{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:4235BCQZUKVZMSPKWSYXFWF5DW","short_pith_number":"pith:4235BCQZ","schema_version":"1.0","canonical_sha256":"e6b7d08a19a2ab9649eab4b172d8bd1d8a7f1818bc09e4fda0b0680368175cc4","source":{"kind":"arxiv","id":"0912.4641","version":2},"attestation_state":"computed","paper":{"title":"Evolution of linear cosmological perturbations and its observational implications in Galileon-type modified gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Daichi Suzuki, Hiroyuki Tashiro, Tsutomu Kobayashi","submitted_at":"2009-12-23T13:50:20Z","abstract_excerpt":"A scalar-tensor theory of gravity can be made not only to account for the current cosmic acceleration, but also to satisfy solar-system and laboratory constraints, by introducing a non-linear derivative interaction for the scalar field. Such an additional scalar degree of freedom is called \"Galileon\". The basic idea is inspired by the DGP braneworld, but one can construct a ghost-free model that admits a self-accelerating solution. We perform a fully relativistic analysis of linear perturbations in Galileon cosmology. Although the Galileon model can mimic the background evolution of standard $"},"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":"0912.4641","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-12-23T13:50:20Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"3eca19c7c91444a66de682754d2d6e7257826358a14284e9c6178bdefd26e427","abstract_canon_sha256":"cd8cddd48e9caf88ae5214c9bd676e5b9e4f16d2244872c0642517775faca369"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:24:45.406794Z","signature_b64":"ZJyceHzrnJd8AO3r1kUKDMeL5+qiDTLZcgFteO8klO/4Evp9x1ll5j1T9V+4vszII+H7qKIU+Jsf3XkeA4HFCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e6b7d08a19a2ab9649eab4b172d8bd1d8a7f1818bc09e4fda0b0680368175cc4","last_reissued_at":"2026-05-18T02:24:45.406307Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:24:45.406307Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evolution of linear cosmological perturbations and its observational implications in Galileon-type modified gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Daichi Suzuki, Hiroyuki Tashiro, Tsutomu Kobayashi","submitted_at":"2009-12-23T13:50:20Z","abstract_excerpt":"A scalar-tensor theory of gravity can be made not only to account for the current cosmic acceleration, but also to satisfy solar-system and laboratory constraints, by introducing a non-linear derivative interaction for the scalar field. Such an additional scalar degree of freedom is called \"Galileon\". The basic idea is inspired by the DGP braneworld, but one can construct a ghost-free model that admits a self-accelerating solution. We perform a fully relativistic analysis of linear perturbations in Galileon cosmology. Although the Galileon model can mimic the background evolution of standard $"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0912.4641","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":"0912.4641","created_at":"2026-05-18T02:24:45.406395+00:00"},{"alias_kind":"arxiv_version","alias_value":"0912.4641v2","created_at":"2026-05-18T02:24:45.406395+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0912.4641","created_at":"2026-05-18T02:24:45.406395+00:00"},{"alias_kind":"pith_short_12","alias_value":"4235BCQZUKVZ","created_at":"2026-05-18T12:25:58.018023+00:00"},{"alias_kind":"pith_short_16","alias_value":"4235BCQZUKVZMSPK","created_at":"2026-05-18T12:25:58.018023+00:00"},{"alias_kind":"pith_short_8","alias_value":"4235BCQZ","created_at":"2026-05-18T12:25:58.018023+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2603.22398","citing_title":"Stable black hole solutions with cosmological hair","ref_index":77,"is_internal_anchor":true},{"citing_arxiv_id":"2603.23634","citing_title":"Testing Dark Energy with Black Hole Ringdown","ref_index":62,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW","json":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW.json","graph_json":"https://pith.science/api/pith-number/4235BCQZUKVZMSPKWSYXFWF5DW/graph.json","events_json":"https://pith.science/api/pith-number/4235BCQZUKVZMSPKWSYXFWF5DW/events.json","paper":"https://pith.science/paper/4235BCQZ"},"agent_actions":{"view_html":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW","download_json":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW.json","view_paper":"https://pith.science/paper/4235BCQZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0912.4641&json=true","fetch_graph":"https://pith.science/api/pith-number/4235BCQZUKVZMSPKWSYXFWF5DW/graph.json","fetch_events":"https://pith.science/api/pith-number/4235BCQZUKVZMSPKWSYXFWF5DW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW/action/storage_attestation","attest_author":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW/action/author_attestation","sign_citation":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW/action/citation_signature","submit_replication":"https://pith.science/pith/4235BCQZUKVZMSPKWSYXFWF5DW/action/replication_record"}},"created_at":"2026-05-18T02:24:45.406395+00:00","updated_at":"2026-05-18T02:24:45.406395+00:00"}