What do the UV Spectra of Narrow-line Seyfert 1 Galaxies tell us about their BLR?

We study the UV spectra of narrow-line Seyfert~1 (NLSy1) galaxies and compare them with ``normal'' AGN. Similar to their optical lines, the NLSy1s show narrower UV lines. They are also characterized by weaker CIV 1549, CIII] 1909, and stronger AlIII 1857 emission. These UV line properties add to the optical and X-ray properties known to be part of the Boroson and Green eigenvector 1. We show that the steep soft-X-rays, which characterize the NLSy1s SEDs, change the equilibrium of the two phase cloud-intercloud medium resulting in somewhat higher BLR cloud densities, lower ionization parameter and larger BLR radii. These modified conditions can explain the unusual emission line properties we find in NLSy1. Using a specific model of an accretion disk with corona presented by Witt, Czerny and Zycki (1997), we also show that the steep soft and hard-X-ray continua can be explained if the $L/L_{Edd}$ ratios are larger than in ``normal'' Seyfert1/QSO strengthening earlier suggestions that the $L/L_{Edd}$ is the physical parameter driving this eigenvector.