Direct Detection and Characterization of Exoplanets Using Imaging Fourier Transform Spectroscopy

IF 3.3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Publications of the Astronomical Society of the Pacific Pub Date : 2024-05-14 DOI:10.1088/1538-3873/ad37d8
Jingwen Zhang, 婧雯 张, Michael Bottom and Eugene Serabyn
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Abstract

Space-based direct imaging provides prospects for detection and spectral characterization of exoplanets at optical and near-infrared wavelengths. Integral field spectrographs (IFS) have been historically baselined for these mission concepts. However, multiple studies have revealed that detector noise is a serious obstacle for such instruments when observing extremely faint targets such as Earth-like planets. Imaging Fourier transform spectrographs (iFTS) are generally less sensitive to detector noise, and have several other compelling features such as simultaneous imaging and spectroscopy, smaller-format detector requirements, and variable spectral resolving power. To date, they have not been studied as options for such missions. Here, we compare the capabilities of IFS and iFTS for directly obtaining spectra from an Earth-like planet using both analytic and numerical models. Specifically, we compare the required exposure times to achieve the same signal-to-noise ratio with the two architectures over a range of detector and optical system parameters. We find that for a 6 m telescope, an IFS outperforms an iFTS at optical wavelengths due to the effects of distributed photon noise. In the near-IR, the relative efficiency of an IFS and iFTS depends critically on the instrument design and detector noise. An iFTS will be more efficient than an IFS if the readout noise of the near-IR detector is above ∼2–3 e− pix−1 frame−1 (tfrm = 1000 s), which correspond to half to one-third of the state-of-art detector noise. However, if the readout noise is reduced below this threshold, the performance of an IFS will experience a substantial improvement and become more efficient. These results motivate consideration of an iFTS as an alternative option for future direct imaging space missions in the near-IR.
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利用成像傅立叶变换光谱直接探测系外行星并确定其特征
天基直接成像为在光学和近红外波长探测系外行星并确定其光谱特征提供了前景。积分场摄谱仪(IFS)历来是这些任务概念的基础。然而,多项研究表明,在观测类地行星等极其微弱的目标时,探测器噪声是这类仪器的一个严重障碍。成像傅立叶变换摄谱仪(iFTS)对探测器噪声的敏感度通常较低,而且还具有其他一些引人注目的特点,如同时成像和分光、对探测器的尺寸要求较小、光谱分辨能力可变等。迄今为止,尚未将它们作为此类任务的备选方案进行研究。在这里,我们利用分析和数值模型比较了 IFS 和 iFTS 直接获取类地行星光谱的能力。具体来说,我们比较了在一定探测器和光学系统参数范围内,使用这两种结构实现相同信噪比所需的曝光时间。我们发现,对于 6 米望远镜来说,由于分布式光子噪声的影响,IFS 在光学波长上优于 iFTS。在近红外波段,IFS 和 iFTS 的相对效率主要取决于仪器设计和探测器噪声。如果近红外探测器的读出噪声高于 ∼2-3 e- pix-1 frame-1 (tfrm = 1000 s),即相当于最先进探测器噪声的一半到三分之一,那么 iFTS 的效率将高于 IFS。然而,如果读出噪声降低到这一阈值以下,IFS 的性能就会得到大幅提升,变得更加高效。这些结果促使人们考虑将 iFTS 作为未来近红外直接成像空间任务的替代选择。
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来源期刊
Publications of the Astronomical Society of the Pacific
Publications of the Astronomical Society of the Pacific 地学天文-天文与天体物理
CiteScore
6.70
自引率
5.70%
发文量
103
审稿时长
4-8 weeks
期刊介绍: The Publications of the Astronomical Society of the Pacific (PASP), the technical journal of the Astronomical Society of the Pacific (ASP), has been published regularly since 1889, and is an integral part of the ASP''s mission to advance the science of astronomy and disseminate astronomical information. The journal provides an outlet for astronomical results of a scientific nature and serves to keep readers in touch with current astronomical research. It contains refereed research and instrumentation articles, invited and contributed reviews, tutorials, and dissertation summaries.
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