“星系中的常见发射线”的版本间差异

2018年9月5日 (三) 09:00的版本

trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[1]
both [CI] and CO emission trace gas that is predominantly molecular, with a density n ~ 500-1000 cm−3, [CII] traces lower density material (n ~ 100 cm−3) [2]

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[3]
[NII]/[OII]: . intermediate mass stars are the main source of nitrogen en- richment in massive galaxies (Moll´a et al. 2015), the gas from their stellar winds should be, on average, extremely nitrogen- rich.

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 [5]

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 * [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]
+:*trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[http://arxiv.org/abs/1504.05216]
-:both [CI] and CO emission trace gas that is predominantly molecular, with a density n ~ 500-1000 cm−3, [CII] traces lower density material (n ~ 100 cm−3)
+:*both [CI] and CO emission trace gas that is predominantly molecular, with a density n ~ 500-1000 cm−3, [CII] traces lower density material (n ~ 100 cm−3) [https://arxiv.org/abs/1809.00489]
 * 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]