{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:IRDSGCYBTPN2UHDRXQP27VRFGS","short_pith_number":"pith:IRDSGCYB","schema_version":"1.0","canonical_sha256":"4447230b019bdbaa1c71bc1fafd625349419a2f3986389e73662daa483e9c566","source":{"kind":"arxiv","id":"2108.09239","version":3},"attestation_state":"computed","paper":{"title":"Relaxing cosmological tensions with a sign switching cosmological constant","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Emre Ozulker, J. Alberto Vazquez, Ozgur Akarsu, Suresh Kumar","submitted_at":"2021-08-20T15:58:21Z","abstract_excerpt":"Inspired by the recent conjecture originated from graduated dark energy that the Universe has recently transitioned from anti-de Sitter vacua to de Sitter vacua, we extend the $\\Lambda$CDM model by a cosmological constant ($\\Lambda_{\\rm s}$) that switches sign at a certain redshift $z_\\dagger$, and we call this model $\\Lambda_{\\rm s}$CDM. We discuss the construction and theoretical features of this model and find out that, when the consistency of $\\Lambda_{\\rm s}$CDM with the CMB data is ensured, (i) $z_\\dagger\\gtrsim1.1$ is implied by the condition that the Universe monotonically expands, (ii"},"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":"2108.09239","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-08-20T15:58:21Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"48891d5ff4f0d1a8eb46e42ef272702cb771cecfc9228a0125d9d16acba18e07","abstract_canon_sha256":"9518b4d41f4cba2a6bf0b872418c48a7aca1a94ba4d627f5e425baf4a3aceb17"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:37:45.209459Z","signature_b64":"buAJ5+/EN4j1A1S6Z4TYNIBcSoLGimXi0BhphQvG7+D7ow2Wi9uSbGnOj2HfXiGTuY4HdTMEumO0Iw3v5CC7BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4447230b019bdbaa1c71bc1fafd625349419a2f3986389e73662daa483e9c566","last_reissued_at":"2026-07-05T03:37:45.208942Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:37:45.208942Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Relaxing cosmological tensions with a sign switching cosmological constant","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Emre Ozulker, J. Alberto Vazquez, Ozgur Akarsu, Suresh Kumar","submitted_at":"2021-08-20T15:58:21Z","abstract_excerpt":"Inspired by the recent conjecture originated from graduated dark energy that the Universe has recently transitioned from anti-de Sitter vacua to de Sitter vacua, we extend the $\\Lambda$CDM model by a cosmological constant ($\\Lambda_{\\rm s}$) that switches sign at a certain redshift $z_\\dagger$, and we call this model $\\Lambda_{\\rm s}$CDM. We discuss the construction and theoretical features of this model and find out that, when the consistency of $\\Lambda_{\\rm s}$CDM with the CMB data is ensured, (i) $z_\\dagger\\gtrsim1.1$ is implied by the condition that the Universe monotonically expands, (ii"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2108.09239","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/2108.09239/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":"2108.09239","created_at":"2026-07-05T03:37:45.209016+00:00"},{"alias_kind":"arxiv_version","alias_value":"2108.09239v3","created_at":"2026-07-05T03:37:45.209016+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2108.09239","created_at":"2026-07-05T03:37:45.209016+00:00"},{"alias_kind":"pith_short_12","alias_value":"IRDSGCYBTPN2","created_at":"2026-07-05T03:37:45.209016+00:00"},{"alias_kind":"pith_short_16","alias_value":"IRDSGCYBTPN2UHDR","created_at":"2026-07-05T03:37:45.209016+00:00"},{"alias_kind":"pith_short_8","alias_value":"IRDSGCYB","created_at":"2026-07-05T03:37:45.209016+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":13,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.11062","citing_title":"A Friendly Phantom: Late-time AdS-to-dS transition and cosmological tensions","ref_index":12,"is_internal_anchor":false},{"citing_arxiv_id":"2606.06495","citing_title":"What it takes to solve the Hubble tension through Modifications of Cosmological Recombination II: in light of ACT DR6 and DESI DR2","ref_index":46,"is_internal_anchor":false},{"citing_arxiv_id":"2606.27436","citing_title":"Three-form dark energy: constraints and multi-probe comparison with $\\Lambda$CDM","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31362","citing_title":"Running into tension: primordial black holes from ultra-slow-roll inflation, spectral running, and the Hubble tension","ref_index":194,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31324","citing_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","ref_index":184,"is_internal_anchor":false},{"citing_arxiv_id":"2402.07716","citing_title":"$\\Lambda_{\\rm s}$CDM cosmology from a type-II minimally modified gravity","ref_index":81,"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":75,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21456","citing_title":"Negative neutrino mass or negative dark energy?","ref_index":33,"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":132,"is_internal_anchor":false},{"citing_arxiv_id":"2602.12347","citing_title":"Sign-Switching Dark Energy: Smooth Transitions with Recent DESI DR2 Observations","ref_index":71,"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":36,"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":49,"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":41,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS","json":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS.json","graph_json":"https://pith.science/api/pith-number/IRDSGCYBTPN2UHDRXQP27VRFGS/graph.json","events_json":"https://pith.science/api/pith-number/IRDSGCYBTPN2UHDRXQP27VRFGS/events.json","paper":"https://pith.science/paper/IRDSGCYB"},"agent_actions":{"view_html":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS","download_json":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS.json","view_paper":"https://pith.science/paper/IRDSGCYB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2108.09239&json=true","fetch_graph":"https://pith.science/api/pith-number/IRDSGCYBTPN2UHDRXQP27VRFGS/graph.json","fetch_events":"https://pith.science/api/pith-number/IRDSGCYBTPN2UHDRXQP27VRFGS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS/action/storage_attestation","attest_author":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS/action/author_attestation","sign_citation":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS/action/citation_signature","submit_replication":"https://pith.science/pith/IRDSGCYBTPN2UHDRXQP27VRFGS/action/replication_record"}},"created_at":"2026-07-05T03:37:45.209016+00:00","updated_at":"2026-07-05T03:37:45.209016+00:00"}