1999/04/26 by G. Efstathiou · 6 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Particle physics theoretical and experimental studies #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.1999.02997.x
9 pages, 8 Postscript figures, uses mn.sty. submitted to MNRAS
arxiv created 1999/04/26 · openalex publication_date 1999/12/11 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
The magnitude—redshift relation for Type Ia supernovae is beginning to provide strong constraints on the cosmic densities contributed by matter, Ωm, and a cosmological constant, ΩΛ, although the results are highly degenerate in the Ωm—ΩΛ plane. Here we estimate the constraints that can be placed on a cosmological constant or quintessence-like component by extending supernovae samples to high redshift. Such measurements, when combined with constraints from anisotropies in the cosmic microwave background (CMB), could provide an important consistency check of systematic errors in the supernovae data. A large campaign of high-z supernovae observations with 10-m class telescopes could constrain Ωm to an accuracy (1σ) of 0.06 and ΩΛ to 0.15. A sample of supernovae at redshift z∼3, as might be achievable with a Next Generation Space Telescope, could constrain Ωm to an accuracy of about 0.02 independently of the value of ΩΛ. The constraints on a more general equation of state, wQpρ, converge slowly as the redshift of the supernovae data is increased. The most promising way of setting accurate constraints on wQ is by combining high-z supernovae and CMB measurements. With feasible measurements it should be possible to constrain wQ to a precision of about 0.06, if the Universe is assumed to be spatially flat. We use the recent supernovae sample of Perlmutter et al. and observations of the CMB anisotropies to constrain the equation of state in quintessence-like models via a likelihood analysis. The 2σ upper limits are wQ<−0.6 if the Universe is assumed to be spatially flat, and wQ<−0.4 for universes of arbitrary spatial curvature. The upper limit derived for a spatially flat Universe is close to the lower limit (wQ≈−0.7) allowed for simple potentials, implying that additional fine tuning may be required to construct a viable quintessence model.