The MAGNUM survey: different gas properties in the outflowing and disk components in nearby active galaxies with MUSE. (arXiv:1811.07935v1 [astro-ph.GA])

The MAGNUM survey: different gas properties in the outflowing and disk components in nearby active galaxies with MUSE. (arXiv:1811.07935v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mingozzi_M/0/1/0/all/0/1">M. Mingozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cresci_G/0/1/0/all/0/1">G. Cresci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venturi_G/0/1/0/all/0/1">G. Venturi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marconi_A/0/1/0/all/0/1">A. Marconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mannucci_F/0/1/0/all/0/1">F. Mannucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perna_M/0/1/0/all/0/1">M. Perna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belfiore_F/0/1/0/all/0/1">F. Belfiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carniani_S/0/1/0/all/0/1">S. Carniani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balmaverde_B/0/1/0/all/0/1">B. Balmaverde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brusa_M/0/1/0/all/0/1">M. Brusa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicone_C/0/1/0/all/0/1">C. Cicone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feruglio_C/0/1/0/all/0/1">C. Feruglio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallazzi_A/0/1/0/all/0/1">A. Gallazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mainieri_V/0/1/0/all/0/1">V. Mainieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiolino_R/0/1/0/all/0/1">R. Maiolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagao_T/0/1/0/all/0/1">T. Nagao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nardini_E/0/1/0/all/0/1">E.Nardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sani_E/0/1/0/all/0/1">E. Sani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tozzi_P/0/1/0/all/0/1">P. Tozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zibetti_S/0/1/0/all/0/1">S. Zibetti</a>

We investigate the interstellar medium properties of the disk and outflowing
gas in the central regions of nine nearby Seyfert galaxies, characterised by
prominent outflows. These objects are part of the MAGNUM (Measuring Active
Galactic Nuclei Under MUSE Microscope) survey, that aims at probing their
physical conditions, by exploiting the unprecedented sensitivity of MUSE. We
study the gas properties in the disk and in the outflow with spatially and
kinematically resolved maps, by dividing the strongest emission lines in
velocity bins. We associate the core of the lines to the disk, consistent with
the stellar velocity, and the redshifted and blueshifted wings to the outflow.
We find that the outflowing gas is characterised by higher values of density
and ionisation parameter than the disk, which presents a higher dust
extinction. Moreover, we distinguish high- and low-ionisation regions across
the portion of spatially resolved narrow line region traced by the outflow. The
high ionisation regions characterised by the lowest [NII]/H{alpha} and
[SII]/H{alpha} line ratios, generally trace the inner parts along the axis of
the emitting cones, where the [SIII]/[SII] line ratio is enhanced, while the
low ionisation ones follow the cone edges and/or the regions perpendicular to
the axis of the outflows, characterized by a higher [OIII] velocity dispersion.
A possible scenario to explain these features relies on the presence of two
distinct populations of line emitting clouds: one is optically thin to the
radiation and characterised by the highest excitation, while the other,
optically thick, is impinged by a harder radiation field, which generates
strong low-excitation lines. The highest values of [NII]/H{alpha} and
[SII]/H{alpha} line ratios may be due to shocks and/or a hard filtered
radiation field from the AGN.

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