A relation between H2 v=1−0 S(1) and 3.28 micron emission in Seyfert and starburst galaxies
A relation between H2 v=1−0 S(1) and 3.28 micron emission in Seyfert and starburst galaxies
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Seyfert 星系和星暴星系中 H2 v=1−0 S(1) 与 3.28 微米发射之间的关系
DOI：
10.1086/185745
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发表时间：
1990
期刊：
影响因子：
--
通讯作者：
M. Nishida
中科院分区：
文献类型：
--
作者：
H. Mouri;K. Kawara;Y. Taniguchi;M. Nishida
这封信报告了在24个包含活动星系核（AGN）或星爆核（SBN）的星系样本上，H2 v = 1-0 S(1)发射线与3.28微米发射特征的比较结果。在SBNs中，这些辐射之间存在良好的线性相关性。如果假设S(1)线是由于超新星事件的激波加热造成的，而3.28微米的特征是由于年轻恒星的紫外线辐射造成的，那么Rieke et al.（1980）和Gehrz et al.（1983）发表的星爆模型很好地解释了这种相关性。另一方面，在agn中，3.28微米特征对S(1)的相对强度小于sbn中的相对强度。这种趋势被解释为由于S(1)的激发增强和来自Seyfert核的大量x射线光子引起的3.28微米发射材料的破坏。参38。
This letter reports the results of a comparison of the H2 v = 1-0 S(1) emission line with the 3.28-micron emission feature on a sample of 24 galaxies containing an active galactic nucleus (AGN) or a starburst nucleus (SBN). In the SBNs, a good linear correlation is found between these emissions. If it is assumed that the S(1) line is due to shock heating by supernova events and the 3.28-micron feature is due to UV radiation of young stars, this correlation is well explained by starburst models published by Rieke et al. (1980) and Gehrz et al. (1983). In the AGNs, on the other hand, the relative strengths of 3.28-micron feature to S(1) are smaller than those in the SBNs. This trend is interpreted as due to enhanced excitation of S(1) and destruction of 3.28-micron-emitting material caused by abundant X-ray photons from the Seyfert nuclei. 38 refs.