Late-time dark matter oscillations and the core-cusp problem

Cline, James M.; Gambini, Guillermo; McDermott, Samuel D.; Puel, Matteo

doi:10.1007/jhep04(2021)223

Cited by 1 publication

(1 citation statement)

References 92 publications

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“…So what happened to the cusps? A popular explanation is that baryonic inflows and outflows early in the galaxy's evolution (e.g., Pontzen & Governato 2012), or something more exotic like emergent dark-matter annihilation (e.g., Cline et al 2021), have smoothed out the precursor DM cusp. While baryonic processes are effective in the low-mass limit, these do not operate well in massive galaxies (V c  150 km s −1 ).…”

Section: Introductionmentioning

confidence: 99%

The Rapid Onset of Stellar Bars in the Baryon-dominated Centers of Disk Galaxies

Bland-Hawthorn

Tepper-García

Agertz

et al. 2023

ApJ

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Recent observations of high-redshift galactic disks (z ≈ 1–3) show a strong negative trend in the dark-matter (DM) fraction f DM with increasing baryon surface density. For this to be true, the inner baryons must dominate over DM in early massive galaxies, as observed in the Milky Way today. If disks are dominant at early times, we show that stellar bars form promptly within these disks, leading to a high bar fraction. New James Webb Space Telescope observations provide the best evidence for mature stellar bars in this redshift range. The disk mass fraction f disk within R s = 2.2 R disk is the dominant factor determining how rapidly a bar forms. Using 3D hydro simulations of halo-bulge-disk galaxies, we confirm the “Fujii relation” for the exponential dependence of the bar formation time τ bar as a function of f disk. For f disk > 0.3, the bar formation time declines exponentially fast with increasing f disk. Instead of Fujii's arbitrary threshold for when a bar appears, for the first time, we exploit the exponential growth timescale associated with the positive feedback cycle as the bar emerges from the underlying disk. A modified, mass-dependent trend is observed for halos relevant to systems at cosmic noon ( 10.5 < log M halo < 12 ), where the bar onset is slower for higher-mass halos at a fixed f disk. If baryons dominate over DM within R ≈ R s , we predict that a high fraction of bars will be found in high-redshift disks long before z = 1.

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Section: Introductionmentioning

confidence: 99%