ARRAKIS: atlas of resonance rings as known in the S<sup>4</sup>G

Comerón, Sébastien; Salo, H.; Laurikainen, Eija; Knapen, Johan H.; Buta, Ronald J.; Herrera-Endoqui, M.; Laine, Jarkko; Holwerda, Benne W.; Sheth, Kartik; Regan, Michael W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Paz, A. Gil de; Menéndez‐Delmestre, Karín; Seibert, Mark; Mizusawa, Trisha; Kim, T.; Erroz-Ferrer, Santiago; Gadotti, Dimitri A.; Athanassoula, E.; Bosma, A.; Ho, Luis C.

doi:10.1051/0004-6361/201321633

Cited by 108 publications

(137 citation statements)

References 98 publications

(189 reference statements)

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“…Buta & Combes 1996;van der Laan et al 2013). This seems to be the same structure as the inner pseudo-ring identified by Comerón et al (2014) around R ∼ 20 (which is star-forming, Comerón 2013). It becomes especially obvious in the dust component separated by the ICA correction of the 3.6 µm image (second panels of Fig.…”

Section: Inflow Rate In M 51supporting

confidence: 59%

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Querejeta

Meidt

Schinnerer

et al. 2016

A&A

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The transport of gas towards the centre of galaxies is critical for black hole feeding and, indirectly, it can control active galactic nucleus (AGN) feedback. We have quantified the molecular gas inflow in the central R < 1 kpc of M 51 to be 1 M /yr, using a new gravitational torque map and the molecular gas traced by the Plateau de Bure Interferometer Arcsecond Whirlpool Survey (PAWS). The nuclear stellar bar is responsible for this gas inflow. We also used torque profiles to estimate the location of dynamical resonances, and the results suggest a corotation for the bar CR bar ∼ 20 , and a corotation for the spiral CR sp ∼ 100 . We demonstrate how important it is to correct 3.6 µm images for dust emission when gravitational torques are to be computed, and we examine further sources of uncertainty. Our observational measurement of gas inflow can be compared with nuclear molecular outflow rates and provide useful constraints for numerical simulations.

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Section: Inflow Rate In M 51supporting

confidence: 59%

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Querejeta

Meidt

Schinnerer

et al. 2016

A&A

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“…These are cases in which the spiral arms strongly influence the potential in the bar region, where both maxima are determined by the combined contribution of the two non-axisymmetric stellar structures and occasionally reach beyond the bar limit. In the case of the ellipticity, bars with r ε /r vis > 1 are explained by the presence of spiral arms and rings, as discussed in E2005 and Comerón et al (2014).…”

Section: Estimation Of Bar Lengths and Ellipticitiesmentioning

confidence: 91%

“…• ) used in Comerón et al (2014) and recommended in Zou et al (2014). Of these non-highly inclined galaxies, 860 are barred according to B2015, forming our sample of barred galaxies for which bar lengths are measured visually.…”

Section: Selection Of Subsamplesmentioning

confidence: 99%

Characterization of galactic bars from 3.6μm S⁴G imaging

Díaz-García

Salo

Laurikainen

et al. 2016

A&A

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Context. Stellar bars play an essential role in the secular evolution of disk galaxies because they are responsible for the redistribution of matter and angular momentum. Dynamical models predict that bars become stronger and longer in time, while their rotation speed slows down. Aims. We use the Spitzer Survey of Stellar Structure in Galaxies (S 4 G) 3.6 µm imaging to study the properties (length and strength) and fraction of bars at z = 0 over a wide range of galaxy masses (M * ≈ 10 8 −10 11 M ) and Hubble types (−3 ≤ T ≤ 10). Methods. We calculated gravitational forces from the 3.6 µm images for galaxies with a disk inclination lower than 65• . We used the maximum of the tangential-to-radial force ratio in the bar region (Q b ) as a measure of the bar-induced perturbation strength for a sample of ∼600 barred galaxies. We also used the maximum of the normalized m = 2 Fourier density amplitude (A max 2 ) and the bar isophotal ellipticity (ε) to characterize the bar. Bar sizes were estimated i) visually; ii) from ellipse fitting; iii) from the radii of the strongest torque; and iv) from the radii of the largest m = 2 Fourier amplitude in the bar region. By combining our force calculations with the H  kinematics from the literature, we estimated the ratio of the halo-to-stellar mass (M h /M * ) within the optical disk and by further using the universal rotation curve models, we obtained a first-order model of the rotation curve decomposition of 1128 disk galaxies. Results. We probe possible sources of uncertainty in our Q b measurements: the assumed scale height and its radial variation, the influence of the spiral arms torques, the effect of non-stellar emission in the bar region, and the dilution of the bar forces by the dark matter halo (our models imply that only ∼10% of the disks in our sample are maximal). We find that for early-and intermediate-type disks (−3 ≤ T < 5), the relatively modest influence of the dark matter halo leads to a systematic reduction of the mean Q b by about 10−15%, which is of the same order as the uncertainty associated with estimating the vertical scale height. The halo correction on Q b becomes important for later types, implying a reduction of ∼20−25% for T = 7−10. Whether the halo correction is included or not, the mean Q b shows an increasing trend with T . However, the mean A max 2 decreases for lower mass late-type systems. These opposing trends are most likely related to the reduced force dilution by bulges when moving towards later type galaxies. Nevertheless, when treated separately, both the early-and late-type disk galaxies show a strong positive correlation between Q b and A max 2 . For spirals the mean ε ≈ 0.5 is nearly independent of T , but it drops among S0s (≈0.2). The Q b and ε show a relatively tight dependence, with only a slight difference between early and late disks. For spirals, all our bar strength indicators correlate with the bar length (scaled to isophotal size). Late-type bars are longer than previously found in the literature. The bar fraction...

