Galactic WR stars coincident with star-forming regions in the range 298° ≤ l ≤ 340°. We consider a WR star to be associated with a star-forming region (Anderson et al. 2014, WISE v1.4) if |$r \le 1.5 R_{\rm {\rm H}\,\small {ii}}$|, although some WR stars will doubtless be foreground sources, such that 53/206 (=26 per cent) WR stars associated with star-forming regions represents a strict upper limit.
| WISE . | d . | |$R_{}{\rm H}\,\small {ii}$| . | Ref . | Cluster? . | WN (r, arcmin) . | WC (r, arcmin) . | Ref . |
|---|---|---|---|---|---|---|---|
| H ii . | kpc . | arcmin . | . | . | . | . | . |
| G298.224−0.334 | 11.1 | 5.0 | a | WR46-7 (5), WR46-18 (8) | b, p | ||
| G298.529−0.251 | 10.5 | 16.2 | a | VVV CL 011 | WR46-8 (15.6), WR46-9 (3.5), WR46-17 (4.9) | WR46-10 (7.6) | b, c, d, e |
| WR46-15 (16.9), WR46-2 (22.4) | g | ||||||
| G298.862−0.432 | 10.7 | 4.8 | a | Mercer 30 | WR46-3 (6.6), WR46-4 (6.6), WR46-5 (6.6), | f | |
| WR46-6 (6.6) | f | ||||||
| G302.503−0.762 | 12.1 | 4.2 | a | WR47b (4.0) | h | ||
| G302.631+0.030 | 4.6 | 14.3 | a | WR47-1 (18.9) | e | ||
| G303.445−0.745 | 12.5 | 7.2 | a | WR47-2 (2.6) | d | ||
| G305.233+0.110 | 4.9 | 11.3 | a | Danks 1/2 | WR48-6 (5.5), WR48-10 (6.5), WR48-7 (7.7) | WR48-1 (8.6), WR48-3 (6.0) | e, g, h, i |
| WR48-9 (6.8), WR48-8 (6.8) | WR48-4 (8.2), WR48a (8.4) | h, i | |||||
| WR48-2 (10.3) | b | ||||||
| G305.322−0.255 | 4.9 | 13.4 | a | WR48-5 (4.7) | h | ||
| G311.991+0.219 | 6.0 | a | VVV CL 036 | WR60-6 (7.8) | c | ||
| G317.030+0.028a | 24.4 | a | VVV CL 041 | WR62-2 (15.7), WR62-1 (19.4), WR63 (34) | h, j | ||
| G321.015−0.527 | 4.1 | 4.0 | a | WR67-3 (6.1) | k | ||
| G321.115−0.546 | 3.8 | 4.2 | a | WR67-1 (1.8) | l | ||
| G326.474−0.292 | 20.9 | a | WR70-5 (17) | m | |||
| G327.824+0.117 | 7.2 | 3.9 | a | WR70-6 (5.2) | g | ||
| G331.020−0.143 | 3.8 | a | WR72-4 (3.5) | n | |||
| G335.794+0.153 | 13.7 | a | VVV CL 073 | WR75-6 (19.7), WR75-25 (6.1), WR75-26 (6.1) | WR75b (16.1), WR75-15 (12.4) | h | |
| WR75-16 (4.2) | n | ||||||
| G336.446−0.198 | 10.4 | a | WR75-9 (11.7), WR75-21 (10.3) | n | |||
| WR75-5 (14.3) | d | ||||||
| G338.350+0.221 | 6.9 | a | WR76-10 (4.7) | n | |||
| G338.430+0.048 | 5.8 | a | Mercer 81 | WR76-2 (3.5), WR76-3 (3.5), WR76-4 (3.5) | o | ||
| WR76-5 (3.5), WR76-6 (3.5), WR76-7 (3.5) | o | ||||||
| WR76-8 (3.5), WR76-9 (3.5) | o | ||||||
| G338.911+0.615 | 4.4 | 3.8 | a | WR76 (1.9) | h |
