“分子氢”的版本间差异
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*Mid-infrared molecular hydrogen (H2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies; （ rotational transition）[https://arxiv.org/abs/1805.09926] |
*Mid-infrared molecular hydrogen (H2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies; （ rotational transition）[https://arxiv.org/abs/1805.09926] |
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*Table 1. H2 Rotational Transitionsa |
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:*Notation b Transition c Rest λµm d Eu=k [K] e A [10−7 s−1] f g (J) g |
:*Notation b Transition c Rest λµm d Eu=k [K] e A [10−7 s−1] f g (J) g |
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:*S(0) J = 2 - 0 28.219 510 0.00029 5 |
:*S(0) J = 2 - 0 28.219 510 0.00029 5 |
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:*S(6) J = 8 - 6 6.109 5829 1.14 17 |
:*S(6) J = 8 - 6 6.109 5829 1.14 17 |
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:*S(7) J = 9 - 7 5.511 7197 2.00 57 |
:*S(7) J = 9 - 7 5.511 7197 2.00 57 |
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* The [C II] 158um emission |
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:correlates with galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dex and without evident systematics: |
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: the [C II]-to-H2 conversion factor (alpha_[C II] ~ 30 Msun/Lsun) is largely independent of galaxies' depletion time, metallicity, and redshift. |
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2018年8月31日 (五) 09:04的最新版本
- Mid-infrared molecular hydrogen (H2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies; （ rotational transition）[1]
- Table 1. H2 Rotational Transitionsa
- Notation b Transition c Rest λµm d Eu=k [K] e A [10−7 s−1] f g (J) g
- S(0) J = 2 - 0 28.219 510 0.00029 5
- S(1) J = 3 - 1 17.035 1015 0.00476 21
- S(2) J = 4 - 2 12.279 1682 0.0276 9
- S(3) J = 5 - 3 9.665 2504 0.0984 33
- S(4) J = 6 - 4 8.025 3474 0.264 13
- S(5) J = 7 - 5 6.910 4586 0.588 45
- S(6) J = 8 - 6 6.109 5829 1.14 17
- S(7) J = 9 - 7 5.511 7197 2.00 57
- The [C II] 158um emission
- correlates with galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dex and without evident systematics:
- the [C II]-to-H2 conversion factor (alpha_[C II] ~ 30 Msun/Lsun) is largely independent of galaxies' depletion time, metallicity, and redshift.