挖掘NGC 6334 I（N）：大质量原恒星团的多波长成像
Digging into NGC 6334I(N): Multiwavelength Imaging of a Massive Protostellar Cluster
摘要：
我们提出了一个高分辨率，多波长的大质量原星团NGC 6334 I（N）的研究，结合新的谱线数据从亚毫米阵列（SMA）和VLA档案VLA连续数据，2 MASS和斯皮策图像的重新分析。如前所示，最亮的1.3 mm源SMA 1包含亚弧秒分辨率的子结构，我们报告了在3.6 cm处首次检测到SMA 1b以及7 mm处的新空间分量（SMA 1d）。我们发现SMA 1（源a，b，c和d的集合）和SMA 4由自由和灰尘成分组成，而SMA 6仅显示灰尘排放。我们的1.5”分辨率1.3 mm分子线图像显示了大量的热芯线发射，朝向SMA 1，并在较小程度上朝向SMA 2。我们发现CH 3OH的旋转温度为165 \pm 9 K和145 \pm 12 K的SMA 1和SMA 2，分别。我们估计SMA 1的热核辐射直径为1400 AU，包括SMA 1b和SMA 1d，并推测这些来源包括一个>800 AU的分离双星，可以解释先前提出的从SMA 1区域发出的外流进动。SMA 1、SMA 2和SMA 4的LSR速度都相差1-2 km/s。在几种分子中观察到来自SMA 1、SMA 2、SMA 4和SMA 6的流出活性，包括SiO（5- 4）和IRAC 4.5微米发射;还检测到来自SMA 4的24微米发射。探测到11个水脉泽群，其中8个与SMA 1、SMA 2、SMA 4和SMA 6相吻合。我们还发现了83个I类CH_3OH 44 GHz脉泽斑点，它们可能是由许多外流的组合活动引起的。我们的观测描绘了原星系团中多个年轻热核的肖像，在此之前，其成员在近红外线中变得可见。
英文摘要：
We present a high-resolution, multi-wavelength study of the massive protostellar cluster NGC 6334I(N) that combines new spectral line data from the Submillimeter Array (SMA) and VLA with a reanalysis of archival VLA continuum data, 2MASS and Spitzer images. As shown previously, the brightest 1.3 mm source SMA1 contains substructure at subarcsecond resolution, and we report the first detection of SMA1b at 3.6 cm along with a new spatial component at 7 mm (SMA1d). We find SMA1 (aggregate of sources a, b, c, and d) and SMA4 to be comprised of free-free and dust components, while SMA6 shows only dust emission. Our 1.5" resolution 1.3 mm molecular line images reveal substantial hot-core line emission toward SMA1 and to a lesser degree SMA2. We find CH3OH rotation temperatures of 165\pm 9 K and 145\pm 12 K for SMA1 and SMA2, respectively. We estimate a diameter of 1400 AU for the SMA1 hot core emission, encompassing both SMA1b and SMA1d, and speculate that these sources comprise a >800 AU separation binary that may explain the previously-suggested precession of the outflow emanating from the SMA1 region. The LSR velocities of SMA1, SMA2, and SMA4 all differ by 1-2 km/s. Outflow activity from SMA1, SMA2, SMA4, and SMA6 is observed in several molecules including SiO(5--4) and IRAC 4.5 micron emission; 24 micron emission from SMA4 is also detected. Eleven water maser groups are detected, eight of which coincide with SMA1, SMA2, SMA4, and SMA6. We also detect a total of 83 Class I CH3OH 44GHz maser spots which likely result from the combined activity of many outflows. Our observations paint the portrait of multiple young hot cores in a protocluster prior to the stage where its members become visible in the near-infrared.
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