PopStar：巨H{ \sc ii}区的光发射谱
PopStar Evolutionary Synthesis Models II: Optical emission-line spectra from Giant H{\sc ii} regions
摘要：
这是一系列报告PopStar进化合成模型结果的第二篇论文。在这里，我们提出了合成的H{ \sc ii}地区的年轻星团光电离的发射线光谱，为7个值的集群质量和年龄之间的0.1和5.2百万年。电离光谱能量分布（SED）是由PopStar代码\citep*{mgb09}获得的六种不同的金属丰度，具有非常低的金属丰度集，Z=0.0001，不包括在以前的类似工作。我们假设H{ \sc ii}区域的半径是电离气体在来自中心电离年轻星系团的风和超新星的机械能作用下沉积的距离。通过这种方式，电离参数作为自由参数被消除，因为现在它的值是从集群的物理性质（质量，年龄和金属丰度）和气体介质的特性（密度和丰度）。我们讨论了我们的结果，并将它们与以前的模型，也与一个大的和数据集的巨型H{ \sc ii}地区的丰度已被推导出在一个均匀的方式。在最低金属丰度星云中，[OIII]线（位于$λλ$ 4363，4959，5007 nm）的值非常弱，与来自非常高金属丰度区域（太阳或太阳上方）的值相似。因此，仅使用氧线不足以区分非常低和非常高的金属量区域。在这些情况下，我们强调需要替代金属性示踪剂的额外支持，如近\textit{IR}中的[SIII]线。
英文摘要：
This is the second paper of a series reporting the results from the PopStar evolutionary synthesis models. Here we present synthetic emission line spectra of H{\sc ii} regions photoionized by young star clusters, for seven values of cluster masses and for ages between 0.1 and 5.2 Myr. The ionizing Spectral Energy Distributions (SEDs) are those obtained by the PopStar code \citep*{mgb09} for six different metallicities, with a very low metallicity set, Z=0.0001, not included in previous similar works. We assume that the radius of the H{\sc ii} region is the distance at which the ionized gas is deposited by the action of the mechanical energy of the winds and supernovae from the central ionizing young cluster. In this way the ionization parameter is eliminated as free argument, since now its value is obtained from the cluster physical properties (mass, age and metallicity) and from the gaseous medium characteristics (density and abundances). We discuss our results and compare them with those from previous models and also with a large and data set of giant H{\sc ii} regions for which abundances have been derived in a homogeneous manner. The values of the [OIII] lines (at $λλ$ 4363, 4959, 5007Å) in the lowest metallicity nebulae are found to be very weak and similar to those coming from very high metallicity regions (solar or over-solar). Thus, the sole use of the oxygen lines is not enough to distinguish between very low and very high metallicity regions. In these cases we emphasize the need of the additional support of alternative metallicity tracers, like the [SIII] lines in the near-\textit{IR}.
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