//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22228 SUBJECT: GRB 171210A: Fermi-LAT detection DATE: 17/12/10 17:48:25 GMT FROM: Elisabetta Bissaldi at U.Innsbruk/IAPP 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." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22232 SUBJECT: GRB 171210A: Swift ToO observations DATE: 17/12/10 20:59:17 GMT FROM: Phil Evans at U of Leicester 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22233 SUBJECT: GRB 171210A: Fermi GBM detection DATE: 17/12/11 04:12:12 GMT FROM: Suraj Poolakkil at UAH 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). 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." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22235 SUBJECT: GRB 171210A: Swift-XRT and UVOT observations DATE: 17/12/11 13:22:48 GMT FROM: Paolo D'Avanzo at INAF-OAB 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), 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22238 SUBJECT: GRB 171210A: MASTER-Net optical observations DATE: 17/12/11 14:56:17 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs 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, 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22244 SUBJECT: Konus-Wind observation of GRB 171210A DATE: 17/12/12 12:58:30 GMT FROM: Anna Kozlova at Ioffe Institute 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, Fermi-GBM observation: Poolakkil et al., GCN 22233) 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22261 SUBJECT: GRB 171210A: Further Swift-XRT observations DATE: 17/12/18 23:58:25 GMT FROM: Paolo D'Avanzo at INAF-OAB 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), 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) 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22267 SUBJECT: GRB 171210A CALET Gamma-Ray Burst Monitor detection DATE: 17/12/23 00:34:09 GMT FROM: Takanori Sakamoto at AGU 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; Poolakkil et al., GCN circ. 22233; Kozlova et al., GCN circ. 22244) 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.