Quantcast
  • Register
PhysicsOverflow is a next-generation academic platform for physicists and astronomers, including a community peer review system and a postgraduate-level discussion forum analogous to MathOverflow.

Welcome to PhysicsOverflow! PhysicsOverflow is an open platform for community peer review and graduate-level Physics discussion.

Please help promote PhysicsOverflow ads elsewhere if you like it.

News

PO is now at the Physics Department of Bielefeld University!

New printer friendly PO pages!

Migration to Bielefeld University was successful!

Please vote for this year's PhysicsOverflow ads!

Please do help out in categorising submissions. Submit a paper to PhysicsOverflow!

... see more

Tools for paper authors

Submit paper
Claim Paper Authorship

Tools for SE users

Search User
Reclaim SE Account
Request Account Merger
Nativise imported posts
Claim post (deleted users)
Import SE post

Users whose questions have been imported from Physics Stack Exchange, Theoretical Physics Stack Exchange, or any other Stack Exchange site are kindly requested to reclaim their account and not to register as a new user.

Public \(\beta\) tools

Report a bug with a feature
Request a new functionality
404 page design
Send feedback

Attributions

(propose a free ad)

Site Statistics

205 submissions , 163 unreviewed
5,082 questions , 2,232 unanswered
5,352 answers , 22,786 comments
1,470 users with positive rep
820 active unimported users
More ...

  What exactly is meant by the "Gaussianity" of CMBR?

+ 7 like - 0 dislike
3757 views

What does it mean when we say that the CMBR is mostly gaussian? What are non-gaussianities in CMBR? How does evaluation of 3-point correlation functions of the inflaton field tells us that there is non-Gaussianity?

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Debangshu
asked Apr 25, 2011 in Theoretical Physics by DebangshuMukherjee (165 points) [ no revision ]

2 Answers

+ 7 like - 0 dislike

(Updated on 27 April to expand on and justify some points in response to comments.)

@dbrane's answer conveys a lot of the flavor of the subject correctly, but I'm sorry to say that it's not right in detail. Because there's plenty of room for confusion here, I'm going to spend quite a bit of time on the mathematics before saying anything about the physics or cosmology. Sorry about that. Feel free to skip to the bottom if you want.

Mathematics.

The definition of Gaussian in this context actually goes like this:

A function $g$ is Gaussian if the $n$-tuple $(g({\bf x}_1),g({\bf x}_2),\ldots,g({\bf x}_n))$ is drawn from an $n$-dimensional Gaussian distribution for all $n$ and for all choices of ${\bf x}_i$.

That is, if you look at any one point, that the value at that point is drawn from a Gaussian distribution. If you look at any two points, the values are drawn from a bivariate Gaussian distribution (possibly with correlations), etc. The above is my phrasing, but it's equivalent to things you'll find elsewhere, e.g., Wikipedia.

That definition is kind of a mouthful, but there's not much I can do about it: it's the way it is!

Before digging into the subject in more detail, it's worth defining one additional term, statistically homogeneous random fields. This just means that the statistical properties are unchanged if you slide all points over by any given amount. For instance, the average value $\langle g({\bf x})\rangle$ is independent of ${\bf x}$ (and indeed so is $\langle g({\bf x})^k\rangle$ for any $k$). Moreover, $\langle g({\bf x}_1)g({\bf x}_2)\rangle$ depends only on the difference ${\bf x}_1-{\bf x}_2$, and so forth. We often assume that the fields in cosmology have this property, because we think that, on average, the Universe is the same everywhere.

In addition, we also often assume that the statistical properties are invariant under rotation -- e.g., two-point correlations depend only on the magnitude of ${\bf x}_1-{\bf x}_2$ and not on its direction. The latter property is called statistical isotropy.

For the next little while, I'm going to focus on mathematical points that don't really depend on how many spatial dimensions we have, so for simplicity I'll work only in one dimension. In that case, of course, there's no such thing as isotropy. (By the way, I'm also going to start abbreviating "statistical homogeneity" as just "homogeneity.")

