JWST/MIRI棱镜宽场无缝光谱的档案校准：方法、性能及GOODS-N/S场中$z=0-4$星系的中红外光谱图集
An Archival Calibration of JWST/MIRI Prism Wide-Field Slitless Spectroscopy: Methodology, Performance, and a Mid-Infrared Spectral Atlas of Galaxies at $z=0-4$ in the GOODS-N/S Fields
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中文总结 AI 辅助
本文通过AI辅助智能体工作流对JWST/MIRI棱镜宽场无缝光谱进行档案校准，提取180个星系光谱并验证PAH 3.3微米作为恒星形成率示踪剂，发布校准文件和光谱图集。
中文摘要 AI 辅助
通过JWST/MIRI的低分辨率光谱（LRS）观测模式，P750L棱镜色散整个约70\"×110\"的成像仪视场，将MIRI转变为在5-14微米波段、光谱分辨率$R\sim100$的宽场无缝光谱仪（WFSS）。利用在GOODS-N/S深场和校准项目中获取的档案MIRI LRS数据，我们在人工监督下通过AI辅助的智能体工作流程，为MIRI WFSS提供了一套完整且精确的校准套件。该校准包括平场、天空背景、光谱轨迹、波长校准、流量校准以及大尺度流量平场（L-flat）。我们介绍了每项校准的方法并量化了其精度。作为演示，我们提取了GOODS-N/S场中180个光谱确认的$z=0.08-3.71$星系的5-14微米无缝光谱。我们在单个源中探测到大量多环芳香烃（PAH）谱带和原子谱线（包括延伸到$z=3.71$的帕申α线）。对于$z\sim1$星系，PAH 3.3微米光度与帕申α光度（通过NIRCam WFSS测量）在约1.5个数量级范围内相关，支持PAH 3.3微米作为直至$z\sim1.6$的恒星形成率示踪剂。我们发布了校准参考文件、处理脚本和中红外光谱图集。我们还介绍了档案校准工作中的注意事项和经验教训。我们的经验灵敏度表征识别出深MIRI WFSS积分（$\gtrsim$几ks）的噪声基底，而较浅的积分则超过JWST曝光时间计算器预测的灵敏度。我们还为未来MIRI WFSS观测项目的规划提供了建议。
英文摘要
Through the Low Resolution Spectroscopy (LRS) observing mode of JWST/MIRI, the P750L prism disperses the entire ~70"$\times$110" imager field, turning MIRI into a wide-field slitless spectrograph (WFSS) at 5-14 $μ$m with spectral resolution $R\sim100$. Using archival MIRI LRS data taken in the GOODS-N/S deep fields and calibration programs, we present a complete and precise calibration suite for MIRI WFSS through an AI-assisted agentic workflow under human supervision. The calibration includes flat field, sky background, spectral tracing, wavelength calibration, flux calibration, and the large-scale flux flat (L-flat). We present the methodology of each calibration and quantify its accuracy. As a demonstration, we extract 5-14 $μ$m slitless spectra of 180 spectroscopically confirmed galaxies at $z=0.08 - 3.71$ in the GOODS-N/S fields. We detect a large number of polycyclic aromatic hydrocarbon (PAH) bands and atomic lines (including Paschen $α$ out to $z=3.71$) in individual sources. The PAH 3.3 $μ$m luminosities correlate with the Paschen $α$ luminosities (measured through NIRCam WFSS) for $z\sim1$ galaxies over a $\sim$1.5-dex range, supporting PAH 3.3 $μ$m as a star-formation-rate tracer out to $z\sim1.6$. We release the calibration reference files, reduction scripts, and the mid-infrared spectral atlas. We also present caveats and lessons learned from our archival calibration work. Our empirical sensitivity characterization identifies a noise floor for deep MIRI WFSS integrations ($\gtrsim$ a few ks), whereas shallower integrations exceed the sensitivity predicted by the JWST Exposure Time Calculator. We also provide suggestions for the planning of future MIRI WFSS observing programs.
发表机构
- Westlake University（西湖大学）
- Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所与高等科学研究中心天体生物学中心）
- Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
- Department of Astronomy and Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文学与天体物理学系）
- Tsinghua University（清华大学）
机构由 AI 辅助整理，请以论文原文为准。
