[{"intvolume":" 527","status":"public","day":"01","type":"journal_article","issue":"4","publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2024-01-23T12:30:45Z","page":"9853-9871","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"02","article_type":"original","date_published":"2024-02-01T00:00:00Z","date_created":"2024-01-22T08:22:17Z","file":[{"date_created":"2024-01-23T12:30:45Z","checksum":"9d02df4035c4951cf63dee0db1e462e9","file_name":"2024_MNAstronomSoc_Kramarenko.pdf","file_size":4521738,"date_updated":"2024-01-23T12:30:45Z","access_level":"open_access","success":1,"creator":"dernst","file_id":"14879","content_type":"application/pdf","relation":"main_file"}],"has_accepted_license":"1","department":[{"_id":"GradSch"},{"_id":"JoMa"}],"abstract":[{"lang":"eng","text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &lt; z &lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"last_name":"Kerutt","full_name":"Kerutt, J","first_name":"J"},{"first_name":"A","full_name":"Verhamme, A","last_name":"Verhamme"},{"first_name":"P A","full_name":"Oesch, P A","last_name":"Oesch"},{"first_name":"L","last_name":"Barrufet","full_name":"Barrufet, L"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"H","full_name":"Kusakabe, H","last_name":"Kusakabe"},{"first_name":"I","full_name":"Goovaerts, I","last_name":"Goovaerts"},{"first_name":"T T","last_name":"Thai","full_name":"Thai, T T"}],"publication_status":"published","citation":{"ieee":"I. Kramarenko et al., “Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape,” Monthly Notices of the Royal Astronomical Society, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stad3853","chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at z ≳ 3 to Lyman Continuum Escape.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2024. https://doi.org/10.1093/mnras/stad3853.","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 2024;527(4):9853-9871. doi:10.1093/mnras/stad3853","mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at z ≳ 3 to Lyman Continuum Escape.” Monthly Notices of the Royal Astronomical Society, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:10.1093/mnras/stad3853.","short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871.","ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871."},"_id":"14852","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","oa_version":"Published Version","quality_controlled":"1","arxiv":1,"volume":527,"date_updated":"2024-01-23T12:33:50Z","oa":1,"article_processing_charge":"Yes (in subscription journal)","title":"Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape","external_id":{"arxiv":["2305.07044"]},"year":"2024","doi":"10.1093/mnras/stad3853","ddc":["520"],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)"}},{"status":"public","intvolume":" 660","type":"journal_article","day":"07","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"publisher":"EDP Sciences","scopus_import":"1","date_published":"2022-04-07T00:00:00Z","article_type":"original","month":"04","date_created":"2022-07-05T14:27:26Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"author":[{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"last_name":"Blaizot","full_name":"Blaizot, Jérémy","first_name":"Jérémy"},{"last_name":"Garel","full_name":"Garel, Thibault","first_name":"Thibault"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Sofia G.","full_name":"Gallego, Sofia G.","last_name":"Gallego"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"first_name":"Roser","last_name":"Pelló","full_name":"Pelló, Roser"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"last_name":"Tresse","full_name":"Tresse, Laurence","first_name":"Laurence"},{"first_name":"Tanya","last_name":"Urrutia","full_name":"Urrutia, Tanya"},{"first_name":"Eloïse","last_name":"Vitte","full_name":"Vitte, Eloïse"}],"abstract":[{"text":"Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic medium (CGM) at high redshifts. In this work, we aim to explore the existence of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters (LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5, and spectroscopic redshifts were assigned or constrained for all the sources thanks to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes 21 galaxies that are purely F775W-magnitude selected within the redshift range z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs and four non-LAHs. We report the first individual detections of extended Lyα emission around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected galaxies generally have a large amount of hydrogen in their CGM. We derived the mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz, is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7. Assuming that Lyα emission and absorption arise in the same gas, this suggests, based on abundance matching, that LAHs trace the same gas as damped Lyα systems (DLAs) and sub-DLAs.","lang":"eng"}],"publication_status":"published","citation":{"ieee":"H. Kusakabe et al., “The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4,” Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.","apa":"Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq, F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142302","chicago":"Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field: Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142302.","mla":"Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.” Astronomy & Astrophysics, vol. 660, A44, EDP Sciences, 2022, doi:10.1051/0004-6361/202142302.","ama":"Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142302","ista":"Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. 660, A44.","short":"H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq, R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara, R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy & Astrophysics 660 (2022)."},"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard, Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges support from Swiss Government Excellence Scholarships and Japan Society for the Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC Starting Grant 757258“TRIPLE”. This work was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy, which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), and other software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Published Version","_id":"11488","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","volume":660,"oa":1,"date_updated":"2022-07-19T09:33:24Z","article_processing_charge":"No","arxiv":1,"external_id":{"arxiv":["2201.07257"]},"title":"The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4","doi":"10.1051/0004-6361/202142302","year":"2022","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2201.07257"}],"article_number":"A44"},{"status":"public","intvolume":" 660","type":"journal_article","day":"30","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"EDP Sciences","date_published":"2022-03-30T00:00:00Z","article_type":"original","month":"03","date_created":"2022-07-05T15:25:35Z","author":[{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Anna","full_name":"Feltre, Anna","last_name":"Feltre"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"last_name":"Verhamme","full_name":"Verhamme, Anne","first_name":"Anne"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / techniques: spectroscopic / galaxies: stellar content / galaxies: formation"],"abstract":[{"lang":"eng","text":"Directly characterising the first generations of stars in distant galaxies is a key quest of observational cosmology. We present a case study of ID53 at z = 4.77, the UV-brightest (but L⋆) star-forming galaxy at z > 3 in the MUSE eXtremely Deep Field with a mass of ≈109 M⊙. In addition to very strong Lyman-α (Lyα) emission, we clearly detect the (stellar) continuum and an N V P Cygni feature, interstellar absorption, fine-structure emission and nebular C IV emission lines in the 140 h spectrum. Continuum emission from two spatially resolved components in Hubble Space Telescope data are blended in the MUSE data, but we show that the nebular C IV emission originates from a subcomponent of the galaxy. The UV spectrum can be fit with recent BPASS stellar population models combined with single-burst or continuous star formation histories (SFHs), a standard initial mass function, and an attenuation law. Models with a young age and low metallicity (log10(age/yr) = 6.5–7.6 and [Z/H] = −2.15 to −1.15) are preferred, but the details depend on the assumed SFH. The intrinsic Hα luminosity of the best-fit models is an order of magnitude higher than the Hα luminosity inferred from Spitzer/IRAC data, which either suggests a high escape fraction of ionising photons, a high relative attenuation of nebular to stellar dust, or a complex SFH. The metallicity appears lower than the metallicity in more massive galaxies at z = 3 − 5, consistent with the scenario according to which younger galaxies have lower metallicities. This chemical immaturity likely facilitates Lyα escape, explaining why the Lyα equivalent width is anti-correlated with stellar metallicity. Finally, we stress that uncertainties in SFHs impose a challenge for future inferences of the stellar metallicity of young galaxies. This highlights the need for joint (spatially resolved) analyses of stellar spectra and photo-ionisation models."}],"citation":{"ista":"Matthee JJ, Feltre A, Maseda M, Nanayakkara T, Boogaard L, Bacon R, Verhamme A, Leclercq F, Kusakabe H, Urrutia T, Wisotzki L. 2022. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy & Astrophysics. 660, A10.","short":"J.J. Matthee, A. Feltre, M. Maseda, T. Nanayakkara, L. Boogaard, R. Bacon, A. Verhamme, F. Leclercq, H. Kusakabe, T. Urrutia, L. Wisotzki, Astronomy & Astrophysics 660 (2022).","ama":"Matthee JJ, Feltre A, Maseda M, et al. