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首页> 外文期刊>The Astrophysical journal >THE CO MOLECULAR OUTFLOWS OF IRAS 16293-2422 PROBED BY THE SUBMILLIMETER ARRAY
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THE CO MOLECULAR OUTFLOWS OF IRAS 16293-2422 PROBED BY THE SUBMILLIMETER ARRAY

机译：次幂阵列引起的IRAS 16293-2422的CO分子流出

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摘要

We have mapped the protobinary source IRAS 16293-2422 in CO 2-1, ~(13)CO 2-1, and CO 3-2 with the Sub-millimeter Array (SMA). The maps with resolution of 1.5"-5" reveal a single small-scale (～3000 AU) bipolar molecular outflow along the east-west direction. We found that the blueshifted emission of this small-scale outflow mainly extends to the east and the redshifted emission to the west from the position of IRAS 16293 A. A comparison with the morphology of the large-scale outflows previously observed by single-dish telescopes at millimeter wavelengths suggests that the small-scale outflow may be the inner part of the large-scale (～ 15,000 AU) east-west outflow. On the other hand, there is no clear counterpart of the large-scale northeast-southwest outflow in our SMA maps. Comparing analytical models to the data suggests that the morphology and kinematics of the small-scale outflow can be explained by a wide-angle wind with an inclination angle of ～30°-40° with respect to the plane of the sky. The high-resolution CO maps show that there are two compact, bright spots in the blueshifted velocity range. An LVG analysis shows that the one located 1" to the east of source A is extremely dense, n(H_2) ～ 10~7 cm~(-3), and warm, T_(kin) ＞ 55 K. The other one located 1" southeast of source B has a higher temperature of T_(kin) ＞ 65 K but slightly lower density of n(H_2) ～ 10~ 6 cm~(-3). It is likely that these bright spots are associated with the hot core-like emission observed toward IRAS 16293. Since both bright spots are blueshifted from the systemic velocity and are offset from the protostellar positions, they are likely formed by shocks.
机译：我们已经用亚毫米波阵列（SMA）映射了CO 2-1，〜（13）CO 2-1和CO 3-2中的原始二进制源IRAS 16293-2422。分辨率为1.5“ -5”的图谱揭示了沿东西方向的单个小规模（〜3000 AU）双极分子流出。我们发现，这种小规模流出物的蓝移发射主要从IRAS 16293 A的位置延伸到东部，而红移发射则向西延伸。与以前用单碟望远镜观测到的大规模流出的形态进行了比较在毫米波长处，表明小规模的流出可能是大规模（〜15,000 AU）东西向流出的内部。另一方面，在我们的SMA地图中，没有大规模的东西向西南流出的明显对应物。将分析模型与数据进行比较表明，小规模流出的形态和运动学可以由相对于天空平面的倾斜角度为〜30°-40°的广角风来解释。高分辨率CO图显示，在蓝移速度范围内有两个紧凑的亮点。 LVG分析显示，位于源A东部1“处的一个非常密，n（H_2）〜10〜7 cm〜（-3），并且温暖，T_（kin）＞ 55K。另一个位于源B东南1“处的T_（kin）＞ 65 K较高，但n（H_2）〜10〜6 cm〜（-3）的密度稍低。这些亮点很可能与朝IRAS 16293观测到的热核样发射有关。由于两个亮点都偏离了系统速度，并且偏离了原恒星的位置，因此很可能是由于撞击而形成的。

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