Table 2.
Best-fit parameters for the relations between the AM of the DM halo and that of the stellar dynamical components.
| log(Jh) = α + β⋅log(Jz) |
log(Jh(< 0.15 r200)) = α + β⋅log(Jz) |
|||||||
|---|---|---|---|---|---|---|---|---|
| Component | α | β | rP | rms | α | β | rP | rms |
| Halos | 9.50 ± 0.42 | 0.46 ± 0.04 | 0.97 | 0.13 | 9.16 ± 0.82 | 0.39 ± 0.07 | 0.87 | 0.26 |
| Disks | 7.03 ± 0.88 | 0.62 ± 0.07 | 0.95 | 0.17 | 6.19 ± 0.35 | 0.58 ± 0.03 | 0.99 | 0.07 |
| Thin disks | 3.83 ± 1.58 | 0.87 ± 0.13 | 0.90 | 0.30 | 2.27 ± 1.75 | 0.90 ± 0.14 | 0.89 | 0.33 |
| Thick disks | 4.74 ± 1.47 | 0.81 ± 0.12 | 0.90 | 0.30 | 3.24 ± 1.64 | 0.84 ± 0.13 | 0.89 | 0.34 |
| Combined disks | 6.15 ± 0.92 | 0.68 ± 0.07 | 0.90 | 0.29 | 4.77 ± 0.91 | 0.70 ± 0.07 | 0.90 | 0.28 |
Notes. The highlighted rows indicate the best stellar component to trace the DM halo angular momentum (stellar halo) and the most practical one given the current observational possibilities (combined disks).
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