Euclid preparation. XXXIX. The effect of baryons on the Halo Mass Function

/ Authors

Euclid Collaboration T. Castro, S. Borgani, M. Costanzi, J. Dakin, K. Dolag, A. Fumagalli, A. Ragagnin, A. Saro, A. Brun, N. Aghanim

and 490 more authors

A. Amara, S. Andreon, N. Auricchio, M. Baldi, S. Bardelli, C. Bodendorf, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, S. Cavuoti, A. Cimatti, G. Congedo, C. Conselice, L. Conversi, Y. Copin, L. Corcione, F. Courbin, H. Courtois, M. Cropper, A. Silva, H. Degaudenzi, A. Giorgio, J. Dinis, F. Dubath, C. Duncan, X. Dupac, M. Farina, S. Farrens, S. Ferriol, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, B. Gillis, C. Giocoli, A. Grazian, F. Grupp, S. Haugan, W. Holmes, F. Hormuth, A. Hornstrup, K. Jahnke, E. Keihanen, S. Kermiche, A. Kiessling, M. Kilbinger, B. Kubik, M. Kunz, H. Kurki-Suonio, S. Ligori, P. Lilje, V. Lindholm, I. Lloro, E. Maiorano, O. Mansutti, O. Marggraf, K. Markovič, N. Martinet, F. Marulli, R. Massey, S. Maurogordato, E. Medinaceli, M. Meneghetti, E. Merlin, G. Meylan, Michele Moresco, L. Moscardini, E. Munari, S. Niemi, C. Padilla, S. Paltani, F. Pasian, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. Starck, P. Tallada-Cresp'i, A. Taylor, I. Tereno, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. Valentijn, L. Valenziano, T. Vassallo, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, J. Zoubian, E. Zucca, A. Biviano, E. Bozzo, C. Cerna, C. Colodro-Conde, D. Ferdinando, N. Mauri, C. Neissner, Z. Sakr, V. Scottez, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, S. Anselmi, C. Baccigalupi, M. Ballardini, A. Borlaff, S. Bruton, C. Burigana, R. Cabanac, A. Cappi, C. Carvalho, G. Castignani, G. C. nas-Herrera, K. Chambers, A. Cooray, J. Coupon, O. Cucciati, A. D'iaz-S'anchez, S. Davini, S. D. Torre, G. Lucia, G. Desprez, S. Domizio, H. Dole, S. Escoffier, I. Ferrero, F. Finelli, L. Gabarra, K. Ganga, J. García-Bellido, F. Giacomini, G. Gozaliasl, H. Hildebrandt, S. Ili'c, A. J. M. noz, J. Kajava, Vanshika Kansal, C. Kirkpatrick, L. Legrand, A. Loureiro, J. Macías-Pérez, M. Magliocchetti, G. Mainetti, R. Maoli, M. Martinelli, C. Martins, S. Matthew, M. Maturi, L. Maurin, R. Metcalf, M. Migliaccio, P. Monaco, G. Morgante, S. Nadathur, L. Patrizii, A. Pezzotta, V. Popa, C. Porciani, D. Potter, M. Pontinen, P. Reimberg, P. Rocci, A. S'anchez, J. Schaye, A. Schneider, E. Sefusatti, M. Sereno, P. Simon, A. Mancini, J. Stadel, S. Stanford, J. Steinwagner, G. Testera, M. Tewes, R. Teyssier, S. Toft, S. Tosi, A. Troja, M. Tucci, J. Valiviita, D. Trieste, 11 ViaG.B.Tiepolo, 34127 Trieste, Italy, Infn, Sezione di Trieste, 2. ViaValerio, TS 34127Trieste, Ifpu, Institute for Fundamental Physics of the Universe, 2. viaBeirut, 34127 Trieste, I. -. C. N. D. R. I. H. P. Computing, Big Data e Quantum Computing, 2. ViaMagnanelli, Bologna, D. Astronomia, U. Trieste, 11 ViaTiepolo, 34127 Trieste, Institute for Computational Science, U. Zurich, Winterthurerstrasse 190, 8093 Zurich, Switzerland., Universitatssternwarte Munchen, F. Physik, Ludwig-Maximilians-Universitat Munchen, 1. Scheinerstrasse, 8. Munchen, Germany., I. Bologna, V. G. 933, 40129 Bologna, D. Bologna, V. G. 932, Laboratoire Univers et Th'eorie, Observatoire de Paris, Universit'e Psl, Universit'e de Paris Cit'e, Cnrs, 92190 Meudon, France, Universit'e Paris-Saclay, I. D. Spatiale, 91405, Orsay, Institute of Cosmology, Gravitation, U. Portsmouth, PO1 3FX, Uk, Inaf Brera, 28 ViaBrera, 20133 Milano, D. Astronomia, U. Bologna, V. G. 932, I. Bologna, 62 vialeBertiPichat, 40129 Bologna, M. F. P. Physics, 1. Giessenbachstr., 85748 Garching, I. Torino, 20 viaOsservatorio, 1. P. Torinese, D. Fisica, 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. Naples, I. D. A. E. C. D. Espacco, U. Porto, Caup, Rua das Estrelas, P. Porto, Portugal, U. Torino, 1. ViaP.Giuria, 10125 Torino, I. Torino, Inaf-Iasf Milano, 12 ViaAlfonsoCorti, 20133 Milano, Institut de F'isica d'Altes Energies, T. Z. F. O. Science, Technology, Campus Uab, 08193 Bellaterra, Spain., Port d'Informaci'o Cient'ifica, C. Sn, I. F. Physics, Cosmology, Rwth Aachen University, 52056 Aachen, I. Roma, 33 viaFrascati, 00078 Monte Porzio Catone, Institute for Astronomy, U. Edinburgh, R. Observatory, B. Hill, Edinburgh EH9 3HJ, J. B. C. F. Astrophysics, D. Physics, Astronomy, U. Manchester, Oxford Road, M13 9PL, European Space AgencyESRIN, 1. LargoGalileoGalilei, 00044 Frascati, Roma, Esacesa, Camino Bajo de Castillo, Sn, Urb. Villafranca del Castillo, 28692 Villanueva de la Canada, Madrid, U. Lyon, 1. UnivClaudeBernardLyon, CNRSIN2p3, I. Lyon, Umr 5822, 69622 Villeurbanne, I. O. Physics, Laboratory of Astrophysics, E. P. F. Lausanne, Observatoire de Sauverny, 1290 Versoix, 1. UCBLyon, Iuf, 4. R. E. Fermi, Mullard Space Science Laboratory, U. London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, Departament de F'isica, F. Ciencias, Universidade Tecnica de Lisboa, C8 Edif'icio, C. Grande, P. Lisboa, 1049-001 Lisboa, D. O. Astronomy, U. Geneva, 16 ch.d'Ecogia, I. D. A. E. P. Spaziali, V. Cavaliere, 100, 00133 Roma, O. University, Keble Road, O. 3RH, Cea, Aim, 91191, Gif-sur-Yvette, Inaf - Padova, 5. Viadell'Osservatorio, 35131 Padova, University Observatory, F. O. Physics, Ludwig-Maximilians-Universitat, 1. Scheinerstr., 81679 Munich, I. Astrophysics, U. Oslo, P. O. B. 1. Blindern, 0315 Oslo, Norway., Jet propulsion Laboratory, C. I. O. Technology., 4800 Oak Grove Drive, Pasadena, Ca, 91109, Usa, von Hoerner Sulger GmbH, 8. Schlossplatz, 68723 Schwetzingen, T. Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark., Cosmic Dawn Center, M. Astronomie, 17 Konigstuhl, 69117 Heidelberg, H. I. O. Physics, 2. GustafHallstrominkatu, 0. Helsinki, Finland., A. Universit'e, Cppm, Marseille, U. Paris, 91191 Gif-sur-Yvette, U. Geneve, D'epartement de Physique Th'eorique, Centre for Theoretical Physics, 24 quai Ernest-Ansermet, 4. CH-1211Geneve, 64 P.O.Box, U. Helsinki, Helsinki, Nova Optical IR Instrumentation Group at Astron, 4. OudeHoogeveensedijk, 7991PD, Dwingeloo, The Netherlands., U. Bonn, Argelander Institut fur Astronomie, 71 AufdemHugel, 53121 Bonn, Cnes, Lam, Institute for Computational Cosmology, D. University, South Road, DH1 3LE, Universit'e Cote d'Azur, Observatoire Cote d'Azur, Laboratoire Lagrange, Bd de l'Observatoire, CS 34229, 4. 06304Nicecedex, European Space AgencyESTEC, 1. Keplerlaan, 2. Noordwijk, Astrophysique, Instrumentation et Mod'elisation Paris-Saclay, S. Center, Italian Space Agency, via del Politecnico snc, 00133 Roma, C. Toulouse, 14 Avenue Edouard Belin, 9. 31401ToulouseCedex, Institute of Space Science, Str. Atomistilor, nr. 409 Muagurele, Ilfov, 077125, România, Instituto de Astrof'isica de Canarias, C. V. L. sn, 38204, San Crist'obal de La Laguna, Tenerife, D. Astrof'isica, U. L. Laguna, 38206, L. Laguna, D. Galilei', U. Padova, 8. viaMarzolo, 35131 Padova, INFN-Padova, Fcfm, U. D. Chile, Blanco Encalada 2008, Santiago, Chile, U. Innsbruck, Institut fur Teilchenphysik

