CaltechAUTHORS
Published August 20, 2014 | Version Submitted + Published
Journal Article Open

Star Formation at 4 < z < 6 from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH)

Creators

  • 1. ROR icon California Institute of Technology
  • 2. ROR icon Infrared Processing and Analysis Center
  • 3. ROR icon University of Tokyo
  • 4. ROR icon Harvard University
  • 5. ROR icon ETH Zurich
  • 6. ROR icon University of Edinburgh
  • 7. ROR icon National Taiwan Normal University
  • 8. ROR icon Institute of Astronomy and Astrophysics, Academia Sinica
  • 9. ROR icon Laboratoire d'Astrophysique de Marseille
  • 10. ROR icon CEA Saclay
  • 11. ROR icon University of Hawaii at Manoa
  • 12. ROR icon Institut d'Astrophysique de Paris
  • 13. ROR icon Kyoto University
  • 14. ROR icon Max Planck Institute for Extraterrestrial Physics
  • 15. ROR icon National Radio Astronomy Observatory
  • 16. ROR icon Princeton University
  • 17. ROR icon Ehime University

Abstract

Using the first 50% of data collected for the Spitzer Large Area Survey with Hyper-Suprime-Cam observations on the 1.8 deg^2 Cosmological Evolution Survey we estimate the masses and star formation rates of 3398 M_* > 10^(10) M_☉ star-forming galaxies at 4 < z < 6 with a substantial population up to M_* ≳ 10^(11.5) M_☉. We find that the strong correlation between stellar mass and star formation rate seen at lower redshift (the "main sequence" of star-forming galaxies) extends to z ~ 6. The observed relation and scatter is consistent with a continued increase in star formation rate at fixed mass in line with extrapolations from lower-redshift observations. It is difficult to explain this continued correlation, especially for the most massive systems, unless the most massive galaxies are forming stars near their Eddington-limited rate from their first collapse. Furthermore, we find no evidence for moderate quenching at higher masses, indicating quenching either has not occurred prior to z ~ 6 or else occurs rapidly, so that few galaxies are visible in transition between star-forming and quenched.

Additional Information

© 2014 The American Astronomical Society. Received 2014 April 7; accepted 2014 June 22; published 2014 August 6. The authors would like to thank Steve Bickerton, Sean Carey, Martin Elvis, and Brian Feldstein for helpful comments.

Attached Files

Published - 2041-8205_791_2_L25.pdf

Submitted - 1407.7030v1.pdf

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1407.7030v1.pdf

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Additional details

Identifiers

Eprint ID
50178
Resolver ID
CaltechAUTHORS:20141002-133810713

Related works

Describes
http://arxiv.org/abs/1407.7030 (URL)

Dates

Created
2014-10-02
Created from EPrint's datestamp field
Updated
2021-11-10
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
COSMOS , Infrared Processing and Analysis Center (IPAC) , SPLASH