用径向速度、依巴谷IAD-Gaia DR2天体测量学和多历元涡旋日冕测量上限约束波江座b的轨道和质量
Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multi-epoch Vortex Coronagraphy Upper Limits
摘要：
$ε$ ~波江座是一个年轻的行星系，拥有一个复杂的多带碎片盘和一颗被证实的类彗星行星，距离其主星3.48天文单位。它的年龄和建筑因此让人想起早期的太阳系。Mawet等人2019年的最新研究结合了径向速度（RV）数据和Ms波段直接成像上限，开始限制行星的轨道参数和质量，但仍然受到大误差条和简并的影响。在这里，我们利用最新的数据汇编从三个不同的技术，以进一步完善$ε$ ~Eridani~b的属性：RV，绝对天体测量从依巴谷~和盖亚~任务，和新的Keck/NIRC 2 MS波段涡旋日冕图像。我们在贝叶斯框架中结合这些数据。我们发现一个新的质量，$M_b$ = $0.66_{-0.09}^{+0.12}$ ~M $_{Jup}$，和倾角，$i$ = $77.95_{-21.06}^{\circ+28.50}$，与以前的不确定性，至少有一个因素2改善。我们还报告更新的约束的经度的升交点，参数的近星点，和近星点通过的时间。有了这些更新的参数，我们可以更好地预测行星在过去和未来任何时期的位置，这可以极大地帮助确定未来观测的战略和规划，以及随后的数据分析。特别是，这些结果可以帮助JWST和Nancy Grace Roman太空望远镜的日冕仪（CGI）进行直接探测。
英文摘要：
$ε$~Eridani is a young planetary system hosting a complex multi-belt debris disk and a confirmed Jupiter-like planet orbiting at 3.48 AU from its host star. Its age and architecture are thus reminiscent of the early Solar System. The most recent study of Mawet et al. 2019, which combined radial velocity (RV) data and Ms-band direct imaging upper limits, started to constrain the planet's orbital parameters and mass, but are still affected by large error bars and degeneracies. Here we make use of the most recent data compilation from three different techniques to further refine $ε$~Eridani~b's properties: RVs, absolute astrometry measurements from the Hipparcos~and Gaia~missions, and new Keck/NIRC2 Ms-band vortex coronagraph images. We combine this data in a Bayesian framework. We find a new mass, $M_b$ = $0.66_{-0.09}^{+0.12}$~M$_{Jup}$, and inclination, $i$ = $77.95_{-21.06}^{\circ+28.50}$, with at least a factor 2 improvement over previous uncertainties. We also report updated constraints on the longitude of the ascending node, the argument of the periastron, and the time of periastron passage. With these updated parameters, we can better predict the position of the planet at any past and future epoch, which can greatly help define the strategy and planning of future observations and with subsequent data analysis. In particular, these results can assist the search for a direct detection with JWST and the Nancy Grace Roman Space Telescope's coronagraph instrument (CGI).
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