[{"department":[{"_id":"JoMa"}],"year":"2026","date_created":"2026-07-12T22:02:18Z","OA_place":"publisher","date_published":"2026-07-01T00:00:00Z","volume":711,"date_updated":"2026-07-13T08:43:41Z","citation":{"mla":"Gentile, F., et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” <i>Astronomy and Astrophysics</i>, vol. 711, A12, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557633\">10.1051/0004-6361/202557633</a>.","chicago":"Gentile, F., E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J. B. Billand, P. Corcho-Caballero, et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557633\">https://doi.org/10.1051/0004-6361/202557633</a>.","apa":"Gentile, F., Daddi, E., Elbaz, D., Enia, A., Magnelli, B., Billand, J. B., … Walton, N. A. (2026). Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557633\">https://doi.org/10.1051/0004-6361/202557633</a>","short":"F. Gentile, E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J.B. Billand, P. Corcho-Caballero, C. Cleland, G. De Lucia, C. D’Eugenio, M. Fossati, M. Franco, C. Lobo, Y. Lyu, M. Magliocchetti, G.A. Mamon, L. Quilley, J.G. Sorce, M. Tarrasse, M. Bolzonella, F. Durret, L. Gabarra, S. Guo, L. Pozzetti, S. Quai, F. Shankar, V. Sangalli, M. Talia, M. Baes, H. Fu, M. Girardi, J.J. Matthee, P.A. Oesch, D. Roberts, J. Schaye, D. Scott, L. Spinoglio, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, R. Bender, A. Biviano, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, K.C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, L. Conversi, Y. Copin, F. Courbin, H.M. Courtois, M. Cropper, A. Da Silva, H. Degaudenzi, C. Dolding, H. Dole, F. Dubath, C.A.J. Duncan, X. Dupac, S. Dusini, S. Escoffier, M. Fabricius, M. Farina, R. Farinelli, S. Ferriol, F. Finelli, N. Fourmanoit, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, J. Gracia-Carpio, A. Grazian, F. Grupp, S. Gwyn, S.V.H. Haugan, J. Hoar, W. Holmes, I.M. Hook, F. Hormuth, A. Hornstrup, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, A.M.C. Le Brun, S. Ligori, P.B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R.J. Massey, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, S.M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W.J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L.A. Popa, F. Raison, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, P. Simon, C. Sirignano, G. Sirri, J. Skottfelt, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A.N. Taylor, H.I. Teplitz, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, I.A. Zinchenko, E. Zucca, V. Allevato, M. Ballardini, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, A. Cappi, D. Di Ferdinando, J.A. Escartin Vigo, W.G. Hartley, M. Huertas-Company, J. Martín-Fleitas, S. Matthew, N. Mauri, R.B. Metcalf, A. Pezzotta, M. Pöntinen, I. Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, I.T. Andika, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, D. Bertacca, M. Bethermin, L. Bisigello, A. Blanchard, L. Blot, H. Böhringer, M. Bonici, S. Borgani, M.L. Brown, S. Bruton, A. Calabro, B. Camacho Quevedo, F. Caro, C.S. Carvalho, T. Castro, F. Cogato, S. Conseil, T. Contini, A.R. Cooray, O. Cucciati, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J.M. Diego, P. Dimauro, P.A. Duc, M.Y. Elkhashab, Y. Fang, A. Finoguenov, A. Fontana, F. Fontanot, A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, R. Gavazzi, E. Gaztanaga, F. Giacomini, F. Gianotti, A.H. Gonzalez, G. Gozaliasl, M. Guidi, C.M. Gutierrez, A. Hall, S. Hemmati, H. Hildebrandt, J. Hjorth, J.J.E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, J. Kim, C.C. Kirkpatrick, S. Kruk, L. Legrand, M. Lembo, F. Lepori, G. Leroy, G.F. Lesci, J. Lesgourgues, L. Leuzzi, T.I. Liaudat, A. Loureiro, J. Macias-Perez, E.A. Magnier, F. Mannucci, R. Maoli, C.J.A.P. Martins, L. Maurin, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, K. Naidoo, A. Navarro-Alsina, S. Nesseris, D. Paoletti, F. Passalacqua, K. Paterson, L. Patrizii, A. Pisani, D. Potter, M. Radovich, G. Rodighiero, S. Sacquegna, M. Sahlén, D.B. Sanders, E. Sarpa, C. Scarlata, A. Schneider, M. Schultheis, D. Sciotti, E. Sellentin, L.C. Smith, S.A. Stanford, K. Tanidis, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N.A. Walton, Astronomy and Astrophysics 711 (2026).","ista":"Gentile F et al. 2026. