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1. INTRODUCTION Manner THE ASTROPHYSICAL JOURNAL, 471:542È570, 1996 November 10 ( 1996. The American Astronomical Society. All rights reserved. Printed in U.S.A. SMALL-SCALE COSMOLOGICAL PERTURBATIONS: AN ANALYTIC APPROACH WAYNE HU1 AND NAOSHI SUGIYAMA2 Received 1995 December 7; accepted 1996 May 16 ABSTRACT Through analytic techniques veriÐed by numerical calculations, we establish general relations between the matter and cosmic microwave background (CMB) power spectra and their dependence on param- eters on small scales. Fluctuations in the CMB, baryons, cold dark matter (CDM), and neutrinos receive a boost at horizon crossing. Baryon drag on the photons causes alternating acoustic peak heights in the CMB and is uncovered in its bare form under the photon di†usion scale. Decoupling of the photons at last scattering and of the baryons at the end of the Compton drag epoch freezes the di†usion-damped acoustic oscillations into the CMB and matter power spectra at di†erent scales. We determine the dependence of the respective acoustic amplitudes and damping lengths on fundamental cosmological parameters. The baryonic oscillations, enhanced by the velocity overshoot e†ect, compete with CDM Ñuctuations in the present matter power spectrum. We present new exact analytic solutions for the cold dark matter Ñuctuations in the presence of a growth-inhibiting radiation and baryon background. Com- bined with the acoustic contributions and baryonic infall into CDM potential wells, this provides a highly accurate analytic form of the small-scale transfer function in the general case. Subject headings: cosmic microwave background È cosmology: theory È dark matter È elementary particles È large-scale structure of universe 1. INTRODUCTION manner. Despite the simplicity of the Ðnal results, the study of small-scale Ñuctuations requires a rather technical expo- Small-scale Ñuctuations in the cosmic microwave back- sition of perturbation theory. For this reason, we divide this ground (CMB) and the matter density provide a unique paper into two components. The main text discusses results opportunity to probe structure formation in the universe. drawn from a series of appendices and illustrates the corre- As CMB anisotropy experiments reach toward smaller and sponding principles in the familiar context of adiabatic cold smaller angles, the region of overlap with large-scale struc- dark matter (CDM), adiabatic baryonic dark matter ture measurements will increase dramatically. Since the (BDM), and isocurvature BDM scenarios for structure CMB and matter power spectra encode information at very formation. di†erent epochs in the formation of structure, comparison We begin in° 2 with a discussion of the central approx- of the two will provide a powerful consistency test for com- imations employed, i.e., the tight coupling limit for the peting scenarios. Unfortunately, the simple relation photons and baryons and the external potential representa- between the two power spectrum at large scales(Sachs & tion for metric Ñuctuations. Details of these methods and Wolfe1967) does not hold at small scales. To establish the the justiÐcation of their use can be found inAppendix A. As general relation, we need to employ a more complete established inAppendix B, all Ñuctuations are given a boost analysis of how gravitational instability a†ects the matter at horizon crossing due to the driving e†ects of gravita- and CMB together. tional infall and dilation. Since the gravitational potential In previous papers (Hu & Sugiyama1995a, 1995b, here- subsequently decays, the driving e†ects disappear well after afterHSa, HSb), we developed a conceptually simple analy- horizon crossing, leaving Ñuctuations to evolve in their tic description of CMB anisotropy formation. The central natural source-free modes. For the photon-baryon system, advance over previous analytic works (e.g., Doroshkevich, these are acoustic oscillations whose zero point is displaced Zeldovich, & Sunyaev1978) involved the inÑuence of gravi- by baryon drag. As described in°° 34, and these oscil- tational potential wells, established by the decoupled lations are frozen into the photon and baryon spectra at last matter, on the acoustic oscillations in the photon-baryon scattering and at the end of the Compton drag epoch, Ñuid. In this paper, we reÐne the analysis for scales much respectively. Since these epochs are not equal, photon di†u- smaller than the horizon at last scattering as is relevant for sion(Silk 1968) sets a di†erent damping scale in the CMB large-scale structure calculations. Furthermore, we extend it and the baryons. This process is described by the acoustic to encompass the photon-baryon back-reaction on the visibility functions introduced in Appendix C. evolution of the cold dark matter and