Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies

By V. Debattista, J. Sellwood. 2000

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We show that bars in galaxy models having halos of moderate density and a variety of velocity distributions all experience a strong drag from dynamical friction unless the halo has large angular momentum in the same sense as the disk. The frictional drag decreases the bar pattern speed, driving the corotation point out to distances well in excess of those estimated in barred galaxies. The halo angular momentum required to avoid strong braking is unrealistically large, even when rotation is confined to the inner halo only. We conclude, therefore, that bars are able to maintain their observed high pattern speeds only if the halo has a central density low enough for the disk to provide most of the central attraction in the inner galaxy. We present evidence that this conclusion holds for all bright galaxies.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ca920d4a217c6fa2675e105af5ec59c682080aa7

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Citations in the corpus

BULGE n AND B/T IN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS (2008, background): “Bars provide the most important internal mechanism for redistributing angular momentum in baryonic and dark matter components (e.g. Weinberg 1985; Debattista & Sellwood 1998, 2000; Athanassoula 2002; Berentzen, Shlosman, & Jogee 2006).”
How Large Are the Bars in Barred Galaxies (2005, methodology): “There is similar variation in how bars are measured even when the galaxy is readily accessible; i.e., in n-body simulations – compare, for example, Debattista & Sellwood (2000), Athanassoula & Misiriotis (2002), and Valenzuela & Klypin (2003).”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, background): “…and concentrations of LSB galaxies are significantly lower than the standard CDM paradigm predicts (e.g., van den Bosch et al. 2000, 2003a; Debattista & Sellwood 2000; Keeton 2001; van den Bosch & Swaters 2001; Alam et al. 2002; Zentner & Bullock 2002, 2003; McGaugh et al. 2003; Kuhlen et…”
Morphology, photometry and kinematics of N‐body bars – I. Three models with different halo central concentrations (2001, background): “In fact rings have not been witnessed before this in purely stellar N-body simulations, with the notable exception of the fiducial simulation of Debattista & Sellwood (2000).”
Secular bar formation in galaxies with a significant amount of dark matter (2002, methodology): “We have also tried other prescriptions, which are to some degree reminiscent of what was used by Debattista & Sellwood (2000).”
Made-to-measure models of the Galactic box/peanut bulge: stellar and total mass in the bulge region (2015, background): “Bars with R > 1.4 are called slow rotators, while those with R 6 1.4 are fast rotators (Debattista & Sellwood 2000).”
Galaxy Masses: A Review (2013, background): “Roughly speaking, systems with smaller values of V 2disk/V 2 tot will be more stable against bar formation, though this ratio alone is an inadequate predictor of whether a bar will form (see, e.g. Debattista & Sellwood (2000) and WPD).”
ΛCDM-based Models for the Milky Way and M31. I. Dynamical Models (2001, methodology): “If the mass of the dark matter surrounding the bar is too large, the dynamical friction could slow down the bar rotation over a short timescale (Weinberg 1985; Debattista & Sellwood 2000), in which case we should not expect to see fast rotating bars.”
What determines the strength and the slowdown rate of bars (2003, background): “This is in agreement with the results of Debattista & Sellwood (1998, 2000), who find a strong temporal decrease of the pattern speed for halo dominated cases and a weak one for disc dominated cases.”
Bar-Halo Interaction and Bar Growth (2002, background): “The pattern speed of MD also decreases with time, but less so (cf. Debattista & Sellwood 1998, 2000).”
Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, background): “…important internal factor that redistributes the angular momentum of the baryonic and dark matter components of disk galaxies (e.g., Weinberg 1985; Debattista & Sellwood 1998, 2000; Athanassoula 2002; Berentzen et al. 2006), thereby driving their dynamical and secular evolution (Kormendy 1993;…”
Dynamical Blueprints for Galaxies (2008, background): “Here vtot is the circular rotation speed at cylindrical radius R and vd is the contribution to vtot from the disk (Debattista & Sellwood 1998, 2000).”
Radial migration in disc galaxies — I. Transient spiral structure and dynamics (2011, methodology): “…most resolutions udies have addressed the resonant couplings between dark matter hlos and bars, but again most often only collisionless simulations were used (e.g. Debattista & Sellwood 2000; Valenzuela & Klypin 2003; Holley-Bockelmann et al. 2005; Weinberg & Katz 2007; Dubinski et al. 2009).”
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, methodology): “Mentally ignoring them, we see that the halo bulk rotation velocity increases considerably with time, contrary to the bar pattern speed, which has been shown to decrease with time (e.g. Debattista & Sellwood 2000; A03; Berentzen et al. 2007).”
The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, background): “Observed pattern speeds imply that barred galaxies host maximal discs (Debattista & Sellwood 1998, 2000), since bars in dense dark matter halos are rapidly decelerated by dynamical friction (Weinberg 1985; Sellwood 2006; Sellwood & Debattista 2006).”
Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution (2016, background): “This places the Milky Way together with the bulk of external barred spiral galaxies, with a bar that can be classified as a fast rotator (R ≤ 1.4, Debattista & Sellwood (2000)).”
Generating Equilibrium Dark Matter Halos: Inadequacies of the Local Maxwellian Approximation (2003, background): “…& Goodman 1986; Velázquez & White 1999; Taylor & Babul 2001; Font et al. 2001), the susceptibility of disks to bar instabilities (Mihos, McGaugh, & de Blok 1997), and the effects of these bars on halo central density cusps (Debattista & Sellwood 2000; Athanassoula 2002; Valenzuela & Klypin 2003).”
Galaxy Zoo:bars in disc galaxies (2010, background): “…galaxies, and are thought to have an important impact on the evolution of galaxies through their ability to transfer angular momentum in both the baryonic and dark matter components of the galaxy (Combes & Sanders 1981; Weinberg 1985; Debattista & Sellwood 2000; Berentzen, Shlosman & Jogee 2006).”