Cosmology with stacked cluster weak lensing and cluster–galaxy cross-correlations

Journal Article · Wed Oct 23 00:00:00 EDT 2019 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stz2963· OSTI ID:1686158

Salcedo, Andrés N.  ^[1]; Wibking, Benjamin D.  ^[1]; Weinberg, David H. ^[1]; Wu, Hao-Yi  ^[1]; Ferrer, Douglas ^[2]; Eisenstein, Daniel ^[2]; Pinto, Philip ^[3]

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1. Department of Astronomy and Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA
2. Harvard-Smithsonian Center for Astrophysics, 60 Garden St, MS-10, Cambridge, MA 02138, USA
3. Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA

Cluster weak lensing is a sensitive probe of cosmology, particularly the amplitude of matter clustering σ₈ and matter density parameter Ω_m. The main nuisance parameter in a cluster weak lensing cosmological analysis is the scatter between the true halo mass and the relevant cluster observable, denoted $$\sigma _{\ln M_\mathrm{ c}}$$. We show that combining the cluster weak lensing observable ΔΣ with the projected cluster–galaxy cross-correlation function w_p,cg and galaxy autocorrelation function w_p,gg can break the degeneracy between σ₈ and $$\sigma _{\ln M_\mathrm{ c}}$$ to achieve tight, percent-level constraints on σ₈. Using a grid of cosmological N-body simulations, we compute derivatives of ΔΣ, w_p,cg, and w_p,gg with respect to σ₈, Ω_m, $$\sigma _{\ln M_\mathrm{ c}}$$, and halo occupation distribution (HOD) parameters describing the galaxy population. We also compute covariance matrices motivated by the properties of the Dark Energy Survey cluster and weak lensing survey and the BOSS CMASS galaxy redshift survey. For our fiducial scenario combining ΔΣ, w_p,cg, and w_p,gg measured over 0.3-30.0 h^-1 Mpc, for clusters at z = 0.35-0.55 above a mass threshold M_c ≈ 2 × 10¹⁴ h^-1 M_⊙, we forecast a $$1.4{{\ \rm per\ cent}}$$ constraint on σ8 while marginalizing over $$\sigma _{\ln M_\mathrm{ c}}$$ and all HOD parameters. Reducing the mass threshold to 1 × 10¹⁴ h^-1 M_⊙ and adding a z = 0.15-0.35 redshift bin sharpens this constraint to $$0.8{{\ \rm per\ cent}}$$. The small-scale (r_p < 3.0 h^-1 Mpc) ‘mass function’ and large-scale (r_p > 3.0 h^-1 Mpc) ‘halo-mass cross-correlation’ regimes of ΔΣ have comparable constraining power, allowing internal consistency tests from such an analysis.

• Research Organization: Krell Institute, Ames, IA (United States)
• Sponsoring Organization: USDOE National Nuclear Security Administration (NNSA); USDOE Office of Science (SC)
• Grant/Contract Number: FG02-97ER25308
• OSTI ID: 1686158
• Alternate ID(s): OSTI ID: 1800902
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 491 Journal Issue: 3; ISSN 0035-8711
• Publisher: Oxford University Press
• Country of Publication: United Kingdom
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
astronomy &amp; astrophysics
methods: numerical
dark matter
cosmology: theory