  In order to study the slope and strength of the non-stellar continuum, we
analyzed a sample of nearby Narrow Line Seyfert 1 (NLS1). Also, we re-examined
the location of NLS1 galaxies on the M $-$ $\sigma$ relation using the stellar
velocity dispersion and the [OIII]$\lambda$5007 emission line as surrogate of
the former. We studied spectra of a sample of 131 NLS1 galaxies taken from the
Sloan Digital Sky Survey (SDSS) DR7. We approached determining the non-stellar
continuum by employing the spectral synthesis technique, which uses the code
{\sc starlight}, and by adopting a power-law base to model the non-stellar
continuum. Composite spectra of NLS1 galaxies were also obtained based on the
sample.In addition, we obtained the stellar velocity dispersion from the code
and by measuring Calcium II Triplet absorption lines and [OIII] emission lines.
From Gaussian decomposition of the H$\beta$ profile we calculated the black
hole mass. We obtained a median slope of $\beta$ = $-$1.6 with a median
fraction of contribution of the non-stellar continuum to the total flux of
0.64. We determined black hole masses in the range of log(M$_{BH}$/M$_{\odot}$)
= 5.6 $-$ 7.5 which is in agreement with previous works. We found a correlation
between the luminosity of the broad component of H$\beta$ and black hole mass
with the fraction of a power-law component. Finally, according to our results,
NLS1 galaxies in our sample are located mostly underneath the MBH -
$\sigma_{\star}$ relation, both considering the stellar velocity dispersion
($\sigma_{\star}$) and the core component of [OIII]$\lambda$5007.
