GRB240411B

This page lists all entries on GRB240411B in GRBweb

Summary IPN Swift GCN 36063 GCN 36064 GCN 36065 GCN 36067 GCN 36069 GCN 36071 GCN 36072 GCN 36074 GCN 36077 GCN 36078 GCN 36179

Summary table
Variable Value Source
T0 15:32:54 UTC GCN_circulars,Swift Det
ra 231.5421° Swift
decl -2.1464° Swift
pos_error 3.37e-04° Swift
GBM_located False
mjd 60411.64784722222 GCN_circulars,Swift Det
IPN table
GRB_name GRB240411B
ra 231.5417°
decl -2.1500°
pos_error 5.00e-02°
Swift table
GRB_name GRB240411B
t_trigger 15:32:54 UTC
ra 231.5421°
decl -2.1464°
pos_error 3.37e-04°
GCN 36063 table
GRB_name GRB240411B
GCN_number 36063
Detection_method Swift Det
t_trigger 15:32:54 UTC
ra 231.5424°
decl -2.1461°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36063 SUBJECT: GRB 240411B: Swift detection of a burst DATE: 24/04/11 16:09:02 GMT FROM: K.L. Page at U Leicester T. M. Parsotan (GSFC), S. Dichiara (PSU), R. A. J. Eyles-Ferris (U Leicester), C. Gronwall (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU), K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB), M. H. Siegel (PSU) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 15:32:54 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240411B (trigger=1221183). Swift slewed immediately to the burst. No further BAT information is available at this time due to a telemetry gap. Further information will be available after the next telemetry pass over a ground station. The XRT began observing the field at approximately 15:35:54 UT, around 180 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 231.54236, -2.14609 which is equivalent to: RA(J2000) = 15h 26m 10.17s Dec(J2000) = -02d 08' 45.9" with an uncertainty of 1.9 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 1.11 x 10^21 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 190 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers none of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.138. Burst Advocate for this burst is T. M. Parsotan (parsotat AT umbc.edu). 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 36064 table
GRB_name GRB240411B
GCN_number 36064
Detection_method Optical
ra 231.5424°
decl -2.1463°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36064 SUBJECT: GRB 240411B: LCO optical afterglow detection DATE: 24/04/11 18:43:10 GMT FROM: luca.izzo@inaf.it L. Izzo (INAF-OACn & DARK/NBI), D. B. Malesani (DAWN/NBI and Radboud Univ.), M. Della Valle and R. Martone (INAF-OACn) report: We observed the field of GRB 240411B (Parsotan et al., GCN 36063) with the Sinistro instrument mounted on the 1-m telescope of the LCO network, located at Siding Spring Observatory, Australia. Observations started on April 11 at 17:02:54 UT (1.5 hours after the GRB trigger). We obtained a series of 3x180 s images in the r filter. In the stacked image, we detect a new source within the XRT position, at the coordinates: RA(J2000) = 15:26:10.17 Dec(J2000) = -02:08:46.8 We measure a preliminary magnitude of r = 21.66 +- 0.22 (AB), calibrated against nearby stars from the Pan-STARRS catalog. This source is not visible in the Pan-STARRS catalog and is thus very likely the optical afterglow of GRB 240411B. This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No 730890.
GCN 36065 table
GRB_name GRB240411B
GCN_number 36065
Detection_method Swift-XRT Det
ra 231.5421°
decl -2.1464°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36065 SUBJECT: GRB 240411B: Enhanced Swift-XRT position DATE: 24/04/11 19:09:04 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 373 s of XRT Photon Counting mode data and 1 UVOT images for GRB 240411B, 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 = 231.54213, -2.14640 which is equivalent to: RA (J2000): 15h 26m 10.11s Dec (J2000): -02d 08' 47.0" with an uncertainty of 2.6 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 36067 table
GRB_name GRB240411B
GCN_number 36067
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36067 SUBJECT: GRB 240411B: OHP/T193 optical observations DATE: 24/04/12 05:38:40 GMT FROM: Benjamin Schneider at MIT B. Schneider (MIT), C. Adami (LAM/Pytheas/AMU), E. Le Floc’h (CEA Paris-Saclay), A. Saccardi (GEPI/Obs. de Paris) report on behalf of a larger collaboration: We observed the field of the GRB 240411B (Parsotan et al., GCN 36063; Goad et al., GCN 36065) and its afterglow candidate (Izzo et al., GCN 36064) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. A total of 10 exposures (8x600s + 2x720s) were obtained in the r-band at 00:44:01.5 UT on 2024-04-12 (~9.2h after the trigger). In the combined frame, we detect a source consistent with the optical afterglow reported by Izzo et al. (GCN 36064). The preliminary magnitude derived for that source is r = 23.1 +/- 0.3 mag (AB) The photometric calibration was performed using nearby stars from the PanSTARRS catalog and the magnitude is not corrected for Galactic extinction. We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN 36069 table
