Gamma-ray Burst 150210A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

• none

• GCN Circular #17432
  E. Burns (UAH) reports on behalf of the Fermi GBM Team:
  "At 22:26:24.28 UT on 10 February 2015, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 150210A (trigger 445299987 / 150210935).
  The on-ground calculated location, using the GBM trigger data, is RA = 112.9, DEC = +12.4 (J2000 degrees, equivalent to 07 h 31 m, 12 d 22 '), with an uncertainty of 2.2 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 55 degrees.
  The GBM light curve consists of a single main FRED-like peak with a duration (T90) of about 31 s (50-300 keV). The time-averaged spectrum from T0+0.002 s to T0+31.681 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.05 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 3118 +/- 216 keV.
  The event fluence (10-1000 keV) in this time interval is (1.35 +/- 0.01)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+1.024 s in the 10-1000 keV band is 19.1 +/- 0.3 ph/s/cm^2.
  The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
• GCN Circular #17438
  S. Zhu (UMD), E. Bissaldi (INFN Bari), J. Racusin (NASA/GSFC), E. Sonbas (Adiyaman Univ.), D. Kocevski (NASA/GSFC), M. Yassine (LUPM) report on behalf of the Fermi-LAT team:
  At 22:26:24.28 UT on 10 February 2015, Fermi-LAT detected high-energy emission from GRB 150210A, which was also detected by Fermi-GBM (trigger 445299987 / 150210935) (Burns, GCN 17432).
  The best LAT on-ground location is found to be
  RA, Dec = (112.15, 13.27) (J2000)
  with an error radius of 0.33 deg (90% containment, statistical error only). This position was 55 deg from the LAT boresight at the time of the trigger and is consistent with the GBM position. It remained in the LAT field of view for about 1000 seconds after trigger, and reentered the field of view at T0+5000 seconds.
  The data from the Fermi-LAT show a significant increase in the event rate within 10 degrees of the GBM location after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. More than 20 photons above 100 MeV are observed in the first 100 seconds, of which ~15 photons are coincident with the GBM peak. The highest-energy photon is a ~1 GeV event which is observed 2 seconds after the GBM trigger. Using the LAT Low Energy (LLE) data selection, an increase in the event rate at > 20 sigma significance above background was observed approximately coincident with the time of the GBM emission.
  A Swift ToO has been requested for this burst.
  The Fermi-LAT point of contact for this burst is Sylvia Zhu (sjzhu@umd.edu).
  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 #17439
  S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
  K. Hurley, on behalf of the IPN,
  V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, and
  A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, report:
  The long-duration, bright GRB 150210A has been detected by Fermi (GBM: Burns, GCN Circ. 17432; LAT: Zhu et al., GCN Circ. 17438), Konus-Wind, and INTEGRAL (SPI-ACS), so far, at about 80784 s UT (22:26:24).
  We have triangulated it to a preliminary, 3 sigma error box whose coordinates are:

    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
     111.853 (07h 27m 25s) +13.832 (+13d 49' 54")
    Corners:
     111.458 (07h 25m 50s) +11.396 (+11d 23' 45")
     111.572 (07h 26m 17s) +16.337 (+16d 20' 13")
     112.332 (07h 29m 20s) +16.259 (+16d 15' 31")
     112.206 (07h 28m 49s) +11.314 (+11d 18' 52")
    ---------------------------------------------
  

