GRB240414A

This page lists all entries on GRB240414A in GRBweb

Summary Fermi GBM IPN Swift GCN 36083 GCN 36084 GCN 36085 GCN 36087 GCN 36095 GCN 36097 GCN 36100 GCN 36101 GCN 36102 GCN 36103 GCN 36104 GCN 36111 GCN 36113 GCN 36115 GCN 36117 GCN 36120 GCN 36131 GCN 36133 GCN 36137 GCN 36140 GCN 36147 GCN 36228 GCN 36229 GCN 36231 GCN 36318 GCN 37576

Summary table
Variable Value Source
GRB_name_Fermi GRB240414098
T0 2:19:54.462 UTC Fermi_GBM
ra 184.7837° Swift
decl 56.7413° Swift
pos_error 5.18e-05° Swift
T90 82.176 s Fermi_GBM
T90_error 4.128 s Fermi_GBM
T90_start 2:19:54.462 UTC Fermi_GBM
fluence 6.57e-06 erg/cm² Fermi_GBM
fluence_error 4.73e-08 erg/cm² Fermi_GBM
redshift 1.8330 GCN_circulars,Optical
T100 82.176 s
GBM_located False
mjd 60414.097158125 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB240414098
trigger_name bn240414098
ra 184.7858°
decl 56.7269°
pos_error 4.31e+00°
datum 2024-04-14
t_trigger 2:20:39.262 UTC
T90 82.176 s
T90_error 4.128 s
T90_start 2:19:54.462 UTC
fluence 6.57e-06 erg/cm²
fluence_error 4.73e-08 erg/cm²
flux_1024 2.66e+00 erg/cm²/s
flux_1024_error 1.89e-01 erg/cm²/s
flux_1024_time -1.92e-01 erg/cm²/s
flux_64 3.99e+00 erg/cm²/s
flux_64_error 9.10e-01 erg/cm²/s
IPN table
GRB_name GRB240414A
ra 184.7875°
decl 56.7333°
pos_error 5.00e-02°
redshift 1.8330
Swift table
GRB_name GRB240414A
t_trigger 2:20:36 UTC
ra 184.7837°
decl 56.7413°
pos_error 5.18e-05°
redshift 1.8330
GCN 36083 table
GRB_name GRB240414A
GCN_number 36083
Detection_method Swift Det
t_trigger 2:20:36 UTC
ra 184.7860°
decl 56.7270°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36083 SUBJECT: GRB 240414A: Swift detection of a burst DATE: 24/04/14 02:36:27 GMT FROM: K.L. Page at U Leicester R. Caputo (GSFC), C. Gronwall (PSU), J.D. Gropp (PSU), A. Y. Lien (U Tampa), M. J. Moss (GSFC), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: At 02:20:36 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240414A (trigger=1221714). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 184.786, +56.727 which is RA(J2000) = 12h 19m 09s Dec(J2000) = +56d 43' 37" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of at least 60 sec, with a possible smaller peak around T+120s (during the XRT observation). The peak count rate was ~2600 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 02:22:19.6 UT, 103.2 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 184.7855, 56.7381 which is equivalent to: RA(J2000) = 12h 19m 8.52s Dec(J2000) = +56d 44' 17.2" with an uncertainty of 4.9 arcseconds (radius, 90% containment). This location is 39 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. UVOT data are not available at this time. Burst Advocate for this burst is R. Caputo (regina.caputo 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 36084 table
GRB_name GRB240414A
GCN_number 36084
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36084 SUBJECT: GRB 240414A : OHP/T193 optical counterpart detection DATE: 24/04/14 03:35:59 GMT FROM: Christophe Adami at LAM B. Schneider (MIT), C. Adami, O. Ilbert, S. de la Torre (LAM/Pytheas/AMU) report on behalf of a larger collaboration: We observed the field of the GRB 240414A (Caputo et al., GCN 36083) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. In a single exposure of 60s in the r-band at 02:56:37UT on 2024-04-14 (36 min after the trigger), we clearly detect a source consistent with the XRT error: The preliminary magnitude derived for that source is r = 17.61 +/- 0.01 mag (AB) The photometric calibration was performed using nearby stars from the PanSTARRS catalog and the magnitude is not corrected for Galactic extinction. Spectroscopy observations using MISTRAL are currently on going. We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN 36085 table
GRB_name GRB240414A
GCN_number 36085
Detection_method Optical
ra 184.7837°
decl 56.7413°
redshift 1.8330