GRB_name GRB240411B
GCN_number 36069
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36069 SUBJECT: GRB 240411B: 1.3m DFOT Optical observations DATE: 24/04/12 10:52:24 GMT FROM: Amit Kumar Ror at ARIES Amit K. Ror, Anshika Gupta, Rahul Gupta, Amar Aryan, Saurabh, and Shashi B. Pandey (ARIES) report: We observed the field of GRB 240411B detected by Swift (Parsotan et al., 2024 GCN 36063) with the 1.3m Devasthal Fast Optical Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2024-04-11 at 19:06:28 UT, i.e., ~ 3.56 hours after the BAT trigger. We have taken multiple frames with an exposure time of 300 s in the R filter. We stacked the images after the alignment. We clearly detected an optical afterglow (Izzo et al., 2024, GCN 36064; Schneider et al., 2024, GCN 36067) in our final stacked image within the error box of enhanced Swift-XRT observation (Goad et al., 2024, GCN 36065). The estimated preliminary magnitude is as follows: Date Start_UT T_start-T0 (hours) Filter Exp time (s) Limiting magnitude ======================================================= 2024-04-11 19:06:28 UT 3.56 R 300*15 22.34 +/- 0.11 The detection of the afterglow is consistent with the observations of Izzo et al. 2024, GCN 36064, and Schneider et al. 2024, GCN 36067. The given magnitude value is not corrected for the Galactic and host extinctions in the direction of the GRB afterglow. Photometric calibration is performed using the standard stars from the USNO-B1.0 catalog. This circular may be cited.
GCN 36071 table
GRB_name GRB240411B
GCN_number 36071
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36071 SUBJECT: GRB 240411B: Swift-XRT refined Analysis DATE: 24/04/12 16:36:29 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), J. D. Gropp (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 3.9 ks of XRT data for GRB 240411B, from 160 s to 74.6 ks after the BAT trigger. The data comprise 10 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. The light curve can be modelled with a power-law decay with a decay index of alpha=0.66 (+0.12, -0.11). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.13 (+0.38, -0.20). The best-fitting absorption column is consistent with the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.1 (+/-1.0) x 10^21 cm^-2 Galactic foreground: 1.1 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 2.13 (+0.38, -0.20) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01221183. This circular is an official product of the Swift-XRT team.
GCN 36072 table
GRB_name GRB240411B
GCN_number 36072
Detection_method Swift-BAT Det
ra 231.5620°
decl -2.1720°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36072 SUBJECT: GRB 240411B: Swift-BAT refined analysis DATE: 24/04/12 17:35:46 GMT FROM: Mike Moss at NASA GSFC A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240411B (trigger #1221183) (Parsotan, et al., GCN Circ. 36063). The BAT ground-calculated position is RA, Dec = 231.562, -2.172 deg which is RA(J2000) = 15h 26m 14.8s Dec(J2000) = -02d 10' 20.9" with an uncertainty of 3.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 53%. The mask-weighted light curve shows two spikes separated by an interval of ~15 seconds. The estimated T90 (15-350 keV) is 33.26 +- 1.49 sec (estimated error including systematics). The time-averaged spectrum from T-0.37 to T+33.92 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.69 +- 0.41. The fluence in the 15-150 keV band is 4.9 +- 1.2 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T+32.87 sec in the 15-150 keV band is 0.9 +- 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/1221183
GCN 36074 table
GRB_name GRB240411B
GCN_number 36074
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36074 SUBJECT: GRB 240411B: HiPERCAM/GTC observation DATE: 24/04/12 19:07:20 GMT FROM: Antonio de Ugarte Postigo at OCA A. de Ugarte Postigo (CNRS, OCA, LAM), N. R. Tanvir (U. Leicester), J. F. Agui Fernandez (CAHA), A. Martin-Carrillo (UCD), C. C. Thoene (ASU-CAS), L. Izzo (INAF-OACn & DARK/NBI), J. P. U. Fynbo (DAWN/NBI), G. Lombardi (GRANTECAN), S. Geier (GRANTECAN) report: We observed the field of GRB 240411B (Parsotan et al. GCN 36063) with HiPERCAM on the 10.4m GTC, at the Roque de Los Muchachos Observatory (Spain). We simultaneously obtained 20x60s exposure in each of the u, g, r, i, and z filters. The transparency was bad due to strong calima and the seeing was also poor. The afterglow (Izzo et al. 36064; Goad et al. GCN 36065; Schneider et al. GCN 36067; Ror et al. GCN 36069) is well detected in g, r, i and z, but not in u-band, where the limit is shallow. Observations had a mean time of 0.4256 days after the burst. We measure an r-band magnitude (AB) of r = 23.21+/- 0.08 mag as compared with field star magnitudes from the SDSS.
