A quasar without broad Lyα emission

The z = 3.02 quasar SDSS J095253.83+011421.9 exhibits broad metal-line emission ( C IV FWHM similar or equal to 9000 km s(-1)), but broad Lyalpha emission is not present. Instead, only a narrow Lyalpha line is observed ( FWHM similar or equal to 1140 km s(-1)). The large C IV/Lyalpha ratio in the broad-line region (BLR) emission from this object can be matched most closely by a BLR dominated by gas at very high densities (10(15) cm(-3)), which suppresses the Lyalpha emission, and illuminated by an incident power law extending to similar to200 mum, which yields increased emission from purely collisionally excited coolant lines (such as C IV, N v, and O VI) but not from recombination lines like Lyalpha. However, the strong C III emission predicted by this model is not observed, and the observed broad C III] emission must come from a lower density BLR component and should be accompanied by broad Lyalpha emission, which is not observed. The least unlikely explanation for this spectrum seems to be that any intrinsic broad Lyalpha emission is removed by smooth N v absorption in the red wing of the Lyalpha emission line and by smooth Lyalpha absorption in the blue wing of the Lyalpha emission line. This postulated smooth absorption would be in addition to the strong, associated, narrow absorption seen in numerous ions. Smooth absorption in Lyalpha, N v, and O vi, but not in C IV, would be unusual, but not impossible, although it is suspicious that the postulated absorption must almost exactly cancel the postulated intrinsic broad emission. We conclude that the spectrum of SDSS J0952+0114 appears unique ( among similar or equal to 3600 SDSS spectra of quasars at z > 2.12) because of some combination of unusual parameters, and we discuss possible observations to determine the combination of circumstances responsible for the spectrum.