The link between X-ray complexity and optical lines in NLS1s
  Narrow-line Seyfert 1 galaxies (NLS1s) are a subclass of active galactic
nuclei (AGN). It is often believed that these AGN have small black hole mass,
which is responsible for the narrowness of the permitted lines. They are also
characterised by a high accretion rate, typically closer to the Eddington
limit. Nevertheless, narrow permitted lines might also be caused by a disk-like
broad-line region (BLR) viewed pole-on. This class of objects presents strong
X-ray emission, which is characterised by a very steep spectral index described
by a single power law. In particular, some of them exhibit particular features
around the iron K-shell energy at 6-8 keV. Recently, this different spectral
behaviour was attributed to inclination. In this work we are going to analyse
optical spectra to measure in different ways the width of H$\beta$, which is
another potential inclination indicator. Our aim is to search for a correlation
between the high-energy spectral complexity and FWHM of H$\beta$, in order to
verify whether or not the broad-line region could be flattened.
