Normal distribution
Probability density function The red curve is the standard normal distribution  
Cumulative distribution function  
Notation  [math]\displaystyle{ \mathcal{N}(\mu,\sigma^2) }[/math]  

Parameters 
[math]\displaystyle{ \mu\in\R }[/math] = mean (location) [math]\displaystyle{ \sigma^2\in\R_{\gt 0} }[/math] = variance (squared scale)  
Support  [math]\displaystyle{ x\in\R }[/math]  
[math]\displaystyle{ \frac{1}{\sigma\sqrt{2\pi}} e^{\frac{1}{2}\left(\frac{x  \mu}{\sigma}\right)^2} }[/math]  
CDF  [math]\displaystyle{ \Phi\left(\frac{x\mu}{\sigma}\right) = \frac{1}{2}\left[1 + \operatorname{erf}\left( \frac{x\mu}{\sigma\sqrt{2}}\right)\right] }[/math]  
Quantile  [math]\displaystyle{ \mu+\sigma\sqrt{2} \operatorname{erf}^{1}(2p1) }[/math]  
Mean  [math]\displaystyle{ \mu }[/math]  
Median  [math]\displaystyle{ \mu }[/math]  
Mode  [math]\displaystyle{ \mu }[/math]  
Variance  [math]\displaystyle{ \sigma^2 }[/math]  
Skewness  [math]\displaystyle{ 0 }[/math]  
Kurtosis  [math]\displaystyle{ 0 }[/math]  
Entropy  [math]\displaystyle{ \frac{1}{2} \log(2\pi e \sigma^2) }[/math]  
MGF  [math]\displaystyle{ \exp(\mu t + \sigma^2t^2/2) }[/math]  
CF  [math]\displaystyle{ \exp(i\mu t  \sigma^2 t^2/2) }[/math]  
Fisher information 
[math]\displaystyle{ \mathcal{I}(\mu,\sigma) =\begin {pmatrix} 1/\sigma^2 & 0 \\ 0 & 2/\sigma^2\end{pmatrix} }[/math] [math]\displaystyle{ \mathcal{I}(\mu,\sigma^2) =\begin {pmatrix} 1/\sigma^2 & 0 \\ 0 & 1/(2\sigma^4)\end{pmatrix} }[/math]  
KullbackLeibler divergence  [math]\displaystyle{ { 1 \over 2 } \left\{ \left( \frac{\sigma_0}{\sigma_1} \right)^2 + \frac{(\mu_1  \mu_0)^2}{\sigma_1^2}  1 + \ln {\sigma_1^2 \over \sigma_0^2} \right\} }[/math] 
Part of a series on statistics 
Probability theory 

