{"paper":{"title":"Baryons still trace dark matter: probing CMB lensing maps for hidden isocurvature","arxiv_id":"1704.03461","primary_cat":"astro-ph.CO","submitted_at":"2017-04-11T18:00:02+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-1.13.0 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 v2","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Compensated isocurvature perturbations (CIPs) are primordial fluctuations that balance baryon and dark-matter isocurvature to leave the total matter density unperturbed.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.03,"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":1.0,"id":"s1","own":false,"role":"background","text":"The effects of CIPs on the cosmic microwave background (CMB) anisotropies are similar to those produced by weak lensing of the CMB: smoothing of the power spectrum, and generation of non-Gaussian features.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.08,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.52,"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":2,"p":1.0,"id":"s2","own":false,"role":"gap","text":"Previous work considered the CIP effects on the CMB power-spectrum but neglected to include the CIP effects on estimates of the lensing potential power spectrum (though its contribution to the non-Gaussian, connected, part of the CMB trispectrum).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.06,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":1.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.68,"id":"s3","own":true,"role":"contribution","text":"Here, the CIP contribution to the standard estimator for the lensing potential power-spectrum is derived, and along with the CIP contributions to the CMB power-spectrum, Planck data is used to place limits on the root-mean-square CIP fluctuations on CMB scales, $\\Delta_{\\rm rms}^2(R_{\\rm CMB})$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.32,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.68,"interpretation":0.0}},{"i":4,"p":0.99,"id":"s4","own":true,"role":"result","text":"The resulting constraint of $\\Delta_{\\rm rms}^2(R_{\\rm CMB}) < 4.3 \\times 10^{-3}$ using this new technique improves on past work by a factor of $\\sim 3$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.47,"quantitative":true,"quantitative_p":0.99,"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":5,"p":0.58,"id":"s5","own":true,"role":"interpretation","text":"We find that for Planck data our constraints almost reach the sensitivity of the optimal CIP estimator.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.61,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.42,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.58}},{"i":6,"p":0.6,"id":"s6","own":true,"role":"result","text":"The method presented here is currently the most sensitive probe of the amplitude of a scale-invariant CIP power spectrum placing an upper limit of $A_{\\rm CIP}< 0.017$ at 95% CL.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.63,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.6,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.39}},{"i":7,"p":0.98,"id":"s7","own":false,"role":"future_work","text":"Future measurements of the large-scale CMB lensing potential power spectrum could probe CIP amplitudes as low as $\\Delta_{\\rm rms}^2(R_{\\rm CMB}) = 8 \\times 10^{-5}$ ($A_{\\rm CIP} = 3.2 \\times 10^{-4}$).","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.41,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.98,"contribution":0.0,"interpretation":0.01}}]},"compiled":{"main_claim":{"p":0.85,"text":"The method presented here is currently the most sensitive probe of the amplitude of a scale-invariant CIP power spectrum placing 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