| WISE . | d . | |$R_{}{\rm H}\,\small {ii}$| . | Ref . | Cluster? . | WN (r, arcmin) . | WC (r, arcmin) . | Ref . |
|---|---|---|---|---|---|---|---|
| H ii . | kpc . | arcmin . | . | . | . | . | . |
| G298.224−0.334 | 11.1 | 5.0 | a | WR46-7 (5), WR46-18 (8) | b, p | ||
| G298.529−0.251 | 10.5 | 16.2 | a | VVV CL 011 | WR46-8 (15.6), WR46-9 (3.5), WR46-17 (4.9) | WR46-10 (7.6) | b, c, d, e |
| WR46-15 (16.9), WR46-2 (22.4) | g | ||||||
| G298.862−0.432 | 10.7 | 4.8 | a | Mercer 30 | WR46-3 (6.6), WR46-4 (6.6), WR46-5 (6.6), | f | |
| WR46-6 (6.6) | f | ||||||
| G302.503−0.762 | 12.1 | 4.2 | a | WR47b (4.0) | h | ||
| G302.631+0.030 | 4.6 | 14.3 | a | WR47-1 (18.9) | e | ||
| G303.445−0.745 | 12.5 | 7.2 | a | WR47-2 (2.6) | d | ||
| G305.233+0.110 | 4.9 | 11.3 | a | Danks 1/2 | WR48-6 (5.5), WR48-10 (6.5), WR48-7 (7.7) | WR48-1 (8.6), WR48-3 (6.0) | e, g, h, i |
| WR48-9 (6.8), WR48-8 (6.8) | WR48-4 (8.2), WR48a (8.4) | h, i | |||||
| WR48-2 (10.3) | b | ||||||
| G305.322−0.255 | 4.9 | 13.4 | a | WR48-5 (4.7) | h | ||
| G311.991+0.219 | 6.0 | a | VVV CL 036 | WR60-6 (7.8) | c | ||
| G317.030+0.028a | 24.4 | a | VVV CL 041 | WR62-2 (15.7), WR62-1 (19.4), WR63 (34) | h, j | ||
| G321.015−0.527 | 4.1 | 4.0 | a | WR67-3 (6.1) | k | ||
| G321.115−0.546 | 3.8 | 4.2 | a | WR67-1 (1.8) | l | ||
| G326.474−0.292 | 20.9 | a | WR70-5 (17) | m | |||
| G327.824+0.117 | 7.2 | 3.9 | a | WR70-6 (5.2) | g | ||
| G331.020−0.143 | 3.8 | a | WR72-4 (3.5) | n | |||
| G335.794+0.153 | 13.7 | a | VVV CL 073 | WR75-6 (19.7), WR75-25 (6.1), WR75-26 (6.1) | WR75b (16.1), WR75-15 (12.4) | h | |
| WR75-16 (4.2) | n | ||||||
| G336.446−0.198 | 10.4 | a | WR75-9 (11.7), WR75-21 (10.3) | n | |||
| WR75-5 (14.3) | d | ||||||
| G338.350+0.221 | 6.9 | a | WR76-10 (4.7) | n | |||
| G338.430+0.048 | 5.8 | a | Mercer 81 | WR76-2 (3.5), WR76-3 (3.5), WR76-4 (3.5) | o | ||
| WR76-5 (3.5), WR76-6 (3.5), WR76-7 (3.5) | o | ||||||
| WR76-8 (3.5), WR76-9 (3.5) | o | ||||||
| G338.911+0.615 | 4.4 | 3.8 | a | WR76 (1.9) | h |
(a) Anderson et al. (2014); (b) Mauerhan, Van Dyk & Morris (2009); (c) Chené et al. (2013); (d) Shara et al. (2009); (e) Hadfield et al. (2007); (f) Kurtev et al. (2007); (g) Mauerhan et al. (2011); (h) van der Hucht (2001); (i) Davies et al. (2012b); (j) Chené et al. (2015); (k) Marston et al. (2013); (l) Roman-Lopes (2011); (m) Wachter et al. (2010); (n) Shara et al. (2012); (o) Davies et al. (2012a); (p) this work.
aAlternatively WR62-2 and WR62-1 may be associated with WISE H ii region G317.236+0.516.
