  Star-forming galaxies, due to their high star-formation rates and hence large
number of supernova remnants therein, are huge reservoirs of cosmic rays (CRs).
These CRs collide with gases in the galaxies and produce high-energy neutrinos
through $pp$ collisions. In this paper, we calculate the neutrino production
efficiency in star-forming galaxies by considering realistic galaxy properties,
such as the gas density and galactic wind in star-forming galaxies. To
calculate the accumulated neutrino flux, we use the infrared luminosity
function of star-forming galaxies obtained by {\em Herschel} PEP/HerMES survey
recently. The intensity of CRs producing PeV neutrinos in star-forming galaxies
is normalized with the observed CR flux at EeV ({1\,EeV=$10^{18}\,$eV}),
assuming that supernova remnants or hypernova remnants in star-forming galaxies
can accelerate protons to EeV energies. Our calculations show that the
accumulated neutrino emission produced by CRs in star-forming galaxies can
account for the flux and spectrum of the sub-PeV/PeV neutrinos under reasonable
assumptions on the CR confinement time in these galaxies.
