{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:QJOBKQS6AOKJI4AHIO4ZJE3DOL","short_pith_number":"pith:QJOBKQS6","schema_version":"1.0","canonical_sha256":"825c15425e039494700743b994936372e68f5bcf7cb566901dd5a507803aa4e4","source":{"kind":"arxiv","id":"2303.12405","version":2},"attestation_state":"computed","paper":{"title":"The formation of globular clusters with top-heavy initial mass functions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Hajime Fukushima, Hidenobu Yajima","submitted_at":"2023-03-22T09:16:04Z","abstract_excerpt":"We study the formation of globular clusters in massive compact clouds with the low-metallicity of $Z=10^{-3}~Z_{\\odot}$ by performing three-dimensional radiative-hydrodynamics simulations. Considering the uncertainty of the initial mass function (IMF) of stars formed in low-metallicity and high-density clouds, we investigate the impacts of the IMF on the cloud condition for the GC formation with the range of the power-law index of IMF as $\\gamma = 1-2.35$. We find that the threshold surface density ($\\Sigma_{\\rm thr}$) for the GC formation increases from $800~M_{\\odot} \\; {\\rm pc^{-2}}$ at $\\g"},"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":"2303.12405","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-03-22T09:16:04Z","cross_cats_sorted":[],"title_canon_sha256":"196995c036dede7554b535a6229f06cea7c44fa522c93da51545504c5f15dfd4","abstract_canon_sha256":"61f48f91b948aed69fb5d813346df00263c1aac5f17b3af8d3e286a343f837d7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:29:44.521938Z","signature_b64":"HajS4jAbuw4xa09vNbZn5N1HywuPmCetTbArM301/hmuxCOcbdLUajlYpoufVvRYuTEVPpBFUPMbaJzNIdP4Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"825c15425e039494700743b994936372e68f5bcf7cb566901dd5a507803aa4e4","last_reissued_at":"2026-07-05T06:29:44.521475Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:29:44.521475Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The formation of globular clusters with top-heavy initial mass functions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Hajime Fukushima, Hidenobu Yajima","submitted_at":"2023-03-22T09:16:04Z","abstract_excerpt":"We study the formation of globular clusters in massive compact clouds with the low-metallicity of $Z=10^{-3}~Z_{\\odot}$ by performing three-dimensional radiative-hydrodynamics simulations. Considering the uncertainty of the initial mass function (IMF) of stars formed in low-metallicity and high-density clouds, we investigate the impacts of the IMF on the cloud condition for the GC formation with the range of the power-law index of IMF as $\\gamma = 1-2.35$. We find that the threshold surface density ($\\Sigma_{\\rm thr}$) for the GC formation increases from $800~M_{\\odot} \\; {\\rm pc^{-2}}$ at $\\g"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.12405","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/2303.12405/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":"2303.12405","created_at":"2026-07-05T06:29:44.521532+00:00"},{"alias_kind":"arxiv_version","alias_value":"2303.12405v2","created_at":"2026-07-05T06:29:44.521532+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2303.12405","created_at":"2026-07-05T06:29:44.521532+00:00"},{"alias_kind":"pith_short_12","alias_value":"QJOBKQS6AOKJ","created_at":"2026-07-05T06:29:44.521532+00:00"},{"alias_kind":"pith_short_16","alias_value":"QJOBKQS6AOKJI4AH","created_at":"2026-07-05T06:29:44.521532+00:00"},{"alias_kind":"pith_short_8","alias_value":"QJOBKQS6","created_at":"2026-07-05T06:29:44.521532+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.04176","citing_title":"Star-forming clump detection in nearby galaxies using Faster R-CNN and $ugrizy$ imaging data from CLAUDS and HSC-SSP","ref_index":70,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL","json":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL.json","graph_json":"https://pith.science/api/pith-number/QJOBKQS6AOKJI4AHIO4ZJE3DOL/graph.json","events_json":"https://pith.science/api/pith-number/QJOBKQS6AOKJI4AHIO4ZJE3DOL/events.json","paper":"https://pith.science/paper/QJOBKQS6"},"agent_actions":{"view_html":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL","download_json":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL.json","view_paper":"https://pith.science/paper/QJOBKQS6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2303.12405&json=true","fetch_graph":"https://pith.science/api/pith-number/QJOBKQS6AOKJI4AHIO4ZJE3DOL/graph.json","fetch_events":"https://pith.science/api/pith-number/QJOBKQS6AOKJI4AHIO4ZJE3DOL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL/action/storage_attestation","attest_author":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL/action/author_attestation","sign_citation":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL/action/citation_signature","submit_replication":"https://pith.science/pith/QJOBKQS6AOKJI4AHIO4ZJE3DOL/action/replication_record"}},"created_at":"2026-07-05T06:29:44.521532+00:00","updated_at":"2026-07-05T06:29:44.521532+00:00"}