Table A.3
Radio information on PACWBs.
| # | Usual ID | Non-thermal (NT) criteria | Ref. | Q |
|
|
||||
| 1 | HD 15558 | variable flux | 1 | II |
| 2 | δ Ori A | variable flux | 1 | II |
| 3 | σ Ori AB | α < 0 or close to 0 | 2 | I |
| 4 | 15 Mon | α < 0, variable flux | 2 | I |
| 5 | WR 8 | α < 0.3 | 3 | II |
| 6 | WR 11 | α ~ 0.3 | 4, 5 | II |
| 7 | WR 14 | α < 0, variable flux | 4, 5 | I |
| 8 | CD–47 4551 | high flux density, α < 0 | 6, 7, 8 | I |
| 9 | WR 21a | α < 0.3 | 9 | II |
| 10 | HD 93129A | high flux density, α < 0, resolved NT emitting region | 10, 6, 7, 11 | I |
| 11 | HD 93250 | high flux density | 12 | II |
| 12 | η Car | – | – | I |
| 13 | WR 39 | α close to 0, offset of about 3” w.r.t optical source | 5 | I |
| 14 | WR 48 | α < 0 | 5 | I |
| 15 | HD 124314 | high flux density, α < 0 | 6, 7, 8 | I |
| 16 | HD 150136 | high flux density, α < 0 | 6, 7, 8 | I |
| 17 | HD 151804 | α < 0 | 13 | I |
| 18 | WR 78 | α < 0 | 13 | I |
| 19 | WR 79a | α < 0, variable flux | 13, 14 | I |
| 20 | HD 152623 | α < 0 | 13 | I |
| 21 | WR 89 | variable flux | 14 | II |
| 22 | WR 90 | α close to 0, variable flux | 5 | I |
| 23 | WR 98 | α < 0.3, variable flux | 3 | I |
| 24 | WR 98a | variable flux, α close to 0 | 14, 15 | I |
| 25 | WR 104 | variable flux, α close to 0 | 14, 15 | I |
| 26 | WR 105 | variable flux, α < 0 | 4, 5, 14 | I |
| 27 | 9 Sgr | high flux density, α < 0 or close to 0, variable flux | 1, 16 | I |
| 28 | WR 112 | α close to 0, variable flux | 5, 15 | I |
| 29 | HD 167971 | high flux density, α < 0, variable flux | 1, 17 | I |
| 30 | HD 168112 | high flux density, α < 0, variable flux | 1, 18, 19 | I |
| 31 | CEN 1a | high flux density, variable flux and α close to 0 | 20, 21 | I |
| 32 | CEN 1b | high flux density, α < 0 | 20, 21 | I |
| 33 | WR 125 | α < 0, variable flux | 5, 22, 23 | I |
| 34 | HD 190603 | α < 0.3 | 24 | II |
| 35 | WR 133 | α < 0 | 3 | I |
| 36 | WR 137 | α close to 0 | 25 | II |
| 37 | WR 140 | high flux density, α < 0 and variable, variable flux, resolved NT emitting region | 26, 27, 28, 29 | I |
| 38 | Cyg OB2 #5 | α < 0, variable flux, resolved NT emitting region | 30, 31, 32 | I |
| 39 | Cyg OB2 #9 | α < 0, variable flux, bow-shaped NT emission | 1, 33, 34, 35 | I |
| 40 | Cyg OB2 #8A | α < 0, variable flux | 1, 36 | I |
| 41 | Cyg OB2-335 | high flux density, α < 0 | 37 | I |
| 42 | WR 146 | high flux density, α < 0, resolved NT emitting region | 25, 37, 38 | I |
| 43 | WR 147 | high flux density, α < 0, resolved NT emitting region | 39, 25, 37, 40 | I |
Reference. 1) Bieging et al. (1989); 2) Drake (1990); 3) Montes et al. (2009); 4) Leitherer et al. (1997); 5) Chapman et al. (1999); 6) Benaglia et al. (2006); 7) Benaglia & Koribalski (2007); 8) Benaglia et al. (2001); 9) Benaglia et al. (2005); 10) Benaglia & Koribalski (2004); 11) Benaglia et al. (2010a); 12) Leitherer et al. (1995); 13) Setia Gunawan et al. (2003a); 14) Cappa et al. (2004); 15) Monnier et al. (2002); 16) Rauw et al. (2002); 17) Blomme et al. (2007); 18) De Becker et al. (2004a); 19) Blomme et al. (2005); 20) Rodríguez et al. (2009); 21) Rodríguez et al. (2012); 22) Abbott et al. (1986); 23) Williams et al. (1992); 24) Scuderi et al. (1998); 25) Dougherty & Williams (2000); 26) Williams et al. (1990); 27) Williams et al. (1994); 28) White & Becker (1995); 29) Dougherty et al. (2005); 30) Contreras et al. (1997); 31) Kennedy et al. (2010); 32) Ortiz-León et al. (2011); 33) van Loo et al. (2008); 34) Dougherty & Pittard (2006); 35) Blomme et al. (2013); 36) Blomme et al. (2010); 37) Setia Gunawan et al. (2003b); 38) O’Connor et al. (2005); 39) Caillault et al. (1985); 40) Williams et al. (1997).
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