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  • Acoustic
    model As the ionization level between recombination and the present increases primary anisotropies are reduced by diffusion and rescattering For sufficiently high ionization here z i simgt 100 the Doppler effect on the new last scattering surface can regenerate some fluctuations at intermediate scales The Vishniac effect dominates at very small angular scales Due to its second order nature it contributes even if the ionization redshift is low The z

    Original URL path: http://background.uchicago.edu/~whu/concepts/figd.html (2015-06-26)
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  • Chuangtzu
    From the Chuang tzu To divide is to leave something undivided To discriminate between alternatives is to leave something which is neither alternative Chuang tzu Chap 2 trans A C

    Original URL path: http://background.uchicago.edu/~whu/concepts/quote.html (2015-06-26)
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  • Acoustic
    power spectrum Figure 2 Weak coupling approximation for the Lambda ISW effect The analytic approximation based on crest trough cancellation traces the full ISW integral to high accuracy and accounts for the falling ISW spectrum As Omega 0 increases the relative contribution of the ISW effect decreases in comparison to the Sachs Wolfe SW effect arbitrarily normalized to unity Here we have chosen a pure power law P k propto k power spectrum Figure 3 Comparison with numerical integration thick solid lines shows that at large scales where Lambda ISW and Sachs Wolfe SW contributions dominate the anisotropy analytic formulae thick dashed lines adequately describe the total anisotropy At small scales the curves depart from the prediction due to the early ISW effect and acoustic contributions Hu Sugiyama 1995a Here we have chosen a high h 1 0 low Omega 0 0 1 model to minimize these effects Also plotted in thin dotted lines is the analytic prediction for a pure P k propto k power spectrum with the same normalization at large scales Figure 4 Comparison of different approximations for evaluating the Vishniac effect for a standard CDM model Omega 0 1 h 0 5 Omega b 0 05

    Original URL path: http://background.uchicago.edu/~whu/weak/figa.html (2015-06-26)
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  • Chuangtzu
    I give a great leap and fly up but I never get more than ten or twelve yards before I come down fluttering among the weeds and brambles And that s the best kind of flying anyway Where does he

    Original URL path: http://background.uchicago.edu/~whu/weak/quote.html (2015-06-26)
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  • Photos
    CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Travelog 1998 2011 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 prev next Loading Please wait Lost in Transition I Beijing 2011 Lost in Transition II Beijing 2011 Modern Junk Hong Kong 2011 Before the Fall Santa Barbara 2011 Reflections on the Wall Washington DC 2011 Through a Glass Cerler Spain 2011 Platonic Shadows Sanibel Is Fl 2010 Terminal Lucidity New Buffalo MI 2010 Tethys of the Fall Gov Dodge Park WI 2010 Isolation Desolation Val de Boi Spain 2010 Sword and Stone Montblanc Spain 2010 UnCowered Col du Tormelet France 2010 On Edge Monserrat Spain 2010 BraBomb Aspen CO 2010 Nuttle Tuttle Campo Do Jordao Brazil 2009 Paupermache SLAC 2009 Empty Lathe Chicago 2009 Divide by Zero Independence Lake CO 2009 Clean Sweep New Delhi India 2009 Surgical Openings Hua Hin Thailand 2009 Symmetry Breaking the Cycle Agra India 2009 Better Half Missing Strada in Chianti Italy 2009 The Crescent and the Cross Florence Italy 2009 Inscribed Fiesole Italy 2009 Arcade Games Bologna Italy 2009 Basket Cases Los Cabos Mexico 2009 Pickup Lines Los Cabos Mexico 2009 Recession Velocity Santa Barbara CA 2008 With Birds I Share Point Lobos CA 2008 Erosion Trust Point Lobos CA 2008 Falling Apart Munich Germany 2008 Masking Madness Neuschwanstein Germany 2008 Remains of the Day Park City UT 2008 Submerged Memories Olous Crete 2008 Light Crossing Time Ois Santorini 2008 Looking for Someone Paris France 2008 AntiPop Avignon France 2008 Inverse Gabon Transform Paris France 2008 Scar Tissue St Tropez France 2008 Trinity s Gate Orange France 2008 Winter s Retreat Masca Spain 2007 Urserving Teide Mt Spain 2007 Boundary Value Lake Geneva WI 2007 Moodscape Sante Fe NM 2007 After the

    Original URL path: http://background.uchicago.edu/~whu/travelog1.html (2015-06-26)
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  • CMB Introduction
    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 Temperature Maps Earth Monopole Dipole COBE Power Precision Features Thermal History Expansion Plasma Glue Pressure Thermal Acoustic Oscillations Gravity Plane Waves Harmonics Extrema Angular Peaks Spatial Angular Oscillation Freeze Frame Streaming Soundscape First Peak Data Curvature Flatness Dark Energy Summary Second Peak Data Inertia Baryonmeter Power Dark Baryons Summary Higher Peaks Driving Force Power Summary Damping Tail Diffusion Ruler Consistency Summary Parameter Estimation Parameters Degeneracy Polarization What and Why Scattering Projection Power Quadrupoles B modes Gravity Waves Summary Seeing Sound Key Concepts Pattern of sound imprinted in the temperature of CMB Compressed regions hotter Rarefied regions colder Of course we don t actually hear the sound of these acoustic waves What we actually see is the pattern of the sound waves that is imprinted on the temperature of the CMB Compressing a gas heats it up

    Original URL path: http://background.uchicago.edu/~whu/intermediate/seeingsound.html (2015-06-26)
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  • CMB Review
    astro ph CO ADS InSpire Review Home Introduction Observables Cosmological Paradigm Temperature Field Polarization Field Acoustic Peaks Introduction Basics Initial Conditions Gravitational Forcing Baryon Loading Radiation Driving Damping Polarization Integral Approach Parameter Sensitivity Matter Power Spectrum Introduction Physical Description Cosmological Implications Gravitational Secondaries Introduction ISW Effect RS Moving Halo Gravitational Waves Gravitational Lensing Scattering Secondaries Introduction Peak Suppression Large Angle Polarization Doppler Effect Modulated Doppler Effect SZ Effect Non Gaussianity Data Analysis Introduction Mapmaking Bandpower Estimation Parameter Estimation Discussion Discussion Bibliography BEYOND THE PEAKS Once the acoustic peaks in the temperature and polarization power spectra have been scaled the days of splendid isolation of cosmic microwave background theory analysis and experiment will have ended Beyond and beneath the peaks lies a wealth of information about the evolution of structure in the Universe and its origin in the early universe As CMB photons traverse the large scale structure of the Universe on their journey from the recombination epoch they pick up secondary temperature and polarization anisotropies These depend on the intervening dark matter dark energy baryonic gas density and temperature distributions and even the existence of primordial gravity waves so the potential payoff of their detection is enormous The price for this extended reach is the loss of the ability both to make precise predictions due to uncertain and or non linear physics and to make precise measurements due to the cosmic variance of the primary anisotropies and the relatively greater importance of galactic and extragalactic foregrounds We begin in 4 1 with a discussion of the matter power spectrum to set the framework for the discussion of secondary anisotropies Secondaries can be divided into two classes those due to gravitational effects and those induced by scattering off of electrons The former are treated in 4 2 and the latter in

    Original URL path: http://background.uchicago.edu/~whu/araa/node16.html (2015-06-26)
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  • Footnotes
    comoving scale does not vary with time At very early times then the wavelengh is much larger than the horizon inflation the potential energy density associated with the scalar field s driving inflation here Aside from COBE experiments to date

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