A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Euclid preparation : LXXVI. Simulating thousands of Euclid spectroscopic skies
Tekijät: Monaco, P.; Parimbelli, G.; Elkhashab, M. Y.; Salvalaggio, J.; Castro, T.; Lepinzan, M. D.; Sarpa, E.; Sefusatti, E.; Stanco, L.; Tornatore, L.; Addison, G. E.; Bruton, S.; Carbone, C.; Castander, F. J.; Carretero, J.; de la Torre, S.; Fosalba, P.; Lavaux, G.; Lee, S.; Markovic, K.; McCarthy, K. S.; Passalacqua, F.; Percival, W. J.; Risso, I.; Scarlata, C.; Tallada Crespí, P.; Viel, M.; Wang, Y.; Altieri, B.; Andreon, S.; Auricchio, N.; Baccigalupi, C.; Baldi, M.; Bardelli, S.; Battaglia, P.; Bernardeau, F.; Biviano, A.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Cañas Herrera, G.; Capobianco, V.; Cardone, V. F.; Casas, S.; Castellano, M.; Castignani, G.; Cavuoti, S.; 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.; Dubath, F.; Ducret, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.; Ealet, A.; Escoffier, S.; Farina, M.; Farinelli, R.; Farrens, S.; Ferriol, S.; Finelli, F.; Fourmanoit, N.; Frailis, M.; Franceschi, E.; Fumana, M.; Galeotta, S.; George, K.; Gillis, B.; Giocoli, C.; Gracia Carpio, J.; Grazian, A.; Grupp, F.; Guzzo, L.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Hornstrup, A.; Jahnke, K.; Jhabvala, M.; Joachimi, B.; Keihänen, E.; Kermiche, S.; Kubik, B.; Kümmel, M.; Kunz, M.; Kurki Suonio, H.; Le Brun, A. M. C.; Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Medinaceli, E.; Mei, S.; Melchior, M.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mora, A.; Moresco, M.; Moscardini, L.; Munari, E.; Nakajima, R.; Neissner, C.; Niemi, S. M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.; Popa, L. A.; Pozzetti, L.; Raison, F.; Renzi, A.; Rhodes, J.; Riccio, G.; Rizzo, F.; Romelli, E.; Roncarelli, M.; Saglia, R.; Sakr, Z.; Sánchez, A. G.; Sapone, D.; Sartoris, B.; Schneider, P.; Schrabback, T.; Scodeggio, M.; Secroun, A.; Seidel, G.; Seiffert, M.; Serrano, S.; Simon, P.; Sirignano, C.; Sirri, G.; Steinwagner, J.; Tavagnacco, D.; Taylor, A. N.; Tereno, I.; Tessore, N.; Toft, S.; Toledo Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Verdoes Kleijn, G.; Veropalumbo, A.; Weller, J.; Zamorani, G.; Zucca, E.; Allevato, V.; Ballardini, M.; Burigana, C.; Cabanac, R.; Calabrese, M.; Cappi, A.; Di Ferdinando, D.; Escartin Vigo, J. A.; Fabbian, G.; Gabarra, L.; Martín Fleitas, J.; Matthew, S.; Mauri, N.; Metcalf, R. B.; Pezzotta, A.; Pöntinen, M.; Porciani, C.; Scottez, V.; Sereno, M.; Tenti, M.; Wiesmann, M.; Akrami, Y.; Alvi, S.; Andika, I. T.; Anselmi, S.; Archidiacono, M.; Atrio Barandela, F.; Avila, S.; Balaguera Antolinez, A.; Bergamini, P.; Bertacca, D.; Bethermin, M.; Blanchard, A.; Blot, L.; Borgani, S.; Brown, M. L.; Calabro, A.; Camacho Quevedo, B.; Caro, F.; Carvalho, C. S.; Cogato, F.; Conseil, S.; Contarini, S.; Cooray, A. R.; Cucciati, O.; Davini, S.; Desprez, G.; Díaz Sánchez, A.; Diaz, J. J.; Di Domizio, S.; Diego, J. M.; Enia, A.; Fang, Y.; Ferrari, A. G.; Finoguenov, A.; Fontanot, F.; Franco, A.; Ganga, K.; García Bellido, J.; Gasparetto, T.; Gautard, V.; Gaztanaga, E.; Giacomini, F.; Gianotti, F.; Gozaliasl, G.; Guidi, M.; Gutierrez, C. M.; Hall, A.; Hemmati, S.; Hernández Monteagudo, C.; Hildebrandt, H.; Hjorth, J.; Joudaki, S.; Kajava, J. J. E.; Kang, Y.; Kansal, V.; Karagiannis, D.; Kiiveri, K.; Kirkpatrick, C. C.; Kruk, S.; Le Brun, V.; Le Graet, J.; Legrand, L.; Lembo, M.; Lepori, F.; Leroy, G.; Lesci, G. F.; Lesgourgues, J.; Leuzzi, L.; Liaudat, T. I.; Macias Perez, J.; Maggio, G.; Magliocchetti, M.; Mancini, C.; Mannucci, F.; Maoli, R.; Martins, C. J. A. P.; Maurin, L.; Miluzio, M.; Montoro, A.; Moretti, C.; Morgante, G.; Nadathur, S.; Naidoo, K.; Navarro Alsina, A.; Nesseris, S.; Paterson, K.; Pisani, A.; Potter, D.; Quai, S.; Radovich, M.; Rodighiero, G.; Sacquegna, S.; Sahlén, M.; Sanders, D. B.; Sciotti, D.; Sellentin, E.; Smith, L. C.; Sorce, J. G.; Tanidis, K.; Tao, C.; Testera, G.; Teyssier, R.; Tosi, S.; Troja, A.; Tucci, M.; Valieri, C.; Venhola, A.; Vernizzi, F.; Verza, G.; Vielzeuf, P.; Walton, N. A.
