Gravitational stability and mass estimation of stellar disks

Saburova, Anna S.; Засов, А. В.

doi:10.1002/asna.201311922

Cited by 14 publications

(15 citation statements)

References 19 publications

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“…The approach to the disk and halo mass decomposition with account for the stellar velocity dispersion applied to several galaxy samples [55,[94][95][96], confirmed that the stellar disk gravitational stability condition for Sab-Sd-galaxies assumes the presence of a more massive dark halo than follows from the maximum disk model.…”

Section: The Disk Gravitational Stability Conditionmentioning

confidence: 68%

Dark matter in galaxies

Засов¹,

Saburova²,

Хоперсков³

et al. 2017

Phys.-Usp.

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Dark matter in galaxies, its abundance, and its distribution remain a subject of long-standing discussion, especially in view of the fact that neither dark matter particles nor dark matter bodies have yet been found. Experts' opinions range from a very large number of completely dark galaxies exist to nonbaryonic dark matter does not exist at all in any significant amounts. We discuss astronomical evidence for the existence of dark matter and its connection with visible matter and examine attempts to estimate its mass and distribution in galaxies from photometry, dynamics, gravitational lensing, and other observations (the cosmological aspects of the existence of dark matter are not considered in this review). In our view, the presence of dark matter in and around galaxies is a well-established fact. We conclude with an overview of mechanisms by which a dark halo can influence intragalactic processes.Comment: 82 pages, 35 figure

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Section: The Disk Gravitational Stability Conditionmentioning

confidence: 68%

Dark matter in galaxies

Засов¹,

Saburova²,

Хоперсков³

et al. 2017

Phys.-Usp.

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“…Consequently, the disk of LSB galaxies is over-stabilized [554] and its mass should be smaller than the limit required to generate spiral modes, unlike what happens in HSB disks [555]; nevertheless, spiral arms and bars are observed in LSB disk galaxies [556][557][558][559]. As a consequence, explaining the amplitude of the rotation curves and the presence of spiral arms and bars in the standard model requires mass-to-light ratios that are inconsistently larger than the expectations from stellar-population-synthesis models [560][561][562]. This tension does not appear in MOND, where there is no dark matter and the spiral modes are naturally generated as in the HSB disk galaxies [548,563,564].…”

Section: Disk Galaxiesmentioning

confidence: 97%

Dark Matters on the Scale of Galaxies

et al. 2020

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The cold dark-matter model successfully explains both the emergence and evolution of cosmic structures on large scales and, when we include a cosmological constant, the properties of the homogeneous and isotropic Universe. However, the cold dark-matter model faces persistent challenges on the scales of galaxies. Indeed, N-body simulations predict some galaxy properties that are at odds with the observations. These discrepancies are primarily related to the dark-matter distribution in the innermost regions of the halos of galaxies and to the dynamical properties of dwarf galaxies. They may have three different origins: (1) the baryonic physics affecting galaxy formation is still poorly understood and it is thus not properly included in the model; (2) the actual properties of dark matter differs from those of the conventional cold dark matter; (3) the theory of gravity departs from General Relativity. Solving these discrepancies is a rapidly evolving research field. We illustrate some of the solutions proposed within the cold dark-matter model, and solutions when including warm dark matter, self-interacting dark matter, axion-like particles, or fuzzy dark matter. We also illustrate some modifications of the theory of gravity: Modified Newtonian Dynamics (MOND), MOdified Gravity (MOG), and f(R) gravity.

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“…The discs of bright spirals are maximal (Sellwood 1999;Freeman 2010), unless they are not (Courteau & Rix 1999;Bershady et al 2011). The discs of low surface brightness galaxies are submaximal (de Blok & McGaugh 1997), unless they are maximal (Fuchs 2002;Saburova & Zasov 2013).…”

Section: Introductionmentioning

confidence: 99%

A new algorithm to quantify maximum discs in galaxies

Starkman

Lelli

McGaugh

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Maximum disc decompositions of rotation curves place a dynamical upper limit to the mass attributable to stars in galaxies. The precise definition of this term, however, can be vague and varies in usage. We develop an algorithm to robustly quantify maximum-disc mass models and apply it to 153 galaxies from the SPARC database. Our automatic procedure recovers classic results from manual decompositions. Highmass, high-surface-brightness galaxies have mean maximum-disc mass-to-light ratios of ∼ 0.7 M /L in the Spitzer 3.6 µm band, which are close to the expectations from stellar population models, suggesting that these galaxies are nearly maximal. Low-mass, low-surface-brightness galaxies have very high maximum-disc mass-to-light ratios (up to 10 M /L ), which are unphysical for standard stellar population models, confirming they are sub-maximal. The maximum-disc mass-to-light ratios are more closely correlated with surface brightness than luminosity. The mean ratio between baryonic and observed velocity at the peak of the baryonic contribution is V bar /V p ≈ 0.88, but correlates with surface brightness, so it is unwise to use this mean value to define the maximum disc concept. Our algorithm requires no manual intervention and could be applied to large galaxy samples from future HI surveys with Apertif, Askap, and SKA.

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Gravitational stability and mass estimation of stellar disks

Cited by 14 publications

References 19 publications

Dark matter in galaxies

Dark matter in galaxies

Dark Matters on the Scale of Galaxies

A new algorithm to quantify maximum discs in galaxies

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