{"scopus_import":"1","quality_controlled":"1","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"oa_version":"Published Version","language":[{"iso":"eng"}],"intvolume":"       638","day":"03","publisher":"EDP Sciences","article_type":"original","year":"2020","date_published":"2020-06-03T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"_id":"11503","author":[{"first_name":"Haruka","full_name":"Kusakabe, Haruka","last_name":"Kusakabe"},{"first_name":"Jérémy","full_name":"Blaizot, Jérémy","last_name":"Blaizot"},{"first_name":"Thibault","full_name":"Garel, Thibault","last_name":"Garel"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"last_name":"Inami","full_name":"Inami, Hanae","first_name":"Hanae"},{"full_name":"Conseil, Simon","first_name":"Simon","last_name":"Conseil"},{"last_name":"Guiderdoni","full_name":"Guiderdoni, Bruno","first_name":"Bruno"},{"first_name":"Alyssa B.","full_name":"Drake, Alyssa B.","last_name":"Drake"},{"first_name":"Edmund","full_name":"Christian Herenz, Edmund","last_name":"Christian Herenz"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Anna Marino","first_name":"Raffaella","full_name":"Anna Marino, Raffaella"},{"last_name":"Borello Schmidt","full_name":"Borello Schmidt, Kasper","first_name":"Kasper"},{"first_name":"Roser","full_name":"Pelló, Roser","last_name":"Pelló"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"first_name":"Josephine","full_name":"Kerutt, Josephine","last_name":"Kerutt"},{"last_name":"Mahler","full_name":"Mahler, Guillaume","first_name":"Guillaume"}],"doi":"10.1051/0004-6361/201937340","article_number":"A12","abstract":[{"text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time.","lang":"eng"}],"publication":"Astronomy & Astrophysics","publication_status":"published","extern":"1","type":"journal_article","date_updated":"2022-07-19T09:35:20Z","volume":638,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"external_id":{"arxiv":["2003.12083"]},"status":"public","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima, Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy (http://www.astropy.org), which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE. This work was supported by the project FOGHAR (Agence Nationale de la Recherche, ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid for Scientic Research 19J01620.","article_processing_charge":"No","month":"06","date_created":"2022-07-06T09:50:48Z","citation":{"chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>.","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy &#38; Astrophysics. 638, A12.","apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>","short":"H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T. Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz, J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló, M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy &#38; Astrophysics 638 (2020).","ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. <i>Astronomy &#38; Astrophysics</i>. 2020;638. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>","mla":"Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” <i>Astronomy &#38; Astrophysics</i>, vol. 638, A12, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>.","ieee":"H. Kusakabe <i>et al.</i>, “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” <i>Astronomy &#38; Astrophysics</i>, vol. 638. EDP Sciences, 2020."}}