pith. sign in

arxiv: 2104.05698 · v1 · pith:CFXGU55Hnew · submitted 2021-04-12 · 🌌 astro-ph.CO

Euclid preparation: XII. Optimizing the photometric sample of the Euclid survey for galaxy clustering and galaxy-galaxy lensing analyses

Euclid Collaboration: A. Pocino , I. Tutusaus , F.J. Castander , P. Fosalba , M. Crocce , A. Porredon , S. Camera , V. Cardone
show 151 more authors
S. Casas T. Kitching F. Lacasa M. Martinelli A. Pourtsidou Z. Sakr S. Andreon N. Auricchio C. Baccigalupi A. Balaguera-Antol\'inez M. Baldi A. Balestra S. Bardelli R. Bender A. Biviano C. Bodendorf D. Bonino A. Boucaud E. Bozzo E. Branchini M. Brescia J. Brinchmann C. Burigana R. Cabanac V. Capobianco A. Cappi C.S. Carvalho M. Castellano G. Castignani S. Cavuoti A. Cimatti R. Cledassou C. Colodro-Conde G. Congedo C.J. Conselice L. Conversi Y. Copin L. Corcione A. Costille J. Coupon H.M. Courtois M. Cropper J.-G. Cuby A. Da Silva S. de la Torre D. Di Ferdinando F. Dubath C. Duncan X. Dupac S. Dusini S. Farrens P.G. Ferreira I. Ferrero F. Finelli S. Fotopoulou M. Frailis E. Franceschi S. Galeotta B. Garilli W. Gillard B. Gillis C. Giocoli G. Gozaliasl J. Graci\'a-Carpio F. Grupp L. Guzzo W. Holmes F. Hormuth K. Jahnke E. Keihanen S. Kermiche A. Kiessling C.C. Kirkpatrick M. Kunz H. Kurki-Suonio S. Ligori P.B. Lilje I. Lloro D. Maino E. Maiorano O. Mansutti O. Marggraf N. Martinet F. Marulli R. Massey S. Maurogordato E. Medinaceli S. Mei M. Meneghetti R.Benton Metcalf G. Meylan M. Moresco B. Morin L. Moscardini E. Munari R. Nakajima C. Neissner R.C. Nichol S. Niemi J. Nightingale C. Padilla S. Paltani F. Pasian L. Patrizii K. Pedersen W.J. Percival V. Pettorino S. Pires G. Polenta M. Poncet L. Popa D. Potter L. Pozzetti F. Raison A. Renzi J. Rhodes G. Riccio E. Romelli M. Roncarelli E. Rossetti R. Saglia A.G. S\'anchez D. Sapone R. Scaramella P. Schneider V. Scottez A. Secroun G. Seidel S. Serrano C. Sirignano G. Sirri L. Stanco F. Sureau A.N. Taylor M. Tenti I. Tereno R. Teyssier R. Toledo-Moreo A. Tramacere E.A. Valentijn L. Valenziano J. Valiviita T. Vassallo M. Viel Y. Wang N. Welikala L. Whittaker A. Zacchei G. Zamorani J. Zoubian E. Zucca
This is my paper
classification 🌌 astro-ph.CO
keywords euclidredshiftbinsdepthgalaxiesgcphsurveycosmological
0
0 comments X
read the original abstract

The accuracy of photometric redshifts (photo-zs) particularly affects the results of the analyses of galaxy clustering with photometrically-selected galaxies (GCph) and weak lensing. In the next decade, space missions like Euclid will collect photometric measurements for millions of galaxies. These data should be complemented with upcoming ground-based observations to derive precise and accurate photo-zs. In this paper, we explore how the tomographic redshift binning and depth of ground-based observations will affect the cosmological constraints expected from Euclid. We focus on GCph and extend the study to include galaxy-galaxy lensing (GGL). We add a layer of complexity to the analysis by simulating several realistic photo-z distributions based on the Euclid Consortium Flagship simulation and using a machine learning photo-z algorithm. We use the Fisher matrix formalism and these galaxy samples to study the cosmological constraining power as a function of redshift binning, survey depth, and photo-z accuracy. We find that bins with equal width in redshift provide a higher Figure of Merit (FoM) than equipopulated bins and that increasing the number of redshift bins from 10 to 13 improves the FoM by 35% and 15% for GCph and its combination with GGL, respectively. For GCph, an increase of the survey depth provides a higher FoM. But the addition of faint galaxies beyond the limit of the spectroscopic training data decreases the FoM due to the spurious photo-zs. When combining both probes, the number density of the sample, which is set by the survey depth, is the main factor driving the variations in the FoM. We conclude that there is more information that can be extracted beyond the nominal 10 tomographic redshift bins of Euclid and that we should be cautious when adding faint galaxies into our sample, since they can degrade the cosmological constraints.

This paper has not been read by Pith yet.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. A unified harmonic framework for dark siren cosmology

    astro-ph.CO 2026-03 unverdicted novelty 6.0

    The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescop...