  Ultra-luminous infrared galaxies (ULIRGs) are the most luminous and intense
starburst galaxies in the Universe. Both their star-formation rate (SFR) and
gas surface mass density are very high, implying a high supernovae rate and an
efficient energy conversion of energetic protons. A small fraction of these
supernovae is the so-called hypernovae with a typical kinetic energy ~1e52 erg
and a shock velocity >=1e9 cm/s. The strong shocks driven by hypernovae are
able to accelerate cosmic ray protons up to 1e17 eV. These energetic protons
lose a good fraction of their energy through proton-proton collision when
ejected into very dense interstellar medium, and as a result, produce high
energy neutrinos (<=5 PeV). Recent deep infrared surveys provide solid
constraints on the number density of ULIRGs across a wide redshift range
0<z<2.3, allowing us to derive the flux of diffuse neutrinos from hypernovae.
We find that at PeV energies, the diffuse neutrinos contributed by ULIRGs are
comparable with the atmosphere neutrinos with the flux of 2e-9GeV cm^-2/s/sr,
by assuming the injected cosmic ray power law spectrum with an index of -2.
