GRB 160910A
GCN Circular 19966
Subject
Possible radio detection of GRB 160910A with the GMRT
Date
2016-09-29T08:34:23Z (10 years ago)
From
Nayana A J at NCRA-TIFR <nayan89deva@gmail.com>
A.J Nayana (NCRA-TIFR) and Poonam Chandra (NCRA-TIFR) report:
We carried out Giant Metrewave Radio Telescope (GMRT) observations of GRB 160910A
(Veres et al. 2016., GCN Circ. 19901. , Racusin et al. 2016., GCN Circ. 19902) at 1390
MHz band on 2016 Sep 27.21 UT. We detect a 4-sigma source within the XRT error circle
(D'Ai et al. 2016., GCN Circ. 19904) with a flux density of 185+/-69 uJy. This is likely
to be the radio afterglow of GRB 160910A. Map rms is 35 uJy.
We thank GMRT staff for making these observations possible.
GCN Circular 19949
Subject
GRB160910A: AstroSat CZTI detection
Date
2016-09-27T16:12:44Z (10 years ago)
From
Varun Bhalerao at IUCAA <varunb@iucaa.in>
V. Bhalerao (IUCAA), V. Kumar (IUCAA), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the Astrosat CZTI collaboration:
Analysis of Astrosat data showed the CZTI detection of a very bright GRB160910A (Fermi-GBM detection: P. Veres et al., GCN Circ. 19901).
The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak at 17:19:47.15 UT, 8 seconds after Fermi Trigger at 17:19:39.15 UT and a peak count rate of 1738 counts/sec above the background (four quadrants summed together), with a total of 7184 counts. The local mean background count rate was 343 counts/sec. Using cumulative rates, we measure a T90 of 9.44 secs.
CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb . CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN Circular 19937
Subject
GRB 160910A: 15 GHz detection from AMI
Date
2016-09-21T22:42:24Z (10 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson
(Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J.
Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K.
Grainge, A. Scaife (Manchester)
We observed the Fermi/LAT GRB 160910A (Racusin et al., GCN 19902) with
the AMI Large Array at 15 GHz on 2016 Sep 12.65, Sep 13.68, Sep 15.67,
and Sep 20.68 (UT) as part of the 4pisky program. We detect the radio
afterglow at the NOT location (Malesani et al., GCN 19908) at flux
densities of 791+/-55 uJy, 1151+/-82 uJy, 840+/-146 uJy, and 462+/-39
uJy respectively.
We thank the AMI staff for scheduling these observations. The AMI-GRB
database is a log of all GRB follow up observations with the AMI, and is
available at http://4pisky.org/ami-grb/.
GCN Circular 19935
Subject
GRB 160910A: TSHAO optical observations
Date
2016-09-18T20:03:32Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), I. Reva
(Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko (IKI)
report on behalf of larger GRB follow-up collaboration:
We observed the field of the GRB 160910A (Veres et al., GCN 19901;
Racusin et al., GCN 19902) with Zeiss-1000 (East) 1-m telescope of Tien
Shan Astronomical Observatory. We obtained several images in R filter
starting on Sep., 12 and Sep., 15. We clearly detected optical afterglow
(Ugarte Postigo et al., GCN 19907; Malesani et al., GCN 19908; Lipunov
et al., GCN 19914). Preliminary photometry of the afterglow is following
Date UT start t-T0 Filter Exp. OT UpLim (3 sigma)
(mid, days) (s)
2016-09-12 14:43:02 1.92176 R 27*120 19.96 +/- 0.08 21.7
2016-09-15 14:31:13 4.91356 R 27*120 21.70 +/- 0.30 21.7
Photometry is based on nearby SDSS-DR9 stars used in GCN 19919 (Mazaeva
et al.).
GCN Circular 19925
Subject
GRB 160910A: Maidanak optical observations
Date
2016-09-16T12:20:32Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), B. Hafizov (UBAI). A. Volnova
(IKI), O. Burhonov (UBAI) report on behalf of larger GRB follow-up
collaboration:
We observed the GRB 160910A (Veres et al., GCN 19901; Racusin et al.,
GCN 19902) with AZT-22 telescope of Maidanak observatory equipped with
SNUCAM in R filter. We clearly detected optical afterglow (de Ugarte
Postigo et al., GCN 19907; Malesani et al., GCN 19908; Lipunov et al.,
GCN 19914; Mazaeva et al., GCN 19919; Hagen et al., GCN 19923).
