{"paper":{"title":"The nonlinear power spectrum in clustering quintessence cosmologies","arxiv_id":"1106.0314","primary_cat":"astro-ph.CO","submitted_at":"2011-06-01T20:23:08+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-1.13-20260917 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 v1","sentences":[{"i":0,"p":0.97,"id":"s0","own":true,"role":"contribution","text":"We study the nonlinear evolution of density perturbations in cosmologies where the late-time accelerated expansion is driven by a quintessence field with vanishing speed of sound.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.88,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.97,"interpretation":0.0}},{"i":1,"p":0.65,"id":"s1","own":false,"role":"method","text":"For these models matter and quintessence perturbations are comoving and it is possible to write a single continuity equation for the total density fluctuations given by a weighted sum of the two components.","hedge":{"p":0.68,"label":"asserted"},"own_p":0.41,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.65,"result":0.01,"background":0.28,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.0}},{"i":2,"p":0.94,"id":"s2","own":true,"role":"method","text":"Including the Euler equation for the common velocity field we solve the evolution equations for the nonlinear, total density power spectrum in the Time-Renormalization Group approach.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.04,"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":3,"p":0.64,"id":"s3","own":false,"role":"interpretation","text":"In fact any cosmological observable is directly related by gravity only to the total density perturbations, with the two components being individually unobservable.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.13,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.03,"background":0.31,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.64}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"We show that the clustering of quintessence perturbations induces small corrections with respect to the nonlinear evolution of power spectrum in smooth quintessence models described by the same equation of state.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.45,"quantitative":true,"quantitative_p":0.75,"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":5,"p":0.51,"id":"s5","own":true,"role":"interpretation","text":"Such small corrections, however, contrast with the large effect of a vanishing speed of sound on the linear growth function at low redshift.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.69,"main_claim_p":0.18,"quantitative":true,"quantitative_p":0.94,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.49,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.51}},{"i":6,"p":0.75,"id":"s6","own":true,"role":"interpretation","text":"For this reason, models with the same normalization of the linear density power spectrum can present significantly different nonlinear corrections depending on the value of the sound speed.","hedge":{"p":0.82,"label":"asserted"},"own_p":0.64,"main_claim_p":0.26,"quantitative":true,"quantitative_p":0.67,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.25,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.75}},{"i":7,"p":0.93,"id":"s7","own":false,"role":"interpretation","text":"Although such differences vanish in the w \\rightarrow -1, {\\Lambda}CDM limit, we argue that the relation between linear and nonlinear growth of structures should be properly taken into account in constraining models with inhomogeneous dark energy.","hedge":{"p":0.43,"label":"hedged_possibility"},"own_p":0.42,"main_claim_p":0.65,"quantitative":false,"quantitative_p":0.31,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.07,"contribution":0.0,"interpretation":0.93}}]},"compiled":{"main_claim":{"p":0.72,"text":"Although such differences vanish in the w \\rightarrow -1, {\\Lambda}CDM limit, we argue that the relation between linear and nonlinear growth of structures should be properly taken into account in constraining models with inhomogeneous dark energy.","location":"abstract s7","hedge_strength":{"p":0.43,"label":"hedged possibility"}},"provenance":{"route":{"via":"OpenRouter","model":"classifier-1.13","endpoint":"https://openrouter.ai/api/v1/systemone","provider":"TypeSafe"},"packing":"one request per 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