# Nonlinear Density Fluctuation Field Theory for Large Scale Structure

Abstract

We develop the effective field theory of density fluctuations for a Newtonian self-gravitating -body system in quasi-equilibrium, apply it to a homogeneous universe with small density fluctuations. Keeping the density fluctuation up to the second order, we obtain the nonlinear field equation of the 2-pt correlation , which contains the 3-pt correlation and formal ultra-violet divergences. By the Groth-Peebles hierarchical ansatz and the mass renormalization, the equation becomes closed with two new terms beyond the Gaussian approximation, and their coefficients are taken as parameters. The analytic solution is obtained in terms of the hypergeometric functions, which is checked numerically. With one single set of fixed two parameters, the correlation and the corresponding power spectrum match simultaneously the results from all the major surveys, such as APM, SDSS, 2dfGRS, and REFLEX. The model gives a unifying understanding of several seemingly unrelated features of large scale structure from a field-theoretical perspective. The theory is worthy to be extended to study the evolution effects in an expanding universe.

PACS numbers:

Keywords: cosmology, large-scale structure, galaxies, clusters, gravitation, hydrodynamics, instabilities

## 1 Introduction

Great progress has been made in understanding the the large scale structure of the universe in past decades. Not only observations of the major galaxy surveys such as SDSS [36, 42, 43], 2dF [6, 22, 26, 29], APM [25, 27], and REFLEX [7, 31] etc, have revealed the cosmic structures of increasingly large sky dimension with new detailed features being found, theoretical studies have also achieved important results, through numerical simulations [39, 34], perturbation method [28, 9, 15, 18, 3, 38], and thermodynamics [30]. From view point of dynamics, the Universe filled with galaxies and clusters is a many-body self-gravitating system in an asymptotic relaxed state, since the cosmic time scale is longer than the local crossing time scale [30]. A systematic approach to statistical mechanics of many-body systems is to convert the degrees of freedom of discrete particles into a continuous field. Thereby, the fully-fledged techniques of field theory can apply to study the systems [47]. The Landau-Ginzburg theory is a known example in this regard. We have formulated such a density field theory of self-gravitating systems and applied it to the large scales structure of the Universe [44]. Under the Gaussian approximation, the field equation of the 2-point correlation function and the solution have been derived explicitly. The result qualitatively interprets some observational features, but it suffers from insufficient clustering on small scales. In this paper, we will go beyond the Gaussian level and include nonlinear terms of density fluctuations up to the second order, yielding a more satisfying description of the large scale structure.

## 2 Nonlinear Field Equation of Correlation Function

The universe is represented by a collection either of galaxies, or of clusters, including their respective dark halos, as the unit cells with random velocities. Although the unit cell, galaxy or cluster, has different mass , both cases correspond to the same mass density . We study the asymptotic relaxed state of this Newtonian self-gravitating system of points of mass with the Hamiltonian . Thus the evolution effects will not be addressed in this paper. By using the Hubbard-Stratonovich transformation [47], the grand partition function of this system at temperature can be cast into the generating functional as a path integral , where is the gravitational field, of dimension , the sound speed, the effective Lagrangian is , and is the Jeans wavenumber. The term has a minus sign because gravity is attractive. By the Poisson’s equation the mass density is related to the field by . So is the constant mass density when . We define a dimensionless re-scaled mass density field and introduce an external source coupling with in the effective Lagrangian [44]

(1) |

is used to handle the functional derivatives with ease. So far is the only parameter in place of temperature , upon which and depend. The field equation of in the presence of is

(2) |

The -point connected correlation function is given by , where is the fluctuation field about the expectation value , and . A standard way to derive the field equation of is to take functional derivative of the expectation value of Eq.(2) w.r.t. the source , and then set [16, 44]. Assuming the large-scale homogeneity of the Universe with a constant background density , and keeping up to the second order of small fluctuation

(3) |

we obtain the field equation of the 2-pt correlation function

(4) | |||||

where has been used. Eq.(4) is not closed, as it involves the 3-pt correlation function . If higher order terms in were allowed in Eq.(3), there would be , etc, in Eq.(4). Therefore, we have a hierarchy of field equations, typical for the kinetic equation of a generic many-body systems. To close Eq.(4), we adopt the Groth-Peebles hierarchical ansatz [20]

(5) |

where the constant ([15, 11, 23, 24]). Then, Eq.(4) becomes closed:

(6) | |||||

where , , and

(7) |

Due to the higher order terms in Eq.(3), the friction term and the nonlinear term occur in Eq.(6). As is expected for an interacting field theory, is modified by an apparently divergent term . We take as the physical wavenumber like in the standard mass renormalization [47]. Eq.(6) is a nonlinear elliptic equation with a point source . Since , so galaxies or clusters with greater mass have a higher correlation amplitude. This naturally explains why the correlations of clusters or of galaxies increase with richness and luminosity [44]. As mentioned earlier, galaxies and clusters are treated on equal footing as gravitating particles differing only by their masses, their correlation functions have the same functional form, differing only in the amplitude . This is the observed facts [21, 2]. By isotropy of the Universe, one puts , then Eq.(6) reduces to

(8) |

where , , and . Both and are treated as two parameters.

