Euclid preparation. Far-infrared predictions for Euclid galaxy catalogues: cluster, protocluster, and field

作者：Euclid Collaboration A. Parmar, D. L. Clements, M. Bolzonella, O. Cucciati, L. Pozzetti, H. Dannerbauer, G. Castignani, S. Serjeant, L. Wang, R. Hill, D. Scott, J. Sorce, M. Magliocchetti, F. Pace, T. Thai, N. Aghanim, B. Altieri, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, S. Bardelli, A. Biviano, W. Bon, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, F. Courbin, H. Courtois, A. Silva, H. Degaudenzi, G. Lucia, H. Dole, M. Douspis, F. Dubath, F. Ducret, C. Duncan, X. Dupac, S. Escoffier, M. Farina, R. Farinelli, S. Ferriol, F. Finelli, S. Fotopoulou, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, J. Graciá-Carpio, A. Grazian, F. Grupp, S. Haugan, W. Holmes, F. Hormuth, A. Hornstrup, K. Jahnke, M. Jhabvala, E. Keihanen, S. Kermiche, A. Kiessling, B. Kubik, M. Kummel, M. Kunz, H. Kurki-Suonio, A. Brun, S. Ligori, P. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, S. Marcin, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R. Massey, S. Maurogordato, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, Michele Moresco, L. Moscardini, R. Nakajima, C. Neißner, S. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. Popa, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, A. S'anchez, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, E. Sefusatti, G. Seidel, M. Seiffert, S. Serrano, P. Simon, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Cresp'i, A. Taylor, H. Teplitz, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, A. Veropalumbo, Y. Wang, J. Weller, G. Zamorani, F. Zerbi, E. Zucca, V. Allevato, M. Ballardini, E. Bozzo, C. Burigana, R. Cabanac, A. Cappi, D. D. Ferdinando, J. Vigo, L. Gabarra, W. Hartley, S. Matthew, M. Maturi, N. Mauri, R. B. Metcalf, A. Pezzotta, M. Pontinen, C. Porciani, I. Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, P. Bergamini, D. Bertacca, M. Bethermin, A. Blanchard, L. Blot, H. Bohringer, M. Bonici, S. Borgani, M. L. Brown, S. Bruton, A. Calabrò, B. Quevedo, F. Caro, C. Carvalho, T. Castro, F. Cogato, S. Conseil, A. Cooray, S. Davini, G. Desprez, A. D'iaz-S'anchez, J. J. Diaz, S. Domizio, J. M. Diego, P. Dimauro, M. Y. Elkhashab, A. Enia, Y. Fang, A. Ferrari, A. Finoguenov, A. Fontana, F. Fontanot, A. Franco, K. Ganga, J. Garc'ia-Bellido, T. Gasparetto, V. Gautard, E. Gaztañaga, F. Giacomini, F. Gianotti, G. Gozaliasl, M. Guidi, C. Gutierrez, A. Hall, S. Hemmati, H. Hildebrandt, J. Hjorth, J. Kajava, Y. Kang, Vanshika Kansal, D. Karagiannis, K. Kiiveri, J. Kim, C. Kirkpatrick, S. Kruk, J. L. Graet, L. Legrand, M. Lembo, F. Lepori, G. Leroy, G. Lesci, J. Lesgourgues, T. Liaudat, A. Loureiro, J. Macías-Pérez, G. Maggio, C. Mancini, F. Mannucci, R. Maoli, C. Martins, L. Maurin, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, K. Naidoo, P. Natoli, A. Navarro-Alsina, S. Nesseris, D. Paoletti, F. Passalacqua, K. Paterson, L. Patrizii, A. Pisani, D. Potter, S. Quai, M. Radovich, P. Rocci, G. Rodighiero, S. Sacquegna, M. Sahl'en, D. Sanders, E. Sarpa, A. Schneider, D. Sciotti, E. Sellentin, F. Shankar, L. Smith, K. Tanidis, C. Tao, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N. A. Group, B. Laboratory, I. -. London, London SW7 2AZ, Uk, I. Bologna, V. G. 933, 40129 Bologna, Italy, Instituto de Astrof'isica de Canarias, E. Laguna, U. L. Laguna, Dpto. Astrof'i sica, E. Laguna, Tenerife, Spain, School of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, Sron Netherlands Institute for Space Research, 12 Landleven, AD 9747, Groningen, The Netherlands, K. Institute, U. Groningen, PO Box 800, 9700 AV Groningen, D. Physics, Astronomy, U. Columbia, Vancouver, BC V6T 1Z1, Canada, U. Lille, Cnrs, Centrale Lille, U. 9. CRIStAL, 59000 Lille, France, Universit'e Paris-Saclay, I. D. Spatiale, 91405, Orsay, I. D. A. E. P. Spaziali, V. Cavaliere, 100, 00133 Roma, D. Fisica, U. Torino, 1. ViaP.Giuria, 10125 