{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:4S7Z73KUDLFX4Y6LUHXUL6JBYE","short_pith_number":"pith:4S7Z73KU","schema_version":"1.0","canonical_sha256":"e4bf9fed541acb7e63cba1ef45f921c10e203392b2fedcc3e83388f47a0785de","source":{"kind":"arxiv","id":"2506.12709","version":3},"attestation_state":"computed","paper":{"title":"Constraints on Dark Energy Models Using Late Universe Probes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Shantanu Desai, Shubham Barua","submitted_at":"2025-06-15T03:43:47Z","abstract_excerpt":"We use late Universe probes - Type Ia Supernovae from the PantheonPlus compilation, Quasars, and Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1) BAO data - along with Cosmic Chronometers or Megamasers to constrain various dark energy parameterizations. These include the standard $\\Lambda$CDM model ($w_0=-1,w_a=0$), as well as the Chevallier-Polarski-Linder (CPL), Barboza-Alcaniz (BA), Jassal-Bagla-Padmanabhan (JBP), Exponential (EXP), and Transitional Dark Energy (TDE) parameterizations. We find that across all parameterizations, the constrained values of $w_0$ and $w_a$ remai"},"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":"2506.12709","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-06-15T03:43:47Z","cross_cats_sorted":[],"title_canon_sha256":"e8d0da8470515501962164c3b586ec984f99b402be5ea596d300a17b74ca5e20","abstract_canon_sha256":"72be855c8e7b0b4139f4fe2738523a7031be447e29b418fa4a9caff1419eab1f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:30:01.908311Z","signature_b64":"vbpQuH0XF058HjsCH7t3GqAqRPFuqDQeEOIDHRO423Cyvq+L5g8um1YODQA5fkC480L6XdnDiqGWGb+tOovFBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e4bf9fed541acb7e63cba1ef45f921c10e203392b2fedcc3e83388f47a0785de","last_reissued_at":"2026-07-05T11:30:01.907869Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:30:01.907869Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraints on Dark Energy Models Using Late Universe Probes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Shantanu Desai, Shubham Barua","submitted_at":"2025-06-15T03:43:47Z","abstract_excerpt":"We use late Universe probes - Type Ia Supernovae from the PantheonPlus compilation, Quasars, and Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1) BAO data - along with Cosmic Chronometers or Megamasers to constrain various dark energy parameterizations. These include the standard $\\Lambda$CDM model ($w_0=-1,w_a=0$), as well as the Chevallier-Polarski-Linder (CPL), Barboza-Alcaniz (BA), Jassal-Bagla-Padmanabhan (JBP), Exponential (EXP), and Transitional Dark Energy (TDE) parameterizations. We find that across all parameterizations, the constrained values of $w_0$ and $w_a$ remai"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2506.12709","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/2506.12709/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":"2506.12709","created_at":"2026-07-05T11:30:01.907923+00:00"},{"alias_kind":"arxiv_version","alias_value":"2506.12709v3","created_at":"2026-07-05T11:30:01.907923+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2506.12709","created_at":"2026-07-05T11:30:01.907923+00:00"},{"alias_kind":"pith_short_12","alias_value":"4S7Z73KUDLFX","created_at":"2026-07-05T11:30:01.907923+00:00"},{"alias_kind":"pith_short_16","alias_value":"4S7Z73KUDLFX4Y6L","created_at":"2026-07-05T11:30:01.907923+00:00"},{"alias_kind":"pith_short_8","alias_value":"4S7Z73KU","created_at":"2026-07-05T11:30:01.907923+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2603.10787","citing_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","ref_index":46,"is_internal_anchor":false},{"citing_arxiv_id":"2604.03756","citing_title":"Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?","ref_index":54,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE","json":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE.json","graph_json":"https://pith.science/api/pith-number/4S7Z73KUDLFX4Y6LUHXUL6JBYE/graph.json","events_json":"https://pith.science/api/pith-number/4S7Z73KUDLFX4Y6LUHXUL6JBYE/events.json","paper":"https://pith.science/paper/4S7Z73KU"},"agent_actions":{"view_html":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE","download_json":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE.json","view_paper":"https://pith.science/paper/4S7Z73KU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2506.12709&json=true","fetch_graph":"https://pith.science/api/pith-number/4S7Z73KUDLFX4Y6LUHXUL6JBYE/graph.json","fetch_events":"https://pith.science/api/pith-number/4S7Z73KUDLFX4Y6LUHXUL6JBYE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE/action/storage_attestation","attest_author":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE/action/author_attestation","sign_citation":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE/action/citation_signature","submit_replication":"https://pith.science/pith/4S7Z73KUDLFX4Y6LUHXUL6JBYE/action/replication_record"}},"created_at":"2026-07-05T11:30:01.907923+00:00","updated_at":"2026-07-05T11:30:01.907923+00:00"}