Gamma-ray Burst 151227B

(All information courtesy of the instrument teams.)

Previous IAU Circulars

• none

• GCN Circular #18727
  Kilian Toelge (MPE) and Elisabetta Bissaldi (Politecnico di Bari) report on behalf of the Fermi GBM Team:
  "At 05:13:48.86 UT on 27 December 2015, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 151227B (trigger 472886032 / 151227218). The on-ground calculated location, using the GBM trigger data, is RA = 287.9, DEC = 31.9 (J2000 degrees, equivalent to 19h 11m, 31d 54'), with an uncertainty of 1 degree (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 angle from the Fermi LAT boresight at the GBM trigger time is 90 degrees.
  The GBM light curve consists of three pulses with a duration (T90) of about 43.0 s (50-300 keV). The time-averaged spectrum from T0+20.0 s to T0+49.7 s is best fit by a Band function with Epeak = 310 +/- 21 keV, alpha = -1.27 +/- 0.02, and beta = -2.17 +/- 0.08.
  The event fluence (10-1000 keV) in this time interval is (8.94 +/- 0.09)E-6 erg/cm^2. The 1-sec peak photon flux measured starting from T0+29.8 s in the 8-1000 keV band is 36.1 +/- 0.5 ph/s/cm^2.
  The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
• GCN Circular #18773
  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,
  S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
  V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM 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, N. Gehrels, 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 GRB 151227B has been detected by Fermi (GBM: Toelge and Bissaldi, GCN Circ. 18727), Konus-Wind, Mars-Odyssey (HEND), INTEGRAL (SPI-ACS), and Swift (BAT), so far, at about 18829 s UT (05:13:49). 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:
     290.284 (19h 21m 08s) +35.415 (+35d 24' 55")
    Corners:
     290.279 (19h 21m 07s) +35.990 (+35d 59' 22")
     290.052 (19h 20m 13s) +36.037 (+36d 02' 12")
     290.288 (19h 21m 09s) +34.841 (+34d 50' 26")
     290.512 (19h 22m 03s) +34.792 (+34d 47' 32")
    ---------------------------------------------
  

  The error box area is 759 sq. arcmin, and its maximum dimension is 1.3 deg (the minimum one is 10.4 arcmin). The Sun distance was 60 deg.
  This box may be improved.
  A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB151227_T18827/IPN/
  The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
• GCN Circular #18781
  S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report:
  The long-duration, intense GRB 151227B (Fermi GBM detection: Toelge & Bissaldi, GCN 18727; IPN Triangulation: Hurley et al., GCN 18773) triggered Konus-Wind at T0=18827.479 s UT (05:13:47.479).
  The burst light curve shows three emission episodes with a total duration of ~48 s. The emission is seen up to ~15 MeV.
  As observed by Konus-Wind, the burst had a fluence of 6.49(-0.72,+0.72)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+29.728 s, of 1.11(-0.20,+0.19)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range).
  The time-integrated spectrum of the burst (measured from T0 to T0+43.776 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -1.19(-0.08,+0.10), the high energy photon index beta = -2.11(-0.18,+0.11), the peak energy Ep = 228(-40,+46) keV, chi2 = 110/97 dof.
  The spectrum near the peak count rate (measured from T0+24.832 to T0+35.584 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -1.25(-0.05,+0.05), the high energy photon index beta = -2.57(-1.09,+0.28), the peak energy Ep = 353(-44,+52) keV, chi2 = 111/93 dof.
  The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB151227_T18827/
  All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
• GCN Circular #18792
  K. Senuma, A. Yoshida, T. Sakamoto, I. Takahashi, Y. Kawakubo, 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 151227B (Toelge et al. GCN Circ. 18727; Hurley et al. GCN Circ. 18773; Golenetskii et al. GCN Circ. 18781) triggered the CALET Gamma-Ray Burst Monitor (CGBM) at 5:13:49.89 UT on 27 December 2015. The clear burst signal was detected by HXM1 and SGM instruments.
  The light curve of the SGM shows three main peaks. The first peak starts at T0, peaks at T0+2 sec and ends at T0+4 sec. The brightest second peak, which consists of various sub-peaks, starts at T0+20 sec, peaks at T0+31 sec and ends at T0+40 sec. The third peak starts at T0+40 sec, peaks at T0+45 sec and ends at T0+50 sec. The T90 duration measured by the SGM data is 42.0 +- 0.3 sec (40-1000 keV).
  The CGBM data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.