Before proceeding further, let me note explicitly that Gaussianity and statistical homogeneity are independent properties: neither one implies the other. For example, suppose that $g$ is Gaussian and homogeneous, and define another random field $h$ by setting $h(x)=[g(x)]^2$. Then $h$ is homogeneous but not Gaussian. (The pdf at any point is not Gaussian, for instance.) On the other hand, if we define $h(x)=xg(x)$, then $h$ is Gaussian but not homogeneous. (For instance, the variance $\langle h(x)^2\rangle$ depends on $x$.)

The nice property that dbrane mentions, namely that the Fourier transform of $g$ has no correlations, $$ \langle \tilde g({k_1})\tilde g({k}_2)\rangle=P_g({k}_1)\delta({k}_1+{k}_2), $$ is actually a consequence of homogeneity, not Gaussianity. (This property means that each Fourier mode $\tilde g({k})$ is uncorrelated with the others.)

This one's actually not hard to prove. The key is to think about the correlations between two points $x$ and $x+y$: $\langle g(x)g(x+y)\rangle$. Writing both of the $g$'s as Fourier integrals, we have $$ \langle g(x)g(x+y)\rangle= \int\int\langle\tilde g(k_1)\tilde g(k_2)\rangle e^{i(k_1+k_2)x}e^{ik_2y}\,dk_1\,dk_2. $$ Let me call the quantity on the left $G(x,y)$. This equation shows that the Fourier transform of $G$ with respect to both variables is given by $$ \tilde G(k_1+k_2,k_2)=\langle \tilde g(k_1)\tilde g(k_2)\rangle. $$ Homogeneity implies that $G$ depends only on $y$, not $x$, so $\tilde G(q,q')=0$ for all $q\ne 0$. Therefore $\langle\tilde g(k_1)\tilde g(k_2)\rangle$ is nonzero only for $k_1+k_2=0$. That proves the desired result.

If you're lucky enough to have both homogeneity and Gaussianity, then the "power spectrum" $P_g$ is a complete description of the statistical properties of $g$. But you have to assume Gaussianity in that argument; it doesn't follow from the assumption of uncorrelated Fourier modes. The simplest cosmological models predict both homogeneity and Gaussianity, so people often forget which useful properties follow from one as opposed to the other.

Digression: Other definitions found in the literature.

In the comments, a couple of people have pointed out quotes from very well-respected cosmologists (Liddle & Lyth, Komatsu) contradicting what I said and defining Gaussianity as uncorrelated Fourier modes. These folks are great cosmologists, but they're just wrong on this. I guess I can't expect you to take my word for it, so let me try to convince you in a couple of ways.

First, let me point out that Gaussian random processes and Gaussian random fields exist in many areas of applied mathematics, and the definition I gave is utterly standard everywhere else. (In case you're wondering, one tends to say "process" in one dimension, especially when you want to think of that one dimension as time, and "field" in 2 or more dimensions.) Wikipedia confirms this, as do plenty of other sources.

Of course, sometimes people in one discipline use a term differently from people in all other disciplines. Maybe cosmologists are doing that here? That turns out not to be the case. For instance, this paper is one of the ones that started the whole idea of considering Gaussianity in cosmology, and it uses the standard definition. Perhaps even more convincing is the fact that the main form of non-Gaussianity that cosmologists try to test these days is called local non-Gaussianity, which is defined as $$ \Phi({\bf x})=\phi({\bf x})+f_{NL}(\phi({\bf x})-\langle\phi\rangle)^2. $$ Here $f_{NL}$ is a constant, $\phi$ is a homogeneous Gaussian random field, and $\Phi$ is the physical field to be measured. The field $\Phi$ has uncorrelated Fourier modes (by the proof I gave above). So if "uncorrelated Fourier modes" were the definition of Gaussianity, then this field would be Gaussian. But if you talk to cosmologists working in the field, you'll find that every single one knows that this field is non-Gaussian -- in fact, it's regarded as the very archetype of non-Gaussianity. (Here's one example out of many I could have chosen.)

By the way, the error these folks have made is quite common. I think that there are several reasons. The main one is that the hypothesis of uncorrelated Fourier modes does imply approximate Gaussianity by a sort of central limit theorem argument, if some additional assumptions hold. Essentially, whatever quantities you're calculating have to have comparably-big contributions from many different Fourier modes, so that non-Gaussianities get "washed out." Back in the old days, people were willing to make that assumption, but when you're actually trying to measure non-Gaussianity, this is precisely the level of approximation you're not allowed to make.

