{
  "bibcode": "2016GCN.20127....1B",
  "body": "E. Burns (UAH), A. Goldstein (USRA), P. Jenke (UAH),\nM. S. Briggs (UAH), and L. Blackburn (CfA) report on behalf\nof the Fermi GBM team:\n\nWe have searched the Fermi Gamma-ray Burst Monitor data for a\ngamma-ray counterpart to the IceCube neutrino 161103\n(Taboada 2016, GCN 20119).\n\nThe location of the neutrino was observed by GBM with good\ngeometry. The closest on-board trigger was more than 10 hours\nbefore the neutrino time and was terrestrial in origin.\n\nMeasurements using the Earth Occultation technique (Wilson-Hodge\net al. 2012, ApJS, 201, 33) around this position place a three sigma one\nday flux upper limit of about 190 mCrab between 12 and 100 keV between\nOctober 31st and November 3rd.\n\nA seeded search for impulsive emission with duration between 0.128 s and\n8.192 s around the time and sky location of the detected neutrino yielded\nno significant candidates above the GBM background. The search method was\ndeveloped to look for electromagnetic counterparts in the GBM data of\nsub-threshold gravitational wave signals found in the LIGO data\n(Blackburn et al. 2015, ApJS, 217, 8), with improvements to be described\nin a forthcoming article. Here the search was run from 30 s before to 30 s\nafter the reported neutrino detection time and seeded with its location.\n\nA blind search for untriggered impulsive emission in the GBM data\ncentered on the neutrino detection looking for events between 0.1 s and\n32 s durations yielded no candidates consistent with the position of the\nneutrino. This search technique was developed for the detection of\nuntriggered short GRBs in the GBM data (Briggs et al., in prep.).\n\nThere are some longer term, low energy fluctuations that localize away\nfrom the neutrino direction. With no impulsive emission found we set\nmodel-dependent 1 second peak flux 3 sigma upper limits on prompt\nemission. Using a cutoff power law model with index -0.42 and Epeak of\n566 keV, representative of a typical short GRB observed by GBM, the limit\nin the 10-1000 keV range is 9.1x10^-5 erg/cm^2. For a Band function with\nEpeak, alpha, beta = 300, -1.0, -2.5, similar to long GRBs, gives an upper\nlimit of 4.6x10^-5 erg/cm^2 in 10-1000 keV. These limits are higher than\nusual as a result of highly variable backgrounds around event time.",
  "circularId": 20127,
  "createdOn": 1478292246000,
  "email": "eb0016@uah.edu",
  "subject": "Fermi GBM Observations of IceCube-161103",
  "submitter": "Eric Burns at U of Alabama  <eb0016@uah.edu>"
}