{
  "bibcode": "2019GCN.23707....1H",
  "body": "R. Hamburg (UAH), P. Veres (UAH), C. Meegan (UAH), E. Burns (GSFC),\nV. Connaughton (USRA), A. Goldstein (USRA), D. Kocevski, and O.J. Roberts\n(USRA)\nreport on behalf of the Fermi GBM Team:\n\n\"At 20:57:02.63 UT on 14 January 2019, the Fermi Gamma-Ray Burst Monitor\ntriggered and located GRB 190114C (trigger 569192227 / 190114873)\nwhich was also detected by the Swift/BAT (Gropp et al. 2019, GCN 23688),\nMASTER (Tyurina et al. 2019, GCN 23690; Lipunov et al. 2019, GCN 23693),\nPan-STARRS (de Ugarte Postigo et al. 2019, GCN 23692), NOT\n(Selsing et al. 2019, GCN 23695), OASDG (Izzo et al. 2019, GCN 23699),\nand GROND (Bolmer et al. 2019, GCN 23702) optical telescopes, and at\nVery High Energy (VHE) by the MAGIC telescope (Mirzoyan et al. 2019,\nGCN 23701). The GBM on-ground location is consistent with the Swift/BAT\nposition.\n\nThe angle from the Fermi LAT boresight at the GBM trigger time is 68\ndegrees.\n\nThe GBM light curve shows a very bright, multi-peaked pulse starting from\nabout T0+0 s to T0+15 s and is followed by a weaker pulse occurring at\napproximately T0+15 s to T0+25 s. There is also evidence of fainter\nemission\nlasting to about T0+200 s. The calculated duration (T90) is about\n116 s (50-300 keV). The time-averaged spectrum from T0-0.00 s to\nT0+38.59 s can be fit by a Band function with Epeak = 998.6 +/- 11.9 keV,\nalpha = -1.058 +/- 0.003, and beta = -3.18 +/- 0.07. The event fluence\n(10-1000 keV) in this time interval is (3.99E-04 +/- 8.10E-07) erg/cm^2.\nThe 1-sec peak photon flux measured starting from T0+3.84 s in the 10-1000\nkeV band is 246.86 +/- 0.86 ph/s/cm^2.\n\nUsing the Band spectral fit and the distance measure of\nz = 0.42 (Selsing et al. 2019), we calculate the energetics of GRB 190114C.\nWe estimate that the isotropic energy release in gamma-rays Eiso = 3E53\nerg,\nand the isotropic peak luminosity Liso = 1E53 erg/s,\nin the 1 keV ��� 10 MeV energy band.\n\nPreliminary spectral analysis shows a strong statistical preference for an\nextra power-law component, previously seen in some bright bursts.\nThe TeV observations by MAGIC and the optical polarization observations by\nMASTER begin at about T0+50 s. This is well after the main peaks observed\nin GBM, but significant GBM emission is evident out to about 200 s,\ncovering\nthe start of these observations.\n\nThe spectral analysis results presented above are preliminary;\nfinal results will be published in the GBM GRB Catalog.\"",
  "circularId": 23707,
  "createdOn": 1547531982000,
  "email": "rkh0007@uah.edu",
  "subject": "GRB 190114C: Fermi GBM detection",
  "submitter": "Rachel Hamburg at UAH  <rkh0007@uah.edu>",
  "eventId": "GRB 190114C"
}