  We analyse new optical spectroscopic, direct-image and X-ray observations of
the recently discovered a high proper motion cataclysmic variable V1838 Aql.
The data were obtained during its 2013 superoutburst and its subsequent
quiescent state. An extended emission around the source was observed up to 30
days after the peak of the superoutburst, interpreted it as a bow--shock formed
by a quasi-continuous outflow from the source in quiescence. The head of the
bow--shock is coincident with the high--proper motion vector of the source
($v_{\perp}=123\pm5$ km s$^{-1}$) at a distance of $d=202\pm7$ pc. The object
was detected as a weak X-ray source ($0.015\pm0.002$ counts s$^{-1}$) in the
plateau of the superoutburst, and its flux lowered by two times in quiescence
(0.007$\pm$0.002 counts s$^{-1}$). Spectroscopic observations in quiescence we
confirmed the orbital period value $P_{\rm{orb}}=0.0545\pm 0.0026$ days,
consistent with early-superhump estimates, and the following orbital
parameters: $\gamma= -21\pm3$ km s$^{-1}$ and $K_1 = 53\pm3$ km s$^{-1}$. The
white dwarf is revealed as the system approaches quiescence, which enables us
to infer the effective temperature of the primary $T_{eff}=11,600\pm400$K. The
donor temperature is estimated $\lesssim 2200$K and suggestive of a system
approaching the period minimum. Doppler maps in quiescence show the presence of
the hot spot in HeI line at the expected accretion disc-stream shock position
and an unusual structure of the accretion disc in H$\alpha$.
