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  • 1705.01101v1

    Rights statement: This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version A A Khostovan, D Sobral, B Mobasher, P N Best, I Smail, J Matthee, B Darvish, H Nayyeri, S Hemmati, J P Stott; The clustering of H β + [O III] and [O II] emitters since z ∼ 5: dependencies with line luminosity and stellar mass, Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 3, 21 August 2018, Pages 2999–3015, https://doi.org/10.1093/mnras/sty925 is available online at: https://academic.oup.com/mnras/article/478/3/2999/4970781

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The clustering of H β + [O III] and [O II] emitters since z ∼ 5: dependencies with line luminosity and stellar mass

Research output: Contribution to journalJournal article

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  • Ali Ahmad Khostovan
  • David Sobral
  • Bahram Mobasher
  • Philip N. Best
  • Ian Smail
  • Jorryt Matthee
  • Behnam Darvish
  • Hooshang Nayyeri
  • Shoubaneh Hemmati
  • John P. Stott
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<mark>Journal publication date</mark>21/08/2018
<mark>Journal</mark>Monthly Notices of the Royal Astronomical Society
Issue number3
Volume478
Number of pages17
Pages (from-to)2999–3015
Publication statusPublished
Original languageEnglish

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 LlineMstar 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.

Bibliographic note

This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version A A Khostovan, D Sobral, B Mobasher, P N Best, I Smail, J Matthee, B Darvish, H Nayyeri, S Hemmati, J P Stott; The clustering of H β + [O III] and [O II] emitters since z ∼ 5: dependencies with line luminosity and stellar mass, Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 3, 21 August 2018, Pages 2999–3015, https://doi.org/10.1093/mnras/sty925 is available online at: https://academic.oup.com/mnras/article/478/3/2999/4970781