GRB180316A

This page lists all entries on GRB180316A in GRBweb

Summary IPN Swift GCN 22500 GCN 22501 GCN 22502 GCN 22503 GCN 22504 GCN 22507 GCN 22508 GCN 22509 GCN 22510 GCN 22511 GCN 22512 GCN 22514 GCN 22516 GCN 22517 GCN 22518 GCN 22519 GCN 22548

Summary table
Variable Value Source
T0 4:57:25 UTC GCN_circulars,Swift Det
ra 265.4286° Swift
decl 0.7483° Swift
pos_error 5.44e-05° Swift
T90 87.0 s Swift
T90_start 4:57:25 UTC Swift
fluence 4.90e-06 erg/cm² Swift
T100 87.0 s
GBM_located False
mjd 58193.20653935185 GCN_circulars,Swift Det
IPN table
GRB_name GRB180316A
ra 265.4375°
decl 0.7333°
pos_error 5.00e-02°
Swift table
GRB_name GRB180316A
t_trigger 4:57:25 UTC
ra 265.4286°
decl 0.7483°
pos_error 5.44e-05°
T90 87.0 s
fluence 4.90e-06 erg/cm²
GCN 22500 table
GRB_name GRB180316A
GCN_number 22500
Detection_method Swift Det
t_trigger 4:57:25 UTC
ra 265.4360°
decl 0.7370°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22500 SUBJECT: GRB 180316A: Swift detection of a burst DATE: 18/03/16 05:09:31 GMT FROM: David Palmer at LANL A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A. Deich (PSU), D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 04:57:25 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180316A (trigger=814677). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 265.436, +0.737 which is RA(J2000) = 17h 41m 45s Dec(J2000) = +00d 44' 11" 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 ~3000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 04:59:00.5 UT, 95.4 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 265.4290, 0.7497 which is equivalent to: RA(J2000) = +17h 41m 42.96s Dec(J2000) = +00d 44' 58.9" with an uncertainty of 6.1 arcseconds (radius, 90% containment). This location is 52 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 took a finding chart exposure of 150 seconds with the White filter starting 104 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.27. Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 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/too.html.)
GCN 22501 table
GRB_name GRB180316A
GCN_number 22501
Detection_method Swift-XRT Other
ra 265.4289°
decl 0.7483°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22501 SUBJECT: GRB 180316A: Prompt enhanced Swift-XRT position DATE: 18/03/16 05:31:08 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 180316A, we find an enhanced XRT position of the afterglow: RA, Dec: 265.4289, 0.7483 which is equivalent to: RA (J2000) = 17 41 42.94 Dec (J2000) = +00 44 54.0 with an uncertainty of 2.1 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/814677. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team.
GCN 22502 table
GRB_name GRB180316A
GCN_number 22502
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22502 SUBJECT: GRB180316A: MASTER-IAC optical detection DATE: 18/03/16 06:23:08 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, N.Tyurina, V.Kornilov, E.Gorbovskoy, P.Balanutsa, V.Vladimirov, A.Krylov, I.Gorbunov, A.Kuznetsov, V.Chazov, D. Kuvshinov, D.Zimnukhov (Lomonosov Moscow State University, SAI), R. Rebolo, M. Serra-Ricart (The Instituto de Astrofisica de Canarias), R.Podesta, C.Lopez, F. Podesta (Observatorio Astronomico Felix Aguilar (OAFA),National University of San Juan, Argentina), H. Levato, C. Saffe (Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina), D.Buckley, S. Potter (South African Astronomical Observatory), O.Gres, N.M.Budnev (Irkutsk State University), A. Tlatov, V.Senik, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) V.Yurkov, A.Gabovich, Yu.Sergienko (Blagoveschensk Educational State University, Blagoveschensk), MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in IAC was pointed to the