GRB221016A

This page lists all entries on GRB221016A in GRBweb

Summary Fermi GBM IPN Swift GCN 32773 GCN 32774 GCN 32775 GCN 32776 GCN 32778 GCN 32782 GCN 32783 GCN 32784 GCN 32785 GCN 32786

Summary table
Variable Value Source
GRB_name_Fermi GRB221016986
T0 23:39:22 UTC GCN_circulars,Fermi GBM final loc
ra 38.9446° Swift
decl -34.6104° Swift
pos_error 2.59e-04° Swift
T90 12.736 s Fermi_GBM
T90_error 1.145 s Fermi_GBM
T90_start 23:39:22.325 UTC Fermi_GBM
fluence 5.11e-06 erg/cm² Fermi_GBM
fluence_error 3.50e-08 erg/cm² Fermi_GBM
T100 23.86 s
GBM_located False
mjd 59868.985671296294 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB221016986
trigger_name bn221016986
ra 38.9492°
decl -34.6239°
pos_error 3.08e+00°
datum 2022-10-16
t_trigger 23:39:22.709 UTC
T90 12.736 s
T90_error 1.145 s
T90_start 23:39:22.325 UTC
fluence 5.11e-06 erg/cm²
fluence_error 3.50e-08 erg/cm²
flux_1024 7.41e+00 erg/cm²/s
flux_1024_error 3.45e-01 erg/cm²/s
flux_1024_time 1.79e+00 erg/cm²/s
flux_64 9.45e+00 erg/cm²/s
flux_64_error 1.48e+00 erg/cm²/s
IPN table
GRB_name GRB221016A
ra 38.9500°
decl -34.6167°
pos_error 5.00e-02°
Swift table
GRB_name GRB221016A
t_trigger 23:39:24 UTC
ra 38.9446°
decl -34.6104°
pos_error 2.59e-04°
T90 21.86 s
fluence 2.30e-06 erg/cm²
GCN 32773 table
GRB_name GRB221016A
GCN_number 32773
Detection_method Fermi GBM final loc
t_trigger 23:39:22 UTC
ra 37.6000°
decl -32.1000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32773 SUBJECT: GRB 221016A: Fermi GBM Final Real-time Localization DATE: 22/10/16 23:50:37 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 23:39:22 UT on 16 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221016A (trigger 687656367.709164 / 221016986). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 37.6, Dec = -32.1 (J2000 degrees, equivalent to J2000 02h 30m, -32d 06'), with a statistical uncertainty of 2.2 degrees. The angle from the Fermi LAT boresight is 98.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221016986/quicklook/glg_skymap_all_bn221016986.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221016986/quicklook/glg_healpix_all_bn221016986.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221016986/quicklook/glg_lc_medres34_bn221016986.gif
GCN 32774 table
GRB_name GRB221016A
GCN_number 32774
Detection_method Swift Det
t_trigger 23:39:24 UTC
ra 38.9490°
decl -34.6240°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32774 SUBJECT: GRB 221016A: Swift detection of a burst DATE: 22/10/16 23:53:22 GMT FROM: David Palmer at LANL K. L. Page (U Leicester), J. A. Kennea (PSU), N. J. Klingler (GSFC/UMBC/CRESSTII), A. Y. Lien (U Tampa), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), A. Tohuvavohu (U Toronto) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 23:39:24 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 221016A (trigger=1129775). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 38.949, -34.624 which is RA(J2000) = 02h 35m 48s Dec(J2000) = -34d 37' 26" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak with tail structure with a duration of about 30 sec. The peak count rate was ~3500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 23:42:24.0 UT, 179.8 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 38.94479, -34.61039 which is equivalent to: RA(J2000) = 02h 35m 46.75s Dec(J2000) = -34d 36' 37.4" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 50 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 https://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 (3.53 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.8 (+3.14/-2.70) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 97 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 none of the XRT error circle. 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 0.026. Burst Advocate for this burst is K. L. Page (kimlpage1978 AT gmail.com). 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/)
GCN 32775 table
GRB_name GRB221016A
GCN_number 32775
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 32775 SUBJECT: GRB 221016A: LCOGT Optical Afterglow Detection DATE: 22/10/17 03:23:46 GMT FROM: Robert Strausbaugh at University of Minnesota R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on behalf of a larger collaboration: We observed the GRB 221016A (Page et al., GCN 32774) field with the LCOGT 1-meter Sinistro instrument at the Cerro Tololo Interamerican Observatory, Chile site, on October 17, from 01:39 to 02:06 (corresponding to 2.00 to 2.55 hours from the GRB trigger time) with the Bessel I and R filters. We performed a series of 3x300s exposures in each band. We detect an uncataloged optical source within the XRT error region (Page et al., GCN 32774), in R band, and marginally in I-band (2-sigma detection). The following magnitudes are calculated using the USNO-B1.0 catalog as reference: R = 21.22 +/- 0.18 I = 20.03 +/- 0.17 These magnitudes are not corrected for galactic extinction. Gemini imaging+spectroscopic follow up is ongoing.
