{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:VUA6BX4KHXDL6N6I6G4XUFFMHP","short_pith_number":"pith:VUA6BX4K","schema_version":"1.0","canonical_sha256":"ad01e0df8a3dc6bf37c8f1b97a14ac3bf1e80ea048886b3df0706b1674c98fe8","source":{"kind":"arxiv","id":"2208.14110","version":1},"attestation_state":"computed","paper":{"title":"The proper motion of stars in dwarf galaxies: distinguishing central density cusps from cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Antonaldo Diaferio, Ivan de Martino, Luisa Ostorero","submitted_at":"2022-08-30T09:47:06Z","abstract_excerpt":"We show that measuring the proper motion of ${{\\sim 2000}}$ stars within a dwarf galaxy, with an uncertainty of 1 km/s at most, can establish whether the Dark Matter (DM) density profile of the dwarf has a central core or cusp. We derive these limits by building mock star catalogues similar to those expected from future astrometric {\\it Theia}-like missions and including celestial coordinates, radial velocity and proper motion of the stars. The density field of the DM halo of the dwarf is sampled from an extended Navarro-Frank-White (eNWF) spherical model, whereas the number density distributi"},"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":"2208.14110","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-08-30T09:47:06Z","cross_cats_sorted":[],"title_canon_sha256":"cc5d1e315592b55634df1d2be8c139de17148ce479da61af10fc0137893c3ef7","abstract_canon_sha256":"ee958501143a9ad6adca177cb154375020dcdbc0a0725490119c46269acbab93"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:53:08.893693Z","signature_b64":"zoayx9LnAhQt/hhGMbGVlUr/SumFfwevh0Vd984b17RUgjk0VsNdKVlC75gMRySunfQAxia/bHEeL62+96OaBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ad01e0df8a3dc6bf37c8f1b97a14ac3bf1e80ea048886b3df0706b1674c98fe8","last_reissued_at":"2026-07-05T04:53:08.893298Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:53:08.893298Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The proper motion of stars in dwarf galaxies: distinguishing central density cusps from cores","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Antonaldo Diaferio, Ivan de Martino, Luisa Ostorero","submitted_at":"2022-08-30T09:47:06Z","abstract_excerpt":"We show that measuring the proper motion of ${{\\sim 2000}}$ stars within a dwarf galaxy, with an uncertainty of 1 km/s at most, can establish whether the Dark Matter (DM) density profile of the dwarf has a central core or cusp. We derive these limits by building mock star catalogues similar to those expected from future astrometric {\\it Theia}-like missions and including celestial coordinates, radial velocity and proper motion of the stars. The density field of the DM halo of the dwarf is sampled from an extended Navarro-Frank-White (eNWF) spherical model, whereas the number density distributi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2208.14110","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/2208.14110/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":"2208.14110","created_at":"2026-07-05T04:53:08.893379+00:00"},{"alias_kind":"arxiv_version","alias_value":"2208.14110v1","created_at":"2026-07-05T04:53:08.893379+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2208.14110","created_at":"2026-07-05T04:53:08.893379+00:00"},{"alias_kind":"pith_short_12","alias_value":"VUA6BX4KHXDL","created_at":"2026-07-05T04:53:08.893379+00:00"},{"alias_kind":"pith_short_16","alias_value":"VUA6BX4KHXDL6N6I","created_at":"2026-07-05T04:53:08.893379+00:00"},{"alias_kind":"pith_short_8","alias_value":"VUA6BX4K","created_at":"2026-07-05T04:53:08.893379+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.21986","citing_title":"Dwarf galaxies in non-local gravity","ref_index":45,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP","json":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP.json","graph_json":"https://pith.science/api/pith-number/VUA6BX4KHXDL6N6I6G4XUFFMHP/graph.json","events_json":"https://pith.science/api/pith-number/VUA6BX4KHXDL6N6I6G4XUFFMHP/events.json","paper":"https://pith.science/paper/VUA6BX4K"},"agent_actions":{"view_html":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP","download_json":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP.json","view_paper":"https://pith.science/paper/VUA6BX4K","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2208.14110&json=true","fetch_graph":"https://pith.science/api/pith-number/VUA6BX4KHXDL6N6I6G4XUFFMHP/graph.json","fetch_events":"https://pith.science/api/pith-number/VUA6BX4KHXDL6N6I6G4XUFFMHP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP/action/storage_attestation","attest_author":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP/action/author_attestation","sign_citation":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP/action/citation_signature","submit_replication":"https://pith.science/pith/VUA6BX4KHXDL6N6I6G4XUFFMHP/action/replication_record"}},"created_at":"2026-07-05T04:53:08.893379+00:00","updated_at":"2026-07-05T04:53:08.893379+00:00"}