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy and Astrophysics. 711, A12.","ama":"Gentile F, Daddi E, Elbaz D, et al. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. <i>Astronomy and Astrophysics</i>. 2026;711. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557633\">10.1051/0004-6361/202557633</a>","ieee":"F. Gentile <i>et al.</i>, “Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field,” <i>Astronomy and Astrophysics</i>, vol. 711. EDP Sciences, 2026."},"scopus_import":"1","supplementarymaterial":"no","type":"journal_article","file_date_updated":"2026-07-13T08:42:10Z","abstract":[{"text":"The well-known bimodality between star-forming discs and quiescent spheroids requires the existence of two main processes: galaxy quenching, causing the strong reduction of star formation, and morphological transformation, causing the transition from disc-dominated structures to bulge-dominated ones. In this paper, we aim to understand the link between these two processes and their relation with the stellar mass of galaxies and their local environment. Taking advantage of the first data released by the Euclid Collaboration, covering more than 60 deg2 with space-based imaging and photometry, we analyse a mass-complete sample of nearly one million galaxies in the range 0.25 < z < 1 with M* > 109.5 M⊙, using a combination of photometric and spectroscopic redshifts. We divide the sample into four sub-populations of galaxies, based on their star-formation activity (star-forming and quiescent) and morphology (disc-dominated and bulge-dominated). We then analyse the physical properties of these populations and their relative abundances in the stellar mass versus local density plane. Together with confirming the passivity-density relation and the morphology-density relation, we find that quiescent discy galaxies are more abundant in the low-mass regime of high-density environment where log10(1 + δ) > 1.3. At the same time, star-forming bulge-dominated galaxies are more common in field regions with log10(1 + δ) < 0.8, preferentially at high masses. Building on these results and interpreting them through comparison with simulations, we propose a scenario where the evolution of galaxies in the field significantly differs from that in higher-density environments. The morphological transformation in the majority of field galaxies takes place before the onset of quenching and is mainly driven by secular processes taking place within the main sequence, leading to the formation of star-forming bulge-dominated galaxies as intermediate-stage galaxies. Conversely, quenching of star formation precedes morphological transformation for most galaxies in higher-density environments. This causes the formation of quiescent disc-dominated galaxies before their transition into bulge-dominated ones.","lang":"eng"}],"das_tickbox":"1","month":"07","acknowledgement":"FaGe, AnEn, EmDa, LoGa, SaQu, GaDe, MaTa, ChDe, LuPo acknowledge support from the ELSA project. “ELSA: Euclid Legacy Science Advanced analysis tools” (Grant Agreement no. 101135203) is funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or Innovate UK. Neither the European Union nor the granting authority can be held responsible for them. UK participation is funded through the UK HORIZON guarantee scheme under Innovate UK grant 10093177. AnEn acknowledge support from the INAF MiniGrant 2023 “ADIEU: Anomaly Detections In EUclid”. CaLo acknowledges support by FCT-Fundação para a Ciência e a Tecnologia through grants UIDB/04434/2020 DOI: 10.54499/UIDB/04434/2020, UIDP/04434/2020 DOI: 10.54499/UIDP/04434/2020. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum für Luft-und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (www.euclid-ec.org). This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org","oa":1,"intvolume":"       711","researchdata_availability":"no","title":"Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field","article_processing_charge":"Yes","doi":"10.1051/0004-6361/202557633","arxiv":1,"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"publisher":"EDP Sciences","keyword":["galaxies: evolution","galaxies: interactions","galaxies: statistics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","article_type":"original","author":[{"full_name":"Gentile, F.","first_name":"F.","last_name":"Gentile"},{"first_name":"E.","full_name":"Daddi, E.","last_name":"Daddi"},{"full_name":"Elbaz, D.","first_name":"D.","last_name":"Elbaz"},{"full_name":"Enia, A.","first_name":"A.","last_name":"Enia"},{"full_name":"Magnelli, B.","first_name":"B.","last_name":"Magnelli"},{"last_name":"Billand","first_name":"J. B.","full_name":"Billand, J. B."