  In a companion paper, we have conducted an in-depth analysis of radial
velocity jitter of over 600 stars, examining the astrophysical origins
including stellar granulation, oscillation, and magnetic activity. In this
paper, we highlight a subsample of those stars, specifically the main sequence
and "retired" F stars -- which we refer to as "MSRF" stars -- that show low
levels of RV jitter ($<10$ m/s). We describe the observational signatures of
these stars that allow them to be identified in radial velocity planet
programs, for instance those performing follow-up of transiting planets
discovered by TESS. We introduce a "jitter metric" that combines the two
competing effects of RV jitter with age: activity and convection. Using
thresholds in the jitter metric, we can select both "complete" and "pure"
samples of low jitter F stars. We also provide recipes for identifying these
stars using only Gaia colors and magnitudes. Finally, we describe a region in
the Gaia color-magnitude diagram where low jitter F stars are most highly
concentrated. By fitting a 9th order polynomial to the Gaia main sequence, we
use the height above the main sequence as a proxy for evolution, allowing for a
crude selection of low jitter MSRF stars when activity measurements are
otherwise unavailable.
