The structure of Doppler peaks induced by active perturbations

Details The structure of Doppler peaks induced by active perturbations The structure of Doppler peaks induced by active perturbations

1996-05-10

arxiv.org/abs/astro-ph/9605047v1

Phys.Rev.D54:3727-3744,1996

Astronomy and Astrophysics

Astrophysics

uuencoded file with tex file and figures, using epsf, a4wide

Scientific paper

10.1103/PhysRevD.54.3727

We investigate how the qualitative structure of Doppler peaks in the angular power spectrum of the cosmic microwave anisotropy is affected by basic assumptions going into theories of structure formation. We define the concepts of ``coherent'' and ``incoherent'' fluctuations, and also of ``active'' and ``passive'' fluctuations. In these terms inflationary fluctuations are passive and coherent while topological defects are active incoherent fluctuations. Causality and scale invariance are shown to have different implementations in theories differing in the above senses. We then extend the formalism of Hu and Sugiyama to treat models with cosmic defects. Using this formalism we show that the existence or absence of secondary Doppler peaks and the rough placing of the primary peak are very sensitive to the fundamental properties defined. We claim therefore that even a rough measurement of the angular power spectrum $C_l$ shape at $100

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