are shown phase folded to highlight the phase coverage we have observed. We did not show the posteriors for the residuals to any of the systems (more than a single planet model fit) unless we detected a unique solution that relates to a second Doppler signal.

HD9174
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HD9174 is classed as a G8 subgiant star in the Hipparcos catalogue ([@perryman97]) since it has a distance from the main sequence ($\Delta M_V$) of 1.5 and a $B-V$ colour of 0.76. The star is also extremely metal-rich, with an \[Fe/H\] of nearly +0.4 dex, indicating a high probability of hosting a giant planet. A signal with a semi-amplitude of 21 has been detected with a period of nearly 1200 days. The star is very chromospherically quiet and exhibits low rotational velocity, indicating it is an ideal subgiant to search for orbiting exoplanets using the radial velocity method, and hence we do not believe the signal is induced by activity features, and therefore conclude that HD9174 hosts an orbiting planet.

In order to understand the significance of the detected signals we present here, we calculated log-Bayesian evidence ratios for each of the signals presented here based on the MCMC samples drawn from 