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The clustering of H $\beta$ + [O III] and [O II] emitters since z \tilde 5: dependencies with line luminosity and stellar mass

Khostovan, A.A.; Sobral, D.; Mobasher, B.; Best, P.N.; Smail, I.; Matthee, J.; Darvish, B.; Nayyeri, H.; Hemmati, S.; Stott, J.P.

The clustering of H $\beta$ + [O III] and [O II] emitters since z \tilde 5: dependencies with line luminosity and stellar mass Thumbnail


Authors

A.A. Khostovan

D. Sobral

B. Mobasher

P.N. Best

Profile image of Ian Smail

Ian Smail ian.smail@durham.ac.uk
Emeritus Professor

J. Matthee

B. Darvish

H. Nayyeri

S. Hemmati

J.P. Stott



Abstract

We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.

Citation

Khostovan, A., Sobral, D., Mobasher, B., Best, P., Smail, I., Matthee, J., …Stott, J. (2018). The clustering of H $\beta$ + [O III] and [O II] emitters since z \tilde 5: dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society, 478(3), 2999-3015. https://doi.org/10.1093/mnras/sty925

Journal Article Type Article
Acceptance Date Mar 31, 2018
Online Publication Date Apr 14, 2018
Publication Date Apr 14, 2018
Deposit Date Jun 28, 2018
Publicly Available Date Jun 29, 2018
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 478
Issue 3
Pages 2999-3015
DOI https://doi.org/10.1093/mnras/sty925
Public URL https://durham-repository.worktribe.com/output/1323074
Publisher URL http://adsabs.harvard.edu/abs/2018MNRAS.478.2999K

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Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Authors.
Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.






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