{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:G5PHFQXW2XAB4IYS4MMVZIVJT2","short_pith_number":"pith:G5PHFQXW","schema_version":"1.0","canonical_sha256":"375e72c2f6d5c01e2312e3195ca2a99eb435fddac229b86f303d4aaeba6be217","source":{"kind":"arxiv","id":"1611.04901","version":2},"attestation_state":"computed","paper":{"title":"Verifying the consistency relation for the scale-dependent bias from local primordial non-Gaussianity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Fabian Schmidt, Matteo Biagetti, Titouan Lazeyras, Tobias Baldauf, Vincent Desjacques","submitted_at":"2016-11-15T15:57:01Z","abstract_excerpt":"We measure the large-scale bias of dark matter halos in simulations with non-Gaussian initial conditions of the local type, and compare this bias to the response of the mass function to a change in the primordial amplitude of fluctuations. The two are found to be consistent, as expected from physical arguments, for three halo-finder algorithms which use different Spherical Overdensity (SO) and Friends-of-Friends (FoF) methods. On the other hand, we find that the commonly used prediction for universal mass functions, that the scale-dependent bias is proportional to the first-order Gaussian Lagr"},"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":"1611.04901","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-11-15T15:57:01Z","cross_cats_sorted":[],"title_canon_sha256":"cbda8f82d2c4cda51d7b1dd82063a0bf40278146ab46e0b9697f9c21af14bbcb","abstract_canon_sha256":"7cb883431fcaadda41a278b691a70c082c3e2d56f7b46f9b83418ea19fa32604"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:44:33.632690Z","signature_b64":"OAKvk1gKMk2Syhlg4WKfFaULJTSl4fG3k7QCqreYTiemvCEKdWHDAVjaaYjkZi1TzQW2z7ZljVQ7UAAHZcgcCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"375e72c2f6d5c01e2312e3195ca2a99eb435fddac229b86f303d4aaeba6be217","last_reissued_at":"2026-05-18T00:44:33.632254Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:44:33.632254Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Verifying the consistency relation for the scale-dependent bias from local primordial non-Gaussianity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Fabian Schmidt, Matteo Biagetti, Titouan Lazeyras, Tobias Baldauf, Vincent Desjacques","submitted_at":"2016-11-15T15:57:01Z","abstract_excerpt":"We measure the large-scale bias of dark matter halos in simulations with non-Gaussian initial conditions of the local type, and compare this bias to the response of the mass function to a change in the primordial amplitude of fluctuations. The two are found to be consistent, as expected from physical arguments, for three halo-finder algorithms which use different Spherical Overdensity (SO) and Friends-of-Friends (FoF) methods. On the other hand, we find that the commonly used prediction for universal mass functions, that the scale-dependent bias is proportional to the first-order Gaussian Lagr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1611.04901","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1611.04901","created_at":"2026-05-18T00:44:33.632327+00:00"},{"alias_kind":"arxiv_version","alias_value":"1611.04901v2","created_at":"2026-05-18T00:44:33.632327+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1611.04901","created_at":"2026-05-18T00:44:33.632327+00:00"},{"alias_kind":"pith_short_12","alias_value":"G5PHFQXW2XAB","created_at":"2026-05-18T12:30:15.759754+00:00"},{"alias_kind":"pith_short_16","alias_value":"G5PHFQXW2XAB4IYS","created_at":"2026-05-18T12:30:15.759754+00:00"},{"alias_kind":"pith_short_8","alias_value":"G5PHFQXW","created_at":"2026-05-18T12:30:15.759754+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21436","citing_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","ref_index":81,"is_internal_anchor":true},{"citing_arxiv_id":"2604.04867","citing_title":"Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6","ref_index":64,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2","json":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2.json","graph_json":"https://pith.science/api/pith-number/G5PHFQXW2XAB4IYS4MMVZIVJT2/graph.json","events_json":"https://pith.science/api/pith-number/G5PHFQXW2XAB4IYS4MMVZIVJT2/events.json","paper":"https://pith.science/paper/G5PHFQXW"},"agent_actions":{"view_html":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2","download_json":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2.json","view_paper":"https://pith.science/paper/G5PHFQXW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1611.04901&json=true","fetch_graph":"https://pith.science/api/pith-number/G5PHFQXW2XAB4IYS4MMVZIVJT2/graph.json","fetch_events":"https://pith.science/api/pith-number/G5PHFQXW2XAB4IYS4MMVZIVJT2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2/action/storage_attestation","attest_author":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2/action/author_attestation","sign_citation":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2/action/citation_signature","submit_replication":"https://pith.science/pith/G5PHFQXW2XAB4IYS4MMVZIVJT2/action/replication_record"}},"created_at":"2026-05-18T00:44:33.632327+00:00","updated_at":"2026-05-18T00:44:33.632327+00:00"}