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142187","mla":"Matthee, Jorryt J., et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” Astronomy & Astrophysics, vol. 660, A10, EDP Sciences, 2022, doi:10.1051/0004-6361/202142187.","chicago":"Matthee, Jorryt J, Anna Feltre, Michael Maseda, Themiya Nanayakkara, Leindert Boogaard, Roland Bacon, Anne Verhamme, et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142187.","apa":"Matthee, J. J., Feltre, A., Maseda, M., Nanayakkara, T., Boogaard, L., Bacon, R., … Wisotzki, L. (2022). Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142187","ieee":"J. J. Matthee et al., “Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field,” Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022."},"publication_status":"published","quality_controlled":"1","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the referee for thoughtful and constructive comments that have improved the quality of this manuscript. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060.","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","_id":"11490","article_processing_charge":"No","volume":660,"oa":1,"date_updated":"2022-07-19T09:33:46Z","arxiv":1,"title":"Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field","external_id":{"arxiv":["2111.14855"]},"doi":"10.1051/0004-6361/202142187","year":"2022","main_file_link":[{"url":"https://arxiv.org/abs/2111.14855","open_access":"1"}],"article_number":"A10"},{"publication":"Astronomy & Astrophysics","intvolume":" 659","status":"public","day":"25","type":"journal_article","date_created":"2022-07-06T08:17:27Z","publisher":"EDP Sciences","scopus_import":"1","language":[{"iso":"eng"}],"month":"03","article_type":"original","date_published":"2022-03-25T00:00:00Z","_id":"11497","extern":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the referee for thoughtful and constructive comments that have improved the quality of this manuscript. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060.","quality_controlled":"1","oa_version":"Published Version","arxiv":1,"oa":1,"volume":659,"date_updated":"2022-07-19T09:47:16Z","article_processing_charge":"No","abstract":[{"text":"Context. The hydrogen Lyman α line is often the only measurable feature in optical spectra of high-redshift galaxies. Its shape and strength are influenced by radiative transfer processes and the properties of the underlying stellar population. High equivalent widths of several hundred Å are especially hard to explain by models and could point towards unusual stellar populations, for example with low metallicities, young stellar ages, and a top-heavy initial mass function. Other aspects influencing equivalent widths are the morphology of the galaxy and its gas properties.\r\nAims. The aim of this study is to better understand the connection between the Lyman α rest-frame equivalent width (EW0) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths.\r\nMethods. We used integral field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the Galfit software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults. The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16% for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW0. The object with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman α spectral or UV continuum morphological properties.\r\nConclusions. The survey depth has to be taken into account when studying EW0 distributions. We find that in general, high EW0 objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW0 values are equally varied.","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"author":[{"first_name":"J.","last_name":"Kerutt","full_name":"Kerutt, J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"first_name":"A.","last_name":"Verhamme","full_name":"Verhamme, A."},{"last_name":"Schmidt","full_name":"Schmidt, K. B.","first_name":"K. B."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"first_name":"E. C.","last_name":"Herenz","full_name":"Herenz, E. C."},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"last_name":"Garel","full_name":"Garel, T.","first_name":"T."},{"first_name":"T.","full_name":"Hashimoto, T.","last_name":"Hashimoto"},{"first_name":"M.","last_name":"Maseda","full_name":"Maseda, M."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Kusakabe","full_name":"Kusakabe, H.","first_name":"H."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"full_name":"Guiderdoni, B.","last_name":"Guiderdoni","first_name":"B."},{"last_name":"Mauerhofer","full_name":"Mauerhofer, V.","first_name":"V."},{"first_name":"T.","full_name":"Nanayakkara, T.","last_name":"Nanayakkara"},{"last_name":"Vitte","full_name":"Vitte, E.","first_name":"E."}],"publication_status":"published","citation":{"ama":"Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 2022;659. doi:10.1051/0004-6361/202141900","mla":"Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” Astronomy & Astrophysics, vol. 659, 183, EDP Sciences, 2022, doi:10.1051/0004-6361/202141900.","short":"J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz, T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye, J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy & Astrophysics 659 (2022).","ista":"Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J, Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 659, 183.","ieee":"J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.","apa":"Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz, E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202141900","chicago":"Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C. Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141900."},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2202.06642"}],"article_number":"183","external_id":{"arxiv":["2202.06642"]},"title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","doi":"10.1051/0004-6361/202141900","year":"2022"},{"publication":"The Astrophysical Journal","issue":"2","day":"31","type":"journal_article","intvolume":" 925","status":"public","date_created":"2022-07-06T12:01:48Z","month":"01","date_published":"2022-01-31T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"IOP Publishing","language":[{"iso":"eng"}],"arxiv":1,"article_processing_charge":"No","volume":925,"oa":1,"date_updated":"2022-07-21T05:51:25Z","extern":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"_id":"11509","oa_version":"Published Version","quality_controlled":"1","acknowledgement":"We thank the referee for the valuable comments. We are also grateful to Koh Takahashi, Nozomu Tominaga, Chiaki Kobayashi, Yutaka Hirai, and Daichi Kashino for having useful discussions. This paper includes data gathered with the 10 m Keck Telescope located at W. M. Keck Observatory, Hawaii. We thank the staff of Keck Observatory for their help with the observations. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Based on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at NAOJ. This work was supported by the joint research program of the Institute for Cosmic Ray Research (ICRR), University of Tokyo. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. S.F. acknowledges support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). This project has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.” This work is supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, as well as the KAKENHI Grant-in-Aid for Scientific Research (A; 15H02064, 17H01110, 17H01114, 20H00180, and 21H04467) through the Japan Society for the Promotion of Science (JSPS). This work has been supported in part by JSPS KAKENHI grant Nos. JP17K05382, JP20K04024, and JP21H04499 (K.N.). Yuki Isobe, Kimihiko Nakajima, Yuichi Harikane, Takashi Kojima, and Masato Onodera are supported by JSPS KAKENHI grant Nos. 21J20785, 20K22373,19J01222, 18J12840, and 17K14257, respectively.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"chicago":"Isobe, Yuki, Masami Ouchi, Akihiro Suzuki, Takashi J. Moriya, Kimihiko Nakajima, Ken’ichi Nomoto, Michael Rauch, et al. “EMPRESS. IV. Extremely Metal-Poor Galaxies Including Very Low-Mass Primordial Systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability Supernovae.” The Astrophysical Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac3509.","ieee":"Y. Isobe et al., “EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae,” The Astrophysical Journal, vol. 925, no. 2. IOP Publishing, 2022.","apa":"Isobe, Y., Ouchi, M., Suzuki, A., Moriya, T. J., Nakajima, K., Nomoto, K., … Xu, Y. (2022). EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac3509","short":"Y. Isobe, M. Ouchi, A. Suzuki, T.J. Moriya, K. Nakajima, K. Nomoto, M. Rauch, Y. Harikane, T. Kojima, Y. Ono, S. Fujimoto, A.K. Inoue, J.H. Kim, Y. Komiyama, H. Kusakabe, C.-H. Lee, M. Maseda, J.J. Matthee, L. Michel-Dansac, T. Nagao, T. Nanayakkara, M. Nishigaki, M. Onodera, Y. Sugahara, Y. Xu, The Astrophysical Journal 925 (2022).","ista":"Isobe Y, Ouchi M, Suzuki A, Moriya TJ, Nakajima K, Nomoto K, Rauch M, Harikane Y, Kojima T, Ono Y, Fujimoto S, Inoue AK, Kim JH, Komiyama Y, Kusakabe H, Lee C-H, Maseda M, Matthee JJ, Michel-Dansac L, Nagao T, Nanayakkara T, Nishigaki M, Onodera M, Sugahara Y, Xu Y. 2022. EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. The Astrophysical Journal. 925(2), 111.","mla":"Isobe, Yuki, et al. “EMPRESS. IV. Extremely Metal-Poor Galaxies Including Very Low-Mass Primordial Systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability Supernovae.” The Astrophysical Journal, vol. 925, no. 2, 111, IOP Publishing, 2022, doi:10.3847/1538-4357/ac3509.","ama":"Isobe Y, Ouchi M, Suzuki A, et al. EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 104-105⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae. The Astrophysical Journal. 