{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:Q3KNIPS6KRQDPLRINVIHI77V46","short_pith_number":"pith:Q3KNIPS6","schema_version":"1.0","canonical_sha256":"86d4d43e5e546037ae286d50747ff5e7b5122a0db7e443d412b8ee231b981b05","source":{"kind":"arxiv","id":"1305.5647","version":2},"attestation_state":"computed","paper":{"title":"Impact on the power spectrum of Screening in Modified Gravity Scenarios","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Patrick Valageas, Philippe Brax","submitted_at":"2013-05-24T08:19:35Z","abstract_excerpt":"We study the effects of screened modified gravity of the $f(R)$, dilaton and symmetron types on structure formation, from the quasi-linear to the non-linear regime, using semi-analytical methods. For such models, where the range of the new scalar field is typically within the Mpc range and below in the cosmological context, non-linear techniques are required to understand the deviations of the power spectrum of the matter density contrast compared to the $\\Lambda$-CDM template. This is nowadays commonly tackled using extensive N-body simulations. Here we present new results combining exact per"},"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":"1305.5647","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-05-24T08:19:35Z","cross_cats_sorted":[],"title_canon_sha256":"afc24f5753c96d54b04f015879eaab465212e5631927c181cdf90f55bf9574bf","abstract_canon_sha256":"f4f5f81743c8abf0c7c6f5e9a0a1a4b284e093f62055fc233aaa316699aafd30"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:49:46.997468Z","signature_b64":"EXNiCPK4Vl6SWbMmraCO6/ZM9s8O+STbVv0aGnSKOdjkpg2BLRzeSQDOBLF7OOU4WKUEwe7q4Zj+rzfGpYxzDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"86d4d43e5e546037ae286d50747ff5e7b5122a0db7e443d412b8ee231b981b05","last_reissued_at":"2026-05-18T01:49:46.996892Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:49:46.996892Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impact on the power spectrum of Screening in Modified Gravity Scenarios","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Patrick Valageas, Philippe Brax","submitted_at":"2013-05-24T08:19:35Z","abstract_excerpt":"We study the effects of screened modified gravity of the $f(R)$, dilaton and symmetron types on structure formation, from the quasi-linear to the non-linear regime, using semi-analytical methods. For such models, where the range of the new scalar field is typically within the Mpc range and below in the cosmological context, non-linear techniques are required to understand the deviations of the power spectrum of the matter density contrast compared to the $\\Lambda$-CDM template. This is nowadays commonly tackled using extensive N-body simulations. Here we present new results combining exact per"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1305.5647","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":"1305.5647","created_at":"2026-05-18T01:49:46.996982+00:00"},{"alias_kind":"arxiv_version","alias_value":"1305.5647v2","created_at":"2026-05-18T01:49:46.996982+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1305.5647","created_at":"2026-05-18T01:49:46.996982+00:00"},{"alias_kind":"pith_short_12","alias_value":"Q3KNIPS6KRQD","created_at":"2026-05-18T12:27:57.521954+00:00"},{"alias_kind":"pith_short_16","alias_value":"Q3KNIPS6KRQDPLRI","created_at":"2026-05-18T12:27:57.521954+00:00"},{"alias_kind":"pith_short_8","alias_value":"Q3KNIPS6","created_at":"2026-05-18T12:27:57.521954+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2604.26433","citing_title":"Studying spherical collapse and its implications in the Eddington-inspired Born-Infeld gravity theory","ref_index":50,"is_internal_anchor":true},{"citing_arxiv_id":"2604.26915","citing_title":"Testing Scale-Dependent Modified Gravity with DESI DR1","ref_index":16,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26433","citing_title":"Studying spherical collapse and its implications in the Eddington-inspired Born-Infeld gravity theory","ref_index":50,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46","json":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46.json","graph_json":"https://pith.science/api/pith-number/Q3KNIPS6KRQDPLRINVIHI77V46/graph.json","events_json":"https://pith.science/api/pith-number/Q3KNIPS6KRQDPLRINVIHI77V46/events.json","paper":"https://pith.science/paper/Q3KNIPS6"},"agent_actions":{"view_html":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46","download_json":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46.json","view_paper":"https://pith.science/paper/Q3KNIPS6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1305.5647&json=true","fetch_graph":"https://pith.science/api/pith-number/Q3KNIPS6KRQDPLRINVIHI77V46/graph.json","fetch_events":"https://pith.science/api/pith-number/Q3KNIPS6KRQDPLRINVIHI77V46/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46/action/storage_attestation","attest_author":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46/action/author_attestation","sign_citation":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46/action/citation_signature","submit_replication":"https://pith.science/pith/Q3KNIPS6KRQDPLRINVIHI77V46/action/replication_record"}},"created_at":"2026-05-18T01:49:46.996982+00:00","updated_at":"2026-05-18T01:49:46.996982+00:00"}