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    The epoch of reionization in the R h = ct universe

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    Author
    Melia, Fulvio
    Fatuzzo, Marco
    Affiliation
    The University of Arizona
    Issue Date
    2016-01-11
    
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    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    The epoch of reionization in the R h =  ct universe 2016, 456 (4):3422 Monthly Notices of the Royal Astronomical Society
    Journal
    Monthly Notices of the Royal Astronomical Society
    Rights
    © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    The measured properties of the epoch of reionization (EoR) show that reionization probably began around $z\sim 12-15$ and ended by $z=6$. In addition, a careful analysis of the fluctuations in the cosmic microwave background indicate a scattering optical depth $\tau\sim 0.066\pm0.012$ through the EoR. In the context of $\Lambda$CDM, galaxies at intermediate redshifts and dwarf galaxies at higher redshifts now appear to be the principal sources of UV ionizing radiation, but only for an inferred (ionizing) escape fraction $f_{ion}\sim 0.2$, which is in tension with other observations that suggest a value as small as $\sim 0.05$. In this paper, we examine how reionization might have progressed in the alternative Friedmann-Robertson Walker cosmology known as the $R_{\rm h}=ct$ Universe, and determine the value of $f_{ion}$ required with this different rate of expansion. We find that $R_{\rm h}=ct$ accounts quite well for the currently known properties of the EoR, as long as its fractional baryon density falls within the reasonable range $0.026\lesssim \Omega_b\lesssim 0.037$. This model can also fit the EoR data with $f_{ion}\sim 0.05$, but only if the Lyman continuum photon production is highly efficient and $\Omega_b \sim 0.037$. These results are still preliminary, however, given their reliance on a particular form of the star-formation rate density, which is still uncertain at very high redshifts. It will also be helpful to reconsider the EoR in $R_{\rm h}=ct$ when complete structure formation models become available.
    ISSN
    0035-8711
    1365-2966
    DOI
    10.1093/mnras/stv2902
    Version
    Final accepted manuscript
    Additional Links
    http://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stv2902
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stv2902
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