论文标题
TOI-1728b：可居住区的行星查找器确认了一个温暖的超海王星
TOI-1728b: The Habitable-zone Planet Finder confirms a warm super Neptune orbiting an M dwarf host
论文作者
论文摘要
我们使用基于地面的光度法，近红外多普勒赛车仪和光谱法与可居住的区域planet finder.toi-1728相结合，证实了TOI-1728B的行星性质。 $ \ sim $ 3.49天的轨道周期。径向速度，苔丝和基于地面的过渡的联合拟合产生的行星半径为$ 5.05 _ { - 0.17}^{+0.16} $ r $ _ {\ oplus} $，质量$ 26.78 _ { - 5.13} $ 0.057 _ { - 0.039}^{+0.054} $。我们估计了恒星特性，并在该行星的过境期间对He10830ÅAbsingpting进行搜索，并声称具有90 \％置信度的上限为1.1 $ \％$的无效检测。在GJ 3470b的行星大气中发现了更深层次的HE10830Å吸收，这是一种可比的气态行星。 TOI-1728b是最大的超级海王星 - 海王星和更大的天然气巨型行星之间的中间行星 - 围绕M矮人发现。 TOI-1728凭借其相对较大的质量和半径，代表了M-DWARF系外行星质量 - 拉迪乌斯图中的一个有价值的数据点，弥合了较轻的Neptune大小的行星与绕轨道M-warfs已知的较重的Jovian行星之间的缝隙。 With a low bulk density of $1.14_{-0.24}^{+0.26}$ g/cm$^3$, and orbiting a bright host star (J $\sim 9.6$, V $\sim 12.4$), TOI-1728b is also a promising candidate for transmission spectroscopy both from the ground and from space, which can be used to constrain planet formation and evolutionary models.
We confirm the planetary nature of TOI-1728b using a combination of ground-based photometry, near-infrared Doppler velocimetry and spectroscopy with the Habitable-zone Planet Finder.TOI-1728 is an old, inactive M0 star with \teff{} $= 3980^{+31}_{-32}$ K, which hosts a transiting super Neptune at an orbital period of $\sim$ 3.49 days. Joint fitting of the radial velocities and TESS and ground-based transits yields a planetary radius of $5.05_{-0.17}^{+0.16}$ R$_{\oplus}$, mass $26.78_{-5.13}^{+5.43}$ M$_{\oplus}$ and eccentricity $0.057_{-0.039}^{+0.054}$. We estimate the stellar properties, and perform a search for He 10830 Åabsorption during the transit of this planet and claim a null detection with an upper limit of 1.1$\%$ with 90\% confidence. A deeper level of He 10830 Å~ absorption has been detected in the planet atmosphere of GJ 3470b, a comparable gaseous planet. TOI-1728b is the largest super Neptune -- the intermediate subclass of planets between Neptune and the more massive gas-giant planets -- discovered around an M dwarf. With its relatively large mass and radius, TOI-1728 represents a valuable datapoint in the M-dwarf exoplanet mass-radius diagram, bridging the gap between the lighter Neptune-sized planets and the heavier Jovian planets known to orbit M-dwarfs. With a low bulk density of $1.14_{-0.24}^{+0.26}$ g/cm$^3$, and orbiting a bright host star (J $\sim 9.6$, V $\sim 12.4$), TOI-1728b is also a promising candidate for transmission spectroscopy both from the ground and from space, which can be used to constrain planet formation and evolutionary models.
