Table 3
ALMA CO(1–0) line fluxes and luminosities of each spaxel and the WR region.
| Reg | Fint | S/N | Fint | L | L′ | MH2, CO | |
| (Jy km s-1) | (10-22 W m-2) | (L⊙) | (106 Kkms-1 pc2) | (106M⊙) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | |
|
|
|||||||
| Host | −0.406 ± 0.316 | −1.3 | −15.6 ± 12.1 | −66.4 ± 51.7 | −1.36 ± 1.05 | −6.8 ± 5.3 | |
| WR | 0.058 ± 0.049 | 1.2 | 2.2 ± 1.9 | 9.5 ± 8.1 | 0.19 ± 0.16 | 1.0 ± 0.8 | |
| 44 | 0.271 ± 0.125 | 2.2 | 10.4 ± 4.8 | 44.4 ± 20.4 | 0.91 ± 0.42 | 4.5 ± 2.1 | |
| 43 | 0.318 ± 0.141 | 2.3 | 12.2 ± 5.4 | 52.1 ± 23.0 | 1.06 ± 0.47 | 5.3 ± 2.3 | |
| 42 | 0.209 ± 0.109 | 1.9 | 8.1 ± 4.2 | 34.3 ± 17.8 | 0.70 ± 0.36 | 3.5 ± 1.8 | |
| 41 | −0.040 ± 0.132 | −0.3 | −1.5 ± 5.1 | −6.5 ± 21.6 | −0.13 ± 0.44 | −0.7 ± 2.2 | |
| 40 | 0.099 ± 0.128 | 0.8 | 3.8 ± 4.9 | 16.3 ± 21.0 | 0.33 ± 0.43 | 1.7 ± 2.1 | |
| 34 | 0.301 ± 0.132 | 2.3 | 11.6 ± 5.1 | 49.2 ± 21.6 | 1.00 ± 0.44 | 5.0 ± 2.2 | |
| 33 | 0.003 ± 0.126 | 0.0 | 0.1 ± 4.9 | 0.5 ± 20.7 | 0.01 ± 0.42 | 0.1 ± 2.1 | |
| 32 | 0.118 ± 0.124 | 0.9 | 4.5 ± 4.8 | 19.3 ± 20.4 | 0.39 ± 0.42 | 2.0 ± 2.1 | |
| 31 | 0.288 ± 0.140 | 2.1 | 11.1 ± 5.4 | 47.1 ± 22.8 | 0.96 ± 0.47 | 4.8 ± 2.3 | |
| 30 | 0.263 ± 0.111 | 2.4 | 10.1 ± 4.3 | 43.1 ± 18.2 | 0.88 ± 0.37 | 4.4 ± 1.9 | |
| 24 | 0.154 ± 0.103 | 1.5 | 5.9 ± 4.0 | 25.1 ± 16.9 | 0.51 ± 0.34 | 2.6 ± 1.7 | |
| 23 | 0.267 ± 0.137 | 2.0 | 10.3 ± 5.3 | 43.7 ± 22.4 | 0.89 ± 0.46 | 4.5 ± 2.3 | |
| 22 | 0.178 ± 0.108 | 1.6 | 6.8 ± 4.2 | 29.1 ± 17.7 | 0.59 ± 0.36 | 3.0 ± 1.8 | |
| 21 | 0.170 ± 0.119 | 1.4 | 6.6 ± 4.6 | 27.9 ± 19.5 | 0.57 ± 0.40 | 2.8 ± 2.0 | |
| 20 | 0.225 ± 0.121 | 1.9 | 8.7 ± 4.7 | 36.9 ± 19.9 | 0.75 ± 0.41 | 3.8 ± 2.0 | |
| 14 | 0.009 ± 0.114 | 0.1 | 0.4 ± 4.4 | 1.5 ± 18.7 | 0.03 ± 0.38 | 0.2 ± 1.9 | |
| 13 | 0.102 ± 0.129 | 0.8 | 3.9 ± 5.0 | 16.7 ± 21.1 | 0.34 ± 0.43 | 1.7 ± 2.2 | |
| 12 | 0.156 ± 0.109 | 1.4 | 6.0 ± 4.2 | 25.5 ± 17.8 | 0.52 ± 0.36 | 2.6 ± 1.8 | |
| 11 | 0.208 ± 0.111 | 1.9 | 8.0 ± 4.3 | 34.1 ± 18.1 | 0.70 ± 0.37 | 3.5 ± 1.9 | |
| 10 | 0.116 ± 0.114 | 1.0 | 4.4 ± 4.4 | 18.9 ± 18.6 | 0.39 ± 0.38 | 1.9 ± 1.9 | |
| 04 | 0.114 ± 0.117 | 1.0 | 4.4 ± 4.5 | 18.6 ± 19.2 | 0.38 ± 0.39 | 1.9 ± 2.0 | |
| 03 | 0.124 ± 0.123 | 1.0 | 4.8 ± 4.7 | 20.3 ± 20.1 | 0.41 ± 0.41 | 2.1 ± 2.1 | |
| 02 | 0.130 ± 0.116 | 1.1 | 5.0 ± 4.5 | 21.3 ± 19.0 | 0.43 ± 0.39 | 2.2 ± 1.9 | |
| 01 | 0.248 ± 0.121 | 2.0 | 9.5 ± 4.7 | 40.5 ± 19.9 | 0.83 ± 0.41 | 4.1 ± 2.0 | |
| 00 | 0.160 ± 0.115 | 1.4 | 6.2 ± 4.4 | 26.2 ± 18.9 | 0.53 ± 0.39 | 2.7 ± 1.9 | |
Notes. (1) The entire host, the WR region, or the spaxel number. (2) Integrated flux within dotted lines in Figs. 9 and 10. (3) Signal-to-noise ratio of the line. (4) Integrated flux in W m-2. (5) Line luminosity in solar luminosity. (6) Line luminosity using Eq. (3) in Solomon et al. (1997). (7) Molecular gas mass estimated assuming the Galactic CO-to-H2 conversion factor αCO = 5 M⊙/ (K km s-1 pc2).
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