Preliminary photometry of the afterglow is following
Preliminary photometry of the afterglow is following
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
2016-09-14 14:40:40 3.89933 R 15*120 21.40 0.14 22.2
Photometry is based on nearby SDSS-DR9 stars
SDSS-DR9_id R(Lupton transformation)
J144549.10+390403.4 16.86
J144552.78+390234.9 17.32
J144538.58+390535.0 18.34
J144541.35+390128.0 17.15
GCN Circular 19923
Subject
GRB 160910A: Swift/UVOT Detection
Date
2016-09-14T17:12:41Z (10 years ago)
From
Lea Hagen at PSU <lea.zernow.hagen@gmail.com>
L. M. Z. Hagen (PSU) and J. R. Cummings (GSFC/UMBC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 160910A
196954 s after the Fermi/GBM (Veres et al., GCN Circ. 19901) and
Fermi/LAT (Racusin et al., GCN Circ. 19902) triggers. We detect a
fading source consistent with the XRT position (D'Ai et al., GCN Circ.
19904) and optical detections (de Ugarte Postigo et al., GCN Circ.
19907; Malesani et al., GCN Circ. 19908; Lipunov et al., GCN Circ.
19914; Mazaeva et al., GCN Circ. 19919).
Preliminary detections 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 196954 267060 1620 20.61+-0.14
white 267064 318724 2326 20.95+-0.14
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 19919
Subject
GRB 160910A: Mondy optical observations
Date
2016-09-13T10:30:41Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), A. Volnova (IKI),
I. Korobtsev (ISTP) report on behalf of larger GRB follow-up collaboration:
We observed the field of the GRB 160910A (Veres et al., GCN 19901; Racusin
et al., GCN 19902) with AZT-33IK telescope of Sayan observatory (Mondy)
starting on Sep., 12 (UT) 14:02:46. We obtained several images in R-filter.
We clearly detected optical afterglow (Ugarte Postigo et al., GCN 19907;
Malesani et al., GCN 19908; Lipunov et al., GCN 19914). Preliminary
photometry of the afterglow is following
Date UT start t-T0 Filter Exp. OT UpLim (3 sigma)
(mid, days) (s)
2016-09-12 14:02:46 1.87506 R 32*60 19.92+/-0.05 22.2
Photometry is based on nearby SDSS-DR9 stars
SDSS-DR9_id R(Lupton transformation)
J144549.10+390403.4 16.86
J144552.78+390234.9 17.32
J144538.58+390535.0 18.34
J144541.35+390128.0 17.15
GCN Circular 19914
Subject
GRB 160910A: Global MASTER Net OT detection before LAT alert
Date
2016-09-12T19:16:03Z (10 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov,
P.Balanutsa, A.Kuznetsov, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute
D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory
R. Rebolo, M. Serra Ricart, N. Lodieu, G. Israelian
The Instituto de Astrofisica de Canarias
K.Ivanov, O.Gres, N.M.Budnev, S.Yazev,
Irkutsk State University
A. Tlatov, V.Senik, D. Dormidontov, A.Parkhomenko
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk
Hugo Levato, Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
R.Podesta, C.Lopez, F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)
MASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in SAAO was pointed to the FERMI GBM GRB160910.72 15 sec after
notice time and 65 sec after trigger time at 2016-09-10 17:20:45 UT.
On our first (20s exposure started 75 sec after GBM trigger) set we do
not found optical transient within FERMI error-box (ra=14 54 00
dec=+39 23 00 r=3.41, trigger 495220783 / 160910722
(Veres and C.Meegan, GCN 19901)) because very low
altitude on horizont ~3 degrees (one tube was under the roof).
Fortunatelly, we saw OT by one of two MASTER Very Wide Field Cameras (5
sec expositon, 0.25 sec readout) .
On MASTER-SAAO VWF Camera we see OT at 3 sigma confidence level with
magnitude 11.6 +- 0.5 mag on a co-added images with total exposure 95
seconds (19 x 5 sec) starting at 17:20:45 i.e. 65 sec after trigger time. Mean
time is 113 sec after trigger.