gravitational poten- The baryonic oscillations may be hidden in CDM models tial as well as baryonic decoupling and evolution. This by larger cold dark matter Ñuctuations. These are discussed makes it possible to extract the relation between CMB and in° 5. The baryon and radiation background also sup- matter Ñuctuations established in the early universe. presses CDM growth before the end of the Compton drag Analytic solutions in terms of elementary functions can be epoch.Appendix D treats this source-free evolution of the constructed in the small-scale limit and serve to illuminate CDM component analytically. After the end of the the physical processes involved in a model-independent Compton drag epoch, the CDM Ñuctuations provide potential wells into which the baryons fall. From the com- 1 Institute for Advanced Study, School of Natural Sciences, Princeton, NJ 08540; whu=sns.ias.edu bined analysis of CMB, baryon, and CDM Ñuctuations, we 2 Department of Physics, Kyoto University, Kyoto 606-01, Japan; obtain accurate analytic expressions for matter and photon sugiyama=tap.scphys.kyoto-u.ac.jp transfer functions in the small-scale limit. This improves 542 SMALL-SCALE COSMOLOGICAL PERTURBATIONS 543 greatly upon the Ðtting functions for the matter power spec- settle into the pure logarithmically growing mode in the trum in the literature(Bardeen et al. 1986, hereafter BBKS; radiation-dominated universe. Peacock& Dodds 1994; Sugiyama 1995) in the case of a signiÐcant baryon fraction. Our form is constructed out of 3. PHOTON FLUCTUATIONS Ðts fromAppendix E for parameters that depend on the detailed physics of recombination, i.e., the last scattering 3.1. Driving E†ects epoch, Compton drag epoch, photon damping length, and Before recombination, the photon-baryon system Silk damping length. behaves as a damped, forced oscillator. As discussed in ° 2, the self-gravity of the acoustic oscillations contributes to the 2. ACOUSTIC APPROXIMATION gravitational force on the oscillator at horizon crossing if Previously we developed an analytic description of the photons or baryons contribute signiÐcantly to the acoustic oscillations in the photons and baryons (HSa; density of the universe at that epoch. Even though the HSb).As discussed in more detail in Appendix A, this detailed behavior at horizon crossing in the radiation- approach is based on two simplifying assumptions: that a dominated epoch is complicated by feedback e†ects, the end perturbative expansion in the Compton scattering time result is extremely simple: Ñuctuations experience a boost between photons and electrons can be extended up to proportional to the potential at horizon crossing. As the recombination and that the gravitational potential may be Ðrst compression of the Ñuid is halted by photon pressure, considered as an external Ðeld. Combined, these two simpli- the self-gravitational potential decays. This leaves the oscil- Ðcations imply that photon pressure resists compression by lator in a highly compressed state and enhances the ampli- infall into potential wells and sets up acoustic oscillations in tude of the subsequent oscillation. For adiabatic initial the photon-baryon Ñuid which then damp by photon di†u- conditions, the amplitude of the potential at horizon cross- sion. However, both these approximations would seem to ing is essentially the initial curvature Ñuctuation. For iso- be problematic for small-scale Ñuctuations. Here the optical curvature initial conditions, it is simply related to the initial depth through a wavelength of the Ñuctuation at last scat- entropy perturbations. tering is small, implying weak rather than tight coupling We quantify these statements inAppendix B and calcu- (see, e.g.,Kaiser 1984; Hu & White 1996). This issue is late the exact boost factor (see eqs.[B5]È[B6]). It represents addressed more fully inAppendix C (below eq. [C3]), where an enhancement in temperature Ñuctuations of a factor of 3 it is shown that only acoustic contributions from the tight over its initial value in the adiabatic case or more impor- coupling regime are visible through the last scattering tantly a factor of5/[1 ] (4/15)f ] over the gravitational red- surface, i.e., those from a time slightly earlier than last scat- shift induced large-scale Ñuctuationsl in a scale-invariant tering when the optical depth to Compton scattering was model(Sachs & Wolfe 1967). Here the fraction of the radi- still high. ation energy density contributed by the neutrinos is f \ l On the other hand, the second issue poses a computa- o /(o ] o ) ^ 0.405 for the standard thermal history with tional problem. Inside the horizon in the radiation- threel l masslessc species. Its presence accounts for neutrino dominated epoch, the acoustic oscillations in the anisotropic stress, which
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