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  • CMB Introduction
    448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Introduction Basic Principles Expansion Cosmic Light History Inflation Mapping Anisotropy Sound Waves Music Curvature Summary Gravitational Instability Key Concepts Wrinkles represent hills and valleys Matter falls into and accumulates in valleys Dense objects such as galaxies form in the valleys If we have small wrinkles or hills and valleys early on in the universe matter will tend

    Original URL path: http://background.uchicago.edu/~whu/beginners/instability.html (2015-06-26)
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  • Gauge
    expansion Now let us choose a surface that is temporally warped from the cosmic frame tilde frame On this surface the background evolution of the density looks like a plane wave density perturbation Thus the numerical values of what we call a density perturbation change even though the physical situation does not So long as the coordinate system is fully specified there is no problem in choosing whatever system we

    Original URL path: http://background.uchicago.edu/~whu/physics/aux/gauge.html (2015-06-26)
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  • get scalar variables which are required for TFfit However if you give this vector inputs you ll get vector output which allows you to look at how the various scalar quantities depend on cosmological parameters set omhh 1 set obhh omhh 2 set f baryon 2 if 3 set theta cmb 3 2 7 else set theta cmb 2 728 2 7 set z equality 25000 omhh theta cmb 4 Really 1 z set k equality 0 0746 omhh theta cmb 2 set z drag b1 0 313 omhh 0 419 1 0 607 omhh 0 674 set z drag b2 0 238 omhh 0 223 set z drag 1291 omhh 0 251 1 0 659 omhh 0 828 1 z drag b1 obhh z drag b2 set R drag 31 5 obhh theta cmb 4 1000 1 z drag set R equality 31 5 obhh theta cmb 4 1000 z equality set sound horizon 2 3 k equality sqrt 6 R equality ln sqrt 1 R drag sqrt R drag R equality 1 sqrt R equality set k silk 1 6 obhh 0 52 omhh 0 73 1 10 4 omhh 0 95 set alpha c a1 46 9 omhh 0 670 1 32 1 omhh 0 532 set alpha c a2 12 0 omhh 0 424 1 45 0 omhh 0 582 set alpha c alpha c a1 f baryon alpha c a2 f baryon 3 set beta c b1 0 944 1 458 omhh 0 708 set beta c b2 0 395 omhh 0 0266 set beta c 1 0 1 beta c b1 1 f baryon beta c b2 1 set yy z equality 1 z drag set alpha b G yy 6 sqrt 1 yy 2 3 yy ln sqrt 1 yy 1 sqrt 1 yy 1 set alpha b 2 07 k equality sound horizon 1 R drag 0 75 alpha b G set beta node 8 41 omhh 0 435 set beta b 0 5 f baryon 3 2 f baryon sqrt 17 2 omhh 2 1 set k peak 2 5 3 14159 1 0 217 omhh sound horizon set sound horizon fit 44 5 ln 9 83 omhh sqrt 1 10 0 obhh 0 75 set alpha gamma 1 0 328 ln 431 0 omhh f baryon 0 38 ln 22 3 omhh f baryon 2 Remove some intermediate variables undelete them if you want to see them delete z drag b1 delete z drag b2 delete alpha c a1 delete alpha c a2 delete beta c b1 delete beta c b2 delete alpha b G delete yy macro TFtransfer function 1 Finding the value of various transfer functions at the given vector of wavenumbers k 1 It is assumed that TFset parameters has been called with the appropriate cosmological information Input 1 The given wavevectors in units of Mpc 1 Output Five different transfer functions are output in global variables tf full The full fitting formula eq 16 for the

    Original URL path: http://background.uchicago.edu/~whu/transfer/tf_fit.sm (2015-06-26)
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  • Animation
    01 nbsp Cosmic Symphony 04 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

    Original URL path: http://background.uchicago.edu/~whu/transfer/poweran4.html (2015-06-26)
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  • Animation
    nbsp Cosmic Symphony 04 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

    Original URL path: http://background.uchicago.edu/~whu/transfer/poweran5.html (2015-06-26)
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  • assumed to be 2 728 set kk 1 2 We ll use Mpc 1 below set hubble 2 set omega matter 3 set omega baryon 4 set omega hdm 5 set omega lambda 6 set redshift 7 set degen hdm 8 The numbered inputs are not used below only the above names are Set the temperature of the CMB set theta cmb 2 728 2 7 This routine would crash if baryons or neutrinos were zero so don t allow set omega baryon omega baryon 0 0 0001 omega baryon set omega hdm omega hdm 0 0 0001 omega hdm set omega curv 1 omega matter omega lambda set omhh omega matter hubble 2 set obhh omega baryon hubble 2 set onhh omega hdm hubble 2 set f baryon omega baryon omega matter set f hdm omega hdm omega matter set f cdm 1 f baryon f hdm set f cb f cdm f baryon set f bnu f baryon f hdm Compute the equality scale set z equality 25000 omhh theta cmb 4 Actually 1 z eq set yy z equality 1 redshift set k equality 0 0746 omhh theta cmb 2 set qq kk omhh theta cmb 2 Compute the drag epoch and sound horizon set z drag b1 0 313 omhh 0 419 1 0 607 omhh 0 674 set z drag b2 0 238 omhh 0 223 set z drag 1291 omhh 0 251 1 0 659 omhh 0 828 1 z drag b1 obhh z drag b2 set y drag z equality 1 z drag set sound horizon fit 44 5 ln 9 83 omhh sqrt 1 10 obhh 0 75 Compute the free streaming infall growth functions set p c 0 25 5 sqrt 1 24 f cdm set p cb 0 25 5 sqrt 1 24 f cb set y freestream 17 2 f hdm 1 0 488 f hdm 7 6 degen hdm qq f hdm 2 set omega denom omega lambda 1 redshift 2 omega curv omega matter 1 redshift set omega lambda z omega lambda omega denom set omega matter z omega matter 1 redshift 3 omega denom set growth k0 yy 2 5 omega matter z omega matter z 4 7 omega lambda z 1 omega matter z 2 1 omega lambda z 70 set growth to z0 yy 2 5 omega matter omega matter 4 7 omega lambda 1 omega matter 2 1 omega lambda 70 set growth to z0 growth k0 growth to z0 set growth cb 1 growth k0 1 y freestream 0 7 p cb 0 7 growth k0 1 p cb set growth cbnu f cb 0 7 p cb growth k0 1 y freestream 0 7 p cb 0 7 growth k0 1 p cb Compute the master function set alpha nu part1 f cdm f cb 5 2 p c p cb 5 4 p cb 1 y drag p cb p c set alpha nu part2 1 0 553 f bnu

    Original URL path: http://background.uchicago.edu/~whu/transfer/tfmdm_fit.sm (2015-06-26)
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  • Animation
    04 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

    Original URL path: http://background.uchicago.edu/~whu/transfer/poweran1.html (2015-06-26)
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  • Animation
    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 Thunch astro ph

    Original URL path: http://background.uchicago.edu/~whu/transfer/poweran2.html (2015-06-26)
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