期刊
ASTROPHYSICAL JOURNAL
卷 638, 期 2, 页码 759-765出版社
IOP PUBLISHING LTD
DOI: 10.1086/498566
关键词
astrochemistry; dust, extinction; galaxies : ISM; infrared : galaxies; infrared : ISM; ISM : evolution
Silicates are an important component of interstellar dust, and the structure of these grains (amorphous or crystalline) is sensitive to the local physical conditions. We have studied the infrared spectra of a sample of ultraluminous infrared galaxies (ULIRGs). Here we report the discovery of weak, narrow absorption features at 11, 16, 19, 23, and 28 mu m, characteristic of crystalline silicates, superimposed on the broad absorption bands at 10 and 18 mu m due to amorphous silicates in a subset of this sample. These features betray the presence of forsterite (Mg2SiO4), the magnesiumrich end member of the olivines. Previously, crystalline silicates have only been observed in circumstellar environments. The derived fraction of forsterite to amorphous silicates is typically 0.1 in these ULIRGs. This is much larger than the upper limit for this ratio in the interstellar medium of the MilkyWay, 0.01. These results suggest that the timescale for injection of crystalline silicates into the ISM is short in a merger-driven starburst environment (e.g., as compared to the total time to dissipate the gas), pointing toward massive stars as a prominent source of crystalline silicates. Furthermore, amorphization due to cosmic rays, which is thought to be of prime importance for the local ISM, lags in vigorous starburst environments.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据