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tokens: . Figure 2.40. SDSSJ2324+0105. The observational data, B-spline-subtracted image, predicted lensed image, final residual, and background source model are shown from left to right, respectively. Images are orientated such that north is up and East is to the left. For each system, the results of the two source models are split into two rows with the parameterized source model on the top and the pixelized source model on the bottom. The white lines in the last panels are the caustics of the lens model. The source plane panels are magnified by factors from 2 to 32 relative to the image plane panel as indicated in each panel. The color bars indicate the intensity levels in units of electrons per second per pixel 2 . Table 2 Strong-lens Model Parameters of the 40 S4TM Grade-A Lenses Note. Column 1 is the SDSS system name. Columns 2–4 are the Einstein radius, minor-to-major axis ratio, and major-axis position angle of the SIE component with respect to the north. Column 5 indicates the number of Sérsic components used. Column 6 is the average magnification. Column 7 is the total projected mass within the Einstein radius from the best-fit lens model. Column 8 is the estimated stellar mass assuming a Chabrier IMF from Shu et al. ( 2015 ). Column 9 is the inferred dark-matter fraction within half of the half-light radius. Column 10 provides the χ 2 value and the dof. 5. Discussion The S4TM survey is optimized to select strong-lens systems with relatively lower-mass lens galaxies as a complementary sample to the SLACS sample. In Figure 3 , we compare the stellar velocity dispersion, Einstein radius, total projected mass within the Einstein radius, and stellar mass between the two lens samples. The SLACS sample refers to the 63 grade-A lenses with lens models in Bolton et al. ( 2008a ). Figure 3. Distributions of the stellar velocity dispersion, Einstein radius, total enclosed mass within the Einstein radius, and stellar mass for the S4TM (solid histograms) and the SLACS (dashed histograms) lens samples. The stellar mass is derived from HST F814W-band photometry assuming a Chabrier IMF as explained in Shu et al. ( 2015 ). The distribution of the stellar velocity dispersions σ SDSS of the S4TM sample has a strong peak at about 200 km s −1 and declines rapidly on both ends. On the other hand, the distribution of σ SDSS of the SLACS sample is almost flat from 200 to 320 km s −1 . As a comparison, the median σ SDSS of the S4TM sample is 203 km s −1 , while it is 243 km s −1 for the SLACS sample. The median Einstein radius of the S4TM sample is 100, almost 15% smaller than that of the SLACS sample (117). The distributions of the Einstein radii for the two samples further suggest that the S4TM sample is more abundant in systems with Einstein radii smaller than 08 (12/40 versus 3/63) and lack systems with Einstein radii larger than 12 (8/40 versus 30/63). We basically expect the distributions of M Ein to be similar to those of b SIE because Σ crit , which is