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“…We believe that this scenario is probably the most common among early-type discs, namely, among lenticular galaxies which possess outer rings in more than half of all cases (Comerón et al 2014). Interestingly, the frequency of strong bars diminishes among lenticular galaxies compared to spirals (Laurikainen et al 2011(Laurikainen et al , 2013, while the frequency of outer rings rises (Comerón et al 2014). …”

Section: Interstellar Gas In Ring Galaxiesmentioning

confidence: 87%

“…Though the rings are certainly stellar structures, they often contain gas and demonstrate some level of star formation. For example, a recent catalogue of ring structures derived from the Spitzer Survey of Stellar Structure in Galaxies (Sheth et al 2010), ARRAKIS (Comerón et al 2014), includes outer stellar rings detected in 50-60% of all nearby S0 galaxies (Laurikainen et al 2011;Comerón et al 2014 half of all rings in S0s are seen in the ultraviolet, in the NUVband being mapped by the GALEX space telescope, and so revealing recent star formation (Kostiuk & Sil'chenko 2015). In early-type (S0) disc galaxies the star formation is mainly organized in large-scale rings (Pogge & Eskridge 1993;Salim et al 2012), and the neutral-hydrogen distributions are also ring-like (Van Driel & van Woerden 1991).…”

Section: Introductionmentioning

confidence: 99%

Magnetic fields in ring galaxies

Moss

Михайлов

Сильченко

et al. 2016

A&A

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Context. Many galaxies contain magnetic fields supported by galactic dynamo action. The investigation of these magnetic fields can be helpful for understanding galactic evolution; however, nothing definitive is known about magnetic fields in ring galaxies. Aims. Here we investigate large-scale magnetic fields in a previously unexplored context, namely ring galaxies, and concentrate our efforts on the structures that appear most promising for galactic dynamo action, i.e. outer star-forming rings in visually unbarred galaxies. Methods. We use tested methods for modelling α − Ω galactic dynamos, taking into account the available observational information concerning ionized interstellar matter in ring galaxies. Results. Our main result is that dynamo drivers in ring galaxies are strong enough to excite large-scale magnetic fields in the ring galaxies studied. The variety of dynamo driven magnetic configurations in ring galaxies obtained in our modelling is much richer than that found in classical spiral galaxies. In particular, various long-lived transients are possible. An especially interesting case is that of NGC 4513, where the ring counter-rotates with respect to the disc. Strong shear in the region between the disc and the ring is associated with unusually strong dynamo drivers in such counter-rotators. The effect of the strong drivers is found to be unexpectedly moderate. With counter-rotation in the disc, a generic model shows that a steady mixed parity magnetic configuration that is unknown for classical spiral galaxies, may be excited, although we do not specifically model NGC 4513. Conclusions. We deduce that ring galaxies constitute a morphological class of galaxies in which identification of large-scale magnetic fields from observations of polarized radio emission, as well as dynamo modelling, may be possible. Such studies have the potential to throw additional light on the physical nature of rings, their lifetimes, and evolution.

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ARRAKIS: atlas of resonance rings as known in the S⁴G

Cited by 108 publications

References 98 publications

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Characterization of galactic bars from 3.6μm S⁴G imaging

Magnetic fields in ring galaxies

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ARRAKIS: atlas of resonance rings as known in the S4G

Cited by 108 publications

References 98 publications

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Gravitational torques imply molecular gas inflow towards the nucleus of M 51

Characterization of galactic bars from 3.6μm S4G imaging

Magnetic fields in ring galaxies

Contact Info

Product

Resources

About

ARRAKIS: atlas of resonance rings as known in the S⁴G

Characterization of galactic bars from 3.6μm S⁴G imaging