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 as a result of theoretical uncertainties in our modeling of these nonlinear scales (primarily based on exams described in Sections V.2.1 and V.3). This gives us six multipole bins that we use in our fiducial evaluation, from the 17 that we originally measure. We derive the covariance matrix of our cosmic shear energy spectra using the mock catalogs described in Section II.5. We accomplish that by measuring the cosmic shear energy spectra, following the same method as our measurement from data, from all 1404 realizations of the mocks, after which utilizing these 1404 power spectra to compute the covariance matrix. Gaussian and non-Gaussian components. We treat these mock catalogs exactly like our real knowledge. We first measure the power spectra from every mock catalog on a area-by-area foundation.
We analytically compute the additive noise bias from shape noise, and subtract it from the measured energy spectra. Finally, we co-add the spectra from each field for each mock realization utilizing 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 shows the correlation matrix from this covariance matrix. Because of this, our covariance estimation ought to be appropriate for this evaluation. This correction issue is computed for every redshift bin (1.14, 0.98, outdoor branch trimmer 0.95 and 0.Ninety nine in order of increasing redshift), and it's roughly constant across the range of scales thought-about. 10,000. This restrict is far smaller than the scales thought-about in this evaluation. The chance, described in Section V.1, makes use of the inverse of the covariance matrix. 0.96, the place 1404 is the number of mock realizations and 60 is the quantity of information factors used in the analysis. This correction assumes Gaussian noise and statistically impartial knowledge vectors. To first order, we do not expect to see any cosmological B𝐵B mode signal, as lensing is caused by a scalar gravitational potential in the lens, and should therefore be curl-free. The presence of B𝐵B modes could also be an indicator of potential systematic results in the data, such as contamination by the PSF. We examine the statistical significance of the B𝐵B mode signal to assess whether any of those effects could also be impacting our measurements. 300, is per zero, as anticipated.
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