“尘埃”的版本间差异
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: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. |
: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. |
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: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] |
: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] |
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*盘星系的尘埃分布,Herschel的结果 |
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:可以延展到2R25，[http://arxiv.org/abs/1607.01020]: |
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密度轮廓比较follow恒星，而不是恒星形成（气体？） |
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:有温度梯度，从中心25K到边缘15K |
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:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象？ |
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2016年7月6日 (三) 01:37的版本
- 消光曲线
- 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.
- 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[1]
- 盘星系的尘埃分布,Herschel的结果
- 可以延展到2R25，[2]:
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？