Response to Editorial on Albrecht et al. (2006)

Albrecht, Phillip J.; Davar, Gudarz; Eisenberg, Elon; Paré, Michel; Rice, Frank L.

doi:10.1016/j.pain.2006.03.007

Cited by 342 publications

(474 citation statements)

References 5 publications

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“…Aiming for launch in 2019, it would cover about 20,000 deg 2 of sky providing around 150 million redshifts in the range z < 2. Here, we consider forecast constraints from EUCLID and a Supernova SNAP-like survey (or dark energy task force stage IV SNe mission) [64].…”

Section: Intermediate Redshifts: Euclid/snap (Distance Measurements)mentioning

confidence: 99%

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

Avgoustidis

Luzzi

Martins

et al. 2012

J. Cosmol. Astropart. Phys.

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Abstract. The relation between redshift and the CMB temperature, T CMB (z) = T 0 (1 + z) is a key prediction of standard cosmology, but is violated in many nonstandard models. Constraining possible deviations to this law is an effective way to test the ΛCDM paradigm and search for hints of new physics. We present state-ofthe-art constraints, using both direct and indirect measurements. In particular, we point out that in models where photons can be created or destroyed, not only does the temperature-redshift relation change, but so does the distance duality relation, and these departures from the standard behaviour are related, providing us with an opportunity to improve constraints. We show that current datasets limit possible deviations of the form T CMB (z) = T 0 (1 + z) 1−β to be β = 0.004 ± 0.016 up to a redshift z ∼ 3. We also discuss how, with the next generation of space and ground-based experiments, these constraints can be improved by more than one order of magnitude.

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Section: Intermediate Redshifts: Euclid/snap (Distance Measurements)mentioning

confidence: 99%

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

Avgoustidis

Luzzi

Martins

et al. 2012

J. Cosmol. Astropart. Phys.

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“…The evolution of w q for these models is poorly described by parametrizations such as w = w 0 + w a z(1 + z) −1 , often used in the literature, e.g. [8,25] and used by the dark energy task force to define a figure of merit for comparing future dark energy surveys [22]. Note that w q for these models varies wildly above z ∼ 5.…”

Section: Dynamical Modelsmentioning

confidence: 99%

“…We will not discuss the relative merits of these methods here. Summaries of many of these projects can be found in [22,23]. Provided systematic errors can be kept under control, it may be possible to constrain w to an accuracy of a percent or so within the next decade.…”

Section: Introductionmentioning

confidence: 99%

Can we ever distinguish between quintessence and a cosmological constant?

Chongchitnan

Efstathiou

2007

Phys. Rev. D

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Many ambitious experiments have been proposed to constrain dark energy and detect its evolution. At present, observational constraints are consistent with a cosmological constant and there is no firm evidence for any evolution in the dark energy equation of state w. In this paper, we pose the following question: suppose that future dark energy surveys constrain w at low redshift to be consistent with −1 to a percent level accuracy, what are the implications for models of dynamical dark energy? We investigate this problem in a model-independent way by following quintessence field trajectories in 'energy' phase-space. Attractor dynamics in this phase-space leads to two classes of acceptable models: 1) models with flat potentials, i.e. an effective cosmological constant, and 2) models with potentials that suddenly flatten with a characteristic kink. The prospect of further constraining the second class of models from distance measurements and fluctuation growth rates at low redshift (z 3) seems poor. However, in some models of this second class, the dark energy makes a significant contribution to the total energy density at high redshift. Such models can be further constrained from observation of the cosmic microwave background anisotropies and from primordial nucleosynthesis. It is possible, therefore, to construct models in which the dark energy at high redshift causes observable effects, even if future dark energy surveys constrain w at low redshift to be consistent with −1 to high precision.

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“…Recently, the Dark Energy Task Force (DETF) [1] released a report to guide the planning of future dark-energy observations. The DETF used a dark-energy ''figure of merit'' (FoM) based on a two-parameter description of the dark-energy evolution in order to produce quantitative findings.…”

Section: Introductionmentioning

confidence: 99%

Evaluating dark energy probes using multidimensional dark energy parameters

Albrecht

Bernstein

2007

Phys. Rev. D

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We investigate the value of future dark-energy experiments by modeling their ability to constrain the darkenergy equation of state. Similar work was recently reported by the Dark Energy Task Force (DETF) using a two dimensional parameterization of the equation-of-state evolution. We examine constraints in a ninedimensional dark-energy parameterization, and find that the best experiments constrain significantly more than two dimensions in our 9D space. Consequently the impact of these experiments is substantially beyond that revealed in the DETF analysis, and the estimated cost per ''impact'' drops by about a factor of 10 as one moves to the very best experiments. The DETF conclusions about the relative value of different techniques and of the importance of combining techniques are unchanged by our analysis. We investigate the value of future dark-energy experiments by modeling their ability to constrain the dark-energy equation of state. Similar work was recently reported by the Dark Energy Task Force (DETF) using a two dimensional parameterization of the equation-of-state evolution. We examine constraints in a nine-dimensional dark-energy parameterization, and find that the best experiments constrain significantly more than two dimensions in our 9D space. Consequently the impact of these experiments is substantially beyond that revealed in the DETF analysis, and the estimated cost per ''impact'' drops by about a factor of 10 as one moves to the very best experiments. The DETF conclusions about the relative value of different techniques and of the importance of combining techniques are unchanged by our analysis. Disciplines Physical Sciences and Mathematics | Physics

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Response to Editorial on Albrecht et al. (2006)

Cited by 342 publications

References 5 publications

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

Can we ever distinguish between quintessence and a cosmological constant?

Evaluating dark energy probes using multidimensional dark energy parameters

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