Observations of Binary Stars with the Differential Speckle Survey Instrument. IX. Observations of Known and Suspected Binaries, and a Partial Survey of Be Stars
Observations of Binary Stars with the Differential Speckle Survey Instrument. IX. Observations of Known and Suspected Binaries, and a Partial Survey of Be Stars
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DOI：
10.3847/1538-3881/ab87a6
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发表时间：
2020-04
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影响因子：
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通讯作者：
E. Horch;G. V. van Belle;J. W. Davidson;D. Willmarth;F. Fekel;M. Muterspaugh;D. Casetti-Dinescu
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文献类型：
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作者：
E. Horch;G. V. van Belle;J. W. Davidson;D. Willmarth;F. Fekel;M. Muterspaugh;D. Casetti-Dinescu
我们报告了双星和多星系统的170个组成部分的370个测量结果，这些测量结果是从2015年至2017年洛厄尔天文台发现频道望远镜的差分散斑巡天仪进行的散斑成像观测中获得的。在研究的系统中，有147颗是双星，10颗是三重系统，还有1颗是四重系统。76个高质量的未检测和15个新解决的组件在我们的观察。相对天体测量中的不确定性似乎与我们以前在洛厄尔的工作相似，即线性测量不确定性约为2等，相对测光似乎在0.1-0.15等水平上不确定。使用这些测量值和文献中的测量值，我们计算了六个新的视觉轨道，其中包括Be 66 Oph星星的一个轨道和两个组合的光谱-视觉轨道。后两个轨道，即HD 22451（YSC 127）和HD 185501（YSC 135），产生了2%或更好水平的单个分量质量，以及独立的距离测量，在一种情况下与盖亚DR 2中发现的值一致，而在另一种情况下与2σ水平不一致。我们发现HD 22451由F6 V + F7 V对组成，轨道周期为2401.1 ± 3.2天，质量为1.342 ± 0.029和。对于HD 185501，两颗恒星都是G5矮星，彼此的公转周期为433.94 ± 0.15天，质量为0.898 ± 0.012和0.898 ± 0.012。我们讨论了新发现和轨道物体的细节。
We report 370 measures of 170 components of binary and multiple-star systems, obtained from speckle imaging observations made with the Differential Speckle Survey Instrument at Lowell Observatory’s Discovery Channel Telescope in 2015 through 2017. Of the systems studied, 147 are binary stars, 10 are seen as triple systems, and 1 quadruple system is measured. Seventy-six high-quality nondetections and 15 newly resolved components are presented in our observations. The uncertainty in relative astrometry appears to be similar to our previous work at Lowell, namely, linear measurement uncertainties of approximately 2 mas, and the relative photometry appears to be uncertain at the 0.1–0.15 mag level. Using these measures and those in the literature, we calculate six new visual orbits, including one for the Be star 66 Oph and two combined spectroscopic–visual orbits. The latter two orbits, which are for HD 22451 (YSC 127) and HD 185501 (YSC 135), yield individual masses of the components at the level of 2% or better, and independent distance measures that in one case agrees with the value found in the Gaia DR2 and in the other disagrees at the 2σ level. We find that HD 22451 consists of an F6V+F7V pair with orbital period of 2401.1 ± 3.2 days and masses of 1.342 ± 0.029 and . For HD 185501, both stars are G5 dwarfs that orbit one another with a period of 433.94 ± 0.15 days, and the masses are 0.898 ± 0.012 and . We discuss the details of both the new discoveries and the orbit objects.