{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:VR3AF4PPTE32BUE54BUFBDQL43","short_pith_number":"pith:VR3AF4PP","schema_version":"1.0","canonical_sha256":"ac7602f1ef9937a0d09de068508e0be6f5a5465b6e10c36f9906a634da45ebfd","source":{"kind":"arxiv","id":"1307.6879","version":2},"attestation_state":"computed","paper":{"title":"The Impact of Different Physical Processes on the Statistics of Lyman-limit and Damped Lyman-alpha Absorbers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Claudio Dalla Vecchia, C. M. Booth, Gabriel Altay, Joop Schaye, Tom Theuns","submitted_at":"2013-07-25T20:53:02Z","abstract_excerpt":"We compute the z = 3 neutral hydrogen column density distribution function f(NHI) for 19 simulations drawn from the OWLS project using a post-processing correction for self-shielding calculated with full radiative transfer of the ionising background radiation. We investigate how different physical processes and parameters affect the abundance of Lyman-limit systems (LLSs) and damped Lyman-alpha absorbers (DLAs) including: i) metal-line cooling; ii) the efficiency of feedback from SNe and AGN; iii) the effective equation of state for the ISM; iv) cosmological parameters; v) the assumed star for"},"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":"1307.6879","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-07-25T20:53:02Z","cross_cats_sorted":[],"title_canon_sha256":"86801b0b79e4dff328592cb40127efb13e5d4ce060f83b535e072118df1c1440","abstract_canon_sha256":"a2d6e11b29fec7a55b6930ddd763280b6a9c618d139d76566006c8e0a8484fa3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:48:34.412351Z","signature_b64":"b/hR4TmpjHiIpwVgdvRX1TN9bvp+Vde85YcA+ofGul7UJHgydu5ax6oJBAVf/b6VBlqa/XIW1KwW8MMaahfrAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ac7602f1ef9937a0d09de068508e0be6f5a5465b6e10c36f9906a634da45ebfd","last_reissued_at":"2026-05-18T01:48:34.411731Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:48:34.411731Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Impact of Different Physical Processes on the Statistics of Lyman-limit and Damped Lyman-alpha Absorbers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Claudio Dalla Vecchia, C. M. Booth, Gabriel Altay, Joop Schaye, Tom Theuns","submitted_at":"2013-07-25T20:53:02Z","abstract_excerpt":"We compute the z = 3 neutral hydrogen column density distribution function f(NHI) for 19 simulations drawn from the OWLS project using a post-processing correction for self-shielding calculated with full radiative transfer of the ionising background radiation. We investigate how different physical processes and parameters affect the abundance of Lyman-limit systems (LLSs) and damped Lyman-alpha absorbers (DLAs) including: i) metal-line cooling; ii) the efficiency of feedback from SNe and AGN; iii) the effective equation of state for the ISM; iv) cosmological parameters; v) the assumed star for"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1307.6879","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":"1307.6879","created_at":"2026-05-18T01:48:34.411814+00:00"},{"alias_kind":"arxiv_version","alias_value":"1307.6879v2","created_at":"2026-05-18T01:48:34.411814+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1307.6879","created_at":"2026-05-18T01:48:34.411814+00:00"},{"alias_kind":"pith_short_12","alias_value":"VR3AF4PPTE32","created_at":"2026-05-18T12:28:04.890932+00:00"},{"alias_kind":"pith_short_16","alias_value":"VR3AF4PPTE32BUE5","created_at":"2026-05-18T12:28:04.890932+00:00"},{"alias_kind":"pith_short_8","alias_value":"VR3AF4PP","created_at":"2026-05-18T12:28:04.890932+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1907.02977","citing_title":"Realistic simulations of galaxy formation in f(R) modified gravity","ref_index":47,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43","json":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43.json","graph_json":"https://pith.science/api/pith-number/VR3AF4PPTE32BUE54BUFBDQL43/graph.json","events_json":"https://pith.science/api/pith-number/VR3AF4PPTE32BUE54BUFBDQL43/events.json","paper":"https://pith.science/paper/VR3AF4PP"},"agent_actions":{"view_html":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43","download_json":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43.json","view_paper":"https://pith.science/paper/VR3AF4PP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1307.6879&json=true","fetch_graph":"https://pith.science/api/pith-number/VR3AF4PPTE32BUE54BUFBDQL43/graph.json","fetch_events":"https://pith.science/api/pith-number/VR3AF4PPTE32BUE54BUFBDQL43/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43/action/storage_attestation","attest_author":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43/action/author_attestation","sign_citation":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43/action/citation_signature","submit_replication":"https://pith.science/pith/VR3AF4PPTE32BUE54BUFBDQL43/action/replication_record"}},"created_at":"2026-05-18T01:48:34.411814+00:00","updated_at":"2026-05-18T01:48:34.411814+00:00"}