{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:I63UGP7VADXWG2NXSDJRUKGGSF","short_pith_number":"pith:I63UGP7V","schema_version":"1.0","canonical_sha256":"47b7433ff500ef6369b790d31a28c691446b373a96beb277aa26335853a9c462","source":{"kind":"arxiv","id":"2001.08711","version":1},"attestation_state":"computed","paper":{"title":"The Uncertain Masses of Progenitors of Core Collapse Supernovae and Direct Collapse Black Holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Eoin Farrell, Georges Meynet, JJ Eldridge, Jose Groh","submitted_at":"2020-01-23T18:03:04Z","abstract_excerpt":"We show that it is not possible to determine the final mass $M_{\\rm fin}$ of a red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity $L$ and effective temperature $T_{\\rm eff}$ alone. Using a grid of stellar models, we demonstrate that for a given value of $L$ and $T_{\\rm eff}$, a RSG can have a range of $M_{\\rm fin}$ as wide as 3 to $45~\\mathrm{M}_{\\odot}$. While the probability distribution within these limits is not flat, any individual determination of $M_{\\rm fin}$ for a RSG will be degenerate. This makes it difficult to determine its evolutionary history and to map $M_"},"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":"2001.08711","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2020-01-23T18:03:04Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"42eac12d33823ebe5b0478d6a8fb2be3158e4b048940259547a095d0fe02f21a","abstract_canon_sha256":"1c90d94e074c3d6aa3ad2e792dc5913c61148bef5fb2aa5ae569a97b40b5184f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:43:47.162223Z","signature_b64":"v1gGkmQR6oY+ld8ylYWKMw2wiEXImglos8K7dYTavHK89ejmv64GBd5qP61T55CKodBbAO1lUUnX9g+NF6JvDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"47b7433ff500ef6369b790d31a28c691446b373a96beb277aa26335853a9c462","last_reissued_at":"2026-07-05T00:43:47.161734Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:43:47.161734Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Uncertain Masses of Progenitors of Core Collapse Supernovae and Direct Collapse Black Holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Eoin Farrell, Georges Meynet, JJ Eldridge, Jose Groh","submitted_at":"2020-01-23T18:03:04Z","abstract_excerpt":"We show that it is not possible to determine the final mass $M_{\\rm fin}$ of a red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity $L$ and effective temperature $T_{\\rm eff}$ alone. Using a grid of stellar models, we demonstrate that for a given value of $L$ and $T_{\\rm eff}$, a RSG can have a range of $M_{\\rm fin}$ as wide as 3 to $45~\\mathrm{M}_{\\odot}$. While the probability distribution within these limits is not flat, any individual determination of $M_{\\rm fin}$ for a RSG will be degenerate. This makes it difficult to determine its evolutionary history and to map $M_"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2001.08711","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2001.08711/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":"2001.08711","created_at":"2026-07-05T00:43:47.161792+00:00"},{"alias_kind":"arxiv_version","alias_value":"2001.08711v1","created_at":"2026-07-05T00:43:47.161792+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2001.08711","created_at":"2026-07-05T00:43:47.161792+00:00"},{"alias_kind":"pith_short_12","alias_value":"I63UGP7VADXW","created_at":"2026-07-05T00:43:47.161792+00:00"},{"alias_kind":"pith_short_16","alias_value":"I63UGP7VADXWG2NX","created_at":"2026-07-05T00:43:47.161792+00:00"},{"alias_kind":"pith_short_8","alias_value":"I63UGP7V","created_at":"2026-07-05T00:43:47.161792+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.06614","citing_title":"Evolution and final fates of massive stars","ref_index":27,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF","json":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF.json","graph_json":"https://pith.science/api/pith-number/I63UGP7VADXWG2NXSDJRUKGGSF/graph.json","events_json":"https://pith.science/api/pith-number/I63UGP7VADXWG2NXSDJRUKGGSF/events.json","paper":"https://pith.science/paper/I63UGP7V"},"agent_actions":{"view_html":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF","download_json":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF.json","view_paper":"https://pith.science/paper/I63UGP7V","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2001.08711&json=true","fetch_graph":"https://pith.science/api/pith-number/I63UGP7VADXWG2NXSDJRUKGGSF/graph.json","fetch_events":"https://pith.science/api/pith-number/I63UGP7VADXWG2NXSDJRUKGGSF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF/action/storage_attestation","attest_author":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF/action/author_attestation","sign_citation":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF/action/citation_signature","submit_replication":"https://pith.science/pith/I63UGP7VADXWG2NXSDJRUKGGSF/action/replication_record"}},"created_at":"2026-07-05T00:43:47.161792+00:00","updated_at":"2026-07-05T00:43:47.161792+00:00"}