},{"full_name":"Corcho-Caballero, P.","first_name":"P.","last_name":"Corcho-Caballero"},{"first_name":"C.","full_name":"Cleland, C.","last_name":"Cleland"},{"first_name":"G.","full_name":"De Lucia, G.","last_name":"De Lucia"},{"first_name":"C.","full_name":"D’Eugenio, C.","last_name":"D’Eugenio"},{"first_name":"M.","full_name":"Fossati, M.","last_name":"Fossati"},{"full_name":"Franco, M.","first_name":"M.","last_name":"Franco"},{"last_name":"Lobo","full_name":"Lobo, C.","first_name":"C."},{"first_name":"Y.","full_name":"Lyu, Y.","last_name":"Lyu"},{"first_name":"M.","full_name":"Magliocchetti, M.","last_name":"Magliocchetti"},{"last_name":"Mamon","first_name":"G. A.","full_name":"Mamon, G. A."},{"full_name":"Quilley, L.","first_name":"L.","last_name":"Quilley"},{"first_name":"J. G.","full_name":"Sorce, J. G.","last_name":"Sorce"},{"last_name":"Tarrasse","first_name":"M.","full_name":"Tarrasse, M."},{"last_name":"Bolzonella","full_name":"Bolzonella, M.","first_name":"M."},{"first_name":"F.","full_name":"Durret, F.","last_name":"Durret"},{"last_name":"Gabarra","first_name":"L.","full_name":"Gabarra, L."},{"full_name":"Guo, S.","first_name":"S.","last_name":"Guo"},{"first_name":"L.","full_name":"Pozzetti, L.","last_name":"Pozzetti"},{"last_name":"Quai","first_name":"S.","full_name":"Quai, S."},{"full_name":"Shankar, F.","first_name":"F.","last_name":"Shankar"},{"last_name":"Sangalli","first_name":"V.","full_name":"Sangalli, V."},{"last_name":"Talia","first_name":"M.","full_name":"Talia, M."},{"last_name":"Baes","full_name":"Baes, M.","first_name":"M."},{"first_name":"H.","full_name":"Fu, H.","last_name":"Fu"},{"last_name":"Girardi","first_name":"M.","full_name":"Girardi, M."},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Oesch, P. A.","first_name":"P. A.","last_name":"Oesch"},{"first_name":"D.","full_name":"Roberts, D.","last_name":"Roberts"},{"last_name":"Schaye","first_name":"J.","full_name":"Schaye, J."},{"full_name":"Scott, D.","first_name":"D.","last_name":"Scott"},{"first_name":"L.","full_name":"Spinoglio, L.","last_name":"Spinoglio"},{"last_name":"Altieri","full_name":"Altieri, B.","first_name":"B."},{"first_name":"A.","full_name":"Amara, A.","last_name":"Amara"},{"full_name":"Andreon, S.","first_name":"S.","last_name":"Andreon"},{"last_name":"Auricchio","full_name":"Auricchio, N.","first_name":"N."},{"full_name":"Baccigalupi, C.","first_name":"C.","last_name":"Baccigalupi"},{"first_name":"M.","full_name":"Baldi, M.","last_name":"Baldi"},{"full_name":"Balestra, A.","first_name":"A.","last_name":"Balestra"},{"last_name":"Bardelli","first_name":"S.","full_name":"Bardelli, S."},{"full_name":"Bender, R.","first_name":"R.","last_name":"Bender"},{"full_name":"Biviano, A.","first_name":"A.","last_name":"Biviano"},{"first_name":"E.","full_name":"Branchini, E.","last_name":"Branchini"},{"full_name":"Brescia, M.","first_name":"M.","last_name":"Brescia"},{"first_name":"J.","full_name":"Brinchmann, J.","last_name":"Brinchmann"},{"first_name":"S.","full_name":"Camera, S.","last_name":"Camera"},{"full_name":"Cañas-Herrera, G.","first_name":"G.","last_name":"Cañas-Herrera"},{"last_name":"Capobianco","full_name":"Capobianco, V.","first_name":"V."},{"first_name":"C.","full_name":"Carbone, C.","last_name":"Carbone"},{"last_name":"Carretero","full_name":"Carretero, J.","first_name":"J."},{"first_name":"S.","full_name":"Casas, S.","last_name":"Casas"},{"last_name":"Castellano","first_name":"M.","full_name":"Castellano, M."},{"first_name":"G.","full_name":"Castignani, G.","last_name":"Castignani"},{"last_name":"Cavuoti","full_name":"Cavuoti, S.","first_name":"S."