/ Abstract

The Euclid photometric survey of galaxy clusters stands as a powerful cosmological tool, with the capacity to significantly propel our understanding of the Universe. Despite being sub-dominant to dark matter and dark energy, the baryonic component in our Universe holds substantial influence over the structure and mass of galaxy clusters. This paper presents a novel model to precisely quantify the impact of baryons on galaxy cluster virial halo masses, using the baryon fraction within a cluster as proxy for their effect. Constructed on the premise of quasi-adiabaticity, the model includes two parameters calibrated using non-radiative cosmological hydrodynamical simulations and a single large-scale simulation from the Magneticum set, which includes the physical processes driving galaxy formation. As a main result of our analysis, we demonstrate that this model delivers a remarkable one percent relative accuracy in determining the virial dark matter-only equivalent mass of galaxy clusters, starting from the corresponding total cluster mass and baryon fraction measured in hydrodynamical simulations. Furthermore, we demonstrate that this result is robust against changes in cosmological parameters and against varying the numerical implementation of the sub-resolution physical processes included in the simulations. Our work substantiates previous claims about the impact of baryons on cluster cosmology studies. In particular, we show how neglecting these effects would lead to biased cosmological constraints for a Euclid-like cluster abundance analysis. Importantly, we demonstrate that uncertainties associated with our model, arising from baryonic corrections to cluster masses, are sub-dominant when compared to the precision with which mass-observable relations will be calibrated using Euclid, as well as our current understanding of the baryon fraction within galaxy clusters.