The Molecular Cloud Ring in NGC 1068
The Molecular Cloud Ring in NGC 1068
复制标题
NGC 1068 中的分子云环
DOI：
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发表时间：
1987
期刊：
影响因子：
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通讯作者：
N. Scoville
中科院分区：
文献类型：
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作者：
S. Myers;N. Scoville
利用Owens Valley毫米波干涉仪以6角秒的分辨率（500 pc）对NGC 1068的核CO辐射进行了测图。大约50%的中央6千秒差距内的总CO排放包含在一个环（或臂）在R = 0.9 - 2.4千秒差距附近的外缘的内盘，在那里的红外观测表明，大质量星星的形成率高。CO的运动学表明，平均圆周和膨胀速度分别为164和71公里/秒，为环假设主轴位置角为55度。(For长轴PA = 82度，圆周速度为185 km/s，膨胀速度小于20 km/s。这个区域内分子云的质量大约是4 × 10的太阳质量的9次方。有人提出，这个环是由一个中央恒星棒的作用所收集的气体形成的;这种气体的流入可能是由与另一个星系的近距离合并所触发的。33篇参考文献。
The Owens Valley Millimeter Interferometer has been used to map the CO emission in the nucleus of NGC 1068 at 6-arcsec resolution (500 pc). Approximately 50 percent of the total CO emission within the central 6 kpc is contained in a ring (or arms) at R = 0.9 - 2.4 kpc near the outer edge of the inner disk, where IR observations have shown a high rate of massive star formation. The CO kinematics indicate mean circular and expansion velocities of 164 and 71 km/s, respectively for the ring assuming a major axis position angle of 55 deg. (For a major axis PA = 82 deg, the circular velocity is 185 km/s and the expansion velocity is less than 20 km/s.) The mass of molecular clouds within this region is approximately 4 x 10 to the 9th solar mass. It is proposed that the ring has formed of gas collected by the action of a central stellar bar; the infall of this gas may have been triggered by a close encounter of merger with another galaxy. 33 references.