The role of the host galaxy kinematics on nuclear activity

Dumas, G.; Mundell, C. G.; Emsellem, Éric; Nagar, Neil M.

doi:10.1002/asna.200811046

Cited by 2 publications

(3 citation statements)

References 169 publications

(324 reference statements)

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“…Its motion agrees with that of the ionized gas in the inner few arcseconds, and disagrees with that of the stellar disk (Sil'chenko & Afanasiev 2004;Dumas et al 2007). The line of largest receding velocity then twists counterclockwise through more than 90…”

Section: Discussionsupporting

confidence: 55%

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NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Sparke

Moorsel

Erwin

et al. 2007

The Astronomical Journal

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NGC 2655, a nearby bright S0/a galaxy in a loose group, has strongly asymmetric central dust lanes and an extended disk of neutral hydrogen gas. Here we present deep optical images showing tidal arms and regions of diffuse starlight well beyond the main galaxy, suggestive of a recent merger. Our maps in the 21 cm line show a layer of neutral hydrogen extending to at least 7.5 or 40 kpc from the center, with a broken streamer of gas trailing off toward the small neighbor galaxy UGC 4714. The global profile has sloping "shoulders" of extreme-velocity gas, usually a sign of interaction. The diffuse stellar light corresponds generally but not in detail with the distribution of H i. In particular, the stellar light of the main tidal arm extends beyond the H i layer, which is limb-brightened as if it had been compressed from outside. The pattern of gas velocities is generally bisymmetric, but the H i layer is strongly warped; it does not share the kinematics of the stellar disk. The gas orbits twist by at least 90• between 1 and 3 of the center, as the H i layer appears to warp through edge-on. The complex optical tails and H i dynamics suggest that the galaxy has undergone multiple mergers. Both at small and at large radii, the gas layer twists in a trailing sense relative to its orbital motion. If the twist results from differential precession in the galaxy's gravitational potential, this would indicate that the dark halo is prolate, elongated along the rotation axis of the disk.

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Section: Discussionsupporting

confidence: 55%

“…Sil 'chenko & Afanasiev (2004) and Dumas et al (2007) performed kinematic observations within a few arcseconds of the galaxy center, to find ionized gas in ordered rotation with the largest receding velocities close to the line PA = 180…”

Section: Introductionmentioning

confidence: 99%

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Sparke

Moorsel

Erwin

et al. 2007

The Astronomical Journal

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“…This is supported by imaging spectroscopic observations of nearby Seyfert galaxies, which show that the gaseous and stellar kinematics are coupled (e.g. Dumas et al 2008). On the other hand, the wing is much broader than the core but narrower than broad lines, indicating that its emitting region is much closer to the nuclei than the core component.…”

Section: Distinction Between the [O Iii] Core And Wingmentioning

confidence: 63%

Connection Between Mid-Infrared Emission Properties and Narrow-Line Region Outflows in Type 1 Active Galactic Nuclei

Zhang

Wang

Yan

et al. 2013

ApJ

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The location of warm dust producing the Mid-infrared (MIR) emission in Type 1 Active Galactic Nuclei (AGNs) is complex and not yet fully known. We explore this problem by studying how the MIR covering factor (CF MIR = L MIR /L bol ) correlates with the fundamental parameters of AGN accretion process (such as L bol , black hole mass M BH , and Eddington ratio L/L Edd ) and the properties of narrow emission lines (as represented by [O III] λ5007), using large data sets derived from the Sloan Digital Sky Spectroscopic Survey (SDSS) and the Wide Infrared Sky Survey (WISE). Firstly we find that the luminosity of the [O III] wing component (L wing ) correlates more tightly with the continuum luminosity (λL λ (5100)) than the luminosity of the line core component (L core ) does, which is in line with our previous conclusion that the wing component, generally blueshifted, originates from the polar outflows in the inner narrow-line region (NLR). We then find that the MIR CF shows the strongest correlation with L wing /L bol rather than with L core /L bol or the above fundamental AGN parameters, and the correlation becomes stronger as the infrared wavelength increases. We also confirm the anticorrelations of CF MIR with L bol and M BH , and the lack of dependence of CF MIR on the Eddington ratio. These results suggest that a large fraction of the warm dust producing MIR emission in AGNs is likely embedded in polar outflows in the NLR instead of in the torus.

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The role of the host galaxy kinematics on nuclear activity

Cited by 2 publications

References 169 publications

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Connection Between Mid-Infrared Emission Properties and Narrow-Line Region Outflows in Type 1 Active Galactic Nuclei

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