//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18570 SUBJECT: GRB 151107B DATE: 15/11/09 21:54:16 GMT FROM: Matthew Stanbro at UAH/Fermi Matthew Stanbro (UAH) and Charles Meegan (UAH) report on behalf of the Fermi GBM Team: "At 20:24:52.30 UT on 07 November 2015, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 151107B (trigger 468620696 / 151107851). The on-ground calculated location, using the GBM trigger data, is RA = 31.3, DEC = 45.6, with an uncertainty of 1.7 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 40 degrees. The GBM light curve consists of 2 separate episodes with a duration (T90) of about 139 s (50-300 keV). The time-averaged spectrum from T0+2 s to T0+137 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.20 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 347 +/- 25 keV The event fluence (10-1000 keV) in this time interval is (3.11 +/- 0.07)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+8.13 s in the 10-1000 keV band is 10.9 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." -- Matthew C. Stanbro Fermi GBM Graduate Research Assistant University of Alabama in Huntsville //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18574 SUBJECT: GRB 151107B: Mini-MegaTORTORA limits on simultaneous optical emission DATE: 15/11/10 17:29:27 GMT FROM: Sergey Karpov at SAO RAS S.Karpov, G.Beskin (SAO RAS and Kazan Federal University, Russia), S.Bondar, E.Ivanov, E.Katkova, A.Perkov, N.Orekhova (OJS RPC PSI, Russia), A.Biryukov (SAI MSU and Kazan Federal University, Russia), V.Sasyuk (Kazan Federal University, Russia) The localization of Fermi GBM trigger 468620696 / GRB 151107B (Stanbro et al, GCN Circ. 18570) has been observed by Mini-MegaTORTORA nine-channel wide-field monitoring system (located at Special Astrophysical Observatory near Russian 6-m telescope and belonging to Kazan Federal University) before, during and after the trigger time at 2015-11-07 20:24:52.30 UT. The whole final 1-sigma localization box (as well as 6 more degrees around it) has been covered since 20:19:23 UT (T-329.3 s) and until 20:25:18 UT (T+25.7 s, thus covering the brightest part of first gamma-ray peak) with temporal resolution of 0.1 s in white light. Dedicated real-time transient detection pipeline did not detect any events longer than 0.3 s and brighter than approximately V=10.5 mag. Visual inspection of co-added images with 10 s effective exposure (summation of 100 consecutive frames each) has not revealed any variable source down to V=12.0 mag during that interval. At 20:25:18 UT the system initiated a repointing following the initially distributed GBM coordinates, and since 20:25:55 UT (T+62.7 s, during the continuing gamma-ray activity) till 20:35:59 UT (T+666.7 s) acquired 20x9 deep images with 30 s exposures in white light in a 30x30 degree field of view centered on RA=24.1 Dec=44.8. The whole final 1-sigma localization was still inside the field of view. Quick-look analysis of the acquired data has not revealed any variable object down to roughly V=13.5 mag over that time interval. The analysis is ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18576 SUBJECT: GRB 151107B: MASTER-NET OT detection inside the FERMI error box DATE: 15/11/10 21:15:27 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias E. Gorbovskoy, V. Lipunov, V.Shumkov, N.Tyurina, V.Kornilov, P.Balanutsa, A.Kuznetsov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institute D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik Kislovodsk Solar Station of the Pulkovo Observatory O.Gress, K.Ivanov, N.M.Budnev, V.A.Poleshchuk Irkutsk State University V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk V.Krushinski, I.Zalozhnih Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER II robotic telescope (MASTER-Net http://observ.pereplet.ru) located in IAC (Tenerife, Spain) was pointed to the FERMI GBM GRB151107B 14 sec after notice time and 60 sec after trigger time at 2015-11-07 20:25:52 UT. Our first (10s exposure) set limit is 16.8 within FERMI error-box (ra=00 