The Degeneracy of M33 Mass Modeling and Its Physical Implications

Hague, P.; Wilkinson, M. I.

doi:10.1088/0004-637x/800/1/15

Cited by 8 publications

(6 citation statements)

References 38 publications

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“…The finding of a dependency of the inner shape of the DM halo on the mass-to-light ratio is in agreement with the analysis of Hague & Wilkinson (2015). These authors used a Bayesian approach to constrain the mass distribution of M33 from the kinematics of Corbelli & Salucci (2000).…”

Section: Comparison With Previous Worksupporting

confidence: 80%

“…They have also shown that the distribution of dark matter is consistent with a model for which the mass density steeply decreases in the centre of the halo (the cosmological cusp à la Navarro-Frenk-White, see Navarro et al 1997), and whose concentration agrees well with the halo mass-concentration relation from Λ Cold Dark Matter simulations (Ludlow et al 2014). Comparable results have been obtained by Hague & Wilkinson (2015), but from a lower resolution Hi curve derived earlier by Corbelli & Salucci (2000). They concluded that models with density profiles with an inner slope shallower than 0.9 (as measured at R ∼ 0.5 kpc, the first velocity point of their rotation curve) are only compatible with 3.6-µm mass-to-light ratios Υ > 2, while cuspier densities can coexist with Υ < 2.…”

Section: Introductionsupporting

confidence: 68%

“…It is another way to illustrate the halo concentrationstellar mass degeneracy shown in Sect. 5.5.1 and in Hague & Wilkinson (2015).…”

Section: Comparison With Previous Workmentioning

confidence: 91%

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H i Kinematics and Mass Distribution of Messier 33

Kam

Carignan

Chemin

et al. 2017

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A new deep Hi survey of the galaxy Messier 33 is presented, based on observations obtained at the Dominion Radio Astrophysical Observatory. We observe a perturbed outer gas distribution and kinematics in M33, and confirm the disk warping as a significant kinematical twist of the major axis of the velocity field, though no strong tilt is measured, in agreement with previous work. Evidence for a new low brightness Hi component with anomalous velocity is reported. It harbours a large velocity scatter, as its kinematics both exceeds and lags the rotation of the disk, and leaks in the forbidden velocity zone of apparent counter-rotation. The observations also reveal wide and multiple peak Hi profiles which can be partly explained by crowded orbits in the framework of the warp model. Asymmetric motions are identified in the velocity field, as possible signatures of a lopsided potential and the warp. The mass distribution modeling of the hybrid Hα-Hi rotation curve favours a cuspy dark matter halo with a concentration in disagreement with the ΛCDM dark halo mass-concentration relationship. The total mass enclosed in 23 kpc is 8 10 10 M , of which 11% are stars and gas. At the virial radius of the cuspy halo, the resulting total mass is 5 10 11 M , but with a baryonic mass fraction of 2% only. This strongly suggests a more realistic radius encompassing the total mass of M33 well smaller than the virial radius of the halo, maybe comparable to the size of the Hi disk.

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Section: Comparison With Previous Worksupporting

confidence: 80%

Section: Introductionsupporting

confidence: 68%

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H i Kinematics and Mass Distribution of Messier 33

Kam

Carignan

Chemin

et al. 2017

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“…These criteria lead to an additional 5 galaxies. Finally we also included the rotation curve of M33 (taken from Corbelli et al 2014), which is a galaxy previously claimed to have a strongly cusped dark matter halo (Corbelli et al 2014;Hague & Wilkinson 2015). For this galaxy Corbelli et al (2014) have not reported the stellar surface brightness profile, but have immediately derived the surface density profile of the stars from a pixel by pixel population synthesis analysis.…”

Section: Sample Selectionmentioning

confidence: 99%

Testing baryon-induced core formation in ΛCDM: A comparison of the DC14 and coreNFW dark matter halo models on galaxy rotation curves

