Dark Matter and Energy in the Universe

Abstract

For the first time, we have a plausible and complete accounting of matter and energy in the Universe. Expressed a fraction of the critical density it goes like this: neutrinos, between 0.3% and 15%; stars, between 0.3% and 0.6%; baryons (total), 5% +/- 0.5%; matter (total), 40% +/- 10%; smooth, dark energy, 80% +/- 20%; totaling to the critical density (within the errors). This accounting is consistent with the inflationary prediction of a flat Universe and defines three dark-matter problems: Where are the dark baryons? What is the nonbaryonic dark matter? What is the nature of the dark energy? The leading candidate for the (optically) dark baryons is diffuse hot gas; the leading candidates for the nonbaryonic dark matter are slowly moving elementary particles left over from the earliest moments (cold dark matter), such as axions or neutralinos; the leading candidates for the dark energy involve fundamental physics and include a cosmological constant (vacuum energy), a rolling scalar field (quintessence), and a network of light, frustrated topological defects.

30 pages LaTeX with 10 eps figures. To be published in Physica Scripta (Proceedings of the Nobel Symposium, Particle Physics and the Universe; Enkoping, Sweden, August 20-25, 1998)

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• First Results of the EDELWEISS WIMP Search using a 320 g Heat-and-Ionization Ge Detector
• How Cold Dark Matter Theory Explains Milgrom's Law
• The Case for Omega_M = 0.33 +/- 0.035
• A model of the Universe including Dark Energy accounted for by both a Quintessence Field and a (negative) Cosmological Constant
• Regular black holes in $f(G)$ gravity
• Extended Quintessence and its Late-time Domination
• One Hundred Years of the Cosmological Constant: from 'Superfluous Stunt' to Dark Energy
• A Supernova Brane Scan
• Constraints on $R^n$ gravity from precession of orbits of S2-like stars: a case of a bulk distribution of mass
• Two viable quintessence models of the Universe: confrontation of theoretical predictions with observational data
• Quintessential Inflation in a thawing realization
• Precision Cosmology and the Density of Baryons in the Universe
• Effects of quintessence on observations of Type Ia SuperNovae in the clumpy Universe
• Dark Energy and the Statistical Study of the Observed Image Separations of the Multiply Imaged Systems in the CLASS Statistical Sample
• Perturbative approach for mass varying neutrinos coupled to the dark sector in the generalized Chaplygin gas scenario
• Massive Compact Halo Objects from the Relics of the Cosmic Quark-Hadron Transition
• DESI Dark Energy Time Evolution is Recovered by Cosmologically Coupled Black Holes
• Constraints in Cosmological Parameter Space from the Sunyaev-Zel'dovich Effect and Thermal Bremsstrahlung
• TASI Lectures: Cosmology for String Theorists
• Generalizations of normal ordering and applications to quantization in classical backgrounds
• Cosmological constraints on a dark matter -- dark energy interaction
• Is the Universe Inflating? Dark Energy and the Future of the Universe
• Probing the dark energy with quasar clustering
• Exploring Fermionic Dark Matter Admixed Neutron Stars in the Light of Astrophysical Observations
• Questions of Identity
• Inhomogeneous cosmologies with Q-matter and varying $\Lambda$
• Dark Energy and the quietness of the Local Hubble Flow
• The Casimir Effect for Parallel Plates Revisited
• On a class of scaling FRW cosmological models
• Gravitational lenses in the dark Universe
• Cosmic rays from AGN, the knee energy mass scale and dark matter particles
• On the Casimir energy for a massive quantum scalar field and the Cosmological constant
• On the cosmological vacuum and dark energy