{"paper":{"title":"A population synthesis study of the Gaia 100 pc unresolved white dwarf-main sequence binary population","arxiv_id":"2502.11593","primary_cat":"astro-ph.SR","submitted_at":"2025-02-17T09:28:18+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-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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dwarf.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.06,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.21,"method":0.0,"result":0.0,"background":0.77,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"contribution","text":"This work aims to comprehensively simulate the population of unresolved WDMS binaries within 100 pc of the Sun and to compare the outcome with the currently most complete volume-limited sample available from Gaia data.","hedge":{"p":0.85,"label":"asserted"},"own_p":0.56,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.9,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"method","text":"We employ a population synthesis code, MRBIN, extensively developed by our group and based on Monte Carlo techniques, which uses a standard binary stellar evolutionary code adapted to cover a wide range of stars across all ages, masses, and metallicities.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.64,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"method","text":"Selection criteria matching those of Gaia observations are applied to generate synthetic populations comparable to the observed WDMS sample.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.91,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"The synthetic data accurately populate the expected regions in the Gaia color-magnitude diagram.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.1,"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":0.58,"id":"s6","own":true,"role":"result","text":"However, simulations predict a lower number of extremely low-mass white dwarfs, suggesting potential issues in observed mass derivations.","hedge":{"p":0.96,"label":"hedged_possibility"},"own_p":0.9,"main_claim_p":0.17,"quantitative":true,"quantitative_p":0.67,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.58,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.42}},{"i":7,"p":0.99,"id":"s7","own":true,"role":"result","text":"Additionally, our analysis constrains the common envelope efficiency to 0.1-0.4, consistent with previous findings, and estimates a total completeness of about 25% for the observed sample, confirming the strong observational limitations for unresolved WDMS.","hedge":{"p":0.78,"label":"asserted"},"own_p":0.93,"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}}]},"compiled":{"main_claim":{"p":0.99,"text":"Additionally, our analysis constrains the common envelope efficiency to 0.1-0.4, consistent with previous findings, and estimates a total completeness of about 25% for the observed sample, confirming the strong observational limitations for unresolved WDMS.","location":"abstract s7","hedge_strength":{"p":0.78,"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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