“星系中的常见发射线”的版本间差异
跳到导航
跳到搜索
无编辑摘要 |
无编辑摘要 |
||
| 第6行： | 第6行： | ||
:trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[http://arxiv.org/abs/1504.05216] |
:trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[http://arxiv.org/abs/1504.05216] |
||
* 发射线的线比可以区分不同的电离机制，金属丰度 [[BPT diagram]],详细的工作可参见[http://arxiv.org/abs/1606.04667] |
* 发射线的线比可以区分不同的电离机制，金属丰度 [[BPT diagram]],详细的工作可参见[http://arxiv.org/abs/1606.04667] |
||
==红外谱线== |
|||
*精细结构线 [http://arxiv.org/abs/1607.02511] |
|||
The new [OIV]25.9μm/[OIII]88μm vs [NeIII]15.6μm/[NeII]12.8μm diagram is proposed as the best diagnostic to separate: i) AGN activity from any kind of star formation; and ii) low-metallicity dwarf galaxies from starburst galaxies. |
|||
2016年7月12日 (二) 03:25的版本
- [OII] doublet (3737A)
- [OIII] (4959A and 5007A)
- Balmer series (6563A, 4861A, 4340A, 4103A, ...).
- [NII]6583A
- [CII] 158$\mu$m fine-structure line
- trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[1]
- 发射线的线比可以区分不同的电离机制，金属丰度 BPT diagram,详细的工作可参见[2]
红外谱线
- 精细结构线 [3]
The new [OIV]25.9μm/[OIII]88μm vs [NeIII]15.6μm/[NeII]12.8μm diagram is proposed as the best diagnostic to separate: i) AGN activity from any kind of star formation; and ii) low-metallicity dwarf galaxies from starburst galaxies.