“星系中的常见发射线”的版本间差异

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* Balmer series (6563A, 4861A, 4340A, 4103A, ...).
* Balmer series (6563A, 4861A, 4340A, 4103A, ...).
* [NII]6583A
* [NII]6583A
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* [CII] 158$\mu$m fine-structure line
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:*trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[http://arxiv.org/abs/1504.05216]
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:*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]
* 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]
*[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.
*[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.
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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.
:*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]
:weak [NII] 205 um: 恒星形成 [http://arxiv.org/abs/1607.02520]
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* [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]
⚫
:*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]

2018年11月16日 (五) 01:28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]
  • 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 [3]
  • [CII] 158$\mu$m fine-structure line
  • trace regions of active star formation and is the main coolant of the cold, neutral atomic medium.[4]
  • 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) [5]
取自“http://202.127.29.3/~shen/wiki/index.php?title=星系中的常见发射线&oldid=2964”