Euclid 准备工作. XXX. 通过广域与深场巡天的光谱模拟评估 NISP 红光栅光谱仪的性能
Euclid preparation. XXX. Performance assessment of the NISP Red-Grism through spectroscopic simulations for the Wide and Deep surveys
AI总结：
本研究通过 NISP 像元级模拟器构建星系光谱库，评估了 Euclid 广域与深场巡天的 NISP 红光栅光谱探测极限，发现其符合要求，并揭示了星系盘尺寸增加会降低发射线信噪比，而堆叠分析可探测暗弱发射线。
摘要：
本工作聚焦于一项模拟活动的试运行，该活动旨在研究 Euclid 近红外光谱仪和光度计（NISP）的光谱探测能力，即星系演化研究背景下的连续谱与发射线探测能力。为此，我们使用 NISP 像元级模拟器构建、模拟并分析了 4992 个红移在 $0.3 \leq z \leq 2.5$ 之间的恒星形成星系的光谱。我们基于包含光谱能量分布（SED）拟合结果增值信息的公开多波段星系目录，以及 Bruzual 和 Charlot (2003) 恒星族模板构建了光谱库。利用经验与理论关系，包含了静止光学和近红外星云发射线。对于具有中位盘半光半径为 \ang{;;0.4} 的恒星形成星系，我们推断了 Euclid 广域巡天在 $H= 19.5\pm0.2\\,$AB$\\,$mag 处以及 Euclid 深场巡天在 $H = 20.8\pm0.6\\,$AB$\\,$mag 处测得的 $H$ 波段连续谱 3.5$\sigma$ NISP 红光栅光谱探测极限。我们发现其与广域和深场巡天的红光栅发射线探测极限要求非常吻合。我们表征了星系形状对红光栅探测能力的影响，并强调了随着盘尺寸增加，提取光谱质量出现退化。具体而言，我们发现当盘尺寸从 \ang{;;0.25} 增加到 \ang{;;1} 时，提取的发射线信噪比（SNR）下降了约 45%。这些趋势导致了发射线 SNR 与星系恒星质量之间的相关性，我们在堆叠分析中证明了这一效应，揭示了原本太暗而无法探测的发射线。
英文摘要：
This work focuses on the pilot run of a simulation campaign aimed at investigating the spectroscopic capabilities of the Euclid Near-Infrared Spectrometer and Photometer (NISP), in terms of continuum and emission line detection in the context of galaxy evolutionary studies. To this purpose we constructed, emulated, and analysed the spectra of 4992 star-forming galaxies at $0.3 \leq z \leq 2.5$ using the NISP pixel-level simulator. We built the spectral library starting from public multi-wavelength galaxy catalogues, with value-added information on spectral energy distribution (SED) fitting results, and from Bruzual and Charlot (2003) stellar population templates. Rest-frame optical and near-IR nebular emission lines were included using empirical and theoretical relations. We inferred the 3.5$σ$ NISP red grism spectroscopic detection limit of the continuum measured in the $H$ band for star-forming galaxies with a median disk half-light radius of \ang{;;0.4} at magnitude $H= 19.5\pm0.2\,$AB$\,$mag for the Euclid Wide Survey and at $H = 20.8\pm0.6\,$AB$\,$mag for the Euclid Deep Survey. We found a very good agreement with the red grism emission line detection limit requirement for the Wide and Deep surveys. We characterised the effect of the galaxy shape on the detection capability of the red grism and highlighted the degradation of the quality of the extracted spectra as the disk size increases. In particular, we found that the extracted emission line signal to noise ratio (SNR) drops by $\sim\,$45$\%$ when the disk size ranges from \ang{;;0.25} to \ang{;;1}. These trends lead to a correlation between the emission line SNR and the stellar mass of the galaxy and we demonstrate the effect in a stacking analysis unveiling emission lines otherwise too faint to detect.
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