“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==
*精细结构线 [http://arxiv.org/abs/1607.02511]
*精细结构线 [http://arxiv.org/abs/1607.02511]
:*最强的线 [CII]158mu [OIII]88mu [OI]64mu
:*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 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.
:*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.
:*[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]
:weak [NII] 205 um: 恒星形成 [http://arxiv.org/abs/1607.02520]

* [CII] 158$\mu$m fine-structure line
*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]
:*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) [https://arxiv.org/abs/1809.00489]
*weak [NII] 205 um: 恒星形成 [http://arxiv.org/abs/1607.02520]

2018年11月16日 (五) 01:30的版本

光学波段

  • [OII] doublet (3737A)
  • [OIII] (4959A and 5007A)
  • Balmer series (6563A, 4861A, 4340A, 4103A, ...).
  • [NII]6583A
  • 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[1]
  • [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.

红外谱线

  • 精细结构线 [2]
  • 最强的线 [CII]158mu [OIII]88mu [OI]64mu
  • 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.
  • [CII] 158$\mu$m fine-structure line,trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[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) [4]
  • weak [NII] 205 um: 恒星形成 [5]