Torino, I. Torino, I. A. D. Torino, 20 viaOsservatorio, 1. P. Torinese, National Space Development Agency of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan., Esacesa, Camino Bajo de Castillo, Sn, Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Inaf Brera, 28 ViaBrera, 20133 Milano, Ifpu, Institute for Fundamental Physics of the Universe, 2. viaBeirut, 34127 Trieste, Inaf - Trieste, 11 viaG.B.Tiepolo, 34127 Trieste, Infn, Sezione di Trieste, 2. ViaValerio, TS 34127Trieste, Sissa, International School for Advanced Studies, Via Bonomea 265, TS 34136Trieste, D. Astronomia, U. Bologna, V. G. 932, I. Bologna, 62 vialeBertiPichat, 40129 Bologna, A. Universit'e, Cnes, Lam, Marseille, U. Genova, 33 viaDodecaneso, 16146, Genova, I. Genova, Department of PhysicsE. Pancini, U. Federico, 6. ViaCinthia, 80126, Napoli, I. -. Capodimonte, 16 viaMoiariello, 80131 Napoli, I. D. A. E. C. D. Espacco, U. Porto, Caup, Rua das Estrelas, P. Porto, Portugal, Faculdade de Ciencias da Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, E. Observatory, Garching, Germany, European Space AgencyESTEC, 1. Keplerlaan, 2. Noordwijk, Institute Lorentz, Leiden University, 2. NielsBohrweg, 2333 CA Leiden, L. Observatory, 55 Einsteinweg, 2333 CC Leiden, Inaf-Iasf Milano, 12 ViaAlfonsoCorti, 20133 Milano, Centro de Investigaciones Energ'eticas, Medioambientales y Tecnol'ogicas, 40 AvenidaComplutense, 28014 Madrid, Port d'Informaci'o Cient'ifica, Campus Uab, C. sn, 08193 Bellaterra, I. F. Physics, Cosmology, Rwth Aachen University, 52056 Aachen, Inafiasf Roma, 33 viaFrascati, 00078 Monte Porzio Catone, I. Naples, D. Bologna, Institute for Astronomy, U. Edinburgh, R. Observatory, B. Hill, Edinburgh EH9 3HJ, J. B. C. F. Astrophysics, U. Manchester, Oxford Road, M13 9PL, European Space AgencyESRIN, 1. LargoGalileoGalilei, 00044 Frascati, Roma, 1. Universit'eClaudeBernardLyon, CNRSIN2p3, I. Lyon, Umr 5822, Villeurbanne, F-69100, Institut de Ci'encies del Cosmos, U. Barcelona, 1. Mart'iiFranques, 08193 Barcelona, I. C. D. R. I. E. Avanccats, 23 PasseigdeLlu'isCompanys, 08193 Barcelona, 1. UCBLyon, Iuf, 4. R. E. Fermi, 69622 Villeurbanne, Departament de F'isica, F. Ciencias, Universidade T'ecnica de Lisboa, C8 Edif'icio, C. Grande, P. Lisboa, 1049-001 Lisboa, D. O. Astronomy, U. Geneva, 16 ch.d'Ecogia, 1290 Versoix, Switzerland., Cppm, INFN-Bologna, 46 ViaIrnerio, 40129 Bologna, S. O. Physics, H. W. P. Laboratory, U. Bristol, Tyndall Avenue, Bristol · 年份：2026 · 研究领域：Physics

The MAMBO mock galaxy catalogue, based on the Millennium Simulation with empirically assigned galaxy properties, provides predictions of FIR fluxes and physical parameters of Euclid-detectable galaxies. Predicted FIR flux distributions confirm that only the brightest Euclid sources will be detectable in existing FIR surveys. We employ stacking to measure the mean dust properties as a function of stellar mass and redshift. We find dust temperatures and infrared luminosities increase with redshift across all mass bins, while dust masses remain roughly constant. FIR number counts from MAMBO show overall good agreement with observations, and the total infrared luminosity function reproduces published estimates across most redshift ranges, extending to z~10. Comparing the Euclid Wide and Deep Surveys, we find that the EDS recovers the total IRLF to fainter luminosities and higher redshifts (up to z~6 in $I_E$), although its detectability falls below 80% at z>4, whereas the EWS becomes strongly incomplete beyond z~2. We also examine the dependence of the IRLF on environment. Schechter fits indicate that the faint-end slope $\alpha$ flattens with redshift for cluster and protocluster galaxies, while remaining approximately constant for field populations. Imposing additional detection limits from Herschel-PACS and SPIRE shows that only the most luminous ($L_{IR}$>$10^{12.5}$ $L_{\odot}$) galaxies remain detectable at z~4, but the limited MAMBO area (3.14$deg^2$) is inadequate for sta...