{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:FX6J6FLAHYJM5TPN5AWYWHC3JW","short_pith_number":"pith:FX6J6FLA","schema_version":"1.0","canonical_sha256":"2dfc9f15603e12cecdede82d8b1c5b4d9128fe0395b6cf55cf20699a13f94aba","source":{"kind":"arxiv","id":"1803.09822","version":1},"attestation_state":"computed","paper":{"title":"The X_CO conversion factor from galactic multiphase ISM simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Chang-Goo Kim, Eve C. Ostriker, Munan Gong","submitted_at":"2018-03-26T20:12:14Z","abstract_excerpt":"CO(J=1-0) line emission is a widely used observational tracer of molecular gas, rendering essential the X_CO factor, which is applied to convert CO luminosity to H_2 mass. We use numerical simulations to study how X_CO depends on numerical resolution, non-steady-state chemistry, physical environment, and observational beam size. Our study employs 3D magnetohydrodynamics (MHD) simulations of galactic disks with solar neighborhood conditions, where star formation and the three-phase interstellar medium (ISM) are self-consistently regulated by gravity and stellar feedback. Synthetic CO maps are o"},"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":"1803.09822","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-03-26T20:12:14Z","cross_cats_sorted":[],"title_canon_sha256":"7b5e45f80c18fef378a3a112759027bc069256fece73a524d5e85f00972affc8","abstract_canon_sha256":"4d43b1aea3b659e5018b8901c6affcb0f459ff1d07d67dca6e611065d68b2e8d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:15:54.985886Z","signature_b64":"R+0W2N8SPH2tpoeQEZQX4o8jvFC5fMItiL93loxBDtAU/Q5YdVQ+WdCYP0wP4zzv2OlJPBMP4dpWiedQwluhBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2dfc9f15603e12cecdede82d8b1c5b4d9128fe0395b6cf55cf20699a13f94aba","last_reissued_at":"2026-05-18T00:15:54.985160Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:15:54.985160Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The X_CO conversion factor from galactic multiphase ISM simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Chang-Goo Kim, Eve C. Ostriker, Munan Gong","submitted_at":"2018-03-26T20:12:14Z","abstract_excerpt":"CO(J=1-0) line emission is a widely used observational tracer of molecular gas, rendering essential the X_CO factor, which is applied to convert CO luminosity to H_2 mass. We use numerical simulations to study how X_CO depends on numerical resolution, non-steady-state chemistry, physical environment, and observational beam size. Our study employs 3D magnetohydrodynamics (MHD) simulations of galactic disks with solar neighborhood conditions, where star formation and the three-phase interstellar medium (ISM) are self-consistently regulated by gravity and stellar feedback. Synthetic CO maps are o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1803.09822","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":""},"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":"1803.09822","created_at":"2026-05-18T00:15:54.985264+00:00"},{"alias_kind":"arxiv_version","alias_value":"1803.09822v1","created_at":"2026-05-18T00:15:54.985264+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1803.09822","created_at":"2026-05-18T00:15:54.985264+00:00"},{"alias_kind":"pith_short_12","alias_value":"FX6J6FLAHYJM","created_at":"2026-05-18T12:32:25.280505+00:00"},{"alias_kind":"pith_short_16","alias_value":"FX6J6FLAHYJM5TPN","created_at":"2026-05-18T12:32:25.280505+00:00"},{"alias_kind":"pith_short_8","alias_value":"FX6J6FLA","created_at":"2026-05-18T12:32:25.280505+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21101","citing_title":"B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12","ref_index":92,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW","json":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW.json","graph_json":"https://pith.science/api/pith-number/FX6J6FLAHYJM5TPN5AWYWHC3JW/graph.json","events_json":"https://pith.science/api/pith-number/FX6J6FLAHYJM5TPN5AWYWHC3JW/events.json","paper":"https://pith.science/paper/FX6J6FLA"},"agent_actions":{"view_html":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW","download_json":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW.json","view_paper":"https://pith.science/paper/FX6J6FLA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1803.09822&json=true","fetch_graph":"https://pith.science/api/pith-number/FX6J6FLAHYJM5TPN5AWYWHC3JW/graph.json","fetch_events":"https://pith.science/api/pith-number/FX6J6FLAHYJM5TPN5AWYWHC3JW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW/action/storage_attestation","attest_author":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW/action/author_attestation","sign_citation":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW/action/citation_signature","submit_replication":"https://pith.science/pith/FX6J6FLAHYJM5TPN5AWYWHC3JW/action/replication_record"}},"created_at":"2026-05-18T00:15:54.985264+00:00","updated_at":"2026-05-18T00:15:54.985264+00:00"}