GRB180316A (Melandri et al GCN22500) 15 sec after notice time and 44 sec after trigger time at 2018-03-16 04:58:09 UT. There is new changing OT at SWIFT XRT (Evans et al. GCN 22501) coordinates 17 41 42.94 +00 44 54.0 The 5-sigma upper limit on the first 10s image is 17.06mag The message may be cited. ==================================================================== The observations made on zenit distance = 42 degrees, galaxy latitude b = 15 degree. The moon ( 2 % bright part) below the horizon (The altitude of the Moon is -22 degree ). The sun altitude is -30.4 degree. The object can be observed till sunrise at 2018-03-16 07:14:55
GCN 22503 table
GRB_name GRB180316A
GCN_number 22503
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22503 SUBJECT: GRB180316A: MASTER-IAC OT light curve DATE: 18/03/16 07:15:51 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, N.Tyurina, V.Kornilov, E.Gorbovskoy, P.Balanutsa, V.Vladimirov, A.Krylov, I.Gorbunov, A.Kuznetsov, V.Chazov, D. Kuvshinov, D.Zimnukhov (Lomonosov Moscow State University, SAI), R. Rebolo, M. Serra-Ricart (The Instituto de Astrofisica de Canarias), R.Podesta, C.Lopez, F. Podesta (Observatorio Astronomico Felix Aguilar (OAFA),National University of San Juan, Argentina), H. Levato, C. Saffe (Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina), D.Buckley, S. Potter (South African Astronomical Observatory), O.Gres, N.M.Budnev (Irkutsk State University), A. Tlatov, V.Senik, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) V.Yurkov, A.Gabovich, Yu.Sergienko (Blagoveschensk Educational State University, Blagoveschensk), MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in IAC was pointed to the GRB180316A (Melandri et al GCN22500) 15 sec after notice time and 44 sec after trigger time at 2018-03-16 04:58:09 UT . There is OT(GCN 22502) as the GRB counterpart coordinates (17h 41m 42s.82, + 00d 44m 53s.6 ) error =+-0.5" The automatical OT light curve available at http://master.sai.msu.ru/static/OT/LC_GRB180316A.png The message may be cited. ==================================================================== The observations made on zenit distance = 42 degrees, galaxy latitude b = 15 degree. The moon ( 2 % bright part) below the horizon (The altitude of the Moon is -22 degree ). The sun altitude is -30.4 degree. The object can be observed till sunrise at 2018-03-16 07:14:55
GCN 22504 table
GRB_name GRB180316A
GCN_number 22504
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22504 SUBJECT: GROND observations of GRB 180316A DATE: 18/03/16 10:40:27 GMT FROM: Patricia Schady at MPE/Swift P. Schady and S. Steinmassl (both MPE) report: We observed the field of GRB 180316A (Swift trigger 814677; Melandri et al., GCN #22500) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 06:46 UT on March 16, 1.8 hours after the GRB trigger. They were performed at an average seeing of 1.5" and at an average airmass of 1.5. We clearly detect the NIR/optical transient of GRB 180316A within the enhanced XRT position (Evans et al., GCN #22501), in agreement with the optical transient detected with MASTER (Lipunov et al., GCN #22502, #22503). Based on the first 4 minutes of exposure, we measure the following magnitudes (all in AB system): g' = 19.4 +/- 0.1 mag r' = 19.0 +/- 0.1 mag i' = 18.9 +/- 0.1 mag z' = 18.8 +/- 0.1 mag J = 18.2 +/- 0.1 mag H = 18.0 +/- 0.1 mag K = 17.8 +/- 0.2 mag Given magnitudes are calibrated against GROND zeropoints in g'r'i'z' and 2MASS field stars in JHK, and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.24 in the direction of the burst (Schlafly & Finkbeiner 2011). We acknowledge the excellent support from the TiO and the current observer at the 2.2m in La Silla, Sam Kim and Charlotte Brand.
