UV spectroscopy with the Hubble Space Telescope shows the Ly profile to be complex, with a narrow (400 kms-1 FWHM) and a broad (1600 kms-1 FWHM) component (Puchnarewicz et al. 1998). The optical continuum is not polarized (Breeveld & Puchnarewicz 1998).
The broad component of the Balmer lines is relatively narrow (FWHM 1500 kms-1) and, consequently, this object has been classified as a NLS1 by Puchnarewicz et al. (1995). Narrow line Seyfert 1 galaxies are defined as Seyfert 1s having ``broad'' Balmer lines narrower than 2000 kms-1 FWHM (Osterbrock 1987). Most NLS1s have a steep soft (< 1 keV) X-ray component and, conversely, most ultra-soft X-ray sources are associated with a NLS1 (Puchnarewicz et al. 1992; Greiner et al. 1996; Boller et al. 1996; Wang et al. 1996).