Table 1
The slope of the DM-mass-luminosity relation of dSph satellite galaxies.
| data | κ | Radius | M 0 |
| [pc] | [107 M⊙] | ||
|
|
|||
| Observational: | |||
| 1 | +0.02 ± 0.03 | 300 | 1.02 ± 0.39 |
| 2 | +0.02 ± 0.03 | 300 | 1.01 ± 0.40 |
| 3 | +0.01 ± 0.03 | 300 | 1.09 ± 0.44 |
| *4 | −0.03 ± 0.05 | 600 | 6.9 ± 4.9 |
|
|
|||
| DM Models: | |||
| A: feedback | 0.21 | 300 | – |
| B1: re-ionisation, SPS | 0.15 ± 0.02 | 300 | 0.24 ± 0.06 |
| B2: re-ionisation | 0.17 ± 0.01 | 300 | 0.18 ± 0.02 |
| C: SAM | 0.42 ± 0.02 | 300 | 2.0 ± 0.9 |
| *D: Aq-D-HR | 0.17 ± 0.02 | 600 | 0.41 ± 0.14 |
| E1: 1keV(WDM) | 0.23 ± 0.04 | 300 | 0.069 ± 0.045 |
| E2: 5keV(WDM) | 0.12 ± 0.02 | 300 | 0.43 ± 0.081 |
| F: Aq-infall | 0.13 ± 0.01 | 300 | 0.32 ± 0.022 |
Notes. Fitted parameters for Eq. (1).Fits to κ = 0.35/η: data 1–4 are observational values, data A–F are models (see Sect. 2).1: our fit to S08 (who give central 300 pc masses, 18 satellites, their Fig. 1). 2: our fit to S08 without Seg.1 (faintest satellite, i.e. 17 satellites, their Fig. 1). 3: our fit to S08 without Seg.1 and without Hercules (i.e. 16 satellites, their Fig. 1). 4: our fit to the observational data plotted by Okamoto & Frenk (2009) (who give central 600 pc masses, only 8 satellites, their Fig. 1). A: Dekel & Silk (1986); Dekel & Woo (2003), stellar feedback (Eq. (5)). B1: our fit to Busha et al. (2010), their SPS model. B2: our fit to Busha et al. (2010), inhomogeneous re-ionisation model. C: our fit to Macciò et al. (2010), semi-analytical modelling (SAM), fit is for LV > 3 × 105LV, ⊙ . D: our fit to Okamoto & Frenk (2009) (Aq-D-HR). E1: our fit to the 1keV WDM model of Macciò & Fontanot (2010). E2: our fit to the 5keV WDM model of Macciò & Fontanot (2010). F: our fit to the Aquarius sub-halo-infall models of Cooper et al. (2010). *: the entries with an asterisk are for the central 600 pc radius region.
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