GCN 36077 table
GRB_name GRB240411B
GCN_number 36077
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36077 SUBJECT: GRB 240411B: Kinder observations with Lulin observatory DATE: 24/04/13 03:50:18 GMT FROM: Amar Aryan A. Aryan, T.-W. Chen, C.-S. Lin, W.-J. Hou, A. Sankar.K, Y.-C. Pan (all NCUIA), S. Yang (HNAS), M.-H. Lee, C.-H. Lai, H.-Y. Hsiao, C.-C. Ngeow, H.-C. Lin, J.-K. Guo (all NCUIA), S. Srivastav (Oxford), M. Fulton, T. Moore, C. Angus, and A. Aamer (all QUB) report: We observed the field of GRB 240411B (Parsotan et al., GCN 36063; Goad et al., GCN 36065; D'Avanzo et al., GCN 36071; Lien et al., GCN 36072) using the Lulin One-meter Telescope (LOT) at Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen et al., AstroNote 2021-92). The optical afterglow candidate of GRB 240411B was identified (Izzo et al., GCN 36064) and followed with several instruments (Schneider et al., GCN 36067; Ror et al., GCN 36069). The first LOT epoch of observations started at 16:45 UT on 11 of April 2024. We followed standard IRAF (Tody D., 1993, ASPC, 52, 173) procedure to reduce the images. Further, PSF photometry was performed using DAOPHOT II (Stetson P. B., 1987, PASP, 99, 191) software. The details of the observations and the preliminary magnitudes (in the AB system) of the afterglow are as follows: Telescope | Filter | MJD | t-t0 | Exposure | Magnitude | avg. Seeing | med. Airmass LOT | r | 60411.698 | 1.25 hrs | 300 sec * 1 | 20.92 +/- 0.12 | 1".16 | 1.17 LOT | i | 60411.715 | 1.65 hrs | 300 sec * 1 | 20.28 +/- 0.15 | 1".0 | 1.13 The presented magnitudes are calibrated using the nearby stars from the PanSTARRS catalog and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V) = 0.14 mag in the direction of the burst (Schlafly & Finkbeiner 2011).
GCN 36078 table
GRB_name GRB240411B
GCN_number 36078
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36078 SUBJECT: GRB 240411B: CrAO/ZTSh optical observations DATE: 24/04/13 07:42:11 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE,IKI), V. Rumyantsev (CrAO), A. Pozanenko (IKI), S. Belkin (IKI) report on behalf of IKI GRB FuN: We observed the field of GRB 240411B (Parsotan et al., GCN 36063; Goad et al., GCN 36065; D'Avanzo et al., GCN 36071; Lien et al., GCN 36072) with ZTSh 2.6m telescope of CrAO observatory starting on 2024-04-11 (UT) 21:18:47. We detect optical afterglow (Izzo et al. GCN 36064; Schneider et al. GCN 36067; Ror et al. GCN 36069; Ugarte Postigo et al. GCN 36074; Aryan et al. GCN 36077). Preliminary photometry of the afterglow in a combined image is following Date UT start t-T0 Filter Exp. OT err UL(3sigma) (mid, days) (s) 2024-04-11 21:18:47 0.283257 R 60*120 22.40 0.25 22.8 The photometry is based on several nearby USNO-B1.0 (R2) stars USNO-B1.0
GCN 36179 table
GRB_name GRB240411B
GCN_number 36179
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 36179 SUBJECT: GRB 240411B: Swift/UVOT Detection DATE: 24/04/19 12:32:47 GMT FROM: Sam LaPorte at PSU S. J. LaPorte (PSU) and T. M. Parsotan (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240411B 190 s after the BAT trigger (Parsotan et al., GCN Circ. 36063). A source consistent with the XRT position (Goad et al., GCN Circ. 36065) and the reported optical transient (Izzo et al. GCN 36064; Schneider et al. GCN 36067; Ror et al. GCN 36069; Ugarte Postigo et al. GCN 36074; Aryan et al. GCN 36077; Pankov et al. GCN 36078) is detected in the initial UVOT exposures. Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag b 6480 6680 196 >19.84 v 7096 7295 196 >18.58 uvw2 6891 7091 196 >19.45 white 6685 6885 196 >20.54 white 198 348 147 20.08+-0.27 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.022 in the direction of the burst (Schlegel et al. 1998).