Kustantaja: EDP Sciences
Julkaisuvuosi: 2025
Lehti: Astronomy and Astrophysics
Artikkelin numero: A306
Vuosikerta: 704
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202556459
Julkaisun avoimuus kirjaamishetkellä: Avoimesti saatavilla
Julkaisukanavan avoimuus : Kokonaan avoin julkaisukanava
Verkko-osoite: https://doi.org/10.1051/0004-6361/202556459
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/508409834
Rinnakkaistallenteen lisenssi: CC BY
Rinnakkaistallennetun julkaisun versio: Kustantajan versio
We present two extensive sets of 3500+1000 simulations of dark matter haloes on the past light cone and two corresponding sets of simulated (mock) galaxy catalogues that represent the spectroscopic sample of Euclid. The simulations were produced with the latest version of the code Pinocchio and provide the largest public set of simulated skies. The mock galaxy catalogues were obtained by populating haloes with galaxies using an halo occupation distribution (HOD) model extracted from the Flagship galaxy catalogue provided by Euclid Collaboration. The Geppetto set of 3500 simulated skies was obtained by tiling a 1.2 h−1 Gpc box to cover a light cone whose sky footprint is a circle with a radius of 30° for an area of 2763 deg2 and a minimum halo mass of 1.5 × 1011h−1 M⊙. The relatively small size of the box means that this set is unsuitable for measuring very large scales. The EuclidLargeBox set consists of 1000 simulations of 3.38 h−1 Gpc and has the same mass resolution and a footprint that covers half of the sky. It excludes the Milky Way zone of avoidance. From this, we produced a set of 1000 EuclidLargeMocks on the 30° radius footprint, whose comoving volume is fully contained in the simulation box. We validated the two sets of catalogues by analysing number densities, power spectra, and two-point correlation functions to show that the Flagship spectroscopic catalogue is consistent with being one of the realisations of the simulated sets. We noted small deviations, however, that are limited to the quadrupole at k > 0.2 h Mpc−1. We infer the cosmological parameters from these catalogues and demonstrate that using one realisation of EuclidLargeMocks in place of the Flagship mock produces the same posteriors to within the expected shift given by the sample variance. These simulated skies will be used for the galaxy clustering analysis of the Euclid Data Release 1 (DR1), and an even larger set of simulations is planned for the next releases.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
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 web site (www.euclid-ec.org). This paper has been supported by: the Fondazione ICSC, Spoke 3 Astrophysics and Cosmos Observations. National Recovery and Resilience Plan (Piano Nazionale di Ripresa e Resilienza, PNRR) Project ID CN_00000013 ‘Italian Research Center on High-Performance Computing, Big Data and Quantum Computing’ funded by MUR Missione 4 Componente 2 Investimento 1.4: Potenziamento strutture di ricerca e creazione di ‘campioni nazionali di R&S (M4C2-19 )’ – Next Generation EU (NGEU); by the National Recovery and Resilience Plan (NRRP), Mission 4, Component 2, Investment 1.1, Call for tender No. 1409 published on 14.9.2022 by the Italian Ministry of University and Research (MUR), funded by the European Union – NextGenerationEU– Project Title ‘Space-based cosmology with Euclid: the role of High-Performance Computing’ – CUP J53D23019100001 – Grant Assignment Decree No. 962 adopted on 30/06/2023 by the Italian Ministry of Ministry of University and Research (MUR). Computing time was obtained from CINECA ISCRA-B grant ‘EuMocks’, from INFN and from the Pleiadi system of INAF. (Taffoni et al. 2020; Bertocco et al. 2020)
