Bar-induced evolution of dark matter cusps

Holley‐Bockelmann, Kelly; Weinberg, Martin D.; Katz, Neal

doi:10.1111/j.1365-2966.2005.09501.x

Cited by 115 publications

(155 citation statements)

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“…The slow growth of a bar occurs through non-linear processes; in particular, the resonant gravitational interaction with the surrounding dark matter halo is known to play a major role. This has been investigated by several authors in the past (Debattista & Sellwood 1998;Athanassoula 2002;Holley-Bockelmann et al 2005;Weinberg & Katz 2007;Ceverino & Klypin 2007;Saha & Naab 2013).…”

Section: Growth Of a Bar And Its Size Evolutionmentioning

confidence: 99%

Spin-up of massive classical bulges during secular evolution

Saha

Gerhard

Martínez-Valpuesta

2016

A&A

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Context. Classical bulges in spiral galaxies are known to rotate, but the origin of this observed rotational motion is not well understood. It has been shown recently that a low-mass classical bulge (ClB) in a barred galaxy can acquire rotation by absorbing a significant fraction of the angular momentum emitted by the bar. Aims. Our aim here is to investigate whether bars can also spin up more massive ClBs during the secular evolution of the bar, and to study the kinematics and dynamics of these ClBs. Methods. We use a set of self-consistent N-body simulations to study the interaction of ClBs with a bar that forms self-consistently in the disk. We use orbital spectral analysis to investigate the angular momentum gain by the classical bulge stars. Results. We show that the ClBs gain on average 2−6% of the disk's initial angular momentum within the bar region. Most of this angular momentum gain occurs via low-order resonances, particularly 5:2 resonant orbits. A density wake forms in the ClB which corotates and aligns with the bar at the end of the evolution. The spin-up process creates a characteristic linear rotation profile and mild tangential anisotropy in the ClB. The induced rotation is small in the centre, but is significant beyond ∼2 bulge half mass radii, where it leads to mass-weighted V/σ ∼ 0.2, and reaches a local V max /σ in ∼ 0.5 at around the scale of the bar. The resulting V/σ is tightly correlated with the ratio of the bulge size to the bar size. In all models, a box/peanut bulge forms suggesting that composite bulges may be common. Conclusions. Bar-bulge resonant interaction in barred galaxies can provide some spin-up of massive ClBs, but the process appears to be less efficient than for low-mass ClBs. Further angular momentum transfer due to nuclear bars or gas inflow would be required to explain the observed rotation if it is not primordial.

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Section: Growth Of a Bar And Its Size Evolutionmentioning

confidence: 99%

Spin-up of massive classical bulges during secular evolution

Saha

Gerhard

Martínez-Valpuesta

2016

A&A

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“…This would flatten the inner density profile of the dark matter halo (Navarro et al 1996b;Gnedin & Zhao 2002;Read & Gilmore 2005;Mashchenko et al 2006Mashchenko et al , 2008Ogiya & Mori 2011, 2014Governato et al 2012;Macciò et al 2012;Teyssier et al 2013;Oñorbe et al 2015;Chan et al 2015;El-Zant et al 2016;Del Popolo & Pace 2016). On the other hand, dark matter can also be gravitationally "heated" by baryons through dynamical friction caused either by selfgravitating gas clouds orbiting near the center of the galaxy (El-Zant et al 2001, El-Zant et al 2004Jardel & Sellwood 2009;Lackner & Ostriker 2010;Cole et al 2011, Del Popolo & Pace 2016 by the presence of a stellar bar (Weinberg & Katz 2002;Holley-Bockelmann et al 2005;Sellwood 2008), by the radiation recoil from coalescing black holes (Merritt et al 2004), or by processes which transfer of angular momentum from baryonic to dark matter (Tonini et al 2006, Del Popolo 2009, 2012, 2014.…”

Section: Introductionmentioning

confidence: 99%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

143

140

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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“…Other solutions to the cusp-core problem, including the analytical NTIS model (Shapiro et al, 1999;Iliev & Shapiro, 2001;Chen, 2005), dynamical friction of substructures (El-Zant et al, 2001;Tonini et al, 2006;Romano-Diaz et al , 2008) and stellar bar-CDM interaction (Weinberg & Katz , 2002;Holley-Bockelmann et al , 2005), face exactly the same embarrassment. Clearly, the solutions proposed so far can produce a large core for each dwarf and LSB galaxy, and thus can successfully explain the observations of rotation curves, but they cannot explain the steep and cuspy centers of massive galaxies, which is favored by stong lensing and x-ray observations.…”

Section: Discussionmentioning

confidence: 99%

“…The less traditional models include warm dark matter and self-interacting dark matter. In LCDM model, some researchers simply deny the validity of the observations, others introduce the baryon-cold dark matter interactions (BCDMIs) such as dynamical friction of substructures (El-Zant et al, 2001;Tonini et al, 2006;Romano-Diaz et al , 2008), stellar bar-CDM interaction (Weinberg & Katz , 2002;Holley-Bockelmann et al , 2005), and baryon energy feedback (Mashchenko et al , 2006;Peirani et al , 2008). In this paper, we focus on the validity of BCDMIs solutions to the cusp-core problem.…”

Section: Introductionmentioning

confidence: 99%

Cusp-core problem and strong gravitational lensing

Chen

2009

Res. Astron. Astrophys.

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Cosmological numerical simulations of galaxy formation have led to the cuspy density profile of pure cold dark matter halo toward the center, which is in sharp contradiction with the observations of the rotation curves of cold dark matter-dominated dwarf and low surface brightness disk galaxies, the latter tends to favor mass profiles with a flat central core. Many efforts have been devoted to resolve this cusp-core problem in recent years, among them, baryon-cold dark matter interactions are considered to be the main physical mechanisms erasing the cold dark matter (CDM) cusp into a flat core in the centers of all CDM halos. Clearly, baryon-cold dark matter interactions are not customized only for CDM-dominated disk galaxies, but for all types, including giant ellipticals. In this paper, we first fit the most recent high resolution observations of rotation curves with the Burkert profile, then use the constrained core size-halo mass relation to calculate the lensing frequency, and compare the predicted results with strong lensing observations. Unfortunately, it turns out that the core size constrained from rotation curves of disk galaxies cannot be extrapolated to giant ellipticals. We conclude that, in standard cosmological paradigm, baryon-cold dark matter interactions are not universal mechanisms for galaxy formation, and therefore, they cannot be true solutions to the cusp-core problem.

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Bar-induced evolution of dark matter cusps

Cited by 115 publications

References 100 publications

Spin-up of massive classical bulges during secular evolution

Spin-up of massive classical bulges during secular evolution

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Cusp-core problem and strong gravitational lensing

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