{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:BY5NAJJNF4MGOASPU2AJI5LC43","short_pith_number":"pith:BY5NAJJN","schema_version":"1.0","canonical_sha256":"0e3ad0252d2f1867024fa680947562e6c14c31de574cfce453f7315d278ccdaf","source":{"kind":"arxiv","id":"astro-ph/0301645","version":3},"attestation_state":"computed","paper":{"title":"Simulations of Early Structure Formation: Primordial Gas Clouds","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Lars Hernquist (CfA), Naoki Yoshida (CfA), Naoshi Sugiyama (NAOJ), Tom Abel (Penn State)","submitted_at":"2003-01-31T14:52:04Z","abstract_excerpt":"(abridged) We use large cosmological simulations to study the origin of primordial star-forming clouds in a Lambda CDM universe, by following the formation of dark matter halos and the cooling of gas within them. To model the physics of chemically pristine gas, we employ a non-equilibrium treatment of the chemistry of 9 species and include cooling by molecular hydrogen. We explore the hierarchical growth of bound structures forming at redshifts z = 25 - 30 with total masses in the range 10^5 - 10^6 Msun. The complex interplay between the gravitational formation of dark halos and the thermodyna"},"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/0301645","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-01-31T14:52:04Z","cross_cats_sorted":[],"title_canon_sha256":"40aa1cdeeedd5d28a0a06ef816761182160033dc8bd2d4582b45bcc51156d379","abstract_canon_sha256":"9ce87be41139a75d6144f7d94580603e62d3733a32d1fe50ee2033e8718bd040"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:36:25.333819Z","signature_b64":"DJWZ/zOcJxPpfZi3ObNXyCWo04OlRt2kAfYY0r9YyEBtgWYEE79kVloEZMeQ0mzoTbJeNmcN0gllsWo4FMKKDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0e3ad0252d2f1867024fa680947562e6c14c31de574cfce453f7315d278ccdaf","last_reissued_at":"2026-07-04T16:36:25.333200Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:36:25.333200Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulations of Early Structure Formation: Primordial Gas Clouds","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Lars Hernquist (CfA), Naoki Yoshida (CfA), Naoshi Sugiyama (NAOJ), Tom Abel (Penn State)","submitted_at":"2003-01-31T14:52:04Z","abstract_excerpt":"(abridged) We use large cosmological simulations to study the origin of primordial star-forming clouds in a Lambda CDM universe, by following the formation of dark matter halos and the cooling of gas within them. To model the physics of chemically pristine gas, we employ a non-equilibrium treatment of the chemistry of 9 species and include cooling by molecular hydrogen. We explore the hierarchical growth of bound structures forming at redshifts z = 25 - 30 with total masses in the range 10^5 - 10^6 Msun. The complex interplay between the gravitational formation of dark halos and the thermodyna"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0301645","kind":"arxiv","version":3},"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/0301645/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/0301645","created_at":"2026-07-04T16:36:25.333259+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0301645v3","created_at":"2026-07-04T16:36:25.333259+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0301645","created_at":"2026-07-04T16:36:25.333259+00:00"},{"alias_kind":"pith_short_12","alias_value":"BY5NAJJNF4MG","created_at":"2026-07-04T16:36:25.333259+00:00"},{"alias_kind":"pith_short_16","alias_value":"BY5NAJJNF4MGOASP","created_at":"2026-07-04T16:36:25.333259+00:00"},{"alias_kind":"pith_short_8","alias_value":"BY5NAJJN","created_at":"2026-07-04T16:36:25.333259+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.00205","citing_title":"Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages","ref_index":113,"is_internal_anchor":true},{"citing_arxiv_id":"2606.00219","citing_title":"21cmEMUv3: a hybrid diffusion-LSTM emulator of 21cmFAST summary observables","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15310","citing_title":"Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization","ref_index":249,"is_internal_anchor":true},{"citing_arxiv_id":"2509.25325","citing_title":"Direct Collapse Black Hole Candidates from Decaying Dark Matter","ref_index":69,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43","json":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43.json","graph_json":"https://pith.science/api/pith-number/BY5NAJJNF4MGOASPU2AJI5LC43/graph.json","events_json":"https://pith.science/api/pith-number/BY5NAJJNF4MGOASPU2AJI5LC43/events.json","paper":"https://pith.science/paper/BY5NAJJN"},"agent_actions":{"view_html":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43","download_json":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43.json","view_paper":"https://pith.science/paper/BY5NAJJN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0301645&json=true","fetch_graph":"https://pith.science/api/pith-number/BY5NAJJNF4MGOASPU2AJI5LC43/graph.json","fetch_events":"https://pith.science/api/pith-number/BY5NAJJNF4MGOASPU2AJI5LC43/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43/action/storage_attestation","attest_author":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43/action/author_attestation","sign_citation":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43/action/citation_signature","submit_replication":"https://pith.science/pith/BY5NAJJNF4MGOASPU2AJI5LC43/action/replication_record"}},"created_at":"2026-07-04T16:36:25.333259+00:00","updated_at":"2026-07-04T16:36:25.333259+00:00"}