GRB240811A

This page lists all entries on GRB240811A in GRBweb

Summary IPN Swift GCN 37137 GCN 37140 GCN 37141 GCN 37142 GCN 37147 GCN 37150 GCN 37155 GCN 37173

Summary table
Variable Value Source
T0 14:07:33 UTC Swift
ra 226.3621° Swift
decl 28.8959° Swift
pos_error 2.72e-04° Swift
T90 66.32 s Swift
T90_start 14:07:33 UTC Swift
fluence 3.00e-06 erg/cm² Swift
T100 66.32 s
GBM_located False
mjd 60533.58857638889 Swift
IPN table
GRB_name GRB240811A
ra 226.3750°
decl 28.8500°
pos_error 5.00e-02°
Swift table
GRB_name GRB240811A
t_trigger 14:07:33 UTC
ra 226.3621°
decl 28.8959°
pos_error 2.72e-04°
T90 66.32 s
fluence 3.00e-06 erg/cm²
GCN 37137 table
GRB_name GRB240811A
GCN_number 37137
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37137 SUBJECT: Swift GRB 240811A: Global MASTER-Net observations report DATE: 24/08/11 17:07:00 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 240811A ( K. L. Page et al., GCN 37136) errorbox 10112 sec after notice time and 10127 sec after trigger time at 2024-08-11 16:56:20 UT, with upper limit up to 16.7 mag. Observations started at twilight. The observations began at zenith distance = 61 deg. The sun altitude is -10.5 deg. The galactic latitude b = 60 deg., longitude l = 44 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2558765 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 10218 | MASTER-SAAO | C | 180 | 16.7 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 37140 table
GRB_name GRB240811A
GCN_number 37140
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 37140 SUBJECT: GRB 240811A: Upper limits with Mephisto DATE: 24/08/11 18:40:19 GMT FROM: Brajesh Kumar at SWIFAR, YNU Guowang Du, Yuan Fang, Xufeng Zhu, Yehao Cheng, Yuze Zhao, Brajesh Kumar, Weikang Lin, Yuanpei Yang, Xinzhong Er, Xiangkun Liu and Xiaowei Liu (SWIFAR, YNU) report on behalf of Mephisto team: We performed simultaneous multi-band photometric observations of GRB 240811A (Page & Gupta, GCN 37136) using 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory. The observations were started ~37 min after the notice and multiple frames in uvgriz bands were acquired. The upper limits of our initial frames are the following: UTC(2024-08-11) Exptime(s) filter Mag(AB) 14:55 180 v >21.07 14:55 60 r >20.96 14:55 120 z >19.98 15:08 180 u >21.03 15:08 60 g >20.97 15:08 120 i >20.86 ---------------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. ----------------------------------------------------------------------------------
GCN 37141 table
GRB_name GRB240811A
GCN_number 37141
Detection_method Swift-XRT Det
ra 226.3623°
decl 28.8961°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37141 SUBJECT: GRB 240811A: Enhanced Swift-XRT position DATE: 24/08/11 22:19:38 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 1050 s of XRT Photon Counting mode data and 2 UVOT images for GRB 240811A, 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 = 226.36231, +28.89615 which is equivalent to: RA (J2000): 15h 05m 26.96s Dec (J2000): +28d 53' 46.1" with an uncertainty of 2.4 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 37142 table
GRB_name GRB240811A
GCN_number 37142
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37142 SUBJECT: GRB 240811A: LCOGT Optical Upper Limit DATE: 24/08/11 22:45:39 GMT FROM: Robert Strausbaugh at Eastern Illinois University R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration: We observed the Swift GRB 240811A (Beardmore et al., GCN 37136) field with the LCOGT 1-meter Sinistro instrument at the Teide Observatory, Tenerife site, on August 11, from 20:43 to 21:13 UT (corresponding to 6.60 to 7.10 hours after the GRB trigger time) with the sdss r and i filters. We performed a series of 3x300s exposures in each band. We do not detect an uncataloged source within the XRT error region in either band. This result is consistent with other optcal upper limits (Lipunov et al., GCN 37137; Du et al., GCN 37140). The following 5-sigma upper limits are calculated using the PanSTARRS catalog as reference: r > 22.6 i > 20.5 These magnitudes are not corrected for galactic extinction.
GCN 37147 table
GRB_name GRB240811A
GCN_number 37147
