Simulation of High-contrast Polarimetric Observations of Debris Disks with the Roman Coronagraph Instrument

IF 3.3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Ramya M Anche, Ewan Douglas, Kian Milani, Jaren Ashcraft, Maxwell A. Millar-Blanchaer, John H Debes, Julien Milli, Justin Hom
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Abstract

The Nancy Grace Roman Space Telescope Coronagraph Instrument will enable the polarimetric imaging of debris disks and inner dust belts in the optical and near-infrared wavelengths, in addition to the high-contrast polarimetric imaging and spectroscopy of exoplanets. The Coronagraph uses two Wollaston prisms to produce four orthogonally polarized images and is expected to measure the polarization fraction with measurement errors <3% per spatial resolution element. To simulate the polarization observations through the Hybrid Lyot Coronagraph (HLC) and Shaped Pupil Coronagraph (SPC), we model disk scattering, the coronagraphic point-response function, detector noise, speckles, jitter, and instrumental polarization and calculate the Stokes parameters. To illustrate the potential for discovery and a better understanding of known systems with both the HLC and SPC modes, we model the debris disks around Epsilon Eridani and HR 4796A, respectively. For Epsilon Eridani, using astrosilicates with 0.37 ± 0.01 as the peak input polarization fraction in one resolution element, we recover the peak disk polarization fraction of 0.33 ± 0.01. Similarly, for HR 4796A, for a peak input polarization fraction of 0.92 ± 0.01, we obtain the peak output polarization fraction as 0.80 ± 0.03. The Coronagraph design meets the required precision, and forward modeling is needed to accurately estimate the polarization fraction.
模拟利用 Roman Coronagraph 仪器对碎片盘进行高对比度偏振观测
南希-格蕾丝-罗曼太空望远镜日冕仪将能够在光学和近红外波段对碎片盘和内部尘埃带进行偏振成像,此外还能对系外行星进行高对比度偏振成像和光谱分析。Coronagraph 使用两个 Wollaston 棱镜来生成四幅正交偏振图像,预计可以测量偏振分数,每个空间分辨率元素的测量误差为 3%。为了模拟通过混合里奥特日冕仪(HLC)和异型瞳孔日冕仪(SPC)进行的偏振观测,我们对圆盘散射、日冕仪点响应函数、探测器噪声、斑点、抖动和仪器偏振进行了建模,并计算了斯托克斯参数。为了说明利用 HLC 和 SPC 模式发现和更好地了解已知系统的潜力,我们分别对 Epsilon Eridani 和 HR 4796A 周围的碎片盘进行了建模。对于 Epsilon Eridani,我们使用天体硅酸盐(0.37 ± 0.01)作为一个分辨率元素的峰值输入偏振分数,恢复了 0.33 ± 0.01 的磁盘峰值偏振分数。同样,对于 HR 4796A,当峰值输入偏振分数为 0.92 ± 0.01 时,我们得到的峰值输出偏振分数为 0.80 ± 0.03。日冕仪的设计达到了所要求的精度,需要进行前向建模来精确估算偏振分数。
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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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