GRB 201017A
GCN Circular 28693
Subject
GRB 201017A iTelescope observation
Date
2020-10-19T23:35:52Z (5 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
K. Hasuda, M. Nakamura, T. Sakamoto (AGU)
We observed the field of GRB 201017A detected by Swift
(D'Ai et al., GCN Circ. 28666) with the iTelescope.Net
(http://www.itelescope.net) T5 (Takahashi Epsilon 250mm) telescope
located at the New Mexico Skies Observatory (NM, USA).
10 images of 60 sec exposures were taken in the Red filter
starting from October 17 on 10:06:37 (UT) about 20.1 min. after
the trigger and stopped on 10:20:44 (UT).
We do not detect the optical afterglow both in the individual
images and the stacked image at the XRT position
(Goad et al., GCN Circ. 28671). The estimated five sigma
upper limit of the combined image (total exposure of 600 sec)
is ~17.3 using the USNO-B1 catalog.
GCN Circular 28692
Subject
GRB 201017A: SAO RAS optical observations
Date
2020-10-19T17:43:25Z (5 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
A. S. Moskvitin, V. N. Aitov (SAO RAS)
on behalf of GRB follow-up team report.
We observed the field of GRB 201017A (Fermi GBM team, GCN #28665;
D'Ai et al., GCN #28666; Poolakkil et al., GCN #28675)
with the 1-m telescope of SAO RAS, Zeiss-1000 + Multi-Mode
Photometer-Polarimeter. We obtained 11 x 300 sec. images in Rc band
on October 17, 22:01:08--23:24:20 UT, t_mid - T0 = 0.5390 days.
We did not detect possible OT reported by Belkin et al. (GCN #28679)
or any sources within the XRT error circle (Goad et al., GCN #28671)
down to a limiting magnitude of 23.0.
GCN Circular 28691
Subject
GRB 201017A: GROWTH-India optical upper limit
Date
2020-10-19T15:40:46Z (5 years ago)
From
Harsh Kumar at Indian Inst of Tech,Bombay <harshkosli13@gmail.com>
H. Kumar (IITB), U. Stanzin(IAO), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA), report on behalf of the GROWTH-India collaboration:
We observed GRB 201017A reported by Fermi GBM Team (GCN #28665) and Swift-BAT
(A. D'Ai et al., GCN #28666; also see:- V. Lipunov et al., GCN #28667; M.R.
Goad et al., GCN #28671; L. P. Xin et al., GCN #28672; S. Poolakkil et al.,
GCN #28675; J.A. Kennea et al., GCN #28678; S. Belkin et al., GCN #28679) with
0.7m GROWTH-India telescope. The field was observed in the SDSS r��� filter
starting at 2020-10-17T12:54:58.41 UT i.e. ~3.13 hrs after the event
detection by Swift-BAT. We did not find any new source in the stacked image
of 10*300 sec exposure, within an uncertainty region of 2.6 arcsec around RA
(J2000): 02h 26m 28.82s, Dec (J2000): +66d 40' 43.6" (GCN 28671) up to r��� >
21.01 mag (5-sigma), calibrated against PanSTARRs PS1 data release,
(Flewelling et al., 2018). Assuming a typical power-law decay, this upper
limit is consistent with the r���=22.9 mag detection by Belkin et al (GCN #
28679).
The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).
GCN Circular 28684
Subject
GRB 201017A: MITSuME Akeno optical upper limits
Date
2020-10-19T14:13:28Z (5 years ago)
From
Ryohei Hosokawa at Tokyo Institute of Technology <hosokawa@hp.phys.titech.ac.jp>
R. Hosokawa, K. L. Murata, R. Adachi, M. Niwano, F. Ogawa, N.
Nakamura, N. Ito, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N.
Kawai (TokyoTech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 201017A (The Fermi GBM team, GCN #28665,
A. D'Ai et al., GCN #28666, V. Lipunov et al., GCN #28667, L. P. Xin
et al., GCN #28672, S. Belkin et al., GCN #28679) 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 at 2020-10-17 12:53:15 UT.(186 min after
trigger) Since some images were heavily affected by bad weather, we
stacked the images with good conditions. We did not find any new point
sources within the enhanced Swift/XRT circle (M. R. Goad et al., GCN
#28671) in all three bands.
We obtained the 5-sigma limits as follows
T0+[min] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
296 17:53:37 9480 g'>20.0,Rc>19.9,Ic>19.2
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used the PS1 catalog for flux calibration.
