论文标题
附近的M矮人GL 514的四分之一世纪的光谱监测。在一个怪异轨道上移入和出口的超级地球
A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514. A super-Earth on an eccentric orbit moving in and out of the habitable zone
论文作者
论文摘要
我们调查了附近(7.6 PC)周围的行星同伴和Bright($ V = 9 $ MAG)早期型M矮人GL 514,分析了近25年来使用雇员,竖琴和唱片谱图收集的540个径向速度。由于出色的活动,该数据受到时间相关信号的影响,在2-3 ms $^{ - 1} $的级别上,我们根据高斯过程回归过滤了测试三个不同模型的测试。作为理智的交叉检查,我们使用用三种不同算法提取的竖琴径向速度重复了分析。我们使用雇用径向速度和Hipparcos-GAIA天文学来对长期伴侣的存在构成约束,并分析了TESS光度数据。我们发现有力的证据表明,GL 514在可能的偏心轨道上拥有超级地球,该轨道居住在保守的可居住区,其轨道时期的近34美元\%$。 Planet GL 514 B具有最低质量$ M_B \ SIN I_B = 5.2 \ PM0.9 $ $ M _ {\ rm EARTH} $,轨道周期$ P_B = 140.43 \ PM0.41 $ days $ days $ days,以及Ectricity $ e_b = 0.45^{+0.45^{+0.15^{+0.15} {+0.15} _.14}在苔丝光曲线中找不到过境的证据。没有证据表明在径向速度上有更长的时期伴侣,并且根据天文统计,我们可以排除$ \ sim0.2 $ $ m _ {\ rm jup} $ jup} $ planet,距离为$ \ sim3-10 $ au,以及巨大的巨型巨型星球/棕色的dwarfs/brown dwarfs to to dwarfs of au的数张力。我们讨论了与GL 514 b相比,与宿主距离短的距离距离较短的第二个低质量伴侣可能存在。 GL 514 B代表了一个有趣的科学案例,用于研究行星在偏心轨道上的可居住性。我们主张进行其他光谱随访,以获得更准确和精确的行星参数。还需要进一步的随访来研究子\ ms和较短的时期信号。
We investigated the presence of planetary companions around the nearby (7.6 pc) and bright ($V=9$ mag) early-type M dwarf Gl 514, analysing 540 radial velocities collected over nearly 25 years with the HIRES, HARPS, and CARMENES spectrographs. The data are affected by time-correlated signals at the level of 2-3 ms$^{-1}$ due to stellar activity, that we filtered out testing three different models based on Gaussian process regression. As a sanity cross-check, we repeated the analyses using HARPS radial velocities extracted with three different algorithms. We used HIRES radial velocities and Hipparcos-Gaia astrometry to put constraints on the presence of long-period companions, and we analysed TESS photometric data. We found strong evidence that Gl 514 hosts a super-Earth on a likely eccentric orbit, residing in the conservative habitable zone for nearly $34\%$ of its orbital period. The planet Gl 514 b has minimum mass $m_b\sin i_b=5.2\pm0.9$ $M_{\rm Earth}$, orbital period $P_b=140.43\pm0.41$ days, and eccentricity $e_b=0.45^{+0.15}_{-0.14}$. No evidence for transits is found in the TESS light curve. There is no evidence for a longer period companion in the radial velocities and, based on astrometry, we can rule out a $\sim0.2$ $M_{\rm Jup}$ planet at a distance of $\sim3-10$ au, and massive giant planets/brown dwarfs out to several tens of au. We discuss the possible presence of a second low-mass companion at a shorter distance from the host than Gl 514 b. Gl 514 b represents an interesting science case to study the habitability of planets on eccentric orbits. We advocate for additional spectroscopic follow-up to get more accurate and precise planetary parameters. Further follow-up is also needed to investigate sub \ms and shorter period signals.