On our second MASTER-SAAO (30s
exposure) set started at 2016-09-10 17:22:26 (167 sec after trigger time)
we found OT within FERMI error-box with unfileterd
magnitide m = 11.6+-0.1 . The second exposition was making after receiving
new Fermi GBM coordinates.
Ra, Dec = 14h 45m 46.03s +39d 04m 00.52s
err = +-0.5 arcsec
(cf. A. D'A. et al., GCN 19904; A. de Ugarte Postigo et al., 19907;
Malesani et al., GCN 19908 )
MASTER-IAC robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in IAC was starting survey on the FERMI GBM GRB160910.72
error-box (ra=14 46 14 dec=+39 25 10 r=1.0) 11142 sec after notice time
and 11239 sec after trigger time at 2016-09-10 20:26:58 UT. The 5-sigma upper
limit on our first (60s exposure) set is about 18.3 mag . The OT
unfiltered magnitude is 17.4+-0.4 .
The light curve is available at
http://master.sai.msu.ru/static/GRB160910A.png
The MASTER-SAAO power law index alpha = 1.30+-0.07 ( I ~ t^-alpha) in
agreement with MASTER-IAC and some
contradiction with late point (Malesani et al., GCN 19908 )
The MASTER-SAAO and NOT combined power law index alpha =
1.17+-0.02 .
All MASTER observations was done before LAT alert.
The message may be cited.
GCN Circular 19913
Subject
Konus-Wind observation of GRB 160910A
Date
2016-09-12T17:19:40Z (10 years ago)
From
Anastasia Tsvetkova at Ioffe Institute <tsvetkova@mail.ioffe.ru>
A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration, very intense GRB 160910A
(Fermi GBM observation: Veres & Meegan, GCN 19901;
Fermi-LAT detection: Racusin & Kocevski, GCN 19902;
CALET Gamma-Ray Burst Monitor detection: Kawakubo et al., GCN 19909)
triggered Konus-Wind at T0=62379.089 s UT (17:19:39.089).
The burst light curve starts with an initial weaker emission followed by
a main bright peak with a duration of ~50 s.
The main pulse is followed by a long weak tail seen up to ~T0+150 s.
The emission is seen up to ~10 MeV.
As observed by Konus-Wind, the burst
had a fluence of 1.36(-0.09,+0.10)x10^-4 erg/cm2,
and a 64-ms peak energy flux, measured from T0+5.120 s,
of 3.51(-0.32,+0.32)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum of the burst
(measured from T0 to T0+47.872 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.81(-0.06,+0.07),
the high energy photon index beta = -2.16(-0.12,+0.09),
the peak energy Ep = 315(-29,+31) keV,
chi2 = 97/98 dof.
The spectrum near the peak count rate
(measured from T0+4.864 to T0+6.400 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.15(-0.10,+0.10),
the high energy photon index beta = -2.27(-0.09,+0.07),
the peak energy Ep = 266(-19,+21) keV,
chi2 = 100/69 dof.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160910_T62379/
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 19911
Subject
GRB 160910A: Correction to GCN 19904
Date
2016-09-12T09:03:37Z (10 years ago)
From
Antonino D'Ai at IASF-PA <antonino.dai@ifc.inaf.it>
A. D'A� reports on behalf of the Swift/XRT team: the reported
absorbed/unabsorbed fluxes in GCN 19904 have been incorrectly reported.
The correct information is:
"The [absorbed] unabsorbed 0.3-10 keV flux is 5.6 (+1.4, -1.2) x 10^-12
erg cm^-2 s^-1 [4.9 (+1.9, -1.4) x 10^-12 erg cm^-2 s^-1]."
We thank M. De Pasquale for spotting the mistake.
We apologize for any confusion.
GCN Circular 19910
Subject
GRB 160910A: XRT results and corrections to GCN 19905 & 19906
Date
2016-09-12T07:29:43Z (10 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Due to technical issues, GCN 19905 was issues with an incorrect encoding
and GCN 19906 was contained the wrong name and URL.
