On numbers and games, Second Edition
On numbers and games, Second Edition
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关于数字和游戏，第二版
DOI：
10.1051/0004-6361/202038259
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发表时间：
2001
影响因子：
6.5
通讯作者：
J. Conway
中科院分区：
文献类型：
--
作者：
J. Conway
猎户座分子云是最接近大质量星星形成的区域。这是一个理想的目标，调查的详细结构的大质量恒星形成的高分辨率和相关的灯丝范例的最早阶段的中间到高质量的星星formation.AimsWithin猎户座A分子云，积分形灯丝（ISF）是一个突出的，度长的结构致密气体和尘埃的最近和正在进行的高质量星星形成的明显迹象。我们的目标是在中等高的角分辨率下，（8 "或~0.016 pc），以测量主灯丝的固有宽度，降至远低于0.1 pc的尺度，这已被确定为灯丝的特征宽度。OMC-2和OMC-3，350和450 μm。我们结合这些数据与Herschel-SPIRE地图恢复扩展发射。Herschel-ArTéMiS组合图提供了致密冷物质分布的详细信息，具有高空间动态范围，从我们的8 "分辨率到图的横向角大小，约10-15“。通过结合Herscheland ArTéMiS在160、250、350和450 μm的数据，我们构建了高分辨率的温度和H2柱密度图。我们从ISF的几个代表性部分的柱密度图中提取径向强度分布，我们用高斯和普卢默模型拟合以获得其固有宽度。我们还比较了由ArTéMiS跟踪的材料的分布，在较高密度的示踪剂N2 H+（1-0），最近观察到的阿尔马interferometer.ResultsAll的径向配置文件，我们提取的显示出明显的偏离高斯，与证据的内部高原，以前没有看到清楚usingHerschel唯一的数据。我们测量的固有半功率宽度在0.06-0.11 pc的范围内。这明显大于在N2 H+中观察到的纤维的高斯宽度，N2 H+可能只跟踪大尺度细丝的致密最内部区域。这些半功率宽度是在各种低质量恒星形成区域附近的大样本中发现的约0.1 pc的值的两倍之内，这往往表明跨临界或超临界细丝内的前星核碎裂的物理条件在每单位长度的大质量范围内是相同的。
ContextThe Orion molecular cloud is the closest region of high-mass star formation. It is an ideal target for investigating the detailed structure of massive star-forming filaments at high resolution and the relevance of the filament paradigm for the earliest stages of intermediate- to high-mass star formation.AimsWithin the Orion A molecular cloud, the integral-shaped filament (ISF) is a prominent, degree-long structure of dense gas and dust with clear signs of recent and ongoing high-mass star formation. Our aim is to characterise the structure of this massive filament at moderately high angular resolution (8′′ or ~0.016 pc) in order to measure the intrinsic width of the main filament, down to scales well below 0.1 pc, which has been identified as the characteristic width of filaments.MethodsWe used the ArTéMiS bolometer camera at APEX to map a ~0.6 × 0.2 deg2region covering OMC-1, OMC-2, and OMC-3 at 350 and 450 μm. We combined these data withHerschel-SPIRE maps to recover extended emission. The combinedHerschel-ArTéMiS maps provide details on the distribution of dense cold material, with a high spatial dynamic range, from our 8′′ resolution up to the transverse angular size of the map, ~10–15′. By combiningHerscheland ArTéMiS data at 160, 250, 350, and 450 μm, we constructed high-resolution temperature and H2column density maps. We extracted radial intensity profiles from the column density map in several representative portions of the ISF, which we fitted with Gaussian and Plummer models to derive their intrinsic widths. We also compared the distribution of material traced by ArTéMiS with that seen in the higher-density tracer N2H+(1–0) that was recently observed with the ALMA interferometer.ResultsAll the radial profiles that we extracted show a clear deviation from a Gaussian, with evidence for an inner plateau that had not previously been seen clearly usingHerschel-only data. We measure intrinsic half-power widths in the range 0.06–0.11 pc. This is significantly larger than the Gaussian widths measured for fibres seen in N2H+, which probably only traces the dense innermost regions of the large-scale filament. These half-power widths are within a factor of two of the value of ~0.1 pc found for a large sample of nearby filaments in various low-mass star-forming regions, which tends to indicate that the physical conditions governing the fragmentation of pre-stellar cores within transcritical or supercritical filaments are the same over a large range of masses per unit length.