Notes. Data for the MW satellites used for fitting the DoS. Seg 1 and 2 (marked in italics) are included in this list for reference, but they have not been included in the fitting because they appear to be diffuse star clusters (Niederste-Ostholt et al. 2009). The positions are given both in Heliocentric coordinates (right ascension α₂₀₀₀, declination δ₂₀₀₀, and Heliocentric distance r_helio for epoch J2000.0) and in Galactocentric coordinates assuming the Sun to have a distance of 8.5 kpc from the MW centre. l_MW gives the Galactic longitude with 0° pointing from the Galactic centre to the Sun. b_MW is the latitude as seen from the Galactic centre and r_MW the radial distance from the centre of the MW. The coordinates were obtained using data from the references listed in the column labelled Ref., where more than one source is given, the distances to the satellites were obtained by error-weighted averaging over the available measurements. The satellite’s line-of-sight velocities with respect to the Galactic standard of rest (GSR) are calculated assuming the Sun to move into the direction l = 90°, b = 0° (in Heliocentric, Galactic coordinates) with a velocity of either 220 km s^-1 () or 250 km^-1 (). The measurement-uncertainties for the radial velocities reported in the respective papers (referred to in column Ref.) are reproduced in the column labelled Δv. Finally, L_V gives the satellite luminosities in the photometric V-band; again uncertainty-weighted averages are quoted when more than one reference is given in column Ref. Data marked with † have measured proper motions, listed in Table 1 of Metz et al. (2008). ^∗: As no distance uncertainties for Pisces II are available in the literature, the error is estimated to be 20 percent of the distance.

References. 1: Adén et al. (2009a), 2: Belokurov et al. (2006), 3: Belokurov et al. (2007), 4: Belokurov et al. (2008), 5: Belokurov et al. (2009), 6: Belokurov et al. (2010), 7: Coleman et al. (2007b), 8: de Jong et al. (2008), 9: de Jong et al. (2010), 10: Dall’Ora et al. (2006), 11: Geha et al. (2009), 12: Greco et al. (2008), 13: Ibata et al. (2006), 14: Koch et al. (2009), 15: Kollmeier et al. (2009), 16: Kuehn et al. (2008), 17: Martin et al. (2008a), 18: Martin et al. (2008b), 19: Mateo (1998), 20: Moretti et al. (2009), 21: Muñoz et al. (2006), 22: Muñoz et al. (2010), 23: Musella et al. (2009), 24: Okamoto et al. (2008), 25: Sakamoto & Hasegawa (2006), 26: Sand et al. (2009), 27: Sand et al. (2010), 28: Siegel (2006), 29: Simon & Geha (2007), 30: Walsh et al. (2007), 31: Walsh et al. (2008), 32: Watkins et al. (2009), 33: Willman et al. (2005a), 34: Willman et al. (2005b), 35: Zucker et al. (2006a), 36: Zucker et al. (2006b), 37: van den Bergh (1999).