  We investigate the flux and the event rate of the supernova relic neutrino
background (SRN) at the SuperKamiokande detector for various neutrino
oscillation models with parameters inferred from recent experimental results. A
realistic model of neutrino emission from supernova explosions and several
models of the cosmic star formation history are adopted in the calculation. The
number flux over entire energy range is found to be $11-15
\mathrm{cm^{-2}s^{-1}}$. We discuss the detection possibility of SRN at
SuperKamiokande, comparing this SRN flux with other background neutrinos in
more detail than previous studies. Even though there is no energy window in
which SRN is dominant, we might detect it as the distortion of the other
background event. We found in the energy range $17-25 \mathrm{MeV}$ the
expected event rate at SuperKamiokande $0.4-0.8 ~\mathrm{yr^{-1}}$. In this
range, ten-year observation might enable us to detect SRN signal (at one sigma
level) in the case of LMA solar neutrino solution. We also investigate event
rate at SNO and KamLAND. Although we can find energy window, the expected event
rate is rather small (0.03 yr$^{-1}$ for SNO, 0.1 yr$^{-1}$ for KamLAND).
