标题： 在存在外星环状尘埃轮廓的情况下探测系外行星 显示英文标题

标题： Detecting Exoplanets in the Presence of Exozodiacal Dust Profiles

摘要： 对于类似地外行星探测器或系外行星探测器这样的地外行星直接探测任务概念，来自星周尘埃的光往往会掩盖图像中的任何地外行星。 用于在这一背景下识别点源的数据分析方法一直非常简单，传统上假设星周尘埃是均匀分布的，就像我们本地的星尘背景在几角秒尺度上是均匀的一样。 然而，星周尘埃云的典型尺寸预计会与典型地外行星轨道半径相当，或者至少是那些最感兴趣区域的轨道半径——即“适居带”范围从0.7-1.5 AU。 当由于成本原因减小直接探测仪器的尺寸时，点扩散函数（PSF）会变得更宽，使得区分点源和星周尘埃光的“斑块”变得更加困难。 在这种情况下，受散粒噪声限制的积分时间可能不够；相反，我们可能需要提高信噪比和/或进行后续测量，以解决图像数据中的歧义，以可计算且高置信度的方式识别点源，并隔离星周尘埃和地外行星对观测光曲线的贡献。 我们将研究一些典型的轮廓以及几种分析图像数据的方法，目标是构建一种解决此数据分析问题的方法。 显示英文摘要

摘要： For exoplanet direct detection mission concepts such as Terrestrial Planet Finder or Exoplanet Probe, light from the exozodiacal dust tends to obscure any exoplanets present in the image. Data analysis methods to identify point sources against this background have been very simple, traditionally with the simplifying assumption that the exozodi is uniformly distributed, just as our local zodiacal background is uniform over several-arcsec scales. However, the typical size of an exozodi cloud is expected to be comparable to the typical exoplanet orbital radii, or at least those of greatest interest_ the "habitable zone" range from 0.7-1.5 AU. When a direct detection instrument is reduced in size for cost reasons, the point spread function (PSF) becomes broader, making it more difficult to distinguish a point source from a "blob" of exozodi light. In this case, the shot-noise limited integration time may not be enough; instead we may need an elevated signal-to-noise ratio and/or later measurements to resolve ambiguities in the image data, identify a point source with a calculable and high confidence level, and isolate the exozodi and exoplanet contributions to the observed light profile. We will examine some typical profiles and a few methods of analyzing image data, with the goal of structuring an approach to this data analysis problem.