Evidence of wind signatures in the gas velocity profiles of Red Geysers
  Spatially resolved spectroscopy from SDSS-IV MaNGA survey has revealed a
class of quiescent, relatively common early-type galaxies, termed "red
geysers", that possibly host large scale active galactic nuclei driven winds.
Given their potential importance in maintaining low level of star formation at
late times, additional evidence confirming that winds are responsible for the
red geyser phenomenon is critical. In this work, we present follow-up
observations with the Echellette Spectrograph and Imager (ESI) at the Keck
telescope of two red geysers (z$<$0.1) using multiple long slit positions to
sample different regions of each galaxy. Our ESI data with a spectral
resolution (R) $\sim$ 8000 improves upon MaNGA's resolution by a factor of
four, allowing us to resolve the ionized gas velocity profiles along the
putative wind cone with an instrumental resolution of $\rm \sigma =
16~km~s^{-1}$. The line profiles of H$\alpha$ and [NII]$\rm \lambda 6584$ show
asymmetric shapes that depend systematically on location $-$ extended blue
wings on the red-shifted side of the galaxy and red wings on the opposite side.
We construct a simple wind model and show that our results are consistent with
geometric projections through an outflowing conical wind oriented at an angle
towards the line of sight. An alternative hypothesis that assigns the
asymmetric pattern to "beam-smearing" of a rotating, ionized gas disk does a
poor job matching the line asymmetry profiles. While our study features just
two sources, it lends further support to the notion that red geysers are the
result of galaxy-scale winds.