Another reason is that everyone learns the "standard" (homogeneous, isotropic, Gaussian) picture of cosmological perturbations really well, then they forget which properties of the standard picture depend on which of the hypotheses. And of course once something is incorrectly stated somewhere, it propagates.

Physics.

As far as the physics is concerned, the main point is that some standard theoretical models, such as inflation, predict that the CMB (among other observables) should be Gaussian, as well as homogeneous and isotropic. If this is true, then the power spectrum, which I called $P_g(k)$ above, is a complete description of the statistical properties of the field. To define a Gaussian distribution, you just need to specify its first two moments, i.e., the mean and the variances & covariances. The mean is zero (mostly because we define it that way -- the observables are fluctuations about the mean). With these assumptions, there are no correlations in Fourier space, so all that leaves is the variances of the Fourier modes. That's what the power spectrum is.

Some slightly more exotic cosmological models (fancier versions of inflation as well as non-inflationary models) predict non-Gaussianity. One form this might take is nonzero 3rd-order correlations: things of the form $\langle g({\bf x}_1)g({\bf x}_2)g({\bf x}_3)\rangle$ should be zero in a Gaussian theory but not in a non-Gaussian one. That's the reason people look for 3-point correlations. If you look for them in position space, you call the thing you're trying to measure the "3-point correlation function." If you try to measure it in Fourier space, you call it the "bispectrum."

But even if there are no 3-point correlations, things might still be non-Gaussian. Gaussianity is a very specific set of mathematical properties, and there are infinitely many ways to be non-Gaussian. As a result, there are tons of proposed tests for non-Gaussianity, all looking at completely different things. For instance, a form of non-Gaussianity that was symmetric under a sign flip (the statistical properties of $-g$ are the same as those of $g$) would have no 3-point correlations, but it could still be non-Gaussian. You could search for that by looking at 4th-order correlations, although at some point thinking of things in terms of these correlations is not the best way to do it.

As a result, there are a bewildering variety of completely different tests people use. To cite one more-or-less randomly chosen example, people calculate the Minkowski functionals of excursion sets in CMB maps. The connection between Minkowski functionals and non-Gaussianity is not obvious, but the point is just that in a Gaussian process you can predict various properties of the functionals, and if the observations give different answers, that's non-Gaussianity.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
answered Apr 25, 2011 by Ted Bunn (140 points) [ no revision ]
Most voted comments show all comments
It's clear that I should expand my answer and justify some of the things I've been saying. I'll try to get to that later today.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
No, the quote I took was from Section 6.3.1 (Pg 88) where they define a Gaussian field using the correlators. What I gathered from that section is that Gaussianity is defined based on the correlator structure.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user dbrane
@dbrane -- I should've been clearer. In my previous comment I meant to refer to the Komatsu review article that Debangshu linked to.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
Edits done. I hope this version lays out the key points more clearly, although it's grown to be quite long! Comments extremely welcome.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
@Ted: very nice read. Thanks for the write-up!

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Willie Wong
Most recent comments show all comments
Thanks for your response! I'll have to go read Lyth and Liddle. I have a lot of respect for them and their work, but that's definitely not right.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
I saw Liddle and Lyth and the way dbrane defined Gaussianity is quite correct (at least according to Liddle and Lyth) however, I have issues regarding dbranes comment "Fourier modes being uncorrelated is precisely equivalent to statistical homogeneity & isotropy, and is completely independent of Gaussianity." Komatsu's review article clearly says the non-correlated Fourier mode is a result of Gaussianity!

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Debangshu
+ 6 like - 0 dislike

The physical meaning of gaussianity is that the CMBR is as random as possible, with no correlation at all between the independent fourier components of the fluctuation field. Each fourier mode of the inflationary perturbations that gave rise to the CMBR anisotropy evolved as independent uncoupled harmonic oscillators (albeit with a time dependent frequency).

