740.一个超级地球在靠近M1V恒星GJ的轨道上。HADES和CARMENES合作
A super-Earth on a close-in orbit around the M1V star GJ 740. A HADES and CARMENES collaboration
摘要：
M型矮星已经被证明是行星径向速度（RV）搜索的理想目标，因为它们具有更高的行星-恒星质量对比度。HADES和CARMENES计划旨在对北半球这类恒星周围的系外行星系统进行广泛的搜索，使我们能够从统计学上解决围绕这些物体运行的行星的特性。在这项工作中，我们进行了光谱和光度的研究程序的恒星（GJ 740），它表现出一个短周期RV信号兼容的行星伴侣。我们进行了光谱分析的基础上采取的时间跨度为6年的129 HARPS-N光谱结合57 HARPS光谱采取了4年，以及32 CARMENES光谱在超过1年，从而在一个数据集的时间覆盖范围为10年。我们还依赖于来自公共ASAS调查的459个测量值，时间覆盖范围为8年，以及来自EXORAP项目的$V$，$B$，$R$和$I$过滤器的5年光度星等，以进行光度研究。这两种分析都是使用马尔可夫链蒙特卡罗（MCMC）模拟和高斯过程回归来模拟恒星的活动。我们发现了一个短周期的超级地球，其轨道周期为2.37756 $^{+0.00013}_{-0.00011}$ d，最小质量为2.96 $^{+0.50}_{-0.48}$ M $_{\oplus}$。我们提供了一个更新的磁周期和旋转周期的恒星，获得的值$P_{\rm rot}$ =35.563 $\pm$ 0.071 d和$P_{\rm cycle}$ =2800 $\pm$ 150 d以前报道的表征。此外，RV的时间序列显示出一个可能的周期性长期信号，可能与土星质量的行星$\sim$ 100 M $_{\oplus}$有关。
英文摘要：
M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast. The HADES and CARMENES programs aim to carry out extensive searches of exoplanetary systems around this type of stars in the northern hemisphere, allowing us to address statistically the properties of the planets orbiting these objects. In this work, we perform a spectroscopic and photometric study of one of the program stars (GJ 740), which exhibits a short-period RV signal compatible with a planetary companion. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time-span of 6 yr combined with 57 HARPS spectra taken over 4 yr, as well as 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10 yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8 yr along with 5 yr of photometric magnitudes from the EXORAP project taken in the $V$, $B$, $R$, and $I$ filters to carry out a photometric study. Both analyses were made using Markov Chain Monte Carlo (MCMC) simulations and Gaussian Process regression to model the activity of the star. We present the discovery of a short-period super-Earth with an orbital period of 2.37756$^{+0.00013}_{-0.00011}$ d and a minimum mass of 2.96$^{+0.50}_{-0.48}$ M$_{\oplus}$. We offer an update to the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of $P_{\rm rot}$=35.563$\pm$0.071 d and $P_{\rm cycle}$=2800$\pm$150 d. Furthermore, the RV time-series exhibits a possibly periodic long-term signal which might be related to a Saturn-mass planet of $\sim$ 100 M$_{\oplus}$.
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