GRB180905A

This page lists all entries on GRB180905A in GRBweb

Summary IPN Swift GCN 23201 GCN 23207 GCN 23208 GCN 23210 GCN 23211 GCN 23212 GCN 23213 GCN 23215

Summary table
Variable Value Source
T0 13:57:46 UTC GCN_circulars,Swift Det
ra 91.0627° Swift
decl -4.5701° Swift
pos_error 1.94e-04° Swift
T90 165.3 s Swift
T90_start 13:57:46 UTC Swift
fluence 4.20e-06 erg/cm² Swift
T100 165.3 s
GBM_located False
mjd 58366.581782407404 GCN_circulars,Swift Det
IPN table
GRB_name GRB180905A
ra 91.0333°
decl -4.5833°
pos_error 5.00e-02°
Swift table
GRB_name GRB180905A
t_trigger 13:57:46 UTC
ra 91.0627°
decl -4.5701°
pos_error 1.94e-04°
T90 165.3 s
fluence 4.20e-06 erg/cm²
GCN 23201 table
GRB_name GRB180905A
GCN_number 23201
Detection_method Swift Det
t_trigger 13:57:46 UTC
ra 91.0350°
decl -4.5910°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23201 SUBJECT: GRB 180905A: Swift detection of a burst DATE: 18/09/05 14:07:32 GMT FROM: David Palmer at LANL V. D'Elia (SSDC), A. D'Ai (INAF-IASFPA), J.D. Gropp (PSU), J. A. Kennea (PSU), M. J. Moss (George Washington University), K. L. Page (U Leicester), D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 13:57:46 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180905A (trigger=859421). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 91.035, -4.591 which is RA(J2000) = 06h 04m 08s Dec(J2000) = -04d 35' 27" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As is usual for an image trigger, no obvious variation is visible in the immediately-available lightcurve. The XRT began observing the field at 14:00:12.3 UT, 145.9 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 91.0602, -4.5724 which is equivalent to: RA(J2000) = 06h 04m 14.45s Dec(J2000) = -04d 34' 20.6" with an uncertainty of 5.1 arcseconds (radius, 90% containment). This location is 112 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. The initial flux in the 2.5 s image was 2.03e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 135 seconds with the White filter starting 153 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 0.60. Burst Advocate for this burst is V. D'Elia (delia AT ssdc.asi.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 23207 table
GRB_name GRB180905A
GCN_number 23207
Detection_method Swift-XRT Det
ra 91.0627°
decl -4.5701°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23207 SUBJECT: GRB 180905A: Enhanced Swift-XRT position DATE: 18/09/05 18:09:33 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 1840 s of XRT Photon Counting mode data and 4 UVOT images for GRB 180905A, 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 = 91.06265, -4.57015 which is equivalent to: RA (J2000): 06h 04m 15.04s Dec (J2000): -04d 34' 12.6" with an uncertainty of 1.8 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 23208 table
GRB_name GRB180905A
GCN_number 23208
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 23208 SUBJECT: GRB 180905A: BOOTES-3/YA optical observations DATE: 18/09/05 20:41:11 GMT FROM: Youdong HU at IAA-CSIC, UGR Y.-D. Hu, E. Fernandez-Garcia, J. C. Tello, A. Ayala and A. J. Castro-Tirado (IAA-CSIC), I. Carrasco and C. Perez del Pulgar (Univ. de Malaga), M. D. Caballero-Garcia (ASU-CAS, CZ) and R. Querel (NIWA), on behalf of a larger collaboration, report: The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New Zealand) automatically responded to the Swift trigger of GRB 180905A (D'Elia et al. GCNC 23201) ~0.55 h after the burst as soon as it became few degrees above the horizon. The first image (clear filter) were obtained starting at 14:30:52 UT. At the position of the Swift/XRT enhanced X-ray position (Beardmore et al. GCNC 23207), no optical afterglow is detected down to 20 mag on a 720s co-added image at 14:38:31 (mid-exposure), in agreement with the non-detection by Swift/UVOT. Further analysis is ongoing. We thank the staff at NIWA for its excellent support.
GCN 23210 table
GRB_name GRB180905A
GCN_number 23210
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23210 SUBJECT: GRB 180905A: Swift-XRT refined Analysis DATE: 18/09/06 02:40:59 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester) and V. D'Elia report on behalf of the Swift-XRT team: We have analysed 9.0 ks of XRT data for GRB 180905A (D'Elia et al. GCN Circ. 23201), from 152 s to 35.0 ks after the BAT trigger. The data comprise 135 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN Circ. 23207). The light curve can be modelled with a power-law decay with a decay index of alpha=1.556 (+0.029, -0.027). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.45 (+0.11, -0.10). The best-fitting absorption column is 5.7 (+1.1, -1.0) x 10^21 cm^-2, in excess of the Galactic value of 3.5 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.68 (+0.28, -0.26) and a best-fitting absorption column of 5.5 (+2.2, -1.8) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.0 x 10^-11 (6.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.5 (+2.2, -1.8) x 10^21 cm^-2 Galactic foreground: 3.5 x 10^21 cm^-2 Excess significance: 1.8 sigma Photon index: 1.68 (+0.28, -0.26) If the light curve continues to decay with a power-law decay index of 1.556, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.9 x 10^-14 (1.2 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/00859421. This circular is an official product of the Swift-XRT team.
