Gemini NIFS survey of feeding and feedback in nearbyActive Galaxies – III. Ionized versus warm molecular gasmasses and distributions. (arXiv:1902.06790v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Schonell_A/0/1/0/all/0/1">Astor J. Sch''onell Jr.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Storchi_Bergmann_T/0/1/0/all/0/1">Thaisa Storchi-Bergmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riffel_R/0/1/0/all/0/1">Rogemar A. Riffel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riffel_R/0/1/0/all/0/1">Rogério Riffel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchin_M/0/1/0/all/0/1">Marina Bianchin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dahmer_Hahn_L/0/1/0/all/0/1">Luis G. Dahmer-Hahn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diniz_M/0/1/0/all/0/1">Marlon R. Diniz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dametto_N/0/1/0/all/0/1">Natacha Z. Dametto</a>
We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) in
the J and K bands to map the distribution, excitation and kinematics of the
ionized H,{sc ii} and warm molecular gas H$_2$, in the inner few 100,pc of 6
nearby active galaxies: NGC,788, Mrk,607, NGC,3227, NGC,3516, NGC,5506,
NGC,5899. {For most galaxies, this is the first time that such maps have been
obtained}. The ionized and H$_2$ gas show distinct kinematics: while the H$_2$
gas is mostly rotating in the galaxy plane with low velocity dispersion
($sigma$), the ionized gas usually shows signatures of outflows associated
with higher $sigma$ values, most clearly seen in the [Fe,{sc ii}] emission
line. These two gas species also present distinct flux distributions: the H$_2$
is more uniformly spread over the whole galaxy plane, while the ionized gas is
more concentrated around the nucleus and/or collimated along the ionization
axis of its Active Galactic Nucleus (AGN), presenting a steeper gradient in the
average surface mass density profile than the H$_2$ gas. The total H,{sc ii}
masses cover the range $2times,10^5-2times,10^7$,M$_{odot}$, with surface
mass densities in the range 3–150,M$_{odot}$,pc$^{-2}$, while for the warm
H$_2$ the values are 10$^{3-4}$ times lower. We estimate that the available gas
reservoir is at least $approx$,100 times more massive than needed to power
the AGN. If this gas form new stars the star-formation rates, obtained from the
Kennicutt-schmidt scalling relation, are in the range 1–260$times$ 10$^{-3}$
M$_{odot}$ yr$^{-1}$. But the gas will also — at least in part — be ejected
in the form of the observed otflows.
We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) in
the J and K bands to map the distribution, excitation and kinematics of the
ionized H,{sc ii} and warm molecular gas H$_2$, in the inner few 100,pc of 6
nearby active galaxies: NGC,788, Mrk,607, NGC,3227, NGC,3516, NGC,5506,
NGC,5899. {For most galaxies, this is the first time that such maps have been
obtained}. The ionized and H$_2$ gas show distinct kinematics: while the H$_2$
gas is mostly rotating in the galaxy plane with low velocity dispersion
($sigma$), the ionized gas usually shows signatures of outflows associated
with higher $sigma$ values, most clearly seen in the [Fe,{sc ii}] emission
line. These two gas species also present distinct flux distributions: the H$_2$
is more uniformly spread over the whole galaxy plane, while the ionized gas is
more concentrated around the nucleus and/or collimated along the ionization
axis of its Active Galactic Nucleus (AGN), presenting a steeper gradient in the
average surface mass density profile than the H$_2$ gas. The total H,{sc ii}
masses cover the range $2times,10^5-2times,10^7$,M$_{odot}$, with surface
mass densities in the range 3–150,M$_{odot}$,pc$^{-2}$, while for the warm
H$_2$ the values are 10$^{3-4}$ times lower. We estimate that the available gas
reservoir is at least $approx$,100 times more massive than needed to power
the AGN. If this gas form new stars the star-formation rates, obtained from the
Kennicutt-schmidt scalling relation, are in the range 1–260$times$ 10$^{-3}$
M$_{odot}$ yr$^{-1}$. But the gas will also — at least in part — be ejected
in the form of the observed otflows.
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