GCN 32776 table
GRB_name GRB221016A
GCN_number 32776
Detection_method Swift-XRT Det
ra 38.9446°
decl -34.6107°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32776 SUBJECT: GRB 221016A: Enhanced Swift-XRT position DATE: 22/10/17 04:07:07 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 165 s of XRT Photon Counting mode data and 1 UVOT images for GRB 221016A, 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 = 38.94459, -34.61073 which is equivalent to: RA (J2000): 02h 35m 46.70s Dec (J2000): -34d 36' 38.6" with an uncertainty of 2.4 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 32778 table
GRB_name GRB221016A
GCN_number 32778
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 32778 SUBJECT: GRB 221016A: z-band upper limit, possible afterglow brightening DATE: 22/10/17 08:56:18 GMT FROM: Daniele B Malesani at Radboud U D. B. Malesani (Radboud Univ. and DAWN/NBI), D. A. Kann (Goethe Univ.), L. Izzo (DARK/NBI), S. Covino, P. D'Avanzo (INAF/OAB), N. R. Tanvir (Univ. Leicester), report on behalf of the Stargate consortium: We observed the field of GRB 221016A (Page et al., GCN 32774) with the ESO VLT UT3 (Melipal), using the acquisition camera of the X-shooter spectrograph. A single 30 s image is available to us, taken on 2022 Oct 17.034 UT (1.17 hr after the trigger). The image seeing was rather poor, about 2.2". No source is detected at the position of the optical counterpart discovered by Strausbaugh & Cucchiara (GCN 32775), down to a 3-sigma limit z > 20.8 (AB; calibrated against one nearby SkyMapper star). Comparison between our limit and the magnitudes reported by Strausbaugh & Cucchiara (GCN 32775) seems to indicate a brightening of the afterglow between ~1 and ~2 hr after the trigger. We acknowledge the ESO staff for a quick reaction to our request, in particular Matias Jones and Felipe Gaete.
GCN 32782 table
GRB_name GRB221016A
GCN_number 32782
Detection_method Fermi GBM Det
t_trigger 23:39:22.710 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 32782 SUBJECT: GRB 221016A: Fermi GBM observation DATE: 22/10/17 13:58:45 GMT FROM: Elisabetta Bissaldi at INFN,Bari E. Bissaldi (Politecnico and INFN Bari), P. Veres (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 23:39:22.71 UT on 16 October 2022, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 221016A (trigger 687656367/221016986), which was also detected by the Swift/BAT (Page et al. GCN 32774). The Fermi GBM Final Real-time Localization (GCN 32773) is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 98 degrees. The GBM light curve shows a single emission episode with a duration (T90) of about 13 s (50-300 keV). The time-averaged spectrum from T0-1.2 s to T0+11 s is best fit by a Band function with Epeak = 119 +/- 12 keV, alpha = -0.51 +/- 0.12, and beta = -2.11 +/- 0.11. The event fluence (10-1000 keV) in this time interval is (6.3 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+1.8 s in the 10-1000 keV band is 7.4 +/- 0.3 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 32783 table
GRB_name GRB221016A
GCN_number 32783
Detection_method Konus-Wind Det
t_trigger 23:39:26.713 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 32783 SUBJECT: Konus-Wind detection of GRB 221016A DATE: 22/10/17 14:06:18 GMT FROM: Anna Ridnaia at Ioffe Institute A.Ridnaia, D. Frederiks, A.Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration GRB 221016A (Fermi-GBM detection: Fermi GBM team, GCN#32773, Bissaldi et al., GCN#32782; Swift-BAT detection: Page et al., GCN#32774) triggered Konus-Wind at T0=85166.713 s UT (23:39:26.713). The burst light curve shows a single emission pulse which starts at ~T0-1.7 s and has a total duration of ~12.5 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB221016_T85166/ As observed by Konus-Wind, the burst had a fluence of 5.46(-0.74,+1.07)x10^-6 erg/cm2, and a 64-ms peak flux, measured from T0+0.800 s, of 1.87(-0.73,+0.74)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 - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.02(-0.33,+0.40) and Ep = 207(-46,+98) keV (chi2 = 60/99 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.0 (chi2 = 60/98 dof). The spectrum near the maximum count rate (measured from T0+0.256 to T0+8.448 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model with alpha = -0.89(-0.30,+0.35) and Ep = 166(-26,+39) keV (chi2 = 81/96 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.4 (chi2 = 81/95 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 32784 table
