发表机构
University of Massachusetts Amherst; University of California, Los Angeles; Siena University（马萨诸塞大学阿默斯特分校; 加州大学洛杉矶分校; 锡耶纳大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用DESI DR1的3457个星系样本构建尘埃消光曲线，发现曲线形状随恒星形成率显著变化，但与电离参数、质量或金属丰度无明显关联。
AI 中文摘要
利用从DESI DR1中选取的3457个星系样本，并与档案GALEX紫外测光数据交叉匹配，我们构建了新的尘埃消光曲线，并测量了这些曲线形状如何随星系性质变化。我们的曲线是通过比较按星云不透明度分箱（通过巴耳末光学深度，即H$\alpha$/H$\beta$比值测量）的星系的中值通量密度而构建的。当不对星系性质施加进一步切割时，我们得到的消光曲线与之前低红移研究的结果非常相似。随后，我们测试了消光曲线如何随星系性质（恒星质量、恒星形成率、金属丰度和电离参数）变化。我们发现，在较高的恒星形成率下，曲线显著变陡。在我们的数据中，电离参数、质量或金属丰度与消光曲线斜率之间没有明显的联系。
英文摘要
Leveraging a sample of 3457 galaxies drawn from DESI DR1 and cross-matched with archival GALEX UV photometry, we construct new dust attenuation curves and measure how the shape of these curves vary as a function of galaxy properties. Our curves are built by comparing the median flux densities of galaxies that have been divided into bins of nebular opacity, measured via the Balmer optical depth (i.e. the H$α$/H$β$ ratio). When no further cuts on galaxy properties are applied, we find an attenuation curve very similar to previous work at low redshifts. We then test how the attenuation curves vary as a function of galaxy properties; stellar mass, specific star formation rate, metallicity, and ionization parameter. We find that the curve steepens significantly at higher specific star formation rate. In our data, there is not a clear link between the ionization parameter, mass, or metallicity and the attenuation curve slope.
