Table A.2
CO luminosities and molecular masses in the regions observed in shell S2 by Charmandaris et al. (2000) that show evidence of star formation, either through TIR or FUV emission.
| Position | ICO |
|
MH2 | SFR |
|
|
| (offset) | (K km s-1) | (K km s-1 pc2) | (M⊙) | (M⊙ yr-1) | (Gyr) | |
|
|
||||||
| 0 | (0′′,0′′) | 1.83 | 9.7 × 105 | 4.5 × 106 | 9.5 × 10-4 | 4.74 |
| 1 | (0′′,22′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 6.1 × 10-4 | <0.75 |
| 2 | (−22′′,22′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 3.1 × 10-4 | <1.48 |
| 3 | (−22′′,0′′) | 0.69 | 3.7 × 105 | 1.7 × 106 | 1.6 × 10-3 | 1.06 |
| 4 | (−22′′,−22′′) | 1.37 | 7.3 × 105 | 3.3 × 106 | 1.2 × 10-3 | 2.75 |
| 5 | (0′′,−22′′) | 2.40 | 1.3 × 106 | 5.8 × 106 | 2.1 × 10-4 | 27.6 |
| 6 | (22′′,−22′′) | 1.60 | 8.5 × 105 | 3.9 × 106 | 4.5 × 10-4 | 8.67 |
| 7 | (22′′,0′′) | 0.80 | 4.2 × 105 | 1.9 × 106 | 3.2 × 10-4 | 5.94 |
| 8 | (22′′,22′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 2.1 × 10-4 | <2.19 |
| 9 | (0′′,44′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 1.9 × 10-4 | <2.42 |
| 10 | (−44′′,44′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | <1.9 × 10-4 | – |
| 11 | (−44′′,0′′) | 0.80 | 4.2 × 105 | 1.9 × 106 | 8.6 × 10-6 | 220 |
| 12 | (−44′′,−44′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 7.0 × 10-4 | <0.66 |
| 13 | (0′′,−44′′) | 2.06 | 1.1 × 106 | 5.0 × 106 | 2.1 × 10-4 | 23.8 |
| 14 | (44′′,−44′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 1.2 × 10-4 | <3.83 |
| 15 | (44′′,0′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 1.1 × 10-4 | <4.18 |
| 16 | (44′′,44′′) | <0.19 | <1.0 × 105 | <4.6 × 105 | 4.0 × 10-4 | <1.15 |
Notes. MH2 is the molecular mass derived from the CO emission. The SFR and were estimated in regions of 44′′, corresponding to the beam of SEST for CO(1−0). The offset (0′′,0′′) is centred on 
, δ = −43:08:34.9. As a result of the cirrus contamination, the SFR and values are subject to high uncertainties.
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