{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:BNPK32Q2YH5FD5XB6CMQVG3M44","short_pith_number":"pith:BNPK32Q2","schema_version":"1.0","canonical_sha256":"0b5eadea1ac1fa51f6e1f0990a9b6ce71574887362e33f7f49a6b11c4f2e9bb0","source":{"kind":"arxiv","id":"1708.06681","version":2},"attestation_state":"computed","paper":{"title":"Comparison between two scalar field models using rotation curves of spiral galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Lizbeth M. Fernandez-Hernandez, Mario A. Rodriguez-Meza, Tonatiuh Matos","submitted_at":"2017-08-22T15:46:09Z","abstract_excerpt":"Scalar fields have been used as candidates for dark matter in the universe, from axions with masses $\\sim10^{-5}$eV until ultra-light scalar fields with masses $\\sim10^{-22}$eV. Axions behave as cold dark matter while the ultra-light scalar fields galaxies are Bose-Einstein condensate drops. The ultra-light scalar fields are also called scalar field dark matter model. In this work we study rotation curves for low surface brightness spiral galaxies using two scalar field models: the Gross-Pitaevskii Bose-Einstein condensate in the Thomas-Fermi approximation and a scalar field solution of the Kl"},"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":"1708.06681","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-08-22T15:46:09Z","cross_cats_sorted":[],"title_canon_sha256":"755d28821f22e3aa760d9fbf3f223bd614f0f831cb1c34a29e334c30a529a4d4","abstract_canon_sha256":"2b31bc060fe14ff81ced27a68b958d04cd623d32ba15817cb38c7ab3e0688df3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:15:21.351768Z","signature_b64":"1zsJ3qdVOO5GDxiDK5LtdXc4tXJEdp/phee0IRFkDHjXsMNgZI5qTEBnIDGaPsng4wTEG5GIITZ0kOb16BqKBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0b5eadea1ac1fa51f6e1f0990a9b6ce71574887362e33f7f49a6b11c4f2e9bb0","last_reissued_at":"2026-05-18T00:15:21.351078Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:15:21.351078Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Comparison between two scalar field models using rotation curves of spiral galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Lizbeth M. Fernandez-Hernandez, Mario A. Rodriguez-Meza, Tonatiuh Matos","submitted_at":"2017-08-22T15:46:09Z","abstract_excerpt":"Scalar fields have been used as candidates for dark matter in the universe, from axions with masses $\\sim10^{-5}$eV until ultra-light scalar fields with masses $\\sim10^{-22}$eV. Axions behave as cold dark matter while the ultra-light scalar fields galaxies are Bose-Einstein condensate drops. The ultra-light scalar fields are also called scalar field dark matter model. In this work we study rotation curves for low surface brightness spiral galaxies using two scalar field models: the Gross-Pitaevskii Bose-Einstein condensate in the Thomas-Fermi approximation and a scalar field solution of the Kl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1708.06681","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":"1708.06681","created_at":"2026-05-18T00:15:21.351182+00:00"},{"alias_kind":"arxiv_version","alias_value":"1708.06681v2","created_at":"2026-05-18T00:15:21.351182+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1708.06681","created_at":"2026-05-18T00:15:21.351182+00:00"},{"alias_kind":"pith_short_12","alias_value":"BNPK32Q2YH5F","created_at":"2026-05-18T12:31:08.081275+00:00"},{"alias_kind":"pith_short_16","alias_value":"BNPK32Q2YH5FD5XB","created_at":"2026-05-18T12:31:08.081275+00:00"},{"alias_kind":"pith_short_8","alias_value":"BNPK32Q2","created_at":"2026-05-18T12:31:08.081275+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.20919","citing_title":"Scalarization and superradiant instability of black hole induced by dark matter halo in the scalar-tensor theory of gravity","ref_index":35,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44","json":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44.json","graph_json":"https://pith.science/api/pith-number/BNPK32Q2YH5FD5XB6CMQVG3M44/graph.json","events_json":"https://pith.science/api/pith-number/BNPK32Q2YH5FD5XB6CMQVG3M44/events.json","paper":"https://pith.science/paper/BNPK32Q2"},"agent_actions":{"view_html":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44","download_json":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44.json","view_paper":"https://pith.science/paper/BNPK32Q2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1708.06681&json=true","fetch_graph":"https://pith.science/api/pith-number/BNPK32Q2YH5FD5XB6CMQVG3M44/graph.json","fetch_events":"https://pith.science/api/pith-number/BNPK32Q2YH5FD5XB6CMQVG3M44/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44/action/storage_attestation","attest_author":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44/action/author_attestation","sign_citation":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44/action/citation_signature","submit_replication":"https://pith.science/pith/BNPK32Q2YH5FD5XB6CMQVG3M44/action/replication_record"}},"created_at":"2026-05-18T00:15:21.351182+00:00","updated_at":"2026-05-18T00:15:21.351182+00:00"}