{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:XQMZZOKRXHYO3LFACJDJKL4TPI","short_pith_number":"pith:XQMZZOKR","schema_version":"1.0","canonical_sha256":"bc199cb951b9f0edaca01246952f937a3ff4427d9cca3d718e661a039fb6e4d1","source":{"kind":"arxiv","id":"2210.16296","version":1},"attestation_state":"computed","paper":{"title":"Resolving the Hubble tension with Early Dark Energy","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Elisa G. M. Ferreira, Laura Herold","submitted_at":"2022-10-28T17:50:05Z","abstract_excerpt":"Early dark energy (EDE) offers a solution to the so-called Hubble tension. Recently, it was shown that the constraints on EDE using Markov Chain Monte Carlo are affected by prior volume effects. The goal of this paper is to present constraints on the fraction of EDE, $f_\\mathrm{EDE}$, and the Hubble parameter, $H_0$, which are not subject to prior volume effects. We conduct a frequentist profile likelihood analysis considering Planck cosmic microwave background, BOSS full-shape galaxy clustering, DES weak lensing, and SH0ES supernova data. Contrary to previous findings, we find that $H_0$ for "},"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":"2210.16296","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-10-28T17:50:05Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"bd46747fb82fe8b26e93fc8498922fa675e1ce51d4333e9f7fd8c6ec97ee88f7","abstract_canon_sha256":"240457bca11f6ea43a20f17578fce4a10157685af6ffb4c19105e97719048d9e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:41:08.221818Z","signature_b64":"dWisGdAs44mvjXVn8FC3CTR37AaqLO6KD6xWevL5CVixnrRuCDq60bVft7Qyyj0xPF9oZu4Gu+BdoIZ6INsvBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bc199cb951b9f0edaca01246952f937a3ff4427d9cca3d718e661a039fb6e4d1","last_reissued_at":"2026-07-05T06:41:08.221375Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:41:08.221375Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Resolving the Hubble tension with Early Dark Energy","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Elisa G. M. Ferreira, Laura Herold","submitted_at":"2022-10-28T17:50:05Z","abstract_excerpt":"Early dark energy (EDE) offers a solution to the so-called Hubble tension. Recently, it was shown that the constraints on EDE using Markov Chain Monte Carlo are affected by prior volume effects. The goal of this paper is to present constraints on the fraction of EDE, $f_\\mathrm{EDE}$, and the Hubble parameter, $H_0$, which are not subject to prior volume effects. We conduct a frequentist profile likelihood analysis considering Planck cosmic microwave background, BOSS full-shape galaxy clustering, DES weak lensing, and SH0ES supernova data. Contrary to previous findings, we find that $H_0$ for "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2210.16296","kind":"arxiv","version":1},"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/2210.16296/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":"2210.16296","created_at":"2026-07-05T06:41:08.221430+00:00"},{"alias_kind":"arxiv_version","alias_value":"2210.16296v1","created_at":"2026-07-05T06:41:08.221430+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2210.16296","created_at":"2026-07-05T06:41:08.221430+00:00"},{"alias_kind":"pith_short_12","alias_value":"XQMZZOKRXHYO","created_at":"2026-07-05T06:41:08.221430+00:00"},{"alias_kind":"pith_short_16","alias_value":"XQMZZOKRXHYO3LFA","created_at":"2026-07-05T06:41:08.221430+00:00"},{"alias_kind":"pith_short_8","alias_value":"XQMZZOKR","created_at":"2026-07-05T06:41:08.221430+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06147","citing_title":"Imprint of swampland-inspired coupled early dark energy","ref_index":130,"is_internal_anchor":true},{"citing_arxiv_id":"2606.20434","citing_title":"The Hubble tension: A decade review","ref_index":280,"is_internal_anchor":false},{"citing_arxiv_id":"2605.26116","citing_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","ref_index":95,"is_internal_anchor":false},{"citing_arxiv_id":"2605.14977","citing_title":"Unified dark sector and Hubble-tension alleviation in scalar-vector-tensor gravity","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2507.23355","citing_title":"SPT-3G D1: Axion Early Dark Energy with CMB experiments and DESI","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2211.04492","citing_title":"The Hubble Tension and Early Dark Energy","ref_index":145,"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":125,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI","json":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI.json","graph_json":"https://pith.science/api/pith-number/XQMZZOKRXHYO3LFACJDJKL4TPI/graph.json","events_json":"https://pith.science/api/pith-number/XQMZZOKRXHYO3LFACJDJKL4TPI/events.json","paper":"https://pith.science/paper/XQMZZOKR"},"agent_actions":{"view_html":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI","download_json":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI.json","view_paper":"https://pith.science/paper/XQMZZOKR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2210.16296&json=true","fetch_graph":"https://pith.science/api/pith-number/XQMZZOKRXHYO3LFACJDJKL4TPI/graph.json","fetch_events":"https://pith.science/api/pith-number/XQMZZOKRXHYO3LFACJDJKL4TPI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI/action/storage_attestation","attest_author":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI/action/author_attestation","sign_citation":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI/action/citation_signature","submit_replication":"https://pith.science/pith/XQMZZOKRXHYO3LFACJDJKL4TPI/action/replication_record"}},"created_at":"2026-07-05T06:41:08.221430+00:00","updated_at":"2026-07-05T06:41:08.221430+00:00"}