GRB_name GRB221016A
GCN_number 32784
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 32784 SUBJECT: GRB 221016A: Swift-XRT refined Analysis DATE: 22/10/17 15:15:27 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , D.N. Burrows (PSU), J. D. Gropp (PSU), S. Dichiara (PSU) and K.L. Page report on behalf of the Swift-XRT team: We have analysed 8.2 ks of XRT data for GRB 221016A (Page et al. GCN Circ. 32774), from 76 s to 44.8 ks after the BAT trigger. The data comprise 83 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 32776). The light curve can be modelled with an initial power-law decay with an index of alpha=2.20 (+0.22, -0.18), followed by a break at T+254 s to an alpha of 0.78 (+0.04, -0.05). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.49 (+0.23, -0.21). The best-fitting absorption column is 7.9 (+4.2, -3.7) x 10^20 cm^-2, in excess of the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.04 (+0.20, -0.19) and a best-fitting absorption column of 1.5 (+0.6, -0.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.3 x 10^-11 (4.4 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.5 (+0.6, -0.5) x 10^21 cm^-2 Galactic foreground: 3.5 x 10^20 cm^-2 Excess significance: 3.5 sigma Photon index: 2.04 (+0.20, -0.19) If the light curve continues to decay with a power-law decay index of 0.78, the count rate at T+24 hours will be 0.019 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.1 x 10^-13 (8.1 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/01129775. This circular is an official product of the Swift-XRT team.
GCN 32785 table
GRB_name GRB221016A
GCN_number 32785
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 32785 SUBJECT: GRB 221016A: Swift/UVOT Detection DATE: 22/10/17 20:13:01 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and K. L. Page (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 221016A 97 s after the BAT trigger (Page et al., GCN Circ. 32774). A source consistent with the enhanced XRT position (Goad et al. GCN Circ. 32776) is detected 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 97 247 147 20.20 +/- 0.23 b 3736 3861 123 >19.8 u 309 349 39 >18.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.026 in the direction of the burst (Schlegel et al. 1998).
GCN 32786 table
GRB_name GRB221016A
GCN_number 32786
Detection_method Swift-BAT Det
ra 38.9380°
decl -34.6150°
Circular_text TITLE: GCN CIRCULAR NUMBER: 32786 SUBJECT: GRB 221016A: Swift-BAT refined analysis DATE: 22/10/17 20:42:14 GMT FROM: Tyler Parsotan at UMBC/GSFC/CRESST II S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+200 sec from the recent telemetry downlink, we report further analysis of BAT GRB 221016A (trigger #1129775) (Page, et al., GCN Circ. 32774). The BAT ground-calculated position is RA, Dec = 38.938, -34.615 deg which is RA(J2000) = 02h 35m 45.2s Dec(J2000) = -34d 36' 54.2" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 53%. The light curve shows a single peaked pulse. T90 (15-350 keV) is 21.86 +- 5.70 sec (estimated error including systematics). The time-averaged spectrum from T-3.18 to T+29.18 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.28 +- 0.08. The fluence in the 15-150 keV band is 2.3 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+0.03 sec in the 15-150 keV band is 3.4 +- 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/1129775/BA/