{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:RI4ALYGJJYI4V7EECW7HGKODR5","short_pith_number":"pith:RI4ALYGJ","schema_version":"1.0","canonical_sha256":"8a3805e0c94e11cafc8415be7329c38f643d3083608e7c583846d812ae4ddd26","source":{"kind":"arxiv","id":"1002.1705","version":1},"attestation_state":"computed","paper":{"title":"The M-Sigma Relation Derived from Sphere of Influence Arguments","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"D. Batcheldor (Florida Institute of Technology)","submitted_at":"2010-02-08T20:18:55Z","abstract_excerpt":"The observed relation between supermassive black hole (SMBH) mass (M) and bulge stellar velocity dispersion (Sigma) is described by log(M) = alpha + beta*log(Sigma/200 km/s). As this relation has important implications for models of galaxy and SMBH formation and evolution, there continues to be great interest in adding to the M catalog. The \"sphere of influence\" (r) argument uses spatial resolution to exclude some M estimates and pre-select additional galaxies for further SMBH studies. This Letter quantifies the effects of applying the r argument to a population of galaxies and SMBHs that do n"},"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":"1002.1705","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-02-08T20:18:55Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"1d5234a5c5952b51f239d7d9076d9eab37cabe9cbfac555ed311f0617eedec7a","abstract_canon_sha256":"69e8e3b3fc33241134a280fde6fbc40ae8171b293c0c53148d04e670e5a6127d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:09:11.152741Z","signature_b64":"7s54LBJ5HQfSgiKoEIpTLLJmhF2yWf5GeA4JNm2j55Xn/krTN7V2IWlId4nIAK0T+HHz/iscn/stJ6zzC5rVAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8a3805e0c94e11cafc8415be7329c38f643d3083608e7c583846d812ae4ddd26","last_reissued_at":"2026-05-18T02:09:11.152039Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:09:11.152039Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The M-Sigma Relation Derived from Sphere of Influence Arguments","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"D. Batcheldor (Florida Institute of Technology)","submitted_at":"2010-02-08T20:18:55Z","abstract_excerpt":"The observed relation between supermassive black hole (SMBH) mass (M) and bulge stellar velocity dispersion (Sigma) is described by log(M) = alpha + beta*log(Sigma/200 km/s). As this relation has important implications for models of galaxy and SMBH formation and evolution, there continues to be great interest in adding to the M catalog. The \"sphere of influence\" (r) argument uses spatial resolution to exclude some M estimates and pre-select additional galaxies for further SMBH studies. This Letter quantifies the effects of applying the r argument to a population of galaxies and SMBHs that do n"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1002.1705","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":"1002.1705","created_at":"2026-05-18T02:09:11.152138+00:00"},{"alias_kind":"arxiv_version","alias_value":"1002.1705v1","created_at":"2026-05-18T02:09:11.152138+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1002.1705","created_at":"2026-05-18T02:09:11.152138+00:00"},{"alias_kind":"pith_short_12","alias_value":"RI4ALYGJJYI4","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_16","alias_value":"RI4ALYGJJYI4V7EE","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_8","alias_value":"RI4ALYGJ","created_at":"2026-05-18T12:26:13.927090+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.08041","citing_title":"Uncertainties in the supermassive black hole abundance and implications for the GW background","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5","json":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5.json","graph_json":"https://pith.science/api/pith-number/RI4ALYGJJYI4V7EECW7HGKODR5/graph.json","events_json":"https://pith.science/api/pith-number/RI4ALYGJJYI4V7EECW7HGKODR5/events.json","paper":"https://pith.science/paper/RI4ALYGJ"},"agent_actions":{"view_html":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5","download_json":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5.json","view_paper":"https://pith.science/paper/RI4ALYGJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1002.1705&json=true","fetch_graph":"https://pith.science/api/pith-number/RI4ALYGJJYI4V7EECW7HGKODR5/graph.json","fetch_events":"https://pith.science/api/pith-number/RI4ALYGJJYI4V7EECW7HGKODR5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5/action/storage_attestation","attest_author":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5/action/author_attestation","sign_citation":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5/action/citation_signature","submit_replication":"https://pith.science/pith/RI4ALYGJJYI4V7EECW7HGKODR5/action/replication_record"}},"created_at":"2026-05-18T02:09:11.152138+00:00","updated_at":"2026-05-18T02:09:11.152138+00:00"}