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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

Khostovan, A. A. and Sobral, D. and Mobasher, B. and Best, P. N. and Smail, I. and Matthee, J. and Darvish, B. and Nayyeri, H. and Hemmati, S. and Stott, J. P. (2018) 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, 478 (3). pp. 2999-3015. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20180829-133152204

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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, r_0, of 1.5–4.0 h^(−1) Mpc and minimum dark matter halo masses of 10^(10.7–12.1) M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r_0 ∼ 2.0–8.3 h^(−1) Mpc and halo masses of 10^(11.5–12.6) M⊙ for our z = 1.5–4.7 [O II] emitters. We find r_0 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 r_0, 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 10^(9.5) M⊙ haloes and the brightest emitters in 10^(13.0) M⊙ haloes. For [O II] emitters, the faintest emitters are found in 10^(10.5) M⊙ haloes and the brightest emitters in 10^(12.6) M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 10^(11) to 10^(12.5) M⊙ for stellar masses of 10^(8.5) to 10^(11.5) M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a L_(line)−M_(star) 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 10^(12.5–13) M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty925DOIArticle
https://arxiv.org/abs/1705.01101arXivDiscussion Paper
ORCID:
AuthorORCID
Sobral, D.0000-0001-8823-4845
Smail, I.0000-0003-3037-257X
Matthee, J.0000-0003-2871-127X
Darvish, B.0000-0003-4919-9017
Nayyeri, H.0000-0001-8242-9983
Hemmati, S.0000-0003-2226-5395
Stott, J. P.0000-0002-1679-9983
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices). Accepted 2018 March 31. Received 2017 May 2; in original form 2018 February 26. Published: 14 April 2018. We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA Earth and Space Science FellowshipNNX16AO92H
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Lancaster UniversityA100679
Science and Technology Facilities Council (STFC)STM001229/1
Science and Technology Facilities Council (STFC)ST/L00075X/1
European Research Council (ERC)321334
Royal SocietyUNSPECIFIED
Leiden UniversityUNSPECIFIED
NASANNX12AE20G
Subject Keywords:galaxies: evolution – galaxies: haloes – galaxies: high-redshift – galaxies: star formation – cosmology: observations – large-scale structure of Universe
Issue or Number:3
Record Number:CaltechAUTHORS:20180829-133152204
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180829-133152204
Official Citation: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
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89282
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:29 Aug 2018 20:48
Last Modified:03 Oct 2019 20:14

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