Table B.3.
EW of the H3+ P-branch transitions and derived column densities.
| Target | P(1,1) (a) | N(1,1) | P(2,2) (b) | N(2,2) | P(3,3) | N(3,3) | P(3,0) | N(3,0) | |
|---|---|---|---|---|---|---|---|---|---|
| 4.070 μm | 4.204 μm | 4.350 μm | 4.355 μm | ||||||
| (10−5 μm) | (1015 cm−2) | (10−5 μm) | (1015 cm−2) | (10−5 μm) | (1015 cm−2) | (10−5 μm) | (1015 cm−2) | ||
| VV 114 SW-s1 | 7.9 ± 0.7 | 5.5 ± 0.5 | < 0.67 | < 0.25 | 8.3 ± 0.6 | 2.5 ± 0.2 | < 0.65 | < 0.48 | |
| VV 114 SW-s2 | ⋯ | ⋯ | 6.4 ± 1.3 | 2.4 ± 0.5 | 17.0 ± 1.1 | 5.1 ± 0.3 | < 3.8 | < 2.8 | |
| VV 114 NE | ⋯ | ⋯ | < 1.0 | < 0.37 | 7.1 ± 0.9 | 2.1 ± 0.3 | < 0.89 | < 0.66 | |
| IRAS 07251 | ⋯ | ⋯ | 45.7 ± 2.8 | 17.0 ± 1.0 | 107.5 ± 2.0 | 32.2 ± 0.6 | 18.3 ± 2.0 | 13.7 ± 1.5 | |
| IRAS 08572 | ⋯ | ⋯ | 5.7 ± 0.8 | 2.1 ± 0.3 | 9.2 ± 0.7 | 2.7 ± 0.2 | 2.1 ± 0.7 | 1.6 ± 0.5 | |
| NGC 3256-S | ⋯ | ⋯ | 6.5 ± 3.5 | 2.4 ± 1.3 | 12.7 ± 3.1 | 3.8 ± 0.9 | < 3.1 | < 2.3 | |
| IRAS 14348 NE | ⋯ | ⋯ | < 1.9 | < 0.70 | 9.9 ± 1.2 | 3.0 ± 0.4 | < 1.2 | < 0.90 | |
| IRAS 14348 SW | ⋯ | ⋯ | 24.8 ± 2.5 | 9.2 ± 0.9 | 70.3 ± 2.1 | 21.1 ± 0.6 | 12.0 ± 2.1 | 9.0 ± 1.6 | |
| Arp 220 W | ⋯ | ⋯ | 13.6 ± 3.3 | 5.1 ± 1.2 | 42.5 ± 2.9 | 12.7 ± 0.9 | < 2.9 | < 2.2 | |
| Arp 220 E | ⋯ | ⋯ | 11.4 ± 3.7 | 4.2 ± 1.4 | 32.1 ± 3.3 | 9.6 ± 1.0 | < 3.4 | < 2.5 | |
| IRAS 05189 | ⋯ | ⋯ | < 1.6 | < 0.59 | < 1.5 | < 0.46 | < 1.5 | < 1.1 | |
| IRAS 09111 | ⋯ | ⋯ | < 12.2 | < 4.5 | < 12.8 | < 3.8 | < 12.9 | < 9.6 | |
| NGC 3256-N | ⋯ | ⋯ | < 3.7 | < 1.4 | < 3.8 | < 1.1 | < 3.8 | < 2.8 | |
| IRAS 13120 | ⋯ | ⋯ | < 2.1 | < 0.77 | < 2.0 | < 0.61 | < 2.0 | < 1.5 | |
| II Zw 096 C0 | ⋯ | ⋯ | < 4.6 | < 1.7 | < 4.8 | < 1.4 | < 4.8 | < 3.6 | |
| II Zw 096 D0 | ⋯ | ⋯ | < 3.3 | < 1.2 | < 3.2 | < 0.94 | < 3.1 | < 2.3 | |
| NGC 7469 | ⋯ | ⋯ | < 1.9 | < 0.69 | < 1.8 | < 0.55 | < 1.8 | < 1.4 | |
Notes. (a) The P(1,1) transition is blended with the H2 1-1 S(13) 4.068 μm. Thus, for most objects it is not possible to derive realiable measurements or upper limits. (b) The P(2,2) transition is affected by the CO2 ice and gas absorptions in some cases (e.g., NGC 3256-S), so the derived EW and column densities for this transition are uncertain.
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