2022;925(2). doi:10.3847/1538-4357/ac3509"},"publication_status":"published","abstract":[{"lang":"eng","text":"We present Keck/LRIS follow-up spectroscopy for 13 photometric candidates of extremely metal-poor galaxies (EMPGs) selected by a machine-learning technique applied to the deep (∼26 AB mag) optical and wide-area (∼500 deg2) Subaru imaging data in the EMPRESS survey. Nine out of the 13 candidates are EMPGs with an oxygen abundance (O/H) less than ∼10% solar value (O/H)⊙, and four sources are contaminants of moderately metal-rich galaxies or no emission-line objects. Notably, two out of the nine EMPGs have extremely low stellar masses and oxygen abundances of 5 × 10⁴x–7 × -10⁵ M⊙ and 2%–3% (O/H)⊙, respectively. With a sample of five EMPGs with (Fe/O) measurements, two (three) of which are taken from this study (the literature), we confirm that two EMPGs with the lowest (O/H) ratios of ∼2% (O/H)⊙ show high (Fe/O) ratios of ∼0.1, close to the solar abundance ratio. Comparing galaxy chemical enrichment models, we find that the two EMPGs cannot be explained by a scenario of metal-poor gas accretion/episodic star formation history due to their low (N/O) ratios. We conclude that the two EMPGs can be reproduced by the inclusion of bright hypernovae and/or hypothetical pair-instability supernovae (SNe) preferentially produced in a metal-poor environment. This conclusion implies that primordial galaxies at z ∼ 10 could have a high abundance of Fe that did not originate from Type Ia SNe with delays and that Fe may not serve as a cosmic clock for primordial galaxies."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"last_name":"Isobe","full_name":"Isobe, Yuki","first_name":"Yuki"},{"last_name":"Ouchi","full_name":"Ouchi, Masami","first_name":"Masami"},{"first_name":"Akihiro","full_name":"Suzuki, Akihiro","last_name":"Suzuki"},{"full_name":"Moriya, Takashi J.","last_name":"Moriya","first_name":"Takashi J."},{"last_name":"Nakajima","full_name":"Nakajima, Kimihiko","first_name":"Kimihiko"},{"last_name":"Nomoto","full_name":"Nomoto, Ken’ichi","first_name":"Ken’ichi"},{"first_name":"Michael","last_name":"Rauch","full_name":"Rauch, Michael"},{"last_name":"Harikane","full_name":"Harikane, Yuichi","first_name":"Yuichi"},{"first_name":"Takashi","full_name":"Kojima, Takashi","last_name":"Kojima"},{"full_name":"Ono, Yoshiaki","last_name":"Ono","first_name":"Yoshiaki"},{"first_name":"Seiji","full_name":"Fujimoto, Seiji","last_name":"Fujimoto"},{"first_name":"Akio K.","last_name":"Inoue","full_name":"Inoue, Akio K."},{"first_name":"Ji Hoon","full_name":"Kim, Ji Hoon","last_name":"Kim"},{"first_name":"Yutaka","full_name":"Komiyama, Yutaka","last_name":"Komiyama"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"first_name":"Chien-Hsiu","last_name":"Lee","full_name":"Lee, Chien-Hsiu"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Leo","full_name":"Michel-Dansac, Leo","last_name":"Michel-Dansac"},{"first_name":"Tohru","full_name":"Nagao, Tohru","last_name":"Nagao"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"},{"last_name":"Nishigaki","full_name":"Nishigaki, Moka","first_name":"Moka"},{"first_name":"Masato","last_name":"Onodera","full_name":"Onodera, Masato"},{"first_name":"Yuma","full_name":"Sugahara, Yuma","last_name":"Sugahara"},{"last_name":"Xu","full_name":"Xu, Yi","first_name":"Yi"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.03850"}],"article_number":"111","year":"2022","doi":"10.3847/1538-4357/ac3509","external_id":{"arxiv":["2108.03850"]},"title":"EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial systems with M∗= 10⁴-10⁵⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae"},{"article_processing_charge":"No","date_updated":"2022-07-19T09:37:42Z","oa":1,"volume":926,"arxiv":1,"quality_controlled":"1","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the reviewer for several valuable comments that improved the clarity of the manuscript. P.F.W. acknowledges the support of the fellowship by the East Asian Core Observatories Association. This work is based on observations made with ESO VLT Telescopes at the La Silla Paranal Observatory under programmes ID 194-A.2005 and 1100.A-0949 (The LEGA-C Public Spectroscopy Survey). This project has received funding from the European Research Council (ERC) under the European Union—Horizon 2020 research and innovation program (grant agreement No. 683184).","extern":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"_id":"11510","citation":{"ama":"Sobral D, van der Wel A, Bezanson R, et al. The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. The Astrophysical Journal. 2022;926(2). doi:10.3847/1538-4357/ac4419","mla":"Sobral, David, et al. “The LEGA-C of Nature and Nurture in Stellar Populations at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly Histories for Quiescent Galaxies in Different Environments.” The Astrophysical Journal, vol. 926, no. 2, 117, IOP Publishing, 2022, doi:10.3847/1538-4357/ac4419.","ista":"Sobral D, van der Wel A, Bezanson R, Bell E, Muzzin A, D’Eugenio F, Darvish B, Gallazzi A, Wu P-F, Maseda M, Matthee JJ, Paulino-Afonso A, Straatman C, van Dokkum PG. 2022. The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. The Astrophysical Journal. 926(2), 117.","short":"D. Sobral, A. van der Wel, R. Bezanson, E. Bell, A. Muzzin, F. D’Eugenio, B. Darvish, A. Gallazzi, P.-F. Wu, M. Maseda, J.J. Matthee, A. Paulino-Afonso, C. Straatman, P.G. van Dokkum, The Astrophysical Journal 926 (2022).","ieee":"D. Sobral et al., “The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments,” The Astrophysical Journal, vol. 926, no. 2. IOP Publishing, 2022.","apa":"Sobral, D., van der Wel, A., Bezanson, R., Bell, E., Muzzin, A., D’Eugenio, F., … van Dokkum, P. G. (2022). The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac4419","chicago":"Sobral, David, Arjen van der Wel, Rachel Bezanson, Eric Bell, Adam Muzzin, Francesco D’Eugenio, Behnam Darvish, et al. “The LEGA-C of Nature and Nurture in Stellar Populations at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly Histories for Quiescent Galaxies in Different Environments.” The Astrophysical Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac4419."},"publication_status":"published","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Arjen","last_name":"van der Wel","full_name":"van der Wel, Arjen"},{"first_name":"Rachel","last_name":"Bezanson","full_name":"Bezanson, Rachel"},{"full_name":"Bell, Eric","last_name":"Bell","first_name":"Eric"},{"full_name":"Muzzin, Adam","last_name":"Muzzin","first_name":"Adam"},{"last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco","first_name":"Francesco"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"last_name":"Gallazzi","full_name":"Gallazzi, Anna","first_name":"Anna"},{"first_name":"Po-Feng","last_name":"Wu","full_name":"Wu, Po-Feng"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"last_name":"Straatman","full_name":"Straatman, Caroline","first_name":"Caroline"},{"full_name":"van Dokkum, Pieter G.","last_name":"van Dokkum","first_name":"Pieter G."}],"abstract":[{"text":"Galaxy evolution is driven by a variety of physical processes that are predicted to proceed at different rates for different dark matter haloes and environments across cosmic times. A record of this evolution is preserved in galaxy stellar populations, which we can access using absorption-line spectroscopy. Here we explore the large LEGA-C survey (DR3) to investigate the role of the environment and stellar mass on stellar populations at z ∼ 0.6–1 in the COSMOS field. Leveraging the statistical power and depth of LEGA-C, we reveal significant gradients in Dn4000 and Hδ equivalent widths (EWs) distributions over the stellar mass versus environment 2D spaces for the massive galaxy population (M > 1010 M⊙) at z ∼ 0.6–1.0. Dn4000 and Hδ EWs primarily depend on stellar mass, but they also depend on environment at fixed stellar mass. By splitting the sample into centrals and satellites, and in terms of star-forming galaxies and quiescent galaxies, we reveal that the significant environmental trends of Dn4000 and Hδ EW, when controlling for stellar mass, are driven by quiescent galaxies. Regardless of being centrals or satellites, star-forming galaxies reveal Dn4000 and Hδ EWs, which depend strongly on their stellar mass and are completely independent of the environment at 0.6 < z < 1.0. The environmental trends seen for satellite galaxies are fully driven by the trends that hold only for quiescent galaxies, combined with the strong environmental dependency of the quiescent fraction at fixed stellar mass. Our results are consistent with recent predictions from simulations that point toward massive galaxies forming first in overdensities or the most compact dark matter haloes.","lang":"eng"}],"article_number":"117","main_file_link":[{"url":"https://arxiv.org/abs/2112.08372","open_access":"1"}],"doi":"10.3847/1538-4357/ac4419","year":"2022","external_id":{"arxiv":["2112.08372"]},"title":"The LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies in different environments","publication":"The Astrophysical Journal","issue":"2","type":"journal_article","day":"17","status":"public","intvolume":" 926","date_created":"2022-07-06T12:38:42Z","article_type":"original","date_published":"2022-02-17T00:00:00Z","month":"02","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"IOP Publishing"},{"status":"public","intvolume":" 924","type":"journal_article","day":"13","publication":"The Astrophysical Journal","issue":"2","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"IOP Publishing","date_published":"2022-01-13T00:00:00Z","article_type":"original","month":"01","date_created":"2022-07-06T12:48:32Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"first_name":"Andrea","last_name":"Gebek","full_name":"Gebek, Andrea"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"abstract":[{"text":"The ratio of α-elements to iron in galaxies holds valuable information about the star formation history (SFH) since their enrichment occurs on different timescales. The fossil record of stars in galaxies has mostly been excavated for passive galaxies, since the light of star-forming galaxies is dominated by young stars, which have much weaker atmospheric absorption features. Here we use the largest reference cosmological simulation of the EAGLE project to investigate the origin of variations in stellar α-enhancement among star-forming galaxies at z = 0, and their impact on integrated spectra. The definition of α-enhancement in a composite stellar population is ambiguous. We elucidate two definitions—termed “mean” and “galactic” α-enhancement—in more detail. While a star-forming galaxy has a high “mean” α-enhancement when its stars formed rapidly, a galaxy with a large “galactic” α-enhancement generally had a delayed SFH. We find that absorption-line strengths of Mg and Fe correlate with variations in α-enhancement. These correlations are strongest for the “galactic” α-enhancement. However, we show that these are mostly caused by other effects that are cross-correlated with α-enhancement, such as variations in the light-weighted age. This severely complicates the retrieval of α-enhancements in star-forming galaxies. The ambiguity is not severe for passive galaxies, and we confirm that spectral variations in these galaxies are caused by measurable variations in α-enhancements. We suggest that this more complex coupling between α-enhancement and SFHs can guide the interpretation of new observations of star-forming galaxies.","lang":"eng"}],"citation":{"ista":"Gebek A, Matthee JJ. 2022. On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. The Astrophysical Journal. 