Molecular gas dynamics around nuclei of galaxies. (arXiv:2205.06106v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">Francoise Combes</a> (Obs-Paris, LERMA)
Recent molecular line observations with ALMA in several nearby Seyferts have
revealed the existence of molecular tori, and the nature of gas flows at
10-20~pc scale. At 100~pc scale, or kpc-scale, previous NOEMA work on
gravitational torques had shown that only about one third of Seyfert galaxies
experienced molecular inflow and central fueling, while in most cases the gas
was stalled in rings. At higher resolution, i.e. 10-20~pc scale, it is possible
now to see in some cases AGN fueling due to nuclear trailing spirals,
influenced by the black hole potential. This brings smoking gun evidence for
nuclear fueling. In our sample galaxies, the angular resolution of up to 60~mas
allows us to reach the black hole (BH) sphere of influence and the BH mass can
be derived more directly than with the M-sigma relation.
Recent molecular line observations with ALMA in several nearby Seyferts have
revealed the existence of molecular tori, and the nature of gas flows at
10-20~pc scale. At 100~pc scale, or kpc-scale, previous NOEMA work on
gravitational torques had shown that only about one third of Seyfert galaxies
experienced molecular inflow and central fueling, while in most cases the gas
was stalled in rings. At higher resolution, i.e. 10-20~pc scale, it is possible
now to see in some cases AGN fueling due to nuclear trailing spirals,
influenced by the black hole potential. This brings smoking gun evidence for
nuclear fueling. In our sample galaxies, the angular resolution of up to 60~mas
allows us to reach the black hole (BH) sphere of influence and the BH mass can
be derived more directly than with the M-sigma relation.
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