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  • Inflation
    we include the important complication that foreground model parameters we use about 500 must be simultaneously measured from the data as well Our results are quite encouraging despite all these complications precision measurements of most cosmological parameters are degraded by less than a factor of 2 for our main foreground model and by less than a factor of 5 in our most pessimistic scenario Parameters measured though large angle polarization

    Original URL path: http://background.uchicago.edu/~whu/foregpars/foregparspage.html (2015-06-26)
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  • Inflation
    with constant comoving curvature are brought into a unified treatment The resulting formalism generalizes and simplifies the calculation of anisotropies and in its integral form allows for a fast calculation of model predictions in linear theory for any FRW metric With this work the perturbation theory of CMB temperature and polarization anisotropy formation through gravitational instability in an FRW universe may be considered complete Pages The Web pages devoted to

    Original URL path: http://background.uchicago.edu/~whu/otamm/otammpage.html (2015-06-26)
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  • Polarization
    in turn correspond directly to the fundamental scalar compressional vector vortical and tensor gravitational wave modes of cosmological perturbations We explain the origin and phenomenology of the geometric distinction between these patterns in terms of the so called electric and magnetic parity modes as well as their correlation with the temperature pattern By its isolation of the last scattering surface and the various perturbation modes the polarization provides unique information

    Original URL path: http://background.uchicago.edu/~whu/polar/polarpage.html (2015-06-26)
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  • Acoustic
    employ these techniques to study the general properties of anisotropy generation from scalar vector and tensor perturbations to the metric and the matter both in the cosmological fluids and from any seed perturbations e g defects that may be present The simpler more transparent form and derivation of the Boltzmann equations brings out the geometric and model independent aspects of temperature and polarization anisotropy formation Large angle polarization provides a robust means to distinguish between isocurvature and adiabatic models for structure formation in principle Vector modes have the unique property that the CMB polarization is dominated by magnetic type parity at small angles and hence potentially distinguishable independent of the model for the seed The tensor modes produce a different sign from the scalars and vectors for the temperature polarization correlations at large angles We explore conditions under which one perturbation type may dominate over the others including a detailed treatment of the photon baryon fluid before recombination Pages The Web pages devoted to this work Full HTML Version are part of the advanced CMB theory tutorial Readers from this series should refer to concepts developed in Anisotropy Review Polarization Review The next set in this series is A Complete

    Original URL path: http://background.uchicago.edu/~whu/tamm/tammpage.html (2015-06-26)
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  • Damping Tail
    cosmological model from small scale CMB anisotropy data We accurately calibrate the model independent effects of diffusion and reionization damping which provide potentially the most robust information on the background cosmology Removing these effects we uncover model dependent processes such as the acoustic peak modulation and gravitational enhancement that can help distinguish between alternate models of structure formation and provide windows into the evolution of fluctuations at various stages in

    Original URL path: http://background.uchicago.edu/~whu/damp/damppage.html (2015-06-26)
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  • Acoustic
    for the causal structure of the early universe A generic pattern for isocurvature initial conditions arises due to backreaction effects but is not robust to exotic source behavior inside the horizon If present the acoustic pattern contains unambiguous information on the curvature of the universe even in the general case By classifying the behavior of the unknown source we determine the minimal observations necessary for robust constraints on the curvature

    Original URL path: http://background.uchicago.edu/~whu/acoustic/acousticpage.html (2015-06-26)
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  • Small
    at last scattering and of the baryons at the end of the Compton drag epoch freezes the diffusion damped acoustic oscillations into the CMB and matter power spectra at different scales We determine the dependence of the respective acoustic amplitudes and damping lengths on fundamental cosmological parameters The baryonic oscillations enhanced by the velocity overshoot effect compete with CDM fluctuations in the present matter power spectrum We present new exact

    Original URL path: http://background.uchicago.edu/~whu/small/smallpage.html (2015-06-26)
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  • Concepts
    discuss gauge choice and gauge invariance and their use in understanding the CMB Acoustic gravitational redshift and ionization effects have robust signatures in the CMB spectrum and may allow determination of classical cosmological parameters as well as reveal general distinctions between models for structure formation We develop the tight and weak coupling approximations as analytic tools to help understand these effects and the robustness of their signatures Files Revised Postscript

    Original URL path: http://background.uchicago.edu/~whu/concepts/conceptspage.html (2015-06-26)
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