{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:AL52BDKO2HTAIB4DR6TXPH6SO5","short_pith_number":"pith:AL52BDKO","schema_version":"1.0","canonical_sha256":"02fba08d4ed1e60407838fa7779fd2774f6802024fadb4e0783f3dbfb8f9993f","source":{"kind":"arxiv","id":"0808.3902","version":2},"attestation_state":"computed","paper":{"title":"A lower bound on the mass of Dark Matter particles","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph"],"primary_cat":"hep-ph","authors_text":"Alexey Boyarsky, Dmytro Iakubovskyi, Oleg Ruchayskiy","submitted_at":"2008-08-28T14:51:47Z","abstract_excerpt":"We discuss the bounds on the mass of Dark Matter (DM) particles, coming from the analysis of DM phase-space distribution in dwarf spheroidal galaxies (dSphs). After reviewing the existing approaches, we choose two methods to derive such a bound. The first one depends on the information about the current phase space distribution of DM particles only, while the second one uses both the initial and final distributions. We discuss the recent data on dSphs as well as astronomical uncertainties in relevant parameters. As an application, we present lower bounds on the mass of DM particles, coming fro"},"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":"0808.3902","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2008-08-28T14:51:47Z","cross_cats_sorted":["astro-ph"],"title_canon_sha256":"b5bcdaa47021d652a493f0a5a7efc2e6545100ae150f03305a3262773bd7479c","abstract_canon_sha256":"a5217dd61b59e7e95abe6f66f26df61aad81c81173df5d8da229c76b993eaea0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:40:23.086191Z","signature_b64":"MVGCjW/UTn4lcpMFlsUgMJS8IL6AoFzEZMC5tkBXPXc0pQWfxiDdB21a7C/zhlPb4fWL06lBh9A2ln0AXo8uCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"02fba08d4ed1e60407838fa7779fd2774f6802024fadb4e0783f3dbfb8f9993f","last_reissued_at":"2026-07-04T15:40:23.085781Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:40:23.085781Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A lower bound on the mass of Dark Matter particles","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph"],"primary_cat":"hep-ph","authors_text":"Alexey Boyarsky, Dmytro Iakubovskyi, Oleg Ruchayskiy","submitted_at":"2008-08-28T14:51:47Z","abstract_excerpt":"We discuss the bounds on the mass of Dark Matter (DM) particles, coming from the analysis of DM phase-space distribution in dwarf spheroidal galaxies (dSphs). After reviewing the existing approaches, we choose two methods to derive such a bound. The first one depends on the information about the current phase space distribution of DM particles only, while the second one uses both the initial and final distributions. We discuss the recent data on dSphs as well as astronomical uncertainties in relevant parameters. As an application, we present lower bounds on the mass of DM particles, coming fro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0808.3902","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0808.3902/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":"0808.3902","created_at":"2026-07-04T15:40:23.085848+00:00"},{"alias_kind":"arxiv_version","alias_value":"0808.3902v2","created_at":"2026-07-04T15:40:23.085848+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0808.3902","created_at":"2026-07-04T15:40:23.085848+00:00"},{"alias_kind":"pith_short_12","alias_value":"AL52BDKO2HTA","created_at":"2026-07-04T15:40:23.085848+00:00"},{"alias_kind":"pith_short_16","alias_value":"AL52BDKO2HTAIB4D","created_at":"2026-07-04T15:40:23.085848+00:00"},{"alias_kind":"pith_short_8","alias_value":"AL52BDKO","created_at":"2026-07-04T15:40:23.085848+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"1906.10316","citing_title":"Constraining light fermionic dark matter with binary pulsars","ref_index":45,"is_internal_anchor":true},{"citing_arxiv_id":"2605.22685","citing_title":"Dwarf Galaxy Constraints on Interacting Fermionic Dark Matter","ref_index":22,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5","json":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5.json","graph_json":"https://pith.science/api/pith-number/AL52BDKO2HTAIB4DR6TXPH6SO5/graph.json","events_json":"https://pith.science/api/pith-number/AL52BDKO2HTAIB4DR6TXPH6SO5/events.json","paper":"https://pith.science/paper/AL52BDKO"},"agent_actions":{"view_html":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5","download_json":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5.json","view_paper":"https://pith.science/paper/AL52BDKO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0808.3902&json=true","fetch_graph":"https://pith.science/api/pith-number/AL52BDKO2HTAIB4DR6TXPH6SO5/graph.json","fetch_events":"https://pith.science/api/pith-number/AL52BDKO2HTAIB4DR6TXPH6SO5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5/action/storage_attestation","attest_author":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5/action/author_attestation","sign_citation":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5/action/citation_signature","submit_replication":"https://pith.science/pith/AL52BDKO2HTAIB4DR6TXPH6SO5/action/replication_record"}},"created_at":"2026-07-04T15:40:23.085848+00:00","updated_at":"2026-07-04T15:40:23.085848+00:00"}