Table 1.
Fornax globular clusters.
| CDM τ | FDM τ | |||||
|---|---|---|---|---|---|---|
| Hui+17 | Here | Hui+17 | Here | Here | ||
| R | MGC | – | – | m22 = 3 | 3 | 20 |
| [kpc] | [105 M⊙] | [Gyr] | [Gyr] | |||
| 1.85 | 0.37 | 112 | 25 | 215 | 393 | 176 |
| 1.21 | 1.82 | 9.7 | 2.56 | 12 | 59 | 26 |
| 0.50 | 3.63 | 0.62 | 0.30 | 2.2 | 19 | 11 |
| 0.28 | 1.32 | 0.37 | 0.24 | 10 | 24 | 13 |
| 1.65 | 1.78 | 21.3 | 5.08 | 31 | 74 | 34 |
Notes. From left to right, the columns report the observed projected distances and masses of the five GCs, followed by a comparison between the infall times τ computed in this work and those from Hui et al. (2017), under both CDM and FDM assumptions for the Fornax halo. We have tested two fixed FDM particle masses of m22 = 3 and 20. The infall times τ correspond to the time for the GC to fall below 0.14 kpc, which corresponds to 10% of the core radius of the FDM halo.
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