Table 10
Census stars with the highest ionising luminosities, wind luminosities and masses and their combined contribution to 30 Dor.
| ID | Star | SpT | r d | Q 0 | L SW |
| # | (pc) | (1049 ph s-1) | (1037erg s-1) | ||
| 10 stars with highest ionising luminosity | |||||
|
|
|||||
| 630 | R136a1 | WN 5h | 0.00 | 66.0 | 10.9 |
| 770 | Mk34 | WN 5h | 2.61 | 49.2 | 9.2 |
| 633 | R136a2 | WN 5h | 0.02 | 48.0 | 8.7 |
| 706 | R136c | WN 5h | 0.83 | 42.0 | 5.4 |
| 493 | R134 | WN 6(h) | 2.86 | 35.3 | 6.2 |
| 613 | R136a3 | WN 5h | 0.12 | 30.0 | 5.6 |
| 1001 | BAT99-122 | WN 5h | 71.71 | 25.0 | 5.5 |
| 580 | Mk 42 | O2 If* | 1.96 | 18.8 | 4.0 |
| 916 | BAT99-118 | WN 6h | 62.27 | 18.2 | 5.3 |
| 375 | BAT99-95 | WN 7h | 21.56 | 15.8 | 7.6 |
|
|
|||||
Total (% of  or
 ): |
348.3 (28%) | 68.4 (29%) | |||
| 10 stars with highest wind luminosity | |||||
|
|
|||||
| 630 | R136a1 | WN 5h | 0.00 | 66.0 | 10.9 |
| 543 | R140a1 | WC 4 | 12.43 | 6.6 | 9.7 |
| 762 | Mk33Sb | WC 5 | 2.90 | 6.3 | 9.4 |
| 770 | Mk34 | WN 5h | 2.61 | 49.2 | 9.2 |
| 633 | R136a2 | WN 5h | 0.02 | 48.0 | 8.7 |
| 375 | BAT99-95 | WN 7h | 21.6 | 15.8 | 7.6 |
| 493 | R134 | WN 6(h) | 2.86 | 35.3 | 6.2 |
| 613 | R136a3 | WN 5h | 0.12 | 30.0 | 5.6 |
| 1001 | BAT99-122 | WN 5h | 71.7 | 25.0 | 5.5 |
| 706 | R136c | WN 5h | 0.83 | 42.0 | 5.4 |
|
|
|||||
| Total (% of or
): |
324.2 (28%) | 78.2 (35%) | |||
| stars with Minit >100 M⊙ | |||||
|
|
|||||
| 630 | R136a1 | WN 5h | 0.00 | 66.0 | 10.9 |
| 770 | Mk34 | WN 5h | 2.61 | 49.2 | 9.2 |
| 633 | R136a2 | WN 5h | 0.02 | 48.0 | 8.7 |
| 706 | R136c | WN 5h | 0.83 | 42.0 | 5.4 |
| 493 | R134 | WN 6(h) | 2.86 | 35.3 | 6.2 |
| 613 | R136a3 | WN 5h | 0.12 | 30.0 | 5.6 |
| 1001 | BAT99-122 | WN 5h | 71.71 | 25.0 | 5.5 |
| 580 | Mk 42 | O2 If* | 1.96 | 18.8 | 4.0 |
| 916 | BAT99-118 | WN 6h | 62.27 | 18.2 | 5.3 |
| 375 | Mk35 | O2 If*/WN 5 | 3.07 | 15.6 | 1.7 |
|
|
|||||
| Total (% of or
): |
348.1 (28%) | 62.5 (28%) | |||
Notes. Entries given in bold are based on tailored W-R analyses (see Table B.1). Other entries rely either on the less reliable W-R star template method or the calibrations discussed in Sect. 6. For more reliable outputs for the Of/WN and WN stars, we direct the reader to Bestenlehner et al., (in prep.).
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