Circular_text TITLE: GCN CIRCULAR NUMBER: 36085 SUBJECT: GRB 240414A : OHP/T193 redshift determination DATE: 24/04/14 04:55:18 GMT FROM: Christophe Adami at LAM C. Adami, O. Ilbert, S. de la Torre (LAM/Pytheas/AMU), A. de Ugarte Postigo (OCA/LAM), report on behalf of a larger collaboration: We observed the optical counterpart of GRB 240414A (Caputo et al., GCN 36083, Schneider et al., GCN 36084) in spectroscopy with the MISTRAL instrument in blue mode using the T193cm telescope at Observatoire de Haute-Provence (France). We detect the optical GRB afterglow at RA = 12:19:08.08 and DEC = +56:44:28.8 (J2000). Our spectra cover the wavelength range 4200-8000 AA and consist of 3 exposures of 900 seconds each. Observations started at 03:17:09 UT on April 14, 2024 (~57 min after the X-ray trigger). We detect a strong continuum with absorption features which we identify as AlII, AlIII, FeII, MnII and MgII at a common redshift of z=1.833 that we interpret as the redshift of GRB 240414A. Our photometric data reduction continue with g' band observations. We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN 36087 table
GRB_name GRB240414A
GCN_number 36087
Detection_method Other
redshift 1.8330
Circular_text TITLE: GCN CIRCULAR NUMBER: 36087 SUBJECT: GRB 240414A: Redshift confirmation from GTC/OSIRIS+ DATE: 24/04/14 07:07:37 GMT FROM: Antonio de Ugarte Postigo at OCA A. de Ugarte Postigo (CNRS, OCA, LAM), G. Lombardi (GRANTECAN), J. F. Agui Fernandez (CAHA), C. C. Thoene (ASU-CAS), J. P. U. Fynbo (DAWN/NBI), L. Izzo (INAF-OACn & DARK/NBI), N. R. Tanvir (U. Leicester), A. Martin-Carrillo (UCD), S. Geier (GRANTECAN) report: We have obtained spectroscopy of the afterglow of GRB 240414A (Caputo et al. GCN 36083, Schneider et al. GCN 36084) with OSIRIS+ on the 10.4m GTC on the Roque de los Muchachos Observatory (Spain). The observation consisted of 3x900s exposure with grism R1000B covering the range between 3600 and 7880 AA at a mean epoch 2.11 hrs after the burst. We detect a strong continuum over all the spectral range with absorption features that we identify as due to OI, CII, SiIV, SiII, CIV, AlII, NiII, AlIII, ZnII, FeII and MnII, as well as SiII* and FeII*, all at a common redshift of 1.833, consistent with the redshift determined by Adami et al. (GCN 36085). Additionally, we identify an absorption system with CIV and MgII at z=1.703 and another one with MgII at z=1.067. Finally, there is a further strong and slightly broadened feature at 4056 AA that could be due to an intervening system of CIV at z=1.618, but there are no other related features to confirm it.
GCN 36095 table
GRB_name GRB240414A
GCN_number 36095
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36095 SUBJECT: Swift GRB 240414A: Global MASTER-Net observations report DATE: 24/04/14 17:28:49 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-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 240414A ( R. Caputo et al., GCN 36083) errorbox 53869 sec after notice time and 53925 sec after trigger time at 2024-04-14 17:19:21 UT, with upper limit up to 17.3 mag. Observations started at twilight. The observations began at zenith distance = 32 deg. The sun altitude is -10.0 deg. The galactic latitude b = 60 deg., longitude l = 131 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2422039 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 54015 | MASTER-Tavrida | C | 180 | 17.3 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 36097 table
GRB_name GRB240414A
GCN_number 36097
Detection_method Optical
ra 184.7838°
