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Title:
Cosmic reionization in dynamic quintessence cosmology
Authors:
Crociani, D.; Viel, M.; Moscardini, L.; Bartelmann, M.; Meneghetti, M.
Affiliation:
AA(Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, I-40127 Bologna, Italy), AB(INAF - Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, I-34131 Trieste, Italy; INFN/National Institute for Nuclear Physics, Sezione di Trieste, via Valerio 2, I-34127 Trieste, Italy), AC(Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, I-40127 Bologna, Italy; INFN/National Institute for Nuclear Physics, Sezione di Bologna, viale Berti Pichat 6/2, I-40127 Bologna, Italy), AD(Zentrum für Astronomie, ITA, Universität Heidelberg, Albert-Überle-Str. 2, D-69120 Heidelberg, Germany), AE(INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 385, Issue 2, pp. 728-736. (MNRAS Homepage)
Publication Date:
04/2008
Origin:
MNRAS
Astronomy Keywords:
galaxies: evolution , intergalactic medium , cosmology: theory
DOI:
10.1111/j.1365-2966.2008.12894.x
Bibliographic Code:
2008MNRAS.385..728C

Abstract

In this paper, we investigate the effects that a dynamic dark energy component dominant in the universe at late epochs has on reionization. We follow the evolution of HII regions with the analytic approach of Furlanetto & Oh in two different universes for which we assume the Peebles & Ratra and Brax & Martin quintessence models and we compare our results to the Λ cold dark matter (ΛCDM) scenario. We show that, for a fixed ionization efficiency, at the same cosmological epoch the morphology of bubbles is dominated by high-mass objects and the characteristic size of the ionized regions is slightly smaller than in the ΛCDM model, especially at the latest stages of reionization, due to the higher recombination efficiency. As a consequence, the bubbles' `epoch of overlap' happens earlier than in ΛCDM. Finally, we show how the different evolution of the HII regions affects the transmission of the high-z quasi-stellar object spectra, reducing the Lyman flux absorption at small optical depths.

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