Table 1
Number ratios for the Quintuplet stars in comparison to other Galactic center clusters.
| NWR | NWR:NO | NWC:NWN | NRSG:NWR | NWNE:NWNL | NWC,binary:NWC | NWN,binary:NWN | |||||||||||||
|
|
|||||||||||||||||||
| Quintuplet* | 21 | –:– | 13:8 | 1:21 | 1:7 | 5+2?:13 | 1?:7 | ||||||||||||
| Quintuplet** | 14 | 14:84 | 9:5 | 1:14 | 0:5 | 5+2?:9 | 1?:5 | ||||||||||||
| Archesa | 17 | 13:15 | 0:17 | –:– | 0:15 | –:– | 2+5?:17 | ||||||||||||
| Central Parsecb | 42 | 30:40 | 24:18 | –:– | 3:12 | 10?:24 | 2:18 | ||||||||||||
| Westerlund 1c | 24 | 24:57 | 8:16 | 10:24 | 12:4 | 6?: 8 | 3+6?:16 | ||||||||||||
|
|
|||||||||||||||||||
| Milky Wayd | 63 | –:– | 38:25 | –:– | 33:26 | 19:38 | 6:25 | ||||||||||||
Notes. Numbers of O stars are lower limits from Martins et al. (2008, Arches), Paumard et al. (2006, Central Parsec), Negueruela et al. (2010, Wd 1); WR numbers are based on van der Hucht (2006) unless otherwise indicated. WC stars showing dust in their spectra (WCd or WCLd classification) are considered binary candidates. Note that the number stars listed in the different columns for each clusters might slightly vary in dependence of the reference and the therein used subsample of stars (see text for details).
WR stars from van der Hucht (2006) corrected for the WR stars newly identified in Liermann et al. (2009): LHO 110 – WN9h, LHO 76 and LHO 79 both WC9d; number of RSGs estimated from the corrected sample of late-type stars; five WCd stars resolved as pinwheel binaries by Tuthill et al. (2006), two further candidates based on WCd classification.
Numbers limited to the LHO field of view of about 40 ′′ × 40 ′′covering the center of the Quintuplet cluster.
Classification as WNL or WNE from Cotera et al. (1999) and Martins et al. (2008); two WN binaries from non-thermal, variable radio plus X-ray detection, further 5 candidates based on either variable radio flux or X-ray detection (van der Hucht 2006).
Classification as WNL or WNE from Paumard et al. (2006), Martins et al. (2008); two Of/WN9 stars detected with radial velocity variations (Martins et al. 2006).
NRSG includes four RSGs by Mengel & Tacconi-Garman (2007) and six yellow hypergiants by Clark et al. (2005); classification as WNL or WNE and WR binaries taken from Crowther et al. (2006).
Numbers from van der Hucht (2001), Table 29. NWNE:NWNL ratio from Hamann et al. (2006).
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