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We measure weak lensing cosmic shear power spectra from the three-12 months galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. 1800 on account of theoretical uncertainties in our modeling of those nonlinear scales (primarily based on checks described in Sections V.2.1 and V.3). This gives us six multipole bins that we use in our fiducial analysis, from the 17 that we originally measure. We derive the covariance matrix of our cosmic shear garden power shears spectra using the mock catalogs described in Section II.5. We achieve this by measuring the cosmic shear energy spectra, following the same methodology as our measurement from knowledge, from all 1404 realizations of the mocks, after which utilizing these 1404 power spectra to compute the covariance matrix. Gaussian and non-Gaussian elements. We deal with these mock catalogs exactly like our real data. We first measure the ability spectra from every mock catalog on a subject-by-area basis.

We analytically compute the additive noise bias from form noise, cordless power shears and subtract it from the measured Wood Ranger Power Shears features spectra. Finally, we co-add the spectra from every field for each mock realization using inverse variance weighting, with the individual covariances measured from the mock energy 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 should be appropriate for this evaluation. This correction factor is computed for each redshift bin (1.14, 0.98, 0.95 and 0.99 so as of increasing redshift), and it's roughly fixed across the range of scales thought-about. 10,000. This restrict is way smaller than the scales thought-about in this analysis. The likelihood, 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 number of knowledge points used within the analysis. This correction assumes Gaussian noise and statistically unbiased information vectors. To first order, we do not count on to see any cosmological B????B mode signal, as lensing is attributable to a scalar gravitational potential in the lens, and may therefore be curl-free. The presence of B????B modes may be an indicator of potential systematic effects in the information, similar to contamination by the PSF. We examine the statistical significance of the B????B mode signal to assess whether any of these results may be impacting our measurements. 300, is in line with zero, as anticipated.

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