GCN 22507 table
GRB_name GRB180316A
GCN_number 22507
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22507 SUBJECT: GRB 180316A: LCO Cerro Tololo observations DATE: 18/03/16 12:10:56 GMT FROM: Renato Martone at Universita' di Ferrara R. Martone, C. Guidorzi (U. Ferrara), S. Kobayashi (LJMU), C.G. Mundell (U. Bath), A. Gomboc (U. Nova Gorica), I.A. Steele (LJMU) on behalf of a large collaboration report: We observed the field of Swift GRB180316A (Melandri et al., GCN 22500) on March 16, from 07:38 to 07:59 UT (mid time of 0.12 days post burst) with a 1-m unit LCO telescope in Cerro Tololo in the SDSS r’ i' filters. We detect the optical afterglow (Lipunov et al., GCN 22502; Schady and Steinmassl, GCN 22504) with the following magnitudes: Mid time since GRB Exp Filter Magnitude (days) (s) ------------------------------------------------------------- 0.11 4x120 SDSS-R 19.04 +- 0.05 0.12 4x120 SDSS-I 18.88 +- 0.05 ------------------------------------------------------------- as calibrated against nearby SDSS stars.
GCN 22508 table
GRB_name GRB180316A
GCN_number 22508
Detection_method Swift-XRT Det
ra 265.4285°
decl 0.7481°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22508 SUBJECT: GRB 180316A: Enhanced Swift-XRT position DATE: 18/03/16 14:26:58 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 4963 s of XRT Photon Counting mode data and 8 UVOT images for GRB 180316A, 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 = 265.42854, +0.74813 which is equivalent to: RA (J2000): 17h 41m 42.85s Dec (J2000): +00d 44' 53.3" with an uncertainty of 1.4 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 22509 table
GRB_name GRB180316A
GCN_number 22509
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22509 SUBJECT: GRB 180316A: RATIR Optical Observations DATE: 18/03/16 14:37:38 GMT FROM: Nat Butler at Az State U Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 180316A (Melandri, et al., GCN 22500) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2018/03 16.39 to 2018/03 16.52 UTC (4.34 to 7.49 hours after the BAT trigger), obtaining a total of 2.29 hours exposure in the r and i bands. The afterglow is well-detected within the Swift-XRT error circle (Evans, et al., GCN 22501). In comparison with the USNO-B1 catalog, we obtain: r = 20.07 +/- 0.02 i = 19.87 +/- 0.02 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. The source appears so fade in flux with time as t^(-1.4+/-0.1). We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 22510 table
GRB_name GRB180316A
GCN_number 22510
Detection_method Swift-UVOT Det
ra 265.4286°
decl 0.7482°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22510 SUBJECT: GRB 180316A: Swift/UVOT Detection DATE: 18/03/16 15:48:27 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (UCL-MSSL) and A. Melandri (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180316A 105 s after the BAT trigger (Melandri et al., GCN Circ. 22500). A fading source consistent with the enhanced XRT position (Evans et al. GCN Circ. 22508) and the optical transient reported by Lipunov et al. (GCN Circ. 22503), Shady & Steinmassl (GCN Circ. 22504) and Martone et al. (GCN Circ. 22507), Butler et al. (GCN Circ. 22509) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 17:41:42.87 = 265.42861 (deg.) Dec (J2000) = +00:44:53.7 = 0.74824 (deg.) with an estimated uncertainty of 0.42 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 finding chart (white_fc) and early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_fc 105 254 147 16.27 ± 0.03 white 596 616 20 17.40 ± 0.11 v 646 839 39 17.15 ± 0.18 b 572 592 20 17.40 ± 0.15 u 317 566 246 16.44 ± 0.04 w1 695 22410 1175 >20.4 m2 12527 12578 50 >19.2 w2 622 6753 255 >19.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.28 in the direction of the burst (Schlegel et al. 1998).
