The gas inflow and outflow rate in star-forming galaxies at $z\sim1.4$
  We try to constrain the gas inflow and outflow rate of star-forming galaxies
at $z\sim1.4$ by employing a simple analytic model for the chemical evolution
of galaxies. The sample is constructed based on a large near-infrared (NIR)
spectroscopic sample observed with Subaru/FMOS. The gas-phase metallicity is
measured from the [\ion{N}{2}]$\lambda$6584/H$\alpha$ emission line ratio and
the gas mass is derived from the extinction corrected H$\alpha$ luminosity by
assuming the Kennicutt-Schmidt law. We constrain the inflow and outflow rate
from the least-$\chi^{2}$ fittings of the observed gas mass fraction, stellar
mass, and metallicity with the analytic model. The joint $\chi^{2}$ fitting
shows the best-fit inflow rate is $\sim1.8$ and the outflow rate is $\sim0.6$
in unit of star-formation rate (SFR). By applying the same analysis to the
previous studies at $z\sim0$ and $z\sim2.2$, it is shown that the both inflow
rate and outflow rate decrease with decreasing redshift, which implies the
higher activity of gas flow process at higher redshift. The decreasing trend of
the inflow rate from $z\sim2.2$ to $z\sim0$ agrees with that seen in the
previous observational works with different methods, though the absolute value
is generally larger than the previous works. The outflow rate and its evolution
from $z\sim2.2$ to $z\sim0$ obtained in this work agree well with the
independent estimations in the previous observational works.