Gaussianity of any cosmological variable $g(\textbf{x})$ (say, the scalar field perturbation $\delta\phi(\textbf{x})$ or the density $\rho(\textbf{x})$) is defined by the structure of the two-point correlator. If it has the form $$\langle g_{\textbf{k}}g_{\textbf{k'}}\rangle=(2\pi)^3\delta^3_{\textbf{k}+\textbf{k'}}P_g(k)$$ then $g(\textbf{x})$ is said to be Gaussian, where we've also assumed isotropy so that the power spectrum depends only on the magnitude $k$. (Homogenity means that $\langle g_{\textbf{k}}\rangle=0$). The 3-point-correlator (and all odd point correlators) vanish. This is the minimal possible correlation that you can have in a stochastic field. You're allowed to have any form for the power spectrum $P_g(k)$, although inflation predicts a nearly scale invariant spectrum, with it depending very weakly on $k$.

If you're wondering where the "gaussianity" actually comes in, it can be shown that the probability distribution for $g(\textbf{x})$ at any given point actually follows an exact gaussian: $$\textbf{P}(g)=\frac{1}{\sqrt{2\pi\sigma}}\exp{(-\frac{g^2}{2\sigma^2})}$$ So, for things like the scalar field, density and curvature, zero-deviation is most likely and higher fluctuations are exponentially suppressed.

You can start introducing additional correlations through the 3-point-correlator by making it non-zero and then you will have destroyed the gaussian structure of $\textbf{P}(g)$ above, hence it's called non-gaussianity. Such deviations are predicted by some models of inflation, but none have been observed so far. Tighter constraints on cosmological parameters from experiments like Planck should start coming in soon.

Chapter 6 of Lyth and Liddle's Primordial Density Perturbation is a good reference for this.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user dbrane
answered Apr 25, 2011 by dbrane (375 points) [ no revision ]
Most voted comments show all comments
@Willie Wong I'm learning about non-gaussianity. As a general rule, people who've just learnt something tend to explain things better than people who've been familiar with the same thing for a long time :)

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user dbrane
@Ted Bunn Yes, sorry about that, isotropy was implicitly assumed when I wrote $P_g(k)$ as a function of the magnitude $k$ alone. And homogenity also needs to be spelt out by stating that $\langle g_{\textbf{k}}\rangle=0$. But given just those conditions, you still have a Gaussian field -- despite the fact that Gaussianity doesn't require homogenity and isotropy -- is that what you meant?

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user dbrane
I'm sorry to rain on the parade, but although you've got some of the ideas right, this is not correct in detail. I'll post why in a separate answer, as it's too long for a comment.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
@dbrane -- no that's still just not correct. The statement about the Fourier modes being uncorrelated is precisely equivalent to statistical homogeneity & isotropy, and is completely independent of Gaussianity.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Ted Bunn
Ted Bunn is right that uncorrelated fourier modes is not equivalent to Gaussianity. As I understand it, Gaussianity just means that the values of the field at any given set of points are distributed according to a multivariate Gaussian. This is equivalent to saying that the two-point correlation function is all you need to describe any higher-order correlations (according to Weinberg).

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Thucydides411
Most recent comments show all comments
The temperature anisotropy of radiation and its power spectrum can be calculated from the scalar metric perturbation (predicted to be Gaussian by inflation, just like the scalar field perturbation and the density perturbation). This is done in great detail in Chapter 9 of Mukhanov's Physical Foundations of Cosmology.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user dbrane
+1 I've heard a whole semester's worth of seminars on nongaussianity, and no one explained it as nicely.

This post imported from StackExchange Physics at 2014-07-28 11:12 (UCT), posted by SE-user Willie Wong

Your answer

Please use answers only to (at least partly) answer questions. To comment, discuss, or ask for clarification, leave a comment instead.
To mask links under text, please type your text, highlight it, and click the "link" button. You can then enter your link URL.
Please consult the FAQ for as to how to format your post.
This is the answer box; if you want to write a comment instead, please use the 'add comment' button.
Live preview (may slow down editor)   Preview
Your name to display (optional):
Privacy: Your email address will only be used for sending these notifications.
Anti-spam verification:
If you are a human please identify the position of the character covered by the symbol $\varnothing$ in the following word:
p$\hbar$ysics$\varnothing$verflow
Then drag the red bullet below over the corresponding character of our banner. When you drop it there, the bullet changes to green (on slow internet connections after a few seconds).
Please complete the anti-spam verification




user contributions licensed under cc by-sa 3.0 with attribution required

Your rights
...