{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:7X7WNSSCRHEJUNMYSZV2HEDSTV","short_pith_number":"pith:7X7WNSSC","schema_version":"1.0","canonical_sha256":"fdff66ca4289c89a3598966ba390729d5ec67519f58e66488a45802ab1682613","source":{"kind":"arxiv","id":"1408.1952","version":2},"attestation_state":"computed","paper":{"title":"Exploring gravitational theories beyond Horndeski","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"David Langlois, Federico Piazza, Filippo Vernizzi, J\\'er\\^ome Gleyzes","submitted_at":"2014-08-08T19:59:18Z","abstract_excerpt":"We have recently proposed a new class of gravitational scalar-tensor theories free from Ostrogradski instabilities, in arXiv:1404.6495. As they generalize Horndeski theories, or \"generalized\" galileons, we call them G$^3$. These theories possess a simple formulation when the time hypersurfaces are chosen to coincide with the uniform scalar field hypersurfaces. We confirm that they contain only three propagating degrees of freedom by presenting the details of the Hamiltonian formulation. We examine the coupling between these theories and matter. Moreover, we investigate how they transform under"},"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":"1408.1952","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-08-08T19:59:18Z","cross_cats_sorted":["gr-qc","hep-th"],"title_canon_sha256":"7305c510aa866002c8164ea164c5031bfc004779c9ed6b49cfd372c59ec08159","abstract_canon_sha256":"61f72631aca965836c486b4212f250ec467a2e5fc19e9dac0a470d69176be66f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:42:22.368728Z","signature_b64":"vWND+2wUkGcHu8EwKfm/voeDIpjnSQ9Y6XtT12iNbautUlUmfPnGrIdyIxLBH43sLOGDKQRNIcMHb5Dgx5PvDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fdff66ca4289c89a3598966ba390729d5ec67519f58e66488a45802ab1682613","last_reissued_at":"2026-05-18T01:42:22.368255Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:42:22.368255Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Exploring gravitational theories beyond Horndeski","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"David Langlois, Federico Piazza, Filippo Vernizzi, J\\'er\\^ome Gleyzes","submitted_at":"2014-08-08T19:59:18Z","abstract_excerpt":"We have recently proposed a new class of gravitational scalar-tensor theories free from Ostrogradski instabilities, in arXiv:1404.6495. As they generalize Horndeski theories, or \"generalized\" galileons, we call them G$^3$. These theories possess a simple formulation when the time hypersurfaces are chosen to coincide with the uniform scalar field hypersurfaces. We confirm that they contain only three propagating degrees of freedom by presenting the details of the Hamiltonian formulation. We examine the coupling between these theories and matter. Moreover, we investigate how they transform under"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1408.1952","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":"1408.1952","created_at":"2026-05-18T01:42:22.368324+00:00"},{"alias_kind":"arxiv_version","alias_value":"1408.1952v2","created_at":"2026-05-18T01:42:22.368324+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1408.1952","created_at":"2026-05-18T01:42:22.368324+00:00"},{"alias_kind":"pith_short_12","alias_value":"7X7WNSSCRHEJ","created_at":"2026-05-18T12:28:19.803747+00:00"},{"alias_kind":"pith_short_16","alias_value":"7X7WNSSCRHEJUNMY","created_at":"2026-05-18T12:28:19.803747+00:00"},{"alias_kind":"pith_short_8","alias_value":"7X7WNSSC","created_at":"2026-05-18T12:28:19.803747+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2503.05651","citing_title":"Inverting no-hair theorems: How requiring General Relativity solutions restricts scalar-tensor theories","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2511.15049","citing_title":"The effects of dark energy on the matter-gravity coupling","ref_index":2,"is_internal_anchor":true},{"citing_arxiv_id":"2512.08972","citing_title":"Degenerate higher-order scalar-tensor theories in metric-affine gravity","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2605.12606","citing_title":"Radio sirens: inferring $H_0$ with binary black holes and neutral hydrogen in the era of the Einstein Telescope and the SKA Observatory","ref_index":98,"is_internal_anchor":true},{"citing_arxiv_id":"2605.06147","citing_title":"Cosmological Dynamics of a Non-Canonical Generalised Brans-Dicke Theory","ref_index":40,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV","json":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV.json","graph_json":"https://pith.science/api/pith-number/7X7WNSSCRHEJUNMYSZV2HEDSTV/graph.json","events_json":"https://pith.science/api/pith-number/7X7WNSSCRHEJUNMYSZV2HEDSTV/events.json","paper":"https://pith.science/paper/7X7WNSSC"},"agent_actions":{"view_html":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV","download_json":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV.json","view_paper":"https://pith.science/paper/7X7WNSSC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1408.1952&json=true","fetch_graph":"https://pith.science/api/pith-number/7X7WNSSCRHEJUNMYSZV2HEDSTV/graph.json","fetch_events":"https://pith.science/api/pith-number/7X7WNSSCRHEJUNMYSZV2HEDSTV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV/action/storage_attestation","attest_author":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV/action/author_attestation","sign_citation":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV/action/citation_signature","submit_replication":"https://pith.science/pith/7X7WNSSCRHEJUNMYSZV2HEDSTV/action/replication_record"}},"created_at":"2026-05-18T01:42:22.368324+00:00","updated_at":"2026-05-18T01:42:22.368324+00:00"}