{
  "id": "1705.07553",
  "version": "v1",
  "published": "2017-05-22T04:54:53.000Z",
  "updated": "2017-05-22T04:54:53.000Z",
  "title": "A Multi-telescope Campaign on FRB 121102: Implications for the FRB Population",
  "authors": [
    "C. J. Law",
    "M. W. Abruzzo",
    "C. G. Bassa",
    "G. C. Bower",
    "S. Burke-Spolaor",
    "B. J. Butler",
    "T. Cantwell",
    "S. H. Carey",
    "S. Chatterjee",
    "J. M. Cordes",
    "P. Demorest",
    "J. Dowell",
    "R. Fender",
    "K. Gourdji",
    "K. Grainge",
    "J. W. T. Hessels",
    "J. Hickish",
    "V. M. Kaspi",
    "T. J. W. Lazio",
    "M. A. McLaughlin",
    "D. Michilli",
    "K. Mooley",
    "Y. C. Perrott",
    "S. M. Ransom",
    "N. Razavi-Ghods",
    "M. Rupen",
    "A. Scaife",
    "P. Scott",
    "P. Scholz",
    "A. Seymour",
    "L. G. Spitler",
    "K. Stovall",
    "S. P. Tendulkar",
    "D. Titterington",
    "R. S. Wharton",
    "P. K. G. Williams"
  ],
  "comment": "17 pages, 7 figures. Submitted to AAS Journals",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "We present results of the coordinated observing campaign that made the first subarcsecond localization of a Fast Radio Burst, FRB 121102. During this campaign, we made the first simultaneous detection of an FRB burst by multiple telescopes: the VLA at 3 GHz and the Arecibo Observatory at 1.4 GHz. Of the nine bursts detected by the Very Large Array at 3 GHz, four had simultaneous observing coverage at other observatories. We use multi-observatory constraints and modeling of bursts seen only at 3 GHz to confirm earlier results showing that burst spectra are not well modeled by a power law. We find that burst spectra are characterized by a ~500 MHz envelope and apparent radio energy as high as $10^{40}$ erg. We measure significant changes in the apparent dispersion between bursts that can be attributed to frequency-dependent profiles or some other intrinsic burst structure that adds a systematic error to the estimate of DM by up to 1%. We use FRB 121102 as a prototype of the FRB class to estimate a volumetric birth rate of FRB sources $R_{FRB} \\approx 5x10^{-5}/N_r$ Mpc$^{-3}$ yr$^{-1}$, where $N_r$ is the number of bursts per source over its lifetime. This rate is broadly consistent with models of FRBs from young pulsars or magnetars born in superluminous supernovae or long gamma-ray bursts, if the typical FRB repeats on the order of thousands of times during its lifetime.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-05-22T04:54:53.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "frb population",
      "multi-telescope campaign",
      "implications",
      "burst spectra",
      "long gamma-ray bursts"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 17,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}