GRB190204A

This page lists all entries on GRB190204A in GRBweb

Summary IPN Swift GCN 23852 GCN 23854 GCN 23856 GCN 23857 GCN 23861 GCN 23862 GCN 23863 GCN 23867 GCN 23868 GCN 23869 GCN 23872 GCN 23877

Summary table
Variable Value Source
T0 5:45:55 UTC GCN_circulars,MAXI Det
ra 351.4774° Swift
decl 54.8764° Swift
pos_error 5.18e-05° Swift
T90 26.4 s Swift
T90_start 5:46:01 UTC Swift
fluence 1.30e-05 erg/cm² Swift
T100 32.4 s
GBM_located False
mjd 58518.240219907406 GCN_circulars,MAXI Det
IPN table
GRB_name GRB190204A
ra 351.5333°
decl 54.8833°
pos_error 5.00e-02°
Swift table
GRB_name GRB190204A
t_trigger 5:46:01 UTC
ra 351.4774°
decl 54.8764°
pos_error 5.18e-05°
T90 26.4 s
fluence 1.30e-05 erg/cm²
GCN 23852 table
GRB_name GRB190204A
GCN_number 23852
Detection_method Swift Det
t_trigger 5:46:01 UTC
ra 351.5140°
decl 54.8780°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23852 SUBJECT: GRB 190204A: Swift detection of a burst with a possible optical counterpart DATE: 19/02/04 06:12:47 GMT FROM: Aaron Tohuvavohu at PSU/Swift A. Y. Lien (GSFC/UMBC), M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), N. J. Klingler (PSU), A. Melandri (INAF-OAB), D. M. Palmer (LANL) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 05:46:01 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190204A (trigger=887579 and 887580). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 351.514, +54.878 which is RA(J2000) = 23h 26m 03s Dec(J2000) = +54d 52' 42" 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 20 sec. The peak count rate was ~28000 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 05:47:15.7 UT, 75.0 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 351.47755, 54.87623 which is equivalent to: RA(J2000) = 23h 25m 54.61s Dec(J2000) = +54d 52' 34.4" with an uncertainty of 3.6 arcseconds (radius, 90% containment). This location is 119 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 http://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 4.36 x 10^21 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 5.72e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 250 seconds with the U filter starting 295 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 23:25:54.58 = 351.47742 DEC(J2000) = +54:52:34.9 = 54.87637 with a 90%-confidence error radius of about 0.63 arc sec. This position is 4.2 arc sec. from the center of the XRT error circle. The estimated magnitude is 17.76 with a 1-sigma error of about 0.15. No correction has been made for the expected extinction corresponding to E(B-V) of 0.38. This GRB resulted in two BAT triggers in the on-board processing (#887579 at 05:46:01 and #887580 at 05:46:06). We adopt the first trigger number and time as T0. Burst Advocate for this burst is A. Y. Lien (amy.y.lien 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: /too.html.)
GCN 23854 table
GRB_name GRB190204A
GCN_number 23854
Detection_method MAXI Det
t_trigger 5:45:55 UTC
ra 351.3410°
decl 54.7610°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23854 SUBJECT: GRB 190204A: MAXI/GSC detection DATE: 19/02/04 07:23:51 GMT FROM: Satoshi Nakahira at RIKEN T. Oeda (Tokyo Tech), M. Nakajima (Nihon U.), S. Nakahira (RIKEN), H. Negoro, A. Sakamaki, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), T. Mihara, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, T. Hashimoto, A. Yoshida (AGU), N. Kawai, M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech), S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, T. Midooka (JAXA), Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), M. Yamauchi, K. Hidaka, S. Iwahori (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), M. Shidatsu (Ehime U.), Y. Kawakubo (LSU) report on behalf of the MAXI team: The MAXI/GSC nova alert system triggered a bright X-ray transient at 05:45:55 UT on February 4, 2019. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (351.341 deg, 54.761 deg) = (23 25 21, +54 45 38) (J2000) with a 90% C.L. statistical error of 0.10 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 2286 +- 126 mCrab (4.0-10.0keV, 1 sigma error). Without assumptions on the source constancy,we obtain a rectangular error box for the transient source with the following corners: (R.A., Dec) = (350.693, 54.635) deg = (23 22 46, +54 38 05) (J2000) (R.A., Dec) = (350.828, 54.512) deg = (23 23 18, +54 30 43) (J2000) (R.A., Dec) = (352.146, 54.985) deg = (23 28 35, +54 59 05) (J2000) (R.A., Dec) = (352.013, 55.110) deg = (23 28 03, +55 06 35) (J2000). The trigger time and position was consistent with that of GRB 190204A detected by Swift (Lien et al. 2019, GCN 23852).
