GRB240619A

This page lists all entries on GRB240619A in GRBweb

Summary Fermi GBM IPN GCN 36694 GCN 36695 GCN 36708 GCN 36715 GCN 36717 GCN 36719 GCN 36720 GCN 36721 GCN 36724 GCN 36739 GCN 36740 GCN 36768 GCN 36813

Summary table
Variable Value Source
GRB_name_Fermi GRB240619155
T0 3:43:28.204 UTC GCN_circulars,Konus-Wind Det
ra 162.0000° IPN
decl 17.3000° IPN
pos_error 1.60e+00° IPN
T90 36.126 s Fermi_GBM
T90_error 0.586 s Fermi_GBM
T90_start 3:43:31.006 UTC Fermi_GBM
fluence 1.00e-05 erg/cm² Fermi_GBM
fluence_error 3.22e-08 erg/cm² Fermi_GBM
redshift 0.3965 GCN_circulars,Optical
T100 38.928 s
GBM_located False
mjd 60480.1551875463 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB240619155
trigger_name bn240619155
ra 162.0900°
decl 17.2700°
pos_error 2.83e+00°
datum 2024-06-19
t_trigger 3:43:31.003 UTC
T90 36.126 s
T90_error 0.586 s
T90_start 3:43:31.006 UTC
fluence 1.00e-05 erg/cm²
fluence_error 3.22e-08 erg/cm²
flux_1024 1.91e+01 erg/cm²/s
flux_1024_error 3.64e-01 erg/cm²/s
flux_1024_time 9.60e-02 erg/cm²/s
flux_64 2.36e+01 erg/cm²/s
flux_64_error 1.50e+00 erg/cm²/s
IPN table
GRB_name GRB240619A
ra 162.0000°
decl 17.3000°
pos_error 1.60e+00°
redshift 0.3965
GCN 36694 table
GRB_name GRB240619A
GCN_number 36694
Detection_method Fermi GBM final loc
t_trigger 3:43:31 UTC
ra 162.1000°
decl 17.3000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36694 SUBJECT: GRB 240619A: Fermi GBM Final Real-time Localization DATE: 24/06/19 03:54:00 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 03:43:31 UT on 19 Jun 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240619A (trigger 740461416.003318 / 240619155). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 162.1, Dec = 17.3 (J2000 degrees, equivalent to J2000 10h 48m, 17d 18'), with a statistical uncertainty of 1.6 degrees. The angle from the Fermi LAT boresight is 63.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240619155/quicklook/glg_skymap_all_bn240619155.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/bn240619155/quicklook/glg_healpix_all_bn240619155.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240619155/quicklook/glg_lc_medres34_bn240619155.gif
GCN 36695 table
GRB_name GRB240619A
GCN_number 36695
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36695 SUBJECT: GRB 240619A: BALROG localization (Fermi Trigger 740461416 / GRB 240619155) DATE: 24/06/19 04:41:44 GMT FROM: Jochen Greiner at MPE T. Preis, B. Biltzinger, J. Burgess & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 740461416 at 03:43:31 on 19 June 2024 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position is: RA(2000.0) = 162.2 deg Decl.(2000.0) = 14.8 deg The 1 sigma statistical error radius is 3.2 deg. We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB240619155/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB240619155/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB240619155/json
GCN 36708 table
GRB_name GRB240619A
GCN_number 36708
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36708 SUBJECT: Fermi GRB 240619A: Global MASTER-Net observations report DATE: 24/06/19 23:45:42 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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 240619A ( Fermi GBM team, GCN 36694) errorbox 55438 sec after notice time and 55481 sec after trigger time at 2024-06-19 19:08:12 UT, with upper limit up to 16.7 mag. The observations began at zenith distance = 68 deg. The sun altitude is -17.7 deg. The galactic latitude b = 60 deg., longitude l = 227 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2499301 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 55512 | 2024-06-19 19:08:12 | MASTER-Kislovodsk | (10h 49m 58.96s , +16d 22m 16.8s) | C | 60 | 16.7 | 57629 | 2024-06-19 19:43:30 | MASTER-Kislovodsk | (10h 43m 55.90s , +14d 27m 58.5s) | C | 60 | 16.3 | 57710 | 2024-06-19 19:44:50 | MASTER-Kislovodsk | (10h 44m 03.04s , +14d 26m 52.8s) | C | 60 | 16.1 | 58111 | 2024-06-19 19:51:32 | MASTER-Kislovodsk | (10h 49m 57.47s , +16d 21m 38.9s) | C | 60 | 15.9 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 36715 table
GRB_name GRB240619A
GCN_number 36715
Detection_method Optical
ra 162.3946°
decl 17.2828°
redshift 0.6300
