# Revisiting the angular momentum growth of protostructures evolved from non-Gaussian initial conditions

###### Abstract

I adopt a formalism previously developed by Catelan and Theuns (CT) in order to estimate the impact of primordial non-Gaussianity on the quasi-linear spin growth of cold dark matter protostructures. A variety of bispectrum shapes are considered, spanning the currently most popular early Universe models for the occurrence of non-Gaussian density fluctuations. In their original work, CT considered several other shapes, and suggested that only for one of those does the impact of non-Gaussianity seem to be perturbatively tractable. For that model, and on galactic scales, the next-to-linear non-Gaussian contribution to the angular momentum variance has an upper limit of with respect to the linear one. I find that all the new models considered in this work can also be seemingly described via perturbation theory. Considering current bounds on for inflationary non-Gaussianity leads to the quasi-linear contribution being of the linear one. This result motivates the systematic study of higher-order non-Gaussian corrections, in order to attain a comprehensive picture of how structure gravitational dynamics descends from the physics of the primordial Universe.

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large-scale structure of the Universe## 1 Introduction

Gravitational instability and hierarchical growth of Cold Dark Matter (CDM) density perturbations provide an elegant description for the acquisition of angular momentum by protostructures. Accordingly, patches of matter are spun up by tidal torques exerted by the surrounding Large-Scale Structure (LSS, see Peebles 1969, 1971; Doroshkevich 1970; White 1984; Heavens & Peacock 1988). At the linear level the spin growth is given by the coupling of the first-order deformation tensor and the inertia tensor of the patch, and it agrees quite well with more accurate numerical results (see the review by Schäfer 2009 and the references therein).

Acquisition of angular momentum beyond the simple linear description has been tackled by means of Lagrangian perturbation theory in a series of papers by Catelan and Theuns (Catelan 1995; Catelan & Theuns 1996a, b, 1997, CT henceforth) almost two decades ago. In particular, they found that the next-to-linear correction to the growth of ensemble-averaged spin is non-vanishing only if primordial density fluctuations are non-Gaussian. CT explored several non-Gaussian models, and concluded that only for one of these does the angular momentum acquisition appear perturbatively tractable: the log-normal model for the gravitational potential of Moscardini et al. (1991). For this template, and adopting a representative mass scale of (with and Gaussian filtering), CT found an upper limit of for the quasi-linear non-Gaussian contribution to the spin variance. This figure translates to a value when rescaled to a smaller and more typical galactic mass of (with and a real-space top-hat filter). For other templates the non-Gaussian contribution is comparable to, or larger than, the linear term, suggesting the impossibility of a perturbative expansion.

Since then, the issue of angular momentum growth in non-Gaussian cosmologies has not been investigated further. On the contrary, new and more general models of primordial non-Gaussianity exist nowadays and, most importantly, constraints on the level of primordial non-Gaussianity coming from the Cosmic Microwave Background (CMB) and the LSS have dramatically improved over the last decade. Given the cosmological relevance of primordial non-Gaussianity (see Bartolo et al. 2004; Chen 2010 for recent reviews) and the significance of the CDM halo angular momentum acquisition for the formation and evolution of galaxies, it is important to update this topic. Specifically, it is interesting to explore the amplitudes and behaviors of the quasi-linear contributions to spin growth given by non-Gaussian models that are popular nowadays. This is the scope of the present letter.

The rest of the manuscript is organized as follows. In Section 2 I review the linear and next-to-linear contributions to the ensemble-averaged spin growth of matter patches. In Section 3 I summarize the non-Gaussian cosmologies explored here. In Section 4 results are displayed and in Section 5 conclusions are drawn. Where needed, I adopted the following cosmological parameters: , , , km s Mpc with , , and .

## 2 Angular momentum acquisition

### 2.1 Lagrangian displacement

In Lagrangian theory the comoving position of a mass element at time can be written in terms of its initial position and a displacement vector field , as

(1) |

Following CT here I used a time variable that is related to the standard cosmic time by (Shandarin, 1980), where is the scale factor.

