Observational Study of Mass Function in Large Magellanic Molecular cloud

大麦哲伦分子云质量函数的观测研究

• 批准号: 09304025
• 负责人: FUKUI Yasuo
• 金额: $ 19.2万
• 依托单位: Nagoya University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (A)
• 财政年份: 1997
• 资助国家: 日本
• 起止时间: 1997 至 1998
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-09304025/
• 关键词: Radio astronomy; Star formation; Molecular cloud; Galaxies; Magellanic Clouds; Interstellar molecules

In order to understand the formation process of populous stellar clusters in the Magellanic Clouds, we have carried out the most extensive observations of molecular clouds by using the 4 m mm-wave telescope. NANTEN, installed at Las Campanas. These observations have covered the Large Magellanic Cloud fully at a linear resolutions of 40 pc, in the ^<12>C0 (J=1-0) emission at 2.6 mm wavelength. The main results are summarized as follows ;(1) There are more than 100 giant molecular clouds. Their mass ranges from l0^5 M<of sun> to 2 \ 10^6 M<of sun>.(2) The line intensity of CO emission in the Large Magellanic Cloud is smaller by a factor of 3 than that in the Galaxy for giant molecular clouds having a similar mass.(3) For the 55 giant molecular clouds significantly detected, we find that they are spatially well correlated with the youngest stellar clusters with < 10 Myr (26 of 55).(4) By comparing the molecular clouds with their associated HII regions, we find giant molecular clouds are rapidly dissipated after formation of stellar clusters.Total molecular mass is calculated as 4-7 \ 10^6 M<of sun>, corresponding to * 10 % of the neutral hydrogen mass.

为了了解麦哲伦星云中人口众多的星团的形成过程，我们用4米毫米波望远镜对分子云进行了最广泛的观测。南滕，安装在拉斯坎帕纳斯。这些观测在2.6 mm波长的^C 0（J=1-0）发射中以40 pc的线性分辨率完全覆盖了大麦哲伦云<12>。主要结果如下：（1）地球上有100多个巨分子云。它们的质量范围从10^5 M<of sun>到210^6 M<of sun>。(2)大麦哲伦云的CO发射线强度比银河系中质量相近的巨分子云的CO发射线强度小3倍。(3)对于55个巨大的分子云显着检测，我们发现，它们在空间上与最年轻的恒星星团&lt; 10万年（55个中的26个）。(4)通过比较分子云和HII区，发现星团形成后巨大分子云迅速消散，总分子质量为4-7 × 10^6 M<of sun>，相当于中性氢质量的10%。

项目成果

H.Matsuhara: "Observations of [C II]158 Micron Line and Far-Infrared Continuum Emission toward the High-Latitude Molecular Clouds in Ursa Major" Astrophysical Journal. v.490. 744-751 (1997)

H.Matsuhara：“对大熊座高纬度分子云的 [C II]158 微米线和远红外连续发射的观测”天体物理学杂志。

A.Obayashi et al.: "Star Formation in the L1333 Molecular Cloud in Cassiopeia" Astrophysical J.115. 274-285 (1998)

A.Obayashi 等人：“仙后座 L1333 分子云中的恒星形成”天体物理学 J.115。

A.Mizuno: "A ^<13>CO(J=1-0)Search for Small Molecular Clouds toward the Chamaeleon-Musca Dark Cloud Complex" Astrophysical Journal Letters. v.507. 83-87 (1998)

A.Mizuno：“A ^<13>CO(J=1-0)寻找变色龙-蝇蝇暗云复合体的小分子云”天体物理学期刊快报。

T.Onishi et al.: "A C^<18>O Survey of Dense Cloud Cores in Taurus : Star Formation" Astrophysical J.502. 296-314 (1998)

T.Onishi 等人：“金牛座稠密云核的 A C^<18>O 调查：恒星形成”天体物理学 J.502。

K.C Xiao et al.: "A Low-noise 230 GHz SIS Receiver for Radio Astronomy Employing Untuned Nb/AlOx/Nb Tunnel Junctions" Astronomi J.19. 15-31 (1998)

K.C Xiao 等人：“采用未调谐 Nb/AlOx/Nb 隧道结的用于射电天文学的低噪声 230 GHz SIS 接收器”Astronomi J.19。