{"paper":{"title":"MUSE Analysis of Gas around Galaxies (MAGG) -- VII. Emission line galaxies near strong blended Ly$\\alpha$ absorption systems at $z\\gtrsim3$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Strong blended Lyα absorption systems at z greater than 3 show a clear spatial and velocity correlation with nearby Lyα emitting galaxies.","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Davide Tornotti, Marta Galbiati, Matteo Fossati, Matthew Pieri, Michele Fumagalli","submitted_at":"2025-12-18T11:19:14Z","abstract_excerpt":"We investigate the connection between strong, blended Ly$\\alpha$ absorption systems (SBLAs) and $\\approx1000$ Ly$\\alpha$ emitting galaxies (LAEs) at $z\\gtrsim3$ in 28 quasar fields from the MUSE Analysis of Gas around Galaxies (MAGG) survey. Selecting SBLAs as spectral regions with transmitted flux $-0.05<F<0.25$ over $\\approx138\\text{ km s}^{-1}$ bins, we find a strong correlation with LAEs within a projected distance of $R\\le300\\rm\\,kpc$ and line-of-sight velocity separation of $|\\Delta v|\\le300 \\text{ km s}^{-1}$. The association rate increases significantly with decreasing flux, a trend th"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We find a strong correlation with LAEs within a projected distance of R≤300 kpc and line-of-sight velocity separation of |Δv|≤300 km s−1. The association rate increases significantly with decreasing flux, a trend that persists also at smaller separations (R<100 kpc).","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the chosen flux thresholds and velocity windows isolate physically associated systems rather than projection effects or unrelated absorbers, with the correlation arising from genuine CGM connections.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Strong blended Lyα absorbers cluster with Lyα emitting galaxies at z>3 within 300 kpc and 300 km/s, confirming they trace the circumgalactic medium interface.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Strong blended Lyα absorption systems at z greater than 3 show a clear spatial and velocity correlation with nearby Lyα emitting galaxies.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"bcb7fc69520386b72c2a791441bee26e61aaeb717c4c8432aab90aaee31e5eab"},"source":{"id":"2512.16422","kind":"arxiv","version":2},"verdict":{"id":"3cbcb5e3-2f4d-47e5-b554-059d0cdb6d69","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-16T21:19:53.593149Z","strongest_claim":"We find a strong correlation with LAEs within a projected distance of R≤300 kpc and line-of-sight velocity separation of |Δv|≤300 km s−1. The association rate increases significantly with decreasing flux, a trend that persists also at smaller separations (R<100 kpc).","one_line_summary":"Strong blended Lyα absorbers cluster with Lyα emitting galaxies at z>3 within 300 kpc and 300 km/s, confirming they trace the circumgalactic medium interface.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the chosen flux thresholds and velocity windows isolate physically associated systems rather than projection effects or unrelated absorbers, with the correlation arising from genuine CGM connections.","pith_extraction_headline":"Strong blended Lyα absorption systems at z greater than 3 show a clear spatial and velocity correlation with nearby Lyα emitting galaxies."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2512.16422/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":42,"sample":[{"doi":"","year":2022,"title":"Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123 Astropy Collaboration, Robitail","work_id":"092a9197-4e92-46c2-92ee-969bae5ceb3f","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2010,"title":"2010, in Society of Photo-Optical In- strumentation Engineers (SPIE) Conference Series, V ol","work_id":"83f0ccde-dbb5-413b-bce6-e6dbf02bed38","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2013,"title":"Becker, G. D., Hewett, P. C., Worseck, G., & Prochaska, J. X. 2013, MNRAS, 430, 2067","work_id":"0ba24fc4-6e85-4b74-9b63-26b18045bf64","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1996,"title":"Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393","work_id":"1ea79dc6-451d-4df0-83f2-e3aa0ebe3e13","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2013,"title":"D., Shanks, T., et al","work_id":"685c3715-b80a-4cb4-a9c4-640e932ea8dc","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":42,"snapshot_sha256":"8e15eda06c1b952d143cb192bde388170c6eff9f8f1ee2f79c635201301758e4","internal_anchors":1},"formal_canon":{"evidence_count":1,"snapshot_sha256":"463320df5f4981c80cafbddd8cdcb98709817d86081e0e52c5f393e4517f18df"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}