The magnitudes are expressed in the AB system.
The images were processed in real-time through the MITSuME GPU
reduction pipeline (Niwano et al., accepted for publication in PASJ,
https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire).
GCN Circular 28682
Subject
GRB 201017A: Swift-BAT refined analysis
Date
2020-10-18T22:26:32Z (5 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
D. M. Palmer (LANL), S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+823 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 201017A (trigger #1000613)
D'Ai, et al., GCN Circ. 28666). The BAT ground-calculated position is
RA, Dec = 36.587, 66.663 deg which is
RA(J2000) = 02h 26m 20.9s
Dec(J2000) = +66d 39' 45.7"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.
The mask-weighted light curve shows a single, symmetrical main peak from roughly
T-5 sec to T+5 sec, peaking at T+1 sec, followed by weaker emission out to T+20 sec.
T90 (15-350 keV) is 22.08 +- 6.25 sec (estimated error including systematics).
The time-averaged spectrum from T-2.77 to T+23.87 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.48 +- 0.25. The fluence in the 15-150 keV band is 9.0 +- 1.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+0.87 sec in the 15-150 keV band
is 1.8 +- 0.4 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/1000613/BA/
GCN Circular 28679
Subject
GRB 201017A: Assy and Mondy optical observations, possible afterglow detection
Date
2020-10-18T10:36:43Z (5 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), V. Kim (AFIF, Pulkovo Observatory), A. Pozanenko (IKI),
E. Klunko (ISTP), M. Krugov (AFIF), N. Pankov (HSE), A. Volnova (IKI)
report on behalf of IKI GRB FuN:
We observed the filed of GRB 201017A (Fermi GBM Team, GCN 28665; D'Ai
et al., GCN 28666; Poolakkil et al., GCN 28675) with AZT-33IK telescope
of Mondy observatory in R-filter starting on Oct. 17 (UT) 14:56:22 and
with AZT-20 telescope of Assy-Turgen observatory starting on Oct. 17
(UT) 14:15:45 in r' -filter. At the edge of enhanced Swift-XRT
position (Goad et al., GCN 28671) we marginally detected the object
which is absent in any Pan-STARRS images and PS1 catalog. Position of
the object is (J2000) 02:26:28.31 +66:40:44.74 with uncertainty of 0.5"
in each coordinate.
Preliminary photometry of the afterglow candidate is following
Date UT start t-T0 Filter Exp. OT Err. UL (3sigma)
(mid, days) (s)
2020-10-17 14:15:45 0.2043 r'(AB) 50*60 22.9 0.3 23.2 (AZT-20)
2020-10-17 14:56:22 0.2362 R 30*120 n/d n/d 21.8 (AZT-33IK)
The photometry is based on the nearby stars of PanSTARRS-PS1 catalog.
RA DEC r
02:26:33.94915 +66:39:38.3372 16.1111
02:26:39.68479 +66:38:36.3089 17.4493
GCN Circular 28678
Subject
GRB 201017A: Swift-XRT refined Analysis
Date
2020-10-18T10:03:03Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU),
A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne
(U. Leicester), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) and A.
D'Ai report on behalf of the Swift-XRT team:
We have analysed 3.5 ks of XRT data for GRB 201017A (D'Ai et al. GCN
Circ. 28666), from 112 s to 23.0 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 28671).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.97 (+0.10, -0.08).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.5, -0.4). The
best-fitting absorption column is 1.6 (+0.6, -0.5) x 10^22 cm^-2, in
excess of the Galactic value of 5.7 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.8 x 10^-11 (1.3 x 10^-10) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.6 (+0.6, -0.5) x 10^22 cm^-2
Galactic foreground: 5.7 x 10^21 cm^-2
Excess significance: 3.6 sigma
Photon index: 2.3 (+0.5, -0.4)
If the light curve continues to decay with a power-law decay index of
0.97, the count rate at T+24 hours will be 1.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.3 x
10^-14 (2.3 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/01000613.
This circular is an official product of the Swift-XRT team.
GCN Circular 28675
Subject
GRB 201017A: Fermi GBM detection
Date
2020-10-18T00:40:30Z (5 years ago)
From
Suraj Poolakkil at UAH <sp0076@uah.edu>
S. Poolakkil (UAH), C. Meegan (UAH) and A. von Kienlin (MPE)
report on behalf of the Fermi GBM Team:
"At 09:46:32.63 UT on 17 October 2020, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 201017A(trigger 624620797 / 201017407),
which was also detected by the Swift/BAT (A. D'Ai et al. 2020, GCN 28666).
