H  kinematics of the SINGS nearby galaxies survey -- I

Daigle, Olivier; Carignan, C.; Amram, P.; Hernandez, O.; Chemin, L.; Balkowski, C.; Kennicutt, Robert C.

doi:10.1111/j.1365-2966.2006.10002.x

Cited by 117 publications

(151 citation statements)

References 60 publications

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“…This is a good compromise between the different values reported in the literature ranging from D = 16.8 Mpc (Tully & Fisher 1988) to D = 22.6 Mpc (LEDA, 2006). Similarly to GB05 we will initially assume that the inclination angle and the position angle of NGC 4579's disk are i = 36 • and PA = 95 • , respectively, in rough agreement with previous determinations based on kinematical model fitting (e.g., Rubin et al 1999;Koopmann et al 2001;Daigle et al 2006) and photometric model fitting (e.g., Young & Currie 1998;Paturel et al 2000). These parameters will be further discussed in Sect.…”

Section: Aims Of This Papermentioning

confidence: 64%

Molecular gas in NUclei of GAlaxies (NUGA)

García‐Burillo

Fernández-García

Combes

et al. 2009

A&A

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In this paper we create a complete gravity torque map of the disk of the LINER/Seyfert 1.9 galaxy NGC 4579. We quantify the efficiency of angular momentum transport and search for signatures of secular evolution in the fueling process from r ∼ 15 kpc down to the inner r ∼ 50 pc around the active galactic nucleus (AGN). We use both the 1−0 and 2−1 line maps of 12 CO obtained with the Plateau de Bure Interferometer (PdBI) as part of the NUclei of Galaxies-(NUGA)-project. The CO(1−0) and CO(2−1) PdBI maps at 2.0 × 1.3 and 1.0 × 0.6 resolution, respectively, include the short spacing correction provided by IRAM-30 m data. We derive the stellar potential from an NIR (K band) wide field image of the galaxy. The K-band image, which reveals a large-scale stellar bar and a weak nuclear oval, together with a high-resolution Hi map of NGC 4579 obtained with the Very Large Array (VLA), allow us to extend the gravity torque analysis to the outer r ≥ 2 kpc disk. The bulk of the gas response traced by the new CO PdBI+30 m maps of NGC 4579 presented here follows the expected gas flow pattern induced by the bar potential in the presence of two inner Lindblad resonances (ILR) at r ∼ 500 pc and r ∼ 1.3 kpc. The morphology of the outer disk traced by Hi suggests that the neutral gas is currently piling up in a pseudo-ring formed by two winding spiral arms that are morphologically decoupled from the bar structure. The pseudo-ring is located inside the bar corotation (r CR ∼ 6 kpc) and close to the predicted position of the ultra harmonic resonance (UHR) (r UHR ∼ 3.8 kpc). The derived gravity torque budget in NGC 4579 shows that inward gas flow is occurring on different spatial scales in the disk. In the outer disk, the decoupling of the spiral allows the gas to efficiently populate the UHR region, and thus produce net gas inflow on intermediate scales. The corotation barrier seems to be overcome by secular evolution processes. The gas in the inner disk (r ≤ 2 kpc) is efficiently funneled by gravity torques down to r ∼ 300 pc. Closer to the AGN (r < 200 pc), gas feels negative torques due to the combined action of the large-scale bar and the inner oval. The two m = 2 modes act in concert to produce net gas inflow down to r ∼ 50 pc, providing clear smoking gun evidence of inward gas transport on short dynamical timescales (∼1−3 rotation periods).

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Section: Aims Of This Papermentioning

confidence: 64%

Molecular gas in NUclei of GAlaxies (NUGA)

García‐Burillo

Fernández-García

Combes

et al. 2009

A&A

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“…They confirm what Roberts (1969) had predicted theoretically: variations of 10 − 30 km s −1 in the velocity are found when the gas crosses the density wave. Bar-induced non-circular motions have also been analysed in the literature, and the first Garrido et al 2002 (GHASP), Daigle et al 2006a (SINGS sample) and Chemin et al 2006 (VIRGO sample), shown along with the characteristics of the data used in this paper. Note) The '-' denotes that there are no galaxies with that criteria (VIRGO, GHASP and this paper), or that no information about the seeing was presented (SINGS).…”

Section: Non-circular Motionsmentioning

confidence: 99%

“…In the Introduction, we mentioned the Hα FP kinematic surveys of Garrido et al 2002 (GHASP), Daigle et al 2006a (SINGS sample) and Chemin et al 2006 (VIRGO sample). These surveys have used instrumentation similar to GHαFaS: Cigale and FaNTOmM (FabryPerot de Nouvelle Technologie de l'Observatoire du Mont Mégantic 3 ).…”

Section: Comparison With Literature Datamentioning

confidence: 99%

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Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in FITS format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

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“…The agreement is within 20%, except where the CO flux approaches the detection limit of the BIMA SONG survey (R > ∼ 2 kpc). One advantage of applying Gaussian fits is that we can get better covering maps if we use a Hanning smoothing algorithm in the spectral direction before fitting the individual Gaussian profiles (e.g., Hernandez et al 2005;Daigle et al 2006). This procedure does not affect the line amplitude or shift.…”

Section: Molecular Gasmentioning

confidence: 99%

What powers the starburst activity of NGC 1068? Star-driven gravitational instabilities caught in the act

Romeo

Fathi

2016

Mon. Not. R. Astron. Soc.

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We explore the role that gravitational instability plays in NGC 1068, a nearby Seyfert galaxy that exhibits unusually vigorous starburst activity. For this purpose, we use the Romeo-Falstad disc instability diagnostics and data from BIMA SONG, SDSS and SAURON. Our analysis illustrates that NGC 1068 is a gravitationally unstable 'monster'. Its starburst disc is subject to unusually powerful instabilities. Several processes, including AGN/stellar feedback, try to quench such instabilities from inside out by depressing the surface density of molecular gas across the central kpc, but they do not succeed. Gravitational instability 'wins' because it is driven by the stars via their much higher surface density. In this process, stars and molecular gas are strongly coupled, and it is such a coupling that ultimately triggers local gravitational collapse/fragmentation in the molecular gas.

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H kinematics of the SINGS nearby galaxies survey -- I

Cited by 117 publications

References 60 publications

Molecular gas in NUclei of GAlaxies (NUGA)

Molecular gas in NUclei of GAlaxies (NUGA)

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

What powers the starburst activity of NGC 1068? Star-driven gravitational instabilities caught in the act

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