decl 56.7413°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36097 SUBJECT: GRB 240414A: Skynet Optical Afterglow Observations DATE: 24/04/14 18:19:53 GMT FROM: Dylan Dutton at UNC Chapel Hill Dylan Dutton, Megan Dubay, Ruide Fu, Donovan Schlekat, Daniel Reichart, Joshua Haislip, Vladimir Kouprianov, Daniel Caton, Lee Hawkins, Dean Glace, Daryl Janzen, Kim Janzen, James Davidson, Edward Murphy, and Carlos Salgado report on behalf of the Skynet Robotic Telescope Network at the University of North Carolina at Chapel Hill. We observed the field of GRB 240414A with three of our North American robotic telescopes. The first detection occurred at 02:36:17 UTC on Apr 14 2024, approximately 15 minutes after the trigger reported by Swift (Caputo et al., GCN 36083). We obtained multiple exposures in the B, V, and R filters. Exposure lengths were calculated using our automated exposure length scaling model. We detect the optical afterglow with coordinates consistent to those reported by OHP/T193 (B. Schneider et al., GCN 36084). The coordinates are: R.A. (J2000): 12:19:08.12 Dec. (J2000): 56:44:28.70 We report the photometry below. We estimate a temporal index of about -0.9 and spectral index of about -0.5. ExpLen | Filter | Mag | Mag Error | MJD ------------------------------------------------ 51.99 | B | 17.02 | 0.066 | 60414.108 52.82 | V | 16.92 | 0.068 | 60414.110 27.18 | R | 16.46 | 0.086 | 60414.111 76.20 | V | 17.77 | 0.122 | 60414.115 38.54 | R | 17.02 | 0.117 | 60414.117 103.4 | B | 17.86 | 0.096 | 60414.120 52.39 | R | 17.26 | 0.117 | 60414.124 138.1 | V | 17.45 | 0.084 | 60414.128 63.67 | R | 17.13 | 0.117 | 60414.130 300 | R | 18.77 | 0.116 | 60414.204 300 | R | 18.61 | 0.101 | 60414.207 300 | V | 19.04 | 0.064 | 60414.208 300 | V | 19.03 | 0.063 | 60414.208 300 | R | 18.89 | 0.126 | 60414.211 300 | V | 18.85 | 0.054 | 60414.211 300 | V | 18.85 | 0.054 | 60414.211 300 | R | 18.54 | 0.091 | 60414.214 300 | V | 18.97 | 0.059 | 60414.215 300 | V | 18.98 | 0.059 | 60414.215 300 | R | 18.92 | 0.134 | 60414.218 300 | V | 19.03 | 0.063 | 60414.218 300 | V | 19.03 | 0.063 | 60414.218 300 | R | 18.94 | 0.138 | 60414.221 300 | V | 19.03 | 0.062 | 60414.222 300 | V | 19.04 | 0.062 | 60414.222 300 | R | 18.67 | 0.106 | 60414.225 300 | V | 19.12 | 0.065 | 60414.225 300 | V | 19.05 | 0.061 | 60414.225 300 | R | 18.67 | 0.106 | 60414.228 300 | V | 19.15 | 0.070 | 60414.229 300 | V | 19.16 | 0.070 | 60414.229 300 | R | 18.96 | 0.137 | 60414.232 300 | V | 19.16 | 0.069 | 60414.233 300 | V | 19.20 | 0.072 | 60414.233 300 | R | 18.72 | 0.113 | 60414.236 300 | V | 19.30 | 0.076 | 60414.236 300 | V | 19.29 | 0.075 | 60414.236 300 | V | 19.16 | 0.071 | 60414.240 300 | V | 19.21 | 0.075 | 60414.240 300x3 | R | 19.02 | 0.138 | 60414.243 300x3 | R | 19.26 | 0.090 | 60414.295 300x3 | R | 19.22 | 0.088 | 60414.306 300x3 | R | 19.35 | 0.080 | 60414.316 300x3 | R | 19.54 | 0.092 | 60414.327 300x3 | R | 19.35 | 0.159 | 60414.337 300x5 | R | 19.59 | 0.147 | 60414.351 Our images have been calibrated using stars from the APASS catalog.
GCN 36100 table
GRB_name GRB240414A
GCN_number 36100
Detection_method Optical
ra 184.7875°
decl 56.7269°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36100 SUBJECT: GRB 240414A: MarSEC Observatory, Vicenza, Italy, UPPER LIMIT DATE: 24/04/14 21:27:52 GMT FROM: I. Peretto at MarSEC (Marana Space Explorer Center) Ivo Peretto (MarSEC, Marana Space Explorer Center, Marana Di Crespadoro, VI, Italy) Member of: UAI/SSV - Unione Astrofili Italiani/Sezione Stelle Variabili, GRB section. AAVSO (American Association Variable Stars Observers) In collaboration with: Stefano Lora and Giovanni Furlato (MarSEC, Marana Space Explorer Center, Marana di Crespadoro, VI, Italy) report: We imaged the field of GRB 240414A detected by SWIFT(trigger=1221714) with the telescope 14” RC Officine Stellari of MarSEC (Marana Space Explorer Center). The observations with a series of 120 sec exposures started at 2024-01-01 18:18 UT, 958 min. after the GRB trigger, with a Ritchey-Chretien telescope D=360 mm f/ 8. at the following position: RA(J2000) = 12h 19m 09s Dec(J2000) = +56d 43' 37" Weather conditions were medium with Moon illuminated 40,5%. We co-added 30 exposures of 120 sec each. Start T0+ End T0+ R lim. 958 min 1018 min 20.82 We did not found any optical counterpart in A.R. 12 19 09, DEC. +56 43 37 position and in the error box of the XRT candidate. ref.: GCN Circular 36083 Magnitudes were estimated with the APASS and are not corrected for galactic dust extinction. Reference: https://www.marsec.org/ The message may be cited.
