{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:LCGXY2CHE7YP4MHA6EUNBGJ2L2","short_pith_number":"pith:LCGXY2CH","schema_version":"1.0","canonical_sha256":"588d7c684727f0fe30e0f128d0993a5eb200303f10f1b7756cc3aada4ce454ff","source":{"kind":"arxiv","id":"2111.10457","version":2},"attestation_state":"computed","paper":{"title":"Model selection applied to reconstructions of the Dark Energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"J. Alberto Vazquez, Luis A. Escamilla","submitted_at":"2021-11-19T22:10:24Z","abstract_excerpt":"The main aim of this paper is to perform a model comparison for some reconstructions of the key properties that describe the dark energy of the Universe i.e. energy density and the equation of state (EoS). We carry out this process by using a binning and a linear interpolation methodologies, and on top of that, we incorporate a correlation function mechanism. An extension of the two of them was also introduced, where internal amplitudes are allowed to vary in height as well as in position. The reconstructions were made with data from the Hubble parameter, Supernovae Type Ia and Baryon Acoustic"},"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":"2111.10457","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-11-19T22:10:24Z","cross_cats_sorted":[],"title_canon_sha256":"147c48dd1d191643d645cee38017cb768e8e1b4b9ea79801d593e112f4407e17","abstract_canon_sha256":"18a66a5f73c522af21ea2633e4661851aee891035f4da7454d60c4d0cba6a0e7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:54:26.741817Z","signature_b64":"gQlPPkxnh1Wupk6GEoQOd/X8npyLVWj+WzKO3LeAbpOUESeeJO4AMIP02DojkSmFxCiMaEllB/WHmRiMKKsqCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"588d7c684727f0fe30e0f128d0993a5eb200303f10f1b7756cc3aada4ce454ff","last_reissued_at":"2026-07-05T05:54:26.741302Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:54:26.741302Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Model selection applied to reconstructions of the Dark Energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"J. Alberto Vazquez, Luis A. Escamilla","submitted_at":"2021-11-19T22:10:24Z","abstract_excerpt":"The main aim of this paper is to perform a model comparison for some reconstructions of the key properties that describe the dark energy of the Universe i.e. energy density and the equation of state (EoS). We carry out this process by using a binning and a linear interpolation methodologies, and on top of that, we incorporate a correlation function mechanism. An extension of the two of them was also introduced, where internal amplitudes are allowed to vary in height as well as in position. The reconstructions were made with data from the Hubble parameter, Supernovae Type Ia and Baryon Acoustic"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.10457","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/2111.10457/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":"2111.10457","created_at":"2026-07-05T05:54:26.741379+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.10457v2","created_at":"2026-07-05T05:54:26.741379+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.10457","created_at":"2026-07-05T05:54:26.741379+00:00"},{"alias_kind":"pith_short_12","alias_value":"LCGXY2CHE7YP","created_at":"2026-07-05T05:54:26.741379+00:00"},{"alias_kind":"pith_short_16","alias_value":"LCGXY2CHE7YP4MHA","created_at":"2026-07-05T05:54:26.741379+00:00"},{"alias_kind":"pith_short_8","alias_value":"LCGXY2CH","created_at":"2026-07-05T05:54:26.741379+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2402.07716","citing_title":"$\\Lambda_{\\rm s}$CDM cosmology from a type-II minimally modified gravity","ref_index":110,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11936","citing_title":"Probing dynamical dark energy with late-time data: Evidence, tensions, and the limits of the $w_0w_a$CDM framework","ref_index":121,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21456","citing_title":"Negative neutrino mass or negative dark energy?","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2510.18741","citing_title":"Nonlinear Matter Power Spectrum from relativistic $N$-body Simulations: $\\Lambda_{\\rm s}$CDM versus $\\Lambda$CDM","ref_index":169,"is_internal_anchor":false},{"citing_arxiv_id":"2604.12987","citing_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","ref_index":75,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2","json":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2.json","graph_json":"https://pith.science/api/pith-number/LCGXY2CHE7YP4MHA6EUNBGJ2L2/graph.json","events_json":"https://pith.science/api/pith-number/LCGXY2CHE7YP4MHA6EUNBGJ2L2/events.json","paper":"https://pith.science/paper/LCGXY2CH"},"agent_actions":{"view_html":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2","download_json":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2.json","view_paper":"https://pith.science/paper/LCGXY2CH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.10457&json=true","fetch_graph":"https://pith.science/api/pith-number/LCGXY2CHE7YP4MHA6EUNBGJ2L2/graph.json","fetch_events":"https://pith.science/api/pith-number/LCGXY2CHE7YP4MHA6EUNBGJ2L2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2/action/storage_attestation","attest_author":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2/action/author_attestation","sign_citation":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2/action/citation_signature","submit_replication":"https://pith.science/pith/LCGXY2CHE7YP4MHA6EUNBGJ2L2/action/replication_record"}},"created_at":"2026-07-05T05:54:26.741379+00:00","updated_at":"2026-07-05T05:54:26.741379+00:00"}