The study of planet occurrence rates informs our understanding of how planets form. One important aspect is how the occurrence rates depend on stellar mass; however, measuring masses of field stars is often difficult.

Over the past decade, a controversy has arisen about the inferred planet occurrence rate around evolved intermediate-mass stars -- the so-called retired A-stars. Particularly, the high masses of these evolved planet hosts, derived using spectroscopic information and stellar evolution models, has been called into question with arguments that they are unlikely to be that high.

We aim to resolve the controversy by determining the mass of evolved planet hosting stars using asteroseismology. In this talk I will present our findings based on data from the SONG telescope of bright nearby planet hosting stars. We find a significant
one-sided offset between the previous spectroscopy-based masses and our seismic results, suggestive that the former are overestimated.

The talk will include published results from 2017 and still unpublished results
from our 2018 campaign.