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Euclid preparation: LIV. Sensitivity to neutrino parameters

Lookup NU author(s): Dr James Nightingale

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This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).


Abstract

© The Authors 2024.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 cross-correlations) and its spectroscopic redshift survey with respect to their sensitivity to cosmological parameters. We include the summed neutrino mass, Σmν, and the effective number of relativistic species, Neff, in the standard Λ CDM scenario and in the dynamical dark energy (w0waCDM) scenario. Methods. We compared the accuracy of different 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 different theory codes, algorithms for numerical derivatives, and assumptions on the non-linear cut-off scale. Results. The Euclid primary probes alone will reach a sensitivity of σ (Σmν = 60 meV) = 56 meV in the Λ CDM+Σmν model, whereas the combination with cosmic microwave background (CMB) data from Planck is expected to achieve σ (Σmν) = 23 meV, offering evidence of a non-zero neutrino mass to at least the 2.6 σ level. This could be pushed to a 4 σ detection if future CMB data from LiteBIRD and CMB Stage-IV were included. In combination with Planck, Euclid will also deliver tight constraints on Δ Neff < 0.144 (95%CL) in the Λ CDM+Σmν+Neff model or even Δ Neff < 0.063 when future CMB data are included. When floating the dark energy parameters, we find that the sensitivity to Neff remains stable, but for Σmν, 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 offer great potential in measuring the neutrino mass and excluding well-motivated scenarios with additional relativistic particles.


Publication metadata

Author(s): Archidiacono M, Lesgourgues J, Casas S, Pamuk S, Schoneberg N, Sakr Z, Parimbelli G, Schneider A, Hervas Peters F, Pace F, Sabarish VM, 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 VF, Carretero J, Castellano M, Cavuoti S, Cimatti A, Congedo G, Conselice CJ, Conversi L, Copin Y, Courbin F, Courtois HM, Da Silva A, Degaudenzi H, Douspis M, Dubath F, Duncan CAJ, 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 SVH, 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 PB, Lindholm V, Lloro I, Maino D, Maiorano E, Mansutti O, Marggraf O, Markovic K, Martinet N, Marulli F, Massey R, Maurogordato S, Mccracken HJ, Medinaceli E, Mei S, Mellier Y, Meneghetti M, Merlin E, Meylan G, Moresco M, Moscardini L, Munari E, Niemi S-M, Nightingale JW, Padilla C, Paltani S, Pasian F, Pedersen K, Percival WJ, Pettorino V, Pires S, Polenta G, Poncet M, Popa LA, 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 AN, 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 CS, Castignani G, Castro T, Canas-Herrera G, Chambers KC, Contarini S, Cooray AR, Coupon J, Davini S, De La Torre S, De Lucia G, Desprez G, Di Domizio S, Diaz-Sanchez A, Escartin Vigo JA, Escoffier S, Ferreira PG, 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 JJE, Kansal V, Karagiannis D, Kirkpatrick CC, Legrand L, Loureiro A, Macias-Perez J, Maggio G, Magliocchetti M, Mannucci F, Maoli R, Martins CJAP, Matthew S, Maurin L, Metcalf RB, Migliaccio M, Morgante G, Nadathur S, Walton NA, Patrizii L, Pezzotta A, Pontinen M, Popa V, Porciani C, Potter D, Reimberg P, Risso I, Rocci P-F, Sahlen M, Sanchez AG, Sefusatti E, Sereno M, Simon P, Spurio Mancini A, 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

Publication type: Article

Publication status: Published

Journal: Astronomy and Astrophysics

Year: 2025

Volume: 693

Print publication date: 01/01/2025

Online publication date: 03/01/2025

Acceptance date: 06/10/2024

Date deposited: 04/02/2025

ISSN (print): 0004-6361

ISSN (electronic): 1432-0746

Publisher: EDP Sciences

URL: https://doi.org/10.1051/0004-6361/202450859

DOI: 10.1051/0004-6361/202450859


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