. Page (U Leicester) report on behalf of the Neil Gehrels Swift Observatory Team: Swift/BAT triggered on the Fermi/GBM reported long GRB 240204A (GCN #35664). Due to a telemetry outage, no realtime BAT data are available. The XRT began observing the field at 15:10:12.2 UT, 154 seconds after the Fermi/GBM trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 104.18190, 1.02767 which is equivalent to: RA(J2000) = 06h 56m 43.66s Dec(J2000) = +01d 01' 39.6" with an uncertainty of 4.0 arcseconds (radius, 90% containment). This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 6.45 x 10^21 cm^-2 (Willingale et al. 2013). Due to a telemetry outage, there are no UVOT data available at this time. Burst Advocate for this burst is S. B. Cenko (brad.cenko 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 35668 table
GRB_name GRB240204A
GCN_number 35668
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35668 SUBJECT: Fermi GRB 240204A: Global MASTER-Net observations report DATE: 24/02/04 16:15:52 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) started inspect of the Fermi GRB 240204A ( Fermi GBM team, GCN 35664) errorbox 818 sec after notice time and 854 sec after trigger time at 2024-02-04 15:21:52 UT, with upper limit up to 20.8 mag. The observations began at zenith distance = 54 deg. The sun altitude is -48.0 deg. The galactic latitude b = -2 deg., longitude l = 216 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2371241 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 884 | 2024-02-04 15:21:52 | MASTER-Tunka | (06h 45m 43.71s , -03d 13m 03.5s) | C | 60 | 19.9 | 944 | 2024-02-04 15:21:52 | MASTER-Tunka | (06h 45m 43.71s , -03d 13m 03.5s) | C | 180 | 20.4 | Coadd 1154 | 2024-02-04 15:21:52 | MASTER-Tunka | (06h 45m 43.71s , -03d 13m 03.5s) | C | 600 | 20.8 | Coadd 947 | 2024-02-04 15:22:56 | MASTER-Tunka | (06h 45m 43.78s , -03d 13m 01.1s) | C | 60 | 19.9 | 1011 | 2024-02-04 15:23:59 | MASTER-Tunka | (06h 45m 43.83s , -03d 12m 59.8s) | C | 60 | 19.9 | 1074 | 2024-02-04 15:25:02 | MASTER-Tunka | (06h 45m 43.88s , -03d 12m 57.8s) | C | 60 | 19.9 | 1134 | 2024-02-04 15:25:02 | MASTER-Tunka | (06h 45m 43.88s , -03d 12m 57.9s) | C | 180 | 20.4 | Coadd 1201 | 2024-02-04 15:27:09 | MASTER-Tunka | (06h 45m 44.01s , -03d 12m 54.0s) | C | 60 | 19.8 | 1264 | 2024-02-04 15:28:12 | MASTER-Tunka | (06h 45m 44.05s , -03d 12m 52.5s) | C | 60 | 19.9 | 1327 | 2024-02-04 15:29:15 | MASTER-Tunka | (06h 45m 44.14s , -03d 12m 50.2s) | C | 60 | 19.9 | 1387 | 2024-02-04 15:29:15 | MASTER-Tunka | (06h 45m 44.14s , -03d 12m 50.2s) | C | 180 | 20.4 | Coadd 1454 | 2024-02-04 15:31:22 | MASTER-Tunka | (06h 45m 44.31s , -03d 12m 46.5s) | C | 60 | 19.8 | 1522 | 2024-02-04 15:32:30 | MASTER-Tunka | (06h 45m 49.39s , -03d 12m 38.6s) | C | 60 | 19.9 | 1585 | 2024-02-04 15:33:33 | MASTER-Tunka | (06h 45m 49.44s , -03d 12m 36.0s) | C | 60 | 20.0 | 1645 | 2024-02-04 15:33:33 | MASTER-Tunka | (06h 45m 49.44s , -03d 12m 36.0s) | C | 180 | 20.5 | Coadd 1648 | 2024-02-04 15:34:37 | MASTER-Tunka | (06h 45m 49.50s , -03d 12m 34.2s) | C | 60 | 20.0 | 1712 | 2024-02-04 15:35:40 | MASTER-Tunka | (06h 45m 49.57s , -03d 12m 32.2s) | C | 60 | 20.0 | 1775 | 2024-02-04 15:36:43 | MASTER-Tunka | (06h 45m 49.60s , -03d 12m 30.7s) | C | 60 | 20.0 | 1835 | 2024-02-04 15:36:43 | MASTER-Tunka | (06h 45m 49.61s , -03d 12m 30.8s) | C | 180 | 20.5 | Coadd 1838 | 2024-02-04 15:37:46 | MASTER-Tunka | (06h 45m 49.68s , -03d 12m 29.1s) | C | 60 | 20.1 | 1901 | 2024-02-04 15:38:50 | MASTER-Tunka | (06h 45m 49.73s , -03d 12m 27.3s) | C | 60 | 20.0 | 1965 | 2024-02-04 15:39:53 | MASTER-Tunka | (06h 45m 49.77s , -03d 12m 25.3s) | C | 60 | 20.0 | 2028 | 2024-02-04 15:40:56 | MASTER-Tunka | (06h 45m 49.82s , -03d 12m 23.8s) | C | 60 | 20.0 | 2091 | 2024-02-04 15:41:59 | MASTER-Tunka | (06h 45m 49.86s , -03d 12m 21.8s) | C | 60 | 20.0 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 35670 table
