{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:Q5Z6HVJ7PYJLQF7MSA65EHXVEI","short_pith_number":"pith:Q5Z6HVJ7","schema_version":"1.0","canonical_sha256":"8773e3d53f7e12b817ec903dd21ef522391236b41191f79159539369f13e6ef5","source":{"kind":"arxiv","id":"astro-ph/0307191","version":2},"attestation_state":"computed","paper":{"title":"Simulating Voids","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"David M. Goldberg, Michael S. Vogeley (Drexel)","submitted_at":"2003-07-09T23:08:39Z","abstract_excerpt":"We present a novel method for simulation of the interior of large cosmic voids, suitable for study of the formation and evolution of objects lying within such regions. Following Birkhoff's theorem, void regions dynamically evolve as universes with cosmological parameters that depend on the underdensity of the void. We derive the values of $\\Omega_M$, $\\Omega_{\\Lambda}$, and $H_0$ that describe this evolution. We examine how the growth rate of structure and scale factor in a void differ from the background universe. Together with a prescription for the power spectrum of fluctuations, these equa"},"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/0307191","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-07-09T23:08:39Z","cross_cats_sorted":[],"title_canon_sha256":"ba47f442902a0deb382ded77e54666c8295770b6c96cd2db9a89484ca46c4d6a","abstract_canon_sha256":"7e4063022f807d15eb55cec56a9b3e092cfe59bd169f1cca619d482e1a21b908"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:52:08.236415Z","signature_b64":"KYb6g4iYQ1NpS3MDUE8Pv2wB0kbZST7vQpdZPv2SSQSzIYxaN03LuQ9yPVp9OwYS5E47rICM+2JqIbXmtC0fAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8773e3d53f7e12b817ec903dd21ef522391236b41191f79159539369f13e6ef5","last_reissued_at":"2026-07-04T16:52:08.235974Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:52:08.235974Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulating Voids","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"David M. Goldberg, Michael S. Vogeley (Drexel)","submitted_at":"2003-07-09T23:08:39Z","abstract_excerpt":"We present a novel method for simulation of the interior of large cosmic voids, suitable for study of the formation and evolution of objects lying within such regions. Following Birkhoff's theorem, void regions dynamically evolve as universes with cosmological parameters that depend on the underdensity of the void. We derive the values of $\\Omega_M$, $\\Omega_{\\Lambda}$, and $H_0$ that describe this evolution. We examine how the growth rate of structure and scale factor in a void differ from the background universe. Together with a prescription for the power spectrum of fluctuations, these equa"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0307191","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/0307191/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/0307191","created_at":"2026-07-04T16:52:08.236035+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0307191v2","created_at":"2026-07-04T16:52:08.236035+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0307191","created_at":"2026-07-04T16:52:08.236035+00:00"},{"alias_kind":"pith_short_12","alias_value":"Q5Z6HVJ7PYJL","created_at":"2026-07-04T16:52:08.236035+00:00"},{"alias_kind":"pith_short_16","alias_value":"Q5Z6HVJ7PYJLQF7M","created_at":"2026-07-04T16:52:08.236035+00:00"},{"alias_kind":"pith_short_8","alias_value":"Q5Z6HVJ7","created_at":"2026-07-04T16:52:08.236035+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.16948","citing_title":"Super sample covariance and the volume scaling of galaxy survey covariance matrices","ref_index":70,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI","json":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI.json","graph_json":"https://pith.science/api/pith-number/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/graph.json","events_json":"https://pith.science/api/pith-number/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/events.json","paper":"https://pith.science/paper/Q5Z6HVJ7"},"agent_actions":{"view_html":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI","download_json":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI.json","view_paper":"https://pith.science/paper/Q5Z6HVJ7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0307191&json=true","fetch_graph":"https://pith.science/api/pith-number/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/graph.json","fetch_events":"https://pith.science/api/pith-number/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/action/storage_attestation","attest_author":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/action/author_attestation","sign_citation":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/action/citation_signature","submit_replication":"https://pith.science/pith/Q5Z6HVJ7PYJLQF7MSA65EHXVEI/action/replication_record"}},"created_at":"2026-07-04T16:52:08.236035+00:00","updated_at":"2026-07-04T16:52:08.236035+00:00"}