[@LovisPepe2007] computes radial velocities by a cross-correlation function technique [@Baranne:1996 e.g.,]. Nevertheless we derived radial velocities by a different approach to exploit as much as possible the Doppler information of spectra [e.g., @Anglada2012]. We performed a maximum likelihood analysis between a stellar template and each individual spectrum following the procedure presented in @Astudillo-Defru2017b. The stellar template corresponds to a true stellar spectrum of the star, enhanced in signal-to-noise. It was made from the median of all the spectra, after shifting them into a common barycentric frame. The resulting template is Doppler shifted by a range of trial radial velocities to construct the maximum likelihood function, from which we derived the HARPS radial velocity used in the subsequent analysis. The obtained radial velocities – listed in Table \[tab:rvHARPS\] – present a dispersion of 4.01 $m/s$ and a median photon uncertainty of 1.71 $m/s$. Figure \[fig:phasedRV\] shows the radial velocities folded to the orbital period.

### PFS

The Planet Finder Spectrograph is an iodine-calibrated, environmentally controlled high resolution PRV spectrograph [@Crane:2006; @Crane:2008; @Crane:2010]. Since first light in October 2009, PFS has been running a long-term survey program to search for planets around nearby stars (e.g.,  @Teske:2016). In January 2018, PFS was upgraded 