{"paper":{"title":"Latent-Space Gaussian Processes for Dark-Energy Reconstruction from Observational \\(H(z)\\) Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Placing a Gaussian process prior directly on dark-energy density f(z) yields viable reconstructions from Hubble data consistent with Lambda CDM.","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Jia-yan Jiang, Tong-Jie Zhang, Wei Hong","submitted_at":"2026-05-13T12:22:36Z","abstract_excerpt":"Using the 37-point cosmic-chronometer subset of observational Hubble parameter (OHD) data, we develop a Bayesian Gaussian-process framework to reconstruct the normalized dark-energy density \\(f(z)\\) and equation of state \\(w(z)\\), focusing on how the choice of latent space affects the inference. We compare a Gaussian-process prior placed directly on \\(f(z)\\) with the conventional latent-\\(H\\) formulation, and also test a log-\\(f\\) branch that enforces \\(f(z)>0\\). We further analyze OHD-like mock data generated from fiducial \\(\\Lambda\\)CDM and mildly evolving \\(w_0w_a\\) models, using both the o"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The latent-f approach is therefore a viable alternative to latent-H, while current constraints are limited mainly by sparse high-redshift OHD and dependence on external priors.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the chosen Gaussian process kernel and external priors do not systematically bias the reconstruction of f(z) and Om(z) in the high-redshift regime where data coverage is poorest.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Latent-f and latent-H Gaussian process reconstructions from OHD data both yield f(z), w(z), and Om(z) consistent with Lambda-CDM, with no strong predictive preference and small prior-dependent residuals mainly at high redshift.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Placing a Gaussian process prior directly on dark-energy density f(z) yields viable reconstructions from Hubble data consistent with Lambda CDM.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"44f4fa35e2316eeedfcad66ec86e22ab27bd26fd4a3a847d9f34bfd40b8553c8"},"source":{"id":"2605.13427","kind":"arxiv","version":1},"verdict":{"id":"7949d9f3-050e-4cb3-a523-c6ffc31f0f67","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-14T18:39:59.401141Z","strongest_claim":"The latent-f approach is therefore a viable alternative to latent-H, while current constraints are limited mainly by sparse high-redshift OHD and dependence on external priors.","one_line_summary":"Latent-f and latent-H Gaussian process reconstructions from OHD data both yield f(z), w(z), and Om(z) consistent with Lambda-CDM, with no strong predictive preference and small prior-dependent residuals mainly at high redshift.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the chosen Gaussian process kernel and external priors do not systematically bias the reconstruction of f(z) and Om(z) in the high-redshift regime where data coverage is poorest.","pith_extraction_headline":"Placing a Gaussian process prior directly on dark-energy density f(z) yields viable reconstructions from Hubble data consistent with Lambda CDM."},"references":{"count":96,"sample":[{"doi":"","year":null,"title":"denser high-z","work_id":"93e6b2d7-3984-4868-814c-34d77e0c80e6","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2025,"title":"TheOm(z)diagnostic Fig. 7 provides a direct visual summary of the prior-dependentOm(z) behavior. Consistent with the real-data entries in Appendix Table X, the inferred ∆Om0.5,1.0 and ∆Om 0.5,1.5 inte","work_id":"f4946de8-9931-4a3a-8e21-d5dd6c8b9ca8","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1989,"title":"S. Weinberg, Rev. Mod. Phys.61, 1 (1989)","work_id":"6c41be21-602f-404b-b69e-b98339d4cdf3","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2001,"title":"S. M. Carroll, Living reviews in relativity4, 1 (2001)","work_id":"c59ba072-3ded-418b-8bb9-527a5112d1cc","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2016,"title":"BeyondΛCDM: Problems, solutions, 13 and the road ahead","work_id":"19b91cf8-a4b4-4dba-b792-3c42323cf916","ref_index":5,"cited_arxiv_id":"1512.05356","is_internal_anchor":true}],"resolved_work":96,"snapshot_sha256":"2d88081fa99ea7336b54088ccc813e8f0cfde1043b04ca384fc05986f1283130","internal_anchors":40},"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"}