Properties of dark matter haloes

Combes, F.

doi:10.1016/s1387-6473(02)00244-0

Cited by 41 publications

(30 citation statements)

References 69 publications

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“…The H i disks in galaxies are typically three times more extended than their stellar counterparts. This property, as well as the fact that the outer parts of galaxies are dominated by dark matter, highlights the importance of the gaseous disk as a tracer of the mass distribution (Sofue & Rubin 2001;Combes 2002). The Galactic outskirts are very interesting in this respect.…”

Section: Introductionmentioning

confidence: 92%

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Dark matter in the Milky Way

Kalberla

Dedes

Kerp

et al. 2007

A&A

179

239

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Context. Gas within a galaxy is forced to establish pressure balance against gravitational forces. The shape of an unperturbed gaseous disk can be used to constrain dark matter models.Aims. We derive the 3D H i volume density distribution for the Milky Way out to a galactocentric radius of 40 kpc and a height of 20 kpc to constrain the Galactic mass distribution. Methods. We used the Leiden/Argentine/Bonn all sky 21-cm line survey. The transformation from brightness temperatures to densities depends on the rotation curve. We explored several models, reflecting different dark matter distributions. Each of these models was set up to solve the combined Poisson-Boltzmann equation in a self-consistent way and optimized to reproduce the observed flaring. Results. Besides a massive extended halo of M ∼ 1.8 × 1012 M , we find a self-gravitating dark matter disk with M = 2 to 3 × 10 11 M , including a dark matter ring at 13 < R < 18.5 kpc with M = 2.2 to 2.8 × 10 10 M . The existence of the ring was previously postulated from EGRET data and coincides with a giant stellar structure that surrounds the Galaxy. The resulting Milky Way rotation curve is flat up to R ∼ 27 kpc and slowly decreases outwards. The H i gas layer is strongly flaring. The HWHM scale height is 60 pc at R = 4 kpc and increases to ∼2700 pc at R = 40 kpc. Spiral arms cause a noticeable imprint on the gravitational field, at least out to R = 30 kpc. Conclusions. Our mass model supports previous proposals that the giant stellar ring structure is due to a merging dwarf galaxy. The fact that the majority of the dark matter in the Milky Way for R < ∼ 40 kpc can be successfully modeled by a self-gravitating isothermal disk raises the question of whether this massive disk may have been caused by similar merger events in the past. The substructure in the Galactic dark matter disk suggests a dissipative nature for the dark matter disk.

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Section: Introductionmentioning

confidence: 92%

“…Despite density enhancements at the center (cusps), no substructures on kpc scale are expected. Clumpyness appears instead to be associated with dissipative matter (Combes 2002).…”

Section: Origin Of the Dark Matter Ring And Diskmentioning

confidence: 99%

Dark matter in the Milky Way

Kalberla

Dedes

Kerp

et al. 2007

A&A

179

239

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“…The H i integrated line profile data were obtained from several published hydrogen observations of PRGs, carried out by, e.g., Richter, Sackett, & Sparke (1994), van Gorkom et al (1987), and van Driel et al (2000, 2002, 2003, with several radio telescopes.…”

Section: Introductionmentioning

confidence: 99%

Polar Ring Galaxies and the Tully‐Fisher Relation: Implications for the Dark Halo Shape

Iodice¹,

Arnaboldi²,

Bournaud³

et al. 2003

ApJ

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We have investigated the Tully-Fisher relation for polar ring galaxies (PRGs), based on near-infrared, optical, and H i data available for a sample of these peculiar objects. The total K-band luminosity, which mainly comes from the central host galaxy, and the measured H i line width at 20% of the peak line flux density, which traces the potential in the polar plane, place most polar rings in the sample far from the TullyFisher relation defined for spiral galaxies, with many PRGs showing larger H i line widths than expected for the observed K-band luminosity. This result is confirmed by a larger sample of objects, based on B-band data. This observational evidence may be related to the dark halo shape and orientation in these systems, which we study by numerical modeling of PRG formation and dynamics: the larger rotation velocities observed in PRGs can be explained by a flattened polar halo, aligned with the polar ring.

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“…All rotation curves can be explained, when the observed surface density of gas is multiplied by a constant factor, around 7-10. This aDM/aHI ratio is almost constant from galaxy to galaxy, being slightly larger for early-types (Combes 2002). A solution to the problem of non-observed CDM cusps is that CDM would not be dominating in LSB galaxy centers, as is already the case in more evolved early-type galaxies, dominated by the stars.…”

Section: Cusps In Galaxy Centersmentioning

confidence: 96%

Galaxy Formation and Baryonic Dark Matter

Combes

2004

Symp. - Int. Astron. Union

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Abstract. The ACDM scenario to form galaxies encounters many problems when confronted with observations, namely the prediction of dark matter cusps in all galaxies, and in particular in dwarf irregulars, dominated by dark matter, or the low angular momentum and consequent small size of galaxy disks, or the high predicted number of small systems. We will consider the hypothesis that the baryonic dark matter could be in the form of gas and could be continuously involved in the galaxy formation scenario. By accreting cold gas throughout a galaxy's life, angular momentum could be increased, galaxy disks could be more dominated by baryons than previously thought, and small systems could merge more frequently.

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Properties of dark matter haloes

Cited by 41 publications

References 69 publications

Dark matter in the Milky Way

Dark matter in the Milky Way

Polar Ring Galaxies and the Tully‐Fisher Relation: Implications for the Dark Halo Shape

Galaxy Formation and Baryonic Dark Matter

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