{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1997:FNBS5F3CFPKTITTM4DAGEVTGED","short_pith_number":"pith:FNBS5F3C","schema_version":"1.0","canonical_sha256":"2b432e97622bd5344e6ce0c062566620d369d08c67237702c4c9ef930622bdaa","source":{"kind":"arxiv","id":"astro-ph/9705113","version":1},"attestation_state":"computed","paper":{"title":"Cosmological Constraints from High-Redshift Damped Lyman-Alpha Systems","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Chung-Pei Ma (U Penn), David H. Weinberg (Ohio State U), Edmund Bertschinger (MIT), Lars Hernquist (UC Santa Cruz), Neal Katz (U Mass)","submitted_at":"1997-05-15T15:24:07Z","abstract_excerpt":"Any viable cosmological model must produce enough structure at early epochs to explain the amount of gas associated with high-redshift damped Ly$\\alpha$ systems. We study the evolution of damped Ly$\\alpha$ systems at redshifts $z\\ge 2$ in cold dark matter (CDM) and cold+hot dark matter (CDM+HDM) models using both N-body and hydrodynamic simulations. Our approach incorporates the effects of gas dynamics, and we find that all earlier estimates which assumed that all the baryons in dark matter halos would contribute to damped Ly$\\alpha$ absorption have overestimated the column density distributio"},"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/9705113","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1997-05-15T15:24:07Z","cross_cats_sorted":[],"title_canon_sha256":"974609c30b1df21e5f19c72826f8286cca63a3c1eac768ab80997ead1b6233f0","abstract_canon_sha256":"56fb4881a2f4f1cba45d5738caf3324aafc12e4f9147f2ad42182a09ba0b10cb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:03:00.800258Z","signature_b64":"Ru2xglIJnfKmq/GXvHiPDI18MOj0bilNkGxjgSI28BED4H24p/oB2r3M7yeyaMSqBkbve6kl8IaXl1D1kOv2Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2b432e97622bd5344e6ce0c062566620d369d08c67237702c4c9ef930622bdaa","last_reissued_at":"2026-07-04T16:03:00.799865Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:03:00.799865Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmological Constraints from High-Redshift Damped Lyman-Alpha Systems","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Chung-Pei Ma (U Penn), David H. Weinberg (Ohio State U), Edmund Bertschinger (MIT), Lars Hernquist (UC Santa Cruz), Neal Katz (U Mass)","submitted_at":"1997-05-15T15:24:07Z","abstract_excerpt":"Any viable cosmological model must produce enough structure at early epochs to explain the amount of gas associated with high-redshift damped Ly$\\alpha$ systems. We study the evolution of damped Ly$\\alpha$ systems at redshifts $z\\ge 2$ in cold dark matter (CDM) and cold+hot dark matter (CDM+HDM) models using both N-body and hydrodynamic simulations. Our approach incorporates the effects of gas dynamics, and we find that all earlier estimates which assumed that all the baryons in dark matter halos would contribute to damped Ly$\\alpha$ absorption have overestimated the column density distributio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9705113","kind":"arxiv","version":1},"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/9705113/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/9705113","created_at":"2026-07-04T16:03:00.799927+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9705113v1","created_at":"2026-07-04T16:03:00.799927+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9705113","created_at":"2026-07-04T16:03:00.799927+00:00"},{"alias_kind":"pith_short_12","alias_value":"FNBS5F3CFPKT","created_at":"2026-07-04T16:03:00.799927+00:00"},{"alias_kind":"pith_short_16","alias_value":"FNBS5F3CFPKTITTM","created_at":"2026-07-04T16:03:00.799927+00:00"},{"alias_kind":"pith_short_8","alias_value":"FNBS5F3C","created_at":"2026-07-04T16:03:00.799927+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.05114","citing_title":"Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges","ref_index":64,"is_internal_anchor":true},{"citing_arxiv_id":"2605.05114","citing_title":"Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges","ref_index":57,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED","json":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED.json","graph_json":"https://pith.science/api/pith-number/FNBS5F3CFPKTITTM4DAGEVTGED/graph.json","events_json":"https://pith.science/api/pith-number/FNBS5F3CFPKTITTM4DAGEVTGED/events.json","paper":"https://pith.science/paper/FNBS5F3C"},"agent_actions":{"view_html":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED","download_json":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED.json","view_paper":"https://pith.science/paper/FNBS5F3C","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9705113&json=true","fetch_graph":"https://pith.science/api/pith-number/FNBS5F3CFPKTITTM4DAGEVTGED/graph.json","fetch_events":"https://pith.science/api/pith-number/FNBS5F3CFPKTITTM4DAGEVTGED/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED/action/storage_attestation","attest_author":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED/action/author_attestation","sign_citation":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED/action/citation_signature","submit_replication":"https://pith.science/pith/FNBS5F3CFPKTITTM4DAGEVTGED/action/replication_record"}},"created_at":"2026-07-04T16:03:00.799927+00:00","updated_at":"2026-07-04T16:03:00.799927+00:00"}