  We examine the demographics of radio-emitting active galactic nuclei (AGN) in
the local universe as a function of host galaxy properties, most notably both
stellar mass and star formation rate. Radio AGN activity is theoretically
implicated in helping reduce star formation rates of galaxies, and therefore it
is natural to investigate the relationship between these two galaxy properties.
We use a sample of around 10, 000 galaxies from the Mapping Nearby Galaxies at
APO (MaNGA) survey, part of the Sloan Digital Sky Survey IV (SDSS-IV), along
with the Faint Images of the Radio Sky at Twenty centimeters (FIRST) radio
survey and the National Radio Astronomy Observatory (NRAO) Very Large Array
(VLA) Sky Survey (NVSS). There are 1,126 galaxies in MaNGA with radio
detections. Using star formation rate and stellar mass estimates based on
Pipe3D, inferred from the high signal-to-noise ratio measurements from MaNGA,
we show that star formation rates are strongly correlated with 20 cm radio
emission, as expected. We identify as radio AGN those radio emitters that are
much stronger than expected from the star formation rate. Using this sample of
AGN, the well-measured stellar velocity dispersions from MaNGA, and the black
hole M-sigma relationship, we examine the Eddington ratio distribution and its
dependence on stellar mass and star formation rate. We find that the Eddington
ratio distribution depends strongly on stellar mass, with more massive galaxies
having larger Eddington ratios. As found in previous studies, the AGN fraction
increases rapidly with stellar mass. We do not find any dependence on star
formation rate, specific star formation rate, or velocity dispersion when
controlling for stellar mass. We conclude that galaxy star formation rates
appear to be unrelated to the presence or absence of a radio AGN, which may be
useful in constraining theoretical models of AGN feedback.
