GRB 171210A

S. Matsukawa, A. Yoshida, T. Sakamoto, V. Pal'shin, Y. Kawakubo, M. Moriyama,
Y. Yamada, A. Tezuka (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
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), A. V. Penacchioni, P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 171210A (Bissaldi et al., GCN circ. 22228
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 ; Poolakkil et al.,
GCN circ. 22233
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 ; Kozlova et al., GCN circ. 22244
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 ) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 11:49:17.22 on 10 December 2017.  The burst signal was seen
by all the instruments.  Because of a problem in one of the ground alert processing
scripts, the GCN notice was not distributed automatically for this event.

The light curve of the SGM shows a single FRED-like pulse. The emission starts
at T-5 sec, peaks at T+5 sec and ends at T+50 sec.  The T90 duration measured
by the SGM data is 47.4 +- 2.5 sec (40-1000 keV).

The emission is seen up to ~T+180 s in the low energy ranges of the HXM data.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1196941607/

The CALET data used in this analysis are provided by the Waseda CALET Operation
Center located at the Waseda University.

P. D���Avanzo, A. Melandri (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the Swift team: 
Swift-XRT has performed a second epoch of observations of the Fermi/LAT-detected burst GRB 171210A (Bissaldi et al. GCN Circ. 22228
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 ), collecting 4.4 ks of Photon Counting (PC) mode data between T0+563.0 ks and T0+662.2 ks. None of the five XRT-detected sources reported in Burrows at al. (GCN Circ. 22235
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 ) show any sign of significant fading between the two epochs of observation. We conclude that we have not detected the GRB afterglow. 
This circular is an official product of the Swift-XRT team.

A.Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 171210A
(Fermi-LAT detection: Bissaldi et al., GCN 22228
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 ,
Fermi-GBM observation: Poolakkil et al., GCN 22233
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 )
triggered Konus-Wind at T0=42556.704 s UT (11:49:16.704).

The burst light curve shows a single pulse
started at ~T0-6.1 s with a total duration of ~186.6 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.15(-0.10,+0.11)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+2.816 s,
of 7.85(-1.73,+1.79)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+140.544 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.76(-0.13,+0.15),
the high energy photon index beta = -2.42(-0.21,+0.14),
the peak energy Ep = 158(-14,+16) keV
(chi2 = 99/88 dof)

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+5.376 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.64(-0.09,+0.11),
the high energy photon index beta = -2.83(-1.36,+0.40),
the peak energy Ep = 426(-46,+46) keV
(chi2 = 70/79 dof)

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB171210_T42556/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.

N.Tyurina, V. Lipunov, E. Gorbovskoy,V.Kornilov, D.Kuvshinov, 
A.V.Krylov,  I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko
Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU

R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA),
National University of San Juan, Argentina

H. Levato, C. Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

O.Gres, K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk,
Irkutsk State University

V.Yurkov, Yu.Sergienko
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory


MASTER-IAC robotic telescope (http://observ.pereplet.ru) started Fermi LAT 
GRB171210A  (Bissaldi et al. GCN 22228
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 , t_trigger=2017-12-10 
11:49:15.26UT, RA, Dec = 335.29, 24.44 (J2000), 0.15deg (90%) 
stat.err.rad.) inspection at
2017-12-10 19:08:16UT (07h19m00.7s after trigger time) just after sunset.

The unfiltered mlim on the single images is 20.4 (180s exposition), and on 
the sum is 21m.

MASTER auto-detection System (Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L)  didn't find optical counterpart.

http://observ.pereplet.ru/images/MASTERGRB171210AFermi.jpg


Observations were made on  zenit distance = 14 degrees, galaxy latitude b 
= -27 degree.

Dist. to Moon: 144.183815
Moon coord.: (176.084576 d, 5.105187 d
Lunar disk: 0.451595
Lunar phase: 95.555548
The sun  altitude  is -12.79


This message can be cited.

D.N. Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), A. Tohuvavohu (PSU), S. J.
LaPorte (PSU), P.A. Evans (U. Leicester), P. D'Avanzo (INAF-OAB) and 
N. P. M. Kuin (UCL-MSSL) report on behalf of the Swift team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 171210A (Bissaldi et al. GCN Circ. 22228
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 ),

collecting 5.0 ks of Photon Counting (PC) mode data between T0+34.7 ks
and T0+46.3 ks. 

Five uncatalogued X-ray sources have been detected, however none of
them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the

afterglow. Details of these sources are given below:

Source 1:
  RA (J2000.0):  335.26545  =  22:21:3.71
  Dec (J2000.0): +24.47028  =  +24:28:13.0
  Error: 2.9 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (7.5 [+1.5, -1.4])e-3 ct s^-1   
  Distance: 182 arcsec from Fermi/LAT position.
  Flux: (2.20 [+0.45, -0.41])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

This source lies 5.0" away from SDSS J222103.88+242817.4, which is
catalogued as a candidate quasar (Brescia et al., 2015, MNRAS, 450,
3893).

