z = 1成星半导体的精细结构FeII ~* 发射和共振MgII发射
Fine-Structure FeII* Emission and Resonant MgII Emission in z = 1 Star-Forming Galaxies
摘要：
我们提出了一个研究的患病率，强度和运动学的紫外Fe II和Mg II发射线在212恒星形成星系在z = 1从DEEP 2调查选择。我们发现FeII* 发射的复合光谱组装的基础上，不同的星系属性，表明FeII* 发射是普遍的z = 1。在这些复合材料中，Fe II * 排放观察到在大致的系统速度。在z = 1时，我们发现FeII* 发射的强度受尘埃衰减的调制最强烈，并且与红移，恒星形成率和[OII]等效宽度相关，因此具有较低尘埃水平，较低恒星形成率和较大[OII]等效宽度的较高红移的系统显示出较强的FeII* 发射。我们检测到MgII发射在至少15%的个人光谱，我们发现，对象显示较强的MgII发射具有较高的特定恒星形成率，较小的[OII]线宽，较大的[OII]等效宽度，较低的尘埃衰减，和较低的恒星质量比样品作为一个整体。MgII发射强度表现出最强的相关性与特定的恒星形成率，虽然我们发现的证据表明，尘埃衰减和恒星质量也发挥作用的MgII发射的调节。未来积分场单位观测的空间范围内的Fe II * 和Mg II发射的星系具有高的特定的恒星形成率，低的尘埃衰减，低恒星质量将是重要的探测环星系气体的形态。
英文摘要：
We present a study of the prevalence, strength, and kinematics of ultraviolet FeII and MgII emission lines in 212 star-forming galaxies at z = 1 selected from the DEEP2 survey. We find FeII* emission in composite spectra assembled on the basis of different galaxy properties, indicating that FeII* emission is prevalent at z = 1. In these composites, FeII* emission is observed at roughly the systemic velocity. At z = 1, we find that the strength of FeII* emission is most strongly modulated by dust attenuation, and is additionally correlated with redshift, star-formation rate, and [OII] equivalent width, such that systems at higher redshifts with lower dust levels, lower star-formation rates, and larger [OII] equivalent widths show stronger FeII* emission. We detect MgII emission in at least 15% of the individual spectra and we find that objects showing stronger MgII emission have higher specific star-formation rates, smaller [OII] linewidths, larger [OII] equivalent widths, lower dust attenuations, and lower stellar masses than the sample as a whole. MgII emission strength exhibits the strongest correlation with specific star-formation rate, although we find evidence that dust attenuation and stellar mass also play roles in the regulation of MgII emission. Future integral field unit observations of the spatial extent of FeII* and MgII emission in galaxies with high specific star-formation rates, low dust attenuations, and low stellar masses will be important for probing the morphology of circumgalactic gas.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
