  We report the analysis of time-series of infrared $JHK_s$ photometry of the
dwarf nova V2051 Oph in quiescence with eclipse mapping techniques to
investigate structures and the spectrum of its accretion disc. The light curves
after removal of the ellipsoidal variations caused by the mass-donor star show
a double-wave modulation signalling the presence of two asymmetric light
sources in the accretion disc. Eclipse maps reveal two spiral arms on top of
the disc emission, one at $R_1= 0.28\pm 0.02 \,R_\mathrm{L1}$ and the other at
$R_2= 0.42\pm 0.02 \,R_\mathrm{L1}$ (where $R_\mathrm{L1}$ is the distance from
disc centre to the inner Lagrangian point), which are seen face-on at binary
phases consistent with the maxima of the double-wave modulation. The wide open
angle inferred for the spiral arms ($\theta_s= 21^o \pm 4^o$) suggests the
quiescent accretion disc of V2051 Oph has high viscosity. The accretion disc is
hot and optically thin in its inner regions ($T_\mathrm{gas}\sim 10-12 \times
10^3\,K$ and surface densities $\sim 10^{-3}-10^{-2}\,g\,cm^{-2}$), and becomes
cool and opaque in its outer regions.
