GRB171001A

This page lists all entries on GRB171001A in GRBweb

Summary IPN Swift GCN 21946 GCN 21952 GCN 21953 GCN 21954 GCN 21955 GCN 21956 GCN 21957 GCN 21958 GCN 21959

Summary table
Variable Value Source
T0 18:25:40 UTC GCN_circulars,Swift Det
ra 22.0774° Swift
decl -11.8941° Swift
pos_error 1.94e-04° Swift
T90 22.8 s Swift
T90_start 18:25:40 UTC Swift
fluence 6.40e-07 erg/cm² Swift
T100 22.8 s
GBM_located False
mjd 58027.76782407407 GCN_circulars,Swift Det
IPN table
GRB_name GRB171001A
ra 22.0875°
decl -11.9000°
pos_error 5.00e-02°
Swift table
GRB_name GRB171001A
t_trigger 18:25:40 UTC
ra 22.0774°
decl -11.8941°
pos_error 1.94e-04°
T90 22.8 s
fluence 6.40e-07 erg/cm²
GCN 21946 table
GRB_name GRB171001A
GCN_number 21946
Detection_method Swift Det
t_trigger 18:25:40 UTC
ra 22.0880°
decl -11.8930°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21946 SUBJECT: GRB 171001A: Swift detection of a burst DATE: 17/10/01 18:38:25 GMT FROM: David Palmer at LANL A. Y. Lien (GSFC/UMBC), P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the Swift Team: At 18:25:40 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 171001A (trigger=775553). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 22.088, -11.893 which is RA(J2000) = 01h 28m 21s Dec(J2000) = -11d 53' 35" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 30 sec. The peak count rate was ~900 counts/sec (15-350 keV), at ~20 sec after the trigger. The XRT began observing the field at 18:28:53.9 UT, 193.7 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 22.0774, -11.8940 which is equivalent to: RA(J2000) = 01h 28m 18.59s Dec(J2000) = -11d 53' 38.5" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 37 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. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (3.56 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.9 (+3.76/-3.10) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 197 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 0.03. 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: http://www.swift.psu.edu/too.html.)
GCN 21952 table
GRB_name GRB171001A
GCN_number 21952
Detection_method Swift-XRT Det
ra 22.0774°
decl -11.8942°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21952 SUBJECT: GRB 171001A: Enhanced Swift-XRT position DATE: 17/10/01 20:57:34 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 1293 s of XRT Photon Counting mode data and 2 UVOT images for GRB 171001A, 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 = 22.07740, -11.89417 which is equivalent to: RA (J2000): 01h 28m 18.58s Dec (J2000): -11d 53' 39.0" 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 21953 table
GRB_name GRB171001A
GCN_number 21953
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21953 SUBJECT: GRB171001A: D50 optical limit DATE: 17/10/01 22:50:08 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek, Jan Strobl and Rene Hudec (ASU CAS Ondrejov) We observed the field of the Swift GRB171001A (trigger #775553, Lien et al. GCNC 21946) with the 0.5m telescope of Ondrejov observatory, the obseration started at 21:17UT, i.e. about 2.9h after trigger and lasted for 30 miutes, when the field became observable. On a series of unfiltered exposures we do not detect any new object within or in the vicinity of the XRT errorbox (Evans et al., GCNC 21952) down to the USNO-B/R2 calibrated limit of R>20.0.
GCN 21954 table
GRB_name GRB171001A
GCN_number 21954
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21954 SUBJECT: GRB 171001A: IRSF Observation DATE: 17/10/02 01:07:51 GMT FROM: Katsuhiro L. Murata at Nagoya U R. Itoh (Tokyo Tech), K. L. Murata (Tokyo Tech), K. Morihana (Nagoya U.) and T. Nagayama (Kagoshima U) We observed the field of GRB 171001A (Lien et al., GCNCircular #21946) with the near-infrared (J, H, Ks) simultaneous imaging camera SIRIUS attached to 1.4 m telescope IRSF (InfraRed Survey Facility) in Sutherland observatory, South Africa. The observations started on 2017-10-01 19:16:51 UT. We detected the afterglow within the enhanced XRT error circle (Evans et al., GCN Circular #21952) in J band. The measured magnitudes (Vega magnitude system) were listed as below. T0+[min] MID-UT T-EXP[sec] J H Ks ------------------------------------------------------------------------------------------------- ~48 19: 31 1270 17.0+-1.1 >16.3 >16.0 ------------------------------------------------------------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time Given magnitudes were calibrated against 2MASS point sources in this field. This observation was carried out by IRSF and OISTER collaboration.
GCN 21955 table
GRB_name GRB171001A
GCN_number 21955
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21955 SUBJECT: GRB 171001A: Swift/UVOT Detection DATE: 17/10/02 09:52:10 GMT FROM: Paul Kuin at MSSL N. P. M. 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 171001A 198 s after the BAT trigger (Lien et al., GCN Circ. 21946). The source was found in the IR J band by Itoh et al. (GCN. Circ. # 21954). We find a source consistent with the XRT position (Evans et al. GCN Circ. 21952) in the initial UVOT exposures. 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 198 1359 373 21.23 +/- 0.30 v 686 1409 58 >18.2 b 612 1503 93 >19.8 u 356 780 265 >20.3 w1 736 1458 58 >20.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.03 in the direction of the burst (Schlegel et al. 1998).
