A1 Refereed original research article in a scientific journal
Euclid preparation: LXXXVI. Cosmic Dawn Survey: Evolution of the galaxy stellar mass function across 0.2 < z ≤ 6.5 measured over 10 square degrees
Authors: Zalesky, L.; Weaver, J. R.; McPartland, C. J. R.; Murphree, G.; Valdes, I.; Jespersen, C. K.; Taamoli, S.; Chartab, N.; Allen, N.; Barrow, S. W. J.; Sanders, D. B.; Toft, S.; Mobasher, B.; Szapudi, I.; Altieri, B.; Amara, A.; Andreon, S.; Auricchio, N.; Baccigalupi, C.; Baldi, M.; Bardelli, S.; Battaglia, P.; Biviano, A.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Caillat, A.; Camera, S.; Canas-Herrera, G.; Capobianco, V.; Carbone, C.; Carretero, J.; Casas, S.; Castander, F. J.; Castellano, M.; Castignani, G.; Cavuoti, S.; Chambers, K. C.; Cimatti, A.; Colodro-Conde, C.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Courbin, F.; Courtois, H. M.; Da Silva, A.; Degaudenzi, H.; De Lucia, G.; Di Giorgio, A. M.; Dole, H.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.; Ealet, A.; Escoffier, S.; Farina, M.; Farinelli, R.; Farrens, S.; Faustini, F.; Ferriol, S.; Finelli, F.; Fosalba, P.; Fotopoulou, S.; Frailis, M.; Franceschi, E.; Fumana, M.; George, K.; Gillis, B.; Giocoli, C.; Gracia-Carpio, J.; Grazian, A.; Grupp, F.; Gwyn, S.; Haugan, S. V. H.; Holmes, W.; Hook, I.; Hormuth, F.; Hornstrup, A.; Jahnke, K.; Jhabvala, M.; Joachimi, B.; Keihanen, E.; Kermiche, S.; Kiessling, A.; Kubik, B.; Kuijken, K.; Kummel, M.; Kunz, M.; Kurki-Suonio, H.; Le Brun, A. M. C.; Le Mignant, D.; Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Mainetti, G.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Maurogordato, S.; McCracken, H. J.; Medinaceli, E.; Mei, S.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mora, A.; Moresco, M.; Moscardini, L.; Nakajima, R.; Neissner, C.; Niemi, S. -M.; Nightingale, J. W.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pettorino, V.; Polenta, G.; Poncet, M.; Popa, L. A.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Saglia, R.; Sakr, Z.; Sapone, D.; Sartoris, B.; Schewtschenko, J. A.; Schirmer, M.; Schneider, P.; Schrabback, T.; Secroun, A.; Sefusatti, E.; Seidel, G.; Serrano, S.; Simon, P.; Sirignano, C.; Sirri, G.; Stanco, L.; Starck, J. -L.; Steinwagner, J.; Tallada-Crespi, P.; Tavagnacco, D.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Tsyganov, A.; Tutusaus, I.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Kleijn, G. Verdoes; Veropalumbo, A.; Wang, Y.; Weller, J.; Zacchei, A.; Zamorani, G.; Zucca, E.; Bolzonella, M.; Bozzo, E.; Burigana, C.; Calabrese, M.; Di Ferdinando, D.; Vigo, J. A. Escartin; Gabarra, L.; Matthew, S.; Mauri, N.; Pezzotta, A.; Pontinen, M.; Porciani, C.; Scottez, V.; Tenti, M.; Viel, M.; Wiesmann, M.; Akrami, Y.; Allevato, V.; Andika, I. T.; Anselmi, S.; Archidiacono, M.; Atrio-Barandela, F.; Ballardini, M.; Bertacca, D.; Bethermin, M.; Blanchard, A.; Blot, L.; Borgani, S.; Brown, M. L.; Bruton, S.; Cabanac, R.; Calabro, A.; Quevedo, B. Camacho; Cappi, A.; Caro, F.; Carvalho, C. S.; Castro, T.; Chary, R.; Cogato, F.; Contini, T.; Cooray, A. R.; Cucciati, O.; Davini, S.; De Paolis, F.; Desprez, G.; Diaz-Sanchez, A.; Di Domizio, S.; Diego, J. M.; Ferrari, A. G.; Finoguenov, A.; Ganga, K.; Garcia-Bellido, J.; Gasparetto, T.; Gaztanaga, E.; Giacomini, F.; Gianotti, F.; Gozaliasl, G.; Gregorio, A.; Guidi, M.; Gutierrez, C. M.; Hall, A.; Hartley, W. G.; Hemmati, S.; Hildebrandt, H.; Hjorth, J.; Huertas-Company, M.; Ilbert, O.; Kajava, J. J. E.; Kang, Y.; Kansal, V.; Karagiannis, D.; Kirkpatrick, C. C.; Kruk, S.; Lattanzi, M.; Le Graet, J.; Legrand, L.; Lembo, M.; Leroy, G.; Lesgourgues, J.; Liaudat, T. I.; Loureiro, A.; Macias-Perez, J.; Maggio, G.; Magliocchetti, M.; Mancini, C.; Mannucci, F.; Maoli, R.; Martin-Fleitas, J.; Martins, C. J. A. P.; Maurin, L.; Metcalf, R. B.; Miluzio, M.; Monaco, P.; Moretti, C.; Morgante, G.; Murray, C.; Naidoo, K.; Natoli, P.; Navarro-Alsina, A.; Nesseris, S.; Paterson, K.; Patrizii, L.; Pisani, A.; Potter, D.; Risso, I.; Rocci, P. -F.; Sahlen, M.; Sarpa, E.; Schaye, J.; Schneider, A.; Schultheis, M.; Sciotti, D.; Sellentin, E.; Sereno, M.; Shankar, F.; Smith, L. C.; Stanford, S. A.; Tanidis, K.; Tao, C.; Testera, G.; Teyssier, R.; Tosi, S.; Troja, A.; Tucci, M.; Valieri, C.; Venhola, A.; Vergani, D.; Verza, G.; Vielzeuf, P.; Walton, N. A.; Euclid Collaboration
