{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:6QFRTTDRAVIQ4QXWB2D6FDRXGA","short_pith_number":"pith:6QFRTTDR","schema_version":"1.0","canonical_sha256":"f40b19cc7105510e42f60e87e28e37301d82af69694504f74ef54835cf7ac118","source":{"kind":"arxiv","id":"2104.10892","version":2},"attestation_state":"computed","paper":{"title":"Radiation hydrodynamics simulations of massive star cluster formation in giant molecular clouds","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Hajime Fukushima, Hidenobu Yajima","submitted_at":"2021-04-22T06:50:45Z","abstract_excerpt":"By performing three-dimensional radiation hydrodynamics simulations, we study the formation of young massive star clusters (YMCs, $M_{*}>10^4~M_{\\odot}$) in clouds with the surface density ranging from $\\Sigma_{\\rm cl} = 80$ to $3200~M_{\\odot}\\;{\\rm pc^{-2}}$. We find that photoionization feedback suppresses star formation significantly in clouds with low surface density. Once the initial surface density exceeds $\\sim 100~M_{\\odot}\\;{\\rm pc^{-2}}$ for clouds with $M_{\\rm cl}=10^{6}~M_{\\odot}$ and $Z= Z_{\\odot}$, most of the gas is converted into stars because the photoionization feedback is in"},"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":"2104.10892","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2021-04-22T06:50:45Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"f914539501b2ae5e6a2a3a3ac17f0c6cab2b0e65114b5f43c4d8a89483fcfe5d","abstract_canon_sha256":"1c5fc0438dfd342b819451f763ea99e54c48cccf056f306c26067b7f0a3d1a60"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:06:24.269182Z","signature_b64":"T2MiZ853aQiWkzL/um6F/S/VWc3Fc1ruGVtJ6xT5ApWUsQGvt23sk4rj4QAISA2sm0a6b25OERI7Rg9TCXv8Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f40b19cc7105510e42f60e87e28e37301d82af69694504f74ef54835cf7ac118","last_reissued_at":"2026-07-05T03:06:24.268715Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:06:24.268715Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radiation hydrodynamics simulations of massive star cluster formation in giant molecular clouds","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Hajime Fukushima, Hidenobu Yajima","submitted_at":"2021-04-22T06:50:45Z","abstract_excerpt":"By performing three-dimensional radiation hydrodynamics simulations, we study the formation of young massive star clusters (YMCs, $M_{*}>10^4~M_{\\odot}$) in clouds with the surface density ranging from $\\Sigma_{\\rm cl} = 80$ to $3200~M_{\\odot}\\;{\\rm pc^{-2}}$. We find that photoionization feedback suppresses star formation significantly in clouds with low surface density. Once the initial surface density exceeds $\\sim 100~M_{\\odot}\\;{\\rm pc^{-2}}$ for clouds with $M_{\\rm cl}=10^{6}~M_{\\odot}$ and $Z= Z_{\\odot}$, most of the gas is converted into stars because the photoionization feedback is in"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2104.10892","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/2104.10892/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":"2104.10892","created_at":"2026-07-05T03:06:24.268770+00:00"},{"alias_kind":"arxiv_version","alias_value":"2104.10892v2","created_at":"2026-07-05T03:06:24.268770+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2104.10892","created_at":"2026-07-05T03:06:24.268770+00:00"},{"alias_kind":"pith_short_12","alias_value":"6QFRTTDRAVIQ","created_at":"2026-07-05T03:06:24.268770+00:00"},{"alias_kind":"pith_short_16","alias_value":"6QFRTTDRAVIQ4QXW","created_at":"2026-07-05T03:06:24.268770+00:00"},{"alias_kind":"pith_short_8","alias_value":"6QFRTTDR","created_at":"2026-07-05T03:06:24.268770+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.22161","citing_title":"Blue-tilted Runnings and the JWST Early Galaxy Tension","ref_index":28,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22161","citing_title":"Blue-tilted Runnings and the JWST Early Galaxy Tension","ref_index":24,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA","json":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA.json","graph_json":"https://pith.science/api/pith-number/6QFRTTDRAVIQ4QXWB2D6FDRXGA/graph.json","events_json":"https://pith.science/api/pith-number/6QFRTTDRAVIQ4QXWB2D6FDRXGA/events.json","paper":"https://pith.science/paper/6QFRTTDR"},"agent_actions":{"view_html":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA","download_json":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA.json","view_paper":"https://pith.science/paper/6QFRTTDR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2104.10892&json=true","fetch_graph":"https://pith.science/api/pith-number/6QFRTTDRAVIQ4QXWB2D6FDRXGA/graph.json","fetch_events":"https://pith.science/api/pith-number/6QFRTTDRAVIQ4QXWB2D6FDRXGA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA/action/storage_attestation","attest_author":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA/action/author_attestation","sign_citation":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA/action/citation_signature","submit_replication":"https://pith.science/pith/6QFRTTDRAVIQ4QXWB2D6FDRXGA/action/replication_record"}},"created_at":"2026-07-05T03:06:24.268770+00:00","updated_at":"2026-07-05T03:06:24.268770+00:00"}