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New Determinations of the UV Luminosity Functions from z ∼ 9 to 2 Show a Remarkable Consistency with Halo Growth and a Constant Star Formation Efficiency

Bouwens, R. J. ; Oesch, P. A. ; Stefanon, M. ; Illingworth, G. ; Labbé, I. ; Reddy, N. ; Atek, H. ; Montes, M. ; Naidu, R. ; Nanayakkara, T. ; Nelson, E. ; Wilkins, S.

The Astronomical journal, 2021-08, Vol.162 (2), p.47 [Periódico revisado por pares]

Madison: The American Astronomical Society

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Título:
New Determinations of the UV Luminosity Functions from z ∼ 9 to 2 Show a Remarkable Consistency with Halo Growth and a Constant Star Formation Efficiency
Autor: Bouwens, R. J. ; Oesch, P. A. ; Stefanon, M. ; Illingworth, G. ; Labbé, I. ; Reddy, N. ; Atek, H. ; Montes, M. ; Naidu, R. ; Nanayakkara, T. ; Nelson, E. ; Wilkins, S.
Assuntos: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; EFFICIENCY ; Evolution ; GALAXIES ; Galaxy evolution ; High-redshift galaxies ; Hubble deep field ; Hubble Space Telescope ; LUMINOSITY ; Luminosity function ; Lyman-break galaxies ; OTHER INSTRUMENTATION ; POLYNOMIALS ; Space telescopes ; Star & galaxy formation ; Star formation ; STARS ; Stellar evolution ; TELESCOPES
É parte de: The Astronomical journal, 2021-08, Vol.162 (2), p.47
Notas: Galaxies and Cosmology
AAS30319
Descrição: Abstract Here we provide the most comprehensive determinations of the rest-frame UV luminosity function (LF) available to date with the Hubble Space Telescope (HST) at z ∼ 2–9. Essentially all of the noncluster extragalactic legacy fields are utilized, including the Hubble Ultra Deep Field, the Hubble Frontier Fields parallel fields, and all five CANDELS fields, for a total survey area of 1136 arcmin 2 . Our determinations include galaxies at z ∼ 2–3 leveraging the deep HDUV, UVUDF, and ERS WFC3/UVIS observations available over an ∼150 arcmin 2 area in the GOODS-North and GOODS-South regions. All together, our collective samples include >24,000 sources, >2.3× larger than previous selections with HST. We identify 5766, 6332, 7240, 3449, 1066, 601, 246, and 33 sources at z ∼ 2, 3, 4, 5, 6, 7, 8, and 9, respectively. Combining our results with an earlier z ∼ 10 LF determination by Oesch et al., we quantify the evolution of the UV LF. Our results indicate that there is (1) a smooth flattening of the faint-end slope α from α ∼ −2.4 at z ∼ 10 to α ∼ −1.5 at z ∼ 2, (2) minimal evolution in the characteristic luminosity M * at z ≥ 2.5, and (3) a monotonic increase in the normalization log 10 ϕ * from z ∼ 10 to 2, which can be well described by a simple second-order polynomial, consistent with an “accelerated” evolution scenario. We find that each of these trends (from z ∼ 10 to 2.5 at least) can be readily explained on the basis of the evolution of the halo mass function and a simple constant star formation efficiency model.
Editor: Madison: The American Astronomical Society
Idioma: Inglês

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New Determinations of the UV Luminosity Functions from z ∼ 9 to 2 Show a Remarkable Consistency with Halo Growth and a Constant Star Formation Efficiency

Bouwens, R. J. ; Oesch, P. A. ; Stefanon, M. ; Illingworth, G. ; Labbé, I. ; Reddy, N. ; Atek, H. ; Montes, M. ; Naidu, R. ; Nanayakkara, T. ; Nelson, E. ; Wilkins, S.

Madison: The American Astronomical Society

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