},{"full_name":"Chambers, K. C.","first_name":"K. C.","last_name":"Chambers"},{"full_name":"Cimatti, A.","first_name":"A.","last_name":"Cimatti"},{"full_name":"Colodro-Conde, C.","first_name":"C.","last_name":"Colodro-Conde"},{"last_name":"Congedo","first_name":"G.","full_name":"Congedo, G."},{"full_name":"Conversi, L.","first_name":"L.","last_name":"Conversi"},{"first_name":"Y.","full_name":"Copin, Y.","last_name":"Copin"},{"last_name":"Courbin","full_name":"Courbin, F.","first_name":"F."},{"full_name":"Courtois, H. M.","first_name":"H. M.","last_name":"Courtois"},{"full_name":"Cropper, M.","first_name":"M.","last_name":"Cropper"},{"last_name":"Da Silva","full_name":"Da Silva, A.","first_name":"A."},{"first_name":"H.","full_name":"Degaudenzi, H.","last_name":"Degaudenzi"},{"last_name":"Dolding","full_name":"Dolding, C.","first_name":"C."},{"last_name":"Dole","first_name":"H.","full_name":"Dole, H."},{"full_name":"Dubath, F.","first_name":"F.","last_name":"Dubath"},{"last_name":"Duncan","full_name":"Duncan, C. A.J.","first_name":"C. A.J."},{"last_name":"Dupac","full_name":"Dupac, X.","first_name":"X."},{"first_name":"S.","full_name":"Dusini, S.","last_name":"Dusini"},{"last_name":"Escoffier","first_name":"S.","full_name":"Escoffier, S."},{"first_name":"M.","full_name":"Fabricius, M.","last_name":"Fabricius"},{"first_name":"M.","full_name":"Farina, M.","last_name":"Farina"},{"last_name":"Farinelli","full_name":"Farinelli, R.","first_name":"R."},{"full_name":"Ferriol, S.","first_name":"S.","last_name":"Ferriol"},{"full_name":"Finelli, F.","first_name":"F.","last_name":"Finelli"},{"last_name":"Fourmanoit","full_name":"Fourmanoit, N.","first_name":"N."},{"full_name":"Frailis, M.","first_name":"M.","last_name":"Frailis"},{"last_name":"Franceschi","first_name":"E.","full_name":"Franceschi, E."},{"first_name":"M.","full_name":"Fumana, M.","last_name":"Fumana"},{"first_name":"S.","full_name":"Galeotta, S.","last_name":"Galeotta"},{"full_name":"George, K.","first_name":"K.","last_name":"George"},{"first_name":"B.","full_name":"Gillis, B.","last_name":"Gillis"},{"last_name":"Giocoli","full_name":"Giocoli, C.","first_name":"C."},{"first_name":"J.","full_name":"Gracia-Carpio, J.","last_name":"Gracia-Carpio"},{"last_name":"Grazian","full_name":"Grazian, A.","first_name":"A."},{"last_name":"Grupp","full_name":"Grupp, F.","first_name":"F."},{"first_name":"S.","full_name":"Gwyn, S.","last_name":"Gwyn"},{"last_name":"Haugan","full_name":"Haugan, S. V.H.","first_name":"S. V.H."},{"last_name":"Hoar","full_name":"Hoar, J.","first_name":"J."},{"last_name":"Holmes","first_name":"W.","full_name":"Holmes, W."},{"last_name":"Hook","first_name":"I. M.","full_name":"Hook, I. M."},{"first_name":"F.","full_name":"Hormuth, F.","last_name":"Hormuth"},{"last_name":"Hornstrup","first_name":"A.","full_name":"Hornstrup, A."},{"last_name":"Jahnke","full_name":"Jahnke, K.","first_name":"K."},{"last_name":"Jhabvala","first_name":"M.","full_name":"Jhabvala, M."},{"first_name":"B.","full_name":"Joachimi, B.","last_name":"Joachimi"},{"first_name":"E.","full_name":"Keihänen, E.","last_name":"Keihänen"},{"last_name":"Kermiche","full_name":"Kermiche, S.","first_name":"S."},{"first_name":"A.","full_name":"Kiessling, A.","last_name":"Kiessling"},{"last_name":"Kubik","full_name":"Kubik, B.","first_name":"B."},{"first_name":"M.","full_name":"Kümmel, M.","last_name":"Kümmel"},{"last_name":"Kunz","first_name":"M.","full_name":"Kunz, M."},{"full_name":"Kurki-Suonio, H.","first_name":"H.","last_name":"Kurki-Suonio"},{"last_name":"Le Brun","first_name":"A. M.C.","full_name":"Le Brun, A. M.C."},{"last_name":"Ligori","full_name":"Ligori, S.","first_name":"S."},{"last_name":"Lilje","first_name":"P. B.","full_name":"Lilje, P. B."},{"last_name":"Lindholm","full_name":"Lindholm, V.","first_name":"V."},{"first_name":"I.","full_name":"Lloro, I.","last_name":"Lloro"},{"first_name":"G.","full_name":"Mainetti, G.","last_name":"Mainetti"},{"last_name":"Maino","full_name":"Maino, D.","first_name":"D."},{"full_name":"Maiorano, E.","first_name":"E.","last_name":"Maiorano"},{"full_name":"Mansutti, O.","first_name":"O.","last_name":"Mansutti"},{"last_name":"Marggraf","first_name":"O.","full_name":"Marggraf, O."},{"last_name":"Martinelli","full_name":"Martinelli, M.","first_name":"M."},{"last_name":"Martinet","first_name":"N.","full_name":"Martinet, N."