Euclid preparation LIV. Sensitivity to neutrino parameters
Archidiacono, M.; Lesgourgues, J.; Casas, S.; Pamuk, S.; Schoneberg, N.; Sakr, Z.; Parimbelli, G.; Schoeneider, A.; Peters, F. Hervas; Pace, F.; Sabarish, V. M.; Costanzi, M.; Camera, S.; Carbone, C.; Clesse, S.; Frusciante, N.; Fumagalli, A.; Monaco, P.; Scott, D.; Viel, M.; Amara, A.; Andreon, S.; Auricchio, N.; Baldi, M.; Bardelli, S.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Capobianco, V.; Cardone, V. F.; Carretero, J.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Courbin, F.; Courtois, H. M.; Da Silva, A.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.; Ealet, A.; Farina, M.; Farrens, S.; Ferriol, S.; Frailis, M.; Franceschi, E.; Galeotta, S.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Guzzo, L.; Haugan, S. V. H.; Hoekstra, H.; Hormuth, F.; Hornstrup, A.; Jahnke, K.; Joachimi, B.; Keihanen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kubik, B.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinet, N.; Marulli, F.; Massey, R.; Maurogordato, S.; McCracken, H. J.; Medinaceli, E.; Mei, S.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. -M.; Nightingale, J. W.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.; 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.; Sapone, D.; Sartoris, B.; Scaramella, R.; Schirmer, M.; Schneider, P.; Schrabback, T.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.; Tallada-Crespi, P.; Taylor, A. N.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valenziano, L.; Vassallo, T.; Veropalumbo, A.; Wang, Y.; Weller, J.; Zamorani, G.; Zoubian, J.; Zucca, E.; Biviano, A.; Boucaud, A.; Bozzo, E.; Burigana, C.; Calabrese, M.; Colodro-Conde, C.; Crocce, M.; Fabbian, G.; Gracia-Carpio, J.; Mainetti, G.; Martinelli, M.; Mauri, N.; Neissner, C.; Scottez, V.; Tenti, M.; Wiesmann, M.; Akrami, Y.; Anselmi, S.; Baccigalupi, C.; Ballardini, M.; Bernardeau, F.; Bertacca, D.; Borgani, S.; Borsato, E.; Bruton, S.; Cabanac, R.; Cappi, A.; Carvalho, C. S.; Castignani, G.; Castro, T.; Canas-Herrera, G.; Chambers, K. C.; Contarini, S.; Cooray, A. R.; Coupon, J.; Davini, S.; de la Torre, S.; De Lucia, G.; Desprez, G.; Di Domizio, S.; Diaz-Sanchez, A.; Vigo, J. A. Escartin; Escoffier, S.; Ferreira, P. G.; Ferrero, I.; Finelli, F.; Gabarra, L.; Ganga, K.; Garcia-Bellido, J.; Gaztanaga, E.; Giacomini, F.; Gozaliasl, G.; Gregorio, A.; Hall, A.; Hildebrandt, H.; Ilic, S.; Kajava, J. J. E.; Kansal, V.; Karagiannis, D.; Kirkpatrick, C. C.; Legrand, L.; Loureiro, A.; Macias-Perez, J.; Maggio, G.; Magliocchetti, M.; Mannucci, F.; Maoli, R.; Martins, C. J. A. P.; Matthew, S.; Maurin, L.; Metcalf, R. B.; Migliaccio, M.; Morgante, G.; Nadathur, S.; Walton, Nicholas A.; Patrizii, L.; Pezzotta, A.; Pontinen, M.; Popa, V.; Porciani, C.; Potter, D.; Reimberg, P.; Risso, I.; Rocci, P. -F.; Sahlen, M.; Sanchez, A. G.; Sefusatti, E.; Sereno, M.; Simon, P.; Mancini, A. Spurio; Steinwagner, J.; Testera, G.; Tewes, M.; Teyssier, R.; Toft, S.; Tosi, S.; Troja, A.; Tucci, M.; Valieri, C.; Valiviita, J.; Vergani, D.; Verza, G.; Vielzeuf, P.; Euclid Collaboration
https://urn.fi/URN:NBN:fi-fe2025082786506
Tiivistelmä
Context. The Euclid mission of the European Space Agency will deliver weak gravitational lensing and galaxy clustering surveys that can be used to constrain the standard cosmological model and extensions thereof.
Aims. We present forecasts from the combination of the Euclid photometric galaxy surveys (weak lensing, galaxy clustering, and their crosscorrelations) and its spectroscopic redshift survey with respect to their sensitivity to cosmological parameters. We include the summed neutrino mass, Sigma m (v), and the e ffective number of relativistic species, N-e ff, in the standard Lambda alpha CDM scenario and in the dynamical dark energy (w (0) w(alpha)CDM) scenario.
Methods. We compared the accuracy of di fferent algorithms predicting the non-linear matter power spectrum for such models. We then validated several pipelines for Fisher matrix and Markov chain Monte Carlo (MCMC) forecasts, using di fferent theory codes, algorithms for numerical derivatives, and assumptions on the non-linear cut-o ff scale.
Results. The Euclid primary probes alone will reach a sensitivity of sigma(Sigma m (v) = 60 meV) = 56 meV in the Lambda CDM +Sigma m (v) model, whereas the combination with cosmic microwave background (CMB) data from Planck is expected to achieve sigma(Sigma m (v)) = 23 meV, o ffering evidence of a non-zero neutrino mass to at least the 2:6 sigma level. This could be pushed to a 4 sigma detection if future CMB data from LiteBIRD and CMB Stage-IV were included. In combination with Planck, Euclid will also deliver tight constraints on Delta N-e ff < 0:144 (95%CL) in the Lambda CDM +Sigma m (v)+N-e ff model or even Delta N-e ff < 0:063 when future CMB data are included. When floating the dark energy parameters, we find that the sensitivity to Ne ff remains stable, but for Sigma m (v), it gets degraded by up to a factor of 2, at most.
Conclusions. This work illustrates the complementarity among the Euclid spectroscopic and photometric surveys and among Euclid and CMB constraints. Euclid will o ffer great potential in measuring the neutrino mass and excluding well-motivated scenarios with additional relativistic particles.
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