arXiv 1402.13352014-02-06astro-ph.GA

人马座C区的高速致密云

High Velocity Compact Clouds in the Sagittarius C Region

Kunihiko Tanaka, Tomoharu Oka, Shinji Matsumura, Makoto Nagai, Kazuhisa Kamegai

备注：: 23 pages, 8 figures, accepted for publication in Astrophysical Journal
DOI：: 10.1088/0004-637X/783/1/62

摘要：

我们报告了银河系中央分子带的两个分子团的极宽发射的检测。我们绘制了人马座C复合体的地图（$-0^\circ.61 < l < -0^\circ.27$，$-0^\circ.29 < b < 0^\circ.04$）在HCN $J$ = 4- 3，$\mathrm{^{13}CO}$ $J$ = 3- 2，$\mathrm{H^{13}CN}$ $J$ = 1- 0线上使用ASTE 10 m和NRO 45 m望远镜，使用$80\mbox{--}120$ \ $\mathrm{km\,s^{-1}}$速度宽度探测明亮发射（在零强度下的全宽）朝向CO $-0.30$ $-0.07$和CO $-0.40$ $-0.22$，这是我们以前的CO $J$ = 3- 2调查确定的高速致密云（HVCC）。我们的数据揭示了一个有趣的内部结构的CO $-0.30$ $-0.07$包括一对高速叶。CO $-0.40$ $-0.22$的空间速度结构也可以理解为多个速度分量，或者是穿过云的速度梯度。它们都位于两个半径约为10 pc的分子壳层的边缘。CO $-0.30$ $-0.07$和CO $-0.40$ $-0.22$的动能分别为$\left(0.8\mbox{--}2\right)\times10^{49}$ erg和$\left(1\mbox{--}4\right)\times10^{49}$ erg。我们提出了几种解释，他们广泛的发射：与壳，双极外流，超新星（SNe）驱动的膨胀，并围绕一个黑暗的大质量物体的云之间的碰撞。由于我们的数据的角度分辨率不足，这些场景无法区分，尽管没有与HVCCs相关的可见能源似乎有利于云-云碰撞场景。这两个分子壳层的动能分别为$1\times10^{51}$ erg和$0.7\times10^{51}$ erg，它们可以由$2\times10^5$ yr内的多次超新星或超新星爆炸提供。这些壳层是过去活跃恒星形成后产生的分子超级气泡的候选者。

英文摘要：

We report the detection of extremely broad emission toward two molecular clumps in the Galactic central molecular zone. We have mapped the Sagittarius C complex ($-0^\circ.61 < l < -0^\circ.27$, $-0^\circ.29 < b < 0^\circ.04$) in the HCN $J$ = 4--3, $\mathrm{^{13}CO}$ $J$ = 3--2, and $\mathrm{H^{13}CN}$ $J$ = 1--0 lines with the ASTE 10 m and NRO 45 m telescopes, detecting bright emission with $80\mbox{--}120$\ $\mathrm{km\,s^{-1}}$ velocity width (in full-width at zero intensity) toward CO$-0.30$$-0.07$ and CO$-0.40$$-0.22$, which are high velocity compact clouds (HVCCs) identified with our previous CO $J$ = 3--2 survey. Our data reveal an interesting internal structure of CO$-0.30$$-0.07$ comprising a pair of high velocity lobes. The spatial-velocity structure of CO$-0.40$$-0.22$ can be also understood as multiple velocity component, or a velocity gradient across the cloud. They are both located on the rims of two molecular shells of about 10 pc in radius. Kinetic energies of CO$-0.30$$-0.07$ and CO$-0.40$$-0.22$ are $\left(0.8\mbox{--}2\right)\times10^{49}$ erg and $\left(1\mbox{--}4\right)\times10^{49}$ erg, respectively. We propose several interpretations of their broad emission: collision between clouds associated with the shells, bipolar outflow, expansion driven by supernovae (SNe), and rotation around a dark massive object. There scenarios cannot be discriminated because of the insufficient angular resolution of our data, though the absence of visible energy sources associated with the HVCCs seems to favor the cloud--cloud collision scenario. Kinetic energies of the two molecular shells are $1\times10^{51}$ erg and $0.7\times10^{51}$ erg, which can be furnished by multiple SN or hypernova explosions in $2\times10^5$ yr. These shells are candidates of molecular superbubbles created after past active star formation.

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英文摘要：

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