924(2), 73.","short":"A. Gebek, J.J. Matthee, The Astrophysical Journal 924 (2022).","ama":"Gebek A, Matthee JJ. On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. The Astrophysical Journal. 2022;924(2). doi:10.3847/1538-4357/ac350b","mla":"Gebek, Andrea, and Jorryt J. Matthee. “On the Variation in Stellar α-Enhancements of Star-Forming Galaxies in the EAGLE Simulation.” The Astrophysical Journal, vol. 924, no. 2, 73, IOP Publishing, 2022, doi:10.3847/1538-4357/ac350b.","chicago":"Gebek, Andrea, and Jorryt J Matthee. “On the Variation in Stellar α-Enhancements of Star-Forming Galaxies in the EAGLE Simulation.” The Astrophysical Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac350b.","apa":"Gebek, A., & Matthee, J. J. (2022). On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac350b","ieee":"A. Gebek and J. J. Matthee, “On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation,” The Astrophysical Journal, vol. 924, no. 2. IOP Publishing, 2022."},"publication_status":"published","oa_version":"Published Version","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank our anonymous referee for the constructive feedback. We extend our gratitude to Maarten Baes, Simon Lilly, Rafael Ottersberg, Gabriele Pezzulli, Alvio Renzini, and Andrea Weibel for insightful discussions. A.G. gratefully acknowledges financial support from the Fund for Scientific Research Flanders (FWO-Vlaanderen, project G.0G04.16N). This work used the DiRAC Data Centric system at Durham University, operated by the ICC on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.\r\n\r\nWe have benefited from the data analysis tool Topcat (Taylor 2013) and the programming language Python, including the numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and scipy (Virtanen et al. 2020) packages.","extern":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"_id":"11511","article_processing_charge":"No","volume":924,"oa":1,"date_updated":"2022-07-19T09:38:03Z","arxiv":1,"external_id":{"arxiv":["2102.04561"]},"title":"On the variation in stellar α-enhancements of star-forming galaxies in the EAGLE simulation","doi":"10.3847/1538-4357/ac350b","year":"2022","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.04561"}],"article_number":"73"},{"year":"2022","doi":"10.1093/mnras/stac801","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","external_id":{"arxiv":["2110.11967"]},"main_file_link":[{"url":"https://arxiv.org/abs/2110.11967","open_access":"1"}],"citation":{"mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:10.1093/mnras/stac801.","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 2022;512(4):5960-5977. doi:10.1093/mnras/stac801","ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","ieee":"J. J. Matthee et al., “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stac801","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2022. https://doi.org/10.1093/mnras/stac801."},"publication_status":"published","abstract":[{"lang":"eng","text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (⁠fesc=50 per cent⁠, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism."}],"author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"last_name":"Hayes","full_name":"Hayes, Matthew","first_name":"Matthew"},{"last_name":"Erb","full_name":"Erb, Dawn","first_name":"Dawn"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"last_name":"Amorín","full_name":"Amorín, Ricardo","first_name":"Ricardo"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"first_name":"Ana Paulino-Afonso","last_name":"Ana Paulino-Afonso","full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso"},{"last_name":"Llerena","full_name":"Llerena, Mario","first_name":"Mario"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"}],"keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"arxiv":1,"article_processing_charge":"No","volume":512,"oa":1,"date_updated":"2022-08-18T10:42:47Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"extern":"1","_id":"11521","quality_controlled":"1","oa_version":"Preprint","acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","date_published":"2022-06-01T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"Oxford University Press","language":[{"iso":"eng"}],"date_created":"2022-07-07T09:21:30Z","day":"01","type":"journal_article","intvolume":" 512","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","page":"5960-5977"},{"citation":{"mla":"Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 < z < 6.4.” Astronomy & Astrophysics, vol. 654, A80, EDP Sciences, 2021, doi:10.1051/0004-6361/202140876.","ama":"Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4. Astronomy & Astrophysics. 2021;654. doi:10.1051/0004-6361/202140876","ista":"Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4. Astronomy & Astrophysics. 654, A80.","short":"K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda, T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz, W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer, J. Richard, J. Schaye, Astronomy & Astrophysics 654 (2021).","ieee":"K. B. Schmidt et al., “Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4,” Astronomy & Astrophysics, vol. 654. EDP Sciences, 2021.","apa":"Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda, M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140876","chicago":"Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 < z < 6.4.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140876."},"publication_status":"published","abstract":[{"lang":"eng","text":"Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The strongest main UV emission line, Lyα, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Lyα emission becomes increasingly challenging at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies’ physical properties and their Lyα emission. The sample of 2052 emission line sources with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Lyα) UV emission lines increases with survey depth, and that the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and [Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 + C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III] λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548 + C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range of 250−500 km s−1 which is in agreement with previous results from the literature. The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III] λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization Model Probability Density Functions” to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"author":[{"first_name":"K. B.","full_name":"Schmidt, K. B.","last_name":"Schmidt"},{"first_name":"J.","full_name":"Kerutt, J.","last_name":"Kerutt"},{"full_name":"Wisotzki, L.","last_name":"Wisotzki","first_name":"L."},{"first_name":"T.","full_name":"Urrutia, T.","last_name":"Urrutia"},{"first_name":"A.","last_name":"Feltre","full_name":"Feltre, A."},{"full_name":"Maseda, M. V.","last_name":"Maseda","first_name":"M. V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"first_name":"R.","full_name":"Bacon, R.","last_name":"Bacon"},{"first_name":"L. A.","last_name":"Boogaard","full_name":"Boogaard, L. A."},{"first_name":"S.","full_name":"Conseil, S.","last_name":"Conseil"},{"first_name":"T.","full_name":"Contini, T.","last_name":"Contini"},{"full_name":"Herenz, E. C.","last_name":"Herenz","first_name":"E. C."},{"last_name":"Kollatschny","full_name":"Kollatschny, W.","first_name":"W."},{"first_name":"M.","full_name":"Krumpe, M.","last_name":"Krumpe"},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"first_name":"G.","last_name":"Mahler","full_name":"Mahler, G."},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Mauerhofer","full_name":"Mauerhofer, V.","first_name":"V."},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."}],"arxiv":1,"article_processing_charge":"No","date_updated":"2022-07-19T09:34:36Z","volume":654,"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","_id":"11498","oa_version":"Published Version","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We would like to thank Charlotte Mason for useful discussions and for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing the observational data for the comparison sample studied by Steidel et al. (2014), also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and we acknowledge support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research Council (NWO). GM received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS – DLV-896778. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. This paper also makes use of observations made with the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of the following programs and open-source packages for Python and we are thankful to their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013, 2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).","doi":"10.1051/0004-6361/202140876","year":"2021","title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","external_id":{"arxiv":["2108.01713"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.01713"}],"article_number":"A80","day":"15","type":"journal_article","intvolume":" 654","status":"public","publication":"Astronomy & Astrophysics","month":"10","article_type":"original","date_published":"2021-10-15T00:00:00Z","scopus_import":"1","publisher":"EDP Sciences","language":[{"iso":"eng"}],"date_created":"2022-07-06T08:49:03Z"},{"external_id":{"arxiv":["2102.05516"]},"title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","year":"2021","doi":"10.1051/0004-6361/202039887","article_number":"A107","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.05516"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"author":[{"full_name":"Bacon, R.","last_name":"Bacon","first_name":"R."},{"last_name":"Mary","full_name":"Mary, D.","first_name":"D."},{"full_name":"Garel, T.","last_name":"Garel","first_name":"T."},{"full_name":"Blaizot, J.","last_name":"Blaizot","first_name":"J."},{"first_name":"M.","full_name":"Maseda, M.","last_name":"Maseda"},{"full_name":"Schaye, J.","last_name":"Schaye","first_name":"J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"first_name":"S.","full_name":"Conseil, S.","last_name":"Conseil"},{"first_name":"J.","last_name":"Brinchmann","full_name":"Brinchmann, J."},{"first_name":"F.","full_name":"Leclercq, F.","last_name":"Leclercq"},{"last_name":"Abril-Melgarejo","full_name":"Abril-Melgarejo, V.","first_name":"V."},{"first_name":"L.","full_name":"Boogaard, L.","last_name":"Boogaard"},{"full_name":"Bouché, N. F.","last_name":"Bouché","first_name":"N. F."},{"first_name":"T.","last_name":"Contini","full_name":"Contini, T."},{"first_name":"A.","last_name":"Feltre","full_name":"Feltre, A."},{"last_name":"Guiderdoni","full_name":"Guiderdoni, B.","first_name":"B."},{"full_name":"Herenz, C.","last_name":"Herenz","first_name":"C."},{"first_name":"W.","last_name":"Kollatschny","full_name":"Kollatschny, W."},{"last_name":"Kusakabe","full_name":"Kusakabe, H.","first_name":"H."},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Michel-Dansac","full_name":"Michel-Dansac, L.","first_name":"L."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"full_name":"Richard, J.","last_name":"Richard","first_name":"J."},{"first_name":"M.","full_name":"Roth, M.","last_name":"Roth"},{"last_name":"Schmidt","full_name":"Schmidt, K. B.","first_name":"K. B."},{"first_name":"M.","last_name":"Steinmetz","full_name":"Steinmetz, M."},{"first_name":"L.","full_name":"Tresse, L.","last_name":"Tresse"},{"first_name":"T.","last_name":"Urrutia","full_name":"Urrutia, T."},{"last_name":"Verhamme","full_name":"Verhamme, A.","first_name":"A."},{"last_name":"Weilbacher","full_name":"Weilbacher, P. M.","first_name":"P. M."},{"last_name":"Zabl","full_name":"Zabl, J.","first_name":"J."},{"first_name":"S. L.","last_name":"Zoutendijk","full_name":"Zoutendijk, S. L."}],"abstract":[{"lang":"eng","text":"We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift."}],"citation":{"short":"R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F. Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe, J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt, M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L. Zoutendijk, Astronomy & Astrophysics 647 (2021).","ista":"Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. 647, A107.","mla":"Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” Astronomy & Astrophysics, vol. 647, A107, EDP Sciences, 2021, doi:10.1051/0004-6361/202039887.","ama":"Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. 2021;647. doi:10.1051/0004-6361/202039887","chicago":"Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039887.","apa":"Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk, S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039887","ieee":"R. Bacon et al., “The MUSE Extremely Deep Field: The cosmic web in emission at high redshift,” Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021."},"publication_status":"published","quality_controlled":"1","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We warmly thank ESO Paranal staff for their great professional support during all MXDF GTO observing runs. We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We also thank Matthew Lehnert for fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support from the GDR ISIS through the Projets exploratoires program (project TASTY). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges support by The Netherlands Organisation for Scientific Research (NWO) through a TOP Grant Module 1 under project number 614.001.652. This research made use of the following open-source software and we are thankful to the developers of these: GNU Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","_id":"11500","article_processing_charge":"No","date_updated":"2022-07-19T09:34:57Z","oa":1,"volume":647,"arxiv":1,"language":[{"iso":"eng"}],"scopus_import":"1","publisher":"EDP Sciences","article_type":"original","date_published":"2021-03-18T00:00:00Z","month":"03","date_created":"2022-07-06T09:31:50Z","status":"public","intvolume":" 647","type":"journal_article","day":"18","publication":"Astronomy & Astrophysics"},{"issue":"1","publication":"The Astrophysical Journal","intvolume":" 916","status":"public","day":"20","type":"journal_article","date_created":"2022-07-06T13:05:50Z","publisher":"IOP Publishing","scopus_import":"1","language":[{"iso":"eng"}],"month":"07","article_type":"original","date_published":"2021-07-20T00:00:00Z","_id":"11512","extern":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"acknowledgement":"We would like to thank the referee for a constructive and helpful report. L.A.B. is grateful to Corentin Schreiber for assisting with the near-infrared spectroscopy during the early stages of this work. L.A.B. acknowledges support from the Leids Kerkhoven-Bosscha Fonds under subsidy numbers 18.2.074 and 19.1.147. D.R. acknowledges support from the National Science Foundation under grant numbers AST-1614213 and AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.F. acknowledges the support from grant PRIN MIUR 201720173ML3WW_001. J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020. H.I. acknowledges support from JSPS KAKENHI grant No. JP19K23462. This work is based on observations collected at the European Southern Observatory under ESO programs 094.A-2089(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 099.A-0858(A), and 0101.A-0725(A). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Preprint","arxiv":1,"oa":1,"volume":916,"date_updated":"2022-07-19T09:32:48Z","article_processing_charge":"No","abstract":[{"text":"We study the molecular gas content of 24 star-forming galaxies at z = 3–4, with a median stellar mass of 109.1 M⊙, from the MUSE Hubble Ultra Deep Field (HUDF) Survey. Selected by their Lyα λ1216 emission and HF160W-band magnitude, the galaxies show an average $\\langle {\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\rangle \\approx 20$ Å, below the typical selection threshold for Lyα emitters (${\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\gt 25$ Å), and a rest-frame UV spectrum similar to Lyman-break galaxies. We use rest-frame optical spectroscopy from KMOS and MOSFIRE, and the UV features observed with MUSE, to determine the systemic redshifts, which are offset from Lyα by 〈Δv(Lyα)〉 = 346 km s−1, with a 100 to 600 km s−1 range. Stacking 12CO J = 4 → 3 and [C i]3P1 → 3P0 (and higher-J CO lines) from the ALMA Spectroscopic Survey of the HUDF, we determine 3σ upper limits on the line luminosities of 4.0 × 108 K km s−1pc2 and 5.6 × 108 K km s−1pc2, respectively (for a 300 km s−1 line width). Stacking the 1.2 mm and 3 mm dust-continuum flux densities, we find a 3σ upper limits of 9 μJy and 1.2 μJy, respectively. The inferred gas fractions, under the assumption of a \"Galactic\" CO-to-H2 conversion factor and gas-to-dust ratio, are in tension with previously determined scaling relations. This implies a substantially higher αCO ≥ 10 and δGDR ≥ 1200, consistent with the subsolar metallicity estimated for these galaxies ($12+\\mathrm{log}({\\rm{O}}/{\\rm{H}})\\approx 7.8\\pm 0.2$). The low metallicity of z ≥ 3 star-forming galaxies may thus make it very challenging to unveil their cold gas through CO or dust emission, warranting further exploration of alternative tracers, such as [C ii].","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"first_name":"Rychard J.","full_name":"Bouwens, Rychard J.","last_name":"Bouwens"},{"full_name":"Riechers, Dominik","last_name":"Riechers","first_name":"Dominik"},{"first_name":"Paul","last_name":"van der Werf","full_name":"van der Werf, Paul"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Stefanon, Mauro","last_name":"Stefanon","first_name":"Mauro"},{"first_name":"Anna","full_name":"Feltre, Anna","last_name":"Feltre"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"first_name":"Manuel","full_name":"Aravena, Manuel","last_name":"Aravena"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"full_name":"Carilli, Chris","last_name":"Carilli","first_name":"Chris"},{"last_name":"Contini","full_name":"Contini, Thierry","first_name":"Thierry"},{"first_name":"Roberto","last_name":"Decarli","full_name":"Decarli, Roberto"},{"last_name":"González-López","full_name":"González-López, Jorge","first_name":"Jorge"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"},{"full_name":"Walter, Fabian","last_name":"Walter","first_name":"Fabian"}],"publication_status":"published","citation":{"short":"L.A. Boogaard, R.J. Bouwens, D. Riechers, P. van der Werf, R. Bacon, J.J. Matthee, M. Stefanon, A. Feltre, M. Maseda, H. Inami, M. Aravena, J. Brinchmann, C. Carilli, T. Contini, R. Decarli, J. González-López, T. Nanayakkara, F. Walter, The Astrophysical Journal 916 (2021).","ista":"Boogaard LA, Bouwens RJ, Riechers D, van der Werf P, Bacon R, Matthee JJ, Stefanon M, Feltre A, Maseda M, Inami H, Aravena M, Brinchmann J, Carilli C, Contini T, Decarli R, González-López J, Nanayakkara T, Walter F. 2021. