2023A&A...679A..40T

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 yr 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 ([O III] and [N II]) 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 [N II]-[O III] 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.