## 5. Mass-to-light ratiosIf we assume that the clusters are reasonably well represented by King models then, following Queloz et al. (1995), we can compute the total mass using Values of , and The in Eq. 3 refers to the
An alternative to the somewhat model-specific method used above is a straightforward application of the Virial theorem: where we have assumed an isotropic velocity distribution and (Spitzer 1987), where is the half-mass radius. The masses computed using this equation are given in column 8 of Table 2. Owing to M 31's low Galactic latitude, obscuration of the
globular clusters by foreground Galactic dust varies significantly
from one side of M 31 to the other. Using the extinction maps of
Burstein & Heiles (1982), E(B-V) was estimated for each cluster
and is given in column 9 of Table 2. Using the The ratios given in Table 2 are remarkably similar to those typically found in Galactic globulars (Pryor & Meylan 1993). Bo158 and 225 might seem a trifle high, but we note that both these clusters have only ground-based measurements of . It is entirely possible that these estimates of suffer from incomplete removal of the effects of seeing and are consequently too high. The largest source of uncertainty in is generally in the estimation of , being of the order of 15% even for the HST-imaged clusters. Uncertainties in the magnitude estimates of Battistini et al., in our estimates of the local extinction, and in the velocity dispersion measurements contribute each to the final uncertainty. Bo343 and 358 are exceptions to this general rule, having reasonably well-measured core radii, but rather less well-determined velocity dispersions. The formally estimated uncertainties in are for those clusters observed with HST, and probably closer to 50% for those clusters imaged only from the ground. Table 2 shows that the ratios derived with Eq. 4(column 11) are systematically 50% larger than those obtained with Eq. 3 (column 10). This gives a rough idea on how model dependent are our estimates. © European Southern Observatory (ESO) 1997 Online publication: June 30, 1998 |