Gas dynamics in dwarf galaxies as testbeds for dark matter and galaxy evolution

Lelli, Federico

doi:10.1038/s41550-021-01562-2

Cited by 27 publications

(16 citation statements)

References 180 publications

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“…LS galaxies By comparing the two tables 1 and 2, we notice that the mass M ef f is almost constant and small for the spirals galaxies, while, it is very important for the dwarf spheroidal galaxies (dSphs) [45]. This shows why the rotation curves of the spirals galaxies are almost static.…”

Section: Rotation Curves Of Galaxiesmentioning

confidence: 85%

Interpretation of galaxy rotation curves from primordial black holes in 4D Einstein-Gauss-Bonnet gravity

Bousder¹

2022

Preprint

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We develop a novel approach to the dark matter halos in the context of 4 dimensional Einstein-scalar-Gauss-Bonnet gravity. This approach gives a possible interpretation of the problem of the galaxy rotation curves. Moreover, the Gauss-Bonnet coupling describes the interior structure of the galaxies, while there is a presence of a scalar field φ in the galaxy edges. This can provide an interesting interpretation for the functional coupling f (φ). We discuss how this comparison can naturally drive the observed percentages of matter and dark matter in the Universe. The effective mass range in our model is 10 −2 kg − 10 3 kg, which is in good agreement with the constraints on primordial black holes.

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Section: Rotation Curves Of Galaxiesmentioning

confidence: 85%

Interpretation of galaxy rotation curves from primordial black holes in 4D Einstein-Gauss-Bonnet gravity

Bousder¹

2022

Preprint

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“…Consequently, larger changes in Q * are needed to impact the fit quality. Indeed, the scatter increases dramatically at precisely the scale where gas typically begins to dominate the mass budget (McGaugh 2011;Lelli 2022).…”

Section: Mond Versus Sfdmmentioning

confidence: 99%

Galactic mass-to-light ratios with superfluid dark matter

Mistele

McGaugh

Hossenfelder

2022

A&A

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Context. We make rotation curve fits to test the superfluid dark matter model. Aims. In addition to verifying that the resulting fits match the rotation curve data reasonably well, we aim to evaluate how satisfactory they are with respect to two criteria, namely, how reasonable the resulting stellar mass-to-light ratios are and whether the fits end up in the regime of superfluid dark matter where the model resembles modified Newtonian dynamics (MOND). Methods. We fitted the superfluid dark matter model to the rotation curves of 169 galaxies in the SPARC sample. Results. We found that the mass-to-light ratios obtained with superfluid dark matter are generally acceptable in terms of stellar populations. However, the best-fit mass-to-light ratios have an unnatural dependence on the size of the galaxy in that giant galaxies have systematically lower mass-to-light ratios than dwarf galaxies. A second finding is that the superfluid often fits the rotation curves best in the regime where the superfluid’s force cannot resemble that of MOND without adjusting a boundary condition separately for each galaxy. In that case, we can no longer expect superfluid dark matter to reproduce the phenomenologically observed scaling relations that make MOND appealing. If, on the other hand, we consider only solutions whose force approximates MOND well, then the total mass of the superfluid is in tension with gravitational lensing data. Conclusions. We conclude that even the best fits with superfluid dark matter are still unsatisfactory for two reasons. First, the resulting stellar mass-to-light ratios show an unnatural trend with galaxy size. Second, the fits do not end up in the regime that automatically resembles MOND, and if we force the fits to do so, the total dark matter mass is in tension with strong lensing data.

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“…Dwarf galaxies have proven to be important laboratories to test principles of current dark energy and cold dark matter cosmology (ΛCDM), despite their difficulty to observe (e.g., Bullock & Boylan-Kolchin 2017;Lelli 2022). Cosmological simulations of cold dark matter predict a cusp-like dark matter density distribution near galaxy centres, meaning the density has a power-law slope (𝛽) between 1 and 1.5 (e.g., Navarro et al 1996b;Moore et al 1999) 1 .…”

Section: Introductionmentioning

confidence: 99%

“…both steeper and shallower slopes) and must be accounted for to understand any underlying physical rotation curve diversity (e.g., Oman et al 2015Oman et al , 2019Santos-Santos et al 2018Jahn et al 2021). Therefore, while care should be taken to properly account for and measure non-circular motions in rotation curve analyses, such errors are unlikely to fully alleviate the core-cusp problem (e.g., Kaplinghat et al 2020;Lelli 2022).…”

Section: Introductionmentioning

confidence: 99%

Cuspy dark matter density profiles in massive dwarf galaxies

Cooke,

Levy,

Bolatto

et al. 2022

Preprint

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Rotation curves of galaxies probe their total mass distributions, including dark matter. Dwarf galaxies are excellent systems to investigate the dark matter density distribution, as they tend to have larger fractions of dark matter compared to higher mass systems. The core-cusp problem describes the discrepancy found in the slope of the dark matter density profile in the centres of galaxies (𝛽 * ) between observations of dwarf galaxies (shallower cores) and dark matter-only simulations (steeper cusps). We investigate 𝛽 * in six nearby spiral dwarf galaxies for which high-resolution CO 𝐽 = 1 − 0 data were obtained with ALMA. We derive rotation curves and decompose the mass profile of the dark matter using our CO rotation curves as a tracer of the total potential and 4.5 𝜇m photometry to define the stellar mass distribution. We find 𝛽 * = 0.6 with a standard deviation of ±0.1 among the galaxies in this sample, in agreement with previous measurements in this mass range. The galaxies studied are on the high stellar mass end of dwarf galaxies and have cuspier profiles than lower mass dwarfs, in agreement with other observations. When the same definition of the slope is used, we observe steeper slopes than predicted by the FIRE and NIHAO simulations. This may signal that these relatively massive dwarfs underwent stronger gas inflows toward their centres than predicted by these simulations, that these simulations over-predict the frequency of accretion or feedback events, or that a combination of these or other effects are at work.

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Gas dynamics in dwarf galaxies as testbeds for dark matter and galaxy evolution

Cited by 27 publications

References 180 publications

Interpretation of galaxy rotation curves from primordial black holes in 4D Einstein-Gauss-Bonnet gravity

Interpretation of galaxy rotation curves from primordial black holes in 4D Einstein-Gauss-Bonnet gravity

Galactic mass-to-light ratios with superfluid dark matter

Cuspy dark matter density profiles in massive dwarf galaxies

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