//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21993 SUBJECT: GRB 171011A: Swift detection of a burst DATE: 17/10/11 18:40:36 GMT FROM: David Palmer at LANL J.D. Gropp (PSU), J. R. Cummings (NASA/UMBC), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the Swift Team: At 18:32:47 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 171011A (trigger=778154). Swift could not slew to the burst due to the Sun observing constraint. The BAT on-board calculated location is RA, Dec 236.761, -10.071 which is RA(J2000) = 15h 47m 03s Dec(J2000) = -10d 04' 14" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak structure with a duration of about 5 sec. The peak count rate was ~10,000 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to a Sun observing constraint, Swift cannot slew to the BAT position until 11:46 UT on 2018 January 03. There will thus be no XRT or UVOT data for this trigger before this time. Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu). 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/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21994 SUBJECT: GRB 171011A: MASTER-SAAO optical observations DATE: 17/10/11 19:12:29 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, 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 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 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 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 II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in SAAO was pointed to the GRB171011A 34 sec after notice time and 273 sec after trigger time at 2017-10-11 18:37:20 UT. On our first (50s exposure) set we not found optical transient within SWIFT error-box (ra=236.758 dec=-10.0703 r=0.1) brighter then 17.7. The observations made on zenit distance = 80 degrees, galaxy latitude b = 33 degree. The moon (59 % bright part) below the horizon (The altitude of the Moon is -51 degree ). The sun altitude is -23.4 degree. The error box can be observed till sunrise at 2017-10-12 03:59:47. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21996 SUBJECT: GRB 171011A: TAROT Calern observatory optical observations DATE: 17/10/11 21:25:44 GMT FROM: Alain Klotz at IRAP-CNRS-OMP Klotz A., Noysena.K., Atteia J.L. (CNRS-OMP-IRAP), Boer, M., Eymar, L. (CNRS-ARTEMIS), Gendre B. (UVI - Etelman Obs.) report: We imaged the field of GRB 171011A detected by SWIFT (trigger 778154) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 41.5s after the GRB trigger (12.6s after the notice). The elevation of the field decreased from 7 degrees above horizon and weather conditions were good. The first image is trailed with a duration of 60.0s (see the description in Klotz et al., 2006, A&A 451, L39). We do not detect any OT with a limiting magnitude of: t0+41.5s to t0+101.5s : Rlim = 16.3 The second image is 30.0s exposure in tracking mode: t0+114.1s to t0+144.1s : Rlim = 16.6 We co-added a series of exposures: t0+114.1s to t0+405.3s : Rlim = 17.4 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 21998 SUBJECT: IPN Triangulation of GRB 171011B (long/very bright) DATE: 17/10/11 22:58:57 GMT FROM: Dmitry Svinkin at Ioffe Institute K. Hurley, on behalf of the IPN, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova, and T. Cline on behalf of the Konus-Wind team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, and W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the GRS-Odyssey GRB team, report: The long-duration, very bright GRB 171011B was detected by Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT) at about 3935 s UT (01:05:35). The burst was outside the coded field of view of the BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 158.860 (10h 35m 26s) +1.646 ( +1d 38' 46") Corners: 159.793 (10h 39m 10s) -2.035 ( -2d 02' 06") 158.437 (10h 33m 45s) +4.418 ( +4d 25' 05") 158.940 (10h 35m 46s) +6.060 ( +6d 03' 36") 159.687 (10h 38m 45s) -0.726 ( +0d 43' 33") --------------------------------------------- The error box area is 2.646 sq. deg, and its maximum dimension is 8.14 deg (the minimum one is 23.5 arcmin). The Sun distance was 37 deg. