{"author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"full_name":"Sobral, D","first_name":"D","last_name":"Sobral"},{"first_name":"B","last_name":"Mobasher","full_name":"Mobasher, B"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Cochrane, R K","first_name":"R K","last_name":"Cochrane"},{"last_name":"Chartab","first_name":"N","full_name":"Chartab, N"},{"last_name":"Jafariyazani","first_name":"M","full_name":"Jafariyazani, M"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"}],"publication":"Monthly Notices of the Royal Astronomical Society","page":"555-573","doi":"10.1093/mnras/stz2149","external_id":{"arxiv":["1811.00556"]},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","citation":{"ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>.","ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019."},"_id":"11535","language":[{"iso":"eng"}],"intvolume":"       489","volume":489,"year":"2019","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","type":"journal_article","day":"01","month":"10","article_processing_charge":"No","date_updated":"2022-08-19T06:38:42Z","date_published":"2019-10-01T00:00:00Z","extern":"1","publication_status":"published","issue":"1","main_file_link":[{"url":"https://arxiv.org/abs/1811.00556","open_access":"1"}],"abstract":[{"text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe.","lang":"eng"}],"oa_version":"Preprint","oa":1,"date_created":"2022-07-07T13:01:03Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","scopus_import":"1","title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","quality_controlled":"1","status":"public"}