标题： 宇宙鼎盛时期星系中贫金属恒星形成结：使用JWST NIRISS的气体流入和化学稀释证据 显示英文标题

标题： Metal-Poor Star-Forming Clumps in Cosmic Noon Galaxies: Evidence for Gas Inflow and Chemical Dilution Using JWST NIRISS

摘要： 星系的形成和演化与重子循环密切相关，重子循环为恒星形成提供燃料，并塑造星系内的化学丰度。 研究大样本星系中恒星形成与金属丰度之间的关系需要昂贵的IFU巡天或复杂的工具来分析光栅数据。 在这里，我们使用Sleuth工具分析JWST NIRISS无狭缝光栅数据，该工具能够正向建模并从光栅数据中推断出空间分辨的物理特性，包括JWST NIRISS/NIRCam的观测数据以及未来如罗马空间望远镜的光栅数据。 Sleuth能够从无狭缝光谱中提取高质量的发射线图，克服了污染和空间变化的恒星种群，这些因素之前限制了此类研究。 利用Sleuth与加拿大NIRISS无偏集群巡天（CANUCS）的数据，我们研究了红移0.6 < z < 1.35范围内星系形成团块中的金属丰度与恒星形成之间的关系。 我们分析了一个包含20个星系的样本，使用Sleuth提取了高质量的发射线图，并详细分析了形成团块的空间分辨特性。 使用$H\alpha$、[SII]和[SIII]发射线图，我们检查了样本的空间分辨金属丰度、电离和恒星形成率。 我们的发现表明，这些形成团块的金属丰度（$\sim$ 0.1 dex）低于其周围的星系环境，表明团块气体中金属丰度稀释了20 $\%$。 我们的分析表明，这些团块表现出增强的恒星形成和较低的金属丰度，这可能是由于贫金属气体的流入所致。 这些团块展示了星系内部恒星形成与化学富集之间的动态关系。 显示英文摘要

摘要： The formation and evolution of galaxies are intricately linked to the baryon cycle, which fuels star formation while shaping chemical abundances within galaxies. Investigating the relationship between star formation and metallicity for large samples of galaxies requires expensive IFU surveys or sophisticated tools to analyze grism data. Here we analyze JWST NIRISS slitless grism data using Sleuth, a tool that forward models and infers spatially resolved physical properties from grism data, including observations from JWST NIRISS/NIRCam and future grism data like that from the Roman Space Telescope. Sleuth enables extraction of high-quality emission line maps from slitless spectra, overcoming contamination and spatially varying stellar populations, which previously limited such studies. Utilizing Sleuth with data from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS), we investigated the relationship between metallicity and star formation in the star-forming clumps of galaxies at 0.6 < z < 1.35. We analyzed a sample of 20 galaxies, extracted high-quality emission line maps with Sleuth, and analyzed, in detail, the spatially resolved properties of star-forming clumps. Using $H\alpha$, [SII], and [SIII] emission line maps, we examined the spatially resolved metallicities, ionization, and star formation rates of our sample. Our findings reveal that these star-forming clumps show lower metallicities ($\sim$ 0.1 dex) than their surrounding galactic environments, indicating a metallicity dilution of 20 $\%$ within the clumps' gas. Our analysis indicates that these clumps exhibit intensified star formation and reduced metallicity, likely due to the inflow of metal-poor gas. These clumps illustrate the dynamic relationship between star formation and chemical enrichment within galaxies.