Dynamical Friction and the Distribution of Dark Matter in Barred Galaxies

Debattista, Victor P.; Sellwood, J. A.

doi:10.1086/311118

Cited by 281 publications

(291 citation statements)

References 32 publications

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“…However, this assumption is in contradiction with a substantial body of astrophysical evidences [13], and a core profile is not sensitive to standard DM candidates. On the contrary, cusped profiles are not excluded for the Local Group dwarf spheroidals (dSphs) that constitute interesting targets since they are much more dominated by DM.…”

Section: B Dm Density Directionalitymentioning

confidence: 80%

Photon spectra from WIMP annihilation

et al. 2011

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If the present dark matter in the Universe annihilates into Standard Model particles, it must contribute to the fluxes of cosmic rays that are detected on the Earth, and in particular, to the observed gamma ray fluxes. The magnitude of such contribution depends on the particular dark matter candidate, but certain features of the produced photon spectra may be analyzed in a rather model-independent fashion. In this work we provide the complete photon spectra coming from WIMP annihilation into Standard Model particle-antiparticle pairs obtained by extensive Monte Carlo simulations. We present results for each individual annihilation channel and provide analytical fitting formulae for the different spectra for a wide range of WIMP masses.a

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Section: B Dm Density Directionalitymentioning

confidence: 80%

Photon spectra from WIMP annihilation

et al. 2011

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“…Hydrodynamical simulations of these systems show that the bar component contributes only between 10 and 20% of the disc potential (e.g., Scannapieco et al 2010), and yet it can produce important changes in the gas dynamics. Bars are thought to be very efficient in redistributing angular momentum, energy and mass in both luminous and dark matter components (e.g., Weinberg 1985; Debattista & Sellwood 1998Athanassoula 2003;Martinez-Valpuesta et al 2006;Sellwood 2006;Sellwood & Debattista 2006;Villa-Vargas et al 2009). The effects of this angular momentum redistribution is different in gas and stars due to their different properties (e.g., Thielheim & Wolff 1982).…”

Section: Introductionmentioning

confidence: 99%

Kinematic alignment of non-interacting CALIFA galaxies

Barrera-Ballesteros

Falcón-Barroso

García-Lorenzo

et al. 2014

A&A

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We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterise the kinematic orientation of non-interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast-external processes, such as major mergers, affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both stellar and nebular components and that internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components (∼90% of the sample has differences smaller than 16 degrees). This relation also holds, generally in barred galaxies across the bar and galaxy disc scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disc. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies.

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“…For example, they are able to contribute to the redistribution of matter in the galaxy by exchanging angular momentum with the disc, bulge and halo (e.g. Debattista & Sellwood 1998 Galactic bars are characterised dynamically by three main parameters: length, strength 1 and pattern speed. Several methods have been proposed to measure them.…”

Section: Introductionmentioning

confidence: 99%

On the morphology of dust lanes in galactic bars

Sánchez-Menguiano¹,

Pérez²,

Zurita³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The aim of our study is to use dynamical simulations to explore the influence of two important dynamical bar parameters, bar strength and bar pattern speed, on the shape of the bar dust lanes. To quantify the shape of the dust lanes we have developed a new systematic method to measure the dust lane curvature. Previous numerical simulations have compared the curvature of bar dust lanes with the bar strength, predicting a relation between both parameters which has been supported by observational studies but with a large spread. We take into account the bar pattern speed to explore, simultaneously, the effect of both parameters on the dust lane shape.To that end, we separate our galactic bars in fast bars (1 < R < 1.4) and slow bars (R > 1.4), obtaining, as previous simulations, an inverse relation between the dust lane curvature and the bar strength for fast bars. For the first time, we extend the study to slow bars, finding a constant curvature as a function of the bar strength. As a result, we conclude that weak bars with straight dust lanes are candidates for slow bars. Finally, we have analysed a pilot sample of ten S 4 G galaxies, obtaining dust lane curvatures lying within the range covered by the simulations.

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Dynamical Friction and the Distribution of Dark Matter in Barred Galaxies

Cited by 281 publications

References 32 publications

Photon spectra from WIMP annihilation

Photon spectra from WIMP annihilation

Kinematic alignment of non-interacting CALIFA galaxies

On the morphology of dust lanes in galactic bars

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