Detecting Radio-AGN signatures in Red geysers
  A new class of quiescent galaxies harboring possible AGN-driven winds has
been discovered using spatially resolved optical spectroscopy from the ongoing
SDSS-IV MaNGA survey. These galaxies, termed "red geysers", constitute $5-10\%$
of the local quiescent population and are characterized by narrow bisymmetric
patterns in ionized gas emission features. Cheung et al. argued that these
galaxies host large-scale AGN-driven winds that may play a role in suppressing
star formation at late times. In this work, we test the hypothesis that AGN
activity is ultimately responsible for the red geyser phenomenon. We compare
the nuclear radio activity of the red geysers to a matched control sample with
similar stellar mass, redshift, rest frame $NUV-r$ color, axis ratio and
presence of ionized gas. We have used the 1.4 GHz radio continuum data from VLA
FIRST survey to stack the radio flux from the red geyser and control samples.
In addition to a 3 times higher FIRST detection rate, we find that red geysers
have a 5$\sigma$ higher level of average radio flux than control galaxies.
After restricting to rest-frame $NUV-r$ color $>$ 5 and checking mid-IR WISE
photometry, we rule out star formation contamination and conclude that red
geysers are associated with more active AGN. Red geysers and a possibly-related
class with disturbed H$\alpha$ emission account for 40\% of all radio-detected
red galaxies with $\rm log~(M_\star/M_\odot) < 11$. Our results support a
picture in which episodic AGN activity drives large-scale-relatively weak
ionized winds that may provide a feedback mechanism for many early-type
galaxies.
