“消光曲线”的版本间差异
跳到导航
跳到搜索
（以“常用消光曲线, * simple power-law <math> \lambda^{-1} </math> * the Milky Way (MW) extinction curve (with a prominent bump at 2175) * the featureless Small Ma...”为内容创建页面） |
无编辑摘要 |
||
| 第1行： | 第1行： | ||
常用消光曲线, |
常用消光曲线, |
||
* simple power-law <math> |
* simple power-law <math>\lambda^{-1}</math> |
||
* the Milky Way (MW) extinction curve (with a prominent bump at 2175) |
* the Milky Way (MW) extinction curve (with a prominent bump at 2175) |
||
* the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV |
* the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV |
||
2015年3月4日 (三) 12:44的版本
常用消光曲线,
- simple power-law
- the Milky Way (MW) extinction curve (with a prominent bump at 2175)
- the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV
- the LargeMagellanic Cloud (LMC) curve being intermediate between that of the MW and the SMC;
- the featureless “Calzetti” attenuation law for the dust in local starburst galaxies (Calzetti et al. 1994);
- the relatively flat “Maiolino” extinction law for the dust in the dense circumnuclear region of AGNs (Maiolino et al. 2001) where the dust size distribution is skewed toward large grains
以上参见图1 [1]
类星体中的尘埃
- 一种认为和SMC差不多 Hopkins et al. (2004)
- 一种认为比较平 (Czerny et al. 2004; Gaskell et al. 2004).