Star formation trends in high-redshift galaxy surveys: The elephant or the tail?

Martin Stringer, Shaun Cole, Carlos S. Frenk, Daniel P Stark

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

Star formation rate and accumulated stellar mass are two fundamental physical quantities that describe the evolutionary state of a forming galaxy. Two recent attempts to determine the relationship between these quantities, by interpreting a sample of star-forming galaxies at redshift of z~ 4, have led to opposite conclusions. Using a model galaxy population, we investigate possible causes for this discrepancy and conclude that minor errors in the conversion from observables to physical quantities can lead to a major misrepresentation when applied without awareness of sample selection. We also investigate, in a general way, the physical origin of the correlation between star formation rate and stellar mass within the hierarchical galaxy formation theory.

Original languageEnglish (US)
Pages (from-to)1927-1936
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Volume414
Issue number3
DOIs
StatePublished - Jul 2011
Externally publishedYes

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elephant
star formation
star formation rate
galaxies
stellar mass
trends
galactic evolution
stars
causes
trend
rate

Keywords

  • Galaxies: evolution
  • Galaxies: formation
  • Galaxies: high redshift

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Star formation trends in high-redshift galaxy surveys : The elephant or the tail? / Stringer, Martin; Cole, Shaun; Frenk, Carlos S.; Stark, Daniel P.

In: Monthly Notices of the Royal Astronomical Society, Vol. 414, No. 3, 07.2011, p. 1927-1936.

Research output: Contribution to journalArticle

Stringer, Martin ; Cole, Shaun ; Frenk, Carlos S. ; Stark, Daniel P. / Star formation trends in high-redshift galaxy surveys : The elephant or the tail?. In: Monthly Notices of the Royal Astronomical Society. 2011 ; Vol. 414, No. 3. pp. 1927-1936.
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