GRB240118A

This page lists all entries on GRB240118A in GRBweb

Summary Fermi GBM IPN GCN 35558 GCN 35560 GCN 35563 GCN 35564 GCN 35567 GCN 35568 GCN 35570 GCN 35572 GCN 35573 GCN 35580 GCN 35588 GCN 35607

Summary table
Variable Value Source
GRB_name_Fermi GRB240118075
T0 1:48:09 UTC GCN_circulars,Fermi GBM final loc
ra 18.5750° IPN
decl 29.7833° IPN
pos_error 5.00e-02° IPN
T90 54.017 s Fermi_GBM
T90_error 0.362 s Fermi_GBM
T90_start 1:48:54.753 UTC Fermi_GBM
fluence 5.52e-04 erg/cm² Fermi_GBM
fluence_error 1.11e-07 erg/cm² Fermi_GBM
redshift 0.6800 GCN_circulars,Optical
T100 99.77 s
GBM_located False
mjd 60327.075104166666 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB240118075
trigger_name bn240118075
ra 14.1000°
decl 30.8800°
pos_error 2.48e+00°
datum 2024-01-18
t_trigger 1:48:09.440 UTC
T90 54.017 s
T90_error 0.362 s
T90_start 1:48:54.753 UTC
fluence 5.52e-04 erg/cm²
fluence_error 1.11e-07 erg/cm²
flux_1024 9.46e+01 erg/cm²/s
flux_1024_error 5.48e-01 erg/cm²/s
flux_1024_time 7.25e+01 erg/cm²/s
flux_64 1.29e+02 erg/cm²/s
flux_64_error 2.40e+00 erg/cm²/s
IPN table
GRB_name GRB240118A
ra 18.5750°
decl 29.7833°
pos_error 5.00e-02°
GCN 35558 table
GRB_name GRB240118A
GCN_number 35558
Detection_method Fermi GBM final loc
t_trigger 1:48:09 UTC
ra 14.1000°
decl 30.9000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35558 SUBJECT: GRB 240118A: Fermi GBM Final Real-time Localization DATE: 24/01/18 01:58:38 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 01:48:09 UT on 18 Jan 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240118A (trigger 727235294.440514 / 240118075). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 14.1, Dec = 30.9 (J2000 degrees, equivalent to J2000 00h 56m, 30d 53'), with a statistical uncertainty of 1.0 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/bn240118075/quicklook/glg_skymap_all_bn240118075.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/bn240118075/quicklook/glg_healpix_all_bn240118075.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240118075/quicklook/glg_lc_medres34_bn240118075.gif
GCN 35560 table
GRB_name GRB240118A
GCN_number 35560
Detection_method Fermi LAT Det
t_trigger 1:48:09.440 UTC
ra 18.5700°
decl 29.7900°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35560 SUBJECT: GRB 240118A: Fermi-LAT detection DATE: 24/01/18 09:58:01 GMT FROM: Elisabetta Bissaldi at Politecnico and INFN Bari E. Bissaldi (Politecnico and INFN Bari), F. Longo (University and INFN Trieste) and Makoto Arimoto (Kanazawa University) report on behalf of the Fermi-LAT Collaboration: At 01:48:09.44 on January, 18, 2024 Fermi-LAT detected high-energy emission from GRB 240118A, which was also detected by Fermi-GBM (trigger 727235294 / 240118075, GCN #35558). The best LAT on-ground location is found to be RA, Dec = 18.57, 29.79 (J2000) with an error radius of 0.05 deg (90 % containment, statistical error only). This was 69 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The photon flux above 100 MeV in the time interval 0-2000 s after the GBM trigger time is (7.3 +/- 1.0)E-6 ph/cm2/s. The estimated photon index above 100 MeV is -1.9 +/- 0.1. The highest-energy photon is a 41 GeV event, which is observed 732 seconds after the GBM trigger. A Swift ToO has been requested for this burst. The Fermi-LAT point of contact for this burst is Elisabetta Bissaldi (elisabetta.bissaldi@ba.infn.it). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 35563 table
GRB_name GRB240118A
GCN_number 35563
Detection_method Fermi GBM Det
