{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:PFYISVMBQQS2DHXTFEMVSSVRFQ","short_pith_number":"pith:PFYISVMB","schema_version":"1.0","canonical_sha256":"79708955818425a19ef32919594ab12c2bcd8e56c4938541ab9fdb0bbf3c9e07","source":{"kind":"arxiv","id":"1401.2473","version":1},"attestation_state":"computed","paper":{"title":"Star Cluster Formation and Feedback","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Fumitaka Nakamura, Hector G. Arce, James E. Dale, Mark R. Krumholz, Matthew R. Bate, Qizhou Zhang, Richard I. Klein, Robert Gutermuth, Zhi-Yun Li","submitted_at":"2014-01-10T21:42:35Z","abstract_excerpt":"Stars do not generally form in isolation. Instead, they form in clusters, and in these clustered environments newborn stars can have profound effects on one another and on their parent gas clouds. Feedback from clustered stars is almost certainly responsible for a number of otherwise puzzling facts about star formation: that it is an inefficient process that proceeds slowly when averaged over galactic scales; that most stars disperse from their birth sites and dissolve into the galactic field over timescales $\\ll 1$ Gyr; and that newborn stars follow an initial mass function (IMF) with a disti"},"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":"1401.2473","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-01-10T21:42:35Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"1c348cd203abe213298d6f012a5cfd747325e65b21344751a9d9b214f5ac9100","abstract_canon_sha256":"3e0f0303c7ede1d3bad410b0310a043ef80d448767dccb31eed31d1b2853b478"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:45:26.548286Z","signature_b64":"LvZGjDvE3eQDEtNy2Rd0fyGeaNbVNSqzhQbJod8LEBcFHRXCP7/3HwO+Z3ZVUoU0Lt68wV0hM3ZkAE90pBvrDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"79708955818425a19ef32919594ab12c2bcd8e56c4938541ab9fdb0bbf3c9e07","last_reissued_at":"2026-05-18T01:45:26.547856Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:45:26.547856Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Star Cluster Formation and Feedback","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Fumitaka Nakamura, Hector G. Arce, James E. Dale, Mark R. Krumholz, Matthew R. Bate, Qizhou Zhang, Richard I. Klein, Robert Gutermuth, Zhi-Yun Li","submitted_at":"2014-01-10T21:42:35Z","abstract_excerpt":"Stars do not generally form in isolation. Instead, they form in clusters, and in these clustered environments newborn stars can have profound effects on one another and on their parent gas clouds. Feedback from clustered stars is almost certainly responsible for a number of otherwise puzzling facts about star formation: that it is an inefficient process that proceeds slowly when averaged over galactic scales; that most stars disperse from their birth sites and dissolve into the galactic field over timescales $\\ll 1$ Gyr; and that newborn stars follow an initial mass function (IMF) with a disti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1401.2473","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":"1401.2473","created_at":"2026-05-18T01:45:26.547930+00:00"},{"alias_kind":"arxiv_version","alias_value":"1401.2473v1","created_at":"2026-05-18T01:45:26.547930+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1401.2473","created_at":"2026-05-18T01:45:26.547930+00:00"},{"alias_kind":"pith_short_12","alias_value":"PFYISVMBQQS2","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_16","alias_value":"PFYISVMBQQS2DHXT","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_8","alias_value":"PFYISVMB","created_at":"2026-05-18T12:28:43.426989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.13666","citing_title":"Centrally concentrated star formation in young clusters II: Jet feedback","ref_index":141,"is_internal_anchor":true},{"citing_arxiv_id":"2606.03261","citing_title":"A nine-member protostellar system forming via filament fragmentation in the high mass protocluster NGC 6334-43","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10558","citing_title":"Hector Galaxy Survey: Linking the low- and high-mass ends of the initial mass function in star-forming galaxies","ref_index":179,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23802","citing_title":"Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps","ref_index":93,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ","json":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ.json","graph_json":"https://pith.science/api/pith-number/PFYISVMBQQS2DHXTFEMVSSVRFQ/graph.json","events_json":"https://pith.science/api/pith-number/PFYISVMBQQS2DHXTFEMVSSVRFQ/events.json","paper":"https://pith.science/paper/PFYISVMB"},"agent_actions":{"view_html":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ","download_json":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ.json","view_paper":"https://pith.science/paper/PFYISVMB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1401.2473&json=true","fetch_graph":"https://pith.science/api/pith-number/PFYISVMBQQS2DHXTFEMVSSVRFQ/graph.json","fetch_events":"https://pith.science/api/pith-number/PFYISVMBQQS2DHXTFEMVSSVRFQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ/action/storage_attestation","attest_author":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ/action/author_attestation","sign_citation":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ/action/citation_signature","submit_replication":"https://pith.science/pith/PFYISVMBQQS2DHXTFEMVSSVRFQ/action/replication_record"}},"created_at":"2026-05-18T01:45:26.547930+00:00","updated_at":"2026-05-18T01:45:26.547930+00:00"}