GRB_name GRB240204A
GCN_number 35670
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35670 SUBJECT: GRB 240204A: Mondy optical afterglow candidate DATE: 24/02/04 18:05:52 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov (HSE, IKI), S. Belkin (IKI, HSE) report on behalf of IKI-GRB-FuN: We observed the field of Swift localization of GRB 240204A (Cenko et al., GCN 35666) which is also detected be GMB/Fermi (Fermi GBM team GCN 35664) with AZT-33IK telescope of Mondy observatory starting on 2024-02-04 (UT) 16:05:26. In the first images of 60 s exposure we detected the object in coordinates of (J2000) 06:56:43.36, +01:01:37.7 with uncertainties of 0.2 arcsec in both coordinates. The position of the object is within XRT afterglow localization (Cenko et al., GCN 35666). The object is absent in PS1 catalogue. Preliminary photometry of the object is R ~ 20.6 based on USNO-B1.0 (R2) nearby stars. We suggest the source is an afterglow of GRB 240204A.
GCN 35671 table
GRB_name GRB240204A
GCN_number 35671
Detection_method Swift-XRT Det
ra 104.1814°
decl 1.0269°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35671 SUBJECT: GRB 240204A: Enhanced Swift-XRT position DATE: 24/02/04 19:44:55 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 1322 s of XRT Photon Counting mode data and 2 UVOT images for GRB 240204A, 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 = 104.18139, +1.02693 which is equivalent to: RA (J2000): 06h 56m 43.53s Dec (J2000): +01d 01' 36.9" with an uncertainty of 2.5 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 35673 table
GRB_name GRB240204A
GCN_number 35673
Detection_method Optical
ra 104.1807°
decl 1.0272°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35673 SUBJECT: GRB 240204A: optical afterglow detection with LCOGT 1m telescopes at Sutherland and Teide Observatories DATE: 24/02/05 02:47:44 GMT FROM: Ismael Perez-Fournon at Instituto de Astrofisica de Canarias I. Pérez-Fournon and F. Poidevin (IAC and ULL) report We observed the field of GRB 240204A, detected by FERMI GBM (Fermi GBM team, GCN 35664) and by Swift XRT (Cenko et al., GCN 35666), centred at the enhanced Swift-XRT position reported by Beardmore et al. (GCN 35671) with LCOGT 1m telescopes at Sutherland and Teide Observatories. We detect a source, not visible in PanSTARRS imaging, at the position RA (J2000) = 06:56:43.367, Dec (J2000) = +01:01:38.06 (+/- 0.5" in both coordinates). We measure the following magnitudes in SDSS filters: r' = 21.10 +/- 0.15 on 2024-02-04 20:37:30 UT (Sutherland Observatory) and i' = 20.79 +/- 0.15 on 2024-02-04 21:29:56 UT (Teide Observatory), calibrated using the Gaia DR3 synthetic photometry catalog generated from the Gaia BP/RP mean spectra (Gaia Collaboration, 2022), uncorrected for interstellar extinction. The reported position agrees within the errors with the enhanced Swift-XRT position and with the positions of the optical source detected by Pozanenko et al. (GCN 35670) and Leonini et al. (GCN 35672). The flux is clearly decreasing in the red bands.