},{"full_name":"Marulli, F.","first_name":"F.","last_name":"Marulli"},{"first_name":"R. J.","full_name":"Massey, R. 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B.","first_name":"D. B."},{"last_name":"Sarpa","first_name":"E.","full_name":"Sarpa, E."},{"full_name":"Scarlata, C.","first_name":"C.","last_name":"Scarlata"},{"last_name":"Schneider","full_name":"Schneider, A.","first_name":"A."},{"last_name":"Schultheis","first_name":"M.","full_name":"Schultheis, M."},{"last_name":"Sciotti","first_name":"D.","full_name":"Sciotti, D."},{"full_name":"Sellentin, E.","first_name":"E.","last_name":"Sellentin"},{"last_name":"Smith","full_name":"Smith, L. C.","first_name":"L. C."},{"first_name":"S. A.","full_name":"Stanford, S. A.","last_name":"Stanford"},{"first_name":"K.","full_name":"Tanidis, K.","last_name":"Tanidis"},{"last_name":"Testera","full_name":"Testera, G.","first_name":"G."},{"full_name":"Teyssier, R.","first_name":"R.","last_name":"Teyssier"},{"full_name":"Tosi, S.","first_name":"S.","last_name":"Tosi"},{"last_name":"Troja","full_name":"Troja, A.","first_name":"A."},{"full_name":"Tucci, M.","first_name":"M.","last_name":"Tucci"},{"last_name":"Valieri","full_name":"Valieri, C.","first_name":"C."},{"first_name":"A.","full_name":"Venhola, A.","last_name":"Venhola"},{"last_name":"Vergani","first_name":"D.","full_name":"Vergani, D."},{"last_name":"Verza","full_name":"Verza, G.","first_name":"G."},{"full_name":"Vielzeuf, P.","first_name":"P.","last_name":"Vielzeuf"},{"full_name":"Walton, N. A.","first_name":"N. A.","last_name":"Walton"}],"quality_controlled":"1","publication":"Astronomy and Astrophysics","publication_status":"published","_id":"22265","oa_version":"Published Version","OA_type":"gold","article_number":"A12","dataavailabilitystatement":"This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org","status":"public","external_id":{"arxiv":["2511.02964"]},"has_accepted_license":"1","day":"01","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"PlanS_conform":"1","language":[{"iso":"eng"}],"file":[{"checksum":"29c087abb97eed26d4aa2a19bbb46666","date_created":"2026-07-13T08:42:10Z","creator":"dernst","success":1,"access_level":"open_access","file_size":3482066,"date_updated":"2026-07-13T08:42:10Z","file_name":"2026_AstronomyAstrophysics_Euclid.pdf","relation":"main_file","content_type":"application/pdf","file_id":"22277"}],"ddc":["520"]},{"scopus_import":"1","type":"journal_article","abstract":[{"text":"Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies. While it originates from many physical processes, for star-forming galaxies the intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star formation rate (SFR) indicator. However, its resonant nature and susceptibility to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs) at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and we show that it constrains a well-defined anti-correlation between ionisation efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0 are easy measurable quantities at high redshift, thus making our relation a practical tool to estimate intrinsic Lyα and LyC luminosities under well controlled and simple assumptions. Our results allow observed Lyα luminosities to be used to compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs. We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6 to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1 and that our calibration might be even applicable for the most luminous LAEs within the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1] = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily tested with future observations with JWST which can obtain Hα and Hβ measurements for high-redshift LAEs.","lang":"eng"}],"date_created":"2022-07-06T11:08:16Z","year":"2019","citation":{"short":"D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).","ama":"Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. 2019;623. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>","ista":"Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy &#38; Astrophysics. 