GCN 23211 table
GRB_name GRB180905A
GCN_number 23211
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 23211 SUBJECT: GRB 180905A: MITSuME Akeno optical upper limits DATE: 18/09/06 05:53:52 GMT FROM: Katsuhiro L. Murata at Nagoya U M. Niwano, R. Itoh, K. L. Murata, Y. Tachibana, S. Harita, K. Morita, K. Shiraishi, K. Iida, R. Adachi, M. Oeda, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 180905A (V. D'Elia et al., GCN Circular #23201) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 2018-09-05 17:29:51.08 UT. We did not find any point source at the enhanced position of the XRT error circle (A.P. Beardmore et al., GCN Circular #23207) in all three bands. We obtained following 5-sigma upper limits for the magnitudes. T0+[min] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------------------------------------------------------- 202.32 18:46:39 8,100 >18.9 >18.6 >18.4 ------------------------------------------------------------------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used UCAC-4 catalog for flux calibration.
GCN 23212 table
GRB_name GRB180905A
GCN_number 23212
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23212 SUBJECT: GRB 180905A: RATIR Optical and NIR Observations DATE: 18/09/06 13:30:04 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 180905A (D'Elia et al., GCN Circ. 23201) 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 2018/09 6.42 to 2018/09 6.51 UTC (20.07 to 22.23 hours after the BAT trigger), obtaining a total of 1.17 hours exposure in the r and i bands and 0.57 hours exposure in the Z, Y, J, and H bands. For a source within the Swift-XRT enhanced error circle (Beardmore et al., GCN Circ. 23207), in comparison with the USNO-B1 and 2MASS catalogs, we obtain the following upper limits (3-sigma): r > 23.26 i > 23.10 Z > 22.21 Y > 22.06 J > 21.60 H > 21.25 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 23213 table
GRB_name GRB180905A
GCN_number 23213
Detection_method Swift-BAT Det
ra 91.0380°
decl -4.5920°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23213 SUBJECT: GRB 180905A, Swift-BAT refined analysis DATE: 18/09/06 16:12:08 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), V. D'Elia (SSDC), 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-239 to T+250 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180905A (trigger #859421) (D'Elia et al., GCN Circ. 23201). The BAT ground-calculated position is RA, Dec = 91.038, -4.592 deg which is RA(J2000) = 06h 04m 09.2s Dec(J2000) = -04d 35' 31.9" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 29%. The mask-weighted light curve shows a weak long pulse that starts at ~T-60 s and ends at ~T+150 s. Note that the burst came into the BAT field of view at T-84 s, and BAT entered the SAA after ~ T+250 s. Therefore, there might be additional burst emission before and after the available event data range. T90 (15-350 keV) is 165.3 +- 28.9 sec (estimated error including systematics). The time-averaged spectrum from T-58.9 to T+146.7 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.60 +- 0.12. The fluence in the 15-150 keV band is 4.2 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-2.09 sec in the 15-150 keV band is 1.0 +- 0.3 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/859421/BA/
GCN 23215 table
GRB_name GRB180905A
GCN_number 23215
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23215 SUBJECT: GRB 180905A: Swift/UVOT Upper Limits DATE: 18/09/09 19:37:38 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and V. D'Elia (SSDC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180905A 154 s after the BAT trigger (D'Elia et al., GCN Circ. 23201). No optical afterglow consistent with the XRT position (D'Elia et al. GCN Circ. 23201) is detected in the initial UVOT exposures, as confirmed by Bootes (Hu et al., GCN Circ. 23208), MITSUME (Niwano et al., GCN Circ. 23211) and RATIR (Watson et al., GCN Circ. 23212). Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 154 289 133 >20.4 white 154 6385 373 >21.1 v 5316 5515 197 >19.1 b 4700 6335 393 >20.5 u 4495 6130 393 >20.3 w1 5726 5925 197 >19.6 m2 5520 5720 197 >19.8 w2 5111 5311 197 >19.2 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.60 in the direction of the burst (Schlegel et al. 1998).