[{"quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","intvolume":"       496","publisher":"Oxford University Press","extern":"1","month":"08","date_created":"2022-07-07T10:20:11Z","page":"1013-1022","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: haloes","galaxies: high-redshift","quasars: absorption lines"],"doi":"10.1093/mnras/staa1347","acknowledgement":"We thank the anonymous referee for useful suggestions. This study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme(s): 094.A-0131(B), 095.A 0200(A), 096.A0222(A), 097.A-0089(A), and 099.A-0159(A). SM acknowledges support from the Alexander von Humboldt Foundation, Germany. SM thanks Christian Herenz for useful discussion. SC gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. JB acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. NB and JZ acknowledge support from ANR grant ANR-17-CE31- 0017 (3DGasFlows). AC and JR acknowledge support from the ERC starting grant 336736-CALENDS. MA acknowledges support from European Union’s H2020 Marie Skłodowska-Curie Actions grant 721463 to the SUNDIAL ITN, and from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2016-76219-P. MA also acknowledges support from the Fundacion BBVA under its 2017 programme of assistance to ´scientific research groups, for the project ‘Using machine-learning techniques to drag galaxies from the noise in deep imaging’. FL and AV acknowledge support from the ERC starting grant ERC757258-TRIPLE.","related_material":{"link":[{"url":"https://doi.org/10.1093/mnras/staa2668","relation":"erratum"}]},"day":"01","type":"journal_article","author":[{"full_name":"Muzahid, Sowgat","first_name":"Sowgat","last_name":"Muzahid"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Marino","full_name":"Marino, Raffaella Anna","first_name":"Raffaella Anna"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"last_name":"Contini","first_name":"Thierry","full_name":"Contini, Thierry"},{"first_name":"Martin","full_name":"Wendt, Martin","last_name":"Wendt"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"last_name":"Zabl","first_name":"Johannes","full_name":"Zabl, Johannes"},{"last_name":"Bouché","full_name":"Bouché, Nicolas","first_name":"Nicolas"},{"full_name":"Akhlaghi, Mohammad","first_name":"Mohammad","last_name":"Akhlaghi"},{"last_name":"Chen","first_name":"Hsiao-Wen","full_name":"Chen, Hsiao-Wen"},{"first_name":"Adélaîde","full_name":"Claeyssens, Adélaîde","last_name":"Claeyssens"},{"first_name":"Sean","full_name":"Johnson, Sean","last_name":"Johnson"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"}],"citation":{"apa":"Muzahid, S., Schaye, J., Marino, R. A., Cantalupo, S., Brinchmann, J., Contini, T., … Verhamme, A. (2020). MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa1347\">https://doi.org/10.1093/mnras/staa1347</a>","ama":"Muzahid S, Schaye J, Marino RA, et al. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;496(2):1013-1022. doi:<a href=\"https://doi.org/10.1093/mnras/staa1347\">10.1093/mnras/staa1347</a>","short":"S. Muzahid, J. Schaye, R.A. Marino, S. Cantalupo, J. Brinchmann, T. Contini, M. Wendt, L. Wisotzki, J. Zabl, N. Bouché, M. Akhlaghi, H.-W. Chen, A. Claeyssens, S. Johnson, F. Leclercq, M. Maseda, J.J. Matthee, J. Richard, T. Urrutia, A. Verhamme, Monthly Notices of the Royal Astronomical Society 496 (2020) 1013–1022.","mla":"Muzahid, Sowgat, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 496, no. 2, Oxford University Press, 2020, pp. 1013–22, doi:<a href=\"https://doi.org/10.1093/mnras/staa1347\">10.1093/mnras/staa1347</a>.","ieee":"S. Muzahid <i>et al.</i>, “MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 496, no. 2. Oxford University Press, pp. 1013–1022, 2020.","ista":"Muzahid S, Schaye J, Marino RA, Cantalupo S, Brinchmann J, Contini T, Wendt M, Wisotzki L, Zabl J, Bouché N, Akhlaghi M, Chen H-W, Claeyssens A, Johnson S, Leclercq F, Maseda M, Matthee JJ, Richard J, Urrutia T, Verhamme A. 2020. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 496(2), 1013–1022.","chicago":"Muzahid, Sowgat, Joop Schaye, Raffaella Anna Marino, Sebastiano Cantalupo, Jarle Brinchmann, Thierry Contini, Martin Wendt, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa1347\">https://doi.org/10.1093/mnras/staa1347</a>."},"title":"MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles","volume":496,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.03593"}],"oa":1,"abstract":[{"text":"Ly α emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons. Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters (LAEs) with a median Ly α flux (luminosity) of ≈10−17 erg cm−2 s−1 (⁠≈1042 erg s−1⁠) and a median star formation rate (SFR) of ≈1.3 M⊙ yr−1 (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by eight background quasars, must be centred on the systemic redshift, we measure an average velocity offset, Voffset = 171\\pm 8 km s−1, between the Ly α emission peak and the systemic redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the Voffset is correlated with the full width at half-maximum of the red peak of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover, we find that Voffset is correlated with SFR with a sub-linear scaling relation, Voffset∝SFR0.16±0.03⁠. Adopting the mass scaling for main-sequence galaxies, such a relation suggests that Voffset scales with the circular velocity of the dark matter haloes hosting the LAEs.","lang":"eng"}],"_id":"11528","date_published":"2020-08-01T00:00:00Z","arxiv":1,"issue":"2","article_processing_charge":"No","date_updated":"2022-08-18T11:00:24Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1910.03593"]},"scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","year":"2020","oa_version":"Preprint"},{"publisher":"Oxford University Press","intvolume":"       489","status":"public","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"555-573","date_created":"2022-07-07T13:01:03Z","extern":"1","month":"10","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).","doi":"10.1093/mnras/stz2149","language":[{"iso":"eng"}],"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"],"title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","citation":{"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>.","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.","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.","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>","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."