In statistics, a normal distribution or Gaussian distribution is a type of continuous probability distribution for a realvalued random variable. The general form of its probability density function is
 [math]\displaystyle{ f(x) = \frac{1}{\sigma \sqrt{2\pi} } e^{\frac{1}{2}\left(\frac{x\mu}{\sigma}\right)^2} }[/math]
The parameter [math]\displaystyle{ \mu }[/math] is the mean or expectation of the distribution (and also its median and mode), while the parameter [math]\displaystyle{ \sigma }[/math] is its standard deviation. The variance of the distribution is [math]\displaystyle{ \sigma^2 }[/math]. A random variable with a Gaussian distribution is said to be normally distributed, and is called a normal deviate.
Normal distributions are important in statistics and are often used in the natural and social sciences to represent realvalued random variables whose distributions are not known.^{[2]}^{[3]} Their importance is partly due to the central limit theorem. It states that, under some conditions, the average of many samples (observations) of a random variable with finite mean and variance is itself a random variable—whose distribution converges to a normal distribution as the number of samples increases. Therefore, physical quantities that are expected to be the sum of many independent processes, such as measurement errors, often have distributions that are nearly normal.^{[4]}
Moreover, Gaussian distributions have some unique properties that are valuable in analytic studies. For instance, any linear combination of a fixed collection of independent normal deviates is a normal deviate. Many results and methods, such as propagation of uncertainty and least squares^{[5]} parameter fitting, can be derived analytically in explicit form when the relevant variables are normally distributed.
A normal distribution is sometimes informally called a bell curve.^{[6]} However, many other distributions are bellshaped (such as the Cauchy, Student's t, and logistic distributions). For other names, see Naming.
The univariate probability distribution is generalized for vectors in the multivariate normal distribution and for matrices in the matrix normal distribution.
Definitions
Standard normal distribution
The simplest case of a normal distribution is known as the standard normal distribution or unit normal distribution. This is a special case when [math]\displaystyle{ \mu=0 }[/math] and [math]\displaystyle{ \sigma =1 }[/math], and it is described by this probability density function (or density):
 [math]\displaystyle{ \varphi(z) = \frac{e^{z^2/2}}{\sqrt{2\pi}}. }[/math]
The variable [math]\displaystyle{ z }[/math] has a mean of 0 and a variance and standard deviation of 1. The density [math]\displaystyle{ \varphi(z) }[/math] has its peak [math]\displaystyle{ 1/\sqrt{2\pi} }[/math] at [math]\displaystyle{ z=0 }[/math] and inflection points at [math]\displaystyle{ z=+1 }[/math] and [math]\displaystyle{ z=1 }[/math].
Although the density above is most commonly known as the standard normal, a few authors have used that term to describe other versions of the normal distribution. Carl Friedrich Gauss, for example, once defined the standard normal as
 [math]\displaystyle{ \varphi(z) = \frac{e^{z^2}}{\sqrt\pi}, }[/math]
which has a variance of 1/2, and Stephen Stigler^{[7]} once defined the standard normal as
 [math]\displaystyle{ \varphi(z) = e^{\pi z^2}, }[/math]
which has a simple functional form and a variance of [math]\displaystyle{ \sigma^2 = 1/(2\pi). }[/math]
General normal distribution
Every normal distribution is a version of the standard normal distribution, whose domain has been stretched by a factor [math]\displaystyle{ \sigma }[/math] (the standard deviation) and then translated by [math]\displaystyle{ \mu }[/math] (the mean value):
 [math]\displaystyle{ f(x \mid \mu, \sigma^2) =\frac 1 \sigma \varphi\left(\frac{x\mu} \sigma \right) }[/math]
The probability density must be scaled by [math]\displaystyle{ 1/\sigma }[/math] so that the integral is still 1.
If [math]\displaystyle{ Z }[/math] is a standard normal deviate, then [math]\displaystyle{ X=\sigma Z + \mu }[/math] will have a normal distribution with expected value [math]\displaystyle{ \mu }[/math] and standard deviation [math]\displaystyle{ \sigma }[/math]. This is equivalent to saying that the standard normal distribution [math]\displaystyle{ Z }[/math] can be scaled/stretched by a factor of [math]\displaystyle{ \sigma }[/math] and shifted by [math]\displaystyle{ \mu }[/math] to yield a different normal distribution, called [math]\displaystyle{ X }[/math]. Conversely, if [math]\displaystyle{ X }[/math] is a normal deviate with parameters [math]\displaystyle{ \mu }[/math] and [math]\displaystyle{ \sigma^2 }[/math], then this [math]\displaystyle{ X }[/math] distribution can be rescaled and shifted via the formula [math]\displaystyle{ Z=(X\mu)/\sigma }[/math] to convert it to the standard normal distribution. This variate is also called the standardized form of [math]\displaystyle{ X }[/math].