42 28 dec=+48 48 58 r=4.5, Stanbro and Meegan, GCN 18570). MASTER II robotic telescope located in Kislovodsk was pointed to the GRB151107B 21 sec after notice time and 66 sec after trigger time at 2015-11-07 20:25:59 UT. Our first (10s exposure) set limit is 18.1 within FERMI error-box . The summary (60sec) unfiltered optical limit is 19.5m. MASTER II robotic telescope located in SAAO (South Africa, Sutherland) was pointed to the GRB151107B 20 sec after notice time and 66 sec after trigger time at 2015-11-07 20:25:58 UT. Our first (10s exposure) set limit is 15.4. There are prompt pointing observations because duration of the GRB is ~140 s (Stanbro and Meegan, GCN 18570) After 5 minutes of alert observations of the center of error box, telescopes in IAC and Kislovodsk started the inspect survey inside large Fermi error box (ra=00 42 28 dec=+48 48 58 r=4.533300) obtained by GCN socket. As a result, we cover more than 98% of 1 sigma+systematic and 85% of 3-sigma + systematic of the FERMI GBM final error box (Stanbro et. al. GCN 18570) with upper limit up to 19 mag during this night. The coverage map is available here: http://master.sai.msu.ru/static/GRB/GRB151107B.png There is 1 possible OTs was found up to now - MASTER OT J015539.85+485955.6 published yesterday (Shumkov et al., Atel #8262). (RA, Dec) = 01h 55m 39.85s +48d 59m 55.6s The OT mag is 15.2 on 2015-11-07.99775 UT. The specrtrum was done by follow up Liverpool Telescope (La Palma) observations shows a broad continuum, consistent with that expected from a dwarf nova in outburst ( Piascik & Steele, ATel #8265). The brightness is not sufficiantly changed after half of the day (during independently ASAS detection Holoin et al., ATEL #8260) and our today imaging (2015-11-10 17:16:26.513UT, m_OT=15.5+-0.1) shows that OT doesn't fade essntially with respect to discovery magnitude contraverse to GRB optical afterglow . The search is continuing. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18577 SUBJECT: IPN triangulation of GRB151107B DATE: 15/11/11 00:48:21 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the IPN, S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline, on behalf of the Konus-Wind team, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the GRS-Odyssey GRB team, report: GRB 151107B (Stanbro and Meegan, GCN 18570) was also observed by Konus-Wind and Mars Odyssey-HEND. We have triangulated it to a preliminary annulus centered at RA, Dec(2000) = 357.447, -2.630, whose radius is 55.156 +/- 0.054 degrees (3 sigma). The minimum distance between the center line of this annulus and the MASTER-NET optical transient (Lipunov et al., GCN 18576) is 3.22 degrees, supporting the conclusion that the OT and the GRB are indeed unrelated. A map has been posted at ssl.berkeley.edu/ipn3/151107B. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18605 SUBJECT: GRB 151107B: CALET Gamma-Ray Burst Monitor detection DATE: 15/11/15 00:45:59 GMT FROM: Takanori Sakamoto at AGU A. Yoshida, T. Sakamoto, I. Takahashi, Y. Kawakubo, K. Senuma, M. Moriyama, Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 151107B (Stanbro et al. GCN Circ. 18570) triggered the CALET Gamma-Ray Burst Monitor (CGBM) at 20:24:54.77 UT on 7 November 2015. The burst was detected by all three CGBM instruments. Based on the signal-to-noise among the instruments, the incident angle of the burst was estimated as ~40-70 deg from the zenith direction of CGBM. This estimated incident angle is roughly consistent with the IPN triangulation (Hurley et al., GCN Circ. 18577). The light curve of the Soft Gamma-ray Monitor (SGM; 30 keV - 20 MeV) shows the main peak starting from T0-5 sec, peaking at T0+5 sec and ending at T0+~30 sec. The second weak peak starts from T0+90 sec, peaks at T0+95 sec and ends at T0+100 sec. The T90 duration measured by the SGM data is 95.0 +- 1.4 s (40-920 keV). Currently, CALET is in the commissioning phase. Further information about CALET and CGBM can be found at http://calet.jp/en/ and http://www.en.yoshida-agu.net/research/calet-gbm