标题： 深入研究NGC 6334I(N)： massive原恒星团的多波段成像 显示英文标题

标题： Digging into NGC 6334I(N): Multiwavelength Imaging of a Massive Protostellar Cluster

摘要： 我们呈现了对大质量原恒星团NGC 6334I(N)的高分辨率、多波段研究，该研究结合了来自亚毫米波阵列（SMA）和甚大天线阵（VLA）的新光谱线数据，以及对存档VLA连续波数据、2MASS和斯皮策图像的重新分析。 正如先前所展示的，最亮的1.3毫米源SMA1在亚角秒分辨率下包含子结构，并且我们报告了首次在3.6厘米波长上探测到SMA1b以及在7毫米波长上的新空间成分SMA1d。 我们发现SMA1（a、b、c和d源的聚合体）和SMA4由自由-自由辐射和尘埃成分组成，而SMA6仅显示出尘埃发射。 我们的1.5弧秒分辨率1.3毫米分子线图像揭示了SMA1和在较小程度上的SMA2附近存在大量的热核线发射。 我们分别测得SMA1和SMA2的CH3OH旋转温度为165\pm 9 K和145\pm 12 K。 我们估计SMA1热核发射的直径为1400天文单位，包括SMA1b和SMA1d，推测这些源可能构成一个大于800天文单位分离的双星系统，这或许可以解释之前建议的来自SMA1区域外流的进动现象。 SMA1、SMA2和SMA4的局部标准速度（LSR）速度相差1-2公里/秒。 观测到SMA1、SMA2、SMA4和SMA6在多个分子中的外流活动，包括SiO(5--4)和IRAC 4.5微米发射；还检测到了SMA4的24微米发射。 检测到11组水脉泽，其中8组与SMA1、SMA2、SMA4和SMA6重合。 我们还检测到总计83个Class I CH3OH 44 GHz脉泽点，这些点可能是许多外流共同活动的结果。 我们的观测描绘了在成员在近红外波段变得可见之前的原星团中多个年轻的热核的图景。 显示英文摘要

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.