GCN 35677 table
GRB_name GRB240204A
GCN_number 35677
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35677 SUBJECT: GRB 240204A: Osservatorio Astronomico Nastro Verde upper limit DATE: 24/02/05 18:30:30 GMT FROM: Nello Ruocco at Osservatorio Nastro Verde - Sorrento (Naples) - Italy - MPC Code C82 Nello Ruocco at Osservatorio Nastro Verde - Sorrento (Naples) - Italy in a large collaboration with: M.G. Dainotti (National Astronomical Observatory of Japan), Y. Niino (Tokyo University, Institute of Astronomy), K. Kalinowski (Aarhus University, Department of Physics and Astronomy), B. De Simone (Universita' degli Studi Di Salerno) report: We image the field of GRB 240204A (Swift triggered on the Fermi/GBM, GCN 35664; Cenko et al., GCN 35666; Pozanenko et al., GCN 35670) with telescope of Nastro Verde Observatory - Sorrento (Naples), Italy. Member of: AAVSO - American Association of Variable Star Observers. UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili. AstroCampania Associazione The observations started at 18:16 UT of 2024/02/04, after about 3 hours after the GRB trigger, at the end of twilight with principal telescope SC 0.35 f/10 with focal reduced + CCD Sbig ST10 XME I took 104 image of 60 sec each. All images are unfiltered, calibrated with masterdark and masterflat,stacked with Tycho Tracker and Astrometrica software We have not detected any clearly visible sources, up to 20th magnitude with clear skies. Start T0+ End T0+ Rlim 18:16:19 UT 21:15:19 UT 19.5 We did not found any optical counterpart in the error box of the XRTcandidate. Magnitudes were estimated with the Gaia DR2 cat. and are not corrected for galactic dust extinction. The message may be cited.
GCN 35680 table
GRB_name GRB240204A
GCN_number 35680
Detection_method Fermi GBM Det
t_trigger 15:07:38.680 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35680 SUBJECT: GRB 240204A: Fermi GBM Observation DATE: 24/02/05 21:17:16 GMT FROM: Lorenzo Scotton at UAH L. Scotton (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 15:07:38.68 UT on 04 February 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240204A (trigger 728752063/240204630), which was also detected by Swift XRT (S. B. Cenko et al. 2024, GCN 35666). The Fermi GBM on-ground location is consistent with the Swift XRT position. The angle from the Fermi LAT boresight is 101 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 15.9 s (50-300 keV). The time-averaged spectrum from T0-6.5 to T0+34.5 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.03 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 84 +/- 2 keV. The event fluence (10-1000 keV) in this time interval is (1.69 +/- 0.02)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+12 s in the 10-1000 keV band is 32.9 +/- 0.5 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 79 +/- 2 keV, alpha = -0.97 +/- 0.04 and beta = -3.0 +/- 0.2. 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 35688 table
GRB_name GRB240204A
GCN_number 35688
Detection_method Swift-BAT Det
ra 104.2900°
decl 1.0780°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35688 SUBJECT: GRB 240204A: Swift-BAT refined analysis DATE: 24/02/06 02:39:23 GMT FROM: Sibasish Laha at GSFC T. Sakamoto (AGU),S. D. Barthelmy (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), M. Stamatikos (OSU) (i.e. the Swift-BAT team): Swift-BAT triggered on GRB 240204A at 15:07:50.63 UT on 2024-02-04. Swift slewed immediately, but didn’t have initial BAT information due to a telemetry gap. Using the data set from T-239 to T+346 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240204A (trigger #1212898) (Cenko, et al., GCN Circ. 35666). The BAT ground-calculated position is RA, Dec = 104.290, 1.078 deg which is RA(J2000) = 06h 57m 09.6s Dec(J2000) = +01d 04' 41.5" with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 9%. The BAT light curve shows a complex structure with a duration of ~ 20 sec. T90 (15-350 keV) is 18.93 +- 2.06 sec (estimated error including systematics). The time-averaged spectrum from T-22.96 to T+8.96 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.21 +- 0.28, and Epeak of 67.8 +- 12.6 keV (chi squared 41.34 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 1.0 +- 0.0 x 10^-05 erg/cm2 and the 1-sec peak flux measured from T+0.08 sec in the 15-150 keV band is 22.1 +- 1.5 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.80 +- 0.06 (chi squared 55.74 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/1212898/BA/
GCN 35690 table
GRB_name GRB240204A
GCN_number 35690