  The error box area is 3.6 sq. deg, and its maximum dimension is 5.1 deg (the minimum one is 44 arcmin). The Sun distance was 148 deg.
  The LAT (statistical-only) error circle (GCN 17438) overlaps the box. The distance between the center of the LAT position and the center of the error box is 0.63 deg.
  This box may be improved.
  A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB150210_T80787/IPN/
  The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
• GCN Circular #17440
  S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, and T. Cline on behalf of the Konus-Wind team, report:
  The long-duration, hard-spectrum GRB 150210A (Fermi-GBM detection: Burns, GCN 17432; Fermi-LAT detection: Zhu et al., GCN 17438; IPN triangulation: Golenetskii et al., GCN 17439) triggered Konus-Wind at T0=80787.209 s UT (22:26:27.209).
  The light curve shows a bright, multi-peaked pulse with a duration of ~3.5 s followed by a much weaker tail visible up to ~T0+30 s. The emission is seen up to ~10 MeV.
  The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB150210_T80787/
  As observed by Konus-Wind, the burst had a fluence of 7.8(-0.8,+0.9)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+2.368 s, of 4.2(-0.3,+0.3)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range).
  The time-averaged spectrum (measured from T0 to T0+24.832 s) is best fit in the 20 keV - 15 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.99(-0.07,+0.08), and the peak energy Ep = 2170(-340,+440) keV, chi2 = 107/98 dof. Fitting this spectrum with the Band model yields the same values of alpha and Ep with an upper limit on the high-energy photon index beta of -2.6
  The spectrum near the peak count rate (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 15 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.89(-0.06,+0.06), and the peak energy Ep = 2250(-240,+280) keV, chi2 = 126/98 dof.
  All the quoted errors are at the 90% sigma confidence level. All the quoted values are preliminary.
• GCN Circular #17441
  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 150210A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00040
  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 Circular #17446
  O. Gres ,K.Ivanov, S.Yazev, N.M.Budnev, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University
  E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya, V.Kornilov, D.Kuvshinov, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich Lomonosov Moscow State University, Sternberg Astronomical Institute, Moscow State University
  A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory
  V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk
  K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University
  V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka
  D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory
  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 Kislovodsk was pointed to the GRB150210A 22 sec after notice time and 1364 sec after trigger time at 2015-02-10 22:49:09 UT by FERMI GBM coordinates (ra=07 31 23 dec=+12 21 33 r=2.200000) (Burns et. al . GCN 17432). We cover a 70% part of FERMI LAT (Zhu et al. GCN 17438) error box with upper limit 17.5
  MASTER II robotic telescope located in Tunka was pointed to the GRB150210A 3444 sec after the LAT notice time and 60443 sec after trigger time at 2015-02-11 15:13:47 UT.
  During LAT error box inspectoion MASTER-Tunka auto-detection system discovered OT source at (RA, Dec) = 07h 29m 40.10s +14d 14m 25.5s on 2015-02-11.64502 UT (Gres et al. ATel 17446).
  The OT unfiltered magnitude is 17.4m (the limit is 20.0m). OT is located at a distance 0.2W 2.8N from a center on unknown galaxy. It seems that this supernova was found by chance during the LAT error box inspection. OT image available here http://master.sai.msu.ru/static/OT/MASTERJ072940.10+141425.5.jpg The OT is seen in 31 images. There is no minor planet at this place. We have reference image without OT on 2012-02-18.58510 UT with unfiltered magnitude limit 19.8m.
  The message may be cited.
  
• GCN Circular #17453
  V. Mangano (PSU), M.C. Stroh (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U. Leicester), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA), A. Maselli (INAF-IASFPA), D.N. Burrows (PSU) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
  Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 150210A (Zhu et al. GCN Circ. 17438) in a series of observations tiled on the sky. The total exposure time is 7.3 ks, distributed over 4 tiles; the maximum exposure at a single sky location was 4.3 ks. The data were collected between T0+66.9 ks and T0+95.4 ks, and are entirely in Photon Counting (PC) mode.
  No uncatalogued X-ray sources have been detected. The 3-sigma upper limit in the field (not including the regions where the tiles overlap) ranges from ~0.004 to ~0.008 ct s^-1, corresponding to a 0.3-10 keV observed flux of 1.5e-13 to 3.3e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum).
  A previously-catalogued X-ray source has been detected, however because it is a catalogued object it is unlikely to be the afterglow.
  The results of the XRT-team automatic analysis of the tiled XRT observations, including a position-specific upper limit calculator, are available at http://www.swift.ac.uk/xrt_products/TILED_GRB00040.
  This circular is an official product of the Swift-XRT team.