{"paper":{"title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Gravitationally induced particle creation fits data like ΛCDM while cutting the Hubble tension to 2.4-3 sigma.","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Eleonora Di Valentino, Giovanni Montani, Luis A. Escamilla, Mariaveronica De Angelis, Tiziano Schiavone","submitted_at":"2026-01-20T18:32:34Z","abstract_excerpt":"The Hubble tension and the unknown origin of dark energy motivate the exploration of alternative mechanisms for late-time cosmic acceleration. We investigate gravitationally induced particle creation (PC) as a non-equilibrium process that can effectively mimic dynamical dark energy. Within the thermodynamic framework of open systems, we adopt an agnostic approach to the extra created component, leaving its equation-of-state parameter $w_E$ free. We consider four phenomenological parametrisations of the PC rate, allowing deviations from the standard cosmological model ($\\Lambda$CDM) only at lat"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"All PC scenarios provide fits comparable to ΛCDM, with one showing effective dynamical dark-energy behaviour. When early- and late-time datasets are analysed separately, the PC models reduce the Hubble tension to ≃2.4σ--3σ, compared to 4.3σ in ΛCDM.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The assumption that particle-creation deviations from ΛCDM are confined to late times (0<z<3) and that the four chosen phenomenological parametrizations of the creation rate accurately capture the underlying gravitational process.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Gravitationally induced particle creation fits data like ΛCDM while cutting the Hubble tension to 2.4-3 sigma.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"be231d608ef9be1a5b462aed2b41975959226b4cf382498fbcc6f2fef0ef7f08"},"source":{"id":"2601.14222","kind":"arxiv","version":2},"verdict":{"id":"9c1b3ac1-2616-4b1f-aea0-811d4caa8d9b","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-16T12:11:07.883785Z","strongest_claim":"All PC scenarios provide fits comparable to ΛCDM, with one showing effective dynamical dark-energy behaviour. When early- and late-time datasets are analysed separately, the PC models reduce the Hubble tension to ≃2.4σ--3σ, compared to 4.3σ in ΛCDM.","one_line_summary":"Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The assumption that particle-creation deviations from ΛCDM are confined to late times (0<z<3) and that the four chosen phenomenological parametrizations of the creation rate accurately capture the underlying gravitational process.","pith_extraction_headline":"Gravitationally induced particle creation fits data like ΛCDM while cutting the Hubble tension to 2.4-3 sigma."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2601.14222/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":153,"sample":[{"doi":"","year":2013,"title":"Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results","work_id":"0bf957ea-774e-48d2-8808-c8107e0f672a","ref_index":1,"cited_arxiv_id":"1212.5225","is_internal_anchor":true},{"doi":"","year":2020,"title":"Planck 2018 results. VI. Cosmological parameters","work_id":"eeae0089-7b56-4c63-ace2-a31de468f6c5","ref_index":2,"cited_arxiv_id":"1807.06209","is_internal_anchor":true},{"doi":"","year":2020,"title":"Planck 2018 results. I. Overview and the cosmological legacy of Planck","work_id":"1d3770c7-d723-44a6-827d-4d71ce851971","ref_index":3,"cited_arxiv_id":"1807.06205","is_internal_anchor":true},{"doi":"","year":2007,"title":"Aiolaet al.(ACT), JCAP12, 047, arXiv:2007.07288 [astro-ph.CO]","work_id":"bb478244-fd3b-4ba3-8dc1-3de468c94476","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\\Lambda$CDM Parameters","work_id":"abcbecb3-ae6f-4748-a925-133dc8647d67","ref_index":5,"cited_arxiv_id":"2503.14452","is_internal_anchor":true}],"resolved_work":153,"snapshot_sha256":"19d90cb98e2ded95ed4d43a835b3951353284e01de6adcd0919d21e87e74b21e","internal_anchors":42},"formal_canon":{"evidence_count":2,"snapshot_sha256":"dfb7b2df32c48dd63577ddace2e4b6b16f1e7d9eaccde6c778c4e1d67d57f0c4"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}