{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:ZUB4RQWDN66OWUJP65Z4SBPTWE","short_pith_number":"pith:ZUB4RQWD","schema_version":"1.0","canonical_sha256":"cd03c8c2c36fbceb512ff773c905f3b13912bdcc3bcf30b6108a57890aad81cf","source":{"kind":"arxiv","id":"2201.07079","version":2},"attestation_state":"computed","paper":{"title":"Testing dark energy after pre-recombination early dark energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Hao Wang, Yun-Song Piao","submitted_at":"2022-01-18T16:01:52Z","abstract_excerpt":"In the studies on pre-recombination early dark energy (EDE), the evolution of Universe after recombination is usually regarded as ${\\Lambda}CDM$-like, which corresponds that the equation of state of dark energy responsible for current accelerated expansion is $w=-1$. However, in realistic models, $w$ might be evolving. We consider the parametrizations of $w$ with respect to the redshift $z$ in Axion-like EDE and AdS-EDE models, respectively. We performed the Monte Carlo Markov chain analysis with recent cosmological data, and found that the bestfit $w(z)$ is compatible with $w_0=-1,w_a=0$ (the"},"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":"2201.07079","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-01-18T16:01:52Z","cross_cats_sorted":["gr-qc","hep-th"],"title_canon_sha256":"a0c0f7294bc789d38203eea4b9f51f5c0c7cd67437c2c4879ba5c041d06d7c76","abstract_canon_sha256":"508203b8693761f5ca133c6b8ed52c98ae0803b086d4a265e9b8bd28b62f0dd3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:53:26.285658Z","signature_b64":"+L5ath3rD/5QOVeiQMZDz75jP9O/iGUTNIt7AyXkacyJuMX8MMaynr9cNe81cWQhgu+BrbbyFrXxPuZsTM+gAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cd03c8c2c36fbceb512ff773c905f3b13912bdcc3bcf30b6108a57890aad81cf","last_reissued_at":"2026-07-05T04:53:26.285230Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:53:26.285230Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing dark energy after pre-recombination early dark energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Hao Wang, Yun-Song Piao","submitted_at":"2022-01-18T16:01:52Z","abstract_excerpt":"In the studies on pre-recombination early dark energy (EDE), the evolution of Universe after recombination is usually regarded as ${\\Lambda}CDM$-like, which corresponds that the equation of state of dark energy responsible for current accelerated expansion is $w=-1$. However, in realistic models, $w$ might be evolving. We consider the parametrizations of $w$ with respect to the redshift $z$ in Axion-like EDE and AdS-EDE models, respectively. We performed the Monte Carlo Markov chain analysis with recent cosmological data, and found that the bestfit $w(z)$ is compatible with $w_0=-1,w_a=0$ (the"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2201.07079","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2201.07079/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":"2201.07079","created_at":"2026-07-05T04:53:26.285277+00:00"},{"alias_kind":"arxiv_version","alias_value":"2201.07079v2","created_at":"2026-07-05T04:53:26.285277+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2201.07079","created_at":"2026-07-05T04:53:26.285277+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZUB4RQWDN66O","created_at":"2026-07-05T04:53:26.285277+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZUB4RQWDN66OWUJP","created_at":"2026-07-05T04:53:26.285277+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZUB4RQWD","created_at":"2026-07-05T04:53:26.285277+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2510.24682","citing_title":"Harrison-Zeldovich attractor: From Planck to ACT results","ref_index":102,"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":131,"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":120,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE","json":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE.json","graph_json":"https://pith.science/api/pith-number/ZUB4RQWDN66OWUJP65Z4SBPTWE/graph.json","events_json":"https://pith.science/api/pith-number/ZUB4RQWDN66OWUJP65Z4SBPTWE/events.json","paper":"https://pith.science/paper/ZUB4RQWD"},"agent_actions":{"view_html":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE","download_json":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE.json","view_paper":"https://pith.science/paper/ZUB4RQWD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2201.07079&json=true","fetch_graph":"https://pith.science/api/pith-number/ZUB4RQWDN66OWUJP65Z4SBPTWE/graph.json","fetch_events":"https://pith.science/api/pith-number/ZUB4RQWDN66OWUJP65Z4SBPTWE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE/action/storage_attestation","attest_author":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE/action/author_attestation","sign_citation":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE/action/citation_signature","submit_replication":"https://pith.science/pith/ZUB4RQWDN66OWUJP65Z4SBPTWE/action/replication_record"}},"created_at":"2026-07-05T04:53:26.285277+00:00","updated_at":"2026-07-05T04:53:26.285277+00:00"}