GCN 36101 table
GRB_name GRB240414A
GCN_number 36101
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36101 SUBJECT: GRB 240414A : OHP/T193 second epoch of optical follow-up and afterglow detection DATE: 24/04/14 21:59:49 GMT FROM: Damien Turpin at CEA-Saclay D. Turpin (CEA Paris-Saclay), B. Schneider (MIT), C. Adami, Ny Avo Rakotondrainibe, Olivier Ilbert, S. Basa (LAM/Pytheas/AMU), A. de Ugarte Postigo (OCA/LAM), E. Le Floc'h (CEA Paris-Saclay), S. D. Vergani (GEPI, Obs. de Paris), report on behalf of a larger collaboration: We performed a second epoch of observation of the GRB 240414A afterglow candidate (Caputo et al., GCN 36083, Schneider et al. GCN 36084, Dutton et al. GCN 36097) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. After stacking 8 r-band images (total exp = 4080sec), we clearly detect the optical afterglow with the following preliminary magnitude: ----------------------------------------------- T-T0 (in days, midtime) | mag | filter ----------------------------------------------- 0.7397 | 21.84 ± 0.16 mag (AB) | r' ----------------------------------------------- We also report the g-band magnitude of the afterglow for the previous night (2x120s): ----------------------------------------------- T-T0 (in days, midtime) | mag | filter ----------------------------------------------- 0.0645 | 18.39 ± 0.03 mag (AB) | g' ----------------------------------------------- Based on our two epochs in r-band, we obtain a temporal slope alpha ~ -1.1 which is roughly consistent with the one of Dutton et al. GCN 36097. We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN 36102 table
GRB_name GRB240414A
GCN_number 36102
Detection_method Swift-XRT Det
ra 184.7836°
decl 56.7406°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36102 SUBJECT: GRB 240414A: Enhanced Swift-XRT position DATE: 24/04/14 22:35:36 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 872 s of XRT Photon Counting mode data and 3 UVOT images for GRB 240414A, 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 = 184.78364, +56.74056 which is equivalent to: RA (J2000): 12h 19m 8.07s Dec (J2000): +56d 44' 26.0" with an uncertainty of 3.2 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 36103 table
GRB_name GRB240414A
GCN_number 36103
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36103 SUBJECT: GRB240414A : J-band upper limits from WINTER DATE: 24/04/14 22:55:41 GMT FROM: Viraj Karambelkar at Indian Inst of Tech,Bombay Viraj Karambelkar (Caltech), Tomas Ahumada (Caltech), Geoffrey Mo (MIT), Danielle Frostig (MIT), Robert Stein (Caltech), Nathan Lourie (MIT), Robert Simcoe (MIT), Mansi Kasliwal (Caltech) We observed the field of the GRB 240414A (GCN #36084, #36083, #36087, #36088, #36093, #36095, #36097, #36100, #36101) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1 square degree WINTER camera (Lourie et al. 2020). Our observations started at UTC 2024-04-14T20:16:20 (MJD 60414.45) and lasted a total of 50 minutes. The images were processed through the WINTER data reduction pipeline implemented using mirar ( https://zenodo.org/records/10888437), with image subtraction performed relative to reference images built from the UKIRT Hemisphere Survey (Dye et al. 2017). We do not detect the optical counterpart reported by GCN #36084, #36085, #36097, #36101 in the J-band WINTER images, and derive a limiting mag. of J ~ 19 mag (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 Lucille Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research
GCN 36104 table
GRB_name GRB240414A
GCN_number 36104
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36104 SUBJECT: GRB 240414A: Swift-XRT refined Analysis DATE: 24/04/15 03:00:26 GMT FROM: Phil Evans at U of Leicester S. Dichiara (PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 5.4 ks of XRT data for GRB 240414A, from 9.9 ks to 74.3 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The light curve can be modelled with a power-law decay with a decay index of alpha=1.0 (+/-0.4). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.0 (+0.4, -0.3). The best-fitting absorption column is 3.7 (+8.5, -2.3) x 10^20 cm^-2, consistent with the Galactic value of 1.4 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 3.2 x 10^-11 (3.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.7 (+8.5, -2.3) x 10^20 cm^-2 Galactic foreground: 1.4 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.0 (+0.4, -0.3) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01221714. This circular is an official product of the Swift-XRT team.
GCN 36111 table
GRB_name GRB240414A
GCN_number 36111
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36111 SUBJECT: GRB 240414A: AKO Optical Upper Limit DATE: 24/04/15 10:28:18 GMT FROM: Mohammad Odeh at Al Khatim Observatory M44 Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International Astronomical Center in Abu Dhabi, UAE), Nidhal Guessoum and Dalya Akl (American University of Sharjah, UAE), report: As a follow-up for the GRB 240414A (Caputo et al., GCN 36083), where the optical afterglow was detected by (Schneider et al., GCN 36084; Adami et al., GCN 36085; de Ugarte Postigo et. al., GCN 36087; Dutton et al., GCN 36097; Turpin et. al., GCN 36101). We observed the field of this GRB using our 0.36m f/7.7 robotic telescope. Our observation started on 14 April 2024 at 21:00:26 UT, 18.7 hours after the GRB trigger. No new optical source was detected within the error box (Osborne et al., GCN 36102) down to 19.9 magnitude in the stacked image (total 20x180s, Ic band). The magnitude was estimated using the Atlas catalogue as a reference, and it is not corrected for galactic extinction. Our non-detection is consistent with the results of (Niwano et al., GCN 36088; Peretto et al., GCN 36100; Karambelkar et al., GCN 36103).
