All Tables

Table 1: NGC 4636 basic data compiled from the literature (1) NED, (2) Tonry et al. (2001), (3) this work, (4) R3C, (5) Dirsch et al. (2005), (6) Bender et al. (1994), (7) Idiart et al. (2003), (8) Forman et al. (1985), and (9) Loewenstein et al. (2001).
Table 2: Summary of observations (ESO program ID 69.B-0366(B)). The seeing values were determined from the acquisition images taken just before the MXU exposures.
Table 3: Basic properties of the globular cluster sample.
Table 4: Projected velocity dispersion as a function of projected galactocentric radius. The upper section shows the values for all, the blue, and the red clusters. The dispersions for the corresponding error-selected samples are listed in the lower section. The data are shown in Fig. 11. The values in brackets are those obtained when omitting the two (blue) GCs with velocities above $1400~{\rm km~s}^{-1}$ .
Table 5: Parameters of the dark matter halos. The first column labels the models. The mass-to-light ratio M/L_R and the dark matter fraction are calculated for two radii ( $7.5~{\rm kpc} \simeq R_{{\rm eff}}$ and $30~\rm kpc$ is the radius within which the GCs used in the analysis are found). From the NFW parameters of our model halos, we calculate the virial radius, the virial mass, and the concentration parameter ${{(c_{\rm {vir}}= {R}_{{\rm vir}}/r_{{\rm dark}})}}$ using the definitions of Bullock et al. (2001). Then we give the total mass within 30 kpc, the mass-to-light ratios (R-band), and the dark matter fraction within 30 kpc and 7.5 kpc (effective radius). Note that the virial quantities were calculated for the dark halos without adding the stellar component. Thus, the virial masses presented below are lower limits.
Table A.1: Globular cluster data.
Table A.2: Star data.