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Properties of the Dark Energy

Published online by Cambridge University Press:  26 May 2016

Peter M. Garnavich  and
Yun. Wang
Peter M. Garnavich
Affiliation:
University of Notre Dame, Notre Dame, IN 46556, USA
Yun. Wang
Affiliation:
University of Oklahoma, Norman, OK 73019, USA

Abstract

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A non-zero cosmological constant is only one of many possible explanations for the observed accelerating expansion of the Universe. Any smoothly distributed, “dark” energy with a significant negative pressure can drive the acceleration. One possible culprit is a dynamical scalar field, but there are many less popular models such as tangled cosmic strings or domain walls. Soon theorists are likely to think up a number of new energies that can accelerate the expansion, meaning that only better observations can solve this question. Dark energy can be parameterized by its equation of state, w = p/ρ, which in the most general form can vary over time. Unlike the CMB, supernova observations cover a range of redshift so they can, in principle, probe the variation in the equation of state of the unknown component. The current SN observations loosely constrain the equation of state to w < −0.6, ruling out non-intercommuting strings and textures (w = −1/3), but consistent with a cosmological constant (w = −1). The constraints achievable from future large SN surveys are limited by our ability to understand systematic effects in SN Ia luminosities. But a large sample of supernovae reaching out to z ˜ 2 should at least discriminate between a cosmological constant and a dynamical scalar field as the source of the observed acceleration.

Type
Part VII: Evidence for non-zero A
Information
Symposium - International Astronomical Union , Volume 201: New Cosmological Data and the Values of the Fundamental Parameters , 2005 , pp. 255 - 259
Copyright
Copyright © Astronomical Society of the Pacific 2005 

References

Armendariz-Picon, C., Mukhanov, V., Steinhardt, P. J. 2000, Phys. Rev. Lett. 85, 4438.CrossRefGoogle Scholar
Balbi, A., et al. 2000, astro-ph/0005124.Google Scholar
Jha, S., et al. 1999, ApJS, 125, 73.CrossRefGoogle Scholar
Caldwell, R. R., Dave, R., Steinhardt, P. J. 1998, Phys. Rev. Lett. 80, 1582.CrossRefGoogle Scholar
de Bernardis, P., et al. 2000, Nature, 404, 955.CrossRefGoogle Scholar
Efstathiou, 1999, MNRAS, 310, 842.CrossRefGoogle Scholar
Garnavich, P. M. et al. 1998, ApJ, 493, L53.CrossRefGoogle Scholar
Garnavich, P. M. et al. 1998, ApJ, 509, 74.CrossRefGoogle Scholar
Moar, I., Brustein, R. & Steinhardt, P. J. 2000, astro-ph/0007297.Google Scholar
Perlmutter, S., et al. 1999, ApJ, 517, 565.CrossRefGoogle Scholar
Phillips, M. M. 1993, ApJ, 413, L105.CrossRefGoogle Scholar
Riess, A. G., Press, W. H. & Kirshner, R. P. 1995, ApJ, 438, L17.CrossRefGoogle Scholar
Riess, A. G., et al. 1998, AJ, 116, 1009.CrossRefGoogle Scholar
Schmidt, B. P., et al. 1998, ApJ, 507, 46.CrossRefGoogle Scholar
Steinhardt, P.J., Wang, L. & Zlatev, I. 1999, Phys. Rev. D59, 123504.Google Scholar
Wald, R. M. 1984, General Relativity, The University of Chicago Press, Chicago and London.CrossRefGoogle Scholar
Wang, Y. & Garnavich, P. M. 2001, astro-ph/0101040.Google Scholar
White, M. 1998, ApJ, 506, 495.CrossRefGoogle Scholar