CARMA OBSERVATIONS OF PROTOSTELLAR OUTFLOWS IN NGC 1333
CARMA OBSERVATIONS OF PROTOSTELLAR OUTFLOWS IN NGC 1333
复制标题
DOI：
10.1088/0004-637x/774/1/22
复制
发表时间：
2013-07
期刊：
影响因子：
--
通讯作者：
A. Plunkett;H. Arce;S. Corder;D. Mardones;A. Sargent;S. Schnee
中科院分区：
文献类型：
--
作者：
A. Plunkett;H. Arce;S. Corder;D. Mardones;A. Sargent;S. Schnee
我们目前的观测流出的恒星形成区域NGC 1333使用组合阵列研究毫米波天文学（CARMA）。我们将12 CO和13 CO（1-0）CARMA镶嵌图与14米五学院射电天文台的数据相结合，以5“到7”（或1000 Au到0.5 pc，距离235 pc）的尺度探测这个原恒星团的中心，最密集和活跃的区域。我们绘制并识别12 CO流出，并沿着13 CO数据，我们估计它们的质量，动量和能量。在7′ × 7′的地图中，5″的分辨率允许对流出和流出候选者的形态和运动学进行详细研究，其中一些以前与该地区的其他流出排放相混淆。总的来说，我们确定了22个外流叶，以及9个密集的拱星信封标记的连续发射，其中6个驱动外流。我们计算出的总流出质量、动量和能量分别位于6 M重力、19 M重力km s−1和7 × 1044 erg的映射区域内。在同一区域内，我们比较外流运动学与湍流和重力能，我们认为，外流可能是重要的代理人在这一地区的湍流的维护。在星星形成的最早阶段，外流还没有提供足够的能量来完全破坏大多数星星形成的聚集区，但随着原恒星源的演变，外流有可能这样做。我们的研究结果可以用来限制外流特性，如外流强度，在数值模拟中的外流驱动的湍流团簇。
We present observations of outflows in the star-forming region NGC 1333 using the Combined Array for Research in Millimeter-Wave Astronomy (CARMA). We combined the 12CO and 13CO (1–0) CARMA mosaics with data from the 14 m Five College Radio Astronomy Observatory to probe the central, most dense, and active region of this protostellar cluster at scales from 5″ to 7′ (or 1000 AU to 0.5 pc at a distance of 235 pc). We map and identify 12CO outflows, and along with 13CO data we estimate their mass, momentum, and energy. Within the 7′ × 7′ map, the 5″ resolution allows for a detailed study of morphology and kinematics of outflows and outflow candidates, some of which were previously confused with other outflow emission in the region. In total, we identify 22 outflow lobes, as well as 9 dense circumstellar envelopes marked by continuum emission, of which 6 drive outflows. We calculate a total outflow mass, momentum, and energy within the mapped region of 6 M☉, 19 M☉ km s−1, and 7 × 1044 erg, respectively. Within this same region, we compare outflow kinematics with turbulence and gravitational energy, and we suggest that outflows are likely important agents for the maintenance of turbulence in this region. In the earliest stages of star formation, outflows do not yet contribute enough energy to totally disrupt the clustered region where most star formation is happening, but have the potential to do so as the protostellar sources evolve. Our results can be used to constrain outflow properties, such as outflow strength, in numerical simulations of outflow-driven turbulence in clusters.