PROBING DARK ENERGY: METHODS AND STRATEGIES

By D. Huterer, M. Turner. 2000

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The presence of dark energy in the Universe is inferred directly from the accelerated expansion of the Universe, and indirectly, from measurements of cosmic microwave background (CMB) anisotropy. Dark energy contributes about 2/3 of the critical density, is very smoothly distributed, and has large negative pressure. Its nature is very much unknown. Most of its discernible consequences follow from its effect on evolution of the expansion rate of the Universe, which in turn affects the growth of density perturbations and the age of the Universe, and can be probed by the classical kinematic cosmological tests. Absent a compelling theoretical model (or even a class of models), we describe the dark energy by an effective equation-of-state w=p_X/\rho_X which is allowed to vary with time. We describe and compare different approaches for determining w(t), including magnitude-redshift (Hubble) diagram, number counts of galaxies and clusters, and CMB anisotropy, focusing particular attention on the use of a sample of several thousand type Ia supernova with redshifts z\lesssim 1.7, as might be gathered by the proposed SNAP satellite. Among other things, we derive optimal strategies for constraining cosmological parameters using type Ia supernovae. While in the near term CMB anisotropy will provide the first measurements of w, supernovae and number counts appear to have the most potential to probe dark energy.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/77b05bd6987667443fe008ea785a3c1677d9e3a7

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Citations in the corpus

Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys (2003, background): “…the physical origin of dark energy (Hui et al. 1999; Cooray & Huterer 1999; Huterer & Turner 1999; Newman & Davis 2000; Haiman et al. 2001; Huterer & Turner 2001; Maor, Brustein, & Steinhardt 2001; Wang & Garnavich 2001; Kujat et al. 2002; Maor, Brustein, McMahon, & Steinhardt 2002;…”
K-Corrections and Spectral Templates of Type Ia Supernovae (2007, background): “The measurement of the equation-of-state parameter can exclude certain theoretical models of dark energy (Huterer & Turner 2001).”
New Hubble Space Telescope Discoveries of Type Ia Supernovae at z ≥ 1: Narrowing Constraints on the Early Behavior of Dark Energy (2006, background): “Citing a popular metric, the area of the 95% confidence interval (Huterer & Turner 2001; Kolb et al. 2006; Albrecht & Bernstein 2006), we note a reduction by 40% or an increase in the figure of merit (inverse area) by a factor of 1.7 by the inclusion of the gold-quality SNe Ia from HSTwith the weak…”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, methodology): “Clusters also can be used as an independent and complementary Dark Energy probe (Starobinsky 1998; Wang & Steinhardt 1998; Huterer & Turner 2001; Haiman et al. 2001; Battye & Weller 2003; Molnar et al. 2004; Hu & Cohn 2006).”
Interpreting DESI's evidence for evolving dark energy (2024, positive): “The use of pivots for dark energy, where the pivot is at a time rather than a length, was initiated by Huterer and Turner [15] who used a pivot within a parametrization of w with redshift.”
The Cosmological Constant and Dark Energy (2002, background): “Either way, with further work galaxy counts may provide an important test for dark energy and its evolution (Newman and Davis, 2000; Huterer and Turner, 2001; Podariu and Ratra, 2001).”
Observational probes of cosmic acceleration (2012, background): “These include the determinant of Fw, which characterizes the total volume of parameter space allowed by a particular combination of experiments in analogy to the 78This partly depends on the choice of fiducial model at which the Fisher matrix used to construct the PCs is computed.”