GCN 36113 table
GRB_name GRB240414A
GCN_number 36113
Detection_method Optical
redshift 1.8330
Circular_text TITLE: GCN CIRCULAR NUMBER: 36113 SUBJECT: GRB 240414A: Mondy optical observations DATE: 24/04/15 13:04:11 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB-IKI-FuN: We observed the field of GRB 240414A (Caputo et. al., GCN 36083) at redshift z=1.833 (Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087) with 1.5-meter AZT-33IK telescope of Sayan observatory at Mondy. The observations were started on 2024-04-14 (UT) 13:56:41, i.e. ~12 hr since the Swift trigger. We took 45 frame 120 s each in the R-filter. The optical counterpart (Schneider et al., GCN 36084; Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087; Niwano et al., GCN 36088; Lipunov et al., GCN 36095; Dutton et al., GCN 36097; Peretto, GCN 36100; Turpin et al., GCN 36101; Karambelkar et al., GCN 36103) is well detected in the stacked image at coordinates of (J2000) 12:19:08.09 +56:44:28.8. Preliminary photometry of the optical source is following: Date UT_start t-T0 Filter Exp. OT err UL(3sigma) (mid, days) (s) 2024-04-14 13:56:41 0.51395 R 44*120 20.60 0.12 22.2 The magnitudes were calibrated with respect to nearby USNO-B1.0 stars. Assuming no spectral evolution between earlier observations(Turpin et al., GCN 36101), we estimate a power law decay index to be alpha~1.2, which is in agreement with SkyNet observations (Dutton et al., GCN 36097).
GCN 36115 table
GRB_name GRB240414A
GCN_number 36115
Detection_method Swift-UVOT Det
ra 184.7837°
decl 56.7413°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36115 SUBJECT: GRB 240414A: Swift/UVOT Detection DATE: 24/04/15 13:29:21 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and R. Caputo (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240414A 9754s after the BAT trigger (Caputo et al., GCN Circ. 36083). A source consistent with the XRT position (Obsorne et al., GCN Circ. 36102) and the previously reported optical counterpart (Schneider et al., GCN Circ. 36084, Aryan et al., GCN Circ. 36094, Dutton et al., GCN Circ. 36097, Xu et al., GCN Circ. 36105, Pankov et al., GCN Circ. 36113) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 12:19:08.09 = 184.78370 (deg.) Dec (J2000) = +56:44:28.6 = 56.74127 (deg.) with an estimated uncertainty of 0.4 arc sec. (radius, 90% confidence). Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag b 9754 10628 853 19.23+/-0.07 uvm2 15403 16303 885 >20.33 u 22136 22862 707 19.29+/-0.11 v 62457 62769 302 >19.60 uvw1 16310 22129 1262 20.04+/-0.18 uvw2 26698 27465 755 >20.54 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 36117 table
GRB_name GRB240414A
GCN_number 36117
Detection_method Optical
redshift 1.8330
Circular_text TITLE: GCN CIRCULAR NUMBER: 36117 SUBJECT: GRB 240414A: Photometric observation from 2.2m CAHA DATE: 24/04/15 15:11:19 GMT FROM: Antonio de Ugarte Postigo at OCA A. de Ugarte Postigo (CNRS, OCA, LAM), J.F. Agui Fernandez (CAHA), C.C. Thoene (ASU-CAS), Y. Calatayud-Borras and S. Gongora (both CAHA) report: We observed the field of GRB 240414A (Caputo et al. GCN 36083) to obtain photometry of the optical afterglow (Schneider et al. GCN 36084, Dutton et al. GCN 36097, Turpin et al. GCN 36101, Pankov et al. GCN 36113, Siegel et al. GCN 36115) at a redshift of 1.833 (Adami et al. GCN 36085, de Ugarte Postigo et al. GCN 36087). The observation was performed with CAFOS, mounted on the 2.2m Calar Alto Telescope, in Almeria (Spain). Our imaging started at 2024-04-14T23:28:42 UT (21.14 hr after the burst onset) and consisted of 5x200s exposures in each of the g, r, and i bands The afterglow is well detected in all three bands, and had decayed to r(AB) = 22.11+/-0.18 mag, as compared to field stars of the SDSS. Further observations are scheduled.
