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Star-formation efficiency at 600Myr of cosmic time

Published online by Cambridge University Press:  04 June 2020

Mauro Stefanon Open the ORCID record for Mauro Stefanon [Opens in a new window] ,
Ivo Labbé ,
Rychard Bouwens  and
Pascal Oesch
Mauro Stefanon
Affiliation:
Leiden Observatory, University of Leiden, Niels Bohrweg, 2 - 2333CA Leiden - The Netherlands email: [email protected]
Ivo Labbé
Affiliation:
Centre for Astrophysics and SuperComputing, Swinburne, University of Technology, Hawthorn, Victoria, 3122, Australia
Rychard Bouwens
Affiliation:
Leiden Observatory, University of Leiden, Niels Bohrweg, 2 - 2333CA Leiden - The Netherlands email: [email protected]
Pascal Oesch
Affiliation:
Observatoire de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
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Abstract

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Current observations suggest an accelerated evolution of the cosmic star formation rate density for 8 < z < 10, indicating that galaxy assembly experienced an extremely intense phase during the first ∼600Myr years of cosmic time. We performed a systematic search of ultrabright star-forming galaxies at z ∼ 8 over the COSMOS/UltraVISTA survey, identifying 16 candidate Lyman-break galaxies. The still large uncertainties on the associated volume density do not yet allow us to ascertain whether a different star-formation efficiency (SFE) existed at early cosmic epochs. Leveraging the deepest Spitzer/IRAC data available from the GREATS program over the CANDELS/GOODS fields, we also constructed stacked SEDs of sub- L* LBGs at z ∼ 8. We find extreme nebular line emission (EW0 (Hα) ∼ 1000Å), high specific star-formation rates (∼10/Gyr) and indication of an inverse Balmer break. These results point toward very young ages (<100 Myr), and, combined with measurements at lower redshifts, that the SFE evolved only marginally during the first ∼1.5Gyr of cosmic history.

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. 115 - 118
Copyright
© International Astronomical Union 2020

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