2010/04/16 by Hong Li, Jun-Qing Xia
Physics and Astronomy · #Baryon acoustic oscillations #CMB cold spot #Cosmic background radiation #Cosmic microwave background #Cosmology and Gravitation Theories #Dark energy #Galaxies: Formation, Evolution, Phenomena #Hubble's law #Observational cosmology #Particle physics theoretical and experimental studies #Scale factor (cosmology) #Supernova #astro-ph.CO
paper · pdf · doi:10.1088/1475-7516/2010/04/026
published as JCAP 1004:026,2010 · 6 pages, 4 figures, accepted for publication in JCAP
arxiv created 2010/04/16 · openalex publication_date 2010/04/26 · arxiv updated 2010/05/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In this paper, we combine the the latest observational data, including the WMAP five-year data (WMAP5), the baryon acoustic oscillations (BAO) and type Ia supernovae (SN) ``union" compilation, and use the Markov Chain Monte Carlo method to determine the dark energy parameters. We pay particular attention to the Integrated Sache-Wolfe (ISW) data from the cross-correlations of cosmic microwave background (CMB) and large scale structure (LSS). In the ΛCDM model, we find that the ISW data, as a complement to the WMAP data, could significantly improve the constraint of curvature Ω k . We also check the improvement of constraints from the new prior on the Hubble constant and find this new prior could improve the constraint of Ω k by a factor of 2. Finally, we study the dynamical evolving EoS of dark energy from the current observational data. Based on the dynamical dark energy model, parameterizing as w ( a ) = w 0 + w a (1− a ), we find that the ΛCDM model remains a good fit to the current data. When taking into account the ISW data, the error bars of w 0 and w a could be shrunk slightly. Current constraints on the dynamical dark energy model are not conclusive. The future precision measurements are needed.