Constraints on models with a break in the primordial power spectrum |
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Authors: | Hong Li Jun-Qing Xia Robert Brandenberger Xinmin Zhang |
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Institution: | 1. Institute of High Energy Physics, Chinese Academy of Science, P.O. Box 918-4, Beijing 100049, PR China;2. Theoretical Physics Center for Science Facilities (TPCSF), Chinese Academy of Science, PR China;3. Kavli Institute for Theoretical Physics, Chinese Academy of Science, Beijing 100190, PR China;4. Scuola Internazionale Superiore di Studi Avanzati, Via Bonomea 265, I-34136 Trieste, Italy;5. Department of Physics, McGill University, 3600 University Street, Montreal, QC, H3A 2T8, Canada |
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Abstract: | One of the characteristics of the “Matter Bounce” scenario, an alternative to cosmological inflation for producing a scale-invariant spectrum of primordial adiabatic fluctuations on large scales, is a break in the power spectrum at a characteristic scale, below which the spectral index changes from ns=1 to ns=3. We study the constraints which current cosmological data place on the location of such a break, and more generally on the position of the break and the slope at length scales smaller than the break. The observational data we use include the WMAP five-year data set (WMAP5), other CMB data from BOOMERanG, CBI, VSA, and ACBAR, large-scale structure data from the Sloan Digital Sky Survey (SDSS, their luminous red galaxies sample), Type Ia Supernovae data (the “Union” compilation), and the Sloan Digital Sky Survey Lyman-α forest power spectrum (Lyα) data. We employ the Markov Chain Monte Carlo method to constrain the features in the primordial power spectrum which are motivated by the matter bounce model. We give an upper limit on the length scale where the break in the spectrum occurs. |
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Keywords: | Bounce cosmology Astronomical observational data |
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