{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:NYX7RRHWNXFUAV63TPMVQO6OTV","short_pith_number":"pith:NYX7RRHW","schema_version":"1.0","canonical_sha256":"6e2ff8c4f66dcb4057db9bd9583bce9d7692a9b3d36b530e373bbea28561fe89","source":{"kind":"arxiv","id":"1810.08629","version":4},"attestation_state":"computed","paper":{"title":"Quantifying baryon effects on the matter power spectrum and the weak lensing shear correlation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Adam Amara, Alexandre Refregier, Amandine M. C. Le Brun, Aurel Schneider, Joachim Stadel, Nora Elisa Chisari, Romain Teyssier","submitted_at":"2018-10-19T18:06:32Z","abstract_excerpt":"Feedback processes from baryons are expected to strongly affect weak-lensing observables of current and future cosmological surveys. In this paper we present a new parametrisation of halo profiles based on gas, stellar, and dark matter density components. This parametrisation is used to modify outputs of gravity-only $N$-body simulations (following the prescription of Schneider and Teyssier [1]) in order to mimic baryonic effects on the matter density field. The resulting baryonic correction model relies on a few well motivated physical parameters and is able to reproduce the redshift zero clu"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1810.08629","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-10-19T18:06:32Z","cross_cats_sorted":[],"title_canon_sha256":"5a4bf278ad5598dcaff2023173dd7869e5be18e66ca50550131e7cb368961d22","abstract_canon_sha256":"00b24002ae2a0a430d30583ca978b136b2019ad12ead041e1c369235b380d011"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:47:15.899263Z","signature_b64":"cVBFcwL3M79b1n73j1+KRqLpioeb+z3jQxRGd5stVLosSgticKK2nhiXPngqpNceZMPRgf9j4B2Jpd0Pyu7nDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6e2ff8c4f66dcb4057db9bd9583bce9d7692a9b3d36b530e373bbea28561fe89","last_reissued_at":"2026-05-17T23:47:15.898715Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:47:15.898715Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quantifying baryon effects on the matter power spectrum and the weak lensing shear correlation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Adam Amara, Alexandre Refregier, Amandine M. C. Le Brun, Aurel Schneider, Joachim Stadel, Nora Elisa Chisari, Romain Teyssier","submitted_at":"2018-10-19T18:06:32Z","abstract_excerpt":"Feedback processes from baryons are expected to strongly affect weak-lensing observables of current and future cosmological surveys. In this paper we present a new parametrisation of halo profiles based on gas, stellar, and dark matter density components. This parametrisation is used to modify outputs of gravity-only $N$-body simulations (following the prescription of Schneider and Teyssier [1]) in order to mimic baryonic effects on the matter density field. The resulting baryonic correction model relies on a few well motivated physical parameters and is able to reproduce the redshift zero clu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.08629","kind":"arxiv","version":4},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1810.08629","created_at":"2026-05-17T23:47:15.898795+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.08629v4","created_at":"2026-05-17T23:47:15.898795+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.08629","created_at":"2026-05-17T23:47:15.898795+00:00"},{"alias_kind":"pith_short_12","alias_value":"NYX7RRHWNXFU","created_at":"2026-05-18T12:32:40.477152+00:00"},{"alias_kind":"pith_short_16","alias_value":"NYX7RRHWNXFUAV63","created_at":"2026-05-18T12:32:40.477152+00:00"},{"alias_kind":"pith_short_8","alias_value":"NYX7RRHW","created_at":"2026-05-18T12:32:40.477152+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":28,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01963","citing_title":"Constraints on Halo Gas Profiles from Joint kSZ and Galaxy Clustering Analysis of ACT DR6 and CMASS","ref_index":10,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV","json":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV.json","graph_json":"https://pith.science/api/pith-number/NYX7RRHWNXFUAV63TPMVQO6OTV/graph.json","events_json":"https://pith.science/api/pith-number/NYX7RRHWNXFUAV63TPMVQO6OTV/events.json","paper":"https://pith.science/paper/NYX7RRHW"},"agent_actions":{"view_html":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV","download_json":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV.json","view_paper":"https://pith.science/paper/NYX7RRHW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.08629&json=true","fetch_graph":"https://pith.science/api/pith-number/NYX7RRHWNXFUAV63TPMVQO6OTV/graph.json","fetch_events":"https://pith.science/api/pith-number/NYX7RRHWNXFUAV63TPMVQO6OTV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV/action/storage_attestation","attest_author":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV/action/author_attestation","sign_citation":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV/action/citation_signature","submit_replication":"https://pith.science/pith/NYX7RRHWNXFUAV63TPMVQO6OTV/action/replication_record"}},"created_at":"2026-05-17T23:47:15.898795+00:00","updated_at":"2026-05-17T23:47:15.898795+00:00"}