Notation
The probability density of the standard Gaussian distribution (standard normal distribution, with zero mean and unit variance) is often denoted with the Greek letter [math]\displaystyle{ \varphi }[/math] (phi).^{[8]} The alternative form of the Greek letter phi, [math]\displaystyle{ \varphi }[/math], is also used quite often.
The normal distribution is often referred to as [math]\displaystyle{ N(\mu,\sigma^2) }[/math] or [math]\displaystyle{ \mathcal{N}(\mu,\sigma^2) }[/math].^{[9]} Thus when a random variable [math]\displaystyle{ X }[/math] is normally distributed with mean [math]\displaystyle{ \mu }[/math] and standard deviation [math]\displaystyle{ \sigma }[/math], one may write
 [math]\displaystyle{ X \sim \mathcal{N}(\mu,\sigma^2). }[/math]
Alternative parameterizations
Some authors advocate using the precision [math]\displaystyle{ \tau }[/math] as the parameter defining the width of the distribution, instead of the deviation [math]\displaystyle{ \sigma }[/math] or the variance [math]\displaystyle{ \sigma^2 }[/math]. The precision is normally defined as the reciprocal of the variance, [math]\displaystyle{ 1/\sigma^2 }[/math].^{[10]} The formula for the distribution then becomes
 [math]\displaystyle{ f(x) = \sqrt{\frac\tau{2\pi}} e^{\tau(x\mu)^2/2}. }[/math]
This choice is claimed to have advantages in numerical computations when [math]\displaystyle{ \sigma }[/math] is very close to zero, and simplifies formulas in some contexts, such as in the Bayesian inference of variables with multivariate normal distribution.
Alternatively, the reciprocal of the standard deviation [math]\displaystyle{ \tau'=1/\sigma }[/math] might be defined as the precision, in which case the expression of the normal distribution becomes
 [math]\displaystyle{ f(x) = \frac{\tau'}{\sqrt{2\pi}} e^{(\tau')^2(x\mu)^2/2}. }[/math]
According to Stigler, this formulation is advantageous because of a much simpler and easiertoremember formula, and simple approximate formulas for the quantiles of the distribution.
Normal distributions form an exponential family with natural parameters [math]\displaystyle{ \textstyle\theta_1=\frac{\mu}{\sigma^2} }[/math] and [math]\displaystyle{ \textstyle\theta_2=\frac{1}{2\sigma^2} }[/math], and natural statistics x and x^{2}. The dual expectation parameters for normal distribution are η_{1} = μ and η_{2} = μ^{2} + σ^{2}.
Cumulative distribution function
The cumulative distribution function (CDF) of the standard normal distribution, usually denoted with the capital Greek letter [math]\displaystyle{ \Phi }[/math] (phi), is the integral
 [math]\displaystyle{ \Phi(x) = \frac 1 {\sqrt{2\pi}} \int_{\infty}^x e^{t^2/2} \, dt }[/math]
Error Function
The related error function [math]\displaystyle{ \operatorname{erf}(x) }[/math] gives the probability of a random variable, with normal distribution of mean 0 and variance 1/2 falling in the range [math]\displaystyle{ [x, x] }[/math]. That is:
 [math]\displaystyle{ \operatorname{erf}(x) = \frac 1 {\sqrt\pi} \int_{x}^x e^{t^2} \, dt = \frac 2 {\sqrt\pi} \int_0^x e^{t^2} \, dt }[/math]
These integrals cannot be expressed in terms of elementary functions, and are often said to be special functions. However, many numerical approximations are known; see below for more.
The two functions are closely related, namely
 [math]\displaystyle{ \Phi(x) = \frac{1}{2} \left[1 + \operatorname{erf}\left( \frac x {\sqrt 2} \right) \right] }[/math]
For a generic normal distribution with density [math]\displaystyle{ f }[/math], mean [math]\displaystyle{ \mu }[/math] and deviation [math]\displaystyle{ \sigma }[/math], the cumulative distribution function is
 [math]\displaystyle{ F(x) = \Phi\left(\frac{x\mu} \sigma \right) = \frac{1}{2} \left[1 + \operatorname{erf}\left(\frac{x\mu}{\sigma \sqrt 2 }\right)\right] }[/math]
The complement of the standard normal cumulative distribution function, [math]\displaystyle{ Q(x) = 1  \Phi(x) }[/math], is often called the Qfunction, especially in engineering texts.^{[11]}^{[12]} It gives the probability that the value of a standard normal random variable [math]\displaystyle{ X }[/math] will exceed [math]\displaystyle{ x }[/math]: [math]\displaystyle{ P(X\gt x) }[/math]. Other definitions of the [math]\displaystyle{ Q }[/math]function, all of which are simple transformations of [math]\displaystyle{ \Phi }[/math], are also used occasionally.^{[13]}
The graph of the standard normal cumulative distribution function [math]\displaystyle{ \Phi }[/math] has 2fold rotational symmetry around the point (0,1/2); that is, [math]\displaystyle{ \Phi(x) = 1  \Phi(x) }[/math]. Its antiderivative (indefinite integral) can be expressed as follows:
