{"paper":{"title":"MUSE-DARK III: The evolution of the radial acceleration relation at intermediate redshifts","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"The radial acceleration relation in galaxies shows a higher characteristic scale at higher redshifts.","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"B. Famaey, B. I. Ciocan, D. Krajnovi\\'c, H. Desmond, J. Fensch, J. Freundlich, N. F. Bouch\\'e, R. Techi","submitted_at":"2026-04-24T14:41:00Z","abstract_excerpt":"The radial acceleration relation (RAR) is a tight empirical correlation between the observed radial acceleration (a_tot) and the baryonic radial acceleration (a_bar) measured across galaxy radii: these two accelerations start to deviate significantly from each other below a characteristic acceleration scale, a0. So far, observational studies of the RAR have predominantly focused on galaxies in the local Universe, leaving its evolution with cosmic time largely unexplored. Using high signal-to-noise data from the MUSE Hubble Ultra Deep Field survey, we investigate the RAR with a sample of 79 sta"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"Parametrizing the z-dependence as a0(z)= a0(0) + a1 * z, we obtain a1 = 1.59+/-0.1 *10^-10 m/s^2, providing evidence for a z-evolution.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The 3D forward modeling with disk-halo decomposition and pressure-support corrections accurately recovers the intrinsic accelerations without significant systematic bias from the choice of dark-matter halo profile or sample selection.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"The radial acceleration relation persists at intermediate redshifts but with a characteristic acceleration scale that increases linearly with redshift.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The radial acceleration relation in galaxies shows a higher characteristic scale at higher redshifts.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"d06999050c1b9c66fdd2d549330f772eeffcb2621f1253e729c66434ab32533e"},"source":{"id":"2604.22613","kind":"arxiv","version":1},"verdict":{"id":"ac35298f-47d5-4e06-883b-8229017623c2","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-08T10:42:37.495648Z","strongest_claim":"Parametrizing the z-dependence as a0(z)= a0(0) + a1 * z, we obtain a1 = 1.59+/-0.1 *10^-10 m/s^2, providing evidence for a z-evolution.","one_line_summary":"The radial acceleration relation persists at intermediate redshifts but with a characteristic acceleration scale that increases linearly with redshift.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The 3D forward modeling with disk-halo decomposition and pressure-support corrections accurately recovers the intrinsic accelerations without significant systematic bias from the choice of dark-matter halo profile or sample selection.","pith_extraction_headline":"The radial acceleration relation in galaxies shows a higher characteristic scale at higher redshifts."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.22613/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"doi_compliance","ran_at":"2026-05-19T23:47:34.070559Z","status":"completed","version":"1.0.0","findings_count":0}],"snapshot_sha256":"7c90b3e0c365edf76c58bfc36089684299265d1e56bd183e53056aace8403dbb"},"references":{"count":73,"sample":[{"doi":"","year":null,"title":", \" * write output.state after.block = add.period write newline","work_id":"","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"write newline","work_id":"","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":", \" * write output.state after.block = add.period write newline","work_id":"","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"write newline","work_id":"","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1939,"title":"Babcock , H. W. 1939, Lick Observatory Bulletin, 498, 41","work_id":"","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":5,"snapshot_sha256":"302f5b0a706a3058c9542e98e2807f9d1337fd016b373b95dcc2bcc095dd1596","internal_anchors":1},"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"}