GRB240419A

This page lists all entries on GRB240419A in GRBweb

Summary IPN Swift GCN 36169 GCN 36170 GCN 36174 GCN 36175 GCN 36182 GCN 36183 GCN 36185 GCN 36200 GCN 36250 GCN 36255

Summary table
Variable Value Source
T0 1:48:01 UTC GCN_circulars,Swift Det
ra 94.5340° Swift
decl -44.9995° Swift
pos_error 2.85e-04° Swift
redshift 5.1780
GBM_located False
mjd 60419.075011574074 GCN_circulars,Swift Det
IPN table
GRB_name GRB240419A
ra 94.5667°
decl -45.0167°
pos_error 5.00e-02°
redshift 5.1780
Swift table
GRB_name GRB240419A
t_trigger 1:48:01 UTC
ra 94.5340°
decl -44.9995°
pos_error 2.85e-04°
redshift 5.1780
GCN 36169 table
GRB_name GRB240419A
GCN_number 36169
Detection_method Swift Det
t_trigger 1:48:01 UTC
ra 94.5680°
decl -45.0110°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36169 SUBJECT: GRB 240419A: Swift detection of a burst DATE: 24/04/19 02:03:17 GMT FROM: Simone Dichiara at Pennsylvania State University M. H. Siegel (PSU), S. Dichiara (PSU), R. Gupta (NASA/GSFC), J. A. Kennea (PSU), S. Laha (GSFC/UMBC), D. M. Palmer (LANL) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 01:48:01 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240419A (trigger=1222955). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 94.568, -45.011 which is RA(J2000) = 06h 18m 16s Dec(J2000) = -45d 00' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 4 sec. The peak count rate was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 01:49:51.1 UT, 110.1 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 94.53468, -45.00073 which is equivalent to: RA(J2000) = 06h 18m 08.32s Dec(J2000) = -45d 00' 02.6" with an uncertainty of 3.5 arcseconds (radius, 90% containment). This location is 92 arcseconds from the BAT onboard position, within the BAT error circle. 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 6.63 x 10^20 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 113 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 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 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 0.069. Burst Advocate for this burst is M. H. Siegel (siegel AT swift.psu.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 36170 table
GRB_name GRB240419A
GCN_number 36170
Detection_method Swift-XRT Other
ra 94.5336°
decl -45.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36170 SUBJECT: GRB 240419A: Prompt enhanced Swift-XRT position DATE: 24/04/19 02:37:35 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 240419A, we find an enhanced XRT position of the afterglow: RA, Dec: 94.53358, -44.99999 which is equivalent to: RA (J2000) = 06 18 08.06 Dec (J2000) = -44 59 60.0 with an uncertainty of 1.9 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/1222955. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team.
GCN 36174 table
GRB_name GRB240419A
GCN_number 36174
Detection_method Swift-XRT Det
ra 94.5341°
decl -44.9995°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36174 SUBJECT: GRB 240419A: Enhanced Swift-XRT position DATE: 24/04/19 08:08:55 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 977 s of XRT Photon Counting mode data and 1 UVOT images for GRB 240419A, 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 = 94.53406, -44.99952 which is equivalent to: RA (J2000): 06h 18m 8.17s Dec (J2000): -44d 59' 58.3" with an uncertainty of 2.2 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 36175 table
GRB_name GRB240419A
GCN_number 36175
Detection_method Optical
ra 94.5340°
decl -44.9993°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36175 SUBJECT: GRB 240419A: VLT optical afterglow detection DATE: 24/04/19 08:17:24 GMT FROM: Daniele B. Malesani at IMAPP / Radboud University B. Schneider (MIT), N. Gaspari (Radboud Univ.), N. R. Tanvir (Univ. Leicester), S. Covino (INAF/Brera), D. B. Malesani (DAWN/NBI and Radboud Univ.), L. Izzo (INAF/Napoli and DARK/NBI), A. Saccardi (GEPI/Obs. Paris), report on behalf of the Stargate collaboration. We observed the field of GRB 240419A (Siegel et al., GCN 36169) using the ESO VLT UT1 equipped with the FORS2 camera. Observations were commenced automatically in rapid-response mode (RRM). The first image was acquired on April 19.0895 UT, that is, 20.9 min after the GRB, and consisted of a 20 s image in the R filter. At a relatively high airmass of 2.1, the delivered PSF was 1.4". A source, not present in archival images, is detected within the UVOT-enhanced XRT error circle (Goad et al., GCN 36174), at coordinates (J2000): RA = 06:18:08.17 Dec = -44:59:57.3 Using FORS2 zeropoints, we measure for the source a magnitude R = 19.88 +- 0.05 (Vega), in excellent agreement with photometry calibrated against nearby stars from the SkyMapper catalog. Further observations have been secured and will be reported at a later time. We acknowledge excellent support from the ESO observing staff in Paranal.