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB171011_T03931/IPN The time history and spectrum will be given in forthcoming GCN Circulars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22005 SUBJECT: Konus-Wind observation of GRB 171011B DATE: 17/10/12 13:27:38 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, A. Tsvetkova, A. Lysenko, A.Kozlova, and T. Cline on behalf of the Konus-Wind team, report: The long-duration, very intense GRB 171011B (IPN triangulation: Hurley et al., GCN Circ. 21998) triggered Konus-Wind at T0=3931.430 s UT (01:05:31.430). The burst light curve shows a multipeaked structure which starts at ~T0-7.3 s and has a total duration of ~18.2 s. The emission is seen up to ~20 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB171011_T03931/ As observed by Konus-Wind, the burst had a fluence of 7.02(-0.56,+0.57)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+1.456 s, of 5.55(-0.61,+0.62)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+10.496 s) is best fit in the 20 keV - 20 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.54(-0.12,+0.14), the high energy photon index beta = -2.28(-0.16,+0.12), the peak energy Ep = 315(-33,+37) keV (chi2 = 98/97 dof). The spectrum near the maximum count rate (measured from T0+0.256 to T0+1.792 s) is best fit in the 20 keV - 20 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.51(-0.11,+0.14), the high energy photon index beta = -2.59(-0.34,+0.21), the peak energy Ep = 416(-48,+50) keV (chi2 = 78/65 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22006 SUBJECT: GRB 171011A: Swift-BAT refined analysis DATE: 17/10/12 14:47:20 GMT FROM: Amy Lien at GSFC J. R. Cummings (CPI), S. D. Barthelmy (GSFC), J.D. Gropp (PSU), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-119 to T+54 sec from the recent telemetry downlink, we report further analysis of BAT GRB 171011A (trigger #778154) (Gropp et al., GCN Circ. 21993). The BAT ground-calculated position is RA, Dec = 236.766, -10.064 deg which is RA(J2000) = 15h 47m 03.7s Dec(J2000) = -10d 03' 50.2" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 63%. The mask-weighted light curve shows a single-peaked light curve that starts and peaks at ~ T0, and ends at ~ T+3 s. T90 (15-350 keV) is 2.27 +- 0.24 sec (estimated error including systematics). The time-averaged spectrum from T-0.06 to T+2.74 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.68 +- 0.08. The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.08 sec in the 15-150 keV band is 7.0 +- 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/778154/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22022 SUBJECT: GRB 171011B CALET Gamma-Ray Burst Monitor detection DATE: 17/10/18 11:57:19 GMT FROM: Takanori Sakamoto at AGU P. S. Marrocchesi (U of Siena), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada, A. Tezuka, S. Matsukawa (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 (U of Siena) and the CALET collaboration: The long-duration GRB 171011B (Hurley et al., GCN Circ. 21998; Svinkin et al., GCN Circ. 22005) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 01:05:36.47 on 11 October 2017. The burst signal was seen by the all CGBM instruments. The light curve of the SGM shows a single peak. The emission starts at T0 sec and the brightest pulse peaks at T+1.5 sec. The entire emission ends at T+3.5 sec. The T90 duration measured by the SGM data is 2.0 +- 0.3 sec (40-1000 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1191719089/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22026 SUBJECT: GRB 171011B: Insight-HXMT detection DATE: 17/10/19 09:45:28 GMT FROM: Juan Zhang at IHEP/CAS/POLAR J. Zhang, J. Y. Liao, C. K. Li, X. B. Li, Y. Huang, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu, J. L. Zhao, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, H. Y. Wang, M. Wu, Y. P. Xu, A. M. Zhang, Y. F. Zhang, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: During the commissioning phase, at 2017-10-11T01:05:36 (T0), Insight-HXMT/HE detected GRB 171011B (trigger ID: HEB171011045) in a routine search of the data, which is also detected by CALET (Marrocchesi et al., GCN 22022) and INTEGRAL, etc. This burst has been localized by IPN triangulation (Hurley et al., GCN Circ. 21998). The Insight-HXMT light curve consists of multi-pulses with a duration (T90) of 1.6 s measured from T0+1.3 s to T0+2.9 s. The 20-ms peak rate, measured from T0+1.98 s, is 23852.4 cnts/sec. The total counts from this burst is 19179.3 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB171011B_LC.pdf The time-averaged spectrum from T0-1 s to T0+7 s is adequately fit by a Band spectrum with alpha = 3.94 +/- 0.86, beta = -2.65 +/- 0.16 and E_peak = 339.29 +/- 19.71. The energy fluence is (5.45 +/- 0.24)E-05 erg/cm^2 in 200 - 5000 keV in this time interval. All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (record energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. The analysis results presented above are preliminary; final results will be published elsewhere. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org/index.php/enhome .