GCN 22511 table
GRB_name GRB180316A
GCN_number 22511
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22511 SUBJECT: GRB 180316A: Swift-XRT refined Analysis DATE: 18/03/16 15:57:42 GMT FROM: Phil Evans at U of Leicester S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A. Tohuvavohu (PSU) and A. Melandri report on behalf of the Swift-XRT team: We have analysed 6.1 ks of XRT data for GRB 180316A (Melandri et al. GCN Circ. 22500), from 101 s to 28.6 ks after the BAT trigger. The data comprise 534 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 22501). The late-time light curve (from T0+4.4 ks) can be modelled with an initial power-law decay with an index of alpha=-0.0 (+/-0.6), followed by a break at T+8729 s to an alpha of 2.1 (+/-0.3). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.94 (+0.07, -0.04). The best-fitting absorption column is 2.038 (+0.286, -0.012) x 10^21 cm^-2, consistent with the Galactic value of 2.0 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.05 (+/-0.16) and a best-fitting absorption column of 3.3 (+/-0.7) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (5.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.3 (+/-0.7) x 10^21 cm^-2 Galactic foreground: 2.0 x 10^21 cm^-2 Excess significance: 3.2 sigma Photon index: 2.05 (+/-0.16) If the light curve continues to decay with a power-law decay index of 2.1, the count rate at T+24 hours will be 2.9 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-13 (1.7 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/00814677. This circular is an official product of the Swift-XRT team.
GCN 22512 table
GRB_name GRB180316A
GCN_number 22512
Detection_method Swift-BAT Det
ra 265.4220°
decl 0.7370°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22512 SUBJECT: GRB 180316A: Swift-BAT refined analysis DATE: 18/03/16 19:49:29 GMT FROM: Amy Lien at GSFC J. R. Cummings (CPI), S. D. Barthelmy (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180316A (trigger #814677) (Melandri et al., GCN Circ. 22500). The BAT ground-calculated position is RA, Dec = 265.422, 0.737 deg which is RA(J2000) = 17h 41m 41.3s Dec(J2000) = +00d 44' 14.3" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 29%. The mask-weighted light curve shows a main structure with several overlapping pulses that starts at ~ T-15 s and ends at ~ T+30 s. The major peak occurs at ~ T+1 s. In addition, there are some weak emission before the main structure that starts at ~ T-80 s, and a weak tail afterward that lasts until ~ T+40 s. T90 (15-350 keV) is 87.0 +- 20.6 sec (estimated error including systematics). The time-averaged spectrum from T-79.73 to T+37.27 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.46 +- 0.12. The fluence in the 15-150 keV band is 4.9 +- 0.4 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+1.27 sec in the 15-150 keV band is 3.3 +- 0.5 ph/cm2/sec. All the quoted errors are at the 90% confidence level.
GCN 22514 table
GRB_name GRB180316A
GCN_number 22514
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 22514 SUBJECT: GRB 180316A: RATIR Optical Observations, Possible Re-brightening DATE: 18/03/17 15:19:48 GMT FROM: Nat Butler at Az State U Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 180316A (Melandri,, et al., GCN 22500) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2018/03 17.39 to 2018/03 17.52 UTC (28.35 to 31.55 hours after the BAT trigger), obtaining a total of 2.36 hours exposure in the r and i bands. The optical afterglow (e.g., Lipunov, et al., GCN 22502) is again cleanly detected. In comparison with the USNO-B1 catalog, we obtain: r = 20.23 +/- 0.02 i = 19.93 +/- 0.01 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. These magnitudes are comparable to those reported for RATIR for 2018/03.16 (Butler, et al., GCN 22509). During that observation, the afterglow was fading strongly. We again observe the afterglow to be fading, as t^(-0.7+/-0.3), and we infer that the afterglow may have brightened between our epochs, at a time around 1 day after the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 22516 table
GRB_name GRB180316A
GCN_number 22516
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22516 SUBJECT: GRB 180316A: TSHAO optical observations DATE: 18/03/18 18:33:32 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), A. Kusakin (FAPHI), A. Pozanenko (IKI), I. Reva (FAPHI), E. Mazaeva (IKI), M. Krugov (FAPHI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB GRB 180316A (Melandri et al., GCN 22500) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on Mar. 17 (UT) 23:19:40. We obtained several images in R-filter. The optical afterglow (Lipunov et al., GCN 22502; Schady et al. GCN 22504; Martone et al. GCN 22507; Butler et al., GCN 22509; Breeveld et al. GCN 22510) is marginally detected in a stacked image. Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-03-17 23:19:40 1.78280 R 36*60 21.5 0.5 21.0 The photometry is based on several nearby USNO-B1.0 stars.
