THE DUST-TO-GAS RATIO IN THE SMALL MAGELLANIC CLOUD TAIL
THE DUST-TO-GAS RATIO IN THE SMALL MAGELLANIC CLOUD TAIL
复制标题
小麦哲伦云尾中的尘气比
DOI：
10.1088/0004-637x/690/1/l76
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发表时间：
2009
期刊：
影响因子：
--
通讯作者：
Gordon K
中科院分区：
文献类型：
--
作者：
Gordon K
小麦哲伦云的尾部区域是使用斯皮策太空望远镜上的MIPS仪器成像的，作为SAGE-SMC斯皮策遗产的一部分。在所有的MIPS波段都探测到了尘埃的漫射红外辐射。利用MIPS观测结合现有的IRAS和H i观测，测得尾气-尘埃比为1200±350。这一气尘比高于根据已知的Tail金属丰度预计的500-800，表明尘埃颗粒可能遭到破坏。在MIPS观测中，尾部的两个星团区域被分解为多个来源，当地的气尘比被测量为10440和10250，表明这些区域有尘埃形成和/或大量的电离气体。这些结果支持了SMC尾是最近从SMC剥离的潮汐尾的解释，其中包括气体，尘埃和年轻恒星。
The Tail region of the Small Magellanic Cloud (SMC) was imaged using the MIPS instrument on the Spitzer Space Telescope as part of the SAGE-SMC Spitzer Legacy. Diffuse infrared emission from dust was detected in all the MIPS bands. The Tail gas-to-dust ratio was measured to be 1200±350 using the MIPS observations combined with existing IRAS and H i observations. This gas-to-dust ratio is higher than the expected 500–800 from the known Tail metallicity indicating possible destruction of dust grains. Two cluster regions in the Tail were resolved into multiple sources in the MIPS observations and local gas-to-dust ratios were measured to be∼ 440 and∼ 250 suggest dust formation and/or significant amounts of ionized gas in these regions. These results support the interpretation that the SMC Tail is a tidal Tail recently stripped from the SMC that includes gas, dust, and young stars.