{"paper":{"title":"Covariances for cosmic shear and galaxy-galaxy lensing in the response approach","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Kosei Shiroyama, Masahiro Takada, Masato Shirasaki, Ryuichi Takahashi, Takahiro Nishimichi","submitted_at":"2018-05-29T18:01:02Z","abstract_excerpt":"In this study, we measure the response of matter and halo projected power spectra $P^{\\rm 2D}_{\\rm XY}(k)$ (X, Y are matter and/or halos), to a large-scale density contrast, $\\delta_{\\rm b}$, using separate universe simulations. We show that the fractional response functions, i.e., $\\mathrm{d}\\ln P^{\\rm 2D}_{\\rm XY}(k)/\\mathrm{d}\\delta_{\\rm b}$, are identical to their respective three-dimensional power spectra within simulation measurement errors. Then, using various $N$-body simulation combinations (small-box simulations with periodic boundary conditions and sub-volumes of large-box simulatio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.11629","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}