GCN 23856 table
GRB_name GRB190204A
GCN_number 23856
Detection_method AstroSat CZTI
t_trigger 5:46:06.500 UTC
T90 11.9 s
Circular_text TITLE: GCN CIRCULAR NUMBER: 23856 SUBJECT: GRB 190204A: AstroSat CZTI detection DATE: 19/02/04 11:43:22 GMT FROM: Vidushi Sharma at IUCAA T. Khanam, V. Sharma, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed the detection of a long GRB 190204A, which was also detected by Swift (Lien A. Y. et al., GCN Circ 23852) and MAXI/GSC (Oeda T. et al., GCN Circ 23854). The source was clearly detected in the 20-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 05:46:06.5 UT. The measured peak count rate is 1455 cts/s above the background in the combined data of four quadrants, with a total of 5579 cts. The local mean background count rate was 569 cts/s. Using cumulative rates, we measure a T90 of 11.9 s. In preliminary analysis, we find that 578 Compton events are associated with this event. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN 23857 table
GRB_name GRB190204A
GCN_number 23857
Detection_method Swift-XRT Other
ra 351.4775°
decl 54.8766°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23857 SUBJECT: GRB 190204A: Swift-XRT refined Analysis DATE: 19/02/04 11:45:54 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU) and A.Y. Lien report on behalf of the Swift-XRT team: We have analysed 6.4 ks of XRT data for GRB 190204A (Lien et al. GCN Circ. 23852), from 81 s to 13.0 ks after the BAT trigger. The data comprise 926 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 351.4775, +54.8766 which is equivalent to: RA (J2000): 23 25 54.59 Dec(J2000): +54 52 35.7 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The late-time light curve (from T0+4.8 ks) can be modelled with a power-law decay with a decay index of alpha=1.36 (+/-0.16). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.740 (+0.022, -0.018). The best-fitting absorption column is consistent with the Galactic value of 4.4 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.83 (+0.12, -0.11) and a best-fitting absorption column of 5.4 (+0.8, -0.7) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.6 x 10^-11 (6.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.4 (+0.8, -0.7) x 10^21 cm^-2 Galactic foreground: 4.4 x 10^21 cm^-2 Excess significance: 2.4 sigma Photon index: 1.83 (+0.12, -0.11) If the light curve continues to decay with a power-law decay index of 1.36, the count rate at T+24 hours will be 9.9 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x 10^-13 (6.8 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/00887579. This circular is an official product of the Swift-XRT team.
GCN 23861 table
GRB_name GRB190204A
GCN_number 23861
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23861 SUBJECT: GRB 190204A: COATLI Optical Detection of the Fading Afterglow DATE: 19/02/04 12:54:35 GMT FROM: Alan M. Watson at Instituto de Astronomia UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego González (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos Román-Zúñiga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja (GSFC) report: We observed the field of GRB 190204A (Lien et al., GCN Circ. 23852) with the COATLI 50-cm telescope and interim imager at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir (http://coatli.astroscu.unam.mx) from 2019-02-04 05:46:35 to 2019-02-04 05:57:30 (from 34 to 689 seconds after the trigger), obtaining a total of 345 seconds of exposure in the w filter. At the position of the UVOT afterglow candidate (Lien et al., GCN Circ. 23852), we detect a source that fades from w = 13.5 to w = 17.5 over the course of our observations. A power-law fit suggest a temporal index of -1.44 +/- 0.03. Our w magnitudes are calibrated against the USNO-B1 catalog (adjusted to an approximate AB system) and are not corrected for Galactic extinction in the direction of the GRB. We thank the COATLI technical team and the staff of the Observatorio Astronómico Nacional.
