arXiv 1805.045222018-05-11astro-ph.GA

银河系隆起和盘中的SiO脉泽：来自BAaDE巡天的动力学

SiO Masers in the Galactic Bulge and Disk: Kinematics from the BAaDE Survey

A. C. Trapp, R. M. Rich, M. R. Morris, L. O. Sjouwerman, Y. M. Pihlstrom, M. Claussen, M. C. Stroh

备注：: 18 pages, 17 Figures; Submitted to ApJ (Accepted May 7)
DOI：: 10.3847/1538-4357/aac382

摘要：

我们目前的第一个结果从BAaDE（膨胀不对称性和动态演化）调查。虽然只是一个完整的调查（$\sim$ 2700出$\sim$ 20000最终来源）的子集，我们的数据包括最大的无线电运动学调查迄今为止的恒星SiO脉泽观测到的银河系的隆起和平面从$-15^\circ < l < +12^\circ$和$-6^\circ < b < +6^\circ$。我们的资料来源包括银河平面内$\pm 1^\circ$高消光区的大量视线（LoS）速度。当与2 MASS测光相匹配时，我们的无线电探测样品明显比第一个红巨星分支尖端更亮，更红，达到了$(J-Ks)_0 > 8$的极端，颜色与Mira变量和质量损失的AGB星一致。我们看到一个干净的划分成两个运动学人口：一个运动学冷（$σ\sim 50\rm\ km\ sec^{-1}$）人口，我们建议是在前景盘，包括巨人与2质量$Ks<5.5$，和运动学热（$σ\sim 100\rm\ km\ sec^{-1}$）候选人隆起/酒吧人口的大多数巨人与$Ks>5.5$。只有运动学上的热巨星与$Ks>5.5$包括最红的恒星。采用8.3千秒差距的银河系中心，并校正前景消光，我们发现，大多数的来源有$M_{bol} \sim -5$，符合他们是明亮的，可能是中间年龄，AGB星。我们注意到一些紧张局势之间的可能中间年龄的运动学热人口，其高速分散相比，磁盘。

英文摘要：

We present the first results from the BAaDE (Bulge Asymmetries and Dynamic Evolution) survey. Though only a subset of the complete survey ($\sim$2700 out of $\sim$20000 final sources), our data comprise the largest radio kinematic survey to date of stellar SiO masers observed toward the Galactic bulge and plane from $-15^\circ < l < +12^\circ$ and $-6^\circ < b < +6^\circ$. Our sources include a substantial number of line-of-sight (LoS) velocities in high extinction regions within $\pm 1^\circ$ of the Galactic plane. When matched with 2MASS photometry, our radio-detected sample lies significantly brighter than and red-ward of the first red giant branch tip, reaching extremes of $(J-Ks)_0 > 8$, colors consistent with Mira variables and mass losing AGB stars. We see a clean division into two kinematic populations: a kinematically cold ($σ\sim 50\rm\ km\ sec^{-1}$) population that we propose is in the foreground disk, consisting of giants with 2MASS $Ks<5.5$, and a kinematically hot ($σ\sim 100\rm\ km\ sec^{-1}$) candidate bulge/bar population for most giants with $Ks>5.5$. Only the kinematically hot giants with $Ks>5.5$ include the reddest stars. Adopting 8.3 kpc to the Galactic Center, and correcting for foreground extinction, we find that most of the sources have $M_{bol} \sim -5$, consistent with their being luminous, and possibly intermediate age, AGB stars. We note some tension between the possibly intermediate age of the kinematically hot population, and its high velocity dispersion compared to the disk.

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英文摘要：

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