GCN 22517 table
GRB_name GRB180316A
GCN_number 22517
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 22517 SUBJECT: GRB 180316A: MITSuME Okayama optical upper limits DATE: 18/03/19 07:23:59 GMT FROM: Katsuhiro L. Murata at Nagoya U K. L. Murata, R. Itoh, T. Yoshii, Y. Tachibana, S. Harita, K. Morita, T. Ozawa, H. Mamiya, K. Shiraishi, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 180316A (A. Melandri et al., GCN Circular #22500) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Okayama Astrophysical Observatory, Japan. The observation started on 16:19:04 UT. We did not find any new point source within enhanced XRT circle (P.A. Evans et al., GCN Circular #22508) in all three bands. We obtained following limits for the magnitudes. T0+[hour] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------------ ------------------------------------------- 12.22 19:44:32 1980 >17.3 >17.4 >17.4 ------------------------------------------------------------ ------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 catalog for flux calibration.
GCN 22518 table
GRB_name GRB180316A
GCN_number 22518
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 22518 SUBJECT: GRB 180316A: MITSuME Akeno optical upper limits DATE: 18/03/19 07:26:57 GMT FROM: Katsuhiro L. Murata at Nagoya U K. L. Murata, R. Itoh, T. Yoshii, Y. Tachibana, S. Harita, K. Morita, T. Ozawa, H. Mamiya, K. Shiraishi, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 180316A (A. Melandri et al., GCN Circular #22500) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 16:39:08 UT. We did not find any new point source within enhanced XRT circle (P.A. Evans et al., GCN Circular #22508) in all three bands. We obtained following limits for the magnitudes. T0+[hour] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------------ ------------------------------------------- 11.71 18:28:36 11620 >20.6 >19.7 >18.9 ------------------------------------------------------------ ------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 catalog for flux calibration.
GCN 22519 table
GRB_name GRB180316A
GCN_number 22519
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22519 SUBJECT: GRB 180316A: RATIR Optical Observations DATE: 18/03/19 14:38:20 GMT FROM: Alan M. Watson at Instituto de Astronomia UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 180316A (Melandri et al., GCN 22500) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2018/03 19.38 to 2018/03 19.52 UTC (76.23 to 79.44 hours after the BAT trigger), obtaining a total of 2.44 hours exposure in the r and i bands. For a source within the Swift-XRT error circle, in comparison with the USNO-B1 and 2MASS catalogs, we obtain the following 3-sigma upper limits: r > 23.72 i > 23.59 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 22548 table
GRB_name GRB180316A
GCN_number 22548
Detection_method Konus-Wind Det
t_trigger 4:57:25.869 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22548 SUBJECT: Konus-Wind observation of GRB 180316A DATE: 18/03/26 15:10:45 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 180316A (Swift detection of a burst: Melandri et al., GCN 22500; Cummings et al., GCN 22512) triggered Konus-Wind at T0=17845.869 s UT (04:57:25.869). The burst light curve shows a single emission episode which starts at ~T0-13 s and has a total duration of ~29 s. The emission is seen up to ~1.2 MeV. As observed by Konus-Wind, the burst had a fluence of 1.43(-0.21,+0.38)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+2.976 s, of 2.77(-1.16,+1.49)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+16.640 s) is best fit in the 20 keV - 1.2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.23(-0.23,+0.27), and Ep = 439(-139,+424) keV (chi2 = 74/60 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -1.87 (chi2 = 74/59 dof). The spectrum near the peak count rate (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model with alpha = -1.19(-0.22,+0.26), and Ep = 498(-165,+498) keV (chi2 = 54/61 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -1.75 (chi2 = 53/60 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB180316_T17845/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.