 [math]\displaystyle{ \int \Phi(x)\, dx = x\Phi(x) + \varphi(x) + C. }[/math]
The cumulative distribution function of the standard normal distribution can be expanded by Integration by parts into a series:
 [math]\displaystyle{ \Phi(x)=\frac{1}{2} + \frac{1}{\sqrt{2\pi}}\cdot e^{x^2/2} \left[x + \frac{x^3}{3} + \frac{x^5}{3\cdot 5} + \cdots + \frac{x^{2n+1}}{(2n+1)!!} + \cdots\right] }[/math]
where [math]\displaystyle{ !! }[/math] denotes the double factorial.
An asymptotic expansion of the cumulative distribution function for large x can also be derived using integration by parts. For more, see Error function.^{[14]}
A quick approximation to the standard normal distribution's cumulative distribution function can be found by using a Taylor series approximation:
 [math]\displaystyle{ \Phi(x) \approx \frac{1}{2}+\frac{1}{\sqrt{2\pi}} \sum_{k=0}^n \frac{(1)^k x^{(2k+1)}}{2^k k! (2k+1)} }[/math]
Recursive computation with Taylor series expansion
The recursive nature of the [math]\displaystyle{ e^{ax^2} }[/math]family of derivatives may be used to easily construct a rapidly converging Taylor series expansion using recursive entries about any point of known value of the distribution,[math]\displaystyle{ \Phi(x_0) }[/math]:
 [math]\displaystyle{ \Phi(x) = \sum_{n=0}^\infty \frac{\Phi^{(n)}(x_0)}{n!}(xx_0)^n }[/math]
where:
 [math]\displaystyle{ \begin{align} \Phi^{(0)}(x_0) &= \frac{1}{\sqrt{2\pi}}\int_{\infty}^{x_0}e^{t^2/2}\,dt \\ \Phi^{(1)}(x_0) &= \frac{1}{\sqrt{2\pi}}e^{x_0^2/2} \\ \Phi^{(n)}(x_0) &= \left(x_0\Phi^{(n1)}(x_0)+(n2)\Phi^{(n2)}(x_0)\right), & n \geq 2 \end{align} }[/math]
Using the Taylor series and Newton's method for the inverse function
An application for the above Taylor series expansion is to use Newton's method to reverse the computation. That is, if we have a value for the cumulative distribution function, [math]\displaystyle{ \Phi(x) }[/math], but do not know the x needed to obtain the [math]\displaystyle{ \Phi(x) }[/math], we can use Newton's method to find x, and use the Taylor series expansion above to minimize the number of computations. Newton's method is ideal to solve this problem because the first derivative of [math]\displaystyle{ \Phi(x) }[/math], which is an integral of the normal standard distribution, is the normal standard distribution, and is readily available to use in the Newton's method solution.
To solve, select a known approximate solution, [math]\displaystyle{ x_0 }[/math], to the desired [math]\displaystyle{ \Phi(x) }[/math]. [math]\displaystyle{ x_0 }[/math] may be a value from a distribution table, or an intelligent estimate followed by a computation of [math]\displaystyle{ \Phi(x_0) }[/math] using any desired means to compute. Use this value of [math]\displaystyle{ x_0 }[/math] and the Taylor series expansion above to minimize computations.
Repeat the following process until the difference between the computed [math]\displaystyle{ \Phi(x_{n}) }[/math] and the desired [math]\displaystyle{ \Phi }[/math], which we will call [math]\displaystyle{ \Phi(\text{desired}) }[/math], is below a chosen acceptably small error, such as 10^{−5}, 10^{−15}, etc.:
[math]\displaystyle{ x_{n+1} = x_n  \frac{\Phi(x_n,x_0,\Phi(x_0))\Phi(\text{desired})}{\Phi'(x_n)} }[/math]
where
 [math]\displaystyle{ \Phi(x,x_0,\Phi(x_0)) }[/math] is the [math]\displaystyle{ \Phi(x) }[/math] from a Taylor series solution using [math]\displaystyle{ x_0 }[/math] and [math]\displaystyle{ \Phi(x_0) }[/math]
 [math]\displaystyle{ \Phi'(x)=\frac{1}{\sqrt{2\pi}}e^{x^2/2} }[/math]
When the repeated computations converge to an error below the chosen acceptably small value, x will be the value needed to obtain a [math]\displaystyle{ \Phi(x) }[/math] of the desired value, [math]\displaystyle{ \Phi(\text{desired}) }[/math].
Standard deviation and coverage
About 68% of values drawn from a normal distribution are within one standard deviation σ away from the mean; about 95% of the values lie within two standard deviations; and about 99.7% are within three standard deviations.^{[6]} This fact is known as the 689599.7 (empirical) rule, or the 3sigma rule.
More precisely, the probability that a normal deviate lies in the range between [math]\displaystyle{ \mun\sigma }[/math] and [math]\displaystyle{ \mu+n\sigma }[/math] is given by
 [math]\displaystyle{ F(\mu+n\sigma)  F(\mun\sigma) = \Phi(n)\Phi(n) = \operatorname{erf} \left(\frac{n}{\sqrt{2}}\right). }[/math]
To 12 significant digits, the values for [math]\displaystyle{ n=1,2,\ldots , 6 }[/math] are:^{[citation needed]}
[math]\displaystyle{ n }[/math]  [math]\displaystyle{ p= F(\mu+n\sigma)  F(\mun\sigma) }[/math]  [math]\displaystyle{ \text{i.e. }1p }[/math]  [math]\displaystyle{ \text{or }1\text{ in }p }[/math]  OEIS  

