Galactic outflow and diffuse gas properties at z>=1 using different
  baryonic feedback models
  We measure and quantify properties of galactic outflows and diffuse gas at $z
\geq 1$ in cosmological hydrodynamical simulations. Our novel sub-resolution
model, MUPPI, implements supernova feedback using fully local gas properties,
where the wind velocity and mass loading are not given as input. We find the
following trends at $z = 2$ by analysing central galaxies having a stellar mass
higher than $10^{9} M_{\odot}$. The outflow velocity and mass outflow rate
($\dot{M}_{\rm out}$) exhibit positive correlations with galaxy mass and with
the star formation rate (SFR). However, most of the relations present a large
scatter. The outflow mass loading factor ($\eta$) is between $0.2 - 10$. The
comparison Effective model generates a constant outflow velocity, and a
negative correlation of $\eta$ with halo mass. The number fraction of galaxies
where outflow is detected decreases at lower redshifts, but remains more than
$80 \%$ over $z = 1 - 5$. High SF activity at $z \sim 2 - 4$ drives strong
outflows, causing the positive and steep correlations of velocity and
$\dot{M}_{\rm out}$ with SFR. The outflow velocity correlation with SFR becomes
flatter at $z = 1$, and $\eta$ displays a negative correlation with halo mass
in massive galaxies. Our study demonstrates that both the MUPPI and Effective
models produce significant outflows at $\sim 1 / 10$ of the virial radius; at
the same time shows that the properties of outflows generated can be different
from the input speed and mass loading in the Effective model. Our MUPPI model,
using local properties of gas in the sub-resolution recipe, is able to develop
galactic outflows whose properties correlate with global galaxy properties, and
consistent with observations.
