A Magellan-Imacs-Ifu Search for Dynamical Drivers of Nuclear Activity. I. Reduction Pipeline and Galaxy Catalog

Westoby, Paul; Mundell, C. G.; Nagar, Neil M.; Maciejewski, Witold; Emsellem, Éric; Roth, Martin; Gerssen, J.; Baldry, I. K.

doi:10.1088/0067-0049/199/1/1

Cited by 11 publications

(15 citation statements)

References 72 publications

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“…Radial profiles of the electron density are shown in . These values are roughly consistent (although at the upper limit) with the usually assumed (e.g., Liu et al 2013b, Harrison et al 2014, Carniani et al 2015 or measured values in the literature (e.g., Holt et al 2006, Westoby et al 2012, Rodríguez Zaurín et al 2013, 100-500 cm −3 . Assuming case B recombination (Osterbrock 1989), we calculate the ionized gas mass based on the measured Hα luminosity at each spaxel: …”

Section: Definitionssupporting

confidence: 91%

Unravelling the Complex Structure of Agn-Driven Outflows. Ii. Photoionization and Energetics

Karouzos

Woo

Bae

2016

ApJ

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Outflows have been shown to be prevalent in galaxies hosting luminous active galactic nuclei (AGNs) and present a physically plausible way to couple the AGN energy output with the interstellar medium of their hosts. Despite their prevalence, accurate characterization of these outflows has been challenging. In the second of a series of papers, we use Gemini Multi-Object Spectrograph IFU data of 6 local (z< 0.1) and moderate-luminosity Type 2 AGNs to study the ionization properties and energetics of AGN-driven outflows. We find strong evidence that connect the extreme kinematics of the ionized gas with the AGN photoionization. The kinematic component related to the AGN-driven outflow is clearly separated from other kinematic components, such as virial motions or rotation, on the velocity and velocity dispersion diagram. Our spatially resolved kinematic analysis reveals that from 30% up to 90% of the total mass and kinetic energy of the outflow is contained within the central kpc of the galaxy. The spatially integrated mass and kinetic energy of the gas entrained in the outflow correlates well with the AGN bolometric luminosity and results in energy conversion efficiencies between 0.01% and 1%. Intriguingly, we detect ubiquitous signs of ongoing circumnuclear star formation. Their small size, the centrally contained mass and energy, and the universally detected circumnuclear star formation cast doubts on the potency of these AGN-driven outflows as agents of galaxy-scale negative feedback.

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Section: Definitionssupporting

confidence: 91%

Unravelling the Complex Structure of Agn-Driven Outflows. Ii. Photoionization and Energetics

Karouzos

Woo

Bae

2016

ApJ

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“…Several works indeed show that the gas and stellar kinematics are not always consistent with each other in the central region of galaxies (Davies et al 2014;Westoby et al 2012;Stoklasová et al 2009). …”

Section: Kinematics Of the Emitting Gasmentioning

confidence: 99%

Feeding versus feedback in AGN from near-infrared IFU observations XI: NGC 2110

Diniz

Riffel

Storchi‐Bergmann

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a two-dimensional mapping of the gas flux distributions, as well as of the gas and stellar kinematics in the inner 220 pc of the Seyfert galaxy NGC 2110, using K-band integral field spectroscopy obtained with the Gemini NIFS at a spatial resolution of ≈ 24 pc and spectral resolution of ≈ 40 km s −1 . The H 2 λ 2.1218 µm emission extends over the whole field-of-view and is attributed to heating by X-rays from the AGN and/or by shocks, while the Brγ emission is restricted to a bi-polar region extending along the South-East-NorthWest direction. The masses of the warm molecular gas and of the ionized gas are M H 2 ≈ 1.4 × 10 3 M ⊙ and M H II ≈ 1.8 × 10 6 M ⊙ , respectively. The stellar kinematics present velocity dispersions reaching 250 km s −1 , and a rotation pattern reaching an amplitude of 200 km s −1 . The gas velocity fields present a similar rotation pattern but also additional components that we attribute to inflows and outflows most clearly observed in the molecular gas emission. The inflows are observed beyond the inner 70 pc and are associated to a spiral arm seen in blueshift to the North-East and another in redshift to the South-West. We have estimated a mass inflow rate in warm molecular gas of ≈ 4.6 × 10 −4 M ⊙ yr −1 . Within the inner 70 pc, another kinematic component is observed in the H 2 emission that can be interpreted as due to a bipolar nuclear outflow oriented along the East-West direction, with a mass-outflow rate of ≈ 4.3 × 10 −4 M ⊙ yr −1 in warm H 2 .

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“…5. We apply the same PA and i when fitting a disk model to the gas kinematics, noting that unless there are clear indications to the contrary, and based on kinematics measured in early and late type galaxies (Sarzi et al 2006;Dumas et al 2007;Davies et al 2011;Westoby et al 2012), our working assumption is that the stellar and molecular gas kinematics are aligned. However, we refer the reader to Section 8 for a discussion of this point.…”

Section: Disk Fits To Stellar Kinematicsmentioning

confidence: 99%

“…Previous studies of matched active and inactive galaxy samples based on optical integral field spectroscopy, such as Dumas et al (2007) and Westoby et al (2012) which we discuss in Sec. 8, have tended to focus on larger scales, from a few kpc down to their resolution limit of 100-200 pc (or more typically 600 pc in the latter study).…”

Section: Introductionmentioning

confidence: 99%

Fueling Active Galactic Nuclei. Ii. Spatially Resolved Molecular Inflows and Outflows

Davies

Maciejewski

Hicks

et al. 2014

ApJ

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128

166

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We analyse the 2-dimensional distribution and kinematics of the stars as well as molecular and ionised gas in the central few hundred parsecs of 5 active and 5 matched inactive galaxies. The equivalent widths of the Brγ line indicate there is no on-going star formation in their nuclei, although recent (terminated) starbursts are possible in the active galaxies. The stellar velocity fields show no signs of non-circular motions, while the 1-0 S(1) H 2 kinematics exhibit significant deviations from simple circular rotation. In the active galaxies the H 2 kinematics reveal inflow and outflow superimposed on disk rotation. Steady-state circumnuclear inflow is seen in three AGN, and hydrodynamical models indicate it can be driven by a large scale bar. In three of the five AGN, molecular outflows are spatially resolved. The outflows are oriented such that they intersect, or have an edge close to, the disk -which may be the source of molecular gas in the outflow. The relatively low speeds imply the gas will fall back onto the disk; and with moderate outflow rates, they will have only a local impact on the host galaxy. H 2 was detected in two inactive galaxies. These exhibit chaotic circumnuclear dust morphologies and have molecular structures that are counter-rotating with respect to the main gas component, which could lead to gas inflow in the near future. In our sample, all four galaxies with chaotic dust morphology in the circumnuclear region exist in moderately dense groups with 10-15 members where accretion of stripped gas can easily occur.

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A Magellan-Imacs-Ifu Search for Dynamical Drivers of Nuclear Activity. I. Reduction Pipeline and Galaxy Catalog

Cited by 11 publications

References 72 publications

Unravelling the Complex Structure of Agn-Driven Outflows. Ii. Photoionization and Energetics

Unravelling the Complex Structure of Agn-Driven Outflows. Ii. Photoionization and Energetics

Feeding versus feedback in AGN from near-infrared IFU observations XI: NGC 2110

Fueling Active Galactic Nuclei. Ii. Spatially Resolved Molecular Inflows and Outflows

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