Parameterizing and Measuring Dark Energy Trajectories from Late Inflatons

• Published in: The Astrophysical journal Vol. 726; no. 2; pp. 64 - jQuery1323911902051='46'
• Main Authors: Huang, Zhiqi, Bond, J. Richard, Kofman, Lev
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 10.01.2011; IOP
• Subjects: Astronomy; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COSMOLOGY; Earth, ocean, space; EVOLUTION; Exact sciences and technology; MATTER; NONLUMINOUS MATTER; RED SHIFT; TRAJECTORIES; Red shift; Galaxies; Power spectra; Cosmic background radiation; Probability; Attractors; Energy density; Lyman alpha forest; Trajectories; Inflaton; cosmology: theory; Markov chain; Type I supernova; Cosmological parameter; Cosmology; Models; Dark energy; cosmological parameters
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/726/2/64

Bulk dark energy (DE) properties are determined by the redshift evolution of its pressure-to-density ratio, w de(z). An experimental goal is to decide if the DE is dynamical, as in the quintessence (and phantom) models treated here. We show that a three-parameter approximation w de(z; Delta *e s , Delta *e{infinity}, Delta *z s ) fits well the ensemble of trajectories for a wide class of late-inflaton potentials V(). Markov Chain Monte Carlo probability calculations are used to confront our w de(z) trajectories with current observational information on Type Ia supernova, cosmic microwave background, galaxy power spectra, weak lensing, and the Ly Delta *a forest. We find that the best-constrained parameter is a low-redshift slope parameter, Delta *e s ({partial differential}ln V/{partial differential})2 when the DE and matter have equal energy densities. A tracking parameter Delta *e{infinity} defining the high-redshift attractor of 1 + w de is marginally constrained. Delta *z s is poorly determined, which characterizes the evolution of Delta *e s , and is a measure of {partial differential}2ln V/{partial differential}2. The constraints we find already rule out some popular quintessence and phantom models, or restrict their potential parameters. We also forecast how the next generation of cosmological observations improve the constraints: by a factor of about five on Delta *e s and Delta *e{infinity}, but with Delta *z s remaining unconstrained (unless the true model significantly deviates from Delta *LCDM). Thus, potential reconstruction beyond an overall height and a gradient is not feasible for the large space of late-inflaton models considered here.