“星系中的常见发射线”的版本间差异
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==红外谱线== |
==红外谱线== |
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*精细结构线 [http://arxiv.org/abs/1607.02511] |
*精细结构线 [http://arxiv.org/abs/1607.02511] |
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:*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. |
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:*the ([NeIII]15.6μm + [NeII]12.8μm)/([SIV]10.5μm + [SIII]18.7μm) ratio is proposed as a promising metallicity tracer to be used in obscured objects, where optical lines fail to accurately measure the metallicity. |
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:weak [NII] 205 um: 恒星形成 [http://arxiv.org/abs/1607.02520] |
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2016年7月12日 (二) 03:31的版本
光学波段
- [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.
- the ([NeIII]15.6μm + [NeII]12.8μm)/([SIV]10.5μm + [SIII]18.7μm) ratio is proposed as a promising metallicity tracer to be used in obscured objects, where optical lines fail to accurately measure the metallicity.
- weak [NII] 205 um: 恒星形成 [4]