标题： 红外成像光谱仪（IRIS）的TMT：数据处理系统 显示英文标题

标题： The Infrared Imaging Spectrograph (IRIS) for TMT: Data Reduction System

摘要： IRIS（红外成像光谱仪）是三十米望远镜（TMT）的衍射极限第一光仪器，由近红外（0.84到2.4$\mu$m）成像仪和积分场光谱仪（IFS）组成。 IFS利用透镜阵列和切片器进行空间采样，将能够以数百种不同的模式运行，包括从4毫角秒（mas）到50 mas的四种板尺度的组合以及广泛的滤光片和光栅。 成像仪的视场为34$\times$34角秒$^{2}$，板尺度为4 mas，并有许多可选滤光片。 我们介绍了IRIS的数据减少系统（DRS）的初步设计，该系统需要解决所有这些观测模式。 IRIS数据的减少将面临独特的挑战，因为它将在观测序列期间提供成像和光谱数据的实时减少和分析，以及高级的后期处理算法。 DRS将支持IRIS的三种基本操作模式；减少来自成像仪、透镜阵列IFS和切片器IFS的数据。 DRS将使用Python编写，利用可用的开源天文学包。 除了实时数据减少外，DRS还将利用实时可视化工具，为天文学家提供目标获取和数据质量的最新评估。 快速查看套件将包括用于1D、2D和3D原始和减少图像的可视化工具。 我们讨论了DRS和可视化工具的整体要求，以及为了在所有宇宙距离尺度上利用科学案例而需要的校准数据，以实现最佳数据质量。 显示英文摘要

摘要： IRIS (InfraRed Imaging Spectrograph) is the diffraction-limited first light instrument for the Thirty Meter Telescope (TMT) that consists of a near-infrared (0.84 to 2.4 $\mu$m) imager and integral field spectrograph (IFS). The IFS makes use of a lenslet array and slicer for spatial sampling, which will be able to operate in 100's of different modes, including a combination of four plate scales from 4 milliarcseconds (mas) to 50 mas with a large range of filters and gratings. The imager will have a field of view of 34$\times$34 arcsec$^{2}$ with a plate scale of 4 mas with many selectable filters. We present the preliminary design of the data reduction system (DRS) for IRIS that need to address all of these observing modes. Reduction of IRIS data will have unique challenges since it will provide real-time reduction and analysis of the imaging and spectroscopic data during observational sequences, as well as advanced post-processing algorithms. The DRS will support three basic modes of operation of IRIS; reducing data from the imager, the lenslet IFS, and slicer IFS. The DRS will be written in Python, making use of open-source astronomical packages available. In addition to real-time data reduction, the DRS will utilize real-time visualization tools, providing astronomers with up-to-date evaluation of the target acquisition and data quality. The quicklook suite will include visualization tools for 1D, 2D, and 3D raw and reduced images. We discuss the overall requirements of the DRS and visualization tools, as well as necessary calibration data to achieve optimal data quality in order to exploit science cases across all cosmic distance scales.