{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:NJNXZTEBN6MPBZNMZXSAFGW4IS","short_pith_number":"pith:NJNXZTEB","schema_version":"1.0","canonical_sha256":"6a5b7ccc816f98f0e5accde4029adc449b7d506f6d6015438adb411ba81b510e","source":{"kind":"arxiv","id":"hep-ph/0507288","version":2},"attestation_state":"computed","paper":{"title":"Dark Energy and Dark Matter in Galaxy Halos","license":"","headline":"","cross_cats":["astro-ph","hep-th"],"primary_cat":"hep-ph","authors_text":"N. Tetradis","submitted_at":"2005-07-25T18:32:01Z","abstract_excerpt":"We consider the possibility that the dark matter is coupled through its mass to a scalar field associated with the dark energy of the Universe. In order for such a field to play a role at the present cosmological distances, it must be effectively massless at galactic length scales. We discuss the effects of the field on the distribution of dark matter in galaxy halos. We show that the profile of the distribution outside the galaxy core remains largely unaffected and the approximately flat rotation curves persist. The dispersion of the dark matter velocity is enhanced by a potentially large fac"},"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":"hep-ph/0507288","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"hep-ph","submitted_at":"2005-07-25T18:32:01Z","cross_cats_sorted":["astro-ph","hep-th"],"title_canon_sha256":"01e6c227f76f91a53927fe216f641f8e48fc53c2249ad0b0423de1a9995a30b3","abstract_canon_sha256":"7639d6bbb0bd3b98506da125f8bbc5f37bbb521d1cf0491d2a99fd37e2e03834"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:55:46.476241Z","signature_b64":"AZKF/r4eHjqbtIjfc5lw1IJiUDFsFrR9v/cIZ57TdH8QNkvT07XOpUQjZc5z/zVtE9Ohsgj/VyPtcYHW81WZBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6a5b7ccc816f98f0e5accde4029adc449b7d506f6d6015438adb411ba81b510e","last_reissued_at":"2026-07-04T16:55:46.475823Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:55:46.475823Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dark Energy and Dark Matter in Galaxy Halos","license":"","headline":"","cross_cats":["astro-ph","hep-th"],"primary_cat":"hep-ph","authors_text":"N. Tetradis","submitted_at":"2005-07-25T18:32:01Z","abstract_excerpt":"We consider the possibility that the dark matter is coupled through its mass to a scalar field associated with the dark energy of the Universe. In order for such a field to play a role at the present cosmological distances, it must be effectively massless at galactic length scales. We discuss the effects of the field on the distribution of dark matter in galaxy halos. We show that the profile of the distribution outside the galaxy core remains largely unaffected and the approximately flat rotation curves persist. The dispersion of the dark matter velocity is enhanced by a potentially large fac"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"hep-ph/0507288","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/hep-ph/0507288/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":"hep-ph/0507288","created_at":"2026-07-04T16:55:46.475886+00:00"},{"alias_kind":"arxiv_version","alias_value":"hep-ph/0507288v2","created_at":"2026-07-04T16:55:46.475886+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.hep-ph/0507288","created_at":"2026-07-04T16:55:46.475886+00:00"},{"alias_kind":"pith_short_12","alias_value":"NJNXZTEBN6MP","created_at":"2026-07-04T16:55:46.475886+00:00"},{"alias_kind":"pith_short_16","alias_value":"NJNXZTEBN6MPBZNM","created_at":"2026-07-04T16:55:46.475886+00:00"},{"alias_kind":"pith_short_8","alias_value":"NJNXZTEB","created_at":"2026-07-04T16:55:46.475886+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.11040","citing_title":"Multi-Channel Di-Higgs Production in the scNMSSM: From Exotic 8b to Boosted 8tau Signatures at the HL-LHC","ref_index":21,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS","json":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS.json","graph_json":"https://pith.science/api/pith-number/NJNXZTEBN6MPBZNMZXSAFGW4IS/graph.json","events_json":"https://pith.science/api/pith-number/NJNXZTEBN6MPBZNMZXSAFGW4IS/events.json","paper":"https://pith.science/paper/NJNXZTEB"},"agent_actions":{"view_html":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS","download_json":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS.json","view_paper":"https://pith.science/paper/NJNXZTEB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=hep-ph/0507288&json=true","fetch_graph":"https://pith.science/api/pith-number/NJNXZTEBN6MPBZNMZXSAFGW4IS/graph.json","fetch_events":"https://pith.science/api/pith-number/NJNXZTEBN6MPBZNMZXSAFGW4IS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS/action/storage_attestation","attest_author":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS/action/author_attestation","sign_citation":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS/action/citation_signature","submit_replication":"https://pith.science/pith/NJNXZTEBN6MPBZNMZXSAFGW4IS/action/replication_record"}},"created_at":"2026-07-04T16:55:46.475886+00:00","updated_at":"2026-07-04T16:55:46.475886+00:00"}