结合Transit和RV的综合人口模型
Combining Transit and RV: A Synthesized Population Model
摘要：
我们提出了一个框架，估计系外行星的发生率综合约束径向速度和过境调查同时进行。我们采用近似贝叶斯计算和各种质量半径（M-R）的关系，探索人口模型描述这些调查，无论是单独和联合拟合。使用这种方法，我们适合的行星分布函数的形式$d^{2} N/d\log{P}d\log{M} \propto P^β M^α$，在$M_{b}$的质量的幂律中的一个突破，行星轨道FGK恒星周期$P = [25, 200]$天和质量$M = [2, 50] M_{\oplus}$。我们发现Otegi等人的M-R关系。（2020），它让岩石和挥发物丰富的种群在质量上重叠，使我们能够找到一个与两种类型的调查一致的模型。我们的联合拟合给出了$M_{b} = 21.6_{-3.2}^{+2.5} M_{\oplus}$（误差反映了68.3%的可信区间）。这几乎是一个三倍高于突破从过境只考虑和M-R关系没有这样的重叠。相应的行星-恒星质量比突变$q_{b} \sim 7\times10^{-5}$可能与微透镜研究（$q_b \sim 6\times10^{-5} - 2\times10^{-4}$）一致。联合拟合还要求重叠区域中的一小部分$F_{\text{rocky}} = 0.63_{-0.04}^{+0.04}$行星属于岩石种群。我们的研究结果强烈表明，未来的M-R关系应该考虑不同类型的行星的混合物，以描述观测到的行星人口。
英文摘要：
We present a framework for estimating exoplanet occurrence rates by synthesizing constraints from radial velocity and transit surveys simultaneously. We employ approximate Bayesian computation and various mass-radius (M-R) relations to explore the population models describing these surveys, both separately and in a joint fit. Using this approach, we fit a planet distribution function of the form $d^{2} N/d\log{P}d\log{M} \propto P^β M^α$, with a break in the power law in mass at $M_{b}$, to planets orbiting FGK stars with periods $P = [25, 200]$ days and masses $M = [2, 50] M_{\oplus}$. We find that the M-R relation from Otegi et al. (2020), which lets rocky and volatile-rich populations overlap in mass, allows us to find a model that is consistent with both types of surveys. Our joint fit gives $M_{b} = 21.6_{-3.2}^{+2.5} M_{\oplus}$ (errors reflect 68.3% credible interval). This is nearly a factor of three higher than the break from transit-only considerations and an M-R relation without such an overlap. The corresponding planet-star mass ratio break $q_{b} \sim 7\times10^{-5}$ may be consistent with microlensing studies ($q_b \sim 6\times10^{-5} - 2\times10^{-4}$). The joint fit also requires that a fraction of $F_{\text{rocky}} = 0.63_{-0.04}^{+0.04}$ planets in the overlap region belong to the rocky population. Our results strongly suggest that future M-R relations should account for a mixture of distinct types of planets in order to describe the observed planet population.
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