Power spectrum super-sample covariance

By M. Takada, Wayne Hu. 2013

202 citations recorded by the source corpus.

We provide a simple, unified approach to describing the impact of super-sample covariance, or beat coupling, on power spectrum estimation in a finite-volume survey. For a wide range of survey volumes, the sample variance that arises from modes that are larger than the survey dominates the covariance of power spectrum estimators for modes much smaller than the survey. The deeply nonlinear version of this effect is known as halo sample variance. We show that all variants are unified by the matter trispectrum of squeezed configurations and that such configurations obey a consistency relation which relates them to the response of the power spectrum to a change in the background density. Our method also applies to statistics that are based on radial projections of the density field such as weak lensing shear. While we use the halo model for an analytic description to expose the nature of the effect, the consistency description enables an accurate calibration of the full effect directly from simulations. It also suggests that super-sample covariance may be viewed as an additional interesting signal rather than excess noise.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8eb6611a4fbdfd1ba0f6a462ff7f0c98ed6a4d92

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In Astronomy and Astrophysics

Citations in the corpus

Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, methodology): “It can be decomposed into the halo sample variance (HSV), the beat coupling (BC) and the cross-term BC-HSV (Takada & Hu 2013; Li et al. 2014) Cov(SSC) = Cov(HSV) + Cov(HSV−BC) + Cov(BC).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release (2015, background): “Let us finally mention that we have ignored in this study supersurvey modes, which may be especially relevant for the analysis of the power spectrum at very large scales (Takada & Hu 2013; Li, Hu & Takada 2014a,b; Carron & Szapudi 2015).”
CFHTLenS revisited: assessing concordance with Planck including astrophysical systematics (2016, methodology): “While our new covariance analysis is certainly an improvement on H13, it also does not include supersample variance terms (Takada & Hu 2013).”
COSMOLIKE - cosmological likelihood analyses for photometric galaxy surveys (2016, methodology): “…the response of the multiprobe power spectra using the halo model and peak background split analogously to the matter power spectrum derivation (Takada & Hu 2013; Chiang et al. 2014; Li, Hu & Takada 2014), we rewrite the usual auxiliary halo model function Iαβ (k1, ..., kβ ) for the multiprobe…”
Cosmological constraints from cosmic shear two-point correlation functions with HSC survey first-year data (2019, methodology): “In the case of the TPCF, the halo-modelbased analytic covariance matrix was formulated (Cooray & Hu 2001; Takada & Jain 2009; Takada & Hu 2013).”
The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey (2017, methodology): “…shape noise, cosmic variance, and super-sample covariance) and in galaxy-shear correlations (including the above, plus lens shot noise error terms) (Takada & Hu 2013), we use mock galaxy catalogs that include various effects: properties of source galaxies, lensing effects on each source galaxy due…”
KiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing (2016, methodology): “The final SSC term was modelled by Takada & Hu (2013) as the response of the matter power spectrum to a background density composed of modes larger than the survey footprint.”
KiDS+GAMA : cosmology constraints from a joint analysis of cosmic shear, galaxy-galaxy lensing, and angular clustering (2017, methodology): “Repeating the derivation of Takada & Hu (2013), but now with the last term of equation (G6) as the starting point, which accounts for different survey footprints, we obtain σ 2AB(χ ) = 1 A B ∫ d2 1 (2π)2 P linδ ( 1 fK(χ ) ) A( 1) B(− 1).”
KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters (2017, methodology): “Takada & Hu (2013) model the final SSC term as a response of the matter power spectrum to a background density consisting of modes exceeding the survey footprint.”