{"paper":{"title":"Modeling color-dependent galaxy clustering in cosmological simulations","arxiv_id":"1301.1217","primary_cat":"astro-ph.CO","submitted_at":"2013-01-07T14:57:07+00:00","version_compiled":"v2"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13-20260917 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 v2","sentences":[{"i":0,"p":0.73,"id":"s0","own":true,"role":"contribution","text":"We extend the subhalo abundance matching method to assign galaxy color to subhalos.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.96,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.02,"role_probabilities":{"gap":0.0,"method":0.27,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.73,"interpretation":0.0}},{"i":1,"p":0.99,"id":"s1","own":true,"role":"method","text":"We separate a luminosity-binned subhalo sample into two groups by a secondary subhalo property which is presumed to be correlated with galaxy color.","hedge":{"p":0.73,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":2,"p":0.94,"id":"s2","own":true,"role":"method","text":"The two subsamples then represent red and blue galaxy populations.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.63,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.94,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.05}},{"i":3,"p":0.98,"id":"s3","own":true,"role":"method","text":"We explore two models for the secondary property, namely subhalo assembly time and local dark matter density around each subhalo.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.88,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.43,"role_probabilities":{"gap":0.0,"method":0.98,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":4,"p":0.83,"id":"s4","own":true,"role":"method","text":"The model predictions for the galaxy two-point correlation functions are compared with the recent results from the Sloan Digital Sky Survey.","hedge":{"p":0.64,"label":"asserted"},"own_p":0.78,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.44,"role_probabilities":{"gap":0.0,"method":0.83,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.16,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"We show that the observed color dependence of galaxy clustering can be reproduced well by our method applied to cosmological N-body simulations without baryonic processes.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.46,"quantitative":false,"quantitative_p":0.31,"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":6,"p":0.63,"id":"s6","own":true,"role":"method","text":"We then compare the model predictions for the color-dependent galaxy-mass cross correlation functions with the results from gravitational lensing observations.","hedge":{"p":0.69,"label":"asserted"},"own_p":0.89,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.43,"role_probabilities":{"gap":0.0,"method":0.63,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.37,"interpretation":0.0}},{"i":7,"p":0.47,"id":"s7","own":true,"role":"interpretation","text":"The comparison allows us to distinguish the models, and also to discuss what subhalo property should be used to assign color to subhalos accurately.","hedge":{"p":0.67,"label":"asserted"},"own_p":0.9,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.1,"result":0.22,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.21,"interpretation":0.47}},{"i":8,"p":0.99,"id":"s8","own":true,"role":"result","text":"We show that the extended abundance matching method using the local dark matter density as a color proxy provides an accurate description of the galaxy populations in the local universe.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.73,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":9,"p":0.88,"id":"s9","own":true,"role":"contribution","text":"We also study impacts of scatter in the local dark matter density-color relations.","hedge":{"p":0.69,"label":"unclear"},"own_p":0.94,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.1,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.88,"interpretation":0.0}},{"i":10,"p":0.97,"id":"s10","own":true,"role":"result","text":"Introducing scatter improves agreements of our model predictions with the observed red and blue galaxy clustering and is needed to explain observed correlation functions in finer color bins.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.11,"quantitative":false,"quantitative_p":0.22,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":11,"p":0.9,"id":"s11","own":true,"role":"result","text":"Finally, we study red galaxy fraction profiles in galaxy group- and cluster-sized halos and find the red fraction profiles have a 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