Table 6
Comparison of different best fitting dynamical models including NFW halos.
| β | ρs | rs | r200 |
|
M(r200)/LR | fDM < Re | fDM < 2Re | χ2 |
| [M⊙ pc-3] | [kpc] | [kpc] | [M⊙] | [M⊙/L⊙] | [%] | [%] | ||
|
|
||||||||
| Stars (ΥR = 3.01) + NFW (c = 5) | ||||||||
| 0.0 | 1.191 × 10-3 | 30 | 150 |
|
7.3 |
|
|
63.0 |
| 0.3 | 1.191 × 10-3 | 25 | 125 |
|
5.6 |
|
|
40.5 |
| MŁ | 1.191 × 10-3 | 1 | 5 | 1.4 + 1.9 × 107 | 3.1 | <1 | <1 | 54.5 |
|
|
||||||||
| Stars (ΥR = 3.01) + NFW (c = 10) | ||||||||
| 0.0 | 6.135 × 10-3 | 9 | 90 |
|
4.1 |
|
|
59.3 |
| 0.3 | 6.135 × 10-3 | 8 | 80 |
|
3.8 |
|
|
42.9 |
| MŁ | 6.135 × 10-3 | 1 | 10 | 0.11 + 7.3 × 109 | 3.1 | <1 | <1 | 54.5 |
Notes. Column 1 indicates the value for the anisotropy considered for the stellar population. MŁ indicates the Mamon & Łokas (2005b) anisotropy profile with parameters decribed in the text. Column 2 gives the characteristic density of the NFW halo, which comes from the chosen concentration as given in Eq. (20). Column 3 gives the best fitting scale radius for the chosen concentration. Columns 4 and 5 give the virial radius and mass of the DM halo, respectively. Masses are also indicated with their 1-σ confidence level. Column 6 indicates the virial M/L. Columns 7 and 8 give the DM fraction within 1 and 2 Re (using the effective radius given by Faber et al. 1989), defined as fDM = MNFW/(MNFW + M⋆), where the baryonic mass is given by Eq. (6). Column 9 gives the χ2 for each model.
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