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CMBFAST:

A Microwave Anisotropy Code. Last updated 12/02/03.
NEW  List of CMBFAST parameters

W e l c o m e to the CMBFAST Website!

This is the most extensively used code for computing cosmic microwave background anisotropy, polarization and matter power spectra. The code has been tested over a wide range of cosmological parameters. We are continuously testing and updating the code based on suggestions from the cosmological community. Do not hesitate to contact us if you have any questions or suggestions.

U. Seljak & M. Zaldarriaga


*  Current Version 4.5.1 More details on the differences with previous versions can be found in the documentation section . This version differs only slightly from 4.4, several improvements related to quintessece were made. The main features of 4.2 , 4.3, 4.4 and 4.5 are:

The CMBFAST package is available as a compressed tar file. You can download a subroutine to calculate the spin harmonics needed in for the analysis of CMB polarization. You can also find:

  • Publications

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  • some on-line documentation.

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    Information about the authors.

  • Uros Seljak

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  • Matias Zaldarriaga

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  • If you are interested in making CMB maps you can use the publically available HEALPIX .
  • The UCSB Physics department CMB curriculum home page . You will find a windows version of CMBFAST among other cool stuff.
  • WMAP team has a web based to run CMBFAST 4.0.
  • If you are interested in fitting models to CMB data check Lloyd Knox's RADPACK .
  • Other CMB websites.

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    Publications

    Papers in postscript (compressed using GNU gzip)

    astro-ph/0306052
             A comparison of cosmological Boltzmann codes: are we ready for precision cosmology?  , U. Seljak, N. Sugiyama, M. White, M.  Zaldarriaga

    astro-ph/0008167
             Towards a refined cosmic concordance model: joint 11-parameter constraints from CMB and large-scale
    structure M. Tegmark, M.  Zaldarriaga, A. J. S. Hamilton. In a section of this paper we discuss the k-splitting method implemented in version 4.0

    astro-ph/9912199   (ApJ Supplements in press)
            CMBFAST for spatially closed universes by M. Zaldarriaga and U. Seljak.
    We extend CMBFAST to closed models.

    Phys.Rev.D:58 023003 (1998)
    Gravitational Lensing effect on Cosmic Microwave Background Polarization by M. Zaldarriaga, U. Seljak.

    We develop the necessary formalism to calculate the gravitational lensing effect on the power spectra.
    Phys.Rev.D:573290-3301,1998
    A Complete Treatment of CMB Anisotropies in a FRW Universe by W. Hu, U. Seljak, M. White, M. Zaldarriaga.

    The total angular momentum method is generalized to non-flat geometries. The equations for tensor and vector modes in non-flat geometries follow inmediately.
    ApJ 494:491-502, 1998
    Integral Solution for the Microwave Background Anisotropies in Non-flat Universes by M. Zaldarriaga, U. Seljak & E. Bertschinger.

    We extend the line of sight approach for solving the photon transport equation to non-flat universes. We also generalize the E &B decomposition of polarization to open models.
    Phys.Rev.Lett.78:2054-2057,1997
    Signature of Gravity Waves in Polarization of the Microwave Background by U. Seljak & M. Zaldarriaga.

    Gravity waves leave a characteristic signature in polarization of the CMB. A particular combination of the Stokes parameters vanishes for scalar modes, but does not for GW. We investigate how this can be used to constrain the presence of GW in the light of the future CMB experiments.
    Phys.Rev.D:1830-1840,1997
    An All-Sky Analysis of Polarization in the Microwave Background by M. Zaldarriaga & U. Seljak.

    We use spin-weighted spherical harmonics to expand the CMB polarization on the sky. We derive the exact expressions for scalar and tensor power spectra needed to characterize the CMB anisotropy and polarization.
    ApJ 469:437-444,1996
    A line of sight approach to Cosmic Microwave Background anisotropies by U. Seljak & M. Zaldarriaga.

    This is the main reference describing the line of sight integration method. It explains our numerical implementation of the integral solution for CMB temperature anisotropies and polarization.

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