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and Cosmology

Extragalactic Astronomy and Cosmology: An Introduction

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8.6 Angular Fluctuations of the Cosmic Microwave Background<br />

considering the fact that two directions which are separated<br />

by more than ∼ 1 ◦ have a spatial separation at<br />

recombination which is larger than the horizon size<br />

at that time – so spacetime curvature explicitly plays<br />

a role. Fortunately, the physical phenomena that need<br />

to be accounted for are (nearly) all of a linear nature.<br />

This means that, although the corresponding system<br />

of coupled equations is complicated, it can nevertheless<br />

easily be solved, since the solution of a system of<br />

linear equations is not a difficult mathematical problem.<br />

Generally accessible software packages exist (i.e.,<br />

CMBFAST), which compute the power spectrum C l for<br />

any combination of cosmological parameters.<br />

8.6.3 The Fluctuation Spectrum<br />

Horizon Scale. To explain the basic features of CMB<br />

fluctuations, we first point out that a characteristic<br />

length-scale exists at z rec , namely the horizon length.<br />

It is specified by (4.71). For cosmological models with<br />

Ω Λ = 0, the horizon spans an angle of – see (4.72) –<br />

θ H,rec ≈ 1.8 ◦ √ Ω m .<br />

This angle is modified for models with a cosmological<br />

constant; if the Universe is flat (Ω m + Ω Λ = 1), one<br />

finds<br />

θ H,rec ≈ 1.8 ◦ , (8.24)<br />

with a very weak dependence on the matter density,<br />

about ∝ Ωm<br />

−0.1 . As we will demonstrate in the following,<br />

this angular scale of the horizon is directly observable.<br />

Fluctuations on Large Scales. On scales ≫ θ H,rec the<br />

Sachs–Wolfe effect dominates, since oscillations in the<br />

baryon–photon fluid can occur only on scales below<br />

the horizon length. For this reason, the CMB angular<br />

spectrum directly reflects the fluctuation spectrum P(k)<br />

of matter. In particular, for a Harrison–Zeldovich<br />

spectrum, P(k) ∝ k one expects that<br />

l(l + 1)C l ≈ const for l ≪ 180◦ ≃ 100 ,<br />

θ H,rec<br />

<strong>and</strong> the amplitude of the fluctuations immediately yields<br />

the amplitude of P(k). This flat behavior of the fluctuation<br />

spectrum for n s = 1 is modified by the integrated<br />

Sachs–Wolfe effect.<br />

Sound Horizon <strong>and</strong> Acoustic Peaks. On angular scales<br />

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