A GMRT survey of regions towards the Taurus molecular cloud at 323 and 608 MHz
A GMRT survey of regions towards the Taurus molecular cloud at 323 and 608 MHz
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在 323 和 608 MHz 下对金牛座分子云区域进行 GMRT 勘测
DOI：
10.1093/mnras/stw1847
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发表时间：
2016
影响因子：
4.8
通讯作者：
Ainsworth R
中科院分区：
文献类型：
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作者：
Ainsworth R
我们目前的观测三个活跃的网站的星星形成的金牛座分子云复杂的在323和608兆赫（90和50厘米，分别）与巨型米波射电望远镜（GMRT）。作为探路者项目的一部分，观测到了三个指向，目标是年轻恒星物体（YSO）L1551 IRS 5，T Tau和DG Tau（这些目标源的结果在以前的论文中介绍）。在本文中，我们寻找其他YSO，并提出了一个调查，包括所有三个领域的副产品的大瞬时视野的GMRT。测量的分辨率为10 arcsec量级，每个指向中心的最佳均方根噪声在323 MHz时为100 μJy波束− 1量级，在608 MHz时为50 μJy波束− 1量级。我们提出了一个目录，1815和687场源检测以上5σrmsat 323和608兆赫分别。在这两个频率下共检测到440个源，对应于2062个源的总唯一源计数。我们比较结果与以前的调查，并展示了一个样本的扩展河外天体。虽然没有进一步的YSO检测到除了目标YSO根据我们的源查找标准，这些数据可以用于有针对性的手动搜索，射电星系的研究或协助校准未来的观测与低频阵列对这些地区。
We present observations of three active sites of star formation in the Taurus molecular cloud complex taken at 323 and 608 MHz (90 and 50 cm, respectively) with the Giant Metrewave Radio Telescope (GMRT). Three pointings were observed as part of a pathfinder project, targeted at the young stellar objects (YSOs) L1551 IRS 5, T Tau and DG Tau (the results for these target sources were presented in a previous paper). In this paper, we search for other YSOs and present a survey comprising of all three fields; a by-product of the large instantaneous field of view of the GMRT. The resolution of the survey is of order 10 arcsec and the best rms noise at the centre of each pointing is of order 100 μJy beam−1at 323 MHz and 50 μJy beam−1at 608 MHz. We present a catalogue of 1815 and 687 field sources detected above 5σrmsat 323 and 608 MHz, respectively. A total of 440 sources were detected at both frequencies, corresponding to a total unique source count of 2062 sources. We compare the results with previous surveys and showcase a sample of extended extragalactic objects. Although no further YSOs were detected in addition to the target YSOs based on our source-finding criteria, these data can be useful for targeted manual searches, studies of radio galaxies or to assist in the calibration of future observations with the Low-Frequency Array towards these regions.