PHASES：一种星载超精密分光光度计的概念
PHASES: a concept for a satellite-borne ultra-precise spectrophotometer
摘要：
行星搜寻和天体地震学探测器分光光度计（PHASES）是一种用于获得通量校准光谱和测量附近恒星微星等光度变化的空间仪器概念。科学驱动力是确定恒星的物理特性和描述绕恒星运行的行星的特征，达到非常高的精度。PHASES计划安装在微型卫星上，由一个20厘米孔径的改进型贝克望远镜组成，向两个探测器供电：跟踪探测器，视场为1平方度，科学探测器用于进行分光光度测定。光学设计的主要目标是避免科学探测器上的杂散光，同时提供波长范围为370-960 nm的光谱，分辨率范围为370 nm时约900至960 nm时约200。在1分钟的积分中，V=10星等的恒星的信噪比在~ 35和140之间变化。对光变曲线的分析限制了行星相对于其母星半径的半径，而母星半径又受到绝对分光光度法和三角分光光度法的严格限制。临时光学设计满足所有科学要求，包括基于明亮A型恒星和模型大气观测的~1% rms通量校准策略，允许确定附近太阳系恒星的恒星角直径为0.5%。这种精度水平将传播到最近恒星的恒星半径，具有高度可靠的依巴谷天体半径，更重要的是，传播到行星半径。
英文摘要：
The Planet Hunting and Asteroseismology Explorer Spectrophotometer, PHASES, is a concept for a space-borne instrument to obtain flux calibrated spectra and measure micro-magnitude photometric variations of nearby stars. The science drivers are the determination of the physical properties of stars and the characterisation of planets orbiting them, to very high precision. PHASES, intended to be housed in a micro-satellite, consists of a 20 cm aperture modified Baker telescope feeding two detectors: the tracking detector, with a field of 1 degree square, and the science detector for performing spectrophotometry. The optical design has been developed with the primary goal of avoiding stray light on the science detector, while providing spectra in the wavelength range 370-960 nm with a resolving power that ranges from ~900 at 370 nm to ~200 at 960 nm. The signal to noise per resolution element obtained for a V=10 magnitude star in a 1 minute integration varies between ~ 35 and 140. An analysis of the light curve constrains the radii of the planets relative to their parent stars' radii, which are, in turn, tightly constrained by the combination of absolute spectrophotometry and trigonometric parallaxes. The provisional optical design satisfies all the scientific requirements, including a ~1% rms flux calibration strategy based on observations of bright A-type stars and model atmospheres, allowing the determination of stellar angular diameters for nearby solar-like stars to 0.5%. This level of accuracy will be propagated to the stellar radii for the nearest stars, with highly reliable Hipparcos parallaxes, and more significantly, to the planetary radii.
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