A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit

π Men hosts a transiting planet detected by the Transiting Exoplanet Survey Satellite space mission and an outer planet in a 5.7 yr orbit discovered by radial velocity (RV) surveys. We studied this system using new RV measurements taken with the HARPS spectrograph on ESO's 3.6 m telescope, as well as archival data. We constrain the stellar RV semiamplitude due to the transiting planet, π Men c, as K <SUB>c</SUB> = 1.21 ± 0.12 m s<SUP>-1</SUP>, resulting in a planet mass of M <SUB>c</SUB> = 3.63 ± 0.38 M <SUB>⊕</SUB>. A planet radius of R <SUB>c</SUB> = 2.145 ± 0.015 R <SUB>⊕</SUB> yields a bulk density of ρ <SUB>c</SUB> = 2.03 ± 0.22 g cm<SUP>-3</SUP>. The precisely determined density of this planet and the brightness of the host star make π Men c an excellent laboratory for internal structure and atmospheric characterization studies. Our HARPS RV measurements also reveal compelling evidence for a third body, π Men d, with a minimum mass M <SUB>d</SUB> sin i <SUB>d</SUB> = 13.38 ± 1.35 M <SUB>⊕</SUB> orbiting with a period of P <SUB>orb,d</SUB> = 125 days on an eccentric orbit (e <SUB>d</SUB> = 0.22). A simple dynamical analysis indicates that the orbit of π Men d is stable on timescales of at least 20 Myr. Given the mutual inclination between the outer gaseous giant and the inner rocky planet and the presence of a third body at 125 days, π Men is an important planetary system for dynamical and formation studies.