Searching for non-axisymmetries in NGC 6503: a weak end-on bar

Naray, Rachel Kuzio de; Arsenault, Cameron A.; Spekkens, Kristine; Sellwood, J. A.; McDonald, Michael; Simon, Joshua D.; Teuben, Peter

doi:10.1111/j.1365-2966.2012.22126.x

Cited by 32 publications

(27 citation statements)

References 43 publications

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“…If we ignore all kinematics pertaining to the filament (i.e., the western blueshifted velocities of Figure 3), the remaining kinematics resemble disk rotation. This observation concurs with those made in Phillips et al (1983), who measured the kinematics of low-ionization lines surrounding the nucleus and found the velocities fit a disk model with a rotation axis of In order to confirm that these kinematics could be due rotation of the host disk, We used DiskFit (Spekkens & Sellwood 2007;Sellwood & Sánchez 2010;Kuzio de Naray et al 2012), a publicly available code which fits non-parametric models to a given velocity field, in order to confirm that these kinematics could be due rotation of the host disk. We applied the rotation model to the kinematics, using the single line plus red component velocity field, an initial rotational major axis position angle of −135…”

Section: Observationssupporting

confidence: 84%

A MINOR MERGER CAUGHT IN THE ACT OF FUELING THE ACTIVE GALACTIC NUCLEUS IN Mrk 509

Fischer

Crenshaw

Kraemer

et al. 2015

ApJ

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In recent observations by the Hubble Space Telescope (HST) as part of a campaign to discover locations and kinematics of AGN outflows, we found that Mrk 509 contains a 3 (∼2100 pc) linear filament in its central region. Visible in both optical continuum and [O iii] imaging, this feature resembles a "check mark" of several knots of emission that travel northwest to southeast before jutting toward the nucleus from the southwest. Space Telescope Imaging Spectrograph (STIS/HST) observations along the inner portion of the filament reveal redshifted velocities, indicating that the filament is inflowing. We present further observations of the nucleus in Mrk 509 using the Gemini Near-Infrared Integral Field Spectrograph, from which we conclude that this structure cannot be related to previously studied, typical narrow line region outflows and instead embodies the remains of an ongoing minor merger with a gas-rich dwarf galaxy, therefore providing a great opportunity to study the fueling of an AGN by a minor merger in progress.

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Section: Observationssupporting

confidence: 84%

A MINOR MERGER CAUGHT IN THE ACT OF FUELING THE ACTIVE GALACTIC NUCLEUS IN Mrk 509

Fischer

Crenshaw

Kraemer

et al. 2015

ApJ

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“…6) shows a rotation component, with the north-eastern side of the disc approaching and the south-western side receding with a velocity amplitude of about 80 km s −1 . To derive the systemic velocity (V s ), orientation of the line of nodes ( 0 ), inclination (i) and eccentricity (e) of the disc, we fitted the stellar velocity field using the DISKFIT code (Spekkens & Sellwood 2007;Sellwood & Sánchez 2010;Kuzio et al 2012).…”

Section: Stellar Kinematics and The Mass Of A Supermassive Black Holementioning

confidence: 99%

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

Riffel

Storchi‐Bergmann

2015

Mon. Not. R. Astron. Soc.

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We present near-infrared emission-line flux distributions, excitation and kinematics, as well as stellar kinematics, of the inner 520 × 520 pc 2 of the Seyfert 2 galaxy NGC 5929. The observations were performed with Gemini's Near-Infrared Integral Field Spectrograph (NIFS) at a spatial resolution of ∼20 pc and spectral resolution of 40 km s −1 in the J and K l bands. The flux distributions of H 2 , [Fe II], [P II] and H recombination lines are extended over most of the field of view, with the highest intensity levels observed along PA = 60/240• , and well correlated with the radio emission. The H 2 and [Fe II] line emission originated in thermal processes, mainly due to heating of the gas by X-rays from the central active galactic nucleus (AGN). The contribution of shocks due to the radio jet is observed at locations co-spatial with the radio hotspots at 0.50 arcsec north-east and 0.60 arcsec south-west of the nucleus, as evidenced by the emission-line ratio and gas kinematics. The stellar kinematics shows rotation with an amplitude at 250 pc from the nucleus of ∼200 km s −1 after correcting for the inferred inclination of 18.3• . The stellar velocity dispersion obtained from the integrated K-band spectrum is σ * = 133 ± 8 km s −1 , which implies a mass for the supermassive black hole of M • = 5.2 1.6 −1.2 × 10 7 M , using the M • -σ * relation. The gas kinematics present three components: (1) gas in the plane of the galaxy in counter-rotation relative to the stars; (2) an outflow perpendicular to the radio jet that seems to be due to an equatorial AGN outflow; and (3) turbulence of the gas observed in association with the radio hotspots, supporting an interaction of the radio jet with the gas of the disc. We estimated the masses of ionized gas and warm molecular gas to be ∼1.3 × 10 6 M and ∼470 M , respectively.

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“…Spekkens and collaborators later developed DiskFit (Sellwood & Spekkens 2015) 2 , an improved version of velfit which is not strictly limited to constant inclination and can also operate on photometric data. Kuzio de Naray et al (2012) applied DiskFit to Hα, CO and H i kinematic data of NGC 6503.…”

Section: Introductionmentioning

confidence: 99%

Radial gas motions in The H i Nearby Galaxy Survey (THINGS)

Schmidt

Bigiel

Klessen

et al. 2016

Mon. Not. R. Astron. Soc.

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The study of 21 cm line observations of atomic hydrogen allows detailed insight into the kinematics of spiral galaxies. We use sensitive high-resolution VLA data from The HI Nearby Galaxy Survey (THINGS) to search for radial gas flows primarily in the outer parts (up to 3 × r 25 ) of ten nearby spiral galaxies. Inflows are expected to replenish the gas reservoir and fuel star formation under the assumption that galaxies evolve approximately in steady state. We carry out a detailed investigation of existing tilted ring fitting schemes and discover systematics that can hamper their ability to detect signatures of radial flows. We develop a new Fourier decomposition scheme that fits for rotational and radial velocities and simultaneously determines position angle and inclination as a function of radius. Using synthetic velocity fields we show that our novel fitting scheme is less prone to such systematic errors and that it is well suited to detect radial inflows in disks. We apply our fitting scheme to ten THINGS galaxies and find clear indications of, at least partly previously unidentified, radial gas flows, in particular for NGC 2403 and NGC 3198 and to a lesser degree for NGC 7331, NGC 2903 and NGC 6946. The mass flow rates are of the same order but usually larger than the star formation rates. At least for these galaxies a scenario in which continuous mass accretion feeds star formation seems plausible. The other galaxies show a more complicated picture with either no clear inflow, outward motions or complex kinematic signatures.

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Searching for non-axisymmetries in NGC 6503: a weak end-on bar

Cited by 32 publications

References 43 publications

A MINOR MERGER CAUGHT IN THE ACT OF FUELING THE ACTIVE GALACTIC NUCLEUS IN Mrk 509

A MINOR MERGER CAUGHT IN THE ACT OF FUELING THE ACTIVE GALACTIC NUCLEUS IN Mrk 509

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

Radial gas motions in The H i Nearby Galaxy Survey (THINGS)

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