Anisotropy of cosmic background radiation from a spherical clustering on large scales

Details Anisotropy of cosmic background radiation from a spherical clustering on large scales Anisotropy of cosmic background radiation from a spherical clustering on large scales

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...408...25f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 408, no. 1, p. 25-32.

Astronomy and Astrophysics

Astrophysics

16

Astronomical Models, Background Radiation, Clusters, Relic Radiation, Universe, Anisotropy, Density Distribution, Frequency Shift, Space Density, Temperature Distribution

Scientific paper

We present an exact frequency shift of a photon passing through a spherically symmetric collapsing in a flat and pressureless universe. This model can be used to study the temperature distortion of cosmic background radiation (CBR) caused by density perturbations lying on the range from last scattering to the vicinity of observer. We found that the signature of the temperature distortion sensitively depends on the density profile and location of the perturbed region. It also is shown that the CBR temperature anisotropy on scales of 5 deg or more would be dominated by large-scale clustering occurring after decoupling, not by the perturbations at the last scattering. Therefore, CBR anisotropies on intermediate and larger angular scales are not only dependent on density and potential structures at the epoch of decoupling and the relevant horizon, but also on the structure formation occurring in the post-decoupling era. If the recent COBE observation on CBR anisotropy at a scale of 10 is caused by such large-scale clustering, the corresponding initial density fluctuation on the comoving spatial scale of 1000/h Mpc is 2.8 x 10 exp -6 and 6.9 x 10 exp -6 for the perturbed regions located on the last scattering surface and at redshift of about 100, respectively. By using the developed mechanism, the CBR dipole anisotropy can also set an effective constraint on the initial density constrast.

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