t_trigger 1:48:09.440 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35563 SUBJECT: GRB 240118A: Fermi GBM Observation DATE: 24/01/18 16:07:47 GMT FROM: rachel.hamburg@ijclab.in2p3.fr R. Hamburg (CNRS/IN2P3), S. Dalessi (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 01:48:09.44 UT on 18 January 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240118A (trigger 727235294/240118075), which was also detected by Fermi-LAT (Bissaldi et al. 2024, GCN 35560). The Fermi GBM on-ground location (GCN 35558) is consistent with the Fermi-LAT position. The angle from the Fermi LAT boresight is 64 degrees. The GBM light curve consists of multiple bright pulses with a duration (T90) of about 54 s (50-300 keV). The time-averaged spectrum from T0+0 s to T0+150 s is best fit by a Band function with Epeak = 374 +/- 3 keV, alpha = -0.71 +/- 0.004, and beta = -2.35 +/- 0.02. The event fluence (10-1000 keV) in this time interval is (5.81 +/- 0.01)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+72.5 s in the 10-1000 keV band is 94.6 +/- 0.5 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 35564 table
GRB_name GRB240118A
GCN_number 35564
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35564 SUBJECT: GRB 240118A: NuSTAR Detection of a Long GRB DATE: 24/01/18 17:14:54 GMT FROM: Brian Grefenstette at Caltech/NuSTAR B. Grefenstette on behalf of the NuSTAR Search for INteresting Gamma-ray Signals (SINGS) working group: The NuSTAR SINGS working group reports the detection of prompt emission of the GRB 240118A in the NuSTAR CsI anti-coincidence shields. Thus GRB was identified through a blind search using the CsI shield rates with a trigger time (2024-01-18 01:48:46). This is consistent with the time of the delayed large peak seen in the GBM lightcurve from Fermi GBM (Fermi Team GCN 35558, Hamburg GCN 35563) which arrives ~40-sec after the initial GBM trigger at 01:48:09. Data from the CdZnTe detectors have not yet been downloaded from the spacecraft. The burst shows at least three broad peaks in the CsI shields from both NuSTAR FPMs, peaking at 3000-5000 counts per second (the background in the shields was roughly 1000 cps). The automated light curve report for this GRB and discovery report can be found here: https://nustarsoc.caltech.edu/NuSTAR_Public/grbs/reports/2024/240118A/ …where further offline analysis will be performed once more data are downloaded from NuSTAR.
GCN 35567 table
GRB_name GRB240118A
GCN_number 35567
Detection_method Konus-Wind Det
t_trigger 1:48:28.107 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35567 SUBJECT: Konus-Wind detection of GRB 240118A DATE: 24/01/18 18:44:56 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long, very bright GRB 240118A (Fermi GBM observation: Hamburg et al., GCN 35563; Fermi LAT detection: Bissaldi et al., GCN 35560; NuSTAR detection: Grefenstette, GCN 35564) triggered Konus-Wind (KW) at T0=6508.107 s UT (01:48:28.107). The burst light curve shows a multi-peaked structure, which starts at ~T0-2.4 s, peaks at ~T0+37.5 s, and has a total duration of ~90 s. The emission is seen up to ~15 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240118_T06508/ As observed by Konus-Wind, the burst had a fluence of (8.24 ± 0.38)x10^-4 erg/cm^2 and a 64-ms peak energy flux, measured from T0 + 37.568 s, of (6.65 ± 0.63)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+90.880 s) is best fit in the 20 keV - 15 MeV range by a GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.69 (-0.03,+0.03), the high energy photon index beta = -2.37 (-0.05,+0.05), the peak energy Ep = 402 (-12,+13) keV, chi2 = 167/97 dof. The spectrum near the peak count rate (measured from T0+36.352 s to T0+38.144 s) is best fit in the 20 keV - 15 MeV range by a GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.61 (-0.06,+0.07), the high energy photon index beta = -2.62 (-0.21,+0.15), the peak energy Ep = 634 (-51,+55) keV, chi2 = 74/66 dof. All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary.