Circular_text TITLE: GCN CIRCULAR NUMBER: 36715 SUBJECT: GRB 240619A: GOTO candidate optical afterglow DATE: 24/06/20 21:07:53 GMT FROM: Ben Gompertz at U of Birmingham B. P. Gompertz, K. Ackley, S. Belkin, T. Killestein, A. J. Levan, B. Godson, R. Starling, M. J. Dyer, J. Lyman, K. Ulaczyk, F. Jimenez-Ibarra, A. Kumar, D. O'Neill, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Pall'e and D. Pollacco report on behalf of the GOTO collaboration: We report on observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022) in response to GRB 240619A (Fermi GBM Team, GCN 36694). Targeted observations were performed by GOTO-South at 08:21:34 UT on 2024-06-19 (3x90s exposures, 4.7 hours after trigger), and by GOTO-North at 21:40:50 UT on 2024-06-19 (4x90s exposures, 18.0 hours after trigger). Observations were taken in the GOTO L-band (400-700 nm). Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using recent survey observations of the same pointings. Source candidates were initially filtered using a classifier (Killestein et al. 2021) and cross-matched against a variety of contextual and minor planet catalogues. Human vetting was carried out in real time on any candidates that passed the above checks. A new optical source AT 2024lwv (GOTO24cvn) is identified within the GBM 90% localisation region at RA = 10:49:34.70, Dec = +17:16:58.07 with an initial magnitude of L = 17.17 +/- 0.17 mags 4.7 hours after trigger, fading to L = 18.38 +/- 0.09 mags at 18.0 hours after trigger. The source is also present in the data available on the ATLAS forced photometry server (Shingles et al. 2021) with an initial magnitude of o = 16.2 +/- 0.04, 2.3 hours after the GRB trigger. Observations are consistent with a power-law decay of approximately t^-0.8. The transient was not detected in the most recent pre-trigger GOTO observation, taken at 21:54:02 UT on 2024-06-17 (~1.25 days prior to the GRB) to a 5-sigma limiting magnitude of L > 19.2 mags. The transient is spatially coincident (0.1” offset) with the catalogued galaxy PSO J162.3946+17.2828 with a photometric redshift of 0.63 +/- 0.19 in the PS1-STRM catalogue (Beck et al. 2020). Due to the galaxy association, rapid decay, and lack of detection in pre-GRB imaging, we propose this source as the optical afterglow of GRB 240619A. Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction. Observations are ongoing. GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).
GCN 36717 table
GRB_name GRB240619A
GCN_number 36717
Detection_method Fermi GBM Det
t_trigger 3:43:31 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36717 SUBJECT: GRB 240619A: Fermi GBM Observation DATE: 24/06/21 01:21:00 GMT FROM: Sarah Dalessi at UAH S. Dalessi (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 03:43:31.00 UT on 19 June 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240619A (trigger 740461416/240619155), which was also detected by the Gravitational-wave Optical Transient Observer (GOTO) (Gompertz et al. 2024, GCN 36715). The Fermi-GBM Final Real-time location (Fermi GBM Team 2024, GCN 36694) is consistent with the GOTO position. The angle from the Fermi LAT boresight is 63 degrees. The GBM light curve two emission episodes with a duration (T90) of about 36.1 s (50-300 keV). The time-averaged spectrum from T0+0.002 to T0+36.129 s is best fit by a Band function with Epeak = 110 +/- 50 keV, alpha = -1.3 +/- 0.2, and beta = -1.70 +/- 0.04. The event fluence (10-1000 keV) in this time interval is (1.19 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.096 s in the 10-1000 keV band is 19.1 +/- 0.4 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 36719 table
GRB_name GRB240619A
GCN_number 36719
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 36719 SUBJECT: GRB 240619A: CALET Gamma-Ray Burst Monitor detection DATE: 24/06/21 07:03:46 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University S. Torii (Waseda U), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 240619A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 36694; BALROG localization: Preis et al., GCN Circ. 36695; Fermi GBM Observation: Dalessi et al., GCN Circ. 36717) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 03:43:30.40 UTC on 19 June 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1402803348/index.html). The burst signal was seen by all CGBM detectors. The burst light curve shows a double-peaked structure that starts at T+0.6 sec, peaks at T+1.1 sec, and ends at T+37.4 sec. The T90 and T50 durations measured by the SGM data are 35.0 +/- 1.3 sec and 28.5 +/- 1.1 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1402803348/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.
