Mapping the core of the Tarantula Nebula with VLT-MUSE
Mapping the core of the Tarantula Nebula with VLT-MUSE
复制标题
使用 VLT-MUSE 绘制狼蛛星云的核心图
DOI：
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发表时间：
2018
影响因子：
6.5
通讯作者：
E. Observatory
中科院分区：
文献类型：
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作者：
N. Castro;P. Crowther;C. Evans;J. Mackey;N. Castro;J. Vink;J. Melnick;F. S. U. O. Michigan;U. Sheffield;UK Astronomy Technology Centre;Dublin Institute for Advanced Studies;Grantecan;Armagh Observatory;Planetarium;E. Observatory
介绍了大麦哲伦星云中蜘蛛星云中心2′× 2′（30 × 30 pc）的VLT-MUSE观测结果。这些观测提供了对R136附近大质量恒星和电离气体的前所未有的光谱普查，R136是位于NGC 2070中的年轻致密星星团，位于本星系群中最富有的恒星形成区域的中心。我们提供了从MUSE数据管中提取的2255个点源的星云气体的分光光度和径向速度估计（叠加在恒星光谱上），我们还提供了270颗早期型恒星的恒星径向速度估计（发现平均系统速度为271 ± 41 km s−1）。我们提出了一个消光图构造的星云巴耳末线，电子密度和温度估计的[S II]，[N II]和[S III]线的强度比。由Hα和[N II] λ6583追踪的星际介质，为恒星可能形成的区域提供了新的见解。气体运动学是复杂的，但与以R136为中心的气体的系统速度相比，具有明显的双峰，蓝移和红移分布。有趣的点状源也出现在东部空洞、西部壳层和R136周围;这些可能与逃逸恒星、喷流、新恒星的形成或气体与沃尔夫-拉叶星的相互作用等现象有关。对核心的仔细检查揭示了最强X射线源周围的红移物质，尽管我们无法详细研究运动学，因为MUSE数据中的恒星在空间上无法分辨。本系列的后续论文将讨论NGC 2070的详细恒星内容及其综合恒星和星云性质。
We introduce VLT-MUSE observations of the central 2′× 2′ (30 × 30 pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming region in the Local Group. Spectrophotometry and radial-velocity estimates of the nebular gas (superimposed on the stellar spectra) are provided for 2255 point sources extracted from the MUSE datacubes, and we present estimates of stellar radial velocities for 270 early-type stars (finding an average systemic velocity of 271 ± 41 km s−1). We present an extinction map constructed from the nebular Balmer lines, with electron densities and temperatures estimated from intensity ratios of the [S II], [N II], and [S III] lines. The interstellar medium, as traced by Hα and [N II] λ6583, provides new insights in regions where stars are probably forming. The gas kinematics are complex, but with a clear bi-modal, blue- and red-shifted distribution compared to the systemic velocity of the gas centred on R136. Interesting point-like sources are also seen in the eastern cavity, western shell, and around R136; these might be related to phenomena such as runaway stars, jets, formation of new stars, or the interaction of the gas with the population of Wolf–Rayet stars. Closer inspection of the core reveals red-shifted material surrounding the strongest X-ray sources, although we are unable to investigate the kinematics in detail as the stars are spatially unresolved in the MUSE data. Further papers in this series will discuss the detailed stellar content of NGC 2070 and its integrated stellar and nebular properties.
影响因子：
56.9
作者：
Abramowski, A.;Aharonian, F.;Zechlin, H-S.
通讯作者：
Zechlin, H-S.