AGN orientation through the spectroscopic correlations and model of dusty cone shell. (arXiv:2110.06687v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lakicevic_M/0/1/0/all/0/1">Ma&#x161;a Laki&#x107;evi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovacevic_Dojcinovic_J/0/1/0/all/0/1">Jelena Kova&#x10d;evi&#x107;-Doj&#x10d;inovi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popovic_L/0/1/0/all/0/1">Luka &#x10c;. Popovi&#x107;</a>

The differences between Narrow Line Seyfert 1 galaxies (NLS1s) and Broad Line
AGNs (BLAGNs) are not completely understood; it is thought that they may have
different inclinations and/or physical characteristics. The
FWHM(Hb)-luminosities correlations are found for NLS1s and their origin is the
matter of debate. Here we investigated the spectroscopic parameters and their
correlations considering a dusty, cone model of AGN. We apply a simple conical
dust distribution (spreading out of broad line region, BLR), assuming that the
observed surface of the model is in a good correlation with MIR emission. The
dusty cone model in combination with a BLR provides the possibility to estimate
luminosity dependence on the cone inclination. The FWHM(Hb)-luminosities
correlations obtained from model in comparison with observational data show
similarities which may indicate the influence of AGN inclination and structure
to this correlation. An alternative explanation for FWHM(Hb)-luminosities
correlations is the selection effect by the black hole mass. These
FWHM(Hb)-luminosities correlations may be related to the starburst in AGNs, as
well. The distinction between spectral properties of the NLS1s and BLAGNs could
be caused by multiple effects: beside physical differencies between NLS1s and
BLAGNs (NLS1s have lighter black hole mass than BLAGNs), inclination of the
conical AGN geometry may have important role as well, where NLS1s may be seen
in lower inclination angles.

The differences between Narrow Line Seyfert 1 galaxies (NLS1s) and Broad Line
AGNs (BLAGNs) are not completely understood; it is thought that they may have
different inclinations and/or physical characteristics. The
FWHM(Hb)-luminosities correlations are found for NLS1s and their origin is the
matter of debate. Here we investigated the spectroscopic parameters and their
correlations considering a dusty, cone model of AGN. We apply a simple conical
dust distribution (spreading out of broad line region, BLR), assuming that the
observed surface of the model is in a good correlation with MIR emission. The
dusty cone model in combination with a BLR provides the possibility to estimate
luminosity dependence on the cone inclination. The FWHM(Hb)-luminosities
correlations obtained from model in comparison with observational data show
similarities which may indicate the influence of AGN inclination and structure
to this correlation. An alternative explanation for FWHM(Hb)-luminosities
correlations is the selection effect by the black hole mass. These
FWHM(Hb)-luminosities correlations may be related to the starburst in AGNs, as
well. The distinction between spectral properties of the NLS1s and BLAGNs could
be caused by multiple effects: beside physical differencies between NLS1s and
BLAGNs (NLS1s have lighter black hole mass than BLAGNs), inclination of the
conical AGN geometry may have important role as well, where NLS1s may be seen
in lower inclination angles.

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