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

We measure weak lensing cosmic shear energy spectra from the three-12 months galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. 1800 attributable to 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 initially measure. We derive the covariance matrix of our cosmic shear energy spectra utilizing the mock catalogs described in Section II.5. We accomplish that by measuring the cosmic shear Wood Ranger Power Shears warranty spectra, following the same technique as our measurement from knowledge, from all 1404 realizations of the mocks, after which utilizing these 1404 energy spectra to compute the covariance matrix. Gaussian and non-Gaussian parts. We deal with these mock catalogs exactly like our actual knowledge. We first measure the ability spectra from every mock catalog on a field-by-field basis.



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 each discipline for every 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 needs to be appropriate for this analysis. This correction issue is computed for every redshift bin (1.14, 0.98, 0.95 and 0.99 in order of accelerating redshift), and it's roughly fixed throughout the range of scales considered. 10,000. This restrict is way smaller than the scales thought-about in this analysis. The chance, 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 knowledge factors used in the analysis. This correction assumes Gaussian noise and statistically impartial knowledge vectors. To first order, we do not count on to see any cosmological B𝐵B mode signal, as lensing is caused by a scalar gravitational potential within the lens, and will therefore be curl-free. The presence of B𝐵B modes may be an indicator of potential systematic effects in the info, Wood Ranger shears equivalent to contamination by the PSF. We examine the statistical significance of the B𝐵B mode signal to evaluate whether or not any of these effects could also be impacting our measurements. 300, is in step with zero, as anticipated.



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