of the mass function and its relationship to stellar metallicity, along with searching for correlations between these parameters and planetary orbital period and we briefly discuss the impact of these results. Finally, in $\S~\ref{conclusions}$ we summerise the main points of the present work.

Observations and Reduction {#observations}
==========================

The radial velocity datasets for these stars were observed using the precision radial velocity spectrographs CORALIE, HARPS, and MIKE. Both the CORALIE and HARPS spectrographs are physically located at the ESO La Silla Observatory in Chile, where CORALIE is mounted on the Swiss Euler telescope and HARPS is fed by light from the ESO 3.6m telescope. The MIKE spectrograph is located at the Las Campanas Observatory and is mounted on the Magellan Clay 6.5m telescope.

In this work, 570 radial velocities are reported, with a fairly even split between CORALIE and HARPS observations, in comparison to the smaller fraction of MIKE data. The baseline of observations for the CORALIE data run from 2009 November 25$^{\rm{th}}$ until 2015 October 23$^{\rm{rd}}$ (BJD 2455160.53623 - 2457318.85147), whereas the HARPS data runs from 2007 May 28$^{\rm{th}}$ until 2013 September 28$^{\rm{th}}$ (BJD 2454248.60231 - 2456563.90982) showing that the HARPS data covers a longer baseline but the CORALIE 