{
  "bibcode": "2018GCN.22689....1M",
  "body": "C. Malacaria (NASA-MFSC/USRA) and E. Bissaldi (Politecnico & INFN Bari)\r\nreport on behalf of the Fermi GBM Team:\r\n\r\n\"At 12:57:09.91 UT on 5 May 2018, the Fermi Gamma-Ray Burst Monitor\r\ntriggered and located GRB 180505A (trigger 547217834 / 180505540).\r\nThe on-ground calculated location, using the GBM trigger data, is\r\n\r\nRA = 4.51, Dec = -59.89\r\n\r\n(J2000 degrees), with an uncertainty of 1.2 degrees (radius, 1-sigma containment,\r\nstatistical only; there is additionally a systematic\r\nerror which we have characterized as a core-plus-tail model, with 90% of\r\nGRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg\r\nsystematic error [Connaughton et al. 2015, ApJS, 216, 32] ).\r\n\r\nThe angle from the Fermi LAT boresight at the GBM trigger time is 124 degrees.\r\n\r\nThe GBM light curve shows multiple peaks\r\nwith a duration (T90) of about 22 s (50-300 keV).\r\nThe time-averaged spectrum from T0-3.5 s to T0+31 s is\r\nbest fit by a power law function with an exponential\r\nhigh-energy cutoff.  The power law index is -1.38 +/- 0.03 and\r\nthe cutoff energy, parameterized as Epeak, is 235 +/- 19 keV\r\n\r\nThe event fluence (10-1000 keV) in this time interval is\r\n(2.38 +/- 0.07)E-05 erg/cm^2. The 1-s peak photon flux measured\r\nstarting from T0+20.99 s in the 10-1000 keV band\r\nis 29.2 +/- 0.8 ph/s/cm^2.\r\n\r\nA Band function fits the spectrum equally well\r\nwith Epeak= 233 +/- 25 keV, alpha = -1.38 +/- 0.04 and beta = -3.09 +/- 1.32.\r\n\r\n\r\nThe spectral analysis results presented above are preliminary;\r\nfinal results will be published in the GBM GRB Catalog.\"",
  "circularId": 22689,
  "createdOn": 1525548784000,
  "email": "christian.malacaria@nasa.gov",
  "subject": "GRB 180505A: Fermi GBM detection",
  "submitter": "Christian Malacaria at U of Alabama/MSFC  <christian.malacaria@nasa.gov>",
  "eventId": "GRB 180505A"
}