Allaert

Gentile

Baes

2017

A&A

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Recent cosmological hydrodynamical simulations suggest that baryonic processes, and in particular supernova feedback following bursts of star formation, can alter the structure of dark matter haloes and transform primordial cusps into shallower cores. To assess whether this mechanism offers a solution to the long-standing cusp-core controversy, simulated haloes must be compared to real dark matter haloes inferred from galaxy rotation curves. For this purpose, two new dark matter density profiles were recently derived from simulations of galaxies in complementary mass ranges: the DC14 halo (10 10 < M halo /M < 8 × 10 11 ) and the coreNFW halo (10 7 < M halo /M < 10 9 ). Both models have individually been found to give good fits to observed rotation curves. For the DC14 model, however, the agreement of the predicted halo properties with cosmological scaling relations was confirmed by one study, but strongly refuted by another. A next important question is whether, despite their different approaches, the two models converge to the same solution in the mass range where both should be appropriate. To investigate this, we tested the DC14 and coreNFW halo models on the rotation curves of a selection of galaxies with halo masses in the range 4 × 10 9 M -7 × 10 10 M and compared their predictions. We further applied the DC14 model to a set of rotation curves at higher halo masses, up to 9 × 10 11 M , to verify the agreement with the cosmological scaling relations. Both models are generally able to reproduce the observed rotation curves, in line with earlier results, and the predicted dark matter haloes are consistent with the cosmological c − M halo and M * − M halo relations. We find that the DC14 and coreNFW models are also in fairly good agreement with each other, even though DC14 tends to predict slightly less extended cores and somewhat more concentrated haloes than coreNFW. While the quality of the fits is generally similar for both halo models, DC14 does perform significantly better than coreNFW for three galaxies. In each of these cases, the problem for coreNFW is related to connection of the core size to the stellar half-mass radius, although we argue that it is justifiable to relax this connection for NGC 3741. A larger core radius brings the coreNFW model for this galaxy in good agreement with the data and the DC14 model.

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“…The parameters are motivated by previous observations and models of M33's rotation curve (e.g. Regan & Vogel 1994;Corbelli & Salucci 2000;Seigar 2011;Hague & Wilkinson 2015;Kam et al 2015). M33 is a fairly low-mass spiral galaxy close to the Milky Way.…”

Section: Galaxy Components and Density Profilesmentioning

confidence: 99%

Large-scale gas flows and streaming motions in simulated spiral galaxies

Ramón-Fox

Bonnell

2022

Monthly Notices of the Royal Astronomical Society

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From a galactic perspective, star formation occurs on the smallest scales within molecular clouds, but it is likely initiated from the large scale flows driven by galactic dynamics. To understand the conditions for star formation, it is important to first discern the mechanisms that drive gas from large-scales into dense structures on the smallest scales of a galaxy. We present high-resolution smoothed particle hydrodynamics simulations of two model spiral galaxies: one with a live stellar disc (N-body) and one with a spiral potential. We investigate the large-scale flows and streaming motions driven by the simulated spiral structure. We find that the strength of the motions in the radial direction tends to be higher than in the azimuthal component. In the N-body model, the amplitude of these motions decreases with galactocentric radius whereas for the spiral potential, it decreases to a minimum at the corotation radius, and increases again after this point. The results show that in both simulations, the arms induce local shocks, an increase in kinetic energy that can drive turbulence and a means of compressing and expanding the gas. These are all crucial elements in forming molecular clouds and driving the necessary conditions for star formation.

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The Degeneracy of M33 Mass Modeling and Its Physical Implications

Cited by 8 publications

References 38 publications

H i Kinematics and Mass Distribution of Messier 33

H i Kinematics and Mass Distribution of Messier 33

Testing baryon-induced core formation in ΛCDM: A comparison of the DC14 and coreNFW dark matter halo models on galaxy rotation curves

Large-scale gas flows and streaming motions in simulated spiral galaxies

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