HOPS中的脉泽源寻找方法
Maser Source Finding Methods in HOPS
摘要：
{ \bf H} $_2$ { \bf O}南银河{ \bf P}道{ \bf S}巡天（HOPS）观测了100平方度的银河平面，使用Mopra射电望远镜搜索12毫米波段（19.5 GHz）多条谱线的发射。其中最重要的谱线可能是22.2GHz的水脉泽跃迁。我们描述的方法来识别水脉泽候选人和随后的确认来源。我们的方法涉及一个简单的确定可能的候选人通过搜索峰值发射图，利用水脉泽发射的内在性质-空间未分辨和光谱窄线。我们估计完整性限制，并将我们的方法与{ \sc Duchamp}源查找器的结果进行比较。我们发现，这两种方法执行类似。我们的结论是，性能的相似性是由于数据的噪声特性的内在限制。我们的方法的优点是，它是稍微更有效地消除虚假检测，是简单的实现。缺点是它是一种手动查找源的方法，因此对于比HOPS大得多的数据集或需要表征的扩展发射数据集不实用。我们概述了一个两阶段的方法，最有效的手段发现脉泽，使用{ \sc杜尚}。
英文摘要：
The {\bf H}$_2${\bf O} Southern Galactic {\bf P}lane {\bf S}urvey (HOPS) has observed 100 square degrees of the Galactic plane, using the Mopra radio telescope to search for emission from multiple spectral lines in the 12\,mm band (19.5\,--\,27.5\,GHz). Perhaps the most important of these spectral lines is the 22.2\,GHz water maser transition. We describe the methods used to identify water maser candidates and subsequent confirmation of the sources. Our methods involve a simple determination of likely candidates by searching peak emission maps, utilising the intrinsic nature of water maser emission - spatially unresolved and spectrally narrow-lined. We estimate completeness limits and compare our method with results from the {\sc Duchamp} source finder. We find that the two methods perform similarly. We conclude that the similarity in performance is due to the intrinsic limitation of the noise characteristics of the data. The advantages of our method are that it is slightly more efficient in eliminating spurious detections and is simple to implement. The disadvantage is that it is a manual method of finding sources and so is not practical on datasets much larger than HOPS, or for datasets with extended emission that needs to be characterised. We outline a two-stage method for the most efficient means of finding masers, using {\sc Duchamp}.
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