Swift-XRT observed the field of GRB 160910A and discovered an afterglow
as reported by D'Ai et al (GCN Circ. 19904). As the afterglow has been
detected, the full XRT results for the GRB are available at
http://www.swift.ac.uk/xrt_products/00020695
Analysis of the entire tiled campaign is at
http://www.swift.ac.uk/xrt_products/TILED_GRB00058/
GCN Circular 19909
Subject
GRB 160910A: CALET Gamma-Ray Burst Monitor detection
Date
2016-09-12T03:42:09Z (10 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
Y. Kawakubo, A. Yoshida, T. Sakamoto, M. Moriyama, Y. Yamada (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu,
T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:
The long-duration GRB 160910A (Veres et al., GCN Circ. 19901; Racusin et al.,
GCN Circ. 19902; INTEGRAL-SPI/ACS trigger #7560) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 17:19:41.25 on 10 September 2016.
The burst signal was seen by all CGBM instruments.
The light curve of the SGM shows an initial weak peak followed by a main
bright peak. The weak initial peak starts at T0, peaks at T+3 sec and ends
at T+4 sec. The main bright peak starts at T+4 sec, peaks at T+6 sec and
ends at T+20 sec. Several overlapping pulses are evident in the main peak.
The T90 duration measured by the SGM data is 20.7 +- 1.5 sec (40-1000 keV).
The light curve is available at
http://cgbm.calet.jp/cgbm_trigger/flight/1157563166/
The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.
GCN Circular 19908
Subject
GRB 160910A: NOT afterglow confirmation
Date
2016-09-11T21:03:05Z (10 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI and DTU Space), D. Xu (NAOC/CAS), A. de Ugarte
Postigo (IAA-CSIC and DARK/NBI), R. Tronsgaard Rasmussen (NOT), P. Blay
(NOT/IAC), report on behalf of a larger collaboration.
We observed the field of the Fermi GRB 160910A (Veres & Meegan, GCN
19901; Racusin & Kocevski, GCN 19902) with the Nordic Optical Telescope
(NOT) equipped with the AlFOSC imaging camera.
Observations started on 2016 Sep 11.847 UT, and consisted of 3x300 s in
the SDSS r filter. We detect the afterglow reported by de Ugarte Postigo
et al. (GCN 19907), and we provide coordinates (J2000):
RA = 14:45:46.04
Dec = +39:04:00.2
The expected uncertainty is <0.5". Comparing with nearby SDSS stars, we
measure for the afterglow a magnitude r = 19.65 +- 0.01 (AB) at a mean
time of Sep 11.8487 UT (27.04 hr after the GRB trigger).
GCN Circular 19907
Subject
GRB 160910A: Afterglow detection from OSN
Date
2016-09-11T20:56:28Z (10 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), L. Izzo (IAA-CSIC),
D.A. Kann (TLS Tautenburg), V. Casanova (IAA-CSIC) report on
behalf of a larger collaboration:
We have observed the field of GRB 160910A (Veres et al. GCN 19901,
Racusin et al. GCN 19902, D���A�� et al. GCN 19904) with the 1.5m
OSN telescope in Granada (Spain). The observation consisted of I-band
imaging and started at 20:15:07 (26.92 hr after the burst). On the first 300 s
image we detect an object within the XRT error box at I(AB) ~ 19.3 mag,
not present in the SDSS images, which we identify as the counterpart of
GRB 160910A
We encourage further follow-up and spectroscopy of this bright afterglow.
GCN Circular 19906
Subject
GRB 160910A: Tiled Swift observations
Date
2016-09-11T17:19:16Z (10 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 series of observations, tiled on the sky, of the
Fermi/LAT GRB 160910A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00059
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: 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 OPS NOTE(12sep16): Per author's request, the "B" in the GRB name
was changed to an "A"; Subject-line and in the first paragraph.]
GCN Circular 19904
Subject
GRB 160910A: Swift-XRT afterglow detection
Date
2016-09-11T15:04:50Z (10 years ago)
From
Antonino D'Ai at IASF-PA <antonino.dai@ifc.inaf.it>
A. D'A� (INAF-IASFPA), V. D'Elia (ISDC), J. Cummings (GSFC/UMBC),
B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R. Roegiers (PSU),
S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester) 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 (Veres
et al., GCN Circ. 19901)
and Fermi/LAT (Racusin et al., GCN Circ. 19902) detected burst GRB
160910A in a series of 4 observations
tiled on the sky. The total exposure time is 5 ks, distributed over 4
tiles.
