查看“星系中的常见发射线”的源代码

==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.[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]

==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.
:*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 [http://arxiv.org/abs/1607.02520]