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35690 SUBJECT: GRB 240204A : OHP/T193/T120 optical afterglow fading detection DATE: 24/02/06 05:05:24 GMT FROM: Christophe Adami at LAM C. Adami, D. Russeil, H. LeCoroller (Pythéas/LAM), E. Abdo, M. Carta, T. Chehab, M. Colliaux, A. Gharibi-Ziarati, E. Pouyer, A. Jacquet, F. Malaval, S. Aftis (AMU), J. Balcaen, Y. Degot-Longhi, (OHP/Pythéas), E. Le Floc'h, D. Götz, F. Schüssler (CEA Paris-Saclay), B. Schneider (MIT), S. Basa (Pytheas/OHP/LAM), A. Saccardi, S. D. Vergani (GEPI, Obs. de Paris), M. Dennefeld (IAP), report on behalf of a larger collaboration We observed the field of GRB 240204A (Fermi-GBM team GCN 35664, Cenko et al. GCN 35666, Pozanenko et al. GCN 35670, Leonini et al. GCN 35672, Pérez-Fournon et al. GCN 35673, Dainotti et al. GCN 35677, Bochenek et al. GCN 35678) using the T193cm telescope equiped with the MISTRAL instrument and with the T120cm telescope at Observatoire de Haute-Provence (France). On the night of 04 February 2024, we made 9 sets of observations with MISTRAL in r band (30min each) and two sets of observations with the T120 telescope (V and i bands: 135min each). On the night of 05 February 2024, we made an additional single set of observations with MISTRAL in r band during 97.5min. Details are given in the table below. All magnitudes were calibrated against the PanStarrs catalog (mean Kron magnitudes), extracted in a radius of 1arcmin around the GRB position. Magnitudes were not corrected for galactic extinction. Our results in r-band show a fading behaviour of typically 0.09+/-0.03 mag/hour over the 10 first hours and of 0.06+/-0.01 mag/hours over the 31 first hours. ----------------------------------------------- T-T0 (in hours) | mag | filter | Telescope ----------------------------------------------- +4.09 | 21.82+/-0.21 | r | MISTRAL@T193 +4.70 | 21.88+/-0.15 | r | MISTRAL@T193 +5.29 | 21.86+/-0.11 | r | MISTRAL@T193 +5.89 | 21.92+/-0.12 | r | MISTRAL@T193 +6.64 | 21.77+/-0.10 | r | MISTRAL@T193 +7.22 | 21.98+/-0.10 | r | MISTRAL@T193 +7.99 | 21.88+/-0.12 | r | MISTRAL@T193 +8.69 | 22.10+/-0.13 | r | MISTRAL@T193 +9.32 | 22.51+/-0.31 | r | MISTRAL@T193 +30.72 | 23.37+/-0.31 | r | MISTRAL@T193 +6.02 | 22.69+/-0.17 | g | T120 +6.02 | 20.33+/-0.13 | i | T120 We acknowledge OHP staff for its excellent support during the AMU M2-Physics 2024 observationnal internship. This work received support from the French government under the France2030 investment plan, as part of the initiative d’Excellence d’Aix-Marseille Universit´e- A*MIDEX (AMX-19-IET-008). We were also supported by the IPhU Graduate School program at Aix-Marseille University. We also acknowledge the support by Master Erasmus Mundus Europhotonics (599098-EPP-1-2018-1-FR-EPPKA1-JMD-MOB) financed by EACEA (European Education and Culture Executive Agency).
GCN 35691 table
GRB_name GRB240204A
GCN_number 35691
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35691 SUBJECT: GRB 240204A: Mondy optical afterglow observations DATE: 24/02/06 07:50:17 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI, HSE), N. Pankov (HSE, IKI), E. Klunko (ISTP), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN: We observed the GRB 240204A (Fermi-GBM team GCN 35664, Cenko et al. GCN 35666, Pozanenko et al. GCN 35670, Leonini et al. GCN 35672, Pérez-Fournon et al. GCN 35673, Dainotti et al. GCN 35677, Bochenek et al. GCN 35678; Adami et al. GCN 35690) with AZT-33IK telescope of Mondy observatory starting on 2024-02-04 (UT) 16:05:26 and 2024-02-05 (UT) 13:10:09. Preliminary photometry of the afterglow based on USNO-B1.0 (R2) nearby stars is following Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) (mid, days) (s) 2024-02-04 16:05:26 0.04292 R 480 19.90 0.10 21.9 2024-02-04 16:13:26 0.04847 R 480 20.01 0.11 21.8 2024-02-04 16:21:26 0.05403 R 480 19.93 0.10 21.9 2024-02-04 16:29:27 0.05959 R 480 19.85 0.09 21.8 2024-02-04 17:31:00 0.11345 R 2400 20.55 0.10 22.5 2024-02-05 13:10:09 0.96772 R 8400 22.4 0.2 23.1
GCN 35692 table
GRB_name GRB240204A
GCN_number 35692
