Table 1
Summary of the important astrophysical parameters of the model for each cluster.
| Cluster | O stars | Luminosity | RHII | Rb | nHII | Log(Age) | D | Fermi-LAT analysis | ξmax | |
| name | (most massive) | (erg s-1) | (pc) | (pc) | (cm-3) | Log(years) | (kpc) | TS |  (cm-2s-1) |
(%) |
|
|
||||||||||
| NGC 2244 | 4 (O4) | 1.0 × 1037 | 16.9 | 6.2 | 15 | 6.28 | 1.55 | 22.1 | 4.61 × 10-10 | 5.80 |
| NGC 1976 | 4 (O7) | 1.5 × 1036 | 3.7 | 2 | 8900 | 6.4 | 0.4 | 5.6 | 3.50 × 10-10 | 6.69 |
|
|
||||||||||
| NGC 2175 | 1 (O6.5) | 1.3 × 1036 | 12 | 2.56* | 13 | 6.3 | 2.2 | 7.1 | 2.14 × 10-10 | 9.81 |
| NGC 3324 | 2 (O6.5) | 1.6 × 1036 | 6.5 | 2.32* | 33 | 6.4 | 3 | 2.7 | 5.54 × 10-10 | 100 |
| RCW 8 | 2 (O8.5) | 4.8 × 1035 | 2.2 | 1.86* | 91 | 6.78 | 4.2 | 11.2 | 1.75 × 10-10 | 100 |
| RCW 62 | 10 (O6) | 9.2 × 1036 | 25.6 | 2.59* | 430 | 6.8 | 2.2 | 0.1 | 3.54 × 10-10 | 0.13 |
| NGC 6618 | 17 (O4) | 3.3 × 1037 | 4 | 1.69* | 470 | 6 | 1.6 | 1.4 | 4.20 × 10-11 | 0.27 |
| NGC 2467 | 3 (O3) | 1.4 × 1037 | 4 | 1.51* | 550 | 6.3 | 4.1 | 3.2 | 9.57 × 10-11 | 7.06 |
Notes. The radius RHII of the HII region and the density nHII , which are fixed by optical observations, the age of the cluster and its distance. The luminosity is computed from the composition of O-stars, according to Nieuwenhuijzen & de Jager (1990) and Massey & Meyer (2001). The bubble radii indicated with a
were computed using Eq. (12) from Weaver et al. (1977). The second part of the table presents the results of the Fermi-LAT analysis. TS is the test statistic value for γ-ray emission at the position of the cluster and is the upper limit on the integrated γ-ray flux at a 95% confidence level. Finally, ξmax gives the upper limit of the stellar wind luminosity converted into particle acceleration, obtained with the one-zone model.
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