Gamma-ray Burst 130216

(All information courtesy of the instrument teams.)

Previous IAU Circulars

• none

• GCN Circular #14226
  J. R. Cummings (NASA/GSFC/CRESST) reports on behalf of the Swift-BAT team
  At 18:58:12 Swift-BAT rate-triggered on GRB 130216B (BAT trigger 548918). No significant source was found in onboard processing. This was the same event as Fermi GBM trigger 382733894. In ground analysis, a significant unknown source was found at RA, Dec 58.875, +2.040, which is:

  RA (J2000)   03h 55m 30.1s
  Dec (J2000)  02d 02m 24s  
  

  with a 90% error radius of approximately 2 arcmin.
  This position is within 2 arcmin of a low-redshift galaxy, 2MASX J03553770+0202484.
  The burst had two peaks each about 2 seconds long, the first weaker, with a total duration about 4 seconds long. A Swift TOO request has been submitted, but the source is in Sun constraint at the present time.
• GCN Circular #14231
  D. A. Perley (Caltech) and S. B. Cenko (UC Berkeley) report:
  We imaged the BAT position of GRB 130216B (Cummings et al., GCN 14226) on 2013-02-17 (UT) in Ks-band at two different epochs: 10 one-minute exposures between 04:11 and 04:26 followed by 11 one-minute exposures between 05:27 and 05:45. The FOV covers the entire BAT error circle.
  No new sources are seen in the field relative to the 2MASS catalog. Digital image subtraction of the two epochs gives a limit on variability of Ks >~ 18.6 mag (5 sigma) between 9.33 and 10.63 hours after the BAT trigger. In particular, we do not identify any variable sources or pointlike objects at the location of the 2MASS galaxy mentioned by Cummings et al, which our observations resolve into a highly-inclined spiral galaxy (major axis diameter ~40 arcsec).
• GCN Circular #14232
  J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):
  Using the data set from T-0 to T+10 sec, we report further analysis of BAT GRB 130216B (trigger #548918) (Cummings, GCN Circ. 14226). The BAT ground- calculated position is RA, Dec 58.866, +2.036, which is:

  RA (J2000)   03h 55m 27.9s 
  Dec (J2000)  02d 02m 10s   
  

  with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 11%.
  The mask-weighted light curve shows two peaks, the smaller from T+0 to T+2 and the larger from T+2 to T+4. Each is symmetrical in time. T90 (15-350 keV) is 3.7 +- 0.5 sec (estimated error including systematics).
  The time-averaged spectrum from T+0 to T+4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.77 +- 0.08. The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-6 +erg/cm2. The 1-sec peak photon flux measured from T+2.5 sec in the 15-150 keV band is 7.4 +- 0.6 ph/cm2/sec. All the quoted errors are at the 90% confidence level.
  Because this burst was not located in onboard processing, the full burst response was not initiated and not all of the normal data products are available. A Swift TOO to determine the position of the x-ray afterglow has been approved, and will take place once the source comes out of constraint on February 19th.
• GCN Circular #14235
  V.Chaplin (UAH) reports on behalf of the Fermi GBM Team:
  "At 18:58:11.70 UT on 16 Feb 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130216B (trigger 382733894 / 130216790), which was also located in Swift/BAT ground analysis (Cummings 2013, GCN 14226). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 93 degrees.
  The GBM light curve shows a single pulse with a duration (T90) of about 15 s (50-300 keV). The time-averaged spectrum from T0-2.5 s to T0+6.8 s is fit by a power law function with an exponential high-energy cutoff. The power law index is -1.7 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 119 +/- 16 keV.
  The event fluence (10-1000 keV) in this time interval is (4.8 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+2.0 s in the 10-1000 keV band is 15.5 +/- 0.5 ph/s/cm^2.
  A Band function fits the spectrum equally well with Epeak= 91 +/- 21 keV, alpha = -1.6 +/- 0.1 and beta = -2.2 +/- 0.2.
  The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
• GCN Circular #14239
  E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich 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
  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-VWF robotic telescope (MASTER-Net: http://observ.pereplet.ru) in Kislovodsk was pointed to the GRB130216A 12 sec after notice time and 53 sec after GRB time at 2013-02-16 18:59:04.829 UT using FERMI coordinates (V.Chaplin et. al. GCN14235). We observ SWIFT error-box ( J. R. Cummings et al. GCN14232 ) by very wide field cameras (FOV=400 sq. deg.) and haven`t found optical transient on images with 5-sigma upper limit has been about 10 mag.
  Observations were made in bad weather condition at zenith distanse z=70 deg.
  The message may be cited.
• GCN Circular #14242
  P. D'Avanzo, S. Campana, A. Melandri (INAF-OAB) report on behalf of the Swift team:
  We have analysed 1.9 ks of XRT data for GRB 130216B (Cummings GCN Circ. 14226; Chaplin GCN Circ. 14235), from 247.9 ks to 277.3 ks after the BAT trigger. The data are all in Photon Counting (PC) mode. No bright X-ray afterglow is detected inside the refined BAT error circle (Cummings et al. GCN Circ. 14232). The 3sigma upper limit is of 9.3 x 10^-3 cts/s.
  This corresponds to an observed 0.3-10 keV flux of 3.6 x 10^-13 erg/cm2/s (assuming a typical GRB spectrum with photon spectral index of 2). If we consider the Galactic absorption in this direction (1.3 x 10^21 cm^-2; Kalberla et al. 2005) this corresponds to an unabsorbed flux of 4.7 x 10^-13 erg/cm2/s.
  We note that there is a flux excess (SNR~2) at the edge (but inside) of the 1.5 arcmin radius BAT error circle, at the following position: RA, Dec=58.84993, +2.05183 which is equivalent to

  RA (J2000): 03h 55m 23.98s
  Dec (J2000): +02d 03' 06.6"
  

  with an uncertainty of 8.6 arcsec (radius, 90% confidence). The count rate at this position is (2.5 +/- 1.4) x 10^-3 cts/s.
• GCN Circular #14249
  T. Yasuda, M. Tashiro, Y. Terada, W. Iwakiri, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki), K. Yamaoka, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata, T. Kawano, K. Takaki, R. Nakamura, Y.Tanaka, M. Ohno, Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), Y. E. Nakagawa (Waseda U.), Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report:
  The GRB 130216B (Cummings 2013, GCN 14226) was triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2013/02/16 18:58:13.41 UT (=T0).
  The observed light curve shows a double-peaked structure starting at T0-3.0 s and ending at T0+4.5 s with a duration (T90) of about 7.44 seconds. The fluence in 100 - 1000 keV was 1.81 (+0.21/-0.35) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0 was 2.62 (+0.46/-0.62) photons/cm^2/s in the same energy range.
  Preliminary result shows that the time-averaged spectrum from T0-1.0 s to T0+6.5 s is well fitted by a single power-law with a photon index of 2.93 (+0.68/-0.35) (chi^2/d.o.f = 12.5/14).
  The light curves for this burst will be available at:
  http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html