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37147 SUBJECT: GRB 240811A: Swift/UVOT Upper Limits DATE: 24/08/12 08:26:46 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL) and K. L. Page (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240811A 102 s after the BAT trigger (Page et al., GCN Circ. 37136). No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 37141) 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 first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 102 252 147 >21.0 u_FC 315 564 246 >20.7 white 102 1191 353 >21.9 v 644 5026 255 >18.7 b 570 1167 58 >20.0 u 315 1142 285 >20.7 w1 1098 5251 34 >19.2 m2 5031 5231 197 >18.8 w2 4622 4821 197 >19.6 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.023 in the direction of the burst (Schlegel et al. 1998).
GCN 37150 table
GRB_name GRB240811A
GCN_number 37150
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 37150 SUBJECT: GRB 240811A: Bassano Bresciano Observatory upper limit DATE: 24/08/12 15:07:22 GMT FROM: Ulisse Quadri at Bassano Bresciano Observatory U.Quadri, L.Strabla and P.Madurini (Bassano Bresciano Astronomical Observatory - Italy), Members of: AAVSO - American Association of Variable Star Observers. UAI/SSV - Unione Astrofili Italiani/SSV-GRB section. GAC - Gruppo Astrofili Cremonesi. 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 imaged the field of GRB 240811A detected by SWIFT(trigger 1248132) with the robotic telescope of (IAU station 565) Bassano Bresciano Observatory, Italy. The observations started 5.56 hour after the GRB trigger, At the end of twilight with our Newton telescope D=450 mm F/D=4.5. Weather conditions were good. We co-added 150 exposures of 20 sec each (total 50 min). Start T0+ End T0+ Vlim 5.56 hour 6.47 hour 21 We did not found any optical counterpart in the error box of the XRTcandidate (K. L. Page & R. Gupta, GCN 37136; v. Lipunov et al., GCN 37137; Guowang Du et al., GCN 37140; A.P. Beardmore et al., GCN 37141; R. Strausbaugh and A. Cucchiara, GCN 37142; N. P. M. Kuin and K. L. Page, GCN 37147; T. Sbarrato et al., GCN 37149). Magnitudes were estimated with the pan-STARRS cat and are derived using Lupton (2005) equations. Not corrected for galactic dust extinction. Reference: http://www.osservatoriobassano.org/grb.asp The message may be cited.
GCN 37155 table
GRB_name GRB240811A
GCN_number 37155
Detection_method Swift-BAT Det
ra 226.3280°
decl 28.8840°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37155 SUBJECT: GRB 240811A: Swift-BAT refined analysis DATE: 24/08/12 18:07:11 GMT FROM: Tyler Parsotan at NASA GSFC A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), 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-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240811A (trigger #1248132) (Page, et al., GCN Circ. 37136). The BAT ground-calculated position is RA, Dec = 226.328, 28.884 deg which is RA(J2000) = 15h 05m 18.8s Dec(J2000) = +28d 53' 02.5" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 71%. The mask-weighted light curve shows a complex structure with many peaks and potential precursor emission ~30 seconds before the trigger time. T90 (15-350 keV) is 66.32 +- 5.22 sec (estimated error including systematics). The time-averaged spectrum from T-42.95 to T+41.32 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.71 +- 0.08. The fluence in the 15-150 keV band is 3.0 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+11.30 sec in the 15-150 keV band is 2.9 +- 0.3 ph/cm2/sec. 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/1248132
GCN 37173 table
GRB_name GRB240811A
GCN_number 37173
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 37173 SUBJECT: Konus-Wind detection of GRB 240811A DATE: 24/08/13 11:13:37 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 240811A (Swift detection: Page & Gupta, GCN 37136; Lien et al., GCN 37155) 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 >18 sigma count rate increase in the interval from T0-34.908 s to T0+35.748 s where T0 = T0(BAT) = 14:07:33.190 UT. The KW light curve of this burst is available at http://www.ioffe.ru/LEA/GRBs/GRB240811A/ Modeling a time-integrated spectrum of the burst (from T0-34.908 s to T0+35.748 s) by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep): yields alpha = -1.22 (-0.27, + 0.80) and Ep = 126(-33,+51) keV. The total burst fluence is 4.65(-0.30,+1.35)x10^-6 erg/cm^2, and the 2.944 s peak energy flux, measured from T0+3.364 s, is 2.43(-0.33,+0.76)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.