Synthesizing Exoplanet Demographics: A Single Population of Long-Period Planetary Companions to M Dwarfs Consistent with Microlensing, Radial Velocity, and Direct Imaging Surveys
Christian Clanton, B. Scott Gaudi
备注：
33 pages, 30 figures. Submitted to ApJ. Comments welcome
We present the first study to synthesize results from five different exoplanet surveys using three independent detection methods: microlensing, radial velocity, and direct imaging. The constraints derived herein represent the most comprehensive picture of the demographics of large-separation (>~ 2 AU) planets orbiting the most common stars in our Galaxy that has been constructed to date. We assume a simple, joint power-law planet distribution function of the form d^2 N_{pl} /[dlog(m_p)dlog(a)] = A(m_p/ M_{Sat} )^{alpha}(a/2.5 AU)^{beta} with an outer cutoff radius of the separation distribution function of a_{out} . Generating populations of planets from these models and mapping them into the relevant observables for each survey, we use actual or estimated detection sensitivities to determine the expected observations for each survey. Comparing with the reported results, we derive constraints on the parameters {alpha, beta, A, a_{out} } that describe a single population of planets that is simultaneously consistent with the results of microlensing, RV, and direct imaging surveys. We find median and 68% confindence intervals of alpha = -0.86^{+0.21}_{-0.19} (-0.85^{+0.21}_{-0.19}), beta = 1.1^{+1.9}_{-1.4} (1.1^{+1.9}_{-1.3}), A = 0.21^{+0.20}_{-0.15} dex^{-2} (0.21^{+0.20}_{-0.15} dex^{-2}), and a_{out} = 10^{+26}_{-4.7} AU (12^{+50}_{-6.2} AU) assuming "hot-start" ("cold-start") planet evolutionary models. These values are consistent with all current knowledge of planets on orbits beyond ~2 AU around M dwarfs.
英文摘要：
We present the first study to synthesize results from five different exoplanet surveys using three independent detection methods: microlensing, radial velocity, and direct imaging. The constraints derived herein represent the most comprehensive picture of the demographics of large-separation (>~ 2 AU) planets orbiting the most common stars in our Galaxy that has been constructed to date. We assume a simple, joint power-law planet distribution function of the form d^2N_{pl}/[dlog(m_p)dlog(a)] = A(m_p/M_{Sat})^{alpha}(a/2.5 AU)^{beta} with an outer cutoff radius of the separation distribution function of a_{out}. Generating populations of planets from these models and mapping them into the relevant observables for each survey, we use actual or estimated detection sensitivities to determine the expected observations for each survey. Comparing with the reported results, we derive constraints on the parameters {alpha, beta, A, a_{out}} that describe a single population of planets that is simultaneously consistent with the results of microlensing, RV, and direct imaging surveys. We find median and 68% confindence intervals of alpha = -0.86^{+0.21}_{-0.19} (-0.85^{+0.21}_{-0.19}), beta = 1.1^{+1.9}_{-1.4} (1.1^{+1.9}_{-1.3}), A = 0.21^{+0.20}_{-0.15} dex^{-2} (0.21^{+0.20}_{-0.15} dex^{-2}), and a_{out} = 10^{+26}_{-4.7} AU (12^{+50}_{-6.2} AU) assuming "hot-start" ("cold-start") planet evolutionary models. These values are consistent with all current knowledge of planets on orbits beyond ~2 AU around M dwarfs.
Campaign 9 of the $K2$ Mission: Observational Parameters, Scientific Drivers, and Community Involvement for a Simultaneous Space- and Ground-based Microlensing Survey
Systematic KMTNet Planetary Anomaly Search. XIII. Complete Sample of 2021 Prime Field Planets
Westlake University（西湖大学）；Chungbuk National University（忠北国立大学）；Ohio State University（俄亥俄州立大学）；Korea Astronomy and Space Science Institute（韩国天文和空间科学研究所）；Massey University（梅西大学）；Osaka University（大阪大学）
Technique-agnostic exoplanet demography for the Roman era -- I. Testing a demography retrieval framework using simulated Kepler-like transit datasets
Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学天体物理学中心）；School of Physical and Chemical Sciences, University of Canterbury（坎特伯雷大学物理与化学科学学院）；Space Telescope Science Institute（太空望远镜科学研究所）；Université Marie et Louis Pasteur, CNRS, Institut UTINAM UMR 6213（玛丽和路易斯·巴斯德大学，法国国家科学研究中心，UTINAM研究所）；IPAC, Caltech（加州理工学院/IPAC）；Department of Astronomy, University of Maryland（马里兰大学天文学系）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Dipartimento di Fisica “E.R. Caianiello”, Università di Salerno（萨莱诺大学“E.R. Caianiello”物理系）