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. 916(1), 12.","ama":"Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. 2021;916(1). doi:10.3847/1538-4357/ac01d7","mla":"Boogaard, Leindert A., et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” The Astrophysical Journal, vol. 916, no. 1, 12, IOP Publishing, 2021, doi:10.3847/1538-4357/ac01d7.","chicago":"Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” The Astrophysical Journal. IOP Publishing, 2021. https://doi.org/10.3847/1538-4357/ac01d7.","ieee":"L. A. Boogaard et al., “Measuring the average molecular gas content of star-forming galaxies at z = 3–4,” The Astrophysical Journal, vol. 916, no. 1. IOP Publishing, 2021.","apa":"Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R., Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac01d7"},"article_number":"12","main_file_link":[{"url":"https://arxiv.org/abs/2105.12489","open_access":"1"}],"external_id":{"arxiv":["2105.12489"]},"title":"Measuring the average molecular gas content of star-forming galaxies at z = 3–4","year":"2021","doi":"10.3847/1538-4357/ac01d7"},{"day":"01","type":"journal_article","intvolume":" 508","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","issue":"3","page":"3697-3709","month":"12","article_type":"original","date_published":"2021-12-01T00:00:00Z","scopus_import":"1","publisher":"Oxford University Press","language":[{"iso":"eng"}],"date_created":"2022-07-07T09:30:21Z","citation":{"chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2762.","apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2762","ieee":"M. Gronke et al., “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” Monthly Notices of the Royal Astronomical Society, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709.","short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:10.1093/mnras/stab2762.","ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 2021;508(3):3697-3709. doi:10.1093/mnras/stab2762"},"publication_status":"published","abstract":[{"lang":"eng","text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations."}],"keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"author":[{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"first_name":"Pierre","full_name":"Ocvirk, Pierre","last_name":"Ocvirk"},{"full_name":"Mason, Charlotte","last_name":"Mason","first_name":"Charlotte"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Sarah E I","last_name":"Bosman","full_name":"Bosman, Sarah E I"},{"last_name":"Sorce","full_name":"Sorce, Jenny G","first_name":"Jenny G"},{"first_name":"Joseph","last_name":"Lewis","full_name":"Lewis, Joseph"},{"first_name":"Kyungjin","last_name":"Ahn","full_name":"Ahn, Kyungjin"},{"first_name":"Dominique","last_name":"Aubert","full_name":"Aubert, Dominique"},{"last_name":"Dawoodbhoy","full_name":"Dawoodbhoy, Taha","first_name":"Taha"},{"last_name":"Iliev","full_name":"Iliev, Ilian T","first_name":"Ilian T"},{"full_name":"Shapiro, Paul R","last_name":"Shapiro","first_name":"Paul R"},{"last_name":"Yepes","full_name":"Yepes, Gustavo","first_name":"Gustavo"}],"arxiv":1,"article_processing_charge":"No","date_updated":"2022-08-18T10:45:56Z","oa":1,"volume":508,"extern":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"_id":"11522","quality_controlled":"1","oa_version":"Preprint","acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2021","doi":"10.1093/mnras/stab2762","external_id":{"arxiv":["2004.14496"]},"title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}]},{"language":[{"iso":"eng"}],"publisher":"Oxford University Press","scopus_import":"1","article_type":"original","date_published":"2021-07-01T00:00:00Z","month":"07","date_created":"2022-07-07T09:33:39Z","status":"public","intvolume":" 505","type":"journal_article","day":"01","page":"1382-1412","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","external_id":{"arxiv":["2102.07779"]},"title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","year":"2021","doi":"10.1093/mnras/stab1304","main_file_link":[{"url":"https://arxiv.org/abs/2102.07779","open_access":"1"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Matthew","last_name":"Hayes","full_name":"Hayes, Matthew"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"first_name":"Rohan P","full_name":"Naidu, Rohan P","last_name":"Naidu"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"last_name":"Amorín","full_name":"Amorín, Ricardo","first_name":"Ricardo"}],"abstract":[{"lang":"eng","text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙."}],"publication_status":"published","citation":{"apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1304","ieee":"J. J. Matthee et al., “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?,” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.","chicago":"Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1304.","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 2021;505(1):1382-1412. doi:10.1093/mnras/stab1304","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:10.1093/mnras/stab1304.","short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the referee for constructive comments and suggestions. We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for useful discussions and suggestions. It is a pleasure to thank the ESO User Support, in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and Lowell Tacconi-Garman for assistance in the preparation and execution of the observations. Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413, 091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779, and 102.A-0652. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY, MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of A. C. J.Matthee (1953–2020).","oa_version":"Preprint","quality_controlled":"1","_id":"11523","extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"volume":505,"date_updated":"2022-08-18T10:49:00Z","oa":1,"article_processing_charge":"No","arxiv":1},{"oa":1,"date_updated":"2022-08-18T10:51:47Z","volume":505,"article_processing_charge":"No","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","quality_controlled":"1","oa_version":"Preprint","_id":"11524","extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","citation":{"chicago":"Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha, J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1218.","apa":"Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha, E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1218","ieee":"S. Santos et al., “The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1. Oxford University Press, pp. 1117–1134, 2021.","short":"S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha, J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the Royal Astronomical Society 505 (2021) 1117–1134.","ista":"Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E, Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.","mla":"Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:10.1093/mnras/stab1218.","ama":"Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 2021;505(1):1117-1134. doi:10.1093/mnras/stab1218"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"],"author":[{"first_name":"S","full_name":"Santos, S","last_name":"Santos"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"first_name":"J","last_name":"Butterworth","full_name":"Butterworth, J"},{"first_name":"A","full_name":"Paulino-Afonso, A","last_name":"Paulino-Afonso"},{"first_name":"B","full_name":"Ribeiro, B","last_name":"Ribeiro"},{"full_name":"da Cunha, E","last_name":"da Cunha","first_name":"E"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"},{"first_name":"A A","full_name":"Khostovan, A A","last_name":"Khostovan"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"P","full_name":"Arrabal Haro, P","last_name":"Arrabal Haro"}],"abstract":[{"text":"We measure the evolution of the rest-frame UV luminosity function (LF) and the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11 and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8⁠. An increasing LLy α cut predominantly lowers the number density of faint MUV and low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple assumptions of the faint end slope. For the UV LF, we find a brightening of the characteristic UV luminosity (M∗UV⁠) with increasing redshift and a decrease of the characteristic number density (Φ*). For the SMF, we measure a characteristic stellar mass (⁠M∗⋆/M⊙⁠) increase with increasing redshift, and a Φ* decline. However, if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0⁠, we find much milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV) of the full sample of LAEs shows moderate evolution and the stellar mass density (ρM) decreases, with both being always lower than the total ρUV and ρM of more typical galaxies but slowly approaching them with increasing redshift. Overall, our results indicate that both ρUV and ρM of LAEs slowly approach the measurements of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in the epoch of reionization.","lang":"eng"}],"main_file_link":[{"url":"https://arxiv.org/abs/2105.00007","open_access":"1"}],"year":"2021","doi":"10.1093/mnras/stab1218","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","external_id":{"arxiv":["2105.00007"]},"page":"1117-1134","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","type":"journal_article","day":"01","status":"public","intvolume":" 505","date_created":"2022-07-07T10:02:59Z","article_type":"original","date_published":"2021-07-01T00:00:00Z","month":"07","language":[{"iso":"eng"}],"publisher":"Oxford University Press","scopus_import":"1"},{"month":"06","article_type":"original","date_published":"2021-06-01T00:00:00Z","scopus_import":"1","publisher":"Oxford University Press","language":[{"iso":"eng"}],"date_created":"2022-07-07T10:07:11Z","day":"01","type":"journal_article","intvolume":" 504","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","page":"16-32","doi":"10.1093/mnras/stab796","year":"2021","external_id":{"arxiv":["2103.09250"]},"title":"Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2103.09250"}],"citation":{"chicago":"Gallego, Sofia G, Sebastiano Cantalupo, Saeed Sarpas, Bastien Duboeuf, Simon Lilly, Gabriele Pezzulli, Raffaella Anna Marino, et al. “Constraining the Cosmic UV Background at z > 3 with MUSE Lyman-α Emission Observations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab796.","apa":"Gallego, S. G., Cantalupo, S., Sarpas, S., Duboeuf, B., Lilly, S., Pezzulli, G., … Mauerhofer, V. (2021). Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab796","ieee":"S. G. Gallego et al., “Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations,” Monthly Notices of the Royal Astronomical Society, vol. 504, no. 1. Oxford University Press, pp. 16–32, 2021.","ista":"Gallego SG, Cantalupo S, Sarpas S, Duboeuf B, Lilly S, Pezzulli G, Marino RA, Matthee JJ, Wisotzki L, Schaye J, Richard J, Kusakabe H, Mauerhofer V. 2021. Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical Society. 504(1), 16–32.","short":"S.G. Gallego, S. Cantalupo, S. Sarpas, B. Duboeuf, S. Lilly, G. Pezzulli, R.A. Marino, J.J. Matthee, L. Wisotzki, J. Schaye, J. Richard, H. Kusakabe, V. Mauerhofer, Monthly Notices of the Royal Astronomical Society 504 (2021) 16–32.","mla":"Gallego, Sofia G., et al. “Constraining the Cosmic UV Background at z > 3 with MUSE Lyman-α Emission Observations.” Monthly Notices of the Royal Astronomical Society, vol. 504, no. 1, Oxford University Press, 2021, pp. 16–32, doi:10.1093/mnras/stab796.","ama":"Gallego SG, Cantalupo S, Sarpas S, et al. Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical Society. 2021;504(1):16-32. doi:10.1093/mnras/stab796"},"publication_status":"published","abstract":[{"text":"The intensity of the Cosmic UV background (UVB), coming from all sources of ionizing photons such as star-forming galaxies and quasars, determines the thermal evolution and ionization state of the intergalactic medium (IGM) and is, therefore, a critical ingredient for models of cosmic structure formation. Most of the previous estimates are based on the comparison between observed and simulated Lyman-α forest. We present the results of an independent method to constrain the product of the UVB photoionization rate and the covering fraction of Lyman limit systems (LLSs) by searching for the fluorescent Lyman-α emission produced by self-shielded clouds. Because the expected surface brightness is well below current sensitivity limits for direct imaging, we developed a new method based on 3D stacking of the IGM around Lyman-α emitting galaxies (LAEs) between 2.9 < z < 6.6 using deep MUSE observations. Combining our results with covering fractions of LLSs obtained from mock cubes extracted from the EAGLE simulation, we obtain new and independent constraints on the UVB at z > 3 that are consistent with previous measurements, with a preference for relatively low UVB intensities at z = 3, and which suggest a non-monotonic decrease of ΓH I with increasing redshift between 3 < z < 5. This could suggest a possible tension between some UVB models and current observations which however require deeper and wider observations in Lyman-α emission and absorption to be confirmed. Assuming instead a value of UVB from current models, our results constrain the covering fraction of LLSs at 3 < z < 4.5 to be less than 25 per cent within 150 kpc from LAEs.","lang":"eng"}],"author":[{"first_name":"Sofia G","last_name":"Gallego","full_name":"Gallego, Sofia G"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"full_name":"Sarpas, Saeed","last_name":"Sarpas","first_name":"Saeed"},{"full_name":"Duboeuf, Bastien","last_name":"Duboeuf","first_name":"Bastien"},{"first_name":"Simon","full_name":"Lilly, Simon","last_name":"Lilly"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"first_name":"Valentin","full_name":"Mauerhofer, Valentin","last_name":"Mauerhofer"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"arxiv":1,"article_processing_charge":"No","volume":504,"date_updated":"2022-08-18T10:54:19Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","_id":"11525","oa_version":"Preprint","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA)."},{"abstract":[{"text":"We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which were selected to be much fainter (20 < iSDSS < 23) than in previous studies of giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect H I Ly α nebulae around 100 per cent of our target quasars, with emission extending to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations between properties of the nebulae and their host quasars, with the goal of connecting variations in the properties of the illuminating QSO to the response in nebular emission. We show that the surface brightness profiles of the nebulae are similar to those of nebulae around bright quasars, but with a lower normalization. Our targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than our bright reference sample, and yet the nebulae around them are only 4.3 times fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find significant correlations between the surface brightness of the nebula and the luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted as evidence for a substantial contribution from unresolved inner parts of the nebulae to the narrow components seen in the Ly α lines of some of our faint quasars, possibly from the inner circumgalactic medium or from the host galaxy’s interstellar medium.","lang":"eng"}],"author":[{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo"},{"first_name":"Raffaella A","full_name":"Marino, Raffaella A","last_name":"Marino"},{"first_name":"Simon","last_name":"Lilly","full_name":"Lilly, Simon"},{"first_name":"Sowgat","full_name":"Muzahid, Sowgat","last_name":"Muzahid"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"publication_status":"published","citation":{"ama":"Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 2021;502(1):494-509. doi:10.1093/mnras/staa3277","mla":"Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society, vol. 502, no. 1, Oxford University Press, 2021, pp. 494–509, doi:10.1093/mnras/staa3277.","ista":"Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.","short":"R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid, J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 502 (2021) 494–509.","ieee":"R. Mackenzie et al., “Revealing the impact of quasar luminosity on giant Lyα nebulae,” Monthly Notices of the Royal Astronomical Society, vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.","apa":"Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid, S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3277","chicago":"Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/staa3277."},"_id":"11526","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"The authors thank Daichi Kashino, for providing access to unpublished zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al. (2020). GP and SC acknowledge the support of the Swiss National Science Foundation [grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship, Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under the MUSE GTO programme. The major analysis and production of figures in this work was conducted in Python, using standard libraries which include NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive command shell IPython (Pérez & Granger 2007). This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used to query galactic extinction maps. topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). This research has made use of the \"Aladin sky atlas\" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000).","oa_version":"Preprint","quality_controlled":"1","arxiv":1,"volume":502,"oa":1,"date_updated":"2022-08-18T10:56:28Z","article_processing_charge":"No","title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","external_id":{"arxiv":["2010.12589"]},"doi":"10.1093/mnras/staa3277","year":"2021","main_file_link":[{"url":"https://arxiv.org/abs/2010.12589","open_access":"1"}],"intvolume":" 502","status":"public","day":"01","type":"journal_article","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"494-509","publisher":"Oxford University Press","scopus_import":"1","language":[{"iso":"eng"}],"month":"03","date_published":"2021-03-01T00:00:00Z","article_type":"original","date_created":"2022-07-07T10:11:15Z"},{"external_id":{"arxiv":["1802.06786"]},"title":"Differences in galaxy colours are not just about the mass","doi":"10.1038/s41550-021-01415-y","year":"2021","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.06786"}],"keyword":["Astronomy and Astrophysics","galaxies","formation - galaxies","evolution - galaxies","star formation - galaxies","abundances"],"author":[{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"abstract":[{"lang":"eng","text":"Observations show that star-forming galaxies reside on a tight three-dimensional plane between mass, gas-phase metallicity and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional relations between mass, SFR and chemical enrichment using absolute and relative C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted toward late times, are more α-enhanced and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements."}],"citation":{"ama":"Matthee JJ. Differences in galaxy colours are not just about the mass. Nature Astronomy. 2021;5:984-985. doi:10.1038/s41550-021-01415-y","mla":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” Nature Astronomy, vol. 5, Springer Nature, 2021, pp. 984–85, doi:10.1038/s41550-021-01415-y.","ista":"Matthee JJ. 2021. Differences in galaxy colours are not just about the mass. Nature Astronomy. 