{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:DX3UOAF4C2OMI372OGOCPBYVKF","short_pith_number":"pith:DX3UOAF4","schema_version":"1.0","canonical_sha256":"1df74700bc169cc46ffa719c27871551754f51178fb2456eea52644321b2dd4e","source":{"kind":"arxiv","id":"2207.01501","version":3},"attestation_state":"computed","paper":{"title":"Restoring cosmological concordance with early dark energy and massive neutrinos?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Alexander Reeves, Blake D. Sherwin, Elisa G. M. Ferreira, Laura Herold, Sunny Vagnozzi","submitted_at":"2022-07-04T15:22:39Z","abstract_excerpt":"The early dark energy (EDE) solution to the Hubble tension comes at the cost of an increased clustering amplitude that has been argued to worsen the fit to galaxy clustering data. We explore whether freeing the total neutrino mass $M_{\\nu}$, which can suppress small-scale structure growth, improves EDE's fit to galaxy clustering. Using Planck Cosmic Microwave Background and BOSS galaxy clustering data, a Bayesian analysis shows that freeing $M_{\\nu}$ does not appreciably increase the inferred EDE fraction $f_{\\rm EDE}$: we find the 95% C.L. upper limits $f_{\\rm EDE}<0.092$ and $M_{\\nu}<0.15\\,{"},"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":"2207.01501","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-07-04T15:22:39Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"4bee9891382cc86e59dd29e4d59d3c668f1502622bc0a7b2ba273882ec26201d","abstract_canon_sha256":"e838c555626dde536693a379d22287e726314328b6d159a073019971b92a4638"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:43:02.943327Z","signature_b64":"/O8vAV/jw4UM7TcbPK2DyH0nkGhJKhyjLpkSPk+CIhm5PEPwvgbf/y0v1sJtFkbutsdp2HzT/rfRSoKvcf/CDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1df74700bc169cc46ffa719c27871551754f51178fb2456eea52644321b2dd4e","last_reissued_at":"2026-07-05T05:43:02.942883Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:43:02.942883Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Restoring cosmological concordance with early dark energy and massive neutrinos?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Alexander Reeves, Blake D. Sherwin, Elisa G. M. Ferreira, Laura Herold, Sunny Vagnozzi","submitted_at":"2022-07-04T15:22:39Z","abstract_excerpt":"The early dark energy (EDE) solution to the Hubble tension comes at the cost of an increased clustering amplitude that has been argued to worsen the fit to galaxy clustering data. We explore whether freeing the total neutrino mass $M_{\\nu}$, which can suppress small-scale structure growth, improves EDE's fit to galaxy clustering. Using Planck Cosmic Microwave Background and BOSS galaxy clustering data, a Bayesian analysis shows that freeing $M_{\\nu}$ does not appreciably increase the inferred EDE fraction $f_{\\rm EDE}$: we find the 95% C.L. upper limits $f_{\\rm EDE}<0.092$ and $M_{\\nu}<0.15\\,{"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2207.01501","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2207.01501/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2207.01501","created_at":"2026-07-05T05:43:02.942938+00:00"},{"alias_kind":"arxiv_version","alias_value":"2207.01501v3","created_at":"2026-07-05T05:43:02.942938+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2207.01501","created_at":"2026-07-05T05:43:02.942938+00:00"},{"alias_kind":"pith_short_12","alias_value":"DX3UOAF4C2OM","created_at":"2026-07-05T05:43:02.942938+00:00"},{"alias_kind":"pith_short_16","alias_value":"DX3UOAF4C2OMI372","created_at":"2026-07-05T05:43:02.942938+00:00"},{"alias_kind":"pith_short_8","alias_value":"DX3UOAF4","created_at":"2026-07-05T05:43:02.942938+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.05005","citing_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","ref_index":116,"is_internal_anchor":false},{"citing_arxiv_id":"2605.26116","citing_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","ref_index":83,"is_internal_anchor":false},{"citing_arxiv_id":"2603.10787","citing_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","ref_index":94,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25813","citing_title":"Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension","ref_index":133,"is_internal_anchor":false},{"citing_arxiv_id":"2604.13535","citing_title":"Double the axions, half the tension: multi-field early dark energy eases the Hubble tension","ref_index":173,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF","json":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF.json","graph_json":"https://pith.science/api/pith-number/DX3UOAF4C2OMI372OGOCPBYVKF/graph.json","events_json":"https://pith.science/api/pith-number/DX3UOAF4C2OMI372OGOCPBYVKF/events.json","paper":"https://pith.science/paper/DX3UOAF4"},"agent_actions":{"view_html":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF","download_json":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF.json","view_paper":"https://pith.science/paper/DX3UOAF4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2207.01501&json=true","fetch_graph":"https://pith.science/api/pith-number/DX3UOAF4C2OMI372OGOCPBYVKF/graph.json","fetch_events":"https://pith.science/api/pith-number/DX3UOAF4C2OMI372OGOCPBYVKF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF/action/storage_attestation","attest_author":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF/action/author_attestation","sign_citation":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF/action/citation_signature","submit_replication":"https://pith.science/pith/DX3UOAF4C2OMI372OGOCPBYVKF/action/replication_record"}},"created_at":"2026-07-05T05:43:02.942938+00:00","updated_at":"2026-07-05T05:43:02.942938+00:00"}