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Getting Around Cosmic Variance

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Getting Around Cosmic Variance PHYSICAL REVIEW D VOLUME 56, NUMBER 8 15 OCTOBER 1997 Getting around cosmic variance Marc Kamionkowski* Department of Physics, Columbia University, 538 West 120th Street, New York, New York 10027 Abraham Loeb† Astronomy Department, Harvard University, Cambridge, Massachusetts 02138 ~Received 16 May 1997! Cosmic microwave background ~CMB! anisotropies probe the primordial density field at the edge of the observable Universe. There is a limiting precision ~‘‘cosmic variance’’! with which anisotropies can determine the amplitude of primordial mass fluctuations. This arises because the surface of last scatter ~SLS! probes only a finite two-dimensional slice of the Universe. Probing other SLS’s observed from different locations in the Universe would reduce the cosmic variance. In particular, the polarization of CMB photons scattered by the electron gas in a cluster of galaxies provides a measurement of the CMB quadrupole moment seen by the cluster. Therefore, CMB polarization measurements toward many clusters would probe the anisotropy on a variety of SLS’s within the observable Universe, and hence reduce the cosmic-variance uncertainty. @S0556-2821~97!04820-0# PACS number~s!: 98.70.Vc, 98.90.1s One of the primary aims of cosmology is recovery of the Therefore, the fractional precision with which we will be primordial spectrum of density perturbations which produced able to determine this variance in the mass distribution is the large-scale structure in the Universe today. This spectrum O(N21/2). should elucidate whether primordial perturbations were pro- To be more precise, the temperature T(nˆ) as a function of duced by inflation, topological defects, or some alternative direction nˆ5(u,f) on the sky can be expanded in terms of mechanism. Although galaxy surveys probe the current mass spherical harmonics distribution, the primordial spectrum is best probed by the cosmic microwave background ~CMB!. Large-angle CMB ˆ T~n!5( almYlm~u,f!, ~1! anisotropies from the Cosmic Background Explorer ~COBE! lm have already probed the spectrum on large distance scales. with Furthermore, future experiments such as NASA’s Micro- wave Anisotropy Probe ~MAP!@1#and ESA’s Planck Sur- ˆ ˆ * ˆ veyor @2# should recover the primordial spectrum to much alm5E dnT~n!Ylm~n!. ~2! smaller distance scales with unprecedented precision. However, there is a fundamental limit to the precision These multipole coefficients alm are distributed with mean with which the CMB can recover the amplitude of primordial ^alm&50 and variance, fluctuations. Theory predicts that the primordial density field a* a 5C , 3 was a single realization of some random process. To test the ^ l8m8 lm& ldll8dmm8 ~ ! theory, we would want to observe and average over a num- ber of realizations of the random process. However, we have where the angular brackets denote an average over all real- only one Universe to observe, so there will be a sample izations of the random field. The set of expectation values Cl is the angular power spectrum of the CMB, the projection of variance, known as ‘‘cosmic variance’’ in the average we the three-dimensional power spectrum P(k) on the two- construct. dimensional SLS. Roughly speaking, C specifies the vari- A given theory provides the three-dimensional power l ance in the mass distribution on a distance scale pR/l. spectrum P(k) as a function of wave number k. This speci- To measure a given expectation value C , we would con- fies roughly the variance in the mass distribution over a l 21 struct the 2l11 ~for m52l,...,l!alm coefficients from the comoving-distance scale l;k . Now suppose, for ex- sky map. The average of the squares of these, ample, that we want to use CMB anisotropies to determine ˆ l 2 the variance in the mass distribution averaged over spheres Cl5(m52lualmu /(2l11) would provide our best estimate of comoving diameter l. The CMB probes a spherical sur- for Cl . However, this average is over a sample with a finite face of last scatter ~SLS! at the edge of the observable Uni- number (2l11) of independent terms. Therefore, the preci- ˆ verse of comoving radius R, as illustrated in Fig. 1. There sion with which the estimator (Cl) will recover the expecta- 2 are only N;4p(R/l) such volumes probed by our SLS. tion value (Cl) is limited. If the distribution of density per- turbations is Gaussian, the 1s cosmic variance with which Cl 1/2 can be estimated is @2/(2l11)# Cl . Although different *Electronic address: [email protected] cosmological models make different predictions for the Cl’s †Electronic address: [email protected] measured by COBE ~i.e., those for l&15!, cosmic variance 0556-2821/97/56~8!/4511~3!