{"paper":{"title":"Galaxy bias of radio AGN and star-forming galaxies from MIGHTEE and CMB lensing","arxiv_id":"2610.23567","primary_cat":"astro-ph.CO","submitted_at":"2026-10-16T14:52:09+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":"Radio galaxies play a significant role in galaxy evolution through feedback mechanisms, making it important to characterize the environments in which they reside.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"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":0.46,"id":"s1","own":true,"role":"method","text":"We measure the cross-correlation between the positions of radio sources in the MIGHTEE survey and cosmic microwave background lensing measurements from the Atacama Cosmology Telescope over $20\\ {\\rm deg}^2$ to flux densities $S_{\\rm 1.4\\,GHz}>40\\ {\\rm \\mu Jy}$, detecting the signal at $\\sim4\\sigma$ significance.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.98,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.46,"result":0.29,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.25,"interpretation":0.0}},{"i":2,"p":0.56,"id":"s2","own":true,"role":"method","text":"By combining this with auto-correlation measurements of low- and high-redshift radio samples, we constrain the redshift evolution of the galaxy bias parameter, $b(z)$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.56,"result":0.07,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.37,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"Fitting different models for the redshift evolution of the bias, we find that both a model inversely proportional to the linear growth factor, $b(z) = (1.63^{+0.19}_{-0.22})/D(z)$, and a model where bias grows linearly with redshift, $b(z) = (0.49^{+0.44}_{-0.32}) + (1.62^{+0.37}_{-0.51})z$, provide comparably good fits to the data, with the current measurements unable to distinguish between them.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.97,"main_claim_p":0.38,"quantitative":true,"quantitative_p":0.98,"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":0.94,"id":"s4","own":true,"role":"method","text":"Using a radio luminosity function, we estimate the fraction of sources that are active galactic nuclei (AGNs) or star-forming galaxies (SFGs) as a function of redshift, and model the individual contributions of AGNs and SFGs to the total bias.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.94,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.06,"interpretation":0.0}},{"i":5,"p":0.53,"id":"s5","own":true,"role":"method","text":"This approach allows us to measure the bias of AGNs and SFGs without individual source classifications.","hedge":{"p":0.95,"label":"asserted"},"own_p":0.84,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.53,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.25,"interpretation":0.2}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"Though no single model is favoured significantly, the best-fitting model gives $b_{\\rm AGN}(z) = (2.60^{+0.65}_{-0.91})/D(z)$ compared to $b_{\\rm SFG}(z) = (0.52^{+0.47}_{-0.34})/D(z)$.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.95,"main_claim_p":0.28,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"Incorporating SFG bias measurements from previous work as a prior tightens these constraints to $b_{\\rm AGN}(z) = (1.96^{+0.37}_{-0.40})/D(z)$ and $b_{\\rm SFG}(z) = (0.90^{+0.06}_{-0.06})/D(z)$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.89,"main_claim_p":0.28,"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}}]},"compiled":{"main_claim":{"p":0.58,"text":"Incorporating SFG bias measurements from previous work as a prior tightens these constraints to $b_{\\rm AGN}(z) = 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