{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:YSFM2QIZFWT4XHAAX5FAMAUT3E","short_pith_number":"pith:YSFM2QIZ","schema_version":"1.0","canonical_sha256":"c48acd41192da7cb9c00bf4a060293d9052af526807187cce829fd2559d91daa","source":{"kind":"arxiv","id":"1507.05047","version":3},"attestation_state":"computed","paper":{"title":"Piercing the Vainshtein screen with anomalous gravitational wave speed: Constraints on modified gravity from binary pulsars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Federico Piazza, Hermano Velten, Jose Beltran Jimenez","submitted_at":"2015-07-17T19:26:45Z","abstract_excerpt":"By using observations of the Hulse-Taylor pulsar we constrain the gravitational wave (GW) speed to the level of $10^{-2}$. We apply this result to scalar-tensor theories that generalize Galileon 4 and 5 models, which display anomalous propagation speed and coupling to matter for GWs. We argue that this effect survives conventional screening due to the persistence of a scalar field gradient inside virialized overdensities, which effectively \"pierces\" the Vainshtein screening. In specific branches of solutions, our result allows to directly constrain the cosmological couplings in the effective f"},"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":"1507.05047","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2015-07-17T19:26:45Z","cross_cats_sorted":["astro-ph.CO","hep-th"],"title_canon_sha256":"475c613319bff867e21ebc1c9e23443f632d709c20fe7878c04f13bfab8cb1c1","abstract_canon_sha256":"bd3456d7894570e11b6850912ac7362efe6802b67686683d0d1fc0bdfacc147d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:20:36.202799Z","signature_b64":"OGUy+BIDHLfuErrw56kqVcTY+SHQZA8d3aflnJebWKNUVaAucl8lvzUy4s7hfFdp55iFbDj91emma48idFEOCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c48acd41192da7cb9c00bf4a060293d9052af526807187cce829fd2559d91daa","last_reissued_at":"2026-05-18T01:20:36.202355Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:20:36.202355Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Piercing the Vainshtein screen with anomalous gravitational wave speed: Constraints on modified gravity from binary pulsars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Federico Piazza, Hermano Velten, Jose Beltran Jimenez","submitted_at":"2015-07-17T19:26:45Z","abstract_excerpt":"By using observations of the Hulse-Taylor pulsar we constrain the gravitational wave (GW) speed to the level of $10^{-2}$. We apply this result to scalar-tensor theories that generalize Galileon 4 and 5 models, which display anomalous propagation speed and coupling to matter for GWs. We argue that this effect survives conventional screening due to the persistence of a scalar field gradient inside virialized overdensities, which effectively \"pierces\" the Vainshtein screening. In specific branches of solutions, our result allows to directly constrain the cosmological couplings in the effective f"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1507.05047","kind":"arxiv","version":3},"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":"1507.05047","created_at":"2026-05-18T01:20:36.202424+00:00"},{"alias_kind":"arxiv_version","alias_value":"1507.05047v3","created_at":"2026-05-18T01:20:36.202424+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1507.05047","created_at":"2026-05-18T01:20:36.202424+00:00"},{"alias_kind":"pith_short_12","alias_value":"YSFM2QIZFWT4","created_at":"2026-05-18T12:29:52.810259+00:00"},{"alias_kind":"pith_short_16","alias_value":"YSFM2QIZFWT4XHAA","created_at":"2026-05-18T12:29:52.810259+00:00"},{"alias_kind":"pith_short_8","alias_value":"YSFM2QIZ","created_at":"2026-05-18T12:29:52.810259+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2601.05145","citing_title":"How deep can a cosmic void be? Voids-informed theoretical bounds in Galileon gravity","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E","json":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E.json","graph_json":"https://pith.science/api/pith-number/YSFM2QIZFWT4XHAAX5FAMAUT3E/graph.json","events_json":"https://pith.science/api/pith-number/YSFM2QIZFWT4XHAAX5FAMAUT3E/events.json","paper":"https://pith.science/paper/YSFM2QIZ"},"agent_actions":{"view_html":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E","download_json":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E.json","view_paper":"https://pith.science/paper/YSFM2QIZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1507.05047&json=true","fetch_graph":"https://pith.science/api/pith-number/YSFM2QIZFWT4XHAAX5FAMAUT3E/graph.json","fetch_events":"https://pith.science/api/pith-number/YSFM2QIZFWT4XHAAX5FAMAUT3E/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E/action/storage_attestation","attest_author":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E/action/author_attestation","sign_citation":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E/action/citation_signature","submit_replication":"https://pith.science/pith/YSFM2QIZFWT4XHAAX5FAMAUT3E/action/replication_record"}},"created_at":"2026-05-18T01:20:36.202424+00:00","updated_at":"2026-05-18T01:20:36.202424+00:00"}