OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES,

By F. Muller-S'anchez, A. Prieto, E. Hicks, H. Vives-Arias, Roger Davies, M. Malkan, L. Tacconi, R. I. D. A. D. Canarias, U. L. Laguna, U. Washington and 4 more. 2011

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As part of an extensive study of the physical properties of active galactic nuclei (AGNs) we report high spatial resolution near-IR integral-field spectroscopy of the narrow-line region (NLR) and coronal-line region (CLR) of seven Seyfert galaxies. These measurements elucidate for the first time the two-dimensional spatial distribution and kinematics of the recombination line Brγ and high-ionization lines [Si vi], [Al ix], and [Ca viii] on scales <300 pc from the AGN. The observations reveal kinematic signatures of rotation and outflow in the NLR and CLR. The spatially resolved kinematics can be modeled as a combination of an outflow bicone and a rotating disk coincident with the molecular gas. High-excitation emission is seen in both components, suggesting it is leaking out of a clumpy torus. While NGC 1068 (Seyfert 2) is viewed nearly edge-on, intermediate-type Seyferts are viewed at intermediate angles, consistent with unified schemes. A correlation between the outflow velocity and the molecular gas mass in r < 30 pc indicates that the accumulation of gas around the AGN increases the collimation and velocity of the outflow. The outflow rate is 2–3 orders of magnitude greater than the accretion rate, implying that the outflow is mass loaded by the surrounding interstellar medium (ISM). In half of the observed AGNs, the kinetic power of the outflow is of the order of the power required by two-stage feedback models to be thermally coupled to the ISM and to match the MBH–σ* relation. In these objects, the radio jet is clearly interacting with the ISM, indicative of a link between jet power and outflow power.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8605539a099d94e801453aa722461082c8804f61

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Citations in the corpus

Revisiting the Unified Model of Active Galactic Nuclei (2015, methodology): “The IFU measurements of Müller-Sánchez et al. (2011) resulted in a kinematic map based on [Sivi]λ1.”
Molecular line emission in NGC 1068 imaged with ALMA: I. An AGN-driven outflow in the dense molecular gas (2014, background): “This is significantly above the mass load rate estimated on similar spatial scales for the ionized gas outflow: ∼ 9 M yr−1 (Müller-Sánchez et al. 2011).”
Massive molecular outflows and evidence for AGN feedback from CO observations (2013, methodology): “While various techniques have been used to identify other phases of outflows in active galaxies, both locally (e.g. Rupke & Veilleux 2011, 2013b; Müller-Sánchez et al. 2011; Mullaney et al. 2013; Emonts et al. 2005; Morganti et al. 2003, 2005; Martin 2005; Soto et al. 2012; Rodríguez Zaurín et al.…”
DUST IN THE POLAR REGION AS A MAJOR CONTRIBUTOR TO THE INFRARED EMISSION OF ACTIVE GALACTIC NUCLEI (2013, methodology): “Several of these lines show blue-shifted cores (e.g. Reunanen et al. 2003; Hicks et al. 2009) and high velocities of up to 1300 km/s (Kraemer et al. 2001; Rodŕıguez-Ardila et al. 2006; Müller-Sánchez et al. 2011), meaning that gas in these extended line-emitting regions is outflowing.”
THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS (2013, background): “However, it differs from those of the narrow line region (NLR) outflows in nearby Seyfert galaxies, which have random orientations with respect to the galaxy disk (Crenshaw & Kraemer 2000; Crenshaw et al. 2000; Fischer et al. 2010b, 2011; Müller-Sánchez et al. 2011).”
Determining Inclinations of Active Galactic Nuclei Via Their Narrow-Line Region Kinematics (2012, result): “These results disagree with previous correlations found by Müller-Sánchez et al. (2011) using similar NLR modeling techniques, where opening angle, maximum outflow velocity, and molecular hydrogen mass within the inner torus, each appeared dependent on one another, indicating that more massive…”
Quasar feedback and the origin of radio emission in radio-quiet quasars (2014, background): “…for their production is excitation by quasar photo-ionization fairly close to the nucleus, akin to an “intermediate” region between the very compact broad-line region and a more extended narrow-line one (Grandi 1978; Gelbord et al. 2009; Mullaney et al. 2009; Müller-Sánchez et al. 2011).”
Observational evidence of quasar feedback quenching star formation at high redshift (2011, background): “The outflow may even be intrinsically symmetric, but the opposite (receding) outflow is likely to be obscured by dust in the host galaxy disk (as observed in local AGNs, Müller-Sánchez et al., 2011).”