GCN 36120 table
GRB_name GRB240414A
GCN_number 36120
Detection_method Fermi GBM Det
t_trigger 2:20:39.260 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 36120 SUBJECT: GRB 240414A: Fermi GBM Observation DATE: 24/04/15 20:36:01 GMT FROM: Ava Myers at NASA GSFC A. Myers (NPP/GSFC) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 02:20:39.26 UT on 14 April 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240414A (trigger 734754044/240414098). which was also detected by Swift BAT (R. Caputo et al. 2024, GCN 36083). The event was originally mislabeled as GRB 240414B (Fermi GBM Team, GCN 36612). The Fermi GBM on-ground location is consistent with the Swift BAT position. The angle from the Fermi LAT boresight is 49 degrees. The GBM light curve contains a double emission episode with a duration (T90) of about 82 s (50-300 keV). The time-averaged spectrum from T0-1.5 to T0+80.4 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.9 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 150 +/- 20 keV. The event fluence (10-1000 keV) in this time interval is (5.556 +/- 1.065)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.19 s in the 10-1000 keV band is 2.7 +/- 0.2 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 36131 table
GRB_name GRB240414A
GCN_number 36131
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36131 SUBJECT: GRB 240414A: GMG observation DATE: 24/04/16 06:54:24 GMT FROM: wangbaiting@ynao.ac.cn B.-T. Wang, R.-Z. Li, J. Mao, X.-L. Zhang, J.-M. Bai (YNAO) report: We observed the field of GRB 240414A (Caputo et al. GCN 36083) by the GMG telescope in Yunnan observatories. The observation time began from UT 14:25:26.531 April 14, 2024, about 12 hours from the trigger. The preliminary results are shown as ---------------------------------------------------- UT filter mag ---------------------------------------------------- 2024-04-14T14:25:26.531 sdssr 20.6 ± 0.3 ----------------------------------------------------
GCN 36133 table
GRB_name GRB240414A
GCN_number 36133
Detection_method Optical
ra 184.7836°
decl 56.7406°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36133 SUBJECT: GRB 240414A: GAD Observatory, La Spezia, Italy ,upper limit DATE: 24/04/16 10:25:27 GMT FROM: Claudio Lopresti Claudio Lopresti (Gruppo Astronomia Digitale - GAD Observatory, La Spezia, Italy) Member of: UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili, GRB section. GAD - Gruppo Astronomia Digitale. 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), Unione Astrofili Italiani (UAI) report: We imaged the field of GRB 240414Adetected by SWIFT(trigger 1221714) with the telescope LX200 12” of GAD Observatory, La Spezia, Italy The observations started 1026 min after the GRB trigger, with a Shmidt-Cassegrain telescope D=304 mm with reducer F/D=4.75. at the following position (+/- 2 arcsec): RA (J2000): 12h 19m 8.07s Dec (J2000): +56d 44' 26.0" scope D=300 mm F/D=4.8. Weather conditions were medium. The observation with a series of exposures started at 024-04-14 19:28:17 UT and ended at 2024-04-14 22:27:10 UT We co-added 88 exposures of 90 sec each. Start T0+ End T0+ R lim 1026 min 1205 min 19,9 We did not found any optical counterpart in 12h 19m 8.07s +56d 44' 26.0" position and in the error box of the XRT candidate. ref.: K.L. Page at U Leicester GCN 36083 Magnitudes were estimated with the Gaia EDR3 cat. and are not corrected for galactic dust extinction. Reference: https://www.parcodellestelle.com/ The message may be cited.
GCN 36137 table
GRB_name GRB240414A
GCN_number 36137
Detection_method Optical
redshift 1.8330
Circular_text TITLE: GCN CIRCULAR NUMBER: 36137 SUBJECT: GRB 240414A: AbAO optical upprer limit DATE: 24/04/16 14:12:25 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), R. Ya. Inasaridze (AbAO), A. Pozanenko (IKI), S. Belkin (IKI) report on behalf of GRB-IKI-FuN: We observed the field of GRB 240414A (Caputo et. al., GCN 36083) at redshift z=1.833 (Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087) with 70-cm AS-32 telescope of Abastumani Observatory (AbAO). The observations were started on 2024-04-14 (UT) 22:06:33, i.e. ~20 hr since the Swift trigger. We took 117 frames 60 sec each in the R-filter. The optical counterpart (Schneider et al., GCN 36084; Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087; Niwano et al., GCN 36088; Lipunov et al., GCN 36095; Dutton et al., GCN 36097; Peretto, GCN 36100; Turpin et al., GCN 36101; Karambelkar et al., GCN 36103; Odeh et al., GCN 36111; Pankov et al., GCN 36113; Siegel & Caputo, GCN 36115; de Ugarte Postigo et al., GCN 36117; Xiong et al., GCN 36130; Wang et al., GCN 36131; Lopresti et al., GCN 36133) is not detected in the stacked image of 113x60 sec. Preliminary photometry is following: Date UT_start t-T0 Filter Exp. OT err UL(3sigma) (mid, days) (s) 2024-04-14 22:06:33 0.86281 R 113*60 n/d n.d 21.4 The magnitudes were calibrated with nearby USNO-B1.0 stars. The result is in agreement with observations carried out by other groups, in particular, with (de Ugarte Postigo et al., GCN 36117) at the similar epoch.
