{"paper":{"title":"Non-Gaussian matter fluctuations from primordial magnetic fields and galaxy luminosity function","arxiv_id":"2611.15188","primary_cat":"astro-ph.CO","submitted_at":"2026-11-11T08:35:51+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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structures.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.08,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.49,"id":"s2","own":true,"role":"contribution","text":"While previous studies have primarily characterized these imprints via the matter power spectrum --- a two-point statistic --- we demonstrate that the one-point statistics of PMF-induced density fluctuations reveal an intrinsically non-Gaussian probability distribution function (PDF), even when the PMFs themselves are statistically Gaussian.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.58,"quantitative":true,"quantitative_p":0.62,"role_probabilities":{"gap":0.25,"method":0.0,"result":0.26,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.49,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"In particular, we find that the high-density tail of the PDF is enhanced by over two orders of magnitude relative to the Gaussian case.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.91,"id":"s4","own":true,"role":"result","text":"Adopting the Press-Schechter formalism, we show that this non-Gaussianity significantly boosts the abundance of rare objects, especially massive halos and those at high redshifts.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.91,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.04}},{"i":5,"p":0.79,"id":"s5","own":true,"role":"contribution","text":"We further compute the ultraviolet luminosity function of galaxies at $z=6$, $12$, and $16$, and compare our predictions with recent James Webb Space Telescope (JWST) observations that have reported an excess of high-redshift galaxies at $z\\sim 12$ -- $16$ relative to standard $\\Lambda$CDM expectations.","hedge":{"p":0.95,"label":"asserted"},"own_p":0.91,"main_claim_p":0.1,"quantitative":true,"quantitative_p":0.95,"role_probabilities":{"gap":0.0,"method":0.14,"result":0.07,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.79,"interpretation":0.0}},{"i":6,"p":0.92,"id":"s6","own":true,"role":"interpretation","text":"Intriguingly, in the limiting case where the total density field inherits this PDF, our results suggest that the non-Gaussian density fluctuations sourced by PMFs can explain the bright-end ($M_\\mathrm{UV}\\lesssim -18$) excess at $z\\gtrsim 12$, without requiring additional astrophysical enhancements to star-formation 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