2002
DOI: 10.1016/s0370-2693(02)01218-2
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Constraining quintessence with the new CMB data

Abstract: The CMB data recently released by BOOMERANG and MAXIMA suggest that the anisotropy spectrum has a third peak in the range 800 < l3 < 900. A combination of this result with constraints from large-scale structure permit us to differentiate between different quintessence models. In particular, we find that inverse power law models with power α > 1 are disfavoured. Models with more than 5% quintessence before last scattering require a spectral index greater than 1. These constraints are compared with supernovae ob… Show more

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Cited by 27 publications
(27 citation statements)
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“…Cosmological constraints derived from the location of the CMB peaks have been presented in previous works (e.g. [24][25][26]). Here our aim is to derive bounds on dark energy which are independent of supernova Ia data and rely only on the cosmic distance information encoded in the angular scale of the sound horizon as inferred from the multipole position of the WMAP peaks and dips, and BAO measurements.…”
Section: Parameter Inferencementioning
confidence: 99%
“…Cosmological constraints derived from the location of the CMB peaks have been presented in previous works (e.g. [24][25][26]). Here our aim is to derive bounds on dark energy which are independent of supernova Ia data and rely only on the cosmic distance information encoded in the angular scale of the sound horizon as inferred from the multipole position of the WMAP peaks and dips, and BAO measurements.…”
Section: Parameter Inferencementioning
confidence: 99%
“…Since the results depend only logarithmically on the cutoffs, this choice is not critical, and in addition ln(M P /H) ≈ 140, which is small. From Equation (17,21,20), we see that, in leading order, the change in the quintessence potential due to this effective fermion coupling would be proportional to V (Φ cl ) and could hence be absorbed upon redefining the pre-factor of the potential (see also figure 5). In next to leading order, the contribution is proportional to V (Φ cl ) 2 , which is negligible.…”
Section: Figmentioning
confidence: 99%
“…If w is found to be different from −1, the dark energy is proven to be different from the simple cosmological constant. Current observational data are consistent with the cosmological constant [7,8], although they are still not enough to impose sufficient constraints on the EOS.Since the dark energy has profound implications on the nature of the universe, it is of great importance to explore the origin of dark energy. Near-future observations will enable us to clarify whether the dark energy is a mere cosmological constant or something else.…”
mentioning
confidence: 99%
“…Near-future observations will enable us to clarify whether the dark energy is a mere cosmological constant or something else. Cosmological observations, such as the Type Ia supernovae [9], CMB fluctuations [6,8,10], cluster mass function [11], weak lensing field [12], and so on, are useful tools to probe the nature of the dark energy.It is shown [13] that an application of the AlcockPaczynski (AP) test [14] to the redshift-space correlation function of the high-redshift objects can be a useful probe of the cosmological constant. In literatures, this method is mainly applied to the Lyman-α forest [15], the Lyman-break galaxies [16], and the quasars [17], etc.…”
mentioning
confidence: 99%
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