{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:JKMP2EH36J3CLRVJKJUU3SV5FD","short_pith_number":"pith:JKMP2EH3","schema_version":"1.0","canonical_sha256":"4a98fd10fbf27625c6a952694dcabd28dd057120e449e4c9fe1024ce0e220102","source":{"kind":"arxiv","id":"1110.0484","version":2},"attestation_state":"computed","paper":{"title":"Structure and Dynamics of the Globular Cluster Palomar 13","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"E. Kirby, F. A. Santana, J. D. Bradford, J. D. Simon, M. Geha, P. B. Stetson, P. Cote, R. Munoz, S. G. Djorgovski","submitted_at":"2011-10-03T20:16:18Z","abstract_excerpt":"We present Keck/DEIMOS spectroscopy and CFHT/MegaCam photometry for the Milky Way globular cluster Palomar 13. We triple the number of spectroscopically confirmed members, including many repeat velocity measurements. Palomar 13 is the only known globular cluster with possible evidence for dark matter, based on a Keck/HIRES 21 star velocity dispersion of sigma=2.2+/-0.4 km/s. We reproduce this measurement, but demonstrate that it is inflated by unresolved binary stars. For our sample of 61 stars, the velocity dispersion is sigma=0.7(+0.6/-0.5) km/s. Combining our DEIMOS data with literature val"},"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":"1110.0484","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-10-03T20:16:18Z","cross_cats_sorted":[],"title_canon_sha256":"ff1a3d83cac5b14c21e9f9d0c800134370c6fabdd73e72e9ed1d8b435a1a70b0","abstract_canon_sha256":"35453180615e99d304dcb0e54e4ca46c66a073bd2992a5fb72bd459cbcb50a8b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:00:18.468939Z","signature_b64":"bYxQ2A8XZRCzU9AhSfEGVN5g13y1o4hydXzB8T5Lz7+aKE6Q0UEmCY1AYy93dAetv1LwBJvpOB/yJwPjHBEfCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4a98fd10fbf27625c6a952694dcabd28dd057120e449e4c9fe1024ce0e220102","last_reissued_at":"2026-05-18T02:00:18.468444Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:00:18.468444Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Structure and Dynamics of the Globular Cluster Palomar 13","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"E. Kirby, F. A. Santana, J. D. Bradford, J. D. Simon, M. Geha, P. B. Stetson, P. Cote, R. Munoz, S. G. Djorgovski","submitted_at":"2011-10-03T20:16:18Z","abstract_excerpt":"We present Keck/DEIMOS spectroscopy and CFHT/MegaCam photometry for the Milky Way globular cluster Palomar 13. We triple the number of spectroscopically confirmed members, including many repeat velocity measurements. Palomar 13 is the only known globular cluster with possible evidence for dark matter, based on a Keck/HIRES 21 star velocity dispersion of sigma=2.2+/-0.4 km/s. We reproduce this measurement, but demonstrate that it is inflated by unresolved binary stars. For our sample of 61 stars, the velocity dispersion is sigma=0.7(+0.6/-0.5) km/s. Combining our DEIMOS data with literature val"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1110.0484","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":""},"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":"1110.0484","created_at":"2026-05-18T02:00:18.468533+00:00"},{"alias_kind":"arxiv_version","alias_value":"1110.0484v2","created_at":"2026-05-18T02:00:18.468533+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1110.0484","created_at":"2026-05-18T02:00:18.468533+00:00"},{"alias_kind":"pith_short_12","alias_value":"JKMP2EH36J3C","created_at":"2026-05-18T12:26:32.869790+00:00"},{"alias_kind":"pith_short_16","alias_value":"JKMP2EH36J3CLRVJ","created_at":"2026-05-18T12:26:32.869790+00:00"},{"alias_kind":"pith_short_8","alias_value":"JKMP2EH3","created_at":"2026-05-18T12:26:32.869790+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.01464","citing_title":"New Venues in Formation and Detection for Primordial Black Hole Dark Matter","ref_index":52,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD","json":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD.json","graph_json":"https://pith.science/api/pith-number/JKMP2EH36J3CLRVJKJUU3SV5FD/graph.json","events_json":"https://pith.science/api/pith-number/JKMP2EH36J3CLRVJKJUU3SV5FD/events.json","paper":"https://pith.science/paper/JKMP2EH3"},"agent_actions":{"view_html":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD","download_json":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD.json","view_paper":"https://pith.science/paper/JKMP2EH3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1110.0484&json=true","fetch_graph":"https://pith.science/api/pith-number/JKMP2EH36J3CLRVJKJUU3SV5FD/graph.json","fetch_events":"https://pith.science/api/pith-number/JKMP2EH36J3CLRVJKJUU3SV5FD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD/action/storage_attestation","attest_author":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD/action/author_attestation","sign_citation":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD/action/citation_signature","submit_replication":"https://pith.science/pith/JKMP2EH36J3CLRVJKJUU3SV5FD/action/replication_record"}},"created_at":"2026-05-18T02:00:18.468533+00:00","updated_at":"2026-05-18T02:00:18.468533+00:00"}