Table 2: Comparison of the observed ratios of H2 to H2 (1-0) S(1) at 2.12 $\mu $m in 3 different regions of the galaxy (see text) with fluorescent and thermal excitation models by Black & van Dishoek (Black 1987). The observed line ratio are in agreement with a fluorescent excitation model.
line $\lambda (\mu$m) NE C SW fl. th.

5-3Q(1)		 1.493 - - - 0.43 $1.0 \times 10^{-4}$
4-2O(3) 1.510 - 0.23 - 0.42 $7.0 \times10^{-4}$
6-4Q(1) 1.601 - 0.20 - 0.33 $1.3\times10^{-4}$
5-3O(3) 1.613 - 0.25 0.17 0.38 $9 \times10^{-5}$
6-4O(3) 1.733 - 0.23 0.12 0.31 $1 \times10^{-5}$
1-0S(3) 1.958 0.69 1.14 0.98 0.67 0.93
2-1S(4) 2.004 - - - 0.12 0.02
1-0S(2) 2.034 0.43 0.41 0.32 0.50 0.38
2-1S(3) 2.073 0.24 0.38 0.32 0.35 0.08
2-1S(2) 2.154 0.19 0.21 0.18 0.28 0.04
1-0S(0) 2.223 0.46 0.53 0.37 0.46 0.21
2-1S(1) 2.248 0.41 0.45 0.34 0.56 0.08
2-1S(0) 2.356 0.15 0.27 0.16 0.26 0.02
3-2S(1) 2.386 - - 0.25 0.29 $5.8 \times10^{-3}$
1-0Q(1) 2.407 0.77 1.18 1.62 0.99 0.70
1-0Q(2) 2.413 - 0.23 - 0.51 0.23
1-0Q(3) 2.424 0.46 0.69 0.75 0.70 0.70
1-0Q(4) 2.437 - 0.14 0.15 0.28 0.21
Br$\gamma $ 2.167 - 11.7 66.6    


Source LaTeX | All tables | In the text