{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:72YSI3YHIMA7H7GQPJ5C7QJVCR","short_pith_number":"pith:72YSI3YH","schema_version":"1.0","canonical_sha256":"feb1246f074301f3fcd07a7a2fc135146fb4cc3a4fe1a3891e8ea7c9e3715fc8","source":{"kind":"arxiv","id":"2106.13812","version":1},"attestation_state":"computed","paper":{"title":"The Star Formation Rates of Elliptical Galaxies from Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Garreth Martin, Ivan K. Baldry, Philip A. James, Sugata Kaviraj, Thomas M. Sedgwick","submitted_at":"2021-06-25T18:00:02Z","abstract_excerpt":"The level of star formation in elliptical galaxies is poorly constrained, due to difficulties in quantifying the contamination of flux-based estimates of star formation from unrelated phenomena, such as AGN and old stellar populations. We here utilise core-collapse supernovae (CCSNe) as unambiguous tracers of recent star formation in ellipticals within a cosmic volume. We firstly isolate a sample of 421 z < 0.2, r < 21.8 mag CCSNe from the SDSS-II Supernova Survey. We then introduce a Bayesian method of identifying ellipticals via their colours and morphologies in a manner unbiased by redshift"},"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":"2106.13812","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2021-06-25T18:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"9df2bfb932c83e3debfab440b903231bec602e070c4d8d83384ed0b3d721c5c4","abstract_canon_sha256":"ffea602d17e16d69a305ef26d98269938ca5d86941fbcbee97854a70e2a90d3c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:52:28.912954Z","signature_b64":"b0vPrTOcZIWkNUswRmXx6PAy2hcVqUnugMNb9b1e/pLNq2X3eOt15jPZnFsb/rbNtx8/nm1SikuzJYoxUXIYDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"feb1246f074301f3fcd07a7a2fc135146fb4cc3a4fe1a3891e8ea7c9e3715fc8","last_reissued_at":"2026-07-05T02:52:28.912538Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:52:28.912538Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Star Formation Rates of Elliptical Galaxies from Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Garreth Martin, Ivan K. Baldry, Philip A. James, Sugata Kaviraj, Thomas M. Sedgwick","submitted_at":"2021-06-25T18:00:02Z","abstract_excerpt":"The level of star formation in elliptical galaxies is poorly constrained, due to difficulties in quantifying the contamination of flux-based estimates of star formation from unrelated phenomena, such as AGN and old stellar populations. We here utilise core-collapse supernovae (CCSNe) as unambiguous tracers of recent star formation in ellipticals within a cosmic volume. We firstly isolate a sample of 421 z < 0.2, r < 21.8 mag CCSNe from the SDSS-II Supernova Survey. We then introduce a Bayesian method of identifying ellipticals via their colours and morphologies in a manner unbiased by redshift"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2106.13812","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/2106.13812/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":"2106.13812","created_at":"2026-07-05T02:52:28.912599+00:00"},{"alias_kind":"arxiv_version","alias_value":"2106.13812v1","created_at":"2026-07-05T02:52:28.912599+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2106.13812","created_at":"2026-07-05T02:52:28.912599+00:00"},{"alias_kind":"pith_short_12","alias_value":"72YSI3YHIMA7","created_at":"2026-07-05T02:52:28.912599+00:00"},{"alias_kind":"pith_short_16","alias_value":"72YSI3YHIMA7H7GQ","created_at":"2026-07-05T02:52:28.912599+00:00"},{"alias_kind":"pith_short_8","alias_value":"72YSI3YH","created_at":"2026-07-05T02:52:28.912599+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.21929","citing_title":"MWA and VLA Observations of Diffuse Radio Lobes in M 87","ref_index":107,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR","json":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR.json","graph_json":"https://pith.science/api/pith-number/72YSI3YHIMA7H7GQPJ5C7QJVCR/graph.json","events_json":"https://pith.science/api/pith-number/72YSI3YHIMA7H7GQPJ5C7QJVCR/events.json","paper":"https://pith.science/paper/72YSI3YH"},"agent_actions":{"view_html":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR","download_json":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR.json","view_paper":"https://pith.science/paper/72YSI3YH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2106.13812&json=true","fetch_graph":"https://pith.science/api/pith-number/72YSI3YHIMA7H7GQPJ5C7QJVCR/graph.json","fetch_events":"https://pith.science/api/pith-number/72YSI3YHIMA7H7GQPJ5C7QJVCR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR/action/storage_attestation","attest_author":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR/action/author_attestation","sign_citation":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR/action/citation_signature","submit_replication":"https://pith.science/pith/72YSI3YHIMA7H7GQPJ5C7QJVCR/action/replication_record"}},"created_at":"2026-07-05T02:52:28.912599+00:00","updated_at":"2026-07-05T02:52:28.912599+00:00"}