Our close sample. Hertzsprung‐Russell diagram for Hipparcos stars closer than 25 pc. Small black dots are Hipparcos stars not being monitored for possible companions by one of the eight high‐precision Doppler surveys considered here (Lineweaver & Grether 2003). Larger blue dots are the subset of Hipparcos stars that are being monitored ("target stars") but have as yet no known planetary companions. The still larger red dots are the subset of target stars hosting detected planets ("planet host stars"), and the green dots are those hosts with larger mass (﹩M_{2}> 13M_{\mathrm{J}\,}﹩) companions ("other host stars"). Only companions in our less biased sample (﹩P< 5﹩ yr and ﹩M_{2}> 10^{-3}\ M_{\odot }﹩) are shown (see § 2.2). Our Sun is shown as the black cross. The gray parallelogram is the region of ﹩M_{V}﹩‐﹩( B-V) ﹩ space that contains the highest fraction (triangles) of Hipparcos stars that are being monitored for exoplanets. This Sun‐like region—late F to early K type main‐sequence stars—contains our Hipparcos Sun‐like Stars. The target fraction needs to be as high as possible to minimize selection effects potentially associated with companion frequency. The target fraction is calculated from the number of main‐sequence stars, i.e., the number of stars in each bin between the two dashed lines. This plot contains 1509 Hipparcos stars, of which 627 are Doppler target stars. The Sun‐like region contains 464 Hipparcos stars, of which 384 are target stars. Thus, the target fraction in the Sun‐like gray parallelogram is ~83% (=384/464).