WHIQII调查：发光致密蓝镓的金属丰度和光谱性质
The WHIQII Survey: Metallicities and Spectroscopic Properties of Luminous Compact Blue Galaxies
摘要：
作为WIYN High Image Quality Indiana Irvine（WHIQII）巡天的一部分，我们展示了123个发射线星系的光谱，这些光谱是从中等红移（.4<z<.8）星系中选出的，这些星系具有蓝色，物理上看起来很紧凑。该样品包括15个真正的发光紧凑型蓝色玻璃（LCBG）和另外27个稍微不那么极端的发射线系统。这些星系代表了一个高度演化的类别，可能在z~1以来恒星形成的衰退中发挥重要作用，但它们的确切性质和演化路径仍然是一个谜。在这里，我们使用发射线来确定金属丰度和电离参数，限制它们的内在属性和恒星形成状态。一些LCBG金属丰度与“爆发矮”的情况是一致的，而其他人的很大一部分不是，进一步证实了LCBG是一个高度异质性的人口，但广泛地与中间红移场一致。与以前的研究一致，我们观察到在中间红移的光度-金属丰度关系的整体演变。我们的样本，特别是LCBG，占据了经验R23-O32平面中的一个区域，该区域不同于发光的本地星系，并且与当前时代的矮不规则星更加一致，这表明即使在描述恒星形成的最基本参数中也可以观察到宇宙“缩小”。我们样本的这些性质也与位于本地星系和高红移星系之间的情况基本一致，正如这种情况所预期的那样。令人惊讶的是，我们的样本在致密性和金属丰度之间没有表现出可检测到的相关性，这强烈表明在这些快速恒星形成的时期，致密恒星形成星系的形态在很大程度上是短暂的。
英文摘要：
As part of the WIYN High Image Quality Indiana Irvine (WHIQII) survey, we present 123 spectra of emission-line galaxies, selected on intermediate redshift (.4<z<.8) galaxies with blue colors that appear physically compact. The sample includes 15 true Luminous Compact Blue Galaxies (LCBGs) and an additional 27 slightly less extreme emission-line systems. These galaxies represent a highly evolving class that may play an important role in the decline of star formation since z~1, but their exact nature and evolutionary pathways remain a mystery. Here, we use emission lines to determine metallicities and ionization parameters, constraining their intrinsic properties and state of star formation. Some LCBG metallicities are consistent with a "bursting dwarf" scenario, while a substantial fraction of others are not, further confirming that LCBGs are a highly heterogeneous population but are broadly consistent with the intermediate redshift field. In agreement with previous studies, we observe overall evolution in the luminosity-metallicity relation at intermediate redshift. Our sample, and particularly the LCBGs, occupy a region in the empirical R23-O32 plane that differs from luminous local galaxies and is more consistent with dwarf Irregulars at the present epoch, suggesting that cosmic "downsizing" is observable in even the most fundamental parameters that describe star formation. These properties for our sample are also generally consistent with lying between local galaxies and those at high redshift, as expected by this scenario. Surprisingly, our sample exhibits no detectable correlation between compactness and metallicity, strongly suggesting that at these epochs of rapid star formation, the morphology of compact star-forming galaxies is largely transient.
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