在Lynx-Cancer虚空中的星系研究。II。元素丰度
Study of galaxies in the Lynx-Cancer void. II. The element abundances
摘要：
在研究Lynx-Cancer空区星系演化状况的框架下，我们给出了SAO RAS 6-m望远镜对该区域20个天体的光谱观测结果。用经典方法测定电子温度和氧丰度（O/H）的主暗线[OIII] 4363 A只在约2/3的研究对象中被清楚地探测到。对于其余的星系来说，这条线要么很微弱，要么没有被探测到。为了获得这些星系中的氧丰度，我们也应用了Izotov和Thuan的半经验方法，和/或Pilyugin等人的经验方法，其仅采用足够强的线的强度。我们还提出了我们的O/H测量22 Lynx-Cancer空星系，其中合适的斯隆数字巡天（SDSS）光谱可用。总之，我们提出了合并的O/H数据的48 Lynx-Cancer空星系，包括从文献中采用的数据和我们自己的早期结果。并将它们在（O/H）-M_B图上的位置与环境较致密区域的本体积矮星系的位置进行了比较。我们推断，大多数来自这个空洞的星系平均显示出约30%的金属丰度低。此外，相当一部分（不少于10%）的空矮星系有更大的O/H不足（高达5倍）。其中大多数属于气体金属丰度Z < Zo/20或12+log（O/H）<~7.35的小天体组。在这一天区中，非常贫金属的星系（Z < Zo/10）的面密度比Hamburg-SAO和SDSS巡天的发射线星系样品的面密度高2- 2.5倍。我们讨论了这些结果对星系演化模型的可能影响。
英文摘要：
In the framework of the study of the evolutionary status of galaxies in the nearby Lynx-Cancer void, we present the results of the SAO RAS 6-m telescope spectroscopy for 20 objects in this region. The principal faint line [OIII]4363A, used to determine the electron temperature and oxygen abundance (O/H) by the classical method, is clearly detected in only about 2/3 of the studied objects. For the remaining galaxies this line is either faint or undetected. To obtain the oxygen abundances in these galaxies we as well apply the semi-empirical method by Izotov and Thuan, and/or the empirical methods of Pilyugin et al., which are only employing the intensities of sufficiently strong lines. We also present our O/H measurements for 22 Lynx-Cancer void galaxies, for which the suitable Sloan Digital Sky Survey (SDSS) spectra are available. In total, we present the combined O/H data for 48 Lynx-Cancer void galaxies, including the data adopted from the literature and our own earlier results. We make a comparison of their locations on the (O/H)-M_B diagram with those of the dwarf galaxies of the Local Volume in the regions with denser environment. We infer that the majority of galaxies from this void on the average reveal an about 30% lower metallicity. In addition, a substantial fraction (not less than 10%) of the void dwarf galaxies have a much larger O/H deficiency (up to a factor of 5). Most of them belong to the tiny group of objects with the gas metallicity Z < Zo/20 or 12+log(O/H) <~7.35. The surface density of very metal-poor galaxies (Z < Zo/10} in this region of the sky is 2--2.5 times higher than that, derived from the emission-line galaxy samples in the Hamburg-SAO and the SDSS surveys. We discuss possible implications of these results for the galaxy evolution models.
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