Multi-phase characterization of AGN winds in 5 local type-2 quasars. (arXiv:2311.10132v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Speranza_G/0/1/0/all/0/1">G. Speranza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almeida_C/0/1/0/all/0/1">C. Ramos Almeida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acosta_Pulido_J/0/1/0/all/0/1">J. A. Acosta-Pulido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Audibert_A/0/1/0/all/0/1">A. Audibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holden_L/0/1/0/all/0/1">L. R. Holden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tadhunter_C/0/1/0/all/0/1">C. N. Tadhunter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lapi_A/0/1/0/all/0/1">A.Lapi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Martin_O/0/1/0/all/0/1">O. González-Martín</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:+Lopez_I/0/1/0/all/0/1">I. E. López</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Musiimenta_B/0/1/0/all/0/1">B. Musiimenta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shankar_F/0/1/0/all/0/1">F. Shankar</a>
We present MEGARA (Multi-Espectr’ografo en GTC de Alta Resoluci’on para
Astronom’ia) Integral Field Unit (IFU) observations of 5 local type-2 quasars
(QSO2s, z $sim 0.1$) from the Quasar Feedback (QSOFEED) sample. These active
galactic nuclei (AGN) have bolometric luminosities of 10$^{45.5-46}$ erg/s and
stellar masses of $sim$10$^{11}$ M$_{odot}$. We explore the kinematics of the
ionized gas through the [O~III]$lambda$5007 $r{A}$ emission line. The nuclear
spectra of the 5 QSO2s, extracted in a circular aperture of $sim$ 1.2″ ($sim$
2.2 kpc) in diameter, show signatures of high velocity winds in the form of
broad (full width at half maximum; 1300$leq$FWHM$leq$2240 km/s and
blueshifted components. We find that 4 out of the 5 QSO2s present outflows that
we can resolve with our seeing-limited data, and they have radii ranging from
3.1 to 12.6 kpc. In the case of the two QSO2s with extended radio emission, we
find that it is well-aligned with the outflows, suggesting that low-power jets
might be compressing and accelerating the ionized gas in these radio-quiet
QSO2s. In the four QSO2s with spatially resolved outflows, we measure ionized
mass outflow rates of 3.3-6.5 Msun/yr when we use [S~II]-based densities, and
of 0.7-1.6 Msun/yr when trans-auroral line-based densities are considered
instead. We compare them with the corresponding molecular mass outflow rates (8
– 16 Msun/yr), derived from CO(2-1) ALMA observations at 0.2″ resolution. Both
phases show lower outflow mass rates than those expected from observational
scaling relations where uniform assumptions on the outflow properties were
adopted. This might be indicating that the AGN luminosity is not the only
driver of massive outflows and/or that these relations need to be re-scaled
using accurate outflow properties. We do not find a significant impact of the
outflows on the global star formation rates.
We present MEGARA (Multi-Espectr’ografo en GTC de Alta Resoluci’on para
Astronom’ia) Integral Field Unit (IFU) observations of 5 local type-2 quasars
(QSO2s, z $sim 0.1$) from the Quasar Feedback (QSOFEED) sample. These active
galactic nuclei (AGN) have bolometric luminosities of 10$^{45.5-46}$ erg/s and
stellar masses of $sim$10$^{11}$ M$_{odot}$. We explore the kinematics of the
ionized gas through the [O~III]$lambda$5007 $r{A}$ emission line. The nuclear
spectra of the 5 QSO2s, extracted in a circular aperture of $sim$ 1.2″ ($sim$
2.2 kpc) in diameter, show signatures of high velocity winds in the form of
broad (full width at half maximum; 1300$leq$FWHM$leq$2240 km/s and
blueshifted components. We find that 4 out of the 5 QSO2s present outflows that
we can resolve with our seeing-limited data, and they have radii ranging from
3.1 to 12.6 kpc. In the case of the two QSO2s with extended radio emission, we
find that it is well-aligned with the outflows, suggesting that low-power jets
might be compressing and accelerating the ionized gas in these radio-quiet
QSO2s. In the four QSO2s with spatially resolved outflows, we measure ionized
mass outflow rates of 3.3-6.5 Msun/yr when we use [S~II]-based densities, and
of 0.7-1.6 Msun/yr when trans-auroral line-based densities are considered
instead. We compare them with the corresponding molecular mass outflow rates (8
– 16 Msun/yr), derived from CO(2-1) ALMA observations at 0.2″ resolution. Both
phases show lower outflow mass rates than those expected from observational
scaling relations where uniform assumptions on the outflow properties were
adopted. This might be indicating that the AGN luminosity is not the only
driver of massive outflows and/or that these relations need to be re-scaled
using accurate outflow properties. We do not find a significant impact of the
outflows on the global star formation rates.
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