GCN 35568 table
GRB_name GRB240118A
GCN_number 35568
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35568 SUBJECT: GRB 240118A: Swift/BAT-GUANO detection of a burst outside the coded FOV DATE: 24/01/18 21:03:45 GMT FROM: Jimmy DeLaunay at Penn State James DeLaunay (PSU), Samuele Ronchini (PSU), Gayathri Raman (PSU), Aaron Tohuvavohu (U Toronto), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report: Swift/BAT did not localize GRB 240118A onboard (T0: 2024-01-18T01:48:09.44 UTC, Fermi trig 727235294, Konus-Wind GCN 35567, NuSTAR GCN 35564) The Fermi notice, distributed in near real-time, triggered the Swift Mission Operations Center operated Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1). Upon trigger by this notice, GUANO sent a command to the Swift Burst Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from [-50,+150] seconds around the time of the burst. All the requested event mode data was delivered to the ground. The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), performed on the temporal window [T0+32 s, T0+72 s] (centered around the peak count rate), detects the burst with a sqrt(TS) of 125.5 in a 16.384 s analysis time bin, starting at T0 + 43.808. NITRATES results are consistent with a burst coming from outside the FOV, with DeltaLLHOut of -930.9. See Section 9.1 and Figures 10 and 17 in the NITRATES paper for brief descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and DeltaLLHOut. GUANO is a fully autonomous, extremely low latency, spacecraft commanding pipeline designed for targeted recovery of BAT event mode data around the times of compelling astrophysical events to enable more sensitive GRB searches. A live reporting of Swift/BAT event data recovered by GUANO can be found at: https://www.swift.psu.edu/guano/
GCN 35570 table
GRB_name GRB240118A
GCN_number 35570
Detection_method Konus-Wind Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 35570 SUBJECT: GRB 240118A: NuSTAR Offline Analysis of the GRB DATE: 24/01/18 21:58:42 GMT FROM: Brian Grefenstette at Caltech/NuSTAR B. Grefenstette on behalf of the NuSTAR Search for INteresting Gamma-ray Signals (SINGS) working group: The NuSTAR SINGS working group has performed additional offline analysis of the GRB 240118A detected by Fermi (Hamburg, GCN 35563), Swift BAT (DeLaunay, GCN 35568), and Konus-Wind (Frederiks, GCN 35567). Using the localization from the Fermi LAT (Bissaldi, GCN 35560) we estimate that the GRB was only ~12-degrees from the telescope boresight at 2024-01-18T01:48:09. The CsI shields do not clearly detect the precursor event that triggered the GBM at 2024-01-18T01:48:09. However, there are multiple strong peaks ~40-sec later. We have updated the automated GRB report to include the recently downloaded X-ray data here: https://nustarsoc.caltech.edu/NuSTAR_Public/grbs/reports/2024/240118A/ This includes enhanced light curves showing 1-Hz CsI anticoincidence shield data as well as the CdZnTe X-ray data binned at 2-s intervals. The shield data clearly resolves the GRB into at least three main peaks with significant substructure. All three peaks are also seen in the X-ray detectors, with excess counts that extend up to at least 200 keV. However, the response files of the detectors is complicated due to the intervening material so detailed spectroscopic analysis of the individual bursts cannot be performed at this time.
GCN 35572 table
GRB_name GRB240118A
GCN_number 35572
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35572 SUBJECT: GRB 240118A: AbAO optical upper limit DATE: 24/01/19 01:25:42 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO), S. Belkin (IKI) report on behalf of IKI GRB FuN: We observed the field of Fermi LAt localization of GRB 240118A (Bissaldi, GCN 35560) and detected also Fermi GBM (Fermi GBM team, GCN 35558; Hamburg, GCN 35563), NuSTAR (Grefenstette, GCN 35564), Swift BAT (DeLaunay, GCN 35568), and Konus-Wind (Frederiks, GCN 35567) with AS-32 telescope of Abastumani observatory (AbAO) in R-filter starting on 2024-01-18 (UT) 16:47:55. No optical candidate is detected in the LAT localization area (Bissaldi, GCN 35560). Preliminary photometry of the filed is following Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) (mid, days) (s) 2024-01-18 16:47:55 0.625069 R 40*60 n/d n/d 17.4 The photometry is based on nearby USNO-B1.0 stars.