## 3 Analytic and Numerical Solution

The Gaussian approximation [5, 44] is recovered by setting and in Eq.(6), i.e. keeping only the term in Eq.(3). The solution is with and , and the power spectrum , where is the spatial number density. This result qualitatively explains several observed features, such as a stronger correlation for more massive galaxies, galaxies with a smaller having a higher [10, 14], the scaling of “correlation length” with the mean cluster separation as [1, 2, 8, 17, 41], and damped oscillations of for clusters with a wave-length hMpc [4, 12, 13, 14, 37, 35]. Here one sees the physical meaning of the sound speed . Using the background mass density leads to . Taking the observed periodic length Mpc and by WMAP [32, 33], yields km/s, which is roughly that of peculiar velocity of clusters or galaxies. Thus, viewing as the random velocity of clusters or galaxies is qualitatively consistent with the observations of the periodicity in , of , and of . The shortcomings of the Gaussian solution are that is too low at small scales, and that has a sharp peak at and becomes negative for [44].

Now these problems are overcome by the nonlinear Eq.(8), whose solution is determined by the boundary condition

(9) |

at some . Note that, in fitting with observational data, the amplitude is higher for clusters than for galaxies, as clarified earlier, and the slope is roughly equal for clusters and for galaxies. The range of parameters are taken , , h Mpc. In computation we take hMpc. Eq.(8) is easily solved numerically. In fact, it has an analytic solution as follows. By perturbation method, since , one sets the solution as a series . Eq.(8) becomes and , where for . The solution for is a linear combination of ([19])

(10) |

where and are the degenerate hypergeometric functions, , and . The solution of is a linear combination of Eq.(10) plus a particular solution

(11) |

where is the Wronskian. The condition in Eq.(9) is satisfied by choosing , , and for . As is checked, up to the order , this analytic solution agrees with the numerical one. Once is known, the power spectrum follows from Fourier transform . For galaxies from APM, 2dFGRAS and SDSS, the calculated and are shown in FIG.1, and in FIG.2, respectively. For REFLEX X-ray clusters the calculated and are given in FIG.3 and FIG.4, respectively. For SDSS clusters, is given in FIG.5. It is seen that, for the fixed parameters , and h Mpc, the calculated , , and their respective match very well all the major surveys for both galaxies and clusters, simultaneously. Thus, our density field theory gives a decent description of the observational data.

## 4 Discussion and Conclusion

Overall, the solution of Eq.(8) improves the Gaussian one considerably, as shown FIG.6, in which the 2dFGRS active galaxies are taken for demonstration purpose. It is found that the nonlinear term has the effects of strongly enhancing on small scales, and making flatter in . The friction term has the following effects: slightly increasing the height of on small scales; moving the zeros of to larger ; strongly damping the amplitude of oscillations of on large scales [4, 37, 12, 13, 14, 35], as seen in FIG.7; smoothing out the sharp peak of at and turning positive for .

The main conclusion of this paper is the following. The universe containing galaxies or clusters is viewed as a many-particle system in asymptotic relaxed state and can be described by an effective density field, whereby the techniques of field theory applies, yielding a perspective on the large scale structure of the universe other than the conventional methods. There appears the Jeans scale hMpc, which is the unique scale underlying the large scale structure as a gravitational system. Up to nonlinear terms beyond the Gaussian approximation, the nonlinear field equation of the 2-pt correlation function of the density fluctuations has been derived and solved analytically. This analytic result of field theory interprets several observed features of large scale structures. With fixed values of the parameters , the solution matches the observed and of both galaxies and of clusters, simultaneously.

Although our results match the observational data on large scales very well, our model is still preliminary at the present stage, there are several problems that need to be further addressed in the future as in the following.

Firstly the calculated for galaxies increases too fast on very small scales Mpc. This indicates that the model may break down on such small scales close to a galaxy size. This may suggest that either higher order terms of perturbations should be taken into account, or the effects of galaxy formation and local virilization need to be included.

Next, there is a limitation in applying the Groth-Peebles ansatz in Eq.(2). As is known, for descriptions of any many-particle dynamic system based on Gibbs-Boltzmann equation, a procedure is usually taken, which decomposes the complicated equation into a set of differential equations, so that each one in the set is possibly manageable. However, thereby, a hierarchy of BBKGY type, or the like, is inevitably arises. Different treatments of the hierarchy are employed for different systems, and a cut-off of the hierarchy is usually is used. For instance, in the case of the photon gas of CMB, the multipole decomposition is involved for the temperature anisotropies and polarization, and the common practice is to cut off the hierarchy of multipoles by letting higher multipole components to zero, yielding a very accurate description of CMB spectra [46, 45, 40]). But for the calculation of in our context, one can not set to zero, since these are important and give rise to nonlinear effects, due to the long range nature of gravity force. The Groth-Peebles ansatz has been used in our analytic treatment, because it is a simple one and an analytic solution can be derived. We would like to mention that the ansatz only approximately reflects the actual distribution since the forms of factor, , is in fact a function of . In this case Eq.(6) for would be more complicated and analytic solutions for the general case would be difficult to derive explicitly.