The GBM on-ground location 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 consists of a single peak followed by some
extended emission with a duration (T90) of about 9 s (50-300 keV).
The time-averaged spectrum from T0-4.09 s to T0+5.12 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.20 +/- 0.17 and
the cutoff energy, parameterized as Epeak, is 144 +/- 35 keV.
The event fluence (10-1000 keV) in this time interval is
(1.402 +/- 0.166)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T0-0.89 s in the 10-1000 keV band
is 2.9 +/- 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 Circular 28672
Subject
GRB 201017A: Xinglong TNT upper limit
Date
2020-10-17T14:11:41Z (5 years ago)
From
Liping Xin at NAOC, SVOM <xlp@nao.cas.cn>
L. P. Xin (NAOC), X. F. Wang(THU), Y. L. Qiu(NAOC), J. Y. Wei(NAOC), J. Wang(GXU),
L. H. Li (NAOC), C. Wu(NAOC), E. W. Liang(GXU), X. H. Han (NAOC)and J. S. Deng(NAOC)report:
We began to observe GRB 201017A ( A. D'Ai et al., GCN 28666)
with Xinglong TNT telescope, China, at 11:10:24.8 (UT), 17th. Otc. 2020,
about 84 min after the burst,
10 x 300 sec R band images were obtained.
No any new source was detected in the XRT errorbox ( A. D'Ai et al., GCN 28666)
down to the limit magnitude of 19.5 mag in R band for any single image.
The brightness is calibrated to the USNO B1.0 R2 mag.
More analysis are still continuing.
We acknowledge the excellent support from Xinglong staff Sen Liu.
The message may be cited.
GCN Circular 28671
Subject
GRB 201017A: Enhanced Swift-XRT position
Date
2020-10-17T14:08:46Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1488 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 201017A, 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 = 36.62010, +66.67877 which is equivalent
to:
RA (J2000): 02h 26m 28.82s
Dec (J2000): +66d 40' 43.6"
with an uncertainty of 2.6 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 Circular 28667
Subject
Swift GRB 201017A: Global MASTER-Net observations report
Date
2020-10-17T11:58:14Z (5 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov, D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko
(Blagoveschensk Educational State University)
MASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB 201017A ( A. D'Ai et al., GCN 28666) errorbox 7302 sec after notice time and 7410 sec after trigger time at 2020-10-17 11:50:02 UT, with upper limit up to 19.1 mag. Observations started at twilight. The observations began at zenith distance = 44 deg. The sun altitude is -16.4 deg.
The galactic latitude b = 6 deg., longitude l = 132 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1463193
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
7501 | MASTER-Tunka | C | 180 | 19.1 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 28666
Subject
GRB 201017A: Swift detection of a burst
Date
2020-10-17T10:03:23Z (5 years ago)
From
Boris Sbarufatti at PSU <bxs60@psu.edu>
A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), T. Sakamoto (AGU) and B. Sbarufatti (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 09:46:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201017A (trigger=1000613). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 36.633, +66.673 which is
RA(J2000) = 02h 26m 32s
Dec(J2000) = +66d 40' 22"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of at least 10 sec. Data from ~T+10 s to
~T+100 s are currently unavailable. There might be additional
burst emission during this interval. The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 09:48:15.1 UT, 103.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 36.6186,
66.6787 which is equivalent to:
RA(J2000) = 02h 26m 28.45s
Dec(J2000) = +66d 40' 43.4"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 29 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.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.70
x 10^21 cm^-2 (Willingale et al. 2013).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 106 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
1.20.
Burst Advocate for this burst is A. D'Ai (antonino.dai AT 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/)
GCN Circular 28665
Subject
GRB 201017A: Fermi GBM Final Real-time Localization
Date
2020-10-17T09:56:54Z (5 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 09:46:32 UT on 17 Oct 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201017A (trigger 624620797.629664 / 201017407).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 21.7, Dec = 63.5 (J2000 degrees, equivalent to J2000 01h 26m, 63d 30'), with a statistical uncertainty of 7.3 degrees.
The angle from the Fermi LAT boresight is 100.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201017407/quicklook/glg_skymap_all_bn201017407.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201017407/quicklook/glg_healpix_all_bn201017407.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201017407/quicklook/glg_lc_medres34_bn201017407.gif