{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:GRI4G5AB7KGGT5ZQN3BFIVP5BA","short_pith_number":"pith:GRI4G5AB","schema_version":"1.0","canonical_sha256":"3451c37401fa8c69f7306ec25455fd081905edfa9b5123c5733503aaf54cbbb6","source":{"kind":"arxiv","id":"astro-ph/9812456","version":2},"attestation_state":"computed","paper":{"title":"Streaming velocities as a dynamical estimator of Omega","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.H. Jaffe, H.A. Feldman, M. Davis, P.G. Ferreira, R. Juszkiewicz","submitted_at":"1998-12-28T16:04:24Z","abstract_excerpt":"It is well known that estimating the pairwise velocity of galaxies, v_{12}, from the redshift space galaxy correlation function is difficult because this method is highly sensitive to the assumed model of the pairwise velocity dispersion. Here we propose an alternative method to estimate v_{12} directly from peculiar velocity samples, which contain redshift-independent distances as well as galaxy redshifts. In contrast to other dynamical measures which determine beta = sigma_8 x Omega^{0.6}, our method can provide an estimate of (sigma_8)^2 x Omega^{0.6} for a range of sigma_8 (here Omega is t"},"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":"astro-ph/9812456","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-12-28T16:04:24Z","cross_cats_sorted":[],"title_canon_sha256":"8b0e7132e26693ff56f59529b34249ac599815004ba7269151a7a3532a37691e","abstract_canon_sha256":"c5176ab09d73f08cebe2125ce9303ef65279a1c20cbdf69a1379211f03eb0d1d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:07:24.137539Z","signature_b64":"1sgRzh40aahKDjmNCkS0yEI7t2kTiMpBJ0KnYiMYDMZxnsXTz5BHIvvTn0AuB49QEAoRK4OI5nxzB+um46CcDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3451c37401fa8c69f7306ec25455fd081905edfa9b5123c5733503aaf54cbbb6","last_reissued_at":"2026-07-04T16:07:24.137064Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:07:24.137064Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Streaming velocities as a dynamical estimator of Omega","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.H. Jaffe, H.A. Feldman, M. Davis, P.G. Ferreira, R. Juszkiewicz","submitted_at":"1998-12-28T16:04:24Z","abstract_excerpt":"It is well known that estimating the pairwise velocity of galaxies, v_{12}, from the redshift space galaxy correlation function is difficult because this method is highly sensitive to the assumed model of the pairwise velocity dispersion. Here we propose an alternative method to estimate v_{12} directly from peculiar velocity samples, which contain redshift-independent distances as well as galaxy redshifts. In contrast to other dynamical measures which determine beta = sigma_8 x Omega^{0.6}, our method can provide an estimate of (sigma_8)^2 x Omega^{0.6} for a range of sigma_8 (here Omega is t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9812456","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9812456/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"astro-ph/9812456","created_at":"2026-07-04T16:07:24.137123+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9812456v2","created_at":"2026-07-04T16:07:24.137123+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9812456","created_at":"2026-07-04T16:07:24.137123+00:00"},{"alias_kind":"pith_short_12","alias_value":"GRI4G5AB7KGG","created_at":"2026-07-04T16:07:24.137123+00:00"},{"alias_kind":"pith_short_16","alias_value":"GRI4G5AB7KGGT5ZQ","created_at":"2026-07-04T16:07:24.137123+00:00"},{"alias_kind":"pith_short_8","alias_value":"GRI4G5AB","created_at":"2026-07-04T16:07:24.137123+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2604.19922","citing_title":"Measuring neutrino mass and asymmetry through galaxy pairwise peculiar velocity","ref_index":49,"is_internal_anchor":true},{"citing_arxiv_id":"2604.14327","citing_title":"The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect","ref_index":23,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA","json":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA.json","graph_json":"https://pith.science/api/pith-number/GRI4G5AB7KGGT5ZQN3BFIVP5BA/graph.json","events_json":"https://pith.science/api/pith-number/GRI4G5AB7KGGT5ZQN3BFIVP5BA/events.json","paper":"https://pith.science/paper/GRI4G5AB"},"agent_actions":{"view_html":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA","download_json":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA.json","view_paper":"https://pith.science/paper/GRI4G5AB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9812456&json=true","fetch_graph":"https://pith.science/api/pith-number/GRI4G5AB7KGGT5ZQN3BFIVP5BA/graph.json","fetch_events":"https://pith.science/api/pith-number/GRI4G5AB7KGGT5ZQN3BFIVP5BA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA/action/storage_attestation","attest_author":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA/action/author_attestation","sign_citation":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA/action/citation_signature","submit_replication":"https://pith.science/pith/GRI4G5AB7KGGT5ZQN3BFIVP5BA/action/replication_record"}},"created_at":"2026-07-04T16:07:24.137123+00:00","updated_at":"2026-07-04T16:07:24.137123+00:00"}