Perturbative approximations to this exact expression can be found by expanding the displacement field in a series,

(2) |

where corresponds to the Zel’dovich approximation . Here is the growth factor of linear density perturbations, which in a Einstein-de Sitter universe reads . The function is the first order (Zel’dovich) displacement potential (Zel’dovich, 1970), related to the linear density perturbation field by the Poisson equation , so that in Fourier space .

The second-order term of the displacement field can also be separated in time and space, according to . The growth factor reads in an Einstein-de Sitter universe, while for its more general expression I refer to CT. The second-order displacement potential can be related to its first-order counterpart in Fourier space by

(3) | |||||

In the previous Equation is a symmetric integration kernel defined as

(4) |

where is the cosine of the angle between the two wavevectors and .

### 2.2 Spin growth

The angular momentum of the matter initially contained in a comoving Lagrangian patch of the Universe at time can be written as an integral over ,

(5) |

By considering the series expansion of the Lagrangian displacement field introduced in Eq. (2), the angular momentum of the patch can be similarly written as

(6) |

The first-order term of the angular momentum series takes the form

(7) |

By expanding the Zel’dovich potential around the center of mass of the patch (assumed to be, without loss of generality, the origin of the reference frame) up to the second order, the previous equation takes the compact form

(8) |

In the previous equation is the fully antisymmetric Levi-Civita tensor, is the Zel’dovich deformation tensor,

(9) |

while is the inertia tensor of the patch,

(10) |

Summation over repeated indices is implicit.

Likewise, the second-order term in the series expansion of the angular momentum reads

(11) |

which, under a second-order Taylor expansion of the displacement potential takes the form

(12) |

It can be shown that the second-order deformation tensor in Fourier space reads

(13) | |||||

in terms of the Zel’dovich potential.

### 2.3 Ensemble averages

In order to simplify the previous results, it is meaningful to consider the ensemble average of the square of the angular momentum. It then follows that, up to the next-to-linear order,

(14) |

where

(15) |

In the previous Equation is the mean deviation of the matter density field smoothed on a scale corresponding to mass , while and are the first and second invariant of the inertia tensor, respectively. To be more precise, if , , and are the three eigenvalues of the inertia tensor, then and .

The next term is non-vanishing only if density fluctuations are non-Gaussian, and reads

(16) |

where

(17) | |||||

In the previous Equation represents the bispectrum of the Zel’dovich potential, which is now explicitly smoothed on a scale . I assumed the standard real-space top-hat smoothing. The Zel’dovich potential can be related to the standard gravitational potential by making use of the Poisson equation,

(18) |

where is the cold dark matter transfer function (Bardeen et al., 1986; Sugiyama, 1995). The integral in Eq. (17) has to be solved numerically for realistic bispectrum shapes. Fortunately, the bispectrum usually depends only on the magnitude of its three arguments, so that the above six-dimensional integral reduces to a three-dimensional one.

## 3 Non-Gaussian shapes

I considered five different shapes for the primordial bispectrum, that are briefly described below. The first four are motivated by inflationary physics, and the amplitude of non-Gaussianity is given by the parameter (assumed to be constant). The fifth is non-inflationary in nature, and hence independent on . See Fedeli et al. (2011) and references therein.

### 3.1 Local shape

This bispectrum shape arises when a light scalar field, additional to the inflaton, contributes to the curvature perturbations (Bernardeau & Uzan, 2002; Babich, Creminelli, & Zaldarriaga, 2004; Sasaki, Väliviita, & Wands, 2006). It is the same shape produced by the standard model of inflation (Falk, Rangarajan, & Srednicki, 1993) but in this case the amplitude can be arbitrary. The potential bispectrum takes the simple form

(19) |

and it is maximized for squeezed configurations. The quantity is the spectral amplitude of the potential (given by ), while is the spectral slope.

