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An older, more quiescent universe from panchromatic SED fitting of the 3D-HST survey

Published online by Cambridge University Press:  04 June 2020

Joel Leja Open the ORCID record for Joel Leja [Opens in a new window] ,
Benjamin D. Johnson ,
Charlie Conroy ,
Pieter van Dokkum ,
Joshua S. Speagle  and
the 3D-HST Team
Joel Leja
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA02138, USA
Benjamin D. Johnson
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA02138, USA
Charlie Conroy
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA02138, USA
Pieter van Dokkum
Affiliation:
Department of Astronomy, Yale University, New Haven, CT06511, USA
Joshua S. Speagle
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA02138, USA
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Abstract

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Galaxies are complicated physical systems which obey complex scaling relationships; as a result, properties measured from broadband photometry are often highly correlated, degenerate, or both. Therefore, the accuracy of basic properties like stellar masses and star formation rates (SFRs) depend on the accuracy of many second-order galaxy properties, including star formation histories (SFHs), stellar metallicities, dust properties, and many others. Here, we re-assess measurements of galaxy stellar masses and SFRs using a 14-parameter physical model built in the Prospector Bayesian inference framework. We find that galaxies are ∼0.2 dex more massive and have ∼0.2 dex lower star formation rates than classic measurements. These measurements lower the observed cosmic star formation rate density and increase the observed buildup of stellar mass, finally bringing these two metrics into agreement at the factor-of-two level at 0.5 < z < 2.5.

Keywords

galaxies: evolutiongalaxies: formationgalaxies: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 99 - 102
Copyright
© International Astronomical Union 2020

References

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