GRB 191001A
GCN Circular 25893
Subject
GRB 191001A: Fermi GBM Final Real-time Localization
Date
2019-10-01T06:50:20Z (6 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 06:41:50 UT on 1 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191001A (trigger 591604915.579128 / 191001279).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 308.9, Dec = 18.5 (J2000 degrees, equivalent to J2000 20h 35m, 18d 30'), with a statistical uncertainty of 3.3 degrees.
The angle from the Fermi LAT boresight is 102.0 degrees.
The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191001279/quicklook/glg_skymap_all_bn191001279.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191001279/quicklook/glg_healpix_all_bn191001279.fit
The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191001279/quicklook/glg_lc_medres34_bn191001279.gif
GCN Circular 25894
Subject
GRB 191001A: BALROG localization (Fermi Trigger 591604915 / GRB 191001279)
Date
2019-10-01T07:00:08Z (6 years ago)
From
Jochen Greiner at MPE,Garching <jcg@mpe.mpg.de>
J. Burgess , F. Kunzweiler, B. Biltzinger, F. Berlato, & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
591604915 at 06:41:50 on 01 Oct. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).
The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 313.4+/-6.0 deg
Decl.(2000.0) = 15.1+/-1.4 deg
We estimate an additional systematic error of 2 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191001279/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191001279/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191001279/json
GCN Circular 25911
Subject
GRB 191001A: DDOTI Optical Counterpart Candidate
Date
2019-10-01T22:28:50Z (6 years ago)
From
Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada <mpereyra@astro.unam.mx>
Margarita Pereyra (UNAM), Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L.
Becerra (UNAM), Diego Gonzalez (UNAM), Alexander Kutyrev (GSFC/UMD),
illiam H. Lee (UNAM), Eleonora Troja (GSFC/UMD), Gabriele Minervini
(INAF/IAPS-Rome) and Tanner Wolfram (ASU), Simone Dichiara (GSFC/UMD)
report:
We observed the field of GRB 191001A (trigger 591604915, Fermi GBM Team,
GCN Circ. 25893) from 2019 Oct 1 06:48:21 UTC (391 seconds after the
trigger) to 06:59:52 UTC with the DDOTI wide-field imager at the
Observatorio Astronomico Nacional on Sierra San Pedro Martir (
http://ddoti.astroscu.unam.mx/). We calibrated our images against the APASS
catalog and obtained a 10-sigma limiting magnitude of w = 18.6.
Comparing our 10-sigma detections against the USNO-B1 and Pan-STARRS DR1
catalogues, we detect an uncatalogued source at 20:20:47.65 +15:05:03.4
that fades at the 2.4 sigma level from w = 16.7 to 17.0. Specifically, it
fades as a power-law in time since trigger with an index of -0.53 +/- 0.23.
Independently and roughly simultaneously, the source was detected at a
similar magnitude by ATLAS as ATLAS19wxr and is cataloged in the Transient
Name Server as AT2019rog (TNS Astronomical Transient Report 48331). The
discovery report states that it was not detected on 2019 Sep 29.
No known minor planets, brighter than V = 24.0, were found in the 5 arcmin
region around the source position at the time our observations were
performed.
The source is about 1 sigma from the Fermi Final Real-Time Localization and
BALROG positions (Fermi GBM Team, GCN Circ. 25893; Burgess et al., GCN
Circ. 25894). We suggest that it might be the optical counterpart of the
GRB and encourage further observations.
We thank the staff of the Observatorio Astronomico Nacional in San Pedro
Martir.
--
GCN Circular 25918
Subject
GRB 191001A: RATIR Optical and NIR Observations
Date
2019-10-02T04:57:45Z (6 years ago)
From
Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada <mpereyra@astro.unam.mx>
Margarita Pereyra (UNAM), Alan M. Watson (UNAM), Eleonora Troja (GSFC), Nat
Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Diego
Gonzalez (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Owen
Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jes��s Gonz��lez (UNAM),
Carlos Rom��n-Z����iga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V.
Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report:
We observed the field of the candidate afterglow of GRB 191001A (trigger
591604915, Fermi GBM Team, GCN Circ. 25893, Pereyra et al. GCN Circ.
25911), centered at 20:20:47.65 +15:05:03.4, with the Reionization and
Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio Astron��mico Nacional on Sierra San
Pedro M��rtir from 2019/10 2.12 to 2019/10 2.17 UTC (20.08 to 21.45 hours
after the Fermi trigger), obtaining a total of 0.34 hours exposure in the g
and r bands, 0.67 hours exposure in the i band and 0.37 hours exposure in
the i, Z, Y, J, and H bands.
