{"paper":{"title":"Exacerbating the cosmological constant problem with interacting dark energy","arxiv_id":"1606.01538","primary_cat":"astro-ph.CO","submitted_at":"2016-06-05T17:47:35+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. 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worse.","hedge":{"p":0.76,"label":"asserted"},"own_p":0.1,"main_claim_p":0.38,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.07,"background":0.86,"limitation":0.01,"future_work":0.0,"contribution":0.01,"interpretation":0.01}},{"i":2,"p":0.81,"id":"s2","own":true,"role":"contribution","text":"We show that this is the case for 'interacting dark energy' models in which the masses of the dark matter states depend on the dark energy sector.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.79,"main_claim_p":0.2,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.16,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.81,"interpretation":0.0}},{"i":3,"p":0.99,"id":"s3","own":false,"role":"interpretation","text":"If realised in nature, these models have far-reaching implications for proposed solutions to the c.c.p. that require the number of vacua to exceed the fine-tuning of the vacuum energy density.","hedge":{"p":0.81,"label":"hedged_possibility"},"own_p":0.31,"main_claim_p":0.18,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.99}},{"i":4,"p":0.99,"id":"s4","own":true,"role":"result","text":"We show that current estimates of the number of flux vacua in string theory, $N_{\\rm vac} \\sim {\\cal O}(10^{272,000})$, is far too small to realise certain simple models of interacting dark energy \\emph{and} solve the cosmological constant problem anthropically.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.75,"main_claim_p":0.51,"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":0.01,"interpretation":0.0}},{"i":5,"p":0.77,"id":"s5","own":false,"role":"interpretation","text":"These models admit distinctive observational signatures that can be targeted by future gamma-ray observatories, hence making it possible to observationally rule out the anthropic solution to the cosmological constant problem in theories with a finite number of vacua.","hedge":{"p":0.62,"label":"hedged_possibility"},"own_p":0.43,"main_claim_p":0.34,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.14,"background":0.0,"limitation":0.0,"future_work":0.07,"contribution":0.02,"interpretation":0.77}}]},"compiled":{"main_claim":{"p":0.43,"text":"Such models do not address the fine-tuning problem of the vacuum energy, i.e. the cosmological constant problem (c.c.p.), but can make it spectacularly worse.","location":"abstract s1","hedge_strength":{"p":0.76,"label":"asserted"}},"provenance":{"route":{"via":"TypeSafe API","model":"classifier-1.13.0","endpoint":"https://api.typesafe.ai/v1/systemone","provider":"TypeSafe"},"packing":"one request per 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