GCN 36182 table
GRB_name GRB240419A
GCN_number 36182
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36182 SUBJECT: GRB 240419A: Swift-XRT refined Analysis DATE: 24/04/19 15:20:33 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti (INAF-OAB), D.N. Burrows (PSU), J. D. Gropp (PSU), S. Dichiara (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 7.8 ks of XRT data for GRB 240419A, from 117 s to 33.6 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=5.3 (+2.7, -0.8). At T+249 s the decay flattens to an alpha of -0.2 (+0.7, -0.6) before breaking again at T+1406 s to a final decay with index alpha=1.20 (+0.32, -0.25). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.30 (+0.30, -0.27). The best-fitting absorption column is 2.4 (+1.1, -0.9) x 10^21 cm^-2, in excess of the Galactic value of 6.6 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.1 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.4 (+1.1, -0.9) x 10^21 cm^-2 Galactic foreground: 6.6 x 10^20 cm^-2 Excess significance: 3.1 sigma Photon index: 2.30 (+0.30, -0.27) If the light curve continues to decay with a power-law decay index of 1.20, the count rate at T+24 hours will be 2.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.7 x 10^-14 (1.4 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01222955. This circular is an official product of the Swift-XRT team.
GCN 36183 table
GRB_name GRB240419A
GCN_number 36183
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36183 SUBJECT: GRB 240419A: REM NIR afterglow detection DATE: 24/04/19 15:36:10 GMT FROM: Matteo Ferro at INAF-OAB M. Ferro, Y.-D. Hu, P. D’Avanzo, R. Brivio, S. Covino, D. Fugazza (INAF-OAB) on behalf of the REM team, report: We observed for the field of GRB 240419A (Siegel et al., GCN 36169) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, J, H, K bands, starting on 2024 April 19 at 01:49:38 UT (i.e. 1.6 minutes after the event), and lasting for about 3 hours. From preliminary photometry we detect the NIR afterglow at a position consistent with the optical afterglow position (Schneider et al., GCN 36175), at the following AB magnitude in the H band: H = 15.7 +- 0.1 (calibrated against 2MASS catalogue) at a mid time of t-t0 ~ 4 minutes after the GRB trigger. The afterglow is not detected in our optical observations, at the following AB magnitude limit in the r band: r > 19.2 (calibrated against SkyMapper catalogue) at a mid time of t-t0 ~ 6.3 minutes after the GRB trigger.
