X-factor (astrophysics)

The X-factor in astrophysics, often labeled XCO, is an empirically determined proportionality constant which converts carbon monoxide (CO) emission line brightness to molecular hydrogen (H2) mass.

Origin

The term X-factor was coined in a 1983 paper titled "Gamma-rays from atomic and molecular gas in the first galactic quadrant" and published in The Astrophysical Journal.[1][2]

Calibration

Calibrating XCO requires an independent method of determining the amount of molecular hydrogen in a given astrophysical region. While direct emission from molecular hydrogen is difficult to observe, there are other ways of inferring molecular hydrogen mass, outlined below.[3]

  • The mass of an individual molecular cloud can be inferred from its velocity dispersion. Assuming that the cloud is self gravitating and virialized, and that nearly all of the gas mass is molecular hydrogen, one obtains an estimate of the cloud's H2 mass.
  • H2 mass can be estimated through gamma ray observations, where gamma ray emission arises from the interaction of cosmic rays with H2 molecules.
  • Using optical and infrared observations, one can estimate the amount of dust in a region and convert to H2 mass through an (empirically determined) dust-to-gas ratio.

References
  1. "CfA Millimeter-Wave Group Homepage". www.cfa.harvard.edu.
  2. Lebrun, F.; Bennett, K.; Bignami, G. F.; Bloemen, J. B. G. M.; Buccheri, R.; Caraveo, P. A.; Gottwald, M.; Hermsen, W.; Kanbach, G.; Mayer-Hasselwander, H. A.; Montmerle, T.; Paul, J. A.; Sacco, B.; Strong, A. W.; Wills, R. D.; Dame, T. M.; Cohen R. S.; Thaddeus, P. (1983). "Gamma-rays from atomic and molecular gas in the first galactic quadrant". The Astrophysical Journal. 274: 231. Bibcode:1983ApJ...274..231L. doi:10.1086/161440. hdl:1887/6430.CS1 maint: uses authors parameter (link)
  3. Carilli, Chris; Walter, Fabian (18 August 2013). "Cool Gas in High Redshift Galaxies". Annual Review of Astronomy and Astrophysics. 51 (1): 105–161. arXiv:1301.0371. Bibcode:2013ARA&A..51..105C. doi:10.1146/annurev-astro-082812-140953. S2CID 119186806.


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