Galactic WR stars coincident with star-forming regions in the range 298° ≤ l ≤ 340°. We consider a WR star to be associated with a star-forming region (Anderson et al. 2014, WISE v1.4) if |$r \le 1.5 R_{\rm {\rm H}\,\small {ii}}$|, although some WR stars will doubtless be foreground sources, such that 53/206 (=26 per cent) WR stars associated with star-forming regions represents a strict upper limit.
| WISE . | d . | |$R_{}{\rm H}\,\small {ii}$| . | Ref . | Cluster? . | WN (r, arcmin) . | WC (r, arcmin) . | Ref . |
|---|---|---|---|---|---|---|---|
| H ii . | kpc . | arcmin . | . | . | . | . | . |
| G298.224−0.334 | 11.1 | 5.0 | a | WR46-7 (5), WR46-18 (8) | b, p | ||
| G298.529−0.251 | 10.5 | 16.2 | a | VVV CL 011 | WR46-8 (15.6), WR46-9 (3.5), WR46-17 (4.9) | WR46-10 (7.6) | b, c, d, e |
| WR46-15 (16.9), WR46-2 (22.4) | g | ||||||
| G298.862−0.432 | 10.7 | 4.8 | a | Mercer 30 | WR46-3 (6.6), WR46-4 (6.6), WR46-5 (6.6), | f | |
| WR46-6 (6.6) | f | ||||||
| G302.503−0.762 | 12.1 | 4.2 | a | WR47b (4.0) | h | ||
| G302.631+0.030 | 4.6 | 14.3 | a | WR47-1 (18.9) | e | ||
| G303.445−0.745 | 12.5 | 7.2 | a | WR47-2 (2.6) | d | ||
| G305.233+0.110 | 4.9 | 11.3 | a | Danks 1/2 | WR48-6 (5.5), WR48-10 (6.5), WR48-7 (7.7) | WR48-1 (8.6), WR48-3 (6.0) | e, g, h, i |
| WR48-9 (6.8), WR48-8 (6.8) | WR48-4 (8.2), WR48a (8.4) | h, i | |||||
| WR48-2 (10.3) | b | ||||||
| G305.322−0.255 | 4.9 | 13.4 | a | WR48-5 (4.7) | h | ||
| G311.991+0.219 | 6.0 | a | VVV CL 036 | WR60-6 (7.8) | c | ||
| G317.030+0.028a | 24.4 | a | VVV CL 041 | WR62-2 (15.7), WR62-1 (19.4), WR63 (34) | h, j | ||
| G321.015−0.527 | 4.1 | 4.0 | a | WR67-3 (6.1) | k | ||
| G321.115−0.546 | 3.8 | 4.2 | a | WR67-1 (1.8) | l | ||
| G326.474−0.292 | 20.9 | a | WR70-5 (17) | m | |||
| G327.824+0.117 | 7.2 | 3.9 | a | WR70-6 (5.2) | g | ||
| G331.020−0.143 | 3.8 | a | WR72-4 (3.5) | n | |||
| G335.794+0.153 | 13.7 | a | VVV CL 073 | WR75-6 (19.7), WR75-25 (6.1), WR75-26 (6.1) | WR75b (16.1), WR75-15 (12.4) | h | |
| WR75-16 (4.2) | n | ||||||
| G336.446−0.198 | 10.4 | a | WR75-9 (11.7), WR75-21 (10.3) | n | |||
| WR75-5 (14.3) | d | ||||||
| G338.350+0.221 | 6.9 | a | WR76-10 (4.7) | n | |||
| G338.430+0.048 | 5.8 | a | Mercer 81 | WR76-2 (3.5), WR76-3 (3.5), WR76-4 (3.5) | o | ||
| WR76-5 (3.5), WR76-6 (3.5), WR76-7 (3.5) | o | ||||||
| WR76-8 (3.5), WR76-9 (3.5) | o | ||||||
| G338.911+0.615 | 4.4 | 3.8 | a | WR76 (1.9) | h |
| WISE . | d . | |$R_{}{\rm H}\,\small {ii}$| . | Ref . | Cluster? . | WN (r, arcmin) . | WC (r, arcmin) . | Ref . |
