2016MNRAS.455L..57M

We have obtained daily high-resolution Echelle spectroscopy of Nova Oph 2015 during its initial evolution. It reveals the presence of pre-existing circumstellar material around the nova, which can be interpreted as the wind of an evolved companion. On earliest observations, the emission line profiles of Nova Oph 2015 displayed a very narrow emission component (full width at half-maximum [FWHM] ∼ 60 km/s), recombining over a time-scale of 5 days and showing constant low velocity (RV_☉ = -4.5 km/s), that we interpret as coming from the wind of the secondary recombining after the ionization from the initial UV-flash of the nova. The underlying broad component underwent a marked reduction in both FWHM and width at zero intensity (the latter declining from 4000 to 2000 km/s in 10 days) while increasing by six times in flux, that we believe is the result of the high-velocity ejecta of the nova being slowed down while trying to expand within the surrounding wind of the companion. Nova Oph 2015 is possibly unique among novae with evolved companions in having displayed a long rise to maximum brightness and a slow decline from it, an Feii-type classification, and a probable sub-giant luminosity class for the secondary.