set are between 7.5-9.5 in the $V$ optical band and after preliminary screening with the FEROS spectrograph ([@jenkins08]), we predominantly selected chromospherically quiet stars, and those that are metal-rich (primary sample having log$R'_{\rm{HK}}$ indices $\le$ -4.9 dex and \[Fe/H\] $\ge$ +0.1 dex, with some stars outside of these selection limits to use as comparisons). The positions of the stars reported here on an HR-diagram are shown in the inset plot in Fig. \[hr\_plot\]. The Y2 isomass tracks are also shown ([@demarque04]) for masses of 1.0-1.3 , increasing in mass towards higher luminosities, and with a fixed metallicity of +0.2 dex. The characteristics of the targets we discuss in this work are shown in Table \[tab:values\].

Since the planets reported here are gas giants, the radial velocity signals of these stars are fairly large, and hence one might expect that we can detect frequencies for all of them using standard periodogram analyses to hunt for power peaks in the Fourier power spectrum, or minimum mean square error (MMSE) spectrum (e.g. [@dawson10]; [@jenkins14a]). However, the search for the best solutions can be complicated, particularly for combined data sets from independent spectrographs because the sets have different baselines, data samplings, and uncertainties that 