@article{22265,
  abstract     = {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.},
  author       = {Gentile, F. and Daddi, E. and Elbaz, D. and Enia, A. and Magnelli, B. and Billand, J. B. and Corcho-Caballero, P. and Cleland, C. and De Lucia, G. and D’Eugenio, C. and Fossati, M. and Franco, M. and Lobo, C. and Lyu, Y. and Magliocchetti, M. and Mamon, G. A. and Quilley, L. and Sorce, J. G. and Tarrasse, M. and Bolzonella, M. and Durret, F. and Gabarra, L. and Guo, S. and Pozzetti, L. and Quai, S. and Shankar, F. and Sangalli, V. and Talia, M. and Baes, M. and Fu, H. and Girardi, M. and Matthee, Jorryt J and Oesch, P. A. and Roberts, D. and Schaye, J. and Scott, D. and Spinoglio, L. and Altieri, B. and Amara, A. and Andreon, S. and Auricchio, N. and Baccigalupi, C. and Baldi, M. and Balestra, A. and Bardelli, S. and Bender, R. and Biviano, A. and Branchini, E. and Brescia, M. and Brinchmann, J. and Camera, S. and Cañas-Herrera, G. and Capobianco, V. and Carbone, C. and Carretero, J. and Casas, S. and Castellano, M. and Castignani, G. and Cavuoti, S. and Chambers, K. C. and Cimatti, A. and Colodro-Conde, C. and Congedo, G. and Conversi, L. and Copin, Y. and Courbin, F. and Courtois, H. M. and Cropper, M. and Da Silva, A. and Degaudenzi, H. and Dolding, C. and Dole, H. and Dubath, F. and Duncan, C. A.J. and Dupac, X. and Dusini, S. and Escoffier, S. and Fabricius, M. and Farina, M. and Farinelli, R. and Ferriol, S. and Finelli, F. and Fourmanoit, N. and Frailis, M. and Franceschi, E. and Fumana, M. and Galeotta, S. and George, K. and Gillis, B. and Giocoli, C. and Gracia-Carpio, J. and Grazian, A. and Grupp, F. and Gwyn, S. and Haugan, S. V.H. and Hoar, J. and Holmes, W. and Hook, I. M. and Hormuth, F. and Hornstrup, A. and Jahnke, K. and Jhabvala, M. and Joachimi, B. and Keihänen, E. and Kermiche, S. and Kiessling, A. and Kubik, B. and Kümmel, M. and Kunz, M. and Kurki-Suonio, H. and Le Brun, A. M.C. and Ligori, S. and Lilje, P. B. and Lindholm, V. and Lloro, I. and Mainetti, G. and Maino, D. and Maiorano, E. and Mansutti, O. and Marggraf, O. and Martinelli, M. and Martinet, N. and Marulli, F. and Massey, R. J. and Medinaceli, E. and Mei, S. and Melchior, M. and Mellier, Y. and Meneghetti, M. and Merlin, E. and Meylan, G. and Mora, A. and Moresco, M. and Moscardini, L. and Nakajima, R. and Niemi, S. M. and Padilla, C. and Paltani, S. and Pasian, F. and Pedersen, K. and Percival, W. J. and Pettorino, V. and Pires, S. and Polenta, G. and Poncet, M. and Popa, L. A. and Raison, F. and Renzi, A. and Rhodes, J. and Riccio, G. and Romelli, E. and Roncarelli, M. and Saglia, R. and Sakr, Z. and Sapone, D. and Sartoris, B. and Schneider, P. and Schrabback, T. and Secroun, A. and Seidel, G. and Serrano, S. and Simon, P. and Sirignano, C. and Sirri, G. and Skottfelt, J. and Stanco, L. and Steinwagner, J. and Tallada-Crespí, P. and Taylor, A. N. and Teplitz, H. I. and Tereno, I. and Tessore, N. and Toft, S. and Toledo-Moreo, R. and Torradeflot, F. and Tutusaus, I. and Valenziano, L. and Valiviita, J. and Vassallo, T. and Verdoes Kleijn, G. and Veropalumbo, A. and Wang, Y. and Weller, J. and Zacchei, A. and Zamorani, G. and Zinchenko, I. A. and Zucca, E. and Allevato, V. and Ballardini, M. and Bozzo, E. and Burigana, C. and Cabanac, R. and Calabrese, M. and Cappi, A. and Di Ferdinando, D. and Escartin Vigo, J. A. and Hartley, W. G. and Huertas-Company, M. and Martín-Fleitas, J. and Matthew, S. and Mauri, N. and Metcalf, R. B. and Pezzotta, A. and Pöntinen, M. and Risso, I. and Scottez, V. and Sereno, M. and Tenti, M. and Viel, M. and Wiesmann, M. and Akrami, Y. and Andika, I. T. and Anselmi, S. and Archidiacono, M. and Atrio-Barandela, F. and Bertacca, D. and Bethermin, M. and Bisigello, L. and Blanchard, A. and Blot, L. and Böhringer, H. and Bonici, M. and Borgani, S. and Brown, M. L. and Bruton, S. and Calabro, A. and Camacho Quevedo, B. and Caro, F. and Carvalho, C. S. and Castro, T. and Cogato, F. and Conseil, S. and Contini, T. and Cooray, A. R. and Cucciati, O. and Desprez, G. and Díaz-Sánchez, A. and Di Domizio, S. and Diego, J. M. and Dimauro, P. and Duc, P. A. and Elkhashab, M. Y. and Fang, Y. and Finoguenov, A. and Fontana, A. and Fontanot, F. and Franco, A. and Ganga, K. and García-Bellido, J. and Gasparetto, T. and Gautard, V. and Gavazzi, R. and Gaztanaga, E. and Giacomini, F. and Gianotti, F. and Gonzalez, A. H. and Gozaliasl, G. and Guidi, M. and Gutierrez, C. M. and Hall, A. and Hemmati, S. and Hildebrandt, H. and Hjorth, J. and Kajava, J. J.E. and Kang, Y. and Kansal, V. and Karagiannis, D. and Kiiveri, K. and Kim, J. and Kirkpatrick, C. C. and Kruk, S. and Legrand, L. and Lembo, M. and Lepori, F. and Leroy, G. and Lesci, G. F. and Lesgourgues, J. and Leuzzi, L. and Liaudat, T. I. and Loureiro, A. and Macias-Perez, J. and Magnier, E. A. and Mannucci, F. and Maoli, R. and Martins, C. J.A.P. and Maurin, L. and Miluzio, M. and Monaco, P. and Moretti, C. and Morgante, G. and Naidoo, K. and Navarro-Alsina, A. and Nesseris, S. and Paoletti, D. and Passalacqua, F. and Paterson, K. and Patrizii, L. and Pisani, A. and Potter, D. and Radovich, M. and Rodighiero, G. and Sacquegna, S. and Sahlén, M. and Sanders, D. B. and Sarpa, E. and Scarlata, C. and Schneider, A. and Schultheis, M. and Sciotti, D. and Sellentin, E. and Smith, L. C. and Stanford, S. A. and Tanidis, K. and Testera, G. and Teyssier, R. and Tosi, S. and Troja, A. and Tucci, M. and Valieri, C. and Venhola, A. and Vergani, D. and Verza, G. and Vielzeuf, P. and Walton, N. A.},
  issn         = {1432-0746},
  journal      = {Astronomy and Astrophysics},
  keywords     = {galaxies: evolution, galaxies: interactions, galaxies: statistics},
  publisher    = {EDP Sciences},
  title        = {{Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field}},
  doi          = {10.1051/0004-6361/202557633},
  volume       = {711},
  year         = {2026},
}

