We measure weak lensing cosmic shear energy spectra from the three-year galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. 1800 resulting from theoretical uncertainties in our modeling of those nonlinear scales (primarily based on assessments 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 energy spectra using the mock catalogs described in Section II.5. We achieve this by measuring the cosmic shear energy spectra, following the identical method as our measurement from data, from all 1404 realizations of the mocks, Wood Ranger Tools and Wood Ranger Tools then utilizing these 1404 energy spectra to compute the covariance matrix. Gaussian and non-Gaussian elements. We deal with these mock catalogs exactly like our actual data. We first measure the facility spectra from every mock catalog on a discipline-by-area foundation.

We analytically compute the additive noise bias from form noise, and subtract it from the measured energy spectra. Finally, we co-add the spectra from every discipline for each mock realization utilizing inverse variance weighting, with the individual covariances measured from the mock energy spectra for each 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 that reason, our covariance estimation must be appropriate for this evaluation. This correction factor is computed for every redshift bin (1.14, 0.98, 0.Ninety five and electric power shears 0.Ninety nine in order of accelerating redshift), and it is roughly constant throughout the range of scales considered. 10,000. This restrict is much smaller than the scales considered on this evaluation. The probability, described in Section V.1, uses the inverse of the covariance matrix. 0.96, where 1404 is the variety of mock realizations and 60 is the quantity of data points used within the evaluation. This correction assumes Gaussian noise and statistically independent data vectors. To first order, we don't count on to see any cosmological B𝐵B mode sign, as lensing is brought on by a scalar gravitational potential within the lens, and will therefore be curl-free. The presence of B𝐵B modes could also be an indicator of potential systematic effects in the data, akin to contamination by the PSF. We examine the statistical significance of the B𝐵B mode sign to assess whether or not any of these results could also be impacting our measurements. 300, is in keeping with zero, as expected.

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