The evolution of the [O II], H β and [O III] emission line luminosity functions over the last nine billions years

Comparat, J.; Zhu, G.; Gonzalez-Perez, V.; Norberg, P.; Newman, J.; Tresse, L.; Richard, J.; Yepes, G.; Kneib, J.-P.; Raichoor, A.; Prada, F.; Maraston, C.; Yèche, C.; Delubac, T.; Jullo, E.

doi:10.1093/mnras/stw1393

The evolution of the [O II], H β and [O III] emission line luminosity functions over the last nine billions years

Comparat, J.; Zhu, G.; Gonzalez-Perez, V.; Norberg, P.; Newman, J.; Tresse, L.; Richard, J.; Yepes, G.; Kneib, J.-P.; Raichoor, A.; Prada, F.; Maraston, C.; Yèche, C.; Delubac, T.; Jullo, E.

Authors

J. Comparat

G. Zhu

V. Gonzalez-Perez

Professor Peder Norberg peder.norberg@durham.ac.uk
Professor

J. Newman

L. Tresse

J. Richard

G. Yepes

J.-P. Kneib

A. Raichoor

F. Prada

C. Maraston

C. Yèche

T. Delubac

E. Jullo

Abstract

Emission line galaxies are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, [OII](λλ3726,3729)[OII](λλ3726,3729) (0.5 < z < 1.3), Hβ (λ4861) (0.3 < z < 0.8) and [OIII](λ5007)[OIII](λ5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of ∼107 Mpc3. We present the first measurement of the Hβ LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity (L*) and density (ϕ*) of all LFs increase with redshift. Using the Schechter model over the redshift ranges considered, we find that, for [OII][OII] emitters, the characteristic luminosity L*(z = 0.5) = 3.2 × 1041 erg s−1 increases by a factor of 2.7 ± 0.2 from z = 0.5 to 1.3; for Hβ emitters L*(z = 0.3) = 1.3 × 1041 erg s−1 increases by a factor of 2.0 ± 0.2 from z = 0.3 to 0.8; and for [OIII][OIII] emitters L*(z = 0.3) = 7.3 × 1041 erg s−1 increases by a factor of 3.5 ± 0.4 from z = 0.3 to 0.8.

Citation

Comparat, J., Zhu, G., Gonzalez-Perez, V., Norberg, P., Newman, J., Tresse, L., …Jullo, E. (2016). The evolution of the [O II], H β and [O III] emission line luminosity functions over the last nine billions years. Monthly Notices of the Royal Astronomical Society, 461(1), 1076-1087. https://doi.org/10.1093/mnras/stw1393

Journal Article Type	Article
Acceptance Date	Jun 7, 2016
Online Publication Date	Jun 9, 2016
Publication Date	Sep 1, 2016
Deposit Date	Sep 28, 2016
Publicly Available Date	Oct 6, 2016
Journal	Monthly Notices of the Royal Astronomical Society
Print ISSN	0035-8711
Electronic ISSN	1365-2966
Publisher	Royal Astronomical Society
Peer Reviewed	Peer Reviewed
Volume	461
Issue	1
Pages	1076-1087
DOI	https://doi.org/10.1093/mnras/stw1393

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This article has been published in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.