archive-edu.com » EDU » U » UCHICAGO.EDU

Total: 278

Choose link from "Titles, links and description words view":

Or switch to "Titles and links view".
  • Animations
    Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Power Spectra Baryons Matter Curvature DarkEnergy Reionization Tensors Damping Tail Baryon Fraction EB Polarization nbsp nbsp Scalar nbsp nbsp

    Original URL path: http://background.uchicago.edu/~whu/animbut/anim4.html (2015-06-26)
    Open archived version from archive


  • Animations
    PhD Thesis 95 Baryon Acoustic Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Power Spectra Baryons Matter Curvature DarkEnergy Reionization Tensors Damping Tail Baryon Fraction EB Polarization

    Original URL path: http://background.uchicago.edu/~whu/animbut/anim5b.html (2015-06-26)
    Open archived version from archive

  • Animations
    Baryon Acoustic Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Power Spectra Baryons Matter Curvature DarkEnergy Reionization Tensors Damping Tail Baryon Fraction EB Polarization nbsp nbsp Scalar nbsp nbsp Vector nbsp nbsp Tensor Polarization Pattern The projection cold red lobe of the quadrupole moment of the temperature anisotropy at last scattering recombination or reionization transverse to the line of site deterines the polarization magnitude and direction Here the effect of a scalar or density perturbation is shown Note the azimuthal symmetry of the pattern EB Modes Polarization patterns can be decomposed into the E and B modes which are polarization analogues of the curl free and divergence free parts of vectors E and B modes have opposite behavior under a parity transform corresponding to the B modes having a polarization direction north west to south east and north east to south west that is 45 degrees from the principal axis for its amplitude variation north south Unlike

    Original URL path: http://background.uchicago.edu/~whu/animbut/anim6.html (2015-06-26)
    Open archived version from archive

  • Animations
    nbsp Polarization Primer 97 nbsp Review 02 nbsp Power Animations nbsp Lensing nbsp Power Prehistory nbsp Legacy Material 96 nbsp PhD Thesis 95 Baryon Acoustic Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP

    Original URL path: http://background.uchicago.edu/~whu/polar/scalaran.html (2015-06-26)
    Open archived version from archive

  • Cosmic Symphony
    Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Cosmic Symphony Wayne Hu and Martin White Scientific American 290N2 44 2004 In the beginning there was light Under the intense

    Original URL path: http://background.uchicago.edu/~whu/symphony.html (2015-06-26)
    Open archived version from archive

  • CMB Introduction
    Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Introduction Acoustic Oscillations Baryonmeter Doppler Effect Driving Effect Damping Projection ISW Effect Power Spectrum Sensitivity Secondary Anisotropy Summary Seing Sound The most prominent and useful features in the anisotropy of the CMB come from acoustic oscillations of the photon baryon fluid Radiation pressure from the photons resists the gravitational compression of the fluid into potential wells and sets up acoustic oscillations in the fluid Figure Radiation Pressure and Gravity Springs represent photon pressure and balls represent the effective mass of the fluid The shorter the wavelength of the potential fluctuation the faster the fluid oscillates such that at last scattering the phase of the oscillation reached scales with the wavelength Since regions of compression maxima represent hot regions and rarefaction minima cold regions there will be a harmonic series of peaks in wavelength associated with the acoustic oscillations It is the features of these peaks that provide us with an

    Original URL path: http://background.uchicago.edu/~whu/physics/acoustic.html (2015-06-26)
    Open archived version from archive

  • CMB Introduction
    Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Introduction Acoustic Oscillations Baryonmeter Doppler Effect Driving Effect Damping Projection ISW Effect Power Spectrum Sensitivity Secondary Anisotropy Summary Baryonmeter Baryons increase the effective mass of the fluid This changes the balance between pressure and gravity in the fluid Gravitational infall now leads to greater compression of the fluid in the potential well Just like a mass on a spring gravity shifts the zero point of the oscillator Figure Baryon Drag This increases the amplitude of the oscillation since the initial conditions now represent a larger displacement from the zero point More importantly it changes the absolute value rms dotted lines of the maxima vs minima of the effective temperature fluctuation Compressions are enhanced over rarefactions of the fluid inside potential wells Thus the relative heights of the peaks present one way of measuring the baryon content of the universe In the scale invariant adiabatic model this is how the anisotropy

    Original URL path: http://background.uchicago.edu/~whu/physics/baryon.html (2015-06-26)
    Open archived version from archive

  • CMB Introduction
    nbsp Power Prehistory nbsp Legacy Material 96 nbsp PhD Thesis 95 Baryon Acoustic Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Introduction Acoustic Oscillations Baryonmeter Doppler Effect Driving Effect Damping Projection ISW Effect Power Spectrum Sensitivity Secondary Anisotropy Summary Doppler Effect Since the turning points of the oscillation are at the extrema the fluid oscillates 90 degrees out of phase with the temperature Its line of sight motion relative to the observer causes a Doppler shift Figure Doppler Effect in red If the baryons are neglected the Doppler oscillations have the same amplitude as the temperature oscillations However as we have seen baryons increase both the amplitude of the oscillation and the rms magnitude of the compressional peaks strongly Furthermore by conservation of energy as the effective mass of the oscillator goes up the velocity goes down as the square root of the mass Together these factors imply that in the real universe which has a significant

    Original URL path: http://background.uchicago.edu/~whu/physics/doppler.html (2015-06-26)
    Open archived version from archive



  •