Week 5: More on Structure Formation

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چکیده

In CDM models, the power spectrum determines everything about structure in the Universe. In particular, it leads to what people refer to as “bottom-up” and/or “hierarchical clustering.” To begin, note that the power spectrum P (k), which decreases at large k (small wavelength) is psychologically inferior to the scaled power spectrum ∆2(k) = (1/2π2)k3P (k). This latter quantity is monotonically increasing with k, or with smaller wavelength, and thus represents what is going on physically a bit more intuitively. Equivalently, the variance σ2(M) of the mass distribution on scales of mean mass M is a monotonically decreasing function of M ; the variance in the mass distribution is largest at the smallest scales and smallest at the largest scales. Either way, the density-perturbation amplitude is larger at smaller scales. It is therefore smaller structures that go nonlinear and undergo gravitational collapse earliest in the Universe. With time, larger and larger structures undergo gravitational collapse. Thus, the first objects to undergo gravitational collapse after recombination are probably globular-cluster–sized halos (although the halos won’t produce stars. As we will see in Week 8, the first dark-matter halos to undergo gravitational collapse and produce stars are probably ∼ 106 M⊙ halos at redshifts z ∼ 20. A typical L∗ galaxy probably forms at redshifts z ∼ 1, and at the current epoch, it is galaxy groups or poor clusters that are the largest mass scales currently undergoing gravitational collapse.

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تاریخ انتشار 2008