GCN 36140 table
GRB_name GRB240414A
GCN_number 36140
Detection_method Swift-BAT Det
ra 184.7810°
decl 56.7340°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36140 SUBJECT: GRB 240414A: Swift-BAT refined analysis DATE: 24/04/16 19:56:23 GMT FROM: Mike Moss at NASA GSFC C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), R. Caputo (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), 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-61 to T+199 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240414A (trigger #1221714) (Caputo, et al., GCN Circ. 36083). The BAT ground-calculated position is RA, Dec = 184.781, 56.734 deg which is RA(J2000) = 12h 19m 07.5s Dec(J2000) = +56d 44' 03.0" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 91%. The mask-weighted light curve shows multiple pulses starting at T0-35 s through T0+40 s, with another pulse at T0+110 s. There may be additional emission prior to the currently available data starting from ~T0-61 s. T90 (15-350 keV) is 88.28 +- 50.41 sec (estimated error including systematics). The time-averaged spectrum from TTBD to TTBD sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.99 +- 0.36, and Epeak of 97.0 +- 62.5 keV (chi squared 46.83 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 3.5 +- 0.2 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T+2.04 sec in the 15-150 keV band is 1.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.49 +- 0.08 (chi squared 53.19 for 57 d.o.f.). 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/1221714
GCN 36147 table
GRB_name GRB240414A
GCN_number 36147
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 36147 SUBJECT: GRB 240414A: Glowbug gamma-ray detection DATE: 24/04/17 14:54:25 GMT FROM: C.C. Cheung at Naval Research Lab C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240414A, which was also detected by Swift/BAT (GCN 36083, 36140) and Fermi/GBM (GCN 36120). The detection occurred during a time of high background, thus complicating the analysis. Using an adaptive window with a resolution of 32-ms, the primary peak was recovered, with a burst onset determined to be 2024-04-14 02:20:36.904 with a duration of 4.1 s and a total significance of about 9.7 sigma. Lower-level emission is observed up to ~T0+30s. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006 Distribution Statement A: Approved for public release. Distribution is unlimited.
GCN 36228 table
GRB_name GRB240414A
GCN_number 36228
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 36228 SUBJECT: GRB 240414A: LBT optical detection DATE: 24/04/22 14:43:25 GMT FROM: Andrea Rossi at INAF A. Rossi, E. Maiorano, E. Palazzi (INAF-OAS), M . De Pasquale (Univ. of Messina), report on behalf of the CIBO collaboration: We observed the field of GRB 240414A (Caputo et al. GCN 36083) simultaneously in the blue and red arms with the g'-, r'-, and z'-bands with the MODS instrument mounted on LBT (Mt Graham, AZ, USA). Observations were obtained at the midtime 05:41 UT on 2024-04-14, 3 hours and 20 minutes after the burst trigger. We detect the optical transient (Schneider et al., GCN 36084, Aryan et al., GCN 36094, Dutton et al., GCN 36097, Xu et al., GCN 36105, Pankov et al., GCN 36113, Wang et al., GCN 36131) in all bands and we measure a preliminary AB magnitudes r'=19.1+-0.1, calibrated against SDSS field stars, and not corrected for the foreground Galactic extinction. We acknowledge the excellent support from the LBTO and LBT-INAF staff, particularly A. Cardwell, J. Williams, F. Cusano and D. Paris, in obtaining these observations.
GCN 36229 table
GRB_name GRB240414A
GCN_number 36229
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36229 SUBJECT: GRB 240414A: AMI-LA radio observations DATE: 24/04/22 15:06:17 GMT FROM: Lauren Rhodes at Oxford Lauren Rhodes, Rob Fender (Oxford), Dave Green, Dave Titterington (Cambridge) report: We observed the field of the afterglow candidate GRB 240414A (GCN #36083) with the Arcminute Microkelvin Imager Large-Array (AMI-LA) at 15.5 GHz beginning at 18:54UT on 20-Apr-2024 for a total of 4 hours. The flux standard 3c286 was used to calibrate the bandpass response and flux scale of the AMI-LA and J1219+4829 was used as an interleaved complex gain calibrator. We do not detect any radio emission at the position of the afterglow candidate as reported in GCN #36102 at a 3 sigma upper limit of 297uJy/beam. We thank the staff at the Mullard Radio Astronomy Observatory for carrying out these observations and operating the AMI-LA.
