  We present 1-D non-Local-Thermodynamic-Equilibrium time-dependent
radiative-transfer simulations for a large grid of supernovae (SNe) IIb/Ib/Ic
that result from the terminal explosion of the mass donor in a close-binary
system. Our sample covers ejecta masses $M_{\rm e}$ of 1.7$-$5.2M$_\odot$,
kinetic energies $E_{\rm kin}$ of 0.6$-$5.0$\times$10$^{51}$erg, and $^{56}$Ni
masses of 0.05$-$0.30M$_\odot$. We find a strong correlation between the
$^{56}$Ni mass and the photometric properties at maximum, and between the rise
time to bolometric maximum and the post-maximum decline rate. We confirm the
small scatter in ($V-R$) at 10d past $R$-band maximum. The quantity $V_{\rm m}
\equiv \sqrt{2E_{\rm kin}/M_{\rm e}}$ is comparable to the Doppler velocity
measured from HeI 5875\AA\ at maximum in SNe IIb/Ib, although some scatter
arises from the uncertain level of chemical mixing. The OI7772\AA\ line may be
used for SNe Ic, but the correspondence deteriorates with higher ejecta
mass/energy. We identify a temporal reversal of the Doppler velocity at maximum
absorption in the $\sim$1.05$\mu$m feature in all models. The reversal is due
to HeI alone and could serve as a test for the presence of helium in SNe Ic.
Because of variations in composition and ionisation, the ejecta opacity shows
substantial variations with both velocity and time. This is in part the origin
of the offset between our model light curves and the predictions from the
Arnett model.
