Table 5:
Parameters of the dark matter halos. The first column labels
the models. The mass-to-light ratio
M/LR and
the dark matter fraction are calculated for two radii
(
and
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
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.
# |
 |
 |
 |
rms |
 |
 |
 |
 |
M/LR |
 |
M/LR |
 |
|
|
[kpc] |
![$[{M}_{\odot}~{\rm pc}^{-3}]$](/articles/aa/full/2006/44/aa3134-05/img215.gif) |
![$[{\rm km~s}^{-1}] $](/articles/aa/full/2006/44/aa3134-05/img82.gif) |
[kpc] |
[
] |
 |
![$ [10^{11}~{M}_{\odot}]$](/articles/aa/full/2006/44/aa3134-05/img217.gif) |
 |
 |
|
M/LR= 6.8,
(cf. Fig. 13, left panels) |
1 |
-2.0 |
5 |
0.12 |
23 |
207 |
0.52 |
41.4 |
5.5 |
10.9 |
0.37 |
9.6 |
0.29 |
2 |
-0.5 |
10 |
0.033 |
20 |
255 |
0.96 |
25.5 |
5.5 |
12.0 |
0.43 |
9.4 |
0.27 |
3 |
0 |
40 |
0.003 |
21 |
395 |
3.6 |
9.9 |
6.6 |
13.1 |
0.48 |
8.4 |
0.19 |
4 |
0.5 |
120 |
0.00075 |
26 |
655 |
16.6 |
5.5 |
7.2 |
14.3 |
0.52 |
8.2 |
0.17 |
5 |
1.0 |
240 |
0.00050 |
46 |
1100 |
77.9 |
4.57 |
9.2 |
18.3 |
0.63 |
8.7 |
0.22 |
|
M/LR= 4.3,
(cf. Fig. 14, left panels) |
6 |
- 2.0 |
5 |
0.195 |
22 |
248 |
0.90 |
49.6 |
5.5 |
10.9 |
0.61 |
8.9 |
0.52 |
7 |
- 0.5 |
5 |
0.230 |
20 |
264 |
1.01 |
52.8 |
6.1 |
12.1 |
0.64 |
9.7 |
0.56 |
8 |
0 |
20 |
0.0135 |
20 |
358 |
2.7 |
17.9 |
5.3 |
10.6 |
0.59 |
5.9 |
0.27 |
9 |
0.5 |
120 |
0.00100 |
25 |
743 |
24.1 |
6.2 |
7.2 |
14.3 |
0.70 |
6.2 |
0.30 |
10 |
1.0 |
120 |
0.00145 |
45 |
870 |
39.0 |
7.3 |
9.4 |
18.7 |
0.77 |
7.0 |
0.37 |
|
M/LR= 6.8,
(cf. Fig. 13, right panels) |
11 |
- 2.0 |
120 |
0.0012 |
18 |
803 |
30.5 |
6.7 |
9.4 |
18.7 |
0.64 |
9.0 |
0.25 |
12 |
- 0.5 |
80 |
0.0019 |
25 |
650 |
16.0 |
8.1 |
9.0 |
26.7 |
0.75 |
10.5 |
0.35 |
13 |
0.0 |
120 |
0.0011 |
32 |
773 |
27.2 |
6.4 |
9.0 |
17.7 |
0.62 |
8.8 |
0.23 |
14 |
0.5 |
120 |
0.0012 |
47 |
803 |
30.5 |
6.7 |
9.5 |
18.7 |
0.64 |
9.0 |
0.25 |
|
M/LR= 4.3,
(cf. Fig. 14, right panels) |
15 |
- 2.0 |
80 |
0.0023 |
16 |
703 |
20.4 |
8.8 |
9.0 |
18.0 |
0.76 |
7.1 |
0.39 |
16 |
- 0.5 |
120 |
0.0011 |
24 |
774 |
27.3 |
6.5 |
7.7 |
15.2 |
0.72 |
6.3 |
0.32 |
17 |
0.0 |
120 |
0.00135 |
27 |
845 |
35.4 |
7.0 |
9.0 |
17.7 |
0.76 |
6.8 |
0.37 |
18 |
0.5 |
120 |
0.0014 |
42 |
858 |
37.0 |
7.15 |
9.2 |
18.2 |
0.76 |
6.9 |
0.38 |