GCN 36185 table
GRB_name GRB240419A
GCN_number 36185
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36185 SUBJECT: Swift GRB 240419A: Global MASTER-Net observations report DATE: 24/04/19 17:03:54 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 240419A ( M. H. Siegel et al., GCN 36169) errorbox 54337 sec after notice time and 54397 sec after trigger time at 2024-04-19 16:54:39 UT, with upper limit up to 17.8 mag. Observations started at twilight. The observations began at zenith distance = 25 deg. The sun altitude is -9.6 deg. The galactic latitude b = -24 deg., longitude l = 253 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2427118 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 54488 | MASTER-SAAO | C | 180 | 17.8 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 36200 table
GRB_name GRB240419A
GCN_number 36200
Detection_method Swift Other
ra 94.5341°
decl -44.9993°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36200 SUBJECT: GRB240419A: Skynet Optical Afterglow Analysis DATE: 24/04/20 21:12:37 GMT FROM: maedubay@unc.edu Megan Dubay, Donovan Schlekat, Dylan Dutton, Daniel Reichart, Joshua Haislip, and Vladimir Kouprianov report on behalf of the Skynet Robotic Telescope Network at the University of North Carolina at Chapel Hill. We observed the field of GRB 240419A with one of Skynet’s 16”-diameter PROMPT telescopes at CTIO. The first detection occurred in the I band approximately 1 hour after the trigger reported by Swift (Siegel et al., GCN 36169). We detect the afterglow with coordinates consistent with those reported by VLT (B. Schneider et al., GCN 36175) and REM (Ferro et al., GCN 36183). The coordinates are: R.A. (J2000): 06:18:08.18 Dec. (J2000): -44:59:57.60 We report the photometry below. ExpLen | Filter | Mag | Mag Error | MJD (Center) ------------------------------------------------ 45x8 | I | 19.06 | 0.199 | 60419.119 60x8 | R | ----- | ----- | 60419.119 We report non-detection in the R-band from the reported time with an upper magnitude limit of 20.39. We note that the large R-I color is consistent with the presence of the Lyman-alpha forest in the R band, given its large redshift (Schneider et al., GCN 36176, Lamb & Reichart 2000). Our images have been calibrated using stars from the APASS catalog.
GCN 36250 table
GRB_name GRB240419A
GCN_number 36250
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36250 SUBJECT: GRB 240419A: Possible ATCA radio detection DATE: 24/04/23 09:51:22 GMT FROM: Gemma Anderson at Curtin U S. Chastain (UNM), G. E. Anderson (Curtin University), J. K. Leung (U. Toronto/HUJI), L. Rhodes (U. Oxford), S. D. Ryder (Macquarie), A. Gulati (U. Sydney), A. J. van der Horst (GWU), on behalf of the PanRadio GRB collaboration The Australia Telescope Compact Array (ATCA) performed rapid follow-up observations of GRB 240419A (Siegel et al., GCN 36169) at 5.5, 9, and 18 GHz as part of the Long-term ATCA "PanRadio GRB" follow-up programme C3542 (PI. Anderson). ATCA began observing at 2024-04-19 04:00 UT (2.2 hours post-burst) up until 12:30 UT. In our preliminary analysis, we have a marginal detect of 63 +/- 18 microJy/beam at 18 GHz that is coincident with the enhanced XRT position (Goad et al., GCN 36174). We obtain 3 sigma upper limits of 39 and 42 microJy/beam at 5.5 and 9.0, respectively. Further observations are planned. We thank the CSIRO Space and Astronomy staff for supporting these observations. We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO.
GCN 36255 table
GRB_name GRB240419A
GCN_number 36255
Detection_method Swift-BAT Det
ra 94.5050°
decl -44.9640°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36255 SUBJECT: GRB 240419A: Swift-BAT refined analysis DATE: 24/04/23 13:00:27 GMT FROM: Mike Moss at NASA GSFC T. Parsotan (GSFC), 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. Sakamoto (AGU), M. H. Siegel (PSU) (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 240419A (trigger #1222955) (Siegel, et al., GCN Circ. 36169). The BAT ground-calculated position is RA, Dec = 94.505, -44.964 deg which is RA(J2000) = 06h 18m 01.3s Dec(J2000) = -44d 57' 50.2" with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 89%. The mask-weighted light curve shows two dim pulses at T0-7 s and T0+0 s, respectively. The T90 (15-350 keV) is 3.00 +- 1.41 sec (estimated error including systematics). The time-averaged spectrum from T-0.43 to T+2.57 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.71 +- 0.38. The fluence in the 15-150 keV band is 8.4 +- 2.1 x 10^-08 erg/cm2. The 1-sec peak photon flux measured from T+0.57 sec in the 15-150 keV band is 0.6 +- 0.1 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/1222955