Location and kinematics of our sample stars (green and purple squares) compared to expectations for the Sag stream from the Law & Majewski (2010) model (gray points; only particles either still bound or stripped in the most recent five pericentric passages are plotted) and from various sources of observations (see legend and main text). The top panel shows the distribution as a function of longitude Λ_⊙ and latitude B_⊙ in a reference system where the equator is aligned with the Sag stream trailing tail (see Majewski et al. 2003) but with modifications proposed by Belokurov et al. (2014), that is Λ increasing in the direction of the Sag motion and latitude axis pointing to the North Galactic Pole. Middle: heliocentric distance versus Λ_⊙. Bottom: galactic standard of Rest velocities versus Λ_⊙. Our targets are shown with large filled squares (green and purple squares) having latitude | B_⊙ | smaller and larger than 30 deg, respectively; green squares with purple border show the sample stars with v_GSR incompatible with the expectations/observations of the Sag stream), while the trend derived in the literature using the tracers as in the legend are shown with small (red, blue, and orange) squares with errorbars (see main text for the references to the original articles). We note that our v_GSR and those for the Sag particles in the LM10 model have been calculated assuming R_⊙ = 8 kpc, a Local Standard of Rest (LSR) velocity of 220  km s^-1 and the solar motion from Dehnen & Binney (1998); in this figure, a factor has been applied to both our velocities and those from the particles in the LM10 model to correct for the different solar motion and v_LSR used in Belokurov et al. (2014).