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Table A.2.

Physical parameters of the detected radio continuum sources that have candidate YSO associations (see Table A.1).

Source S5.8 GHz Deff ne EM NLyc MH II Spectral type M*
[mJy] [pc] [cm−3] [105 cm−6 pc] [log(photon s−1)] [M⊙] (single ZAMS star (a)) [M⊙]
3 2.8 1.0 62 0.029 46.3 0.50 B0-B0.5 12.8
5 26.9 1.4 127 0.158 47.3 2.35 B0-B0.5 16.2
34 69.6 2.0 115 0.192 47.7 6.66 O9.5-B0 18.4
44 10.7 0.9 142 0.136 46.9 0.83 B0-B0.5 14.5
51 2.1 0.8 71 0.032 46.2 0.33 B0.5-B1 12.4
54 10.1 1.1 104 0.088 46.8 1.07 B0-B0.5 14.5
64 7.7 0.8 140 0.119 46.7 0.61 B0-B0.5 14.1
66 4.5 1.1 73 0.042 46.5 0.67 B0-B0.5 13.4
78 5.4 0.9 106 0.074 46.6 0.56 B0-B0.5 13.7
80 13.4 1.1 115 0.110 47.0 1.29 B0-B0.5 14.8
82 6.8 1.1 87 0.061 46.7 0.86 B0-B0.5 13.9
87 190.1 2.6 126 0.302 48.1 16.66 O8.5-O9 21.3
89 16.8 1.3 108 0.110 47.1 1.71 B0-B0.5 15.2
91 5.2 1.1 76 0.047 46.6 0.76 B0-B0.5 13.6
93 5.8 1.2 69 0.042 46.6 0.94 B0-B0.5 13.7
115 13.9 0.9 170 0.189 47.0 0.90 B0-B0.5 14.9
135 9.7 0.9 134 0.122 46.8 0.80 B0-B0.5 14.4
140 60.5 1.4 185 0.345 47.6 3.61 O9.5-B0 18.1
157 120.9 1.2 326 0.922 47.9 4.10 O9-O9.5 19.6
230 15.9 1.2 115 0.117 47.0 1.53 B0-B0.5 15.1
234 436.9 2.6 195 0.712 48.5 24.79 O7.5-O8 25.5
235 73.6 1.1 297 0.691 47.7 2.74 O9.5-B0 18.5
262 33.8 1.2 162 0.237 47.4 2.31 O9.5-B0 16.8
277 54.6 1.2 222 0.424 47.6 2.72 O9.5-B0 17.8
284 43.3 1.4 147 0.227 47.5 3.25 O9.5-B0 17.3
296 40.8 1.9 92 0.120 47.5 4.87 O9.5-B0 17.2
299 240.2 1.9 236 0.754 48.2 11.24 O8-O8.5 22.4
307 87.0 1.5 186 0.391 47.8 5.17 O9.5-B0 18.9
311 1010.2 1.2 951 7.775 48.8 11.77 O6-O6.5 33.7
315 7.3 0.9 117 0.092 46.7 0.69 B0-B0.5 14.0
323 37.8 1.3 153 0.228 47.4 2.74 O9.5-B0 17.0

Notes. From left to right: source ID, 5.8 GHz integrated flux (S5.8 GHz), effective diameter (Deff), electron number density (ne), emission measure (EM), Lyman continuum photon flux (NLyc), H II region mass (MH II), spectral type, and interpolated stellar mass from values (M*) given by Davies et al. (2011). We calculated these values using the same caveat as in Immer et al. (2012a), where we assume radio sources are spherically symmetric H II regions. In our study, however, we adopted this assumption for extended sources as well, which have been marked in Table A.1.

(a)

Obtained from Panagia (1973).

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