“星系中的常见发射线”的版本间差异
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参见[[SFR]] |
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==电离势== |
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*H0 13.6 |
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*He0 24.6 |
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* S++ 34.8, O+ 35.1 |
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* He+ 54.4, O++ 54.9 |
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*O0可以电离到3种不同的O+状态(4S,2D,2P),从O0(3P)到O+的电离势为13.62 |
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==光学波段== |
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* [OII] doublet (3737A) |
* [OII] doublet (3737A) |
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* [OIII] (4959A and 5007A) |
* [[OIII5007 | [OIII] (4959A and 5007A) ]] |
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* Balmer series (6563A, 4861A, 4340A, 4103A, ...). |
* Balmer series (6563A, 4861A, 4340A, 4103A, ...). |
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* [NII]6583A |
* [NII]6583A |
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* 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] |
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*[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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*[[SII]]:电离势 10.4ev |
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==红外谱线== |
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*精细结构线 [http://arxiv.org/abs/1607.02511] |
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:*最强的线 [CII]158mu [OIII]88mu [OI]64mu,[OIII]来自HII区 |
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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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:*[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] |
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:*C原子的电离势11.2eV,因此C+在中性和电离去都存在,因此[CII]158mu能不能做SFR的指针有争议 (arXiv1910.0541),[CII]是PDR区域最有效的冷却线 |
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:*[NII]205mu, N原子的电离势是14.5ev,比H要高,因此[NII]线是在HII区才有 |
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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] |
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*weak [NII] 205 um: 恒星形成 [http://arxiv.org/abs/1607.02520] |
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==coronal lines == |
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* Higher-ionization, collisionally excited optical forbid�den lines, known as optical “coronal lines” (CLs; first discovered in the solar corona) |
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:为什么在AGN中很弱?因为尘埃的沉降效应使得它们很弱[https://arxiv.org/abs/2408.15229] |
2024年8月28日 (三) 14:25的最新版本
参见SFR
电离势
- H0 13.6
- He0 24.6
- S++ 34.8, O+ 35.1
- He+ 54.4, O++ 54.9
- O0可以电离到3种不同的O+状态(4S,2D,2P),从O0(3P)到O+的电离势为13.62
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.
- SII:电离势 10.4ev
红外谱线
- 精细结构线 [2]
- 最强的线 [CII]158mu [OIII]88mu [OI]64mu,[OIII]来自HII区
- 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]
- C原子的电离势11.2eV,因此C+在中性和电离去都存在,因此[CII]158mu能不能做SFR的指针有争议 (arXiv1910.0541),[CII]是PDR区域最有效的冷却线
- [NII]205mu, N原子的电离势是14.5ev,比H要高,因此[NII]线是在HII区才有
- 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]
coronal lines
- Higher-ionization, collisionally excited optical forbid�den lines, known as optical “coronal lines” (CLs; first discovered in the solar corona)
- 为什么在AGN中很弱?因为尘埃的沉降效应使得它们很弱[6]