{"paper":{"title":"New and updated stellar parameters for 90 transit hosts. The effect of the surface gravity","arxiv_id":"1309.1998","primary_cat":"astro-ph.EP","submitted_at":"2013-09-08T19:32:34+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":1.0,"id":"s0","own":false,"role":"background","text":"Context.","hedge":{"p":1.0,"label":"unclear"},"own_p":0.02,"main_claim_p":0.01,"quantitative":false,"quantitative_p":0.02,"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":"Precise stellar parameters are crucial in exoplanet research for correctly determining of the planetary parameters.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"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":"background","text":"For stars hosting a transiting planet, determining of the planetary mass and radius depends on the stellar mass and radius, which in turn depend on the atmospheric stellar parameters.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.02,"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":3,"p":0.63,"id":"s3","own":false,"role":"background","text":"Different methods can provide different results, which leads to different planet characteristics.}%Spectroscopic surface gravities have shown to be poorly constrained, but the photometry of the transiting planet can provide an independent measurement of the surface gravity. Aims.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.09,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.36,"method":0.0,"result":0.0,"background":0.63,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.97,"id":"s4","own":true,"role":"contribution","text":"In this paper, we use a uniform method to spectroscopically derive stellar atmospheric parameters, chemical abundances, stellar masses, and stellar radii for a sample of 90 transit hosts.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.97,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.88,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.97,"interpretation":0.0}},{"i":5,"p":0.95,"id":"s5","own":true,"role":"method","text":"Surface gravities are also derived photometrically using the stellar density as derived from the light curve.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.95,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.0}},{"i":6,"p":0.92,"id":"s6","own":true,"role":"contribution","text":"We study the effect of using these different surface gravities on the determination of the chemical abundances and the stellar mass and radius. Methods.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.79,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":0.07,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.92,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"method","text":"A spectroscopic analysis based on Kurucz models in LTE was performed through the MOOG code to derive the atmospheric parameters and the chemical abundances.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"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":8,"p":1.0,"id":"s8","own":true,"role":"method","text":"The photometric surface gravity was determined through isochrone fitting and the use of the stellar density, directly determined from the light curve.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"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":9,"p":1.0,"id":"s9","own":true,"role":"method","text":"Stellar masses and radii are determined through calibration formulae. Results.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.83,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"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":10,"p":1.0,"id":"s10","own":true,"role":"result","text":"Spectroscopic and photometric surface gravities differ, but this has very little effect on the precise determination of the stellar mass in our spectroscopic analysis.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.33,"quantitative":true,"quantitative_p":0.83,"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":11,"p":0.95,"id":"s11","own":true,"role":"result","text":"The stellar radius, and hence the planetary radius, is most affected by the surface gravity discrepancies.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.41,"quantitative":true,"quantitative_p":0.71,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.95,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.05}},{"i":12,"p":0.97,"id":"s12","own":true,"role":"result","text":"For the chemical abundances, the difference is, as expected, only noticable for the abundances derived from analyzing of lines of ionized species.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.84,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.36,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.03}}]},"compiled":{"main_claim":{"p":0.9,"text":"The stellar radius, and hence the planetary radius, is most affected by the surface gravity discrepancies.","location":"abstract s11","hedge_strength":{"p":1.0,"label":"asserted"}},"provenance":{"route":{"via":"OpenRouter","model":"classifier-1.13","endpoint":"https://openrouter.ai/api/v1/systemone","provider":"TypeSafe"},"packing":"one request per paper","requests":1,"input_tokens":9501,"cost_usd_reported":0.000399},"compiled_at":"2026-09-23","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13-20260917","abstract_states":{"claims_first":0.04,"states_limitation":0.63,"human_participants":0.01,"controlled_comparison":0.28,"randomized_assignment":0.01,"states_quantitative_result":0.23,"compares_with_prior_results":0.85,"mentions_code_or_data_availability":0.02},"evidential_basis":{"p":0.82,"value":"analysis of existing data","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":0.82,"observation_or_experiment":0.17,"simulation_or_computation":0.01}},"contribution_type":{"p":0.79,"value":"empirical study","probabilities":{"review":0.0,"method_or_tool":0.0,"empirical_study":0.79,"simulation_study":0.0,"theoretical_result":0.0,"dataset_or_benchmark":0.21,"position_or_commentary":0.0}},"contribution_statement":{"p":0.98,"text":"In this paper, we use a uniform method to spectroscopically derive stellar atmospheric parameters, chemical abundances, stellar masses, and stellar radii for a sample of 90 transit hosts.","location":"abstract s4"}},"coverage":{"tier":"abstract","levels_run":["P abstract"],"not_examined":["full text","figures and tables","references and citing sentences","relations to other papers"],"sources_read":["arXiv listing abstract v1"],"levels_not_run":["S sections","T body sentences","C citations","R cross-paper relations"],"sentences_examined":13,"sentences_in_abstract":13},"measured_accuracy":{"url":"https://pith.science/accuracy","measured_on":"2026-10-02","method":"two independent model families labelled a fresh random sample blind; the figure is how often the published label matches their consensus","sentence_role_agreement":0.92,"main_claim_agreement":0.908,"typed_citation_agreement":0.933,"typed_citation_agreement_95_interval":[0.917,0.945],"review_comments_accurate":0.758,"review_comments_accurate_95_interval":[0.684,0.82],"review_caught_admitted_error_found_or_related":0.448}}