### 3.2 Equilateral shape

This shape is a consequence of the inflaton Lagrangian being non-standard, and containing higher-order derivatives of the field (Alishahiha, Silverstein, & Tong 2004; Arkani-Hamed et al. 2004; Li, Wang, & Wang 2008). The resulting bispectrum is maximized for equilateral configurations. A template for the equilateral bispectrum can be found in Creminelli et al. (2007), however the expression is rather cumbersome and I did not report it here. The same applies to the following shapes.

### 3.3 Enfolded shape

The enfolded shape results from primordial non-Gaussianity being evaluated without the regular Bunch-Davies vacuum hypothesis (Chen et al., 2007; Holman & Tolley, 2008). In this case the bispectrum is maximized for squashed configurations. A template for such a bispectrum is reported in Meerburg, van der Schaar, & Corasaniti (2009).

### 3.4 Orthogonal shape

This shape is defined as being orthogonal (with respect to a suitably defined scalar product) to both the local and equilateral forms. The resulting bispectrum is maximized for both equilateral and squashed configurations, and a template can be found in Senatore, Smith, & Zaldarriaga (2010).

### 3.5 Matter bounce shape

This configuration is the consequence of a model universe without inflation, but with a scale factor that bounces in a non-singular way (Brandenberger, 2009; Cai et al., 2009). The matter bounce leads to a scale-invariant spectrum of density fluctuations, and to a bispectrum whose shape is similar to the local shape. Being non-inflationary in origin, the non-Gaussianity induced by a matter bounce model has no dependence on . It can instead be shown that the matter bounce bispectrum is comparable to the local one with a fixed . I considered explicitly the matter bounce because it is in principle possible that a weighted integral of the bispectrum, such as the one in Eq. (17), would magnify its differences with respect to the local model. As I show below this is actually not the case.

## 4 Results

In Figure 1 I show as a function of the mass scale for the five non-Gaussian cosmologies considered in this letter. In all cases, except for the matter bounce, I selected in order to purely highlight the effect of the bispectrum shape. It is however easy to see that is simply proportional to . All curves decrease with increasing mass, implying that larger matter patches acquire lower amounts of angular momentum than smaller ones. This behavior is similar to the mass dependence of the linear term given in Eq. (15). Also, curves referring to different models are rather similar in shape. Besides the matter bounce model, the local model is the one having the largest effect, while the orthogonal model has the lowest. This is different from the behavior of, e.g., the halo bias, for which the equilateral model displays the smallest effect. The function for the matter bounce is virtually identical to that for the local model when assuming , in agreement with the previous discussion.

As can be seen from the structure of Eqs. (15) and (16), the relative importance of the non-Gaussian contribution with respect to the linear one is

(20) |

The acquisition of angular momentum by protostructures happens at high redshift where, under the assumption of flat spatial geometry, the Universe is well approximated by an Einstein-de Sitter model. Corrections due to the presence of a cosmological constant can be considered to be negligible. If this is the case, then

(21) |

Note that the negative sign cancels with the negative sign in the definition of , so that the non-Gaussian contribution is positive (increases the spin growth) for a model with positive skewness and negative otherwise. This has already been noticed by CT. The previous equation also shows that the non-Gaussian contribution to spin acquisition grows faster than the linear one.

If the matter patch under consideration is an overdense region, it is reasonable to assume that the spin growth induced by tidal torques occurs until the overdensity detaches from the overall expansion of the Universe and collapses into a bound structure. This moment can be naively identified as . For an Einstein-de Sitter cosmological model this implies , and thus

(22) |

In Figure 2 I show the mass dependence of the function for the various non-Gaussian cosmologies that have been considered in this work. For models with inflationary non-Gaussianity I assumed . As can be seen the mass dependence is in all cases relatively weak. In the local and matter bounce models is basically unchanged for masses ranging between and . For the equilateral and enfolded models increases by over the same interval, while for the orthogonal case it decreases by a factor of . Hence, despite the fact that the linear and non-Gaussian contributions to the spin growth both decrease with mass, their relative importance remains relatively unchanged. The only exception is represented by the orthogonal model.

