We measure weak lensing cosmic shear power spectra from the three-yr galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. 1800 resulting from theoretical uncertainties in our modeling of these nonlinear scales (based mostly on tests described in Sections V.2.1 and V.3). This provides us six multipole bins that we use in our fiducial analysis, from the 17 that we initially measure. We derive the covariance matrix of our cosmic shear power spectra utilizing the mock catalogs described in Section II.5. We do so by measuring the cosmic shear power spectra, following the identical methodology as our measurement from knowledge, from all 1404 realizations of the mocks, and then using these 1404 power spectra to compute the covariance matrix. Gaussian and non-Gaussian components. We deal with these mock catalogs precisely like our real knowledge. We first measure the power spectra from every mock catalog on a discipline-by-field basis.

We analytically compute the additive noise bias from shape noise, and subtract it from the measured power spectra. Finally, we co-add the spectra from every field for each mock realization utilizing inverse variance weighting, with the individual covariances measured from the mock Wood Ranger Power Shears shop spectra for every of the fields. We then use the 1404 co-added spectra to compute the covariance matrix. Figure 2 exhibits the correlation matrix from this covariance matrix. For this reason, our covariance estimation must be acceptable for this evaluation. This correction factor is computed for every redshift bin (1.14, 0.98, 0.Ninety five and 0.99 in order of increasing redshift), and it's approximately fixed throughout the vary of scales thought-about. 10,000. This restrict is much smaller than the scales thought of on this evaluation. The probability, described in Section V.1, makes use of the inverse of the covariance matrix. 0.96, where 1404 is the variety of mock realizations and 60 is the quantity of data factors used within the evaluation. This correction assumes Gaussian noise and statistically independent knowledge vectors. To first order, we do not anticipate to see any cosmological B𝐵B mode sign, as lensing is brought on by a scalar gravitational potential within the lens, and may therefore be curl-free. The presence of B𝐵B modes may be an indicator of potential systematic results in the info, comparable to contamination by the PSF. We verify the statistical significance of the B𝐵B mode sign to evaluate whether any of these results may be impacting our measurements. 300, Wood Ranger Power Shears shop is consistent with zero, as anticipated.

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