On the morphology of dust lanes in galactic bars

Sánchez-Menguiano, L.; Pérez, I.; Zurita, A.; Martínez-Valpuesta, I.; Aguerri, J. A. L.; Sanchez, Sebastian Francisco Sanchez; Comerón, Sébastien; Díaz-García, Simón

doi:10.1093/mnras/stv782

Cited by 14 publications

(17 citation statements)

References 64 publications

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“…By increasing the Lagrangian radius, i.e. reducing the pattern speed of the bar, the distance of the shocks from the centre of the bar increases -in accordance with previous results in the literature (Athanassoula 1992b;Sánchez-Menguiano et al 2015) -while the shocks formed at the leading edge of the bar are also stronger. For very high pattern speeds the shocks move towards the inside of where the dust lanes occur (see model 007 in Figure 6).…”

Section: Effect Of Lagrangian Radiussupporting

confidence: 90%

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Fragkoudi

Athanassoula

Bosma

2016

Mon. Not. R. Astron. Soc.

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We present a pilot study on the nearby massive barred galaxy NGC 1291, in which we use dynamical modelling to constrain the disc mass-to-light ratio (M/L), thus breaking the degeneracy between the baryonic and dark matter in its central regions. We use the gas, specifically the morphology of the dust lanes on the leading side of the bar, as a tracer of the underlying gravitational potential. We run a large number of hydrodynamic gas response simulations, in potentials obtained directly from near-infrared images of the galaxy, which have three free parameters: the M/L, the bar pattern speed and the height function. We explore the three-dimensional parameter space, by comparing the morphology of the shocks created in the gas response simulations with those of the observed dust lanes, and find the best-fitting models; these suggest that the M/L of NGC 1291 agrees with that predicted by stellar population synthesis models in the near-infrared (≈0.6 M /L ), which leads to a borderline maximum disc for this galaxy. Furthermore, we find that the bar rotates fast, with a corotation radius which is 1.4 times the bar length.

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Section: Effect Of Lagrangian Radiussupporting

confidence: 90%

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Fragkoudi

Athanassoula

Bosma

2016

Mon. Not. R. Astron. Soc.

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“…The procedure followed here to separate the arm and interarm regions was used in Sánchez-Menguiano et al (2017) for CALIFA data. The outline of the spiral arms was based on previous and successful tracing of other morphological features such as dust lanes in galactic bars (see Sánchez-Menguiano et al 2015).…”

Section: Separation Of Arm and Interarm Regionsmentioning

confidence: 99%

“…In this regard, the advent of Integral Field Spectroscopy (IFS) instruments combining large field-of-views (FoV) and high spatial resolution has meant a revolution in the progress of 2D abundance distribution studies. Since then, a growing number of works have been able to detect such elusive variations in individual galaxies: NGC 6754 (Sánchez-Menguiano et al 2016b, see also Sánchez et al 2015), NGC 1365 (Ho et al 2017), HCG 91c (Vogt et al 2017), and NGC 2997 (Ho et al 2018). The magnitude of the reported variations differ from study to study (from 0.06 in NGC 2997 to 0.4 dex in NGC 1365), but in all cases more metal-rich gas has been observed associated with the spiral structure.…”

Section: Introductionmentioning

confidence: 99%

Arm–interarm gas abundance variations explored with MUSE: the role of spiral structure in the chemical enrichment of galaxies

Sánchez-Menguiano

Sánchez

Pérez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Spiral arms are the most characteristic features of disc galaxies, easily distinguishable due to their association with ongoing star formation. However, the role of spiral structure in the chemical evolution of galaxies is unclear. Here we explore gas-phase abundance variations between arm and interarm regions for a sample of 45 spiral galaxies using high spatial resolution VLT/MUSE Integral Field Spectroscopy data. We report the presence of more metal-rich H ii regions in the spiral arms with respect to the corresponding interarm regions for a large subsample of galaxies (45 − 65% depending on the adopted calibrator for the abundance derivation). A small percentage of the sample is observed to display the opposite trend, that is, more metal-poor H ii regions in the spiral arms compared to that of the interarms (5−20% depending on the calibrator). We investigate the dependence of the variations with three galaxy properties: the stellar mass, the presence of bars, and the flocculent/grand design appearance of spiral arms. In all cases, we observe that the arm-interarm abundance differences are larger (positive) in more massive and grand-design galaxies. This is confirmed by an analogous spaxel-wise analysis, which also shows a noticeable effect of the presence of galactic bars, with barred systems presenting larger (positive) arm-interarm abundance variations than unbarred systems. The comparison of our results with new predictions from theoretical models exploring the nature of the spirals would highly impact on our knowledge on how these structures form and affect their host galaxies.

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“…There are alternative ways of estimating the strength of the bars photometrically, namely by calculating their intrinsic ellipticity (Martin 1995; and from the normalized Fourier intensity amplitude (Laurikainen et al 2004b. Another indirect method is provided by studying dust lanes, whose curvature is inversely proportional to the bar strength according to the studies of Athanassoula (1992) (probed in Knapen et al 2002;Comerón et al 2009;Sánchez-Menguiano et al 2015), or by 2D decomposition, fitting generalized ellipses to the bar component and using the boxyness as a proxy of the bar strength (Gadotti 2011). Bar lengths have also been measured by different methods in the literature (for a detailed review see Erwin 2005, hereafter E2005) such as ellipse fitting to bar isophotes (e.g.…”

Section: Introductionmentioning

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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On the morphology of dust lanes in galactic bars

Cited by 14 publications

References 64 publications

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Arm–interarm gas abundance variations explored with MUSE: the role of spiral structure in the chemical enrichment of galaxies

Characterization of galactic bars from 3.6μm S⁴G imaging

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On the morphology of dust lanes in galactic bars

Cited by 14 publications

References 64 publications

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Constraining the dark matter content of NGC 1291 using hydrodynamic gas response simulations

Arm–interarm gas abundance variations explored with MUSE: the role of spiral structure in the chemical enrichment of galaxies

Characterization of galactic bars from 3.6μm S4G imaging

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Characterization of galactic bars from 3.6μm S⁴G imaging