Thirdly, in fitting the observation of galaxies, we have not separated the dark matter from galaxies in our present model. Therefore, no bias is introduced and the baryon acoustic oscillations are not incorporated in our model. A comprehensive treatment of two components, dark matter and baryons, in our theory would require substantial extensions to the model discussed the present paper.

Finally, it should be mentioned that our theoretical model deals with only the quasi-relaxed state of the large scale structure of the universe, which, as an assumption, is qualitatively good approximation since the overall expansion rate is smaller than the particle collision rate. It would be much desired to have an extension of the present model to take into account of an evolutionary description. These issues will to be addressed in our further studies.

ACKNOWLEDGMENT: Y. Zhang’s research work was supported by the CNSF No.10773009, SRFDP, and CAS.

## References

- [1] Bahcall N.A., 1996 in “Unsolved Problems in Astrophysics”, edited by J.P.Bahcall and J.P.Ostriker, Princeton University Press, New Jersey
- [2] Bahcall N.A., et al., 2003, ApJ, 599, 814
- [3] Bernardeau F., Colombi S., Gonzanaga E., and Sccoccimarro R., 2002, Phys. Rep. 367, 1
- [4] Broadhurst T.J., et al, 1990, Nature 343, 726
- [5] Chavanis P.H., 2006, Physica A 361, 550
- [6] Colless M., et al. 2001, MNRAS, 328, 1039
- [7] Collins C.A., et al., 2000, MNRAS, 319, 939
- [8] Croft R., et al., 1997, MNRAS, 291, 305
- [9] Davis M. and Peebles P.J.E., 1983, ApJ, 267, 465
- [10] Davis M. and Geller M.J., 1976 ApJ, 208, 13
- [11] Efstathiou G. and Jedrzejewski R.I., 1984 Adv.Space.Res. 3, 397
- [12] Einasto J., et al., 1997, Nature, 385, 139
- [13] Einasto J., et al., 1997, MNRAS, 289, 801
- [14] Einasto M., et. al., 2002, AJ, 123, 51
- [15] Fry J.N., 1984, ApJ, 277, L5
- [16] Goldenfeld N., 1992, Lectures on Phase Transitions and the Renormalization Group, Addison-Wesley
- [17] Gonzalez A. , et al., 2002, ApJ, 571, 129
- [18] Goroff M.H., Grinstein B., Rey S.-J., Wise M.B., 1986, ApJ, 311, 6.
- [19] Gradshteyn I.S. and Ryzhik I.M., 1980, Tables of Integrals, Series, and Products, Academic Press
- [20] Groth E.J. and Peebles P.J.E. , 1977, ApJ, 217, 385
- [21] Guzzo L., et al., 2000, A&A, 355, 1
- [22] Hawkins E., et al, 2003, MNRAS,, 346, 78
- [23] Jing Y.P. and Borner G., 1998, ApJ, 503, 37
- [24] Jing Y.P. and Borner G., 2004, ApJ, 607, 104
- [25] Maddox S.J., Efstathiou G, Sutherland W.J., 1996, MNRAS,, 238, 1227
- [26] Madgwick D.S., et al., 2003, MNRAS,, 344, 847
- [27] Padilla N.D and Baugh C.M., 2003, MNRAS,, 343, 796
- [28] Peebles P.J.E., 1980, The Large Scale Structure of the Universe, Princeton Univ. Press, New Jersey
- [29] Percival W.J., 2005, MNRAS,, 356, 1168
- [30] Saslaw W.C., 2000, The Distribution of Galaxies, Cambridge University Press, Cambridge
- [31] Schueker P., et al, 2001, A&A, 368, 86
- [32] Spergel D.N., et al., 2003, ApJS, 148, 175;
- [33] Spergel D.N. , et al., 2007, ApJS, 170, 377
- [34] Springel S., et al, 2005, Nature, 435, 629
- [35] Tago E., et al., 2002, AJ, 123, 37
- [36] Tegmark M., et al., 2004, ApJ, 606, 702
- [37] Tucker D.L., et al., 1997, MNRAS,, 285, L5
- [38] Valageas P., 2004, A&A, 421, 23
- [39] White S.D.M. & Frenk C.S., 1991, ApJ, 379, 52
- [40] Xia T.Y. and Zhang Y., 2008, Phys.Rev.D78, 123005
- [41] Zandivarez A., et al., 2003, MNRAS,, 344, 247
- [42] Zehavi I., et al., 2002, ApJ, 571, 172;
- [43] Zehavi I. , et al, 2005, ApJ, 630, 1
- [44] Zhang Y., 2007, A&A, 464, 811
- [45] Zhang Y., et al., 2008, Int.JMPD Vol 17, 1105
- [46] Zhao W. and Zhang Y., 2006, Phys.Rev.D74, 083006
- [47] Zinn-Justin J., 1996, Quatum Field Theory and Critical Phenomena, Oxford University Press, Oxford