Source 2:
  RA (J2000.0):  335.2458  =  22:20:58.99
  Dec (J2000.0): +24.6016  =  +24:36:05.7
  Error: 5.7 arcsec (radius, 90% conf.)
  Count-rate: (2.23 [+0.98, -0.76])e-3 ct s^-1	 
  Distance: 618 arcsec from Fermi/LAT position.
  Flux: (2.44 [+1.07, -0.83])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

This source lies 6.4" away from SDSS J222058.65+243610.1, which is
catalogued as a candidate quasar (Brescia et al., 2015, MNRAS, 450,
3893).

Source 3:
  RA (J2000.0):  335.4135  =  22:21:39.23
  Dec (J2000.0): +24.5534  =  +24:33:12.4
  Error: 7.0 arcsec (radius, 90% conf.)
  Count-rate: (3.01 [+1.11, -0.90])e-3 ct s^-1	 
  Distance: 530 arcsec from Fermi/LAT position.
  Flux: (8.4 [+3.1, -2.5])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)
This source lies 2.6" away from SDSS J222139.19+243314.9, which is
catalogued as a candidate quasar (Brescia et al., 2015, MNRAS, 450,
3893).

Source 4:
  RA (J2000.0):  335.42877  =  22:21:42.90
  Dec (J2000.0): +24.30996  =  +24:18:35.9
  Error: 2.4 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0137 +/- 0.0022 ct s^-1   
  Distance: 608 arcsec from Fermi/LAT position.
  Flux: (4.08 [+0.66, -0.64])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

This source lies 1.3" away from SDSS J222142.87+241837.0, which is
catalogued as a candidate quasar (Brescia et al., 2015, MNRAS, 450,
3893).

Source 5:
  RA (J2000.0):  335.37378  =  22:21:29.71
  Dec (J2000.0): +24.49242  =  +24:29:32.7
  Error: 2.3 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (8.8 [+1.9, -1.8])e-3 ct s^-1   
  Distance: 281 arcsec from Fermi/LAT position.
  Flux: (3.00 [+0.65, -0.63])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

This source lies 1.7" away from SDSS J222129.58+242933.1, which is
catalogued as a candidate quasar (Brescia et al., 2015, MNRAS, 450,
3893).


The results of the XRT-team automatic analysis of the XRT observations,

including a position-specific upper limit calculator, are available at
http://www.swift.ac.uk/ToO_GRBs/00020785.


Simultaneous with the XRT, the UVOT observed the target region of GRB
171210A. Due to the smaller field of view, two of the candidate sources
(#2 and #4) are not on the UVOT image. The other candidate regions have
been examined but do not show any new sources. A further comparison of
the whole UVOT observation to the DSS survey shows no new sources. 

We acknowledge the use of the VizieR catalogue access tool, CDS,
Strasbourg, France.


This circular is an official product of the Swift team.

S. Poolakkil (UAH), C. Meegan (UAH) and A. von Kienlin (MPE) report on
behalf of the Fermi GBM Team:

"At 11:49:15.26 UT on 10 December 2017, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 171210A (trigger 534599360 / 171210493)
which was also detected by the Fermi LAT (E. Bissaldi et al. 2017, GCN
22228
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 ). The GBM on-ground
location is consistent with the LAT position.

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 best location is 51 degrees.

The GBM light curve consists of a single bright peak
with a duration (T90) of about 143 s (50-300 keV).
The time-averaged spectrum from T0-1.02 s to T0+103.42 s is
best fit by a Band function with Epeak= 145 +/- 3 keV, alpha = -0.65 +/-
0.02
and beta = -2.34 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(7.33 +/- 0.08)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.46 s in the 10-1000 keV band
is 16.7 +/- 0.36 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a ToO observation of the Fermi/LAT GRB 171210A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020785

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/LAT 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.

E. Bissaldi (Politecnico & INFN Bari), F. Longo (Univ & INFN Trieste) 
and D. Kocevski (MSFC) report��on behalf of the Fermi-LAT team:

"At 11:49:15.26 UT on December 10, 2017 Fermi-LAT detected high-energy emission from GRB 171210A,��which was also detected by Fermi-GBM (trigger 534599360 / 171210493).

The best LAT on-ground location is found to be

RA, Dec = 335.29, 24.44 (J2000)

with an error radius of 0.15 deg (90 % containment, statistical error only).��

This was 50 deg from the LAT boresight at the time of the trigger��and triggered an autonomous repoint of the spacecraft.

The data from the Fermi-LAT show a significant increase in the event rate that is spatially correlated with the trigger with high significance.��

The highest-energy photon is a 12��GeV��event which is observed��1400��seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is Elisabetta Bissaldi (Elisabetta.Bissaldi@ba.infn.it).

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."