Publisher: EDP Sciences
Publication year: 2026
Journal: Astronomy and Astrophysics
Article number: A104
Volume: 708
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202555728
Publication's open availability at the time of reporting: Open Access
Publication channel's open availability : Open Access publication channel
Web address : https://doi.org/10.1051/0004-6361/202555728
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/523250112
Self-archived copy's licence: CC BY
Self-archived copy's version: Publisher`s PDF
The Cosmic Dawn Survey pre-launch catalogues cover an e ffective 10.13 deg(2) area with uniform deep Spitzer/IRAC data (m similar to 25 mag, 5 sigma), the largest area covered to these depths at IR wavelengths. We used these data to gain new insight into the growth of stellar mass across cosmic history by characterising the evolution of the galaxy stellar mass function through 0.2 < z <= 6.5. The total volume (0.62 Gpc(3)) represents an order of magnitude increase compared to previous works that explored z > 3 and significantly reduces cosmic variance, thus yielding strong constraints on the abundance of galaxies above the characteristic stellar mass (M-*) across this ten billion year period. The evolution of the galaxy stellar mass function is generally consistent with results from the literature but now provides firm estimates of the number density where only upper limits were previously available. Contrasting the galaxy stellar mass function with the dark matter halo mass function suggests that massive galaxies ( M greater than or similar to 10(11) M-circle dot) at z > 3.5 required integrated star-formation e fficiencies of M/(M-h f(b))greater than or similar to 0.25-0.5, in excess of the commonly held view of a 'universal peak e fficiency' from studies on the stellar-to-halo mass relation. Such increased e fficiencies imply an evolving peak in the stellar-tohalo mass relation at z > 3.5 that can be maintained if feedback mechanisms from active galactic nuclei and stellar processes are ine ffective at early times. In addition, a significant fraction of the most massive quiescent galaxies are observed to be in place by z similar to 2.5-3. The apparent lack of change in their number density by z similar to 0.2 is consistent with relatively little mass growth from mergers. Utilising the unique volume, we find evidence of an environmental dependence of the galaxy stellar mass function all the way through z similar to 3.5 for the first time, though a more careful characterisation of the density field is ultimately required for confirmation.
Downloadable publication This is an electronic reprint of the original article. |  |
Funding information in the publication:
J.R.W. acknowledges that support for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. 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 Forschungsforderungsgesellschaft funded through BMIMI, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum fur Luft-und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d'Etudes Spatiales, the Fundacao para a Ciencia e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovacion 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 Swiss Space O ffice (SSO) at the State Secretariat for Education, Research, and Innovation (SERI), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid web site (www.euclid-ec.org/consortium/community/).
