Constraining the dark energy with galaxy clusters X-ray data
| dc.creator | Lima, J. A. S. | |
| dc.creator | Cunha, J. V. | |
| dc.creator | Alcaniz, J. S. | |
| dc.date | 2003-03-17 | |
| dc.date.accessioned | 2026-07-07T11:08:11Z | |
| dc.date.available | 2026-07-07T11:08:11Z | |
| dc.description | The equation of state characterizing the dark energy component is constrained by combining Chandra observations of the X-ray luminosity of galaxy clusters with independent measurements of the baryonic matter density and the latest measurements of the Hubble parameter as given by the HST key project. By assuming a spatially flat scenario driven by a "quintessence" component with an equation of state $p_x = ωρ_x$ we place the following limits on the cosmological parameters $ω$ and $Ω_{\rm{m}}$: (i) $-1 \leq ω\leq -0.55$ and $Ω_{\rm m} = 0.32^{+0.027}_{-0.014}$ (1$σ$) if the equation of state of the dark energy is restricted to the interval $-1 \leq ω< 0$ (\emph{usual} quintessence) and (ii) $ω= -1.29^{+0.686}_{-0.792}$ and $Ω_{\rm{m}} = 0.31^{+0.037}_{-0.034}$ ($1σ$) if $ω$ violates the null energy condition and assume values $< -1$ (\emph{extended} quintessence or ``phantom'' energy). These results are in good agreement with independent studies based on supernovae observations, large-scale structure and the anisotropies of the cosmic background radiation. | |
| dc.description | 6 pages, 4 figures, LaTeX | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0303388 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0303388 | |
| dc.identifier | Phys.Rev.D68:023510,2003 | |
| dc.identifier | doi:10.1103/PhysRevD.68.023510 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/190052 | |
| dc.subject | Astrophysics | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | Constraining the dark energy with galaxy clusters X-ray data | |
| dc.type | text |