GCN 36720 table
GRB_name GRB240619A
GCN_number 36720
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36720 SUBJECT: GRB 240619A: Swift ToO observations DATE: 24/06/21 07:31:35 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/GBM GRB 240619A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021697 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/GBM event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team.
GCN 36721 table
GRB_name GRB240619A
GCN_number 36721
Detection_method Swift-XRT Other
ra 162.3944°
decl 17.2829°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36721 SUBJECT: GRB 240619A: Swift-XRT probable afterglow detection DATE: 24/06/21 08:07:28 GMT FROM: Phil Evans at U of Leicester M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), S. Dichiara (PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/GBM-detected burst GRB 240619A (GCN Circ. 36694), collecting 1.7 ks of Photon Counting (PC) mode data between T0+174.0 ks and T0+175.7 ks at the location of the GOTO afterglow candidate AT 2024lw (Gompertz et al., GCN Circ. 36715). An uncatalogued X-ray source is detected at RA, Dec=162.3944, +17.2829 which is equivalent to: RA (J2000): 10:49:34.66 Dec(J2000): +17:16:58.5 with an uncertainty of 4.3 arcsec (radius, 90% confidence). This position is 0.7 arcsec from the GOTO position and thus we suggest it is related to that object and likely the GRB afterglow. The source has a mean count rate of 2.5e-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/00021697. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/00021697. This circular is an official product of the Swift-XRT team.
GCN 36724 table
GRB_name GRB240619A
GCN_number 36724
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 36724 SUBJECT: GRB 240619A: GRBAlpha detection DATE: 24/06/21 14:40:54 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa, M. Kolar (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Duriskova, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. The long-duration GRB 240619A (Fermi/GBM detection: GCN 36694; CALET/CGBM detection: GCN 36719; INTEGRAL/SPI-ACS peak detection at 2024-06-19 ~03:43:31 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..40P/abstract). The detection was confirmed at the peak time 2024-06-19 03:43:30.7 UTC. The T90 duration measured by GRBAlpha is 4.5 s and the overall significance during T90 reaches 10 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240619A_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.
GCN 36739 table
GRB_name GRB240619A
GCN_number 36739
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36739 SUBJECT: GRB 240619A: J-band detection with WINTER DATE: 24/06/23 01:24:30 GMT FROM: Geoffrey Mo at MIT Geoffrey Mo (MIT), Robert Stein (Caltech), Benjamin Schneider (MIT), Viraj Karambelkar (Caltech), Danielle Frostig (MIT), Nathan Lourie (MIT), Tomas Ahumada (Caltech), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report: We observed the field of GRB 240619A (Fermi GBM team, GCN 36694; Greiner et al., GCN 36695; Dalessi et al., GCN 36717; Torii et al., GCN 36719; Dafcikova et al., GCN 36724) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1-square degree WINTER camera (Lourie et al. 2020). Observations began at 2024-06-21T03:44:09 UTC (~48 hours after the GRB) and consisted of 30 x 120 s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.10888436), with image subtraction performed relative to J-band images from the UKIRT Hemisphere survey (Dye et al., 2017). We report the marginal (3-sigma) detection of a source at the position of the GOTO-discovered counterpart (Gompertz et al., GCN 36715; Lipunov et al., GCN 36708; Evans et al., GCN 36720; Capalbi et al., GCN 36721), with magnitude J ~ 19.3 (AB). WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research.
GCN 36740 table
GRB_name GRB240619A
GCN_number 36740
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36740 SUBJECT: GRB 240619A: J-band detection with WINTER (duplicate submission of GCN 36739) DATE: 24/06/23 01:24:00 GMT FROM: Geoffrey Mo at MIT This was a duplicate submission of GCN 36739.
