{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:OF4CC4JV3I7KJGX3QQFHJABFYT","short_pith_number":"pith:OF4CC4JV","schema_version":"1.0","canonical_sha256":"7178217135da3ea49afb840a748025c4ca52756375599e4234658948b1f656ad","source":{"kind":"arxiv","id":"0908.2995","version":6},"attestation_state":"computed","paper":{"title":"Accurate masses for dispersion-supported galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Frank F. Avedo, Gregory D. Martinez, James S. Bullock, Joe Wolf, Joshua D. Simon, Manoj Kaplinghat, Marla Geha, Ricardo R. Munoz","submitted_at":"2009-08-21T16:09:41Z","abstract_excerpt":"We derive an accurate mass estimator for dispersion-supported stellar systems and demonstrate its validity by analyzing resolved line-of-sight velocity data for globular clusters, dwarf galaxies, and elliptical galaxies. Specifically, by manipulating the spherical Jeans equation we show that the dynamical mass enclosed within the 3D deprojected half-light radius r_1/2 can be determined with only mild assumptions about the spatial variation of the stellar velocity dispersion anisotropy. We find M_1/2 = 3 \\sigma_los^2 r_1/2 / G ~ 4 \\sigma_los^2 R_eff / G, where \\sigma_los^2 is the luminosity-wei"},"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":"0908.2995","kind":"arxiv","version":6},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-08-21T16:09:41Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"c31baa2b2a30fcba161ddb45c282b5f2f3e68357a37e3b0d25ed8a376917e261","abstract_canon_sha256":"f9c999cddbc043037647e6f0d7a21cb76ae20da631a0df39e58ac335e81c9027"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:12:24.626641Z","signature_b64":"x2GszRGoXe+9F72lkrnHBeGqiKUia4z0EzUMJ9ETit9OzElZdRnChFAPa9IXt9OtQ5tJLrwp94Rje3sXwMdCBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7178217135da3ea49afb840a748025c4ca52756375599e4234658948b1f656ad","last_reissued_at":"2026-05-18T02:12:24.625858Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:12:24.625858Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Accurate masses for dispersion-supported galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Frank F. Avedo, Gregory D. Martinez, James S. Bullock, Joe Wolf, Joshua D. Simon, Manoj Kaplinghat, Marla Geha, Ricardo R. Munoz","submitted_at":"2009-08-21T16:09:41Z","abstract_excerpt":"We derive an accurate mass estimator for dispersion-supported stellar systems and demonstrate its validity by analyzing resolved line-of-sight velocity data for globular clusters, dwarf galaxies, and elliptical galaxies. Specifically, by manipulating the spherical Jeans equation we show that the dynamical mass enclosed within the 3D deprojected half-light radius r_1/2 can be determined with only mild assumptions about the spatial variation of the stellar velocity dispersion anisotropy. We find M_1/2 = 3 \\sigma_los^2 r_1/2 / G ~ 4 \\sigma_los^2 R_eff / G, where \\sigma_los^2 is the luminosity-wei"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0908.2995","kind":"arxiv","version":6},"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":"0908.2995","created_at":"2026-05-18T02:12:24.625998+00:00"},{"alias_kind":"arxiv_version","alias_value":"0908.2995v6","created_at":"2026-05-18T02:12:24.625998+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0908.2995","created_at":"2026-05-18T02:12:24.625998+00:00"},{"alias_kind":"pith_short_12","alias_value":"OF4CC4JV3I7K","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_16","alias_value":"OF4CC4JV3I7KJGX3","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_8","alias_value":"OF4CC4JV","created_at":"2026-05-18T12:26:01.383474+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.22685","citing_title":"Dwarf Galaxy Constraints on Interacting Fermionic Dark Matter","ref_index":18,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15330","citing_title":"A metric solution for rotating black holes embedded in dark matter halos with central spikes","ref_index":11,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT","json":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT.json","graph_json":"https://pith.science/api/pith-number/OF4CC4JV3I7KJGX3QQFHJABFYT/graph.json","events_json":"https://pith.science/api/pith-number/OF4CC4JV3I7KJGX3QQFHJABFYT/events.json","paper":"https://pith.science/paper/OF4CC4JV"},"agent_actions":{"view_html":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT","download_json":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT.json","view_paper":"https://pith.science/paper/OF4CC4JV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0908.2995&json=true","fetch_graph":"https://pith.science/api/pith-number/OF4CC4JV3I7KJGX3QQFHJABFYT/graph.json","fetch_events":"https://pith.science/api/pith-number/OF4CC4JV3I7KJGX3QQFHJABFYT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT/action/storage_attestation","attest_author":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT/action/author_attestation","sign_citation":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT/action/citation_signature","submit_replication":"https://pith.science/pith/OF4CC4JV3I7KJGX3QQFHJABFYT/action/replication_record"}},"created_at":"2026-05-18T02:12:24.625998+00:00","updated_at":"2026-05-18T02:12:24.625998+00:00"}