Cool outflows in MaNGA: a systematic study and comparison to the warm
  phase
  This paper investigates the neutral gas phase of galactic winds via the Na I
D$\lambda\lambda 5890,5895${\AA} feature within $z \sim 0.04$ MaNGA galaxies,
and directly compares their incidence and strength to the ionized winds
detected within the same parent sample. We find evidence for neutral outflows
in 127 galaxies ($\sim 5$ per cent of the analysed line-emitting sample). Na I
D winds are preferentially seen in galaxies with dustier central regions and
both wind phases are more often found in systems with elevated SFR surface
densities, especially when there has been a recent upturn in the star formation
activity according to the SFR$_{5Myr}$/SFR$_{800Myr}$ parameter. We find the
ionized outflow kinematics to be in line with what we measure in the neutral
phase. This demonstrates that, despite their small contributions to the total
outflow mass budget, there is value to collecting empirical measurements of the
ionized wind phase to provide information on the bulk motion in the outflow.
Depending on dust corrections applied to the ionized gas diagnostics, the
neutral phase has $\sim 1.2 - 1.8$ dex higher mass outflow rates
($\dot{M}_{out}$), on average, compared to the ionized phase. We quantify
scaling relations between $\dot{M}_{out}$ and the strengths of the physical
wind drivers (SFR, $L_{AGN}$). Using a radial-azimuthal stacking method, and by
considering inclination dependencies, we find results consistent with biconical
outflows orthogonal to the disk plane. Our work complements other multi-phase
outflow studies in the literature which consider smaller samples, more extreme
objects, or proceed via stacking of larger samples.
