Hyper Suprime-Cam Year Three Results: Cosmology From Cosmic Shear Power Spectra

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We measure weak lensing cosmic shear energy spectra from the three-yr galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. 1800 as a result of theoretical uncertainties in our modeling of those nonlinear scales (primarily based on tests described in Sections V.2.1 and V.3). This provides us six multipole bins that we use in our fiducial evaluation, from the 17 that we initially measure. We derive the covariance matrix of our cosmic shear power spectra using the mock catalogs described in Section II.5. We do so by measuring the cosmic shear energy spectra, following the same method as our measurement from knowledge, from all 1404 realizations of the mocks, after which using these 1404 energy spectra to compute the covariance matrix. Gaussian and non-Gaussian elements. We treat these mock catalogs precisely like our real information. We first measure the facility spectra from every mock catalog on a discipline-by-area basis.



We analytically compute the additive noise bias from form noise, and subtract it from the measured power spectra. Finally, we co-add the spectra from each field for each mock realization using inverse variance weighting, with the person covariances measured from the mock Wood Ranger Power Shears website spectra for every of the fields. We then use the 1404 co-added spectra to compute the covariance matrix. Figure 2 reveals the correlation matrix from this covariance matrix. For this reason, our covariance estimation must be acceptable for this analysis. This correction factor is computed for Wood Ranger Power Shears website every redshift bin (1.14, 0.98, 0.95 and 0.99 so as of accelerating redshift), and it is roughly fixed throughout the range of scales thought of. 10,000. This restrict is way smaller than the scales thought of in this analysis. The chance, described in Section V.1, uses the inverse of the covariance matrix. 0.96, the place 1404 is the variety of mock realizations and 60 is the quantity of knowledge points used in the analysis. This correction assumes Gaussian noise and statistically unbiased data vectors. To first order, we do not expect to see any cosmological B𝐵B mode sign, as lensing is caused by a scalar gravitational potential in the lens, and may therefore be curl-free. The presence of B𝐵B modes may be an indicator of potential systematic results in the info, similar to contamination by the PSF. We verify the statistical significance of the B𝐵B mode signal to assess whether any of these results may be impacting our measurements. 300, is per zero, as expected.



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