GCN 36231 table
GRB_name GRB240414A
GCN_number 36231
Detection_method Other
ra 184.7837°
decl 56.7413°
Circular_text TITLE: GCN CIRCULAR NUMBER: 36231 SUBJECT: GRB 240414A: radio detection with the VLA DATE: 24/04/22 16:59:02 GMT FROM: Stefano Giarratana at University of Bologna S. Giarratana (INAF-OAB), M. Giroletti (INAF-IRA), G. Ghirlanda (INAF-OAB), N. Di Lalla (Stanford Univ.), N. Omodei (Stanford Univ.) At 01:42:45 UT on 2024 April 17 (T_mid = 2.99 days post-burst) the Karl G. Jansky VLA started observing the field of GRB 240414A (Caputo et al., GCN 36083) at a central frequency of 6 and 10 GHz. The standard J1331+3030 (3C286) was used as bandpass and flux density calibrator, while J1217+5835 was used as complex gain calibrator. From a preliminary analysis, an unresolved radio source is clearly detected at both frequencies at a position: RA: 12:19:08.08 +- 0.01 Dec: +56:44:28.7 +- 0.2 The surface brightness peak is 40 uJy/beam and 60 uJy/beam at 6 and 10 GHz, respectively. The r.m.s. noise level of the images is 7 uJy/beam at both 6 and 10 GHz. The synthesized beams are 4.1 x 3.0 arcsec (PA: 70deg) at 6 GHz and 2.7 x 1.9 arcsec (PA: 76deg) at 10 GHz. While no source is detected at the aforementioned position in previous radio surveys (FIRST, NVSS, VLASS), their r.m.s. noise levels (1sigma) is above 100 uJy/b, well above the derived surface brightness peak. Therefore, we cannot exclude the contribution from the GRB host galaxy yet. We would like to thank the staff of the VLA for approving, executing, and processing the observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. These observations were carried out as part of project SF161095, approved in the framework of the Fermi - NRAO joint program agreement.
GCN 36318 table
GRB_name GRB240414A
GCN_number 36318
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 36318 SUBJECT: GRB 240414A: NOEMA detection DATE: 24/04/26 15:39:53 GMT FROM: Antonio de Ugarte Postigo at OCA A. de Ugarte Postigo (CNRS/OCA & LAM), M. Bremer (IRAM), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez (CAHA), S. Antier (OCA), S. Basa (LAM), M. Michalowski (AOI-AMU), D. A. Perley (LJMU), J.-G. Ducoin (CPPM) report: We observed the field of GRB 240414A (Caputo et al. GCN 36083; Myers et al. GCN 36120; Cheung et al. GCN 36147) with the NOEMA interferometer, located at the Plateau de Bure (France). The observation, performed on the 23rd April, was tuned with sidebands at 74 and 90 GHz. When combining all the data, we obtain a weak, 3-sigma detection at the position of the afterglow (Schneider et al. GCN 36084; Adami et al. GCN 36085; de Ugarte Postigo GCN 36087; Dutton et al. 36097; Turpin et al. GCN 36101; Osborne et al. GCN 36102; Dichiara et al. GCN 36104; Pankov et al. GCN 36113; Siegel et al. GCN 36115; de Ugarte Postigo et al. GCN 36117; Wang et al. GCN 36131; Rossi et al. GCN 36228; Rhodes et al. GCN 36229; Giarratana et al. GCN 36231) with a flux density of ~55 uJy. Based on observations carried out under project number W23DI with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
GCN 37576 table
GRB_name GRB240414A
GCN_number 37576
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37576 SUBJECT: GRB 240414A: further radio observations with the VLA DATE: 24/09/20 14:43:52 GMT FROM: Stefano Giarratana at INAF-OAB S. Giarratana (INAF-OAB), M. Giroletti (INAF-IRA), G. Ghirlanda (INAF-OAB), N. Di Lalla (Stanford Univ.), N. Omodei (Stanford Univ.), O. S. Salafia (INAF-OAB) At 01:21:27 UT on 2024 April 23 (T_mid = 8.98 days post-burst) and at 05:22:12 on 2024 May 15 (T_mid = 31.15 days post-burst) the Karl G. Jansky VLA started observing the field of GRB 240414A (Caputo et al., GCN 36083) at a central frequency of 6 and 10 GHz. The standard J1331+3030 (3C286) was used as bandpass and flux density calibrator, while J1217+5835 was used as complex gain calibrator. From a preliminary analysis, the radio source coincident with GRB 240414A (Rhodes et al., GCN 36229; Giarratana et al., GCN 36231; de Ugarte Postigo et al., GCN 36318) is detected at both frequencies: ================================================================ T_mid Freq Peak r.m.s. Beam PA [days] [GHz] [uJy/b] [uJy/b] [arcsec] [deg] ================================================================ 8.98 6 33 9 4.64x3.44 -86 8.98 10 48 7 3.16x2.24 -82 31.15 6 18 6 1.15x0.92 -40 31.15 10 21 6 0.67x0.56 -38 ================================================================ We would like to thank the staff of the VLA for approving, executing, and processing the observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. These observations were carried out as part of project SF161095, approved in the framework of the Fermi - NRAO joint program agreement.