{"paper":{"title":"The independence of the mid-infrared RR Lyrae Period-Luminosity relation from metallicity from a study of three globular clusters in the Large Magellanic Cloud","arxiv_id":"2609.21494","primary_cat":"astro-ph.SR","submitted_at":"2026-09-18T08:48:24+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. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"RR Lyrae are pulsating variable stars tracing old ($>10$ Gyr) stellar populations, and exhibit a strong mid-infrared Period-Luminosity (PL) relation that can be calibrated with known parallaxes to infer distances.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.06,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.93,"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":1,"p":0.99,"id":"s1","own":true,"role":"contribution","text":"Here we present Period-Luminosity relations and distance moduli for three isolated globular clusters in the Large Magellanic Cloud: Reticulum, NGC 1841, and NGC 1466.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.8,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.99,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"method","text":"Our analysis uses legacy \\textit{Spitzer Space Telescope} images obtained by the Carnegie RR Lyrae Program, and an internally self-consistent sample restricted to RRab stars, with cluster membership confirmed using Gaia DR3 proper motions and photometry.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.84,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.22,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"result","text":"In the Spitzer 3.6~$\\mu$m band, we simultaneously fit a PL for these clusters using a slope derived from Galactic Globular Clusters, yielding extinction-corrected distance moduli of $18.47\\pm0.09$ mag for Reticulum, $18.29\\pm0.09$ mag for NGC 1841, and $18.61\\pm0.09$ mag for NGC 1466.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.04,"result":0.95,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":0.67,"id":"s4","own":true,"role":"result","text":"The latter two are the first RR Lyrae PL-based distance moduli for these clusters, and all three are consistent with literature values from other techniques.","hedge":{"p":0.69,"label":"asserted"},"own_p":0.77,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.67,"role_probabilities":{"gap":0.05,"method":0.0,"result":0.67,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.15,"interpretation":0.13}},{"i":5,"p":0.93,"id":"s5","own":true,"role":"result","text":"Additionally we fit a PL with slope as a free parameter, and find that this LMC-derived PL is consistent with that derived from Galactic GCs.","hedge":{"p":0.62,"label":"asserted"},"own_p":0.97,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.71,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.93,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.0}},{"i":6,"p":0.92,"id":"s6","own":true,"role":"result","text":"Simultaneously fitting a PLZ for the three clusters yields a metallicity coefficient $c= -0.03\\pm0.05~\\mathrm{mag}~\\mathrm{dex}^{-1}$ which can be considered a negligible dependence of the PL on metallicity ($|c| <0.1$ mag dex$^{-1}$).","hedge":{"p":0.75,"label":"asserted"},"own_p":0.96,"main_claim_p":0.8,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.92,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.08}},{"i":7,"p":0.52,"id":"s7","own":true,"role":"interpretation","text":"Modelling an intrinsic width, $W$, to the PL/ PLZ yields a consistent value $W\\approx0.1\\pm0.02~\\mathrm{mag}$, suggesting intrinsic width is not driven by metallicity.","hedge":{"p":0.95,"label":"hedged_possibility"},"own_p":0.95,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.48,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.52}}]},"compiled":{"main_claim":{"p":1.0,"text":"Simultaneously fitting a PLZ for the three clusters yields a metallicity coefficient $c= 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