Sagittarius & 5.6 & -14.1 & 24.0 & 140.0 & 150.3 & 16.4 & 169.2\
Sgr DIG UKS1927-177& 21.1 & -16.3 & 1060.0 & -79.0 & -68.8 & 1052.8 & 0.3\
NGC 6822 DDO209& 25.3 & -18.4 & 490.0 & -54.0 & -44.5 & 483.2 & 36.6\
DDO210 Aquarius& 34.0 & -31.3 & 800.0 & -137.0 & -127.8 & 794.4 & -32.2\
IC 5152 & 343.9 & -50.2 & 1590.0 & 124.0 & 123.0 & 1585.1 & 87.5\
UKS2323-326 UGCA438& 11.9 & -70.9 & 1320.0 & 62.0 & 62.1 & 1317.5 & 75.6\
Pegasus DDO216& 94.8 & -43.5 & 955.0 & -182.0 & -177.9 & 955.5 & -33.3\
UGC 4879 VV124& 164.7 & 42.9 & 1100.0 & -80.0 & -81.3 & 1105.7 & -42.5\

KL sample: Kulessa and Lynden-Bell (1992). K sample: Kochanek (1996): Globular clusters and satellite galaxies. SF sample: Local Group galaxies from Sawa and Fujimoto (2006), whose list is mainly based on Mateo (1998). See the literature for original references. VV124: Kopylov et al. (2008).

\[tab1-con\]

In figures and \[fig-150\] and \[fig-vgc\] we show the calculated rotation curves for the three dark halo models: isothermal, NFW and Burkert profiles. The dark halo models are so chosen that 