论文标题
通过罗马冠状器工具对碎屑盘的偏光观测模拟
Simulations of polarimetric observations of debris disks through the Roman Coronagraph Instrument
论文作者
论文摘要
罗马冠冕仪器将展示高对比度的成像技术，从而实现微弱的碎屑磁盘的成像，内部灰尘带和行星的发现。碎片盘的极化研究提供了有关粉尘粒的大小，形状和分布的信息。 The Roman coronagraph uses a polarization module comprising two Wollaston prism assemblies to produce four orthogonally polarized images ($I_{0}$, $I_{90}$, $I_{45}$, and $I_{135}$), each measuring 3.2 arcsecs in diameter and separated by 7.5 arcsecs in the sky.线性极化分数测量中的预期RMS误差为3乘3像素的每个分辨率元素为1.66 \％。我们提出了一个数学模型，以通过罗马CGI模拟极化强度图像，包括仪器极化和其他不确定性。我们使用磁盘建模软件McFost，用于$ Q $，$ U $和碎片磁盘的极化强度，Epsilon-Eridani。极化强度与结合PSF形态的冠状动脉吞吐量进行了卷积。我们包括模型不确定性，检测器噪声，斑点噪声和抖动。最终极化分数为0.4 $ \ pm $ 0.0251，在后处理后获得。
The Roman coronagraph instrument will demonstrate high-contrast imaging technology, enabling the imaging of faint debris disks, the discovery of inner dust belts, and planets. Polarization studies of debris disks provide information on dust grains' size, shape, and distribution. The Roman coronagraph uses a polarization module comprising two Wollaston prism assemblies to produce four orthogonally polarized images ($I_{0}$, $I_{90}$, $I_{45}$, and $I_{135}$), each measuring 3.2 arcsecs in diameter and separated by 7.5 arcsecs in the sky. The expected RMS error in the linear polarization fraction measurement is 1.66\% per resolution element of 3 by 3 pixels. We present a mathematical model to simulate the polarized intensity images through the Roman CGI, including the instrumental polarization and other uncertainties. We use disk modeling software, MCFOST, to model $q$, $u$, and polarization intensity of the debris disk, Epsilon-Eridani. The polarization intensities are convolved with the coronagraph throughput incorporating the PSF morphology. We include model uncertainties, detector noise, speckle noise, and jitter. The final polarization fraction of 0.4$\pm$0.0251 is obtained after the post-processing.
