Accès ouvert déclaré
2025
preprint
Euclid preparation. Establishing the quality of the 2D reconstruction of the filaments of the cosmic web with DisPerSE using Euclid photometric redshifts
Nicola Malavasi, Florian Sarron, Ulrike Kuchner, C. Laigle, Katarina Kraljic, P. Jablonka, Michael L. Balogh, S. Bardelli, M Bolzonella, J. Brinchmann, G. De Lucia, Fabio Fontanot, Michaela Hirschmann, Y Kang, M. Magliocchetti, T. Moutard, Marta Spinelli, L. Wang, Lang Xie, Eleni Tsaprazi, O Cucciati, G. Zamorani, M de Petris, Esra Bülbül, Rien van de Weygaert, N. Aghanim, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, Marco Baldi, A. Biviano, E. Branchini, M. Brescia, S. Camera, G Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, Santiago Casas, M Castellano, G Castignani, S Cavuoti, G. Congedo, L. Conversi, Y. Copin, F Courbin, M. Cropper, A. Da Silva, H. Degaudenzi, S. de la Torre, J. Dinis, H. Dole, F. Dubath, X Dupac, S Dusini, A. Ealet, S. Escoffier, M. Farina, S. Farrens, F Faustini, S. Ferriol, F. Finelli⋆, S. Fotopoulou, M. Frailis, E. Franceschi, S. Galeotta, K George, W. Gillard, B. Gillis, C. Giocoli, P Gómez-Álvarez, J. Graciá‐Carpio, A. Grazian, F. Grupp, L. Guzzo, W. A. Holmes, I. Hook, F. Hormuth, A. Hornstrup, P. Hudelot, S. Ilić, K. Jahnkę, M Jhabvala, Benjamin Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, M. Kilbinger, B. Kubik, M Kümmel, M. Kunz, H. Kurki‐Suonio, S. Ligori, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E Maiorano, O. Mansutti, S Marcin, O. Marggraf, K. Markovič, 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, M. Moresco, L. Moscardini, S Mourre, C Neissner, S. Paltani, F. Pasian, K Pedersen, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. Pozzetti, F. Raison, R. Rébolo, A Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, R. P. Saglia, Z. Sakr, D. Sapone, B. Sartoris, M Schirmer, P. C. Schneider, T. Schrabback, M. Scodeggio, A. Secroun, E. Sefusatti, G. Seidel, S. Serrano, Pardis Simon, C. Sirignano, G. Sirri, A. Spurio Mancini, L. Stanco, J. Steinwagner, P. Tallada-Crespí, I. Tereno, Sune Toft, R. Toledo-Moreo, F Torradeflot, A. Tsyganov, I. Tutusaus, L. Valenziano, J. Väliviita, T. Vassallo, A Veropalumbo, Yan Wang, J. Weller, E Zucca, E. Bozzo, C. Burigana, M. Calabrese, D. Di Ferdinando, L. Gabarra, S Matthew, N. Mauri, A Pezzotta, M. Pöntinen, C Porciani, V Scottez, M. Tenti, Matteo Viel, M. Wiesmann, Y. Akrami, V. Allevato, S Anselmi, M. Archidiacono, F. Atrio‐Barandela, A. Balaguera-Antolínez, M. Ballardini, Christophe Benoıst, Daniele Bertacca, M. Béthermin, Alain Blanchard, L Blot, H. Böhringer, S. Borgani, S Bruton, R Cabanac, Anthony Calabro, B. Camacho Quevedo, A. Cappi, F Caro, T. Castro, F Cogato, S. Contarini, T. Contini, S. Davini, F. De Paolis, G. Desprez, A. Díaz‐Sánchez, S. Di Domizio, A Finoguenov, A. Fontana, K. Ganga, J. García-Bellido, E. Gaztañaga, F. Giacomini, F. Gianotti, G. Gozaliasl, M Guidi, A Hall, Shoubaneh Hemmati, C. Hernández-Monteagudo, H Hildebrandt, J Hjorth, A. Jiménez Muñoz, V. Kansal, D Karagiannis, Sergey Kruk, M. Lattanzi, S. Lee, L. Legrand, M Lembo, J Lesgourgues, A. Loureiro, J. F. Macías–Pérez, G. Maggio, F. Mannucci, J Martín-Fleitas, L. Maurin, M Miluzio, Pierluigi Monaco, Claudio Moretti, G. Morgante, Krishna Naidoo, A Navarro-Alsina, Savvas Nesseris, K. Paterson, L. Patrizii, A Pisani, V. Popa, D. Potter, I Risso, M Sahlén, E Sarpa, A. Schneider, D Sciotti, Elena Sellentin, M. Sereno, A. Silvestri, K Tanidis, Chunhui Tao, G. Testera, R Teyssier, Sébastien Tosi, A. Troja, M Tucci, C Valieri, D. Vergani, G Verza
0Citations signalées, ce qui n’est pas une note de qualité
28Institutions déclarées
1Pays d’affiliation déclarés
Rattachement africain : fr.
Niveau de preuve : code pays fourni par la source.
Le résumé fourni par la source
Cosmic filaments are prominent structures of the matter distribution of the Universe. Modern detection algorithms are an efficient way to identify filaments in large-scale observational surveys of galaxies. Many of these methods were originally designed to work with simulations and/or well-sampled spectroscopic surveys. When spectroscopic redshifts are not available, the filaments of the cosmic web can be detected in projection using photometric redshifts in slices along the Line of Sight, which enable the exploration of larger cosmic volumes. However, this comes at the expense of a lower redshift precision. It is therefore crucial to assess the differences between filaments extracted from exact redshifts and from photometric redshifts for a specific survey. We apply this analysis to capture the uncertainties and biases of filament extractions introduced by using the photometric sample of the Euclid Wide Survey. The question that we address in this work is how can we compare two filament samples derived with redshifts of different precisions in the Euclid Wide Survey context. We apply the cosmic web detection algorithm DisPerSE, in the redshift range $0.1 \leq z \leq 0.5$, to the GAlaxy Evolution and Assembly (GAEA) simulated galaxy sample which reproduces several characteristics of the Euclid Wide Survey. We develop a method to compare skeletons derived from photometric redshifts to those derived from true galaxy positions. This method expands the commonly used measure of distance between filaments to include geometrical (angles between filaments) and astrophysical considerations (galaxy mass gradients and connectivity-mass relations). We assess whether this approach strengthens our ability to correctly identify filaments in very large surveys such as the Euclid Wide Survey. [abridged]
Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.
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Les sujets associés
Advanced Theoretical and Applied Studies in Material Sciences and GeometryAstronomy and Astrophysical Research