GCN 36768 table
GRB_name GRB240619A
GCN_number 36768
Detection_method Konus-Wind Det
t_trigger 3:43:28.204 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36768 SUBJECT: Konus-Wind detection of GRB 240619A DATE: 24/06/26 21:43:33 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 240619A (Fermi-GBM detection: The Fermi GBM team, GCN 36694; CALET-CGBM detection: Torii et al., GCN 36719; GRBAlpha detection: Dafcikova et al., GCN 36724; GOTO OT detection: Gompertz et al., GCN 36715; Swift-XRT afterglow detection: Capalbi et al., GCN 36721) triggered Konus-Wind at T0=13408.204 s UT (03:43:28.204). The burst light curve shows two separated emission episodes. The initial harder episode starts at ~T0-0.2 s and has a total duration of ~14 s. The following softer episode starts at ~T0+22 s and ends at ~T0+36 s. The total burst duration is ~36 s. The emission is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240619_T13408/ As observed by Konus-Wind, the burst had a fluence of 1.35(-0.36,+0.79)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+0.052 s, of 1.48(-0.50,+0.49)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+41.216 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 = -1.62(-0.21,+0.32) and Ep = 557(-300,+4475) keV (chi2 = 93/86 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -1.9 (chi2 = 93/85 dof). The spectrum near the maximum count rate (measured from T0 to T0+0.256 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.60(-0.52,+0.86), the high energy photon index beta = -1.98(-8.02,+0.25), the peak energy Ep = 480(-218,+870) keV (chi2 = 29/40 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 36813 table
GRB_name GRB240619A
GCN_number 36813
Detection_method Optical
redshift 0.3965
Circular_text TITLE: GCN CIRCULAR NUMBER: 36813 SUBJECT: GRB 240619A: Host galaxy redshift from VLT/X-shooter DATE: 24/07/03 15:58:09 GMT FROM: Laura Cotter L. Cotter (UCD), B. Schneider (MIT), D. Xu (NAOC), J. T. Palmerio (GEPI, Obs. de Paris), D. B. Malesani (DAWN/NBI and Radboud Univ.), A. de Ugarte Postigo (CNRS, OCA, LAM), G. Pugliese (Amsterdam), B. P. Gompertz (Birmingham), A. Martin-Carrillo (UCD), A. Rossi (INAF), D. Hartmann (Clemson Univ.), T. Aishwarya (INAF), N. R. Tanvir (Leicester), A. J. Levan (Radboud) report on behalf of the Stargate collaboration: We observed the location (Gompertz et al., GCN 36715; Capalbi et al., GCN 36721; Mo et al., GCN 36739; Rhodes et al., GCN 36744) of the Fermi GRB 240619A (Fermi GBM team, GCN 36694; Preis et al., GCN 36695; Dalessi et al., GCN 36717) using the X-shooter spectrograph mounted on the ESO VLT UT3 (Melipal). The observation was performed on 2024 July 02 (13.8 days after the GRB). It consisted of 4 exposures of 600 s each and covered the wavelength range 3000-21000 AA. The target is faintly detected in the r-band acquisition image, with an AB magnitude r ~ 22.8 (calibration is difficult due to paucity of calibrators in the field). This is significantly brighter than the archival object visible in the Pan-STARRS and Legacy surveys, first noticed by Gompertz et al. (GCN 36715), and likely includes a transient contribution. In a preliminary reduction, we detect several strong emission lines that we identify as H-alpha, H-beta, H-gamma, the [O II] doublet, [O III] 4959, [O III] 5007, and [Ne III] 3869 at a common redshift of z = 0.3965, which is lower than the photometric value reported in the PS1-STRM catalog (Beck et al. 2020) for galaxy PSO J162.3946+17.2828. We therefore propose this to be the redshift of the GRB. The Legacy survey images also show a second, fainter object about 1.7" west of the optical afterglow position. This was also included in the slit, and we measure for it z = 1.338 from detection of [O II] and H-alpha. Given the larger offset, we consider this galaxy to be unrelated to the GRB. We acknowledge expert support from the ESO staff in Paranal, in particular Matias Jones and Thomas Szeifert.