Detection of a double-peaked H$alpha$ component from the accretion disc of NGC 4958. (arXiv:1904.03095v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_T/0/1/0/all/0/1">T.V. Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steiner_J/0/1/0/all/0/1">J.E. Steiner</a>
Active Galactic Nuclei are objects associated with the presence of an
accretion disc around supermassive black holes found in the very central region
of galaxies with a well-defined bulge. In the optical range of the spectrum, a
possible signature of the accretion disc is the presence of a broad
double-peaked component that is mostly seen in H$alpha$. In this paper, we
report the detection of a double-peaked feature in the H$alpha$ line in the
nucleus of the galaxy NGC 4958. The narrow line region of this object has an
emission that is typical of a LINER galaxy, which is the usual classification
for double-peaked emitters. A central broad component, related to the broad
line region (BLR) of this object, is seen in H$alpha$ and also in H$beta$. We
concluded that the double-peaked emission is emitted by a circular relativistic
Keplerian disc with an inner radius $xi_{rm i}$ = 570$pm$ 83, an outer
radius $xi_{rm o}$ = 860$pm$170 (both in units of $GM_{rm SMBH}/c^2$), an
inclination to the line of sight $i$ = 27.2$^o pm$0.7$^o$ and a local
broadening parameter $sigma$ = 1310$pm$70 km s$^{-1}$.
Active Galactic Nuclei are objects associated with the presence of an
accretion disc around supermassive black holes found in the very central region
of galaxies with a well-defined bulge. In the optical range of the spectrum, a
possible signature of the accretion disc is the presence of a broad
double-peaked component that is mostly seen in H$alpha$. In this paper, we
report the detection of a double-peaked feature in the H$alpha$ line in the
nucleus of the galaxy NGC 4958. The narrow line region of this object has an
emission that is typical of a LINER galaxy, which is the usual classification
for double-peaked emitters. A central broad component, related to the broad
line region (BLR) of this object, is seen in H$alpha$ and also in H$beta$. We
concluded that the double-peaked emission is emitted by a circular relativistic
Keplerian disc with an inner radius $xi_{rm i}$ = 570$pm$ 83, an outer
radius $xi_{rm o}$ = 860$pm$170 (both in units of $GM_{rm SMBH}/c^2$), an
inclination to the line of sight $i$ = 27.2$^o pm$0.7$^o$ and a local
broadening parameter $sigma$ = 1310$pm$70 km s$^{-1}$.
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