The extended rotation curve and the dark matter halo of M33

Corbelli, E.; Salucci, Paolo

doi:10.1046/j.1365-8711.2000.03075.x

Cited by 372 publications

(404 citation statements)

References 31 publications

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“…This is also clear from the values of reduced-χ 2 . We therefore, conclude that the NFW model best represents these data, and this is consistent with the results of Corbelli and Salucci [16]. This is somewhat surprising for a late type, bulgeless galaxy like M33, since these late-type galaxies are often shown to have constant density cores (e.g., [10,11]).…”

Section: The Dark Halo Contributionsupporting

confidence: 89%

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The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

Seigar

2011

ISRN Astronomy and Astrophysics

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We investigate the dark matter halo density profile of M33. We find that the HÁ rotation curve of M33 is best described by an NFW dark matter halo density profile model, with a halo concentration of c vir = 4.0±1.0 and a virial mass of M vir = (2.2±0.1)×10 11 M . We go on to use the NFW concentration (c vir ) of M33, along with the values derived for other galaxies (as found in the literature), to show that c vir correlates with both spiral arm pitch angle and supermassive black hole mass.

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Section: The Dark Halo Contributionsupporting

confidence: 89%

“…In this paper, we have chosen to model the HÁ rotation curve of M33 from Crobelli and Salucci [16]. Due to its proximity, M33 can be studied in exquisite detail, and it, therefore, provides a crucial testing ground of our ideas of galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

Seigar

2011

ISRN Astronomy and Astrophysics

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“…Because of its proximity, the rotation curve can be traced with unprecedented spatial resolution. M 33 is in fact one of the very few objects for which it has been possible to combine a high quality and high resolution extended rotation curve (Corbelli & Salucci 2000) with a well determined distance (assumed in this paper to be D = 840 kpc, Freedman et al 1991;Gieren et al 2013), and with an overwhelming quantity of data across the electromagnetic spectrum. Previous analyses have shown that the HI and CO velocity fields are very regular and cannot be explained by Newtonian dynamic without including a massive dark matter halo (Corbelli 2003).…”

Section: Introductionmentioning

confidence: 99%

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Corbelli

Thilker

Zibetti

et al. 2014

A&A

153

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Aims. We determine the mass distribution of stars, gas, and dark matter in M 33 to test cosmological models of galaxy formation and evolution. Methods. We map the neutral atomic gas content of M 33 using high resolution Very Large Array and Green Bank Telescope observations of the 21 cm HI line emission. A tilted ring model is fitted to the HI datacube to determine the varying spatial orientation of the extended gaseous disk and the rotation curve. We derive the stellar mass surface density map of M 33's optical disk via pixel-SED fitting methods based on population synthesis models that allow for positional changes in star formation history. Stellar and gas maps are used in the dynamical analysis of the rotation curve to constrain the dark halo properties. Results. The disk of M 33 warps from 8 kpc outward without substantial change of its inclination with respect to the line of sight; the line of nodes rotates clockwise toward the direction of M 31. Rotational velocities rise steeply with radius in the inner disk, reaching 100 km s −1 in 4 kpc, then the rotation curve becomes more perturbed and flatter with velocities as high as 120-130 km s −1 out to 2.7 R 25 . The stellar surface density map highlights a star-forming disk with a varying mass-to-light ratio. At larger radii, a dynamically relevant fraction of the baryons are in gaseous form. A dark matter halo with a Navarro-Frenk-White density profile, as predicted by hierarchical clustering and structure formation in a ΛCDM cosmology, provides the best fits to the rotation curve. Dark matter is relevant at all radii in shaping the rotation curve and the most likely dark halo has a concentration C 9.5 and a total mass of 4.3(±1.0) × 10 11 M . This imples a baryonic fraction of order 0.02 and the evolutionary history of this galaxy should therefore account for loss of a large fraction of its original baryonic content.

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“…Then, for (6) and (7), M vir = η M 0 , with η ≃ 12 for (Ω 0 , Ω b ,z) = (0.3, 0.03, 3), and the limiting halo mass implies a lack of objects with ρ 0 > 4 × 10 −25 g/cm 3 and r 0 > 30 kpc, as is evident in Fig. 3.…”

Section: Halo Density Profilesmentioning

confidence: 71%

“…Then, although dark halo might extend down to the galaxy centers, it is only for r > r IBD that they give a non-negligible contribution to the circular velocity. b) DM is distributed in a different way with respect to any of the various baryonic components [16,6], and c) HI contribution to the circular velocity at r < r opt , is negligible [e.g. 17].…”

Section: Dark Matter Properties From the Universal Rotation Curvementioning

confidence: 99%

The Intriguing Distribution of Dark Matter in Galaxies

Salucci

Borriello

2003

Particle Physics in the New Millennium

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Abstract. We review the most recent evidence for the amazing properties of the density distribution of the dark matter around spiral galaxies. Their rotation curves, coadded according to the galaxy luminosity, conform to an Universal profile which can be represented as the sum of an exponential thin disk term plus a spherical halo term with a flat density core. From dwarfs to giants, these halos feature a constant density region of size r0 and core density ρ0 related by ρ0 = 4.5 × 10 −2 (r0/kpc) −2/3 M⊙pc −3 . At the highest masses ρ0 decreases exponentially with r0, revealing a lack of objects with disk masses > 10 11 M⊙ and central densities > 1.5 × 10 −2 (r0/kpc) −3 M⊙pc −3 implying a maximum mass of ≈ 2 × 10 12 M⊙ for a dark halo hosting a stellar disk. The fine structure of dark matter halos is obtained from the kinematics of a number of suitable low-luminosity disk galaxies. The halo circular velocity increases linearly with radius out to the edge of the stellar disk, implying a constant dark halo density over the entire disk region. The properties of halos around normal spirals provide substantial evidence of a discrepancy between the mass distributions predicted in the Cold Dark Matter scenario and those actually detected around galaxies.

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The extended rotation curve and the dark matter halo of M33

Cited by 372 publications

References 31 publications

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

The Dark Matter Halo Density Profile, Spiral Arm Morphology, and Supermassive Black Hole Mass of M33

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

The Intriguing Distribution of Dark Matter in Galaxies

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