Gamma-ray Burst 101114A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

• none

• GCN Circular #11405
  T. Sakamoto (GSFC/UMBC), 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), C. B. Markwardt (GSFC), D. M. Palmer (LANL), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team):
  Based on the ground data processing, we found the GRB 101114A (trigger=438392) at T0=00:32:50 UT. The BAT onboard analysis of the trigger was prematurely terminated by a slew to a different target. We have only limited event-by-event data on the ground for this trigger.
  Using the data set from T0 to T0+4.1 sec, the BAT ground-calculated position in the 15-200 keV band is RA, Dec = 303.193, 14.029 deg which is

     RA(J2000)  =  20h 12m 46.3s 
     Dec(J2000) = +14d 01' 44.4" 
  

  with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The image significance is 13.6 sigma. The partial coding was 30%.
  The mask-weighted light curve shows a sigle FRED-like spike starting before T0, peaking at T0+2 sec and ending after T0+10sec. Because of the incomplete data (the event data are only available from T0 to T0+10 sec), we can only state that the duration of the burst is >10 sec.
  The time-averaged spectrum from T0 to T0+10 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.29 +- 0.17. The fluence in the 15-150 keV band is 8.0 +- 0.8 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+2.00 sec in the 15-150 keV band is 1.8 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level.
  A Swift TOO is being done to get an XRT position.
• GCN Circular #11406
  P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
  We have analysed 7.9 ks of XRT data for GRB 101114A (Sakamoto et al. et al. GCN Circ. 11405), from 73.3 ks to 91.1 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. An uncatalogued X-ray source is detected inside the BAT error circle; the source shows weak (~1-sigma) evidence of fading in this observation. Using 1631 s of PC mode data and 1 UVOT image, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 303.21110, +14.03270 which is equivalent to:

  RA (J2000): 20h 12m 50.67s
  Dec(J2000): +14d 01' 57.6"
  

  with an uncertainty of 2.8 arcsec (radius, 90% confidence). This is 64 arcsec from the BAT position of Sakamoto et al. (GCN Circ. 11405)
  A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.1 (+1.1, -0.6). The best-fitting absorption column is 1.6 (+2.5, -0.3) x 10^21 cm^-2, consistent with the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (5.5 x 10^-11) erg cm^-2 count^-1.
  The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020150.
  This circular is an official product of the Swift-XRT team.
• GCN Circular #11408
  S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team report:
  The long GRB 101114A discovered in BAT ground analysis (Sakamoto et al., GCN 11405) was detected by Konus-Wind in the waiting mode.
  The burst light curve shows a rather bright pulse at ~T0(BAT) preceded by two weak pulses at ~T0(BAT)-100 s and ~T0(BAT)-50 s. The total burst duration is ~110 s.
  As observed by Konus-Wind, the burst had a fluence of (4.7 +/- 2.4)x10^-6 erg/cm2 (in the 20 - 1200 keV energy range).
  Modeling the K-W 3-channel spectrum of the main pulse (accumulated from T0-2.2 s to T0+6.6 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = -1.15 +/- 0.29, Ep = 296 +/- 129 keV.
  All the quoted errors are estimated at the 1 sigma confidence level.
  The K-W light curve of this burst is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB101114A/
• GCN Circular #11409
  GRB 101114A: GROND Upper limits
  J. Elliott, R. Filgas and J. Greiner (all MPE Garching) report on behalf of the GROND team:
  We observed the field of GRB 101114A (Swift trigger 438392; Sakamoto et al., GCN #11405) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile).
  Observations started at 00:42 UT in twilight and just before reaching the 20 deg above horizon telescope limit, on November 16, 48 hours after the GRB trigger, and have total exposure of 425 s in g'r'i'z' and 720 s in JHK. They were performed at an average seeing of 2.5" and at an average airmass of 2.7.
  We do not detect a source within the Swift-XRT error circle reported by Evans (GCN #11406) down to the following 3 sigma upper limits (all in AB):
  g' > 21.8,
  r' > 22.1,
  i' > 21.7,
  z' > 21.5,
  J > 20.3,
  H > 19.8 and
  K > 19.2
  The given limits are derived based on calibrating the images against GROND zeropoints and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.19 in the direction of the burst (Schlegel et al. 1998).
• GCN Circular #11415
  P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
  We have performed a second epoch observation with Swift-XRT of GRB 101114A (Sakamoto et al., GCN Circ. 11405). This observation was 5.5 ks in length, beginning 3.5 days after the GRB trigger. The source reported by Evans et al. (GCN Circ. 11406) is still detected, but has faded significantly to a level of 1.6 (+/- 0.9) x 10^-3 ct/sec. We thus confirm that this is the afterglow of GRB 101114A.
  This circular is an official product of the Swift-XRT team.
• GCN Circular #11416
  W. Landsman (GSFC/Adnet) and T. Sakamoto (GSFC/UMBC) report on behalf of the Swift/UVOT team:
  The Swift/UVOT began settled observations of the field of GRB 101114A 20.3 hrs after the BAT trigger (Sakamoto et al., GCN 11405). We do not detect any source at the enhanced Swift XRT position (Evans GCN 11406, 11415). UVOT magnitude 3-sigma upper limits are reported in the following table:

  Filter  T_start  T_stop  Exp(s)  Mag (3-sigma upper limit)
  -------------------------------------------------------------
  white     74084    86413   2325 > 21.9
  v         74901    87330   2567 > 20.5
  u         73267    91074   2822 > 21.0
  

  The quoted upper limits have not been corrected for the expected Galactic extinction along the line of sight of E_(B-V) = 0.19 (Schlegel et al. 1998). All photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627).