A.A. Khostovan
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.
Authors
D. Sobral
B. Mobasher
P.N. Best
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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