  Many important details of the mechanisms underlying the ejection of material
during a (classical) nova eruption are still not understood. Here we present
optical spectroscopy and narrow-band images of the nova V1425 Aql, 23 years
after the nova eruption. We find that the ejecta consist of two significantly
different components. The first resembles what is commonly seen in novae, that
is, a symmetric distribution centred on the position of the underlying
cataclysmic binary and presenting both allowed (hydrogen and helium) and
forbidden ([OIII] and [NII]) transitions. The second one, on the other hand,
consists of material travelling at an approximately three times higher velocity
that is not visible in the allowed transitions, presents a significantly
different [NII] - [OIII] ratio, and is located at approximately 2.3 arcsec to
the southwest of the position of the binary. Comparing the velocities and
spatial extensions of the two ejecta, we find that both originated in the same
nova eruption. We explore possible extrinsic and intrinsic mechanisms for the
asymmetry of the high-velocity material in the form of asymmetrically
distributed interstellar material and magnetic accretion, respectively, but
find the available data to be inconclusive. From the expansion parallax, we
derive a distance for the nova of 3.3(3) kpc.