|---|---|---|---|---|---|---|---|
| H ii . | kpc . | arcmin . | . | . | . | . | . |
| G298.224−0.334 | 11.1 | 5.0 | a | WR46-7 (5), WR46-18 (8) | b, p | ||
| G298.529−0.251 | 10.5 | 16.2 | a | VVV CL 011 | WR46-8 (15.6), WR46-9 (3.5), WR46-17 (4.9) | WR46-10 (7.6) | b, c, d, e |
| WR46-15 (16.9), WR46-2 (22.4) | g | ||||||
| G298.862−0.432 | 10.7 | 4.8 | a | Mercer 30 | WR46-3 (6.6), WR46-4 (6.6), WR46-5 (6.6), | f | |
| WR46-6 (6.6) | f | ||||||
| G302.503−0.762 | 12.1 | 4.2 | a | WR47b (4.0) | h | ||
| G302.631+0.030 | 4.6 | 14.3 | a | WR47-1 (18.9) | e | ||
| G303.445−0.745 | 12.5 | 7.2 | a | WR47-2 (2.6) | d | ||
| G305.233+0.110 | 4.9 | 11.3 | a | Danks 1/2 | WR48-6 (5.5), WR48-10 (6.5), WR48-7 (7.7) | WR48-1 (8.6), WR48-3 (6.0) | e, g, h, i |
| WR48-9 (6.8), WR48-8 (6.8) | WR48-4 (8.2), WR48a (8.4) | h, i | |||||
| WR48-2 (10.3) | b | ||||||
| G305.322−0.255 | 4.9 | 13.4 | a | WR48-5 (4.7) | h | ||
| G311.991+0.219 | 6.0 | a | VVV CL 036 | WR60-6 (7.8) | c | ||
| G317.030+0.028a | 24.4 | a | VVV CL 041 | WR62-2 (15.7), WR62-1 (19.4), WR63 (34) | h, j | ||
| G321.015−0.527 | 4.1 | 4.0 | a | WR67-3 (6.1) | k | ||
| G321.115−0.546 | 3.8 | 4.2 | a | WR67-1 (1.8) | l | ||
| G326.474−0.292 | 20.9 | a | WR70-5 (17) | m | |||
| G327.824+0.117 | 7.2 | 3.9 | a | WR70-6 (5.2) | g | ||
| G331.020−0.143 | 3.8 | a | WR72-4 (3.5) | n | |||
| G335.794+0.153 | 13.7 | a | VVV CL 073 | WR75-6 (19.7), WR75-25 (6.1), WR75-26 (6.1) | WR75b (16.1), WR75-15 (12.4) | h | |
| WR75-16 (4.2) | n | ||||||
| G336.446−0.198 | 10.4 | a | WR75-9 (11.7), WR75-21 (10.3) | n | |||
| WR75-5 (14.3) | d | ||||||
| G338.350+0.221 | 6.9 | a | WR76-10 (4.7) | n | |||
| G338.430+0.048 | 5.8 | a | Mercer 81 | WR76-2 (3.5), WR76-3 (3.5), WR76-4 (3.5) | o | ||
| WR76-5 (3.5), WR76-6 (3.5), WR76-7 (3.5) | o | ||||||
| WR76-8 (3.5), WR76-9 (3.5) | o | ||||||
| G338.911+0.615 | 4.4 | 3.8 | a | WR76 (1.9) | h |
(a) Anderson et al. (2014); (b) Mauerhan, Van Dyk & Morris (2009); (c) Chené et al. (2013); (d) Shara et al. (2009); (e) Hadfield et al. (2007); (f) Kurtev et al. (2007); (g) Mauerhan et al. (2011); (h) van der Hucht (2001); (i) Davies et al. (2012b); (j) Chené et al. (2015); (k) Marston et al. (2013); (l) Roman-Lopes (2011); (m) Wachter et al. (2010); (n) Shara et al. (2012); (o) Davies et al. (2012a); (p) this work.
aAlternatively WR62-2 and WR62-1 may be associated with WISE H ii region G317.236+0.516.
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
