{
  "id": "1405.5759",
  "version": "v2",
  "published": "2014-05-22T14:04:07.000Z",
  "updated": "2014-06-08T16:39:15.000Z",
  "title": "Star Formation Rates from [CII] 158 um and Mid Infrared Emission Lines for Starbursts and AGN",
  "authors": [
    "Lusine Sargsyan",
    "Anahit Samsonyan",
    "Vianney Lebouteiller",
    "Daniel Weedman",
    "Donald Barry",
    "Jeronimo Bernard-Salas",
    "James Houck",
    "Henrik Spoon"
  ],
  "comment": "Accepted 2014 May 21 for publication in The Astrophysical Journal; submitted 2013 September 4; corrected arXiv version adds a reference",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "A summary is presented for 130 galaxies observed with the Herschel PACS instrument to measure fluxes for the [CII] 158 um emission line. Sources cover a wide range of active galactic nucleus to starburst classifications, as derived from polycyclic aromatic hydrocarbon (PAH) strength measured with the Spitzer Infrared Spectrograph. Redshifts from [CII] and line to continuum strengths (equivalent width of [CII]) are given for the full sample, which includes 18 new [CII] flux measures. Calibration of L([CII)]) as a star formation rate (SFR) indicator is determined by comparing [CII] luminosities with mid-infrared [NeII] and [NeIII] emission line luminosities; this gives the same result as determining SFR using bolometric luminosities of reradiating dust from starbursts: log SFR = log L([CII)]) - 7.0, for SFR in solar masses per year and L([CII]) in solar luminosities. We conclude that L([CII]) can be used to measure SFR in any source to a precision of ~ 50%, even if total source luminosities are dominated by an AGN component. The line to continuum ratio at 158 um, EW([CII]), is not significantly greater for starbursts (median EW([CII]) = 1.0 um) compared to composites and AGN (median EW([CII]) = 0.7 um), showing that the far infrared continuum at 158 um scales with [CII] regardless of classification. This indicates that the continuum at 158 um also arises primarily from the starburst component within any source, giving log SFR = log vLv(158 um) - 42.8 for SFR in solar masses per year and vLv(158 um) in erg per sec.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2014-06-08T16:39:15.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "star formation rate",
      "infrared emission lines",
      "luminosities",
      "median ew",
      "solar masses"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/790/1/15",
      "journal": "The Astrophysical Journal",
      "year": 2014,
      "month": "Jul",
      "volume": 790,
      "number": 1,
      "pages": 15
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2014ApJ...790...15S"
    }
  }
}