{"paper":{"title":"An Updated Characterization of Luminous Ly{\\alpha} emitters at the End of Reionization","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Luminous Lyα emitters at redshift 6 are low-mass ultra-young dwarf starbursts with high escape fractions.","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Linhua Jiang, Qiong Li, Si-Yue Yu, Xiaodi Yu, Yuanhang Ning, Yucheng Guo, Zheng Cai, Zhen-Ya Zheng","submitted_at":"2026-05-14T03:24:02Z","abstract_excerpt":"We present a multi-wavelength physical characterization of 14 luminous Ly$\\alpha$ emitters (LAEs) at $z\\approx6$, integrating deep ground-based Magellan/M2FS spectroscopy with heterogeneous JWST/NIRCam broad- and medium-band imaging. Identified via strong Ly$\\alpha$ lines with extreme Ly$\\alpha$ luminosities of ${>}10^{42.6}$ erg s$^{-1}$, the sample exhibits very large rest-frame equivalent widths (${\\gtrsim}100$ \\AA) and steeply blue UV continua ($\\beta_{\\rm median}\\simeq-2.2$, $-18.2>M_{\\rm 1500}>-20.2$ mag). Crucially, the integration of NIRCam medium-band photometry (F410M) breaks the deg"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The tightly constrained spectral energy distribution modeling demonstrates that these luminous LAEs tend to be unequivocally low-mass, ultra-young dwarf starbursts; half the sample is characterized by stellar masses of M_* < 10^8 M_⊙, ages ≲10 Myr, and negligible dust attenuation. The f_esc^Lyα values are exceptionally high, with a median of ≳40%.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The SED modeling assumptions that the medium-band F410M photometry fully breaks the degeneracy between nebular emission lines and Balmer breaks without residual template mismatches or unaccounted-for emission-line contributions from other species.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Luminous Lyα emitters at z≈6 are low-mass ultra-young dwarf starbursts with median Lyα escape fractions above 40 percent, driven by vigorous star formation and low dust content.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Luminous Lyα emitters at redshift 6 are low-mass ultra-young dwarf starbursts with high escape fractions.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"07a7f21f91549adedd02eb7ce7c8904e5ecb9e443b11c19684d9e550f2ebdaae"},"source":{"id":"2605.14313","kind":"arxiv","version":1},"verdict":{"id":"708e47f5-5e65-40f7-99c8-bb0aa073eaa8","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-15T02:32:32.317939Z","strongest_claim":"The tightly constrained spectral energy distribution modeling demonstrates that these luminous LAEs tend to be unequivocally low-mass, ultra-young dwarf starbursts; half the sample is characterized by stellar masses of M_* < 10^8 M_⊙, ages ≲10 Myr, and negligible dust attenuation. The f_esc^Lyα values are exceptionally high, with a median of ≳40%.","one_line_summary":"Luminous Lyα emitters at z≈6 are low-mass ultra-young dwarf starbursts with median Lyα escape fractions above 40 percent, driven by vigorous star formation and low dust content.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The SED modeling assumptions that the medium-band F410M photometry fully breaks the degeneracy between nebular emission lines and Balmer breaks without residual template mismatches or unaccounted-for emission-line contributions from other species.","pith_extraction_headline":"Luminous Lyα emitters at redshift 6 are low-mass ultra-young dwarf starbursts with high escape fractions."},"references":{"count":106,"sample":[{"doi":"","year":2023,"title":"Arrabal Haro, P., Dickinson, M., Finkelstein, S. L., et al. 2023, ApJL, 951, L22","work_id":"f7b7c2b1-b953-45c5-a37d-ea5a53169584","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2026,"title":"2026, arXiv e-prints, arXiv:2601.20045, 10.48550/arXiv.2601.20045","work_id":"f926f596-e9b1-46e4-9d9d-77357a67c1d3","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2016,"title":"2016, The Journal of Open Source Software, 1, 58","work_id":"45eba808-0360-4204-88c2-c299cf3a7c49","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1996,"title":"1996, A&AS, 117, 393","work_id":"f652ac43-6dc5-4a32-8469-36b2e87902e5","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2015,"title":"Bouwens, R. J., Illingworth, G. D., Oesch, P. A., et al. 2015, ApJ, 803, 34 Luminous LAEs at z ∼ 6 13","work_id":"ae4364a3-b03b-45ea-bf89-c79b51922e52","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":106,"snapshot_sha256":"b6640f67e1ac3ae79fe03c99ab6ae223003453265d16f5cc1891c063d0f1bcad","internal_anchors":4},"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"}