{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:7MUBRH7ZAYBMN6GKBXO5G7ZY5D","short_pith_number":"pith:7MUBRH7Z","schema_version":"1.0","canonical_sha256":"fb28189ff90602c6f8ca0dddd37f38e8cac36ae6bf0012c52530b1bc512d53e8","source":{"kind":"arxiv","id":"1311.4765","version":2},"attestation_state":"computed","paper":{"title":"Model-independent constraints on the cosmological anisotropic stress","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"2), (2) U. Bologna, (3) U. Geneva, 4), (4) African Inst. Math. Sci., Adrian Vollmer (1) ((1) U. Heidelberg, Alejandro Guarnizo (1), Cape Town), ITP, Luca Amendola (1), Martin Kunz (3, Simone Fogli (1","submitted_at":"2013-11-19T15:04:56Z","abstract_excerpt":"The effective anisotropic stress or gravitational slip $\\eta=-\\Phi/\\Psi$ is a key variable in the characterisation of the physical origin of the dark energy, as it allows to test for a non-minimal coupling of the dark sector to gravity in the Jordan frame. It is however important to use a fully model-independent approach when measuring $\\eta$ to avoid introducing a theoretical bias into the results. In this paper we forecast the precision with which future large surveys can determine $\\eta$ in a way that only relies on directly observable quantities. In particular, we do not assume anything co"},"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":"1311.4765","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-11-19T15:04:56Z","cross_cats_sorted":["gr-qc","hep-th"],"title_canon_sha256":"d5e5575b54df2dbdee85b9ec25c9090f58a431d8c60ea4d6194c0eeb815f980b","abstract_canon_sha256":"258842059d1afa387d7ad423f9dd6f2b525a102bbebb94707151a02652fe3a42"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:55:10.818614Z","signature_b64":"jbs+YmgzS9wMe2gJ0fahybPDQf6G+FUoPnkr/FNOSJdh63ws1DwM8q6gw8mT2E1VBhc5BL883/SOmxOr+3tgAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fb28189ff90602c6f8ca0dddd37f38e8cac36ae6bf0012c52530b1bc512d53e8","last_reissued_at":"2026-05-18T02:55:10.818097Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:55:10.818097Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Model-independent constraints on the cosmological anisotropic stress","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"2), (2) U. Bologna, (3) U. Geneva, 4), (4) African Inst. Math. Sci., Adrian Vollmer (1) ((1) U. Heidelberg, Alejandro Guarnizo (1), Cape Town), ITP, Luca Amendola (1), Martin Kunz (3, Simone Fogli (1","submitted_at":"2013-11-19T15:04:56Z","abstract_excerpt":"The effective anisotropic stress or gravitational slip $\\eta=-\\Phi/\\Psi$ is a key variable in the characterisation of the physical origin of the dark energy, as it allows to test for a non-minimal coupling of the dark sector to gravity in the Jordan frame. It is however important to use a fully model-independent approach when measuring $\\eta$ to avoid introducing a theoretical bias into the results. In this paper we forecast the precision with which future large surveys can determine $\\eta$ in a way that only relies on directly observable quantities. In particular, we do not assume anything co"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1311.4765","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":"1311.4765","created_at":"2026-05-18T02:55:10.818179+00:00"},{"alias_kind":"arxiv_version","alias_value":"1311.4765v2","created_at":"2026-05-18T02:55:10.818179+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1311.4765","created_at":"2026-05-18T02:55:10.818179+00:00"},{"alias_kind":"pith_short_12","alias_value":"7MUBRH7ZAYBM","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_16","alias_value":"7MUBRH7ZAYBMN6GK","created_at":"2026-05-18T12:27:36.564083+00:00"},{"alias_kind":"pith_short_8","alias_value":"7MUBRH7Z","created_at":"2026-05-18T12:27:36.564083+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.26690","citing_title":"Nonlinear Relativistic Effects on Cosmological Redshift Drift","ref_index":64,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D","json":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D.json","graph_json":"https://pith.science/api/pith-number/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/graph.json","events_json":"https://pith.science/api/pith-number/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/events.json","paper":"https://pith.science/paper/7MUBRH7Z"},"agent_actions":{"view_html":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D","download_json":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D.json","view_paper":"https://pith.science/paper/7MUBRH7Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1311.4765&json=true","fetch_graph":"https://pith.science/api/pith-number/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/graph.json","fetch_events":"https://pith.science/api/pith-number/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/action/storage_attestation","attest_author":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/action/author_attestation","sign_citation":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/action/citation_signature","submit_replication":"https://pith.science/pith/7MUBRH7ZAYBMN6GKBXO5G7ZY5D/action/replication_record"}},"created_at":"2026-05-18T02:55:10.818179+00:00","updated_at":"2026-05-18T02:55:10.818179+00:00"}