 for a survey is defined to be the number of galaxies with an accurate redshift measurement per unit of comoving volume and *not* the number of galaxies targeted down to an arbitrary magnitude limit.

[^2]: We adopt this simplified color-cut to be more restrictive at the faint end of the red sequence, where dusty star-forming galaxies are more prominent [@lotz08]. However, using a luminosity-dependent color-cut [e.g., Equation 19 of @willmer06] yields no significant changes in our results.

[^3]: Limiting the sample to those sources with $\sigma_{n} < 0.75$ excludes very few (only $2$ out of $625$) objects. Removing this selection criterion or making it more restrictive (e.g., $\sigma_{n} < 0.5$) yields no significant changes in our results.

[^4]: Selecting the top 10% or 20% of the environment distribution yields similar results.

[^5]: Note that the two-sided probability for the WMW $U$ test is given by doubling the one-sided probability. Here, we report only the one-sided probability.

[^6]: The average sizes for cluster, group, and field early-types as given in Table 1 of @raichoor11 are all consistent at the $1\sigma$ level.


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abstract: 'We present the first Doppler images of the active eclipsing binary system SZ Psc, based on the high-resolution spectral data sets obtained in 2004 November and 2006 September–December. The least-squares deconvolution technique was applied to derive high signal-to-noise profiles from the observed spectra of SZ Psc. Absorption features contributed by a third component of the system were detected in the LSD profiles at all observed phases. We estimated the mass and period of the third component to be about $0.9 M_{\odot}$ and $1283 \pm 10$ d, respectively. After removing the contribution of the third body from the LSD profiles, we derived the surface maps of SZ Psc. The resulting Doppler images indicate significant starspot activities on the surface of the K subgiant component. The distributions of starspots are more complex than that revealed by previous photometric stu