5, 984–985.","short":"J.J. Matthee, Nature Astronomy 5 (2021) 984–985.","ieee":"J. J. Matthee, “Differences in galaxy colours are not just about the mass,” Nature Astronomy, vol. 5. Springer Nature, pp. 984–985, 2021.","apa":"Matthee, J. J. (2021). Differences in galaxy colours are not just about the mass. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-021-01415-y","chicago":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” Nature Astronomy. Springer Nature, 2021. https://doi.org/10.1038/s41550-021-01415-y."},"publication_status":"published","quality_controlled":"1","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the Topcat software (Taylor 2013) for assisting in rapid exploration of multi-dimensional datasets and the use of Python and its numpy, matplotlib and pandas packages.","publication_identifier":{"eissn":["2397-3366"]},"extern":"1","_id":"11585","article_processing_charge":"No","volume":5,"oa":1,"date_updated":"2022-08-19T08:37:58Z","arxiv":1,"language":[{"iso":"eng"}],"scopus_import":"1","publisher":"Springer Nature","date_published":"2021-07-05T00:00:00Z","article_type":"original","month":"07","date_created":"2022-07-14T13:13:39Z","status":"public","intvolume":" 5","type":"journal_article","day":"05","page":"984-985","publication":"Nature Astronomy"},{"date_published":"2020-09-18T00:00:00Z","article_type":"original","month":"09","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"EDP Sciences","date_created":"2022-07-06T09:38:16Z","type":"journal_article","day":"18","status":"public","intvolume":" 641","publication":"Astronomy & Astrophysics","year":"2020","doi":"10.1051/0004-6361/202038133","title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","external_id":{"arxiv":["2007.01878"]},"main_file_link":[{"url":"https://arxiv.org/abs/2007.01878","open_access":"1"}],"article_number":"A118","citation":{"short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy & Astrophysics 641 (2020).","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 641, A118.","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 2020;641. doi:10.1051/0004-6361/202038133","mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics, vol. 641, A118, EDP Sciences, 2020, doi:10.1051/0004-6361/202038133.","chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202038133.","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038133","ieee":"A. Feltre et al., “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3,” Astronomy & Astrophysics, vol. 641. EDP Sciences, 2020."},"publication_status":"published","author":[{"last_name":"Feltre","full_name":"Feltre, Anna","first_name":"Anna"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"first_name":"Jayadev","full_name":"Pradeep, Jayadev","last_name":"Pradeep"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"first_name":"Kasper B.","full_name":"Schmidt, Kasper B.","last_name":"Schmidt"},{"first_name":"Jeremy","full_name":"Blaizot, Jeremy","last_name":"Blaizot"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"first_name":"Leindert","full_name":"Boogaard, Leindert","last_name":"Boogaard"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"first_name":"David","full_name":"Carton, David","last_name":"Carton"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"first_name":"Wolfram","full_name":"Kollatschny, Wolfram","last_name":"Kollatschny"},{"first_name":"Raffaella A.","last_name":"Marino","full_name":"Marino, Raffaella A."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"full_name":"Tresse, Laurence","last_name":"Tresse","first_name":"Laurence"},{"last_name":"Urrutia","full_name":"Urrutia, Tanya","first_name":"Tanya"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"},{"first_name":"Peter M.","last_name":"Weilbacher","full_name":"Weilbacher, Peter M."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"abstract":[{"text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z >  2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.","lang":"eng"}],"article_processing_charge":"No","date_updated":"2022-07-19T09:35:43Z","volume":641,"oa":1,"arxiv":1,"oa_version":"Published Version","quality_controlled":"1","acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","_id":"11501"},{"day":"03","type":"journal_article","intvolume":" 638","status":"public","publication":"Astronomy & Astrophysics","month":"06","date_published":"2020-06-03T00:00:00Z","article_type":"original","publisher":"EDP Sciences","scopus_import":"1","language":[{"iso":"eng"}],"date_created":"2022-07-06T09:50:48Z","publication_status":"published","citation":{"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. Astronomy & Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340","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.” Astronomy & Astrophysics, vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.","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 & Astrophysics 638 (2020).","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 & Astrophysics. 638, A12.","ieee":"H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy & Astrophysics, vol. 638. EDP Sciences, 2020.","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937340","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.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340."},"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"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"author":[{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"last_name":"Blaizot","full_name":"Blaizot, Jérémy","first_name":"Jérémy"},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"last_name":"Verhamme","full_name":"Verhamme, Anne","first_name":"Anne"},{"last_name":"Bacon","full_name":"Bacon, Roland","first_name":"Roland"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"last_name":"Hashimoto","full_name":"Hashimoto, Takuya","first_name":"Takuya"},{"first_name":"Hanae","full_name":"Inami, Hanae","last_name":"Inami"},{"first_name":"Simon","full_name":"Conseil, Simon","last_name":"Conseil"},{"first_name":"Bruno","full_name":"Guiderdoni, Bruno","last_name":"Guiderdoni"},{"first_name":"Alyssa B.","full_name":"Drake, Alyssa B.","last_name":"Drake"},{"first_name":"Edmund","last_name":"Christian Herenz","full_name":"Christian Herenz, Edmund"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"last_name":"Oesch","full_name":"Oesch, Pascal","first_name":"Pascal"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Raffaella","full_name":"Anna Marino, Raffaella","last_name":"Anna Marino"},{"last_name":"Borello Schmidt","full_name":"Borello Schmidt, Kasper","first_name":"Kasper"},{"last_name":"Pelló","full_name":"Pelló, Roser","first_name":"Roser"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"first_name":"Floriane","last_name":"Leclercq","full_name":"Leclercq, Floriane"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"full_name":"Mahler, Guillaume","last_name":"Mahler","first_name":"Guillaume"}],"arxiv":1,"volume":638,"date_updated":"2022-07-19T09:35:20Z","oa":1,"article_processing_charge":"No","_id":"11503","extern":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Published Version","doi":"10.1051/0004-6361/201937340","year":"2020","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","external_id":{"arxiv":["2003.12083"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2003.12083"}],"article_number":"A12"},{"publication":"Astronomy & Astrophysics","day":"11","type":"journal_article","intvolume":" 635","status":"public","date_created":"2022-07-06T09:56:20Z","month":"03","date_published":"2020-03-11T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"EDP Sciences","language":[{"iso":"eng"}],"arxiv":1,"article_processing_charge":"No","volume":635,"oa":1,"date_updated":"2022-07-19T09:36:58Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","_id":"11504","quality_controlled":"1","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"F.L., R.B., and S.C. acknowledge support from the ERC advanced grant 339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds (PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan.","citation":{"ieee":"F. Leclercq et al., “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3,” Astronomy & Astrophysics, vol. 635. EDP Sciences, 2020.","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339","chicago":"Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937339.","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339","mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences, 2020, doi:10.1051/0004-6361/201937339.","ista":"Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 635, A82.","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020)."},"publication_status":"published","abstract":[{"text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >  MUV >  −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV <  −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs.","lang":"eng"}],"author":[{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"first_name":"Jérémy","last_name":"Blaizot","full_name":"Blaizot, Jérémy"},{"first_name":"Jarle","full_name":"Brinchmann, Jarle","last_name":"Brinchmann"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens"},{"first_name":"Simon","last_name":"Conseil","full_name":"Conseil, Simon"},{"full_name":"Contini, Thierry","last_name":"Contini","first_name":"Thierry"},{"last_name":"Hashimoto","full_name":"Hashimoto, Takuya","first_name":"Takuya"},{"last_name":"Herenz","full_name":"Herenz, Edmund Christian","first_name":"Edmund Christian"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Mitchell","full_name":"Mitchell, Peter","first_name":"Peter"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"first_name":"Kasper Borello","last_name":"Schmidt","full_name":"Schmidt, Kasper Borello"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"article_number":"A82","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2002.05731"}],"year":"2020","doi":"10.1051/0004-6361/201937339","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3","external_id":{"arxiv":["2002.05731"]}}]