{"paper":{"title":"Occurrence rates of small planets from HARPS: Focus on the Galactic context","arxiv_id":"2010.03237","primary_cat":"astro-ph.EP","submitted_at":"2020-10-07T07:35:19+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":"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":"The stars in the Milky Way thin and thick disks can be distinguished by several properties such as metallicity and kinematics.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.13,"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":0.97,"id":"s2","own":false,"role":"gap","text":"It is not clear whether the two populations also differ in the properties of planets orbiting the stars.","hedge":{"p":0.62,"label":"unclear"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.97,"method":0.0,"result":0.0,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.51,"id":"s3","own":false,"role":"background","text":"In order to study this, a careful analysis of both the chemical composition and mass detection limits is required for a sufficiently large sample.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.06,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.43,"method":0.05,"result":0.0,"background":0.51,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":0.94,"id":"s4","own":false,"role":"gap","text":"Currently, this information is still limited only to large radial-velocity (RV) programs.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.01,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.94,"method":0.0,"result":0.0,"background":0.06,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"contribution","text":"Based on the recently published archival database of the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, we present a first analysis of low-mass (small) planet occurrence rates in a sample of thin- and thick-disk stars. Aims.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.9,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.08,"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":6,"p":0.89,"id":"s6","own":false,"role":"contribution","text":"We aim to assess the effects of stellar properties on planet occurrence rates and to obtain first estimates of planet occurrence rates in the thin and thick disks of the Galaxy.","hedge":{"p":0.62,"label":"unclear"},"own_p":0.21,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.1,"contribution":0.89,"interpretation":0.0}},{"i":7,"p":0.89,"id":"s7","own":false,"role":"contribution","text":"As a baseline for comparison, we also aim to provide an updated value for the small close-in planet occurrence rate and compare it to results of previous RV and transit ($\\textit{Kepler}$) works. Methods.","hedge":{"p":0.66,"label":"unclear"},"own_p":0.41,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.44,"role_probabilities":{"gap":0.0,"method":0.04,"result":0.0,"background":0.02,"limitation":0.0,"future_work":0.05,"contribution":0.89,"interpretation":0.0}},{"i":8,"p":1.0,"id":"s8","own":true,"role":"method","text":"We used archival HARPS RV datasets to calculate detection limits of a sample of stars that were previously analysed for their elemental abundances.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"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":"For stars with known planets we first subtracted the Keplerian orbit.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.94,"main_claim_p":0.01,"quantitative":false,"quantitative_p":0.03,"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":0.98,"id":"s10","own":true,"role":"method","text":"We then used this information to calculate planet occurrence rates according to a simplified Bayesian model in different regimes of stellar and planet properties. Results.","hedge":{"p":0.83,"label":"asserted"},"own_p":0.94,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.98,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":11,"p":0.98,"id":"s11","own":true,"role":"result","text":"Our results suggest that metal-poor stars and more massive stars host fewer low-mass close-in planets.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.93,"main_claim_p":0.43,"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}},{"i":12,"p":1.0,"id":"s12","own":true,"role":"result","text":"We find the occurrence rates of these planets in the thin and thick disks to be comparable.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.38,"quantitative":true,"quantitative_p":0.93,"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":13,"p":1.0,"id":"s13","own":true,"role":"result","text":"In the iron-poor regimes, we find these occurrence rates to be significantly larger at the high-$\\alpha$ region (thick-disk stars) as compared with the low-$\\alpha$ region (thin-disk stars).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.2,"quantitative":true,"quantitative_p":0.97,"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":14,"p":0.99,"id":"s14","own":true,"role":"result","text":"In general, we find the...","hedge":{"p":0.89,"label":"unclear"},"own_p":0.77,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.17,"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":0.55,"text":"We find the occurrence rates of these planets in the thin and thick disks to be comparable.","location":"abstract s12","hedge_strength":{"p":1.0,"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 paper","requests":1,"input_tokens":10748,"cost_usd_reported":0.0},"compiled_at":"2026-09-23","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13.0","abstract_states":{"claims_first":0.78,"states_limitation":0.41,"human_participants":0.02,"controlled_comparison":0.81,"randomized_assignment":0.01,"states_quantitative_result":0.22,"compares_with_prior_results":0.96,"mentions_code_or_data_availability":0.03},"evidential_basis":{"p":1.0,"value":"analysis of existing data","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":1.0,"observation_or_experiment":0.0,"simulation_or_computation":0.0}},"contribution_type":{"p":1.0,"value":"empirical study","probabilities":{"review":0.0,"method_or_tool":0.0,"empirical_study":1.0,"simulation_study":0.0,"theoretical_result":0.0,"dataset_or_benchmark":0.0,"position_or_commentary":0.0}},"contribution_statement":{"p":0.99,"text":"Based on the recently published archival database of the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, we present a first analysis of low-mass (small) planet occurrence rates in a sample of thin- and thick-disk stars. 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