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Annual Review of Astronomy and Astrophysics

Volume 55, 2017

Small-Scale Challenges to the CDM Paradigm

Abstract

The dark energy plus cold dark matter (ΛCDM) cosmological model has been a demonstrably successful framework for predicting and explaining the large-scale structure of the Universe and its evolution with time. Yet on length scales smaller than ∼1 Mpc and mass scales smaller than ∼1011M, the theory faces a number of challenges. For example, the observed cores of many dark matter–dominated galaxies are both less dense and less cuspy than naïvely predicted in ΛCDM. The number of small galaxies and dwarf satellites in the Local Group is also far below the predicted count of low-mass dark matter halos and subhalos within similar volumes. These issues underlie the most well-documented problems with ΛCDM: cusp/core, missing satellites, and too-big-to-fail. The key question is whether a better understanding of baryon physics, dark matter physics, or both is required to meet these challenges. Other anomalies, including the observed planar and orbital configurations of Local Group satellites and the tight baryonic/dark matter scaling relations obeyed by the galaxy population, have been less thoroughly explored in the context of ΛCDM theory. Future surveys to discover faint, distant dwarf galaxies and to precisely measure their masses and density structure hold promising avenues for testing possible solutions to the small-scale challenges going forward. Observational programs to constrain or discover and characterize the number of truly dark low-mass halos are among the most important, and achievable, goals in this field over the next decade. These efforts will either further verify the ΛCDM paradigm or demand a substantial revision in our understanding of the nature of dark matter.

Keyword(s): cosmology, dark matter, dwarf galaxies, galaxy formation, Local Group

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2017-08-18
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/content/journals/10.1146/annurev-astro-091916-055313
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Small-Scale Challenges to the ΛCDM Paradigm
Annual Review of Astronomy and Astrophysics 55, 343 (2017); https://doi.org/10.1146/annurev-astro-091916-055313
/content/journals/10.1146/annurev-astro-091916-055313
/content/journals/10.1146/annurev-astro-091916-055313
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    The missing satellites problem: predicted ΛCDM substructure () versus known MW satellites (). Panel (by M. Pawlowski in collaboration with the authors) shows the current census of MW satellite galaxies, with galaxies discovered since 2015 in red. The Galactic disk is represented by a circle of radius 15 kpc at the center, and the outer sphere has a radius of 250 kpc. The 11 brightest (classical) MW satellites are labeled by name. Sizes of the symbols are not to scale but are rather proportional to the log of each satellite galaxy's stellar mass. Currently, there are ∼50 satellite galaxies known in the MW as compared to thousands of predicted subhalos with ≳107M. Abbreviations: dSph, dwarf spheroidal; LMC, Large Magellanic Cloud; MW, Milky Way; SMC, Small Magellanic Cloud.

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