/$10.0056 4511 © 1997 The American Physical Society 4512 MARC KAMIONKOWSKI AND ABRAHAM LOEB 56 these quadrupole moments would allow us to map the pri- mordial three-dimensional density field and thereby reduce the cosmic-variance limit to the amplitude of primordial mass fluctuations when smoothed over a given distance scale. Consider clusters located at the points along the 1xˆ2 line of sight indicated by the heavy dots in Fig. 1. The sphere centered on each cluster is the SLS observed by it. Clearly, the SLS’s of many clusters spread throughout the observable Universe ~through many different lines of sight! would span the entire volume of the observable Universe. The lines per- pendicular to the line of sight to each cluster indicate the plane of the quadrupole anisotropy probed by the polariza- tion of the scattered radiation we observe. The filled squares show the points on each SLS where those quadrupole mo- ments receive their greatest contribution. Although none of these squares lies closer than R/& from us ~and the closest is for a cluster at z53!, the volume accessible to the squares is still (12223/2)'65% of the observable volume. Although Fig. 1 shows hypothetical clusters with z.3, the location of the squares indicates that the accessible volume is equally well probed by a sample of clusters with z&3. In principle, FIG. 1. The x350 slice of the observable Universe in comoving our approach could be applied to other objects, such as ga- coordinates. We are at the origin and the xˆ3 direction is out of the page. The heavy circle is our surface of last scatter ~SLS! located a lactic halos which exist at higher redshifts. comoving distance R from our position at the origin. Clusters at Crudely speaking, each polarization signal measures dif- redshifts z50.5, 3, 10, and 45 are located at the comoving positions ferences in the primordial density at points indicated by the indicated by the heavy dots along the 1xˆ2 line of sight ~assuming a squares in Fig. 1. Therefore, by mapping the polarization of critical-density universe!. The circle centered on each cluster is the clusters throughout the Universe, we can reconstruct the pri- SLS seen by it. The filled squares show the primary plane of the mordial three-dimensional density field through most of the quadrupole moment which polarizes the radiation scattered to us. volume of the observable Universe in much the same way as COBE maps the temperature on the sky from measured tem- restricts our ability to discriminate between these different perature differences. Therefore, polarization measurements models with COBE measurements. of the CMB through a number of distant clusters would al- If we could send observers to numerous distant locations low us to probe a larger volume of the observable Universe in the Universe and have them report back to us on the CMB than that accessible just from our SLS. anisotropies measured at each of these locations, then we The variance in the mass distribution on a comoving- would have additional independent multipole coefficients length scale l can be measured with only N;4p(R/l)2 and therefore be able to overcome the cosmic-variance limit. independent regions of size l on our SLS. However, the Although this is not practical, we can probe the anisotropy volume of the Universe contains roughly (R/l)3 indepen- seen by distant observers. dent regions of size l. Therefore, if we can map the primor- If one looks at the CMB through a cluster of galaxies, a dial density field from cluster polarizations, then the cosmic fraction of the photons have been scattered by the electron variance in the determination of the primordial amplitude of gas in the cluster @giving rise to the Sunyaev-Zel’dovich ~SZ! density fluctuations could be reduced by up to O(Al/R). effect @3##. If the radiation incident on the cluster has a quad- In addition to reducing the cosmic variance to the ampli- rupole anisotropy in the plane normal to the line of sight to tude of primordial inhomogeneities, the measured signals the cluster, the scattered radiation will be linearly polarized could provide information complementary to that obtained @4,5#. Moreover, the polarization vector will be determined from CMB anisotropy experiments. First, the SLS’s for clus- by the amplitude and orientation of the quadrupole anisot- ters at high redshift will be smaller than ours, so their quad- ropy of the incident radiation. By determining the linear po- rupole moments probe smaller scales, comparable to those larization of the CMB through a distant cluster, we are mea- probed by our higher-l moments. Therefore, by observing suring two components of the quadrupole moment of the the redshift dependence of the mean cluster polarization, we cluster’s SLS. obtain an independent measure of the shape of the power The quadrupole moments we probe in this way are those spectrum. Furthermore, if the Universe does not have a criti- measured at earlier times when the Hubble radius is smaller cal density, additional anisotropies will be produced along than the current Hubble radius.
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