The data were collected between T0+35 ks and T0+47 ks, and are entirely
in Photon Counting (PC) mode.
An uncatalogued X-ray source is detected and is above the RASS limit,
and is therefore likely the GRB afterglow.
The position of this source is RA, Dec.=221.4423, 39.0668 which is
equivalent to:
RA (J2000) = 14h45m46.16s
Dec (J2000) = +39:04:00.64
with an uncertainty of 4.3 arcsec (radius, 90% confidence).
This position is 0.34 deg from the Fermi/LAT position and 0.6 deg from
the GBM position.
The light curve built with the data collected so far is consistent with
a constant source of mean
count rate (1.0 +/- 0.1)e-01 ct/sec. More data are required to search
for a fading behaviour.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.7 (+0.6, -0.6).
The best-fitting absorption column is 1.3 (+1.7, -1.3) x 10^21 cm^-2,
consistent with the Galactic value of 1.0 x 10^20 cm^-2 (Willingale et
al. 2013).
The [absorbed] unabsorbed 0.3-10 keV flux is 5.1 (+1.6, -1.0)e^-10 erg
cm^-2 s^-1 [4.7 (+2.1, -1.3) e-10 erg cm^-2 s^-1].
This circular is an official product of the Swift-XRT team.
GCN Circular 19902
Subject
GRB 160910A: Fermi-LAT detection
Date
2016-09-11T02:07:29Z (10 years ago)
From
Judith Racusin at GSFC <judith.racusin@nasa.gov>
J. L. Racusin (NASA/GSFC) and D. Kocevski (NASA/GSFC) report on behalf of the Fermi-LAT team:
At 17:19:39 on September 10, 2016 Fermi-LAT detected high-energy emission from GRB 160910A, which was also detected by Fermi-GBM (trigger 495220782/160910722; Veres et al. GCN #19901).
The best LAT on-ground location is found to be
RA, Dec = 221.26, 38.76 (J2000)
with an error radius of 0.35 deg (90 % containment, statistical error only).
The GBM location was initially at the edge of the LAT field of view at an angle of 71 degrees to the LAT boresight and triggered an autonomous repoint of the spacecraft. The highest-energy photon is a 500 MeV event which is observed 9 ks after the GBM trigger.
A Swift ToO has been requested for this burst.
The Fermi-LAT point of contact for this burst is Dan Kocevski (daniel.kocevski@nasa.gov).
The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN Circular 19901
Subject
GRB 160910A: Fermi GBM observation
Date
2016-09-11T01:49:14Z (10 years ago)
From
Peter Veres at UAH <veresp@gmail.com>
P Veres (UAH) and C Meegan (UAH) report on behalf of the Fermi GBM Team:
"At 17:19:39.15 UT on 10 September 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160910A (trigger 495220783 / 160910722).
The on-ground calculated location, using the GBM trigger data, is RA =
221.8, DEC = 39.6 (J2000 degrees, equivalent to 14 h 47 m, 39 d 38 '), with
an uncertainty of 1 degrees (radius, 1-sigma containment, statistical only;
there is additionally a systematic error which we have characterized as a
core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small
tail suffering a larger than 10 deg systematic error. [Connaughton et al.
2015, ApJS, 216, 32] ).
The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM
Flight Software owing to the high peak flux of the GRB. This ARR was
accepted and the spacecraft slewed to the GBM in-flight location. The
initial angle from the Fermi LAT boresight to the GBM ground location is 71
degrees.
The GBM light curve shows a single pulse with a duration (T90) of about
24.3 s (50-300 keV). The time-averaged spectrum from T0 to T0+32.3 s is
best fit by a Band function with Epeak = 347 +/- 9 keV, alpha = -0.78 +/-
0.01, and beta = -2.23 +/- 0.04.
The event fluence (10-1000 keV) in this time interval is (8.41 +/- 0.06)E-5
erg/cm^2. The 1-sec peak photon flux measured starting from T0+8.2 s in the
10-1000 keV band is 76.5 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary; final
results will be published in the GBM GRB Catalog."