{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:GK2V7JKEDICMVEUU67ZCTOUOC5","short_pith_number":"pith:GK2V7JKE","schema_version":"1.0","canonical_sha256":"32b55fa5441a04ca9294f7f229ba8e177c8c3a8f0a77455f21383ecfa6a5729e","source":{"kind":"arxiv","id":"2406.07526","version":2},"attestation_state":"computed","paper":{"title":"Cosmological constraints on $\\Lambda_{\\rm s}$CDM scenario in a type II minimally modified gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Anita Yadav, Antonio De Felice, Eleonora Di Valentino, Emre \\\"Oz\\\"ulker, J. Alberto Vazquez, \\\"Ozg\\\"ur Akarsu, Rafael C. Nunes, Suresh Kumar","submitted_at":"2024-06-11T17:53:58Z","abstract_excerpt":"The idea of a rapid sign-switching cosmological constant (mirror AdS-dS transition) in the late universe at $z\\sim1.7$, known as the $\\Lambda_{\\rm s}$CDM model, has significantly improved the fit to observational data and provides a promising scenario for alleviating major cosmological tensions, such as the $H_0$ and $S_8$ tensions. However, in the absence of a fully predictive model, implementing this fit required conjecturing that the dynamics of the linear perturbations are governed by general relativity. Recent work embedding the $\\Lambda_{\\rm s}$CDM model with the Lagrangian of a type 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":"2406.07526","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-06-11T17:53:58Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"6d6390f9bf1d9f231a01438d70a7f553aef22e654b9b18248029d64ff35e6507","abstract_canon_sha256":"032b2ca2a9729888f580f72c4ab87696d301760b6eb8e64688bce89aaa573f75"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:39:55.446551Z","signature_b64":"yonBZfLeat2YKD+rSQpfnq19l2PiYn1Ygyc5H/6L7xRtBj0/kwYTk5pmL1bD12qlfqkblgNUlI2THCU4Xvg6AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"32b55fa5441a04ca9294f7f229ba8e177c8c3a8f0a77455f21383ecfa6a5729e","last_reissued_at":"2026-07-05T09:39:55.445926Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:39:55.445926Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmological constraints on $\\Lambda_{\\rm s}$CDM scenario in a type II minimally modified gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Anita Yadav, Antonio De Felice, Eleonora Di Valentino, Emre \\\"Oz\\\"ulker, J. Alberto Vazquez, \\\"Ozg\\\"ur Akarsu, Rafael C. Nunes, Suresh Kumar","submitted_at":"2024-06-11T17:53:58Z","abstract_excerpt":"The idea of a rapid sign-switching cosmological constant (mirror AdS-dS transition) in the late universe at $z\\sim1.7$, known as the $\\Lambda_{\\rm s}$CDM model, has significantly improved the fit to observational data and provides a promising scenario for alleviating major cosmological tensions, such as the $H_0$ and $S_8$ tensions. However, in the absence of a fully predictive model, implementing this fit required conjecturing that the dynamics of the linear perturbations are governed by general relativity. Recent work embedding the $\\Lambda_{\\rm s}$CDM model with the Lagrangian of a type II "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2406.07526","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/2406.07526/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":"2406.07526","created_at":"2026-07-05T09:39:55.445984+00:00"},{"alias_kind":"arxiv_version","alias_value":"2406.07526v2","created_at":"2026-07-05T09:39:55.445984+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2406.07526","created_at":"2026-07-05T09:39:55.445984+00:00"},{"alias_kind":"pith_short_12","alias_value":"GK2V7JKEDICM","created_at":"2026-07-05T09:39:55.445984+00:00"},{"alias_kind":"pith_short_16","alias_value":"GK2V7JKEDICMVEUU","created_at":"2026-07-05T09:39:55.445984+00:00"},{"alias_kind":"pith_short_8","alias_value":"GK2V7JKE","created_at":"2026-07-05T09:39:55.445984+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":13,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.12464","citing_title":"Kinematic Probes of Type-II MMG: Pad\\'e Cosmographic Analysis of VCDM","ref_index":18,"is_internal_anchor":false},{"citing_arxiv_id":"2606.11062","citing_title":"A Friendly Phantom: Late-time AdS-to-dS transition and cosmological tensions","ref_index":27,"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":107,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31324","citing_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","ref_index":188,"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":84,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22599","citing_title":"The impact of evolving dark energy on the Weyl potential measured from the Dark Energy Survey Year 3 data","ref_index":25,"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":81,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21456","citing_title":"Negative neutrino mass or negative dark energy?","ref_index":89,"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":135,"is_internal_anchor":false},{"citing_arxiv_id":"2601.02077","citing_title":"Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity","ref_index":93,"is_internal_anchor":false},{"citing_arxiv_id":"2602.12347","citing_title":"Sign-Switching Dark Energy: Smooth Transitions with Recent DESI DR2 Observations","ref_index":76,"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":55,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14490","citing_title":"Spatially covariant gravity with two degrees of freedom: A perturbative analysis up to cubic order","ref_index":83,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5","json":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5.json","graph_json":"https://pith.science/api/pith-number/GK2V7JKEDICMVEUU67ZCTOUOC5/graph.json","events_json":"https://pith.science/api/pith-number/GK2V7JKEDICMVEUU67ZCTOUOC5/events.json","paper":"https://pith.science/paper/GK2V7JKE"},"agent_actions":{"view_html":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5","download_json":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5.json","view_paper":"https://pith.science/paper/GK2V7JKE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2406.07526&json=true","fetch_graph":"https://pith.science/api/pith-number/GK2V7JKEDICMVEUU67ZCTOUOC5/graph.json","fetch_events":"https://pith.science/api/pith-number/GK2V7JKEDICMVEUU67ZCTOUOC5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5/action/storage_attestation","attest_author":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5/action/author_attestation","sign_citation":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5/action/citation_signature","submit_replication":"https://pith.science/pith/GK2V7JKEDICMVEUU67ZCTOUOC5/action/replication_record"}},"created_at":"2026-07-05T09:39:55.445984+00:00","updated_at":"2026-07-05T09:39:55.445984+00:00"}