“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]
:*Table 1. H2 Rotational Transitionsa
*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
:*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(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
:*S(7) J = 9 - 7 5.511 7197 2.00 57
:*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.

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.