Statistics of intensity in adaptive-optics images and their usefulness for detection and photometry of exoplanets.
Statistics of intensity in adaptive-optics images and their usefulness for detection and photometry of exoplanets.
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自适应光学图像中的强度统计及其对于系外行星检测和光度测量的有用性。
DOI：
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发表时间：
2010
影响因子：
1.9
通讯作者：
J. Christou
中科院分区：
文献类型：
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作者：
S. Gladysz;N. Yaitskova;J. Christou
本文介绍了自适应光学散斑的概率密度函数建模问题。我们表明，使用修正的莱斯分布无法描述轴上光的统计数据。提出了双重解决方案：用于离轴散斑的修正莱斯分布和用于点扩散函数核心的基于伽马的分布。从这两个分布中，我们得出真实源和准静态散斑之间的最佳统计鉴别器。在本文的第二部分中，两个概率密度函数之间的形态差异用于约束系外行星位置处的一维“盲”迭代反卷积。在我们对 SPHERE 行星探测器的模拟中，信号和散斑的概率密度函数的分离产生了精确的微分光度测量。
This paper is an introduction to the problem of modeling the probability density function of adaptive-optics speckle. We show that with the modified Rician distribution one cannot describe the statistics of light on axis. A dual solution is proposed: the modified Rician distribution for off-axis speckle and gamma-based distribution for the core of the point spread function. From these two distributions we derive optimal statistical discriminators between real sources and quasi-static speckles. In the second part of the paper the morphological difference between the two probability density functions is used to constrain a one-dimensional, "blind," iterative deconvolution at the position of an exoplanet. Separation of the probability density functions of signal and speckle yields accurate differential photometry in our simulations of the SPHERE planet finder instrument.