Euclid preparation. TBD. Forecast impact of super-sample covariance on
3x2pt analysis with Euclid
Euclid Collaboration,D. Sciotti,S. Gouyou Beauchamps,V. F. Cardone,S. Camera,I. Tutusaus,F. Lacasa,A. Barreira,A. Gorce,M. Aubert,P. Baratta,R. E. Upham,M. Bonici,C. Carbone,S. Casas,S. Ilić,M. Martinelli,Z. Sakr,A. Schneider,R. Maoli,R. Scaramella,S. Escoffier,W. Gillard,N. Aghanim,A. Amara,S. Andreon,N. Auricchio,M. Baldi,S. Bardelli,D. Bonino,E. Branchini,M. Brescia,J. Brinchmann,V. Capobianco,J. Carretero,F. J. Castander,M. Castellano,S. Cavuoti,A. Cimatti,R. Cledassou,G. Congedo,C. J. Conselice,L. Conversi,Y. Copin,L. Corcione,F. Courbin,H. M. Courtois,M. Cropper,A. Da Silva,H. Degaudenzi,J. Dinis,F. Dubath,X. Dupac,S. Dusini,M. Farina,S. Farrens,P. Fosalba,M. Frailis,E. Franceschi,M. Fumana,S. Galeotta,B. Garilli,B. Gillis,C. Giocoli,A. Grazian,F. Grupp,L. Guzzo,S. V. H. Haugan,W. Holmes,I. Hook,F. Hormuth,A. Hornstrup,P. Hudelot,K. Jahnke,B. Joachimi,E. Keihänen,S. Kermiche,A. Kiessling,M. Kunz,H. Kurki-Suonio,P. B. Lilje,V. Lindholm,I. Lloro,D. Maino,O. Mansutti,O. Marggraf,K. Markovic,N. Martinet,F. Marulli,R. Massey,S. Maurogordato,E. Medinaceli,S. Mei,Y. Mellier,M. Meneghetti,G. Meylan,M. Moresco,L. Moscardini,E. Munari,S. -M. Niemi,C. Padilla,S. Paltani,F. Pasian,K. Pedersen,V. Pettorino,S. Pires,G. Polenta,M. Poncet,L. A. Popa,F. Raison,R. Rebolo,A. Renzi,J. Rhodes,G. Riccio,E. Romelli,M. Roncarelli,R. Saglia,D. Sapone,B. Sartoris,M. Schirmer,P. Schneider,A. Secroun,G. Seidel,S. Serrano,C. Sirignano,G. Sirri,L. Stanco,J. -L. Starck,P. Tallada-Crespí,A. N. Taylor,I. Tereno,R. Toledo-Moreo,F. Torradeflot,E. A. Valentijn,L. Valenziano,T. Vassallo,A. Veropalumbo,Y. Wang,J. Weller,A. Zacchei,G. Zamorani,J. Zoubian,E. Zucca,A. Biviano,A. Boucaud,E. Bozzo,C. Colodro-Conde,D. Di Ferdinando,R. Farinelli,J. Graciá-Carpio,N. Mauri,C. Neissner,V. Scottez,M. Tenti,Y. Akrami,V. Allevato,C. Baccigalupi,M. Ballardini,F. Bernardeau,A. Blanchard,S. Borgani,A. S. Borlaff,C. Burigana,R. Cabanac,A. Cappi,C. S. Carvalho,G. Castignani,T. Castro,G. Ca\ {n}as-Herrera,K. C. Chambers,A. R. Cooray,J. Coupon,A. Díaz-Sánchez,S. Davini,G. De Lucia,G. Desprez,S. Di Domizio,J. A. Escartin Vigo,I. Ferrero,F. Finelli,L. Gabarra,K. Ganga,J. Garcia-Bellido,E. Gaztanaga,F. Giacomini,G. Gozaliasl,H. Hildebrandt,J. Jacobson,J. J. E. Kajava,V. Kansal,C. C. Kirkpatrick,L. Legrand,A. Loureiro,J. Macias-Perez,M. Magliocchetti,G. Mainetti,C. J. A. P. Martins,S. Matthew,L. Maurin,R. B. Metcalf,M. Migliaccio,P. Monaco,G. Morgante,S. Nadathur,A. A. Nucita,M. Pöntinen,L. Patrizii,V. Popa,C. Porciani,D. Potter,A. Pourtsidou,A. G. Sánchez,E. Sefusatti,M. Sereno,P. Simon,A. Spurio Mancini,J. Stadel,J. Steinwagner,R. Teyssier,S. Toft,M. Tucci,C. Valieri,J. Valiviita,M. Viel
arXiv (Cornell University)（2023）
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摘要
Deviations from Gaussianity in the distribution of the fields probed by large-scale structure surveys generate additional terms in the data covariance matrix, increasing the uncertainties in the measurement of the cosmological parameters. Super-sample covariance (SSC) is among the largest of these non-Gaussian contributions, with the potential to significantly degrade constraints on some of the parameters of the cosmological model under study -- especially for weak lensing cosmic shear. We compute and validate the impact of SSC on the forecast uncertainties on the cosmological parameters for the Euclid photometric survey, obtained with a Fisher matrix analysis, both considering the Gaussian covariance alone and adding the SSC term -- computed through the public code PySSC. The photometric probes are considered in isolation and combined in the `3$\times$2pt' analysis. We find the SSC impact to be non-negligible -- halving the Figure of Merit of the dark energy parameters ($w_0$, $w_a$) in the 3$\times$2pt case and substantially increasing the uncertainties on $\Omega_{{\rm m},0}, w_0$, and $\sigma_8$ for cosmic shear; photometric galaxy clustering, on the other hand, is less affected due to the lower probe response. The relative impact of SSC does not show significant changes under variations of the redshift binning scheme, while it is smaller for weak lensing when marginalising over the multiplicative shear bias nuisance parameters, which also leads to poorer constraints on the cosmological parameters. Finally, we explore how the use of prior information on the shear and galaxy bias changes the SSC impact. Improving shear bias priors does not have a significant impact, while galaxy bias must be calibrated to sub-percent level to increase the Figure of Merit by the large amount needed to achieve the value when SSC is not included.
