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tokens: can be asymmetric both in position (i.e. different distances from disc centre) and brightness (e.g. Baptista, Harlaftis Steeghs 2000b ; Baptista et al. 2005 ). Aside of the transient spiral structures seen during dwarf nova outbursts, spiral shocks were also observed in nova-like systems – where they presumably are persistent, tidally induced effects in permanently large and hot accretion discs (Baptista Bortoletto 2008 ; Saito et al. 2010 ). V348 Puppis is the optical counterpart of the faint HEAO X-ray source 1H0709-36, identified by Tuohy et al. ( 1990 ) as an eclipsing CV inside the period gap ( P orb = 2.44 h, Baptista et al. 1996b ; Rolfe, Haswell Patterson 2000 ). Its light curve, which shows the gradual eclipse of an extended source, and the observed rotational disturbance in its emission lines during eclipse indicate the presence of a bright, high mass accretion rate disc outshining the contributions from the WD at disc centre and the bright spot at disc rim. The detection as a hard X-ray source, the presence of a strong He ii λ4686 emission line in the spectrum and the possible existence of a second periodicity close to the orbital period led to the suggestion that V348 Pup might be a magnetic CV of the DQ Her type close to synchronize (Tuohy et al. 1990 ; Rosen et al. 1994 ). However, its spectrum exhibits strong single-peaked Balmer and He i emission lines that remain largely unobscured during disc eclipse (indicating significant contribution from above the orbital plane) and displays absorption components at phases opposite to the disc eclipse (φ = 0.4–0.5). This spectroscopic behaviour led Rodríguez-Gil et al. ( 2001 ) to classify V348 Pup as a nova-like variable of the SW Sex type. Moreover, the nature of the second periodicity became clear with the discovery of long-lasting, positive superhumps (with a period 6 per cent longer than P orb ), resulting from the gravitational interaction between a slowly precessing non-axisymmetric accretion disc and the mass-donor star (Rolfe et al. 2000 ). Its eclipsing nature and the location within the period gap make V348 Pup an obvious target for an investigation of its accretion disc properties with eclipse mapping techniques (Horne 1985 ). For this purpose, time series of UV and optical spectroscopy of V348 Pup were collected with the Hubble Space Telescope ( HST ). A first analysis of this data set were reported by Froning, Long Baptista ( 2003 ). They found that the HST out-of-eclipse spectrum is characterized by a blue continuum with strong emission lines and a broad dip in the spectral range λ2000–3000 Å (attributed to a blend of Fe ii absorption lines known as the ‘Fe ii curtain’; Horne et al. 1994 ), but the Balmer jump is shallow or absent. The eclipses are remarkably shallow across the observed spectral range (≃40–50 per cent of the out-of-eclipse light remains visible at mid-eclipse in the continuum, and up to 80 per cent in the emission lines) indicating that a significant