Table 5
Derived physical parameters from the best-fit two-component models.
| NGC 104 | NGC 5139 | |||
| RG | no RG | RG | no RG | |
|
|
||||
| r tr | 71 | 153 | 90 | 89 |
| R c,1 | 34.1 | 16.3 | 176 | 155 |
| R c,2 | 21.1 | 10.2 | 133 | 117 |
| r M,1 | 8.7 | 5.2 | 11.7 | 10.4 |
| r M,2 | 3.3 | 1.8 | 7.9 | 7.0 |
| M 1 | 7.0 | 5.5 | 25.6 | 22.7 |
| M 2 | 2.3 | 1.8 | 8.5 | 7.5 |
| log ρ0,1 | 4.3 | 5.1 | 3.19 | 3.30 |
| log ρ0,2 | 4.8 | 5.6 | 3.11 | 3.21 |
| (M/L)V,1 | 3.76 | 1.13 | 5.31 | 1.53 |
| (M/L)V,2 | 0.83 | / | 1.18 | / |
Notes. For two clusters considered either by including or by not including RG stars in the heavier component, we provide the relevant physical quantities relative to the light component 1 and the heavy component 2. The truncation radius rtr and the half-mass radius are expressed in pc; the core radius Rc is expressed in units of arcsec. The total mass is expressed in units of 105M⊙ and the central mass density ρ0 in M⊙ pc-3. Finally, the mass-to-light ratio is given in solar units M⊙/L⊙.
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