Characterization of the continuum and kinematical properties of nearby NLS1. (arXiv:1906.07909v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Oio_G/0/1/0/all/0/1">Gabriel A. Oio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vega_L/0/1/0/all/0/1">Luis R. Vega</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmidt_E/0/1/0/all/0/1">Eduardo O. Schmidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferreiro_D/0/1/0/all/0/1">Diego Ferreiro</a>
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$5007 emission line as surrogate of
the former. We studied spectra of a sample of 131 NLS1 galaxies taken from the
Sloan Digital Sky Survey (SDSS) DR7. We approached the determination of the
non-stellar continuum using the spectral synthesis technique using the code
{sc starlight}, adopting a power-law base to model the non-stellar continuum.
A composite spectra of NLS1 galaxies was also obtained based on the sample. In
addition, we obtained the stellar velocity dispersion from the code and by
measuring Calcium II Triplet absorption lines and [OIII] emission lines. From
Gaussian decomposition of the H$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 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 power law component. Finally, according to our results, NLS1
galaxies in our sample follow the relation M $-$ $sigma$, both considering the
stellar velocity dispersion ($sigma_{star}$), and the core component of
[OIII]$lambda$5007.
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$5007 emission line as surrogate of
the former. We studied spectra of a sample of 131 NLS1 galaxies taken from the
Sloan Digital Sky Survey (SDSS) DR7. We approached the determination of the
non-stellar continuum using the spectral synthesis technique using the code
{sc starlight}, adopting a power-law base to model the non-stellar continuum.
A composite spectra of NLS1 galaxies was also obtained based on the sample. In
addition, we obtained the stellar velocity dispersion from the code and by
measuring Calcium II Triplet absorption lines and [OIII] emission lines. From
Gaussian decomposition of the H$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 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 power law component. Finally, according to our results, NLS1
galaxies in our sample follow the relation M $-$ $sigma$, both considering the
stellar velocity dispersion ($sigma_{star}$), and the core component of
[OIII]$lambda$5007.
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