{"paper":{"title":"Host star metallicity of directly imaged wide-orbit planets: implications for planet formation","arxiv_id":"2012.13694","primary_cat":"astro-ph.EP","submitted_at":"2020-12-26T07:57:34+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":"Directly imaged planets are self-luminous companions of pre-main sequence and young main sequence stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.01,"quantitative":false,"quantitative_p":0.06,"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":"They reside in wider orbits ($\\sim10\\mathrm{s}-1000\\mathrm{s}$~AU) and generally are more massive compared to the close-in ($\\lesssim 10$~AU) planets.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.08,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.99,"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":0.98,"id":"s2","own":false,"role":"background","text":"Determining the host star properties of these outstretched planetary systems is important to understand and discern various planet formation and evolution scenarios.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.04,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.02,"method":0.0,"result":0.0,"background":0.98,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"contribution","text":"We present the stellar parameters and metallicity ([Fe/H]) for a subsample of 18 stars known to host planets discovered by the direct imaging technique.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.93,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.98,"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":4,"p":1.0,"id":"s4","own":true,"role":"method","text":"We retrieved the high-resolution spectra for these stars from public archives and used the synthetic spectral fitting technique and Bayesian analysis to determine the stellar properties in a uniform and consistent way.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.08,"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":0.51,"id":"s5","own":true,"role":"result","text":"For eight sources, the metallicities are reported for the first time, while the results are consistent with the previous estimates for the other sources.","hedge":{"p":0.78,"label":"asserted"},"own_p":0.89,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.03,"method":0.0,"result":0.51,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.46,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"Our analysis shows that metallicities of stars hosting directly imaged planets are close to solar with a mean [Fe/H] = $-0.04\\pm0.27$~dex.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.38,"quantitative":true,"quantitative_p":0.99,"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":7,"p":1.0,"id":"s7","own":true,"role":"interpretation","text":"The large scatter in metallicity suggests that a metal-rich environment may not be necessary to form massive planets at large orbital distances.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.92,"main_claim_p":0.54,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}},{"i":8,"p":0.98,"id":"s8","own":true,"role":"result","text":"We also find that the planet mass-host star metallicity relation for the directly imaged massive planets in wide-orbits is very similar to that found for the well studied population of short period ($\\lesssim 1$~yr) super-Jupiters and brown-dwarfs around main-sequence stars.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.28,"quantitative":true,"quantitative_p":0.9,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.02}}]},"compiled":{"main_claim":{"p":0.88,"text":"The large scatter in metallicity suggests that a metal-rich 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