ALMA OBSERVATIONS OF THE IRDC CLUMP G34.43+00.24 MM3: 278 GHz CLASS I METHANOL MASERS
ALMA OBSERVATIONS OF THE IRDC CLUMP G34.43+00.24 MM3: 278 GHz CLASS I METHANOL MASERS
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DOI：
10.1088/2041-8205/794/1/l10
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发表时间：
2014-09
期刊：
影响因子：
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通讯作者：
T. Yanagida;T. Sakai;T. Hirota;N. Sakai;J. Foster;P. Sanhueza;J. Jackson;K. Furuya;Y. Aikawa;S. Yamamoto
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文献类型：
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作者：
T. Yanagida;T. Sakai;T. Hirota;N. Sakai;J. Foster;P. Sanhueza;J. Jackson;K. Furuya;Y. Aikawa;S. Yamamoto
我们利用阿塔卡玛大型毫米/亚毫米阵列在CH 3OH JK = 9−1-80 E、50-40 E和5−1-4−1 E谱线上以亚弧秒分辨率观测到与红外暗云G34.43+00.24相关的分子团（MM 3）。通过比较CH 3OH JK = 9−1-80 E发射与CH 3OH 50-40 E和5−1-4−1 E发射，我们发现CH 3OH JK = 9−1-80 E发射是激射的。我们已经清楚地表明，CH 3OH JK = 9−1-80脉泽产生于外流和周围稠密气体之间相互作用区域的后冲击气体。在CH_3OH脉泽发射的最强峰附近，SiO_J = 6-5的发射很弱。这表明CH_3OH脉泽辐射跟踪相对老的地震或弱的地震。
We have observed a molecular clump (MM3) associated with the infrared dark cloud G34.43+00.24 in the CH3OH JK = 9−1–80 E, 50–40 E, and 5−1–4−1 E lines at sub-arcsecond resolution by using the Atacama Large Millimeter/submillimeter Array. By comparing the CH3OH JK = 9−1–80 E emission with the CH3OH 50–40 E and 5−1–4−1 E emission, we have found that the CH3OH JK = 9−1–80 E emission is masing. We have clearly shown that the CH3OH JK = 9−1–80 masers arise from the post shocked gas in the interacting regions between the outflows and ambient dense gas. Toward the strongest peak of the CH3OH maser emission, SiO J = 6–5 emission is very weak. This indicates that the CH3OH maser emission traces relatively old shocks or weak shocks.