},"author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"last_name":"Mobasher","full_name":"Mobasher, B","first_name":"B"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"R K","full_name":"Cochrane, R K","last_name":"Cochrane"},{"first_name":"N","full_name":"Chartab, N","last_name":"Chartab"},{"full_name":"Jafariyazani, M","first_name":"M","last_name":"Jafariyazani"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"full_name":"Santos, S","first_name":"S","last_name":"Santos"},{"first_name":"J","full_name":"Calhau, J","last_name":"Calhau"}],"type":"journal_article","day":"01","main_file_link":[{"url":"https://arxiv.org/abs/1811.00556","open_access":"1"}],"oa":1,"publication_status":"published","volume":489,"issue":"1","article_processing_charge":"No","arxiv":1,"abstract":[{"lang":"eng","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."}],"_id":"11535","date_published":"2019-10-01T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T06:38:42Z","external_id":{"arxiv":["1811.00556"]},"scopus_import":"1","year":"2019","oa_version":"Preprint","article_type":"original"},{"_id":"11549","date_published":"2018-08-01T00:00:00Z","abstract":[{"text":"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.","lang":"eng"}],"article_processing_charge":"No","issue":"3","arxiv":1,"volume":478,"main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"publication_status":"published","year":"2018","oa_version":"Published Version","article_type":"original","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","external_id":{"arxiv":["1705.01101"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T06:53:39Z","date_created":"2022-07-08T11:48:48Z","month":"08","extern":"1","page":"2999-3015","intvolume":"       478","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press","type":"journal_article","author":[{"last_name":"Khostovan","full_name":"Khostovan, A A","first_name":"A A"},{"full_name":"Sobral, D","first_name":"D","last_name":"Sobral"},{"last_name":"Mobasher","full_name":"Mobasher, B","first_name":"B"},{"full_name":"Best, P N","first_name":"P N","last_name":"Best"},{"last_name":"Smail","full_name":"Smail, I","first_name":"I"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Darvish","full_name":"Darvish, B","first_name":"B"},{"last_name":"Nayyeri","full_name":"Nayyeri, H","first_name":"H"},{"first_name":"S","full_name":"Hemmati, S","last_name":"Hemmati"},{"full_name":"Stott, J P","first_name":"J P","last_name":"Stott"}],"day":"01","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","citation":{"mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>.","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 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), 2999–3015.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … 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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015. doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015."},"doi":"10.1093/mnras/sty925","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"],"language":[{"iso":"eng"}],"acknowledgement":"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."},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T07:18:20Z","scopus_import":"1","external_id":{"arxiv":["1609.05897"]},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"article_type":"original","year":"2017","oa_version":"Preprint","volume":466,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1609.05897"}],"oa":1,"_id":"11562","abstract":[{"text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii.","lang":"eng"}],"date_published":"2017-04-01T00:00:00Z","arxiv":1,"issue":"1","article_processing_charge":"No","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"doi":"10.1093/mnras/stw3090","acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","day":"01","type":"journal_article","author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Best, Philip","first_name":"Philip","last_name":"Best"},{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"first_name":"Iván","full_name":"Oteo, Iván","last_name":"Oteo"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"last_name":"Morabito","full_name":"Morabito, Leah","first_name":"Leah"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"}],"citation":{"short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258.","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>."},"title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","intvolume":"       466","publisher":"Oxford University Press","extern":"1","month":"04","date_created":"2022-07-12T12:04:16Z","page":"1242-1258"},{"volume":465,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1608.08218"}],"oa":1,"_id":"11565","abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"date_published":"2017-02-01T00:00:00Z","arxiv":1,"article_processing_charge":"No","issue":"2","scopus_import":"1","external_id":{"arxiv":["1608.08218"]},"date_updated":"2022-08-19T07:56:07Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"article_type":"original","oa_version":"Preprint","year":"2017","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","intvolume":"       465","status":"public","publisher":"Oxford University Press","month":"02","extern":"1","date_created":"2022-07-12T12:25:08Z","page":"2381-2396","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stw2884","acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","day":"01","type":"journal_article","author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"last_name":"Crain","full_name":"Crain, Robert A.","first_name":"Robert A."},{"last_name":"Schaller","full_name":"Schaller, Matthieu","first_name":"Matthieu"},{"first_name":"Richard","full_name":"Bower, Richard","last_name":"Bower"},{"last_name":"Theuns","first_name":"Tom","full_name":"Theuns, Tom"}],"citation":{"chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>","apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>"},"title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation"}]