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Many important details of the mechanisms underlying the ejection of materialduring a (classical) nova eruption are still not understood. Here we presentoptical spectroscopy and narrow-band images of the nova V1425 Aql, 23 yearsafter the nova eruption. We find that the ejecta consist of two significantlydifferent components. The first resembles what is commonly seen in novae, thatis, a symmetric distribution centred on the position of the underlyingcataclysmic binary and presenting both allowed (hydrogen and helium) andforbidden ([OIII] and [NII]) transitions. The second one, on the other hand,consists of material travelling at an approximately three times higher velocitythat is not visible in the allowed transitions, presents a significantlydifferent [NII] - [OIII] ratio, and is located at approximately 2.3 arcsec tothe southwest of the position of the binary. Comparing the velocities andspatial extensions of the two ejecta, we find that both originated in the samenova eruption. We explore possible extrinsic and intrinsic mechanisms for theasymmetry of the high-velocity material in the form of asymmetricallydistributed interstellar material and magnetic accretion, respectively, butfind the available data to be inconclusive. From the expansion parallax, wederive a distance for the nova of 3.3(3) kpc.

The peculiar ejecta of the nova V1425 Aquilae