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 35692 SUBJECT: GRB 240204A: AstroSat CZTI detection DATE: 24/02/06 14:39:17 GMT FROM: Varun Bhalerao at IIT Bombay J. Joshi (IUCAA), G. Waratkar (IITB), 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 240204A which was also detected by Fermi-GBM (Fermi GBM Team, GCN Circ. 35664), and Swift (Cenko et al., GCN Circ. 35666). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2024-02-04 15:07:49.50 UTC. The measured peak count rate associated with the burst is 201 (+40 -25) counts/s above the background in the combined data of four quadrants, with a total of 1125 (+193 -176) counts. The local mean background count rate was 308 (+5 -6) counts/s. Using cumulative rates, we measure a T90 of 10.5 (+1.1 -2.5) s. The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-02-04 15:07:49.4 UTC. The measured peak count rate associated with the burst is 388 (+65, -60) counts/s above the background in the combined data of all quadrants, with a total of 2008 (+336, -351) counts. The local mean background count rate was 1276 (+6, -6) counts/s. We measure a T90 of 8.5 (+3.1, -2.1) 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 35705 table
GRB_name GRB240204A
GCN_number 35705
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35705 SUBJECT: GRB240204A: Swift/UVOT Upper Limits DATE: 24/02/08 15:37:24 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and and S. B Cenko (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240204A 4.8 ks after the BAT trigger (Cenko et al., GCN Circ 35666). No optical afterglow consistent with either the optical (Pozanenko et al., GCN Circ. 35670) or X-ray (Beardmore et al., GCN Circ. 35671) position is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures of the candidate afterglow field are: Filter T_start(s) T_stop(s) Exp(s) Mag white 5887 6087 196 >20.70 v 4862 6498 393 >19.32 b 5683 5882 196 >19.98 u 5477 28539 1048 >20.54 uvw1 5272 5472 196 >19.26 uvm2 5067 6669 360 >19.36 uvw2 6093 6293 196 >19.42 The magnitudes in the table are not corrected for the Galactic extinction due to the high but uncertain reddening in the direction of the burst (Schlegel et al. 1998).
GCN 35714 table
GRB_name GRB240204A
GCN_number 35714
Detection_method Konus-Wind Det
t_trigger 15:07:53.519 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35714 SUBJECT: Konus-Wind detection of GRB 240204A DATE: 24/02/11 19:46:09 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 240204A (Fermi-GBM detection: The Fermi GBM team, GCN 35664; Swift-BAt detection: Cenko et al., GCN 35666; AstroSat-CZTI detection: Joshi et al., GCN 35692) triggered Konus-Wind at T0=54473.519 s UT (15:07:53.519). The burst light curve shows a single pulse which starts at ~T0-4.5 s and has a total duration of ~21.5 s. The emission is seen up to ~1 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240204_T54473/ As observed by Konus-Wind, the burst had a fluence of 1.37(-0.07,+0.07)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+2.448 s, of 4.22(-1.15,+1.15)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 = -1.29(-0.16,+0.17) and Ep = 81(-6,+6) keV (chi2 = 87/83 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.9 (chi2 = 86/82 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 35922 table
GRB_name GRB240204A
GCN_number 35922
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35922 SUBJECT: GRB240204A: VIRT optical upper limit DATE: 24/03/14 00:11:58 GMT FROM: Priya Gokuldass at ERAU K. Smith (UVI), P. Gokuldass (ERAU), N. Orange (OrangeWave Innovative Science, LLC), D. Morris (NASA), T. Lombardi (Eckerd College), K. Noonan (UVI), R. Querrard (UVI), D. Smith (UVI) report: We observed the field of GRB240204A (Cenko et al., GCN 35666) with the 0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin Islands' Etelman Observatory on 02-05-2024 starting at 00:36:35 (T+10.04 hrs). We performed a series of exposures in an R filter with a total exposure of 4000s. The weather conditions were clear during the hours of observation with an average airmass of 1.08. We do not detect any source within the enhanced XRT position (Beardmore et al. GCN 35671). This non-detection is consistent with the upper limits and detections of the faint optical transient reported by Master (Lipunov et al., GCN 35668), Mondy (Pozanenko et al., GCN 35670), Montarrenti Observatory (Leonini et al., GCN 35672), LCOGT (Perez-Fournon and Poidevin, GCN 35673), Osservatorio Nastro Verde (Ruocco et al., GCN 35677), Liverpool Telescope (Bochenek et al., GCN 35678), and Observatoire de Haute-Provence (Adami et al., GCN 35690). We report the following 3-sigma upper limit: T_mid ||Exposure ||Filter ||Limit T+ 10.04 hrs || 4000s || R || >20.9 The limit is estimated from comparison to nearby USNO B1 stars and is not corrected for Galactic extinction. The VIRT is still in the commissioning phase. We acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001 and NASA EPSCoR award 80NNSC22M0063. R.Q and N.B.O also acknowledge financial support from South Carolina Space Grant award 80NSSC20M0054. This message can be cited.