GCN 35573 table
GRB_name GRB240118A
GCN_number 35573
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35573 SUBJECT: GRB 240118A: Swift ToO observations DATE: 24/01/19 04:29:59 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/LAT GRB 240118A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021644 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/LAT 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 35580 table
GRB_name GRB240118A
GCN_number 35580
Detection_method Fermi LAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 35580 SUBJECT: GRB 240118A: GRBAlpha detection DATE: 24/01/19 17:40:49 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa (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. Kolar, 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 bright long-duration GRB 240118A (Fermi/GBM detection: GCN 35558; Fermi/LAT detection: GCN 35560; NuSTAR detection: GCN 35564; Konus/Wind detection: GCN 35567; Swift/BAT detection: GCN 35522; INTEGRAL/SPI-ACS detection: trigger no. 10477) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048). The detection was confirmed at the peak time 2024-01-18 01:49:22 UTC. The T90 duration measured by GRBAlpha is 58 s and the overall significance during T90 reaches 174 sigma. The light curve shows a multiple-peaked structure which is consistent with light curves observed by other missions. However, GRBAlpha was passing through the van Allen radiation belt during the entire burst duration and therefore the measured count rate is subject to a higher variable background which cannot be distinguished from the burst itself. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240118A_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 35588 table
GRB_name GRB240118A
GCN_number 35588
Detection_method Optical
redshift 0.6800
Circular_text TITLE: GCN CIRCULAR NUMBER: 35588 SUBJECT: GRB 240118A: Mondy optical observations DATE: 24/01/20 23:54:29 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of IKI GRB FuN: We observed the field of Fermi LAT localization of GRB 240118A (Bissaldi, GCN 35560), which was also detected by Fermi GBM (Fermi GBM team, GCN 35558; Hamburg, GCN 35563), NuSTAR (Grefenstette, GCN 35564), Konus-Wind (Frederiks, GCN 35567), Swift BAT (DeLaunay, GCN 35568), and GRBAlpha (Dafcikova et al., GCN 35580), and the localization area observed by MASTER-Tunka observatory (Lipunov et al., GCN 35561) and Abastumani observatory (Pankov et al., GCN 35572). Observations started on 2024-01-18 (UT) 14:13:46 with AZT-33IK telescope of Sayan observatory (Mondy) in the R-filter. The observations have been carried out in moderate weather conditions with FWHM of 2.5". We report observations of XRT candidates detected in the Swift TOO program (Evans et al., GCN 35573). XRT #1 - out of FOV XRT #2 - matches bright USNO-B1.0 star with R2=9.98 mag XRT #3 - within the XRT #3 error circle we detect a faint source, which matches SDSS J011408.49+294753.1 source with SDSS DR12 r'= 22.117 and redshift of z_phot = 0.68 XRT #4 - out of FOV XRT #5 - matches bright Gaia DR3 star with G=6.48 mag XRT #6 - out of FOV XRT #7 - out of FOV Preliminary photometry of the faint source XRT #3 suggested as an X-ray afterglow (Beardmore et al., GCN 35587) is following Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) (mid, days) (s) 2024-01-18 14:13:46 0.537932 R 29*120 22.1 0.3 22.1 The photometry is based on nearby USNO-B1.0 stars. At this time we cannot say anything about the variability of the source. The source at coordinates 01:14:08.48 +29:47:53.2, spatially coinciding with the galaxy SDSS J011408.49+294753.1 with a redshift of 0.68 could be a host galaxy of GRB 240118A.
GCN 35607 table
GRB_name GRB240118A
GCN_number 35607
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35607 SUBJECT: GRB 240118A: Swift/UVOT Upper Limits DATE: 24/01/23 17:35:39 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240118A 96191 s after the LAT trigger (Bissaldi et al., GCN Circ. 35560). No optical afterglow consistent with the LAT position or the XRT position (Beardmore et al., GCN Circ. 35587) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag u 96191 103639 3161 >20.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.056 in the direction of the burst (Schlegel et al. 1998).