{"paper":{"title":"Late time approaches to the Hubble tension deforming $H(z)$, worsen the growth tension","arxiv_id":"2103.04045","primary_cat":"astro-ph.CO","submitted_at":"2021-03-06T06:28:34+00:00","version_compiled":"v3"},"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 v3","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Many late time approaches for the solution of the Hubble tension use late time smooth deformations of the Hubble expansion rate $H(z)$ of the Planck18/$\\Lambda$CDM best fit to match the locally measured value of $H_0$ while effectively keeping the comoving distance to the last scattering surface and $\\Omega_{0m} h^2$ fixed to maintain consistency with Planck CMB measurements.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.29,"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":false,"role":"background","text":"A well known problem of these approaches is that they worsen the fit to low $z$ distance probes.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.06,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.26,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.0,"background":0.99,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.76,"id":"s2","own":true,"role":"result","text":"Here we show that another problem of these approaches is that they worsen the level of the $\\Omega_{0m}-\\sigma_8$ growth tension.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.82,"main_claim_p":0.77,"quantitative":false,"quantitative_p":0.44,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.76,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.19,"interpretation":0.0}},{"i":3,"p":0.93,"id":"s3","own":true,"role":"method","text":"We use the generic class of CPL parametrizations corresponding to evolving dark energy equation of state parameter $w(z)=w_0+w_1\\frac{z}{1+z}$ with local measurements $H_0$ prior and identify the pairs $(w_0, w_1)$ that satisfy this condition.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.94,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.17,"role_probabilities":{"gap":0.0,"method":0.93,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.07,"interpretation":0.0}},{"i":4,"p":0.54,"id":"s4","own":false,"role":"background","text":"This is a generic class of smooth deformations of $H(z)$ that are designed to address the Hubble tension.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.11,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.42,"result":0.0,"background":0.54,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"We show that for these models the growth tension between dynamical probe data and CMB constraints is worse than the corresponding tension of the standard Planck18/$\\Lambda$CDM model.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.81,"quantitative":true,"quantitative_p":0.91,"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":0.99,"id":"s6","own":true,"role":"method","text":"We justify this feature using a full numerical solution of the growth equation and fit to the data, as well as by using an approximate analytic approach.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.94,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.05,"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":7,"p":0.76,"id":"s7","own":true,"role":"result","text":"The problem does not affect recent proposed solutions of the Hubble crisis involving a SnIa intrinsic luminosity transition at $z_t\\simeq 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