At the position of the transient source AT2019rog discovered independently
by ATLAS and DDOTI, in comparison with the USNO-B1, PS1 and 2MASS catalogs,
we obtain the following upper limits (3-sigma):
g > 23.20
r > 23.01
i > 23.26
Z > 21.40
Y > 21.49
J > 21.22
H > 20.92
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
The non-detection implies that the source has faded by about 6 magnitudes
in 20 hours. This is consistent with it being the afterglow of GRB 191001A.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 25919
Subject
GRB 191001A: KAIT Optical Upper Limit
Date
2019-10-02T05:54:41Z (6 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the GBM GRB 191001A (Fermi GBM team,
GCN 25893) starting at ~21.8 hours after the burst. We observed
the afterglow candidate AT2019rog, which was discovered independently
by ATLAS (Tonry et al., TNSTR 1954) and DDOTI (Pereyra et al., GCN 25911),
obtaining 17 x 60s images in the clear (roughly R) filters. We do not
detect the afterglow candidate in our co-add images with limiting mag
of ~21.5. Our non-detection result is consistent with observations from
RATIR (Pereyra et al., GCN 25918).
GCN Circular 25924
Subject
GRB 191001A: Swift ToO observations
Date
2019-10-02T14:08:17Z (6 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the Fermi/GBM GRB 191001A.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00020949
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Fermi/GBM event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a
GCN Circular after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
GCN Circular 25926
Subject
IPN triangulation of GRB 191001A
Date
2019-10-02T18:21:00Z (6 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,
K. Hurley, on behalf of the IPN, and
A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team, report:
The long duration GRB 191001A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 25893;
BALROG localization: Burgess et al., GCN Circ. 25894)
was detected by Fermi (GBM trigger 591604915), Konus-Wind,
and Swift (BAT) at about 24110 s UT (06:41:50).
The burst was outside the coded field of view of the BAT.
We have triangulated this GRB to a Konus-GBM annulus centered at
RA(2000)=346.113 deg (23h 04m 27s) Dec(2000)=-7.939 deg (-7d 56' 21"),
whose radius is 46.475 +/- 2.251 deg (3 sigma).
The distance between the optical transient ATLAS19wxr
(Smartt, et al., GCN Circ. 25922; Pereyra et al., GCN Circ. 25911)
and the annulus center line is 9.3 arcmin,
supporting the association of the transient and the GRB.
This annulus may be improved.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB191001_T24130/IPN
GCN Circular 25938
Subject
GRB 191001A: Fermi GBM observation
Date
2019-10-03T17:42:48Z (6 years ago)
From
Rachel Hamburg at UAH <rkh0007@uah.edu>
E. Bissaldi (Politecnico & INFN Bari), R. Hamburg (UAH)
and C. Meegan (UAH) report on behalf of the Fermi GBM Team:
"At 06:41:50.58 UT on 1 October 2019, the Fermi Gamma-Ray
Burst Monitor (GBM) triggered and located GRB 191001A
(trigger 591604915 / 191001279). The on-ground calculated
location has been reported in GCN #25893, and an IPN
annulus consistent with the GBM localization was reported
in GCN #25926. The ATLAS and DDOTI (GCN #25911) optical
counterpart position are consistent with the GBM localization.
The GBM light curve consists of several pulses
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0-4.99 s to T0+25.73 s
is best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.8 +/- 0.1
and the cutoff energy, parameterized as Epeak, is 114 +/- 9 keV.
The event fluence (10-1000 keV) in this time interval is
(4.7 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+15.7 s in the 10-1000 keV band
is 10.5 +/- 0.4 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 Circular 25942
Subject
GRB 191001A: Swift-XRT observations
Date
2019-10-03T20:26:43Z (6 years ago)
From
Antonino D'Ai at IASF-PA <antonino.dai@inaf.it>
D.N. Burrows (PSU), J. D. Gropp (PSU), A. Tohuvavohu (U. Toronto), K.L.
Page (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo
(INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the Fermi/GBM
detected burst GRB 191001A (GCN Circ. 25893, 25894), collecting 5.2 ks
of Photon Counting (PC) mode data between T0+114.2 ks and T0+161.3 ks.
No X-ray sources have been detected consistent with being within 2.0
arcsec of the likely associated optical transient AT2019rog (GCN Circ.
25911, 25918, 25919 and Tonry et al., TNSTR 1954). The 3-sigma upper
limit in the field ranges from ~0.002 to ~0.003 ct s^-1, corresponding
to a 0.3-10 keV observed flux of 8.6e-14 to 1.0e-13 erg cm^-2 s^-1
(assuming a typical GRB spectrum).
The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00020949.
This circular is an official product of the Swift-XRT team.