Next, I selected a reference mass scale of and computed the dependence of on , shown in Figure 3. As previously mentioned, this dependence is always linear, however the Figure is important in order to understand for what value of a certain non-Gaussian model provides a given contribution to the total angular momentum variance. The matter bounce non-Gaussianity is independent of , hence its contribution is always at the percent (negative) level compared to the linear one. As for the other models, in order for the non-Gaussian contribution to be comparable to the linear one, primordial non-Gaussianity would need to be at the unrealistic level of for the local case, and substantially larger than that for other bispectrum shapes.

Figure 3 allows one to determine the non-Gaussian contribution, in units of the linear contribution, for the current bounds on . Constraints from the CMB (Komatsu et al., 2011) imply at Confidence Level (CL) for the local shape^{1}^{1}1I converted all constraints mentioned here to the LSS convention, which has been adopted throughout. See Fedeli & Moscardini (2010) and references therein for a discussion., meaning that the non-Gaussian contribution can be at most of the linear one. The same CMB data constrain for the equilateral shape, implying a relative importance. The tighter constraints on the level of non-Gaussianity for the enfolded shape come from the LSS (Xia et al., 2011), corresponding to at confidence level. This means that the non-Gaussian contribution is at most of the linear one. Finally, for the orthogonal shape the CMB data by Komatsu et al. (2011) bear , implying a maximum (negative) relative strength. These numbers can be appreciated also by looking at the positions of the filled circles in Figure 3. For comparison, the black dotted line shows the upper limit to the non-Gaussian contribution found by CT, after assuming a log-normal distribution for the primordial gravitational potential and after rescaling it to the scale . I stress the fact that, while CT adopted a Gaussian window function and , I used a real-space top-hat filter and . Moreover, while CT calibrated the level of primordial non-Gaussianity using a value for the skewness of the matter density field on a scale Mpc, I adopted, conservatively, . This value results from the large-scale skewness per unit for local non-Gaussianity (, e.g., Figure 1 of Fedeli et al. 2011) multiplied by the most recent upper limit on the level of non-Gaussianity for the same shape ().

## 5 Conclusions

I reconsidered the impact of primordial non-Gaussianity on the acquisition of angular momentum by CDM protostructures. Non-Gaussian initial conditions provide a next-to-linear correction to the spin growth that is absent when density fluctuations are normally distributed. Previous results, obtained by CT after assuming a log-normal primordial gravitational potential, resulted in a contribution to the spin variance of with respect to the linear one. This value holds for a scale (with the cosmology of this work) and is based on a matter skewness of , as deduced in the previous Section. Other models turned out to give a very large quasi-linear effect, suggesting that Lagrangian perturbation theory could not be successfully applied in those cases. I found that for several current models of non-Gaussian initial conditions, the contribution to the galactic spin variance during the mildly non-linear regime is similar to what predicted assuming a log-normal primordial gravitational potential. Considering the upper limits to the current constraints on the level of inflationary primordial non-Gaussianity returns a next-to-linear contribution at the level of . These results imply that the spin growth induced by inflationary non-Gaussianity seems to be generically tractable via perturbation theory.

CT also demonstrated that higher-order contributions in the case of Gaussian density fluctuations provide a correction to the angular momentum variance equal to of the linear term. This means that the next-to-linear non-Gaussian contribution estimated here has a significant impact on the spin acquisition by protostructures. Such an impact could potentially be even larger, because higher-order non-Gaussian corrections, that have not been considered here, depend on the trispectrum of the Zel’dovich potential, and hence also react to primordial non-Gaussianity. The results presented in this letter motivate the study of these higher-order contributions, and show how it is possible to consistently describe the dynamics of protostructures based on largely general cosmological initial conditions.

## Acknowledgements

I thank the University of Florida for support through the Theoretical Astrophysics Fellowship. I credit L. Moscardini for insightful comments on the manuscript and I am deeply indebted to the anonymous referee for help in substantially improving this work.

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