MAYONNAISE：近红外星周盘和系外行星成像的形态成分分析管道
MAYONNAISE: a morphological components analysis pipeline for circumstellar disks and exoplanets imaging in the near infrared
摘要：
在近红外成像拱星盘提供了前所未有的信息的形成和演化的行星系统。然而，目前的高对比度成像后处理技术，使用地面望远镜有一个有限的灵敏度扩展信号和他们的形态往往是困扰着强烈的形态失真。此外，当两个组成部分接近或交织在一起时，从磁盘中解开行星信号是具有挑战性的。我们提出了一个管道，能够检测各种各样的磁盘，并保持其形状和通量分布。通过构造，我们的方法将行星与盘分离开来。在分析了当前的角度差分成像（ADI）后处理技术所引起的失真后，我们建立了一个直接的模型的不同组成部分构成的时间序列的高对比度图像。在一个逆问题框架中，我们联合估计星光残差和潜在的扩展源和隐藏在图像中的点源，使用低复杂度先验的每个信号。为了验证和估计我们的方法的性能，我们在VLT/SPHERE-IRDIS数据上进行了测试，其中我们注入了合成磁盘和行星。我们还将我们的方法应用于包含真实磁盘的观测。我们的技术使得有可能检测磁盘从ADI数据集的对比度以上$3\times10^{-6}$相对于主机星。由于没有特定形状的磁盘被假定，我们能够提取各种各样的磁盘，包括面对磁盘。被检测盘的强度分布被准确地保存，并且即使靠近盘，也可以区分点源。
英文摘要：
Imaging circumstellar disks in the near-infrared provides unprecedented information about the formation and evolution of planetary systems. However, current post-processing techniques for high-contrast imaging using ground-based telescopes have a limited sensitivity to extended signals and their morphology is often plagued with strong morphological distortions. Moreover, it is challenging to disentangle planetary signals from the disk when the two components are close or intertwined. We propose a pipeline that is capable of detecting a wide variety of disks and preserving their shapes and flux distributions. By construction, our approach separates planets from disks. After analyzing the distortions induced by the current angular differential imaging (ADI) post-processing techniques, we establish a direct model of the different components constituting a temporal sequence of high-contrast images. In an inverse problem framework, we jointly estimate the starlight residuals and the potential extended sources and point sources hidden in the images, using low-complexity priors for each signal. To verify and estimate the performance of our approach, we tested it on VLT/SPHERE-IRDIS data, in which we injected synthetic disks and planets. We also applied our approach on observations containing real disks. Our technique makes it possible to detect disks from ADI datasets of a contrast above $3\times10^{-6}$ with respect to the host star. As no specific shape of the disks is assumed, we are capable of extracting a wide diversity of disks, including face-on disks. The intensity distribution of the detected disk is accurately preserved and point sources are distinguished, even close to the disk.
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