Circumnuclear Rings and Lindblad Resonances in Spiral Galaxies

Schmidt, E. O.; Mast, D.; Díaz, Rubén; Agüero, M. P.; Günthardt, G.; Gimeno, G.; Oío, G. A.; Gaspar, G.

doi:10.3847/1538-3881/ab2882

Cited by 12 publications

(22 citation statements)

References 65 publications

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“…3). However, it is still hard to predict the location and the size of the nuclear ring as it depends on several factors, such as the random turbulent motion of interstellar clouds, the sound speed of the gas, the pattern speed of the bar, and the bar strength (Patsis & Athanassoula 2000;Kim et al 2012;Schmidt et al 2019;Seo et al 2019). Nevertheless, our results confirm the existence of the nuclear molecular ring between two ILRs and close to the IILR.…”

Section: The Nuclear Ringmentioning

confidence: 57%

“…14. Inner rings located between the two ILRs are also found in other galaxies, such as NGC 1097, IC 1438, IC 4214, NGC 1512, and NGC 6753 (Piñol-Ferrer et al 2014Schmidt et al 2019) and could be explained by different scenarios. For example, Combes (1996) proposed that a nuclear ring forms between the IILR and the OILR when there are two ILRs.…”

Section: The Nuclear Ringmentioning

confidence: 89%

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Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Trejo

Espada

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present results obtained from ALMA CO (2–1) data of the double-barred galaxy NGC 3504. With three times higher angular resolution (∼ 0.″8) than previous studies, our observations reveal an inner molecular gas bar, a nuclear ring, and four inner spiral arm-like structures in the central 1 kpc region. Furthermore, the CO emission is clearly aligned with the two dust lanes in the outer bar region, with differences in shape and intensity between them. The total molecular gas mass in the observed region (50″ × 57″) is estimated to be ∼3.1 × 109 M⊙, which is 17 per cent of the stellar mass. We used the Kinemetry package to fit the velocity field and found that circular motion strongly dominates at R = 0.3 − 0.8 kpc, but radial motion becomes important at R < 0.3 kpc and R = 1.0 − 2.5 kpc, which is expected due to the presence of the inner and outer bars. Finally, assuming that the gas moves along the dust lanes in the bar rotating frame, we derived the pattern speed of the outer bar to be 18 ± 5 km s−1 kpc−1, the average streaming velocities on each of the two dust lanes to be 165 and 221 km s−1, and the total mass inflow rate along the dust lanes to be 12 M⊙ yr−1. Our results give a new example of an inner gas bar within a gas-rich double-barred galaxy and suggest that the formation of double-barred galaxies could be associated with the existence of such gas structures.

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Section: The Nuclear Ringmentioning

confidence: 57%

Section: The Nuclear Ringmentioning

confidence: 89%

Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Trejo

Espada

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Section: Samples and Datamentioning

confidence: 99%

“…In addition, we analyze PS1 images of IC 1438 and NGC 2835 whose frequency curves were derived by Schmidt et al (2019) to compare the results from this analysis on photometry with those measured from spectroscopy. Schmidt et al (2019) derived their frequency curves from the potential by fitting the rotation curves along with three other galaxies. They measured the corotation radius using two photometric estimations: Fourier analysis of azimuthal profile (Puerari & Dottori 1997) and the change of the dust lane (Roberts et al 1979;Prendergast 1983).…”

Section: Samples and Datamentioning

confidence: 99%

“…Each of these curves decreases with increasing galactocentric radius, such that if the bar pattern speed decreases with time, the radius of corotation, the locations of the inner and outer Lindblad resonances (ILR, OLR) and ultraharmonic resonance (inner 4:1 resonance, or UHR) all increase with time. To construct frequency curves, Schmidt et al (2019) estimated a potential profile from velocity curves by assuming an axisymmetric Miyamoto-Nagai gravitational potential (Miyamoto & Nagai 1975). Garma-Oehmichen et al (2020) obtained angular velocity curves from spectroscopic data by fitting the VELFIT model (Spekkens & Sellwood 2007).…”

Section: Introductionmentioning

confidence: 99%

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Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

Lee,

Park,

Hwang

et al. 2021

Preprint

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We test the idea that bar pattern speeds decrease with time owing to angular momentum exchange with a dark matter halo. If this process actually occurs, then the locations of the corotation resonance and other resonances should generally increase with time. We therefore derive the angular velocity Ω and epicyclic frequency κ as functions of galactocentric radius for 85 barred galaxies using photometric data. Mass maps are constructed by assuming a dynamical mass-to-light ratio and then solving the Poisson equation for the gravitatonal potential. The location of Lindblad resonances and the corotation resonance radius are then derived using the standard precession frequency curves in conjunction with bar pattern speeds recently estimated from the Tremaine-Weinberg method as applied to Integral Field Spectroscopy (IFS) data. Correlations between physical properties of bars and their host galaxies indicate that bar length and the corotation radius depend on the disk circular velocity while bar strength and pattern speed do not. As the bar pattern speed decreases, bar strength, length, and corotation radius incease, but when bars are subclassified into fast, medium, and slow domains, no significant change in bar length is found. Only a hint of an increase of bar strength from fast to slow bars is found. These results suggest that bar length in galaxies undergoes little evolution, being instead determined mainly by the size of their host galaxy.

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The Hiin Ring Galaxies Survey (Hi-RINGS)—Effects of the bar on the Higas in ring galaxies

Murugeshan

Džudžar

Bagge

et al. 2023

Publ. Astron. Soc. Aust.

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We present a new high-resolution neutral atomic hydrogen (H i) survey of ring galaxies using the Australia Telescope Compact Array (ATCA). We target a sample of 24 ring galaxies from the Buta (1995) Southern Ring Galaxy Survey Catalogue in order to study the origin of resonance-, collisional- and interaction-driven ring galaxies. In this work, we present an overview of the sample and study their global and resolved H i properties. In addition, we also probe their star formation properties by measuring their star formation rates (SFR) and their resolved SFR surface density profiles. We find that a majority of the barred galaxies in our sample are H i deficient, alluding to the effects of the bar in driving their H i deficiency. Furthermore, for the secularly evolving barred ring galaxies in our sample, we apply Lindblad’s resonance theory to predict the location of the resonance rings and find very good agreement between predictions and observations. We identify rings of H i gas and/or star formation co-located at one or the other major resonances. Lastly, we measure the bar pattern speed (Ωbar) for a sub-sample of our galaxies and find that the values range from 10 – 90 km s−1kpc−1, in good agreement with previous studies.

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Circumnuclear Rings and Lindblad Resonances in Spiral Galaxies

Cited by 12 publications

References 65 publications

Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data

Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies

The Hiin Ring Galaxies Survey (Hi-RINGS)—Effects of the bar on the Higas in ring galaxies

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