查看“尘埃”的源代码


*发射线的消光可能和连续谱的消光不同
*Halpha/Hbeta 线比
:内禀数值：2.86（恒星形成），3.1（AGN） 参见Osterbrock  & Ferland 2006
*尘埃在8000A左右有一个Extended Red Emission(ERE)的连续谱发射
*尘埃的红外发射: dustEM
*尘埃与气体有关，气体的光深可以从low-ionization interstellar (IS) absorption lines(e.g., Si II, O I, Fe II)获得 (Shapley et al. 2003)
:e.g. If the two Si II transitions at 1260 and 1527A are optically thin, then the ratio of their equivalent widths will be W1260/W1527 > 6. The observed ratio is W1260/W1527 ~ 1,  implying that the lines are saturated and hence their depths are sensitive to the covering fraction of Si II-enriched material.
*银河系盘外围区域的气尘比可能会偏大 [https://arxiv.org/abs/1708.05359]
: We find a weak trend of decreasing infrared to ~20 cm flux density ratios with increasing Rgal, in agreement with previous extragalactic results, possibly indicating a decreased dust abundance in the outer Galaxy.



:对于比912A更短的波长来说，气体的吸收消光是最主要的而不是dust，但是气体和尘埃是相关的，参见[http://arxiv.org/abs/1606.00434]
*模型THEMIS The Heterogeneous dust Evolution Model for Interstellar Solids) [http://www.ias.u-psud.fr/themis/]

==多波段==
*DustPedia [https://arxiv.org/abs/1708.05335]
:875个近距离星系 v<3000km/s
:42 个波段 （UV - micro-wave）
:孔径匹配 Comprehensive & Adaptable Aperture Photometry Routine (CAAPR)

==[[消光曲线]]==
*分子云中的turblence导致尘埃粒子按照颗粒大小分层分布，可以解释分子云中的消光曲线和其它地方不同[https://arxiv.org/abs/1706.05055]

==盘星系的尘埃分布==
:可以延展到2R25，[http://arxiv.org/abs/1607.01020]:
:密度轮廓比较follow恒星，而不是恒星形成（气体？）
:有温度梯度，从中心25K到边缘15K
:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象？
:多波段结果进行对比[https://arxiv.org/abs/1706.05351]