高磁膨胀G矮星MOA-2006-BLG-099S的高分辨光谱
A High-Resolution Spectrum of the Highly Magnified Bulge G-Dwarf MOA-2006-BLG-099S
摘要：
我们分析了一个高分辨率的光谱微透镜G-矮星在银河系的隆起，收购时，恒星被放大了110倍。我们测量的光谱温度，来自翅膀的巴耳末线，这是相同的光度温度，来自使用标准微透镜技术确定的颜色。我们测得[Fe/H]=0.36 +/-0.18，这使这颗恒星位于膨胀巨星金属丰度分布的上端。特别是，这颗恒星比任何具有高分辨率丰度的核球M巨星都更富含金属。我们发现，α和铁峰元素的丰度比与具有相同金属丰度的膨胀巨星相似。我们首次测量了一颗恒星的K和Zn丰度。[K/Mg]比值与在晕和盘中测得的值相似，表明K的产生密切跟踪α的产生。[Cu/Fe]和[Zn/Fe]比值支持了这些元素是在II型SNe中产生的理论，而不是Ia型SNe。我们还测量了第一个C和N丰度的凸起，没有受到影响的第一次疏浚。[C/Fe]和[N/Fe]的比值接近太阳，与巨星只经历正则混合的假设一致。
英文摘要：
We analyze a high-resolution spectrum of a microlensed G-dwarf in the Galactic bulge, acquired when the star was magnified by a factor of 110. We measure a spectroscopic temperature, derived from the wings of the Balmer lines, that is the same as the photometric temperature, derived using the color determined by standard microlensing techniques. We measure [Fe/H]=0.36 +/-0.18, which places this star at the upper end of the Bulge giant metallicity distribution. In particular, this star is more metal-rich than any bulge M giant with high-resolution abundances. We find that the abundance ratios of alpha and iron-peak elements are similar to those of Bulge giants with the same metallicity. For the first time, we measure the abundances of K and Zn for a star in the Bulge. The [K/Mg] ratio is similar to the value measured in the halo and the disk, suggesting that K production closely tracks alpha production. The [Cu/Fe] and [Zn/Fe] ratios support the theory that those elements are produced in Type II SNe, rather than Type Ia SNe. We also measured the first C and N abundances in the Bulge that have not been affected by first dredge-up. The [C/Fe] and [N/Fe] ratios are close to solar, in agreement with the hypothesis that giants experience only canonical mixing.
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