623, A157.","ieee":"D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator,” <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.","mla":"Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A157, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>.","chicago":"Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>.","apa":"Sobral, D., &#38; Matthee, J. J. (2019). Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>"},"date_updated":"2022-07-19T09:37:20Z","extern":"1","date_published":"2019-03-26T00:00:00Z","volume":623,"article_processing_charge":"No","doi":"10.1051/0004-6361/201833075","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","arxiv":1,"month":"03","acknowledgement":"We thank the anonymous referees for multiple comments and suggestions which have improved the manuscript. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017, 2018a) and we also provide the toy model used as a PYTHON script.","oa":1,"intvolume":"       623","publication":"Astronomy & Astrophysics","quality_controlled":"1","oa_version":"Published Version","_id":"11507","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1803.08923","open_access":"1"}],"publisher":"EDP Sciences","article_type":"original","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"day":"26","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"language":[{"iso":"eng"}],"status":"public","external_id":{"arxiv":["1803.08923"]},"article_number":"A157"},{"quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","main_file_link":[{"url":"https://arxiv.org/abs/1712.04451","open_access":"1"}],"_id":"11558","publication_status":"published","oa_version":"Preprint","publisher":"Oxford University Press","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Sérgio","full_name":"Santos, Sérgio","last_name":"Santos"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"first_name":"Bruno","full_name":"Ribeiro, Bruno","last_name":"Ribeiro"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"full_name":"Khostovan, Ali A","first_name":"Ali A","last_name":"Khostovan"}],"article_type":"original","day":"01","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"page":"4725-4752","language":[{"iso":"eng"}],"status":"public","external_id":{"arxiv":["1712.04451"]},"scopus_import":"1","type":"journal_article","abstract":[{"lang":"eng","text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape."}],"year":"2018","date_created":"2022-07-12T10:41:08Z","date_published":"2018-06-01T00:00:00Z","volume":476,"citation":{"short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>","ieee":"D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>.","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>."},"date_updated":"2022-08-19T07:04:45Z","extern":"1","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","article_processing_charge":"No","doi":"10.1093/mnras/sty378","arxiv":1,"month":"06","issue":"4","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","oa":1,"intvolume":"       476"},{"month":"04","intvolume":"       466","oa":1,"issue":"1","acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","doi":"10.1093/mnras/stw3090","article_processing_charge":"No","arxiv":1,"year":"2017","date_created":"2022-07-12T12:04:16Z","volume":466,"date_published":"2017-04-01T00:00:00Z","extern":"1","date_updated":"2024-10-14T11:35:37Z","citation":{"ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>","ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>."},"scopus_import":"1","abstract":[{"text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii.","lang":"eng"}],"type":"journal_article","external_id":{"arxiv":["1609.05897"]},"status":"public","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"day":"01","page":"1242-1258","language":[{"iso":"eng"}],"publisher":"Oxford University Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Best, Philip","first_name":"Philip","last_name":"Best"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"},{"full_name":"Smail, Ian","first_name":"Ian","last_name":"Smail"},{"last_name":"Morabito","first_name":"Leah","full_name":"Morabito, Leah"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"}],"article_type":"original","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","main_file_link":[{"url":"https://arxiv.org/abs/1609.05897","open_access":"1"}],"_id":"11562","oa_version":"Preprint","publication_status":"published"}]