GCN 21956 table
GRB_name GRB171001A
GCN_number 21956
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21956 SUBJECT: GRB 171001A: Swift-XRT refined Analysis DATE: 17/10/02 11:19:25 GMT FROM: Phil Evans at U of Leicester J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU) and A.Y. Lien report on behalf of the Swift-XRT team: We have analysed 6.0 ks of XRT data for GRB 171001A (Lien et al. GCN Circ. 21946), from 176 s to 52.2 ks after the BAT trigger. The data comprise 11 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 21952). The light curve can be modelled with an initial rise, with a power-law index of alpha=-0.13 (+0.19, -0.21), followed by a break at T+1318 s to an alpha of 1.88 (+0.24, -0.18). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.09 (+0.21, -0.19). The best-fitting absorption column is 6.2 (+4.6, -2.7) x 10^20 cm^-2, consistent with the Galactic value of 3.6 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 3.1 x 10^-11 (3.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.2 (+4.6, -2.7) x 10^20 cm^-2 Galactic foreground: 3.6 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.09 (+0.21, -0.19) If the light curve continues to decay with a power-law decay index of 1.88, the count rate at T+24 hours will be 2.1 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.6 x 10^-15 (7.8 x 10^-15) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00775553. This circular is an official product of the Swift-XRT team.
GCN 21957 table
GRB_name GRB171001A
GCN_number 21957
Detection_method Optical
ra 22.0778°
decl -11.8942°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21957 SUBJECT: GRB 171001A: Nanshan-0.36m optical afterglow detections DATE: 17/10/02 12:21:09 GMT FROM: Dong Xu at NAOC/CAS H.J. Tan (CCU), H.X. Feng, D. Xu, Z.P. Zhu (NAOC), Y.D. Hu (IAA-CSIC), Y. Qin (Geneva Obs.), X. Gao (Urumqi No.1 Senior High School) report: We observed the field of GRB 171001A (Lien et al., GCN 21946) using the 0.36m robotic telescope located at Nanshan, Xinjiang, China. Observations started at 18:37:21 UT on 2017-10-01, i.e, 701 sec after the BAT trigger, and all imaged were taken without filter. The optical afterglow was detected at the XRT position (Evans et al., GCN 21952) with coordinates R.A. (J2000) = 01:28:18.67 Dec. (J2000) = -11:53:39.0 with an uncertainty of ~0.5 arcsec. Our photometry was summarized as follows: ======================================== Tmid(s)+T0 Exptime(s) Mag(R) MagErr 741 40*2 >17.60 902 60*2 17.93 0.13 1102 60*3 18.00 0.11 1328 90*2 18.55 0.11 1522 90*2 18.60 0.20 3327 90*8 >18.75 ======================================== Note: (1) Photometry is calibrated with stars in the USNO B1 catalogue in the R-filter, although images were taken without filter. (2) MagErr is the only statistical error of the measurement. (3) The magnitudes are not corrected for the Galactic extinction.
GCN 21958 table
GRB_name GRB171001A
GCN_number 21958
Detection_method Swift-BAT Det
ra 22.0800°
decl -11.9280°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21958 SUBJECT: GRB 171001A: Swift-BAT refined analysis DATE: 17/10/02 14:11:12 GMT FROM: Amy Lien at GSFC M. Stamatikos (OSU), 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), T. Sakamoto (AGU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 171001A (trigger #775553) (Lien et al., GCN Circ. 21946). The BAT ground-calculated position is RA, Dec = 22.080, -11.928 deg which is RA(J2000) = 01h 28m 19.2s Dec(J2000) = -11d 55' 39.6" with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 72%. The mask-weighted light curve shows a multi-peaked structure that starts at ~T+11 s and ends at ~T+37 s. The major peaks occur at ~T+13 s, ~T+17 s, and ~T+32 s, respectively. T90 (15-350 keV) is 22.8 +- 2.0 sec (estimated error including systematics). The time-averaged spectrum from T+11.40 to T+37.02 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.48 +- 0.19. The fluence in the 15-150 keV band is 6.4 +- 0.8 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+31.42 sec in the 15-150 keV band is 0.9 +- 0.2 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/775553/BA/
GCN 21959 table
GRB_name GRB171001A
GCN_number 21959
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21959 SUBJECT: GRB 171001A: RATIR Optical and NIR Observations DATE: 17/10/02 15:46:07 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 171001A (Lien, et al., GCN 21946) 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 2017/10 2.17 to 2017/10 2.51 UTC (9.63 to 17.69 hours after the BAT trigger), obtaining a total of 5.31 hours exposure in the r and i bands and 2.24 hours exposure in the Z, Y, J, and H bands. We do not detect a source within the XRT error region (Evans, et al., GCN 21952) or at the position of the Nanshan optical transient (Tan, et al., GCN 21957). In comparison with the USNO-B1 and 2MASS catalogs, we obtain the following upper limits (3-sigma): r > 24.15 i > 23.98 Z > 22.96 Y > 22.77 J > 22.43 H > 22.03 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.