A unified solution to the small scale problems of the $\Lambda$CDM model

Abstract

We study, by means of the model proposed in Del Popolo (2009), the effect of baryon physics on the small scale problems of the CDM model. We show that, using this model, the cusp/core problem, the missing satellite problem (MSP), the Too Big to Fail (TBTF) problem, and the angular momentum catastrophe can be reconciled with observations. Concerning the cusp/core problem, the interaction among dark matter (DM) and baryonic clumps of 1% the mass of the halo, through dynamical friction (DF), is able to flatten the inner cusp of the density profiles. We moreover assume that haloes form primarily through quiescent accretion, in agreement with the spherical collapse model (SCM)-secondary infall model (SIM) prescriptions. The results of this paper follow from the two assumptions above. Concerning the MSP and TBTF problem, applying to the Via Lactea II (VL2) subhaloes a series of corrections similar to those of Brooks et al. (2013), namely applying a Zolotov et al. (2012)-like correction obtained with our model, and further correcting for the UV heating and tidal stripping, we obtain that the number of massive, luminous satellites is in agreement with the number observed in the MW. The model also produces an angular momentum distribution in agreement with observations, that is with the distribution of the angular spin parameter and angular momentum of the dwarfs studied by van den Bosch, Burkert, & Swaters (2001). In conclusion, the small scale problems of the CDM model can all be solved by introducing baryon physics.

29 pages; 6 Figures; JCAP accepted

References in corpus (21)

• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Cold streams in early massive hot haloes as the main mode of galaxy formation
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• Massloss of galaxies due to a UV-background
• Stellar Feedback in Dwarf Galaxy Formation
• Cosmological puzzle resolved by stellar feedback in high redshift galaxies
• Detection of a 60 Degree-Long Dwarf Galaxy Debris Stream
• The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach
• Clumpy Galaxies in GOODS and GEMS: Massive Analogs of Local Dwarf Irregulars
• Erasing Dark Matter Cusps in Cosmological Galactic Halos with Baryons
• Baryonic Pinching of Galactic Dark Matter Halos
• Dark matter subhalos and the dwarf satellites of the Milky Way
• Dissecting Galaxy Formation: I. Comparison Between Pure Dark Matter and Baryonic Models
• The Structure of Halos: Implications for Group and Cluster Cosmology
• Discovery of a Faint Old Stellar System at 150 kpc
• Dark matter and structure formation a review
• Discreteness Effects in Lambda Cold Dark Matter Simulations: A Wavelet-Statistical View
• Shear and rotation in Chaplygin cosmology
• Is the Concentration of Dark Matter Halos at Virialization Universal ?
• Secondary infall and dark matter haloes
• f(R) and f(T) theories of modified gravity

Cited by in corpus (15)

• Is there a "too big to fail" problem in the field?
• Self-Scattering for Dark Matter with an Excited State
• Dark compact objects: an extensive overview
• On the surface density of dark matter haloes
• A high precision semi-analytic mass function
• Simulations of galaxies formed in warm dark matter halos of masses at the filtering scale
• A unified solution to the small scale problems of the $\Lambda$CDM model II: introducing parent-satellite interaction
• Modified gravity models and the central cusp of dark matter halos in galaxies
• The flat density profiles of massive, and relaxed galaxy clusters
• Re-examining the Too-Big-To-Fail Problem for Dark Matter Haloes with Central Density Cores
• Running with BICEP2: Implications for Small-Scale Problems in CDM
• Ejection of supermassive black holes and implications for merger rates in fuzzy dark matter haloes
• Matter-Antimatter Asymmetry Induced by a Running Vacuum Coupling
• Quantifying Departures from Equilibrium with the Spherical Jeans Equation
• Cluster density slopes from Dark Matter-Baryons Energy Transfer