Covariance matrices for galaxy cluster weak lensing: from virial regime to uncorrelated large-scale structure
ABSTRACT Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent constraints on growth of structure and cosmic acceleration. In these experiments, accurate modelling of covariance matrices of cluster weak lens...
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Published in | Monthly notices of the Royal Astronomical Society Vol. 490; no. 2; pp. 2606 - 2626 |
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Main Authors | , , , , |
Format | Journal Article |
Language | English |
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United States
Royal Astronomical Society
01.12.2019
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Abstract | ABSTRACT
Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent constraints on growth of structure and cosmic acceleration. In these experiments, accurate modelling of covariance matrices of cluster weak lensing plays the key role in obtaining robust measurements of the mean mass of clusters and cosmological parameters. We use a combination of analytical calculations and high-resolution N-body simulations to derive accurate covariance matrices that span from the virial regime to linear scales of the cluster-matter cross-correlation. We validate this calculation using a public ray-tracing lensing simulation and provide a software package for calculating covariance matrices for a wide range of cluster and source sample choices. We discuss the relative importance of shape noise and density fluctuations, the impact of radial bin size, and the impact of off-diagonal elements. For a weak lensing source density ns = 10 arcmin−2, shape noise typically dominates the variance on comoving scales $r_{\rm p}\lesssim 5\ h^{-1} \, \rm Mpc$. However, for ns = 60 arcmin−2, potentially achievable with future weak lensing experiments, density fluctuations typically dominate the variance at $r_{\rm p}\gtrsim 1\ h^{-1} \, \rm Mpc$ and remain comparable to shape noise on smaller scales. |
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AbstractList | ABSTRACT
Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent constraints on growth of structure and cosmic acceleration. In these experiments, accurate modelling of covariance matrices of cluster weak lensing plays the key role in obtaining robust measurements of the mean mass of clusters and cosmological parameters. We use a combination of analytical calculations and high-resolution N-body simulations to derive accurate covariance matrices that span from the virial regime to linear scales of the cluster-matter cross-correlation. We validate this calculation using a public ray-tracing lensing simulation and provide a software package for calculating covariance matrices for a wide range of cluster and source sample choices. We discuss the relative importance of shape noise and density fluctuations, the impact of radial bin size, and the impact of off-diagonal elements. For a weak lensing source density ns = 10 arcmin−2, shape noise typically dominates the variance on comoving scales $r_{\rm p}\lesssim 5\ h^{-1} \, \rm Mpc$. However, for ns = 60 arcmin−2, potentially achievable with future weak lensing experiments, density fluctuations typically dominate the variance at $r_{\rm p}\gtrsim 1\ h^{-1} \, \rm Mpc$ and remain comparable to shape noise on smaller scales. Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent constraints on growth of structure and cosmic acceleration. In these experiments, accurate modelling of covariance matrices of cluster weak lensing plays the key role in obtaining robust measurements of the mean mass of clusters and cosmological parameters. We use a combination of analytical calculations and high-resolution N-body simulations to derive accurate covariance matrices that span from the virial regime to linear scales of the cluster-matter cross-correlation. We validate this calculation using a public ray-tracing lensing simulation and provide a software package for calculating covariance matrices for a wide range of cluster and source sample choices. We discuss the relative importance of shape noise and density fluctuations, the impact of radial bin size, and the impact of off-diagonal elements. For a weak lensing source density ns = 10 arcmin-2, shape noise typically dominates the variance on comoving scales $r_{\rm p}\lesssim 5\ h^{-1} \, \rm Mpc$. However, for ns = 60 arcmin-2, potentially achievable with future weak lensing experiments, density fluctuations typically dominate the variance at $r_{\rm p}\gtrsim 1\ h^{-1} \, \rm Mpc$ and remain comparable to shape noise on smaller scales. |
Author | Salcedo, Andrés N Zu, Ying Weinberg, David H Wibking, Benjamin D Wu, Hao-Yi |
Author_xml | – sequence: 1 givenname: Hao-Yi orcidid: 0000-0002-7904-1707 surname: Wu fullname: Wu, Hao-Yi organization: Department of Physics, Department of Astronomy, and Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA – sequence: 2 givenname: David H surname: Weinberg fullname: Weinberg, David H organization: Department of Physics, Department of Astronomy, and Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA – sequence: 3 givenname: Andrés N orcidid: 0000-0003-1420-527X surname: Salcedo fullname: Salcedo, Andrés N organization: Department of Physics, Department of Astronomy, and Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA – sequence: 4 givenname: Benjamin D orcidid: 0000-0003-3175-2291 surname: Wibking fullname: Wibking, Benjamin D organization: Department of Physics, Department of Astronomy, and Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA – sequence: 5 givenname: Ying orcidid: 0000-0001-6966-6925 surname: Zu fullname: Zu, Ying organization: Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Minhang, Shanghai 200240, China |
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Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent... Next-generation optical imaging surveys will revolutionize the observations of weak gravitational lensing by galaxy clusters and provide stringent constraints... |
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SubjectTerms | astronomy & astrophysics ASTRONOMY AND ASTROPHYSICS cosmological parameters cosmology: theory galaxies: clusters: general gravitational lensing: weak |
Title | Covariance matrices for galaxy cluster weak lensing: from virial regime to uncorrelated large-scale structure |
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