GCN 23862 table
GRB_name GRB190204A
GCN_number 23862
Detection_method Swift-XRT Det
ra 351.4782°
decl 54.8764°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23862 SUBJECT: GRB 190204A: Enhanced Swift-XRT position DATE: 19/02/04 13:35:49 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 2532 s of XRT Photon Counting mode data and 6 UVOT images for GRB 190204A, 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 = 351.47820, +54.87637 which is equivalent to: RA (J2000): 23h 25m 54.77s Dec (J2000): +54d 52' 34.9" with an uncertainty of 1.5 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 23863 table
GRB_name GRB190204A
GCN_number 23863
Detection_method Swift-UVOT Det
ra 351.4774°
decl 54.8764°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23863 SUBJECT: GRB 190204A: Swift/UVOT Detection DATE: 19/02/04 13:47:25 GMT FROM: Paul Kuin at MSSL Paul Kuin (UCL/MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190204A 84 s after the BAT trigger (Lien et al., GCN Circ. 23852). The updated UVOT position is: The preliminary UVOT position is: RA (J2000) = 23:25:54.58 = 351.47744 (deg.) Dec (J2000) = +54:52:35.1 = 54.87642 (deg.) with an estimated uncertainty of 0.4 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 84 233 147 16.84 +/- 0.07 white 576 596 20 18.66 +/- 0.20 v 626 1247 78 18.30 +/- 0.23 b 551 1507 85 19.29 +/- 0.21 u 296 546 246 17.85 +/- 0.10 w1 676 1470 97 >18.3 m2 651 1444 97 >19.5 w2 602 1395 97 >18.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.38 in the direction of the burst (Schlegel et al. 1998).
GCN 23867 table
GRB_name GRB190204A
GCN_number 23867
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 23867 SUBJECT: GRB 190204A: Mondy optical upper limit DATE: 19/02/04 18:55:55 GMT FROM: Alina Volnova at SAI MSU A. Volnova (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), R. Inasaridze (AbAO), E. Mazaeva (IKI), S. Belkin (IKI) report on behalf of IKI-GRB-FuN: We observed the field of localization of GRB 190204A (Lien et al. GCN 23852) with AZT-33IK telescope of Sayan observatory (Mondy). We started observations on Feb. 04 (UT) 13:10:12 in R-filter. We do not detect the optical afterglow (Lien et al. GCN 23852; Watson et al., GCN 23861; Kuin et al., GCN 23863). Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) (3 sigma) 2019-02-04 13:10:12 0.32583 R 25*120 n/d n/d 20.3 The photometry is based on nearby SDSS stars: SDSS_id R_Lupton J232549.70+545348.8 16.978 0.014 J232550.46+545253.5 17.052 0.014 J232544.33+545253.6 16.085 0.013 Our observation confirm rapid initial decay of the afterglow detected by UVOT (Kuin et al., GCN 23863).
GCN 23868 table
GRB_name GRB190204A
GCN_number 23868
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 23868 SUBJECT: GRB 190204A: SAO RAS optical observations DATE: 19/02/04 19:02:35 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin (SAO RAS) report on behalf of larger GRB follow-up team. We observed the field of the GRB 190204A (Lien et al., GCNC #23852) with the Zeiss-1000 telescope of SAO RAS (+ CCD photometer) on February, 4, 15:36:17--16:44:07 UT (mid. time 16:10:12). The observations were carried out in Rc band. We detected the OT (Lien et al., GCNC #23852; Watson et al., GCNC #23861; Kuin & Lien, GCNC #23863) in the stacked 12 x 300 sec. image. Preliminary brightness of OT is R = 21.9 +/- 0.1 (T-T0 = 0.4335 d). The calibrations is based on nearby SDSS stars (Volnova et al., GCNC #23867), magnitudes converted with the Lupton 2005 equations.
GCN 23869 table
GRB_name GRB190204A
GCN_number 23869
Detection_method Konus-Wind Det
t_trigger 5:45:55.832 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 23869 SUBJECT: Konus-Wind observation of GRB 190204A DATE: 19/02/04 19:23:03 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 190204A (Swift detection: Lien et al., GCN Circ. 23852; MAXI/GSC detection: Oeda et al., GCN Circ. 23854; AstroSat CZTI detection: Khanam et al., GCN Circ. 23856) triggered Konus-Wind at T0=20755.832 s UT (05:45:55.832). The burst light curve shows a multipeaked structure started at ~T0-1 s with a total duration of ~49 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 5.31(-0.51,+0.53)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+8.288 s, of 2.17(-0.28,+0.29)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+17.408 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 = -0.88(-0.07,+0.08), the high energy photon index beta = -2.43(-0.30,+0.18), the peak energy Ep = 308(-30,+33) keV (chi2 = 76/98 dof). The spectrum near the maximum count rate (measured from T0+7.680 to T0+9.472 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 = -0.85(-0.07,+0.08), the high energy photon index beta = -2.70(-0.58,+0.25), the peak energy Ep = 387(-39,+46) keV (chi2 = 69/66 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB190204_T20755/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 23872 table
GRB_name GRB190204A
GCN_number 23872
Detection_method Swift-BAT Det
ra 351.4910°
decl 54.8840°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23872 SUBJECT: GRB 190204A: Swift-BAT refined analysis DATE: 19/02/05 03:33:29 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-234 to T+968 sec from the recent telemetry downlink, we report further analysis of BAT GRB 190204A (trigger #887579 and #887580) (Lien et al., GCN Circ. 23852). In this circular, we adopted the trigger time from the first trigger (#887579), 2019-02-04 05:46:01 UT, to be consistent with the T0 quoted in other circulars. The BAT ground-calculated position is RA, Dec = 351.491, 54.884 deg which is RA(J2000) = 23h 25m 57.8s Dec(J2000) = +54d 53' 02.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 48%. The mask-weighted light curve shows several overlapping pulses that starts at ~T-7 s and ends at ~T+55 s. The main peak occurs at ~T+5 s. T90 (15-350 keV) is 26.4 +- 7.5 sec (estimated error including systematics). The time-averaged spectrum from T-6.93 to T+53.82 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.30 +- 0.04. The fluence in the 15-150 keV band is 1.3 +- 0.03 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+4.55 sec in the 15-150 keV band is 30.5 +- 0.9 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/887580/BA/ (Please note that this page shows the automatic analysis from the 2nd trigger #887580, because BAT associated most of the data with this trigger ID. Thus, the T0 displayed in the webpage is 4.995 sec later than the trigger time referenced in this circular.)
GCN 23877 table
GRB_name GRB190204A
GCN_number 23877
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 23877 SUBJECT: GRB 190204A: CALET Gamma-Ray Burst Monitor detection DATE: 19/02/06 14:36:42 GMT FROM: Valentin Pal'shin at AGU T. Ito, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, H. Morita, Y. Sone (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), A. V. Penacchioni, P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 190204A (Swift-BAT triggers #887579 and #887580: Lien et al., GCN Circ. 23852, Sakamoto et al., GCN Circ.23872; MAXI/GSC detection: Oeda et al., GCN Circ. 23854; AstroSat CZTI detection: Khanam et al., GCN Circ. 23856; Konus-Wind observation: Kozlova et al., GCN Circ. 23869) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 05:46:05.075 UTC on 4 February 2019. No real-time CGBM GCN notice was distributed about this trigger because the real-time communication from the ISS was off (loss of signal). The burst signal was seen by all CGBM detectors. The burst light curve shows a single pulse which starts at T-7.7 sec, peaks at 1.1 sec and ends at T+5.8 sec. The T90 and T50 durations measured by the SGM data are 11.0 +- 2.0 sec and 2.2 +- 0.5 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1233294225/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.