星系的分子气体性质：SMA CO（2-1）B0DEGA遗留项目
Molecular gas properties of galaxies: The SMA CO(2-1) B0DEGA legacy project
摘要：
在过去的二十年中，对大约150个星系的高分辨率（< 5角秒）CO观测提供了大量关于环核区域分子气体形态的信息。虽然在“正常”星系的样本中，大约50%的星系的分子气体似乎并没有朝着核区域达到峰值，但棒星系和合并星系显示出更大的浓度。然而，从观测的角度来看，我们并不确切地知道星系的分子气体性质是如何由于相互作用而演变的。在这里，我们提出了SMA CO（2-1）B 0 DEGA（低于0度星系）的遗留项目，在该项目中，我们正在对附近红外明亮的螺旋星系的大样本（~ 70）的环核区域（1弧分）的CO（2-1）线进行成像，可能相互作用，并且由于其位于南半球，仍然未被探索。我们发现不同的分子气体形态，如环，核臂，核棒和不对称。我们发现一个中心峰值浓度约85%的星系的典型尺寸尺度约0.5 - 1千秒差距。这可能与最近的相互作用产生的扰动有关。
英文摘要：
In the last two decades high resolution (< 5 arcsec) CO observations for ~ 150 galaxies have provided a wealth of information about the molecular gas morphologies in the circumnuclear regions. While in samples of 'normal' galaxies the molecular gas does not seem to peak toward the nuclear regions for about 50% of the galaxies, barred galaxies and mergers show larger concentrations. However, we do not exactly know from an observational point of view how the molecular gas properties of a galaxy evolve as a result of an interaction. Here we present the SMA CO(2-1) B0DEGA (Below 0 DEgree GAlaxies) legacy project in which we are imaging the CO(2-1) line of the circumnuclear regions (1 arcmin) of a large (~ 70) sample of nearby IR-bright spiral galaxies, likely interacting, and that still remained unexplored due to its location in the southern hemisphere. We find different molecular gas morphologies, such as rings, nuclear arms, nuclear bars and asymmetries. We find a centrally peaked concentration in about 85% of the galaxies with typical size scales of about 0.5 - 1 kpc. This might be related to perturbations produced by recent interactions.
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