论文标题
HST/FGS三角形的M-dwarf Eclips Binaries
HST/FGS Trigonometric Parallaxes of M-dwarf Eclipsing Binaries
论文作者
论文摘要
获得了哈勃太空望远镜（HST）精细的引导传感器（FGS）三角视差观测值，以直接确定与附近五个M-dwarf / m-dwarf Ecrelipsing二进制系统的距离。这些系统在本质上是有趣的，它是用于建立低质量恒星的基本物理参数（例如光度L和Radius R. HST/FGS距离）的基本物理参数，这也是对Gaia三角差距的少数直接检查之一，鉴于大小的敏感性在大小限制的限制和阵利偏角的确定下。进行了每个系统混合通量输出的光谱能分布（SED）拟合，从而估算每个系统的主要和次要组件的降压通量。从恒星M，L和R值中，将L和M之间的低质量恒星关系与R和M之间的低质量恒星关系与对此类恒星的理想化期望进行了比较。分析了对这些近级/m紫色对纳入这些紧密的M-dwarf/m-warf对的检查。这5个系统中的每个系统都表明是CPM系统的一部分。还提出了在视差参考恒星网格中发现的有趣物体的意外距离，其中包括附近的M矮人和白色矮人。
Hubble Space Telescope (HST) Fine Guidance Sensor (FGS) trigonometric parallax observations were obtained to directly determine distances to five nearby M-dwarf / M-dwarf eclipsing binary systems. These systems are intrinsically interesting as benchmark systems for establishing basic physical parameters for low-mass stars, such as luminosity L, and radius R. HST/FGS distances are also one of the few direct checks on Gaia trigonometric parallaxes, given the comparable sensitivity in both magnitude limit and determination of parallactic angles. A spectral energy distribution (SED) fit of each system's blended flux output was carried out, allowing for estimation of the bolometric flux from the primary and secondary components of each system. From the stellar M, L, and R values, the low-mass star relationships between L and M, and R and M, are compared against idealized expectations for such stars. An examination on the inclusion of these close M-dwarf/M-dwarf pairs in higher-order common proper motion (CPM) pairs is analysed; each of the 5 systems has indications of being part of a CPM system. Unexpected distances on interesting objects found within the grid of parallactic reference stars are also presented, including a nearby M dwarf and a white dwarf.
