{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:LUHZDF6I2ROSAG35QUT5FUMK4Q","short_pith_number":"pith:LUHZDF6I","schema_version":"1.0","canonical_sha256":"5d0f9197c8d45d201b7d8527d2d18ae418f0c619772009070eecff076a79d386","source":{"kind":"arxiv","id":"1808.02472","version":3},"attestation_state":"computed","paper":{"title":"Ups and Downs in Dark Energy: phase transition in dark sector as a proposal to lessen cosmological tensions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Abdolali Banihashemi, Amir H. Shirazi, Nima Khosravi","submitted_at":"2018-08-07T17:47:36Z","abstract_excerpt":"Based on tensions between the early and late time cosmology, we proposed a double valued cosmological constant which could undergo a phase transition in its history. It is named \"double-$\\Lambda$ Cold Dark Matter\": $\\Lambda\\Lambda$CDM. An occurred phase transition results in (micro-) structures for the dark sector with a proper (local) interaction. In this paper, inspired by the physics of critical phenomena, we study a simplified model such that the cosmological constant has two values before a transition scale factor, $a_t$, and afterwards it becomes single-valued. We consider both the backg"},"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":"1808.02472","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-08-07T17:47:36Z","cross_cats_sorted":[],"title_canon_sha256":"7b271776e85988363a367b98a2918d6c4b9046cefbdd2c82574251cb641fc5ae","abstract_canon_sha256":"49747ccf57091c4601216678ff443d1e2b303e04652a06771716e856e85ddfaf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:14:21.703755Z","signature_b64":"xE3A0GK/tXAqp8LiVTbZVdTvaLDXUMqh2fbDnUbyFOrbDn6pEhQnw9peVAGs5nyA+Kmtu7jcIKS6Z8wvxbVoCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5d0f9197c8d45d201b7d8527d2d18ae418f0c619772009070eecff076a79d386","last_reissued_at":"2026-07-05T01:14:21.703166Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:14:21.703166Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Ups and Downs in Dark Energy: phase transition in dark sector as a proposal to lessen cosmological tensions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Abdolali Banihashemi, Amir H. Shirazi, Nima Khosravi","submitted_at":"2018-08-07T17:47:36Z","abstract_excerpt":"Based on tensions between the early and late time cosmology, we proposed a double valued cosmological constant which could undergo a phase transition in its history. It is named \"double-$\\Lambda$ Cold Dark Matter\": $\\Lambda\\Lambda$CDM. An occurred phase transition results in (micro-) structures for the dark sector with a proper (local) interaction. In this paper, inspired by the physics of critical phenomena, we study a simplified model such that the cosmological constant has two values before a transition scale factor, $a_t$, and afterwards it becomes single-valued. We consider both the backg"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1808.02472","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/1808.02472/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":"1808.02472","created_at":"2026-07-05T01:14:21.703229+00:00"},{"alias_kind":"arxiv_version","alias_value":"1808.02472v3","created_at":"2026-07-05T01:14:21.703229+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1808.02472","created_at":"2026-07-05T01:14:21.703229+00:00"},{"alias_kind":"pith_short_12","alias_value":"LUHZDF6I2ROS","created_at":"2026-07-05T01:14:21.703229+00:00"},{"alias_kind":"pith_short_16","alias_value":"LUHZDF6I2ROSAG35","created_at":"2026-07-05T01:14:21.703229+00:00"},{"alias_kind":"pith_short_8","alias_value":"LUHZDF6I","created_at":"2026-07-05T01:14:21.703229+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"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":98,"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":105,"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":150,"is_internal_anchor":false},{"citing_arxiv_id":"2604.12587","citing_title":"Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation","ref_index":57,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q","json":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q.json","graph_json":"https://pith.science/api/pith-number/LUHZDF6I2ROSAG35QUT5FUMK4Q/graph.json","events_json":"https://pith.science/api/pith-number/LUHZDF6I2ROSAG35QUT5FUMK4Q/events.json","paper":"https://pith.science/paper/LUHZDF6I"},"agent_actions":{"view_html":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q","download_json":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q.json","view_paper":"https://pith.science/paper/LUHZDF6I","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1808.02472&json=true","fetch_graph":"https://pith.science/api/pith-number/LUHZDF6I2ROSAG35QUT5FUMK4Q/graph.json","fetch_events":"https://pith.science/api/pith-number/LUHZDF6I2ROSAG35QUT5FUMK4Q/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q/action/storage_attestation","attest_author":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q/action/author_attestation","sign_citation":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q/action/citation_signature","submit_replication":"https://pith.science/pith/LUHZDF6I2ROSAG35QUT5FUMK4Q/action/replication_record"}},"created_at":"2026-07-05T01:14:21.703229+00:00","updated_at":"2026-07-05T01:14:21.703229+00:00"}