潜在原双星系统NGC 2264 CMM3中分子发射线丰度显著差异的发现
Discovery of Striking Difference of Molecular-Emission-Line Richness in the Potential Proto-Binary System NGC 2264 CMM3
摘要：
利用ALMA对年轻的大质量原恒星候选者NGC2264CMM3进行了0.8mm波段的干涉谱线测量。CMM3被分解为两个连续峰CMM3A和CMM3B，角间距为0.9”。因此，CMM3被认为是一个二元系统的候选者。我们已经检测到与CMM3A和CMM3B相关的分子外流，表明活跃的恒星形成。在CMM3A和CMM3B周围还发现了6个微弱的连续谱峰，其中大部分被认为是演化的低质量原恒星。发现CMM3A富含分子线发射，包括复杂的有机分子，如HCOOCH 3和CH 3OCH 3。复杂有机分子的发射分布在CMM3A连续峰周围的紧凑区域内。因此，CMM3A显然拥有一个热核心。另一方面，CMM3B是缺乏分子线发射，虽然它的连续通量几乎是可比的CMM3A。讨论了CMM3A和CMM3B之间显著差异的可能原因。
英文摘要：
We have conducted an interferometric line survey in the 0.8 mm band toward the young high-mass protostar candidate NGC 2264 CMM3 with ALMA. CMM3 is resolved into the two continuum peaks, CMM3A and CMM3B, at an angular separation of 0.9". Thus, CMM3 is found to be a binary system candidate. We have detected molecular outflows associated with CMM3A and CMM3B each, indicating active star formation. In addition to the two peaks, six faint continuum peaks are detected around CMM3A and CMM3B, most of which are thought to be evolved low-mass protostars. CMM3A is found to be rich in molecular line emission including complex organic molecules such as HCOOCH3 and CH3OCH3. The emission of complex organic molecules is distributed within a compact region around the continuum peak of CMM3A. Hence, CMM3A apparently harbors a hot core. On the other hand, CMM3B is deficient in molecular line emission, although its continuum flux is almost comparable to that of CMM3A. Possible origins of the striking difference between CMM3A and CMM3B are discussed.
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