用CHARA阵列II：$ω$仙女座、HD 178911和仙王座分离的边缘包观测
Separated Fringe Packet Observations with the CHARA Array II: $ω$ Andromeda, HD 178911, and ξ Cephei
摘要：
当使用光学长基线干涉仪（OLBI）观测时，双星中的组成部分被充分分离，产生它们自己的干涉条纹包;这些被称为分离条纹包（SFP）双星。这些SFP二进制可以重叠的角度分离与制度的系统可分辨的散斑干涉在单一的，大口径望远镜，并可以提供额外的测量初步轨道缺乏良好的相位覆盖，帮助约束元素已经建立的轨道，并定位新的二进制之间的边界的光谱调查和散斑干涉的欠采样制度。在这个过程中，能见度校准星是不需要的，和分离的条纹包可以提供一个准确的矢量分离。在本文中，我们将SFP方法应用于ω仙女座，HD 178911和仙王座，在CHARA阵列上使用CLIMB三光束合束器。对于这些系统，我们确定ω仙女座的组件质量和视差为0.963 ${\pm}$ 0.049 $M_{\odot}$和0.860 ${\pm}$ 0.051 $M_{\odot}$和39.54 ${\pm}$ 1.85毫角秒（mas），对于HD 178911，0.802 ${\pm}$ <0.055 $M_{\odot}$和0.622 ${\pm}$ <0.053 $M_{\odot}$，28.26 ${\pm}$ <1.70 mas，造父变星的质量为1.045 ${\pm}$ 0.031 $M_{\odot}$和0.408 ${\pm}$ 0.066 $M_{\odot}$和38.10 ${\pm}$ 2.81 mas。
英文摘要：
When observed with optical long-baseline interferometers (OLBI), components of a binary star which are sufficiently separated produce their own interferometric fringe packets; these are referred to as Separated Fringe Packet (SFP) binaries. These SFP binaries can overlap in angular separation with the regime of systems resolvable by speckle interferometry at single, large-aperture telescopes and can provide additional measurements for preliminary orbits lacking good phase coverage, help constrain elements of already established orbits, and locate new binaries in the undersampled regime between the bounds of spectroscopic surveys and speckle interferometry. In this process, a visibility calibration star is not needed, and the separated fringe packets can provide an accurate vector separation. In this paper, we apply the SFP approach to ω Andromeda, HD 178911, and ξ Cephei with the CLIMB three-beam combiner at the CHARA Array. For these systems we determine component masses and parallax of 0.963${\pm}$0.049 $M_{\odot}$ and 0.860${\pm}$0.051 $M_{\odot}$ and 39.54${\pm}$1.85 milliarcseconds (mas) for ω Andromeda, for HD 178911 of 0.802${\pm}$0.055 $M_{\odot}$ and 0.622${\pm}$0.053 $M_{\odot}$ with 28.26${\pm}$1.70 mas, and masses of 1.045${\pm}$0.031 $M_{\odot}$ and 0.408${\pm}$0.066 $M_{\odot}$ and 38.10${\pm}$2.81 mas for ξ Cephei.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