@article{11507,
  abstract     = {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.},
  author       = {Sobral, David and Matthee, Jorryt J},
  issn         = {1432-0746},
  journal      = {Astronomy & Astrophysics},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics, galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM},
  publisher    = {EDP Sciences},
  title        = {{Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator}},
  doi          = {10.1051/0004-6361/201833075},
  volume       = {623},
  year         = {2019},
}

@article{11558,
  abstract     = {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.},
  author       = {Sobral, David and Santos, Sérgio and Matthee, Jorryt J and Paulino-Afonso, Ana and Ribeiro, Bruno and Calhau, João and Khostovan, Ali A},
  issn         = {1365-2966},
  journal      = {Monthly Notices of the Royal Astronomical Society},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics, galaxies: evolution, galaxies: formation, galaxies: high-redshift, galaxies: luminosity function, mass function, galaxies: statistics},
  number       = {4},
  pages        = {4725--4752},
  publisher    = {Oxford University Press},
  title        = {{Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6}},
  doi          = {10.1093/mnras/sty378},
  volume       = {476},
  year         = {2018},
}

@article{11562,
  abstract     = {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.},
  author       = {Sobral, David and Matthee, Jorryt J and Best, Philip and Stroe, Andra and Röttgering, Huub and Oteo, Iván and Smail, Ian and Morabito, Leah and Paulino-Afonso, Ana},
  issn         = {1365-2966},
  journal      = {Monthly Notices of the Royal Astronomical Society},
  keywords     = {Space and Planetary Science, Astronomy and Astrophysics, galaxies: evolution, galaxies: haloes, galaxies: high-redshift, galaxies: luminosity function, mass function, galaxies: statistics, cosmology: observations},
  number       = {1},
  pages        = {1242--1258},
  publisher    = {Oxford University Press},
  title        = {{The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23}},
  doi          = {10.1093/mnras/stw3090},
  volume       = {466},
  year         = {2017},
}