TY - JOUR
T1 - Probing for dynamics of dark energy and curvature of universe with latest cosmological observations
AU - Zhao, Gong-Bo
AU - Xia, Jun-Qing
AU - Li, Hong
AU - Tao, Charling
AU - Virey, Jean-Marc
AU - Zhu, Zong-Hong
AU - Zhang, Xinmin
N1 - The wrongly-generated last page of pdf file is removed.
PY - 2007/4/26
Y1 - 2007/4/26
N2 - We use the newly released 182 Type Ia supernova data combined with the third-year Wilkinson Microwave Anisotropic Probe data (WMAP3) and large scale structure (LSS) information including SDSS and 2dFGRS to constrain the dark energy equation of state (EoS) as well as the curvature of universe ΩK. Using the full dataset of Cosmic Microwave Background (CMB) and LSS rather than the shift parameter and linear growth factor, we make a Markov Chain Monte Carlo (MCMC) global fit, while paying particular attention to the dark energy perturbation. Parameterizing the EoS as wDE (a) = w0 +w1 (1-a), we find the best fit of (w0,w1) is (-1.053,0.944) and for ωDE(a) = ω0 + ω1 sin(3/2 π In(a)), the best fit for (w0, w1) is (-1.614,-1.046). We find that a flat universe is a good approximation, namely, |ΩK|>0.06 has been excluded by 2σ yet the inclusion of ΩK can affect the measurement of DE parameters owing to their correlation and the present systematic effects of SNIa measurements.
AB - We use the newly released 182 Type Ia supernova data combined with the third-year Wilkinson Microwave Anisotropic Probe data (WMAP3) and large scale structure (LSS) information including SDSS and 2dFGRS to constrain the dark energy equation of state (EoS) as well as the curvature of universe ΩK. Using the full dataset of Cosmic Microwave Background (CMB) and LSS rather than the shift parameter and linear growth factor, we make a Markov Chain Monte Carlo (MCMC) global fit, while paying particular attention to the dark energy perturbation. Parameterizing the EoS as wDE (a) = w0 +w1 (1-a), we find the best fit of (w0,w1) is (-1.053,0.944) and for ωDE(a) = ω0 + ω1 sin(3/2 π In(a)), the best fit for (w0, w1) is (-1.614,-1.046). We find that a flat universe is a good approximation, namely, |ΩK|>0.06 has been excluded by 2σ yet the inclusion of ΩK can affect the measurement of DE parameters owing to their correlation and the present systematic effects of SNIa measurements.
KW - astro-ph
U2 - 10.1016/j.physletb.2007.02.070
DO - 10.1016/j.physletb.2007.02.070
M3 - Article
VL - 648
SP - 8
EP - 13
JO - Physical Letters B
JF - Physical Letters B
IS - 1
ER -