1  0.682689492137  0.317310507863 

OEIS: A178647  
2  0.954499736104  0.045500263896 

OEIS: A110894  
3  0.997300203937  0.002699796063 

OEIS: A270712  
4  0.999936657516  0.000063342484 
 
5  0.999999426697  0.000000573303 
 
6  0.999999998027  0.000000001973 

For large [math]\displaystyle{ n }[/math], one can use the approximation [math]\displaystyle{ 1  p \approx \frac{e^{n^2/2}}{n\sqrt{\pi/2}} }[/math].
Quantile function
The quantile function of a distribution is the inverse of the cumulative distribution function. The quantile function of the standard normal distribution is called the probit function, and can be expressed in terms of the inverse error function:
 [math]\displaystyle{ \Phi^{1}(p) = \sqrt2\operatorname{erf}^{1}(2p  1), \quad p\in(0,1). }[/math]
For a normal random variable with mean [math]\displaystyle{ \mu }[/math] and variance [math]\displaystyle{ \sigma^2 }[/math], the quantile function is
 [math]\displaystyle{ F^{1}(p) = \mu + \sigma\Phi^{1}(p) = \mu + \sigma\sqrt 2 \operatorname{erf}^{1}(2p  1), \quad p\in(0,1). }[/math]
The quantile [math]\displaystyle{ \Phi^{1}(p) }[/math] of the standard normal distribution is commonly denoted as [math]\displaystyle{ z_p }[/math]. These values are used in hypothesis testing, construction of confidence intervals and Q–Q plots. A normal random variable [math]\displaystyle{ X }[/math] will exceed [math]\displaystyle{ \mu + z_p\sigma }[/math] with probability [math]\displaystyle{ 1p }[/math], and will lie outside the interval [math]\displaystyle{ \mu \pm z_p\sigma }[/math] with probability [math]\displaystyle{ 2(1p) }[/math]. In particular, the quantile [math]\displaystyle{ z_{0.975} }[/math] is 1.96; therefore a normal random variable will lie outside the interval [math]\displaystyle{ \mu \pm 1.96\sigma }[/math] in only 5% of cases.
The following table gives the quantile [math]\displaystyle{ z_p }[/math] such that [math]\displaystyle{ X }[/math] will lie in the range [math]\displaystyle{ \mu \pm z_p\sigma }[/math] with a specified probability [math]\displaystyle{ p }[/math]. These values are useful to determine tolerance interval for sample averages and other statistical estimators with normal (or asymptotically normal) distributions.^{[15]} The following table shows [math]\displaystyle{ \sqrt 2 \operatorname{erf}^{1}(p)=\Phi^{1}\left(\frac{p+1}{2}\right) }[/math], not [math]\displaystyle{ \Phi^{1}(p) }[/math] as defined above.
[math]\displaystyle{ p }[/math]  [math]\displaystyle{ z_p }[/math]  [math]\displaystyle{ p }[/math]  [math]\displaystyle{ z_p }[/math]  

0.80  1.281551565545  0.999  3.290526731492  
0.90  1.644853626951  0.9999  3.890591886413  
0.95  1.959963984540  0.99999  4.417173413469  
0.98  2.326347874041  0.999999  4.891638475699  
0.99  2.575829303549  0.9999999  5.326723886384  
0.995  2.807033768344  0.99999999  5.730728868236  
0.998  3.090232306168  0.999999999  6.109410204869 
For small [math]\displaystyle{ p }[/math], the quantile function has the useful asymptotic expansion [math]\displaystyle{ \Phi^{1}(p)=\sqrt{\ln\frac{1}{p^2}\ln\ln\frac{1}{p^2}\ln(2\pi)}+\mathcal{o}(1). }[/math]^{[citation needed]}
Properties
The normal distribution is the only distribution whose cumulants beyond the first two (i.e., other than the mean and variance) are zero. It is also the continuous distribution with the maximum entropy for a specified mean and variance.^{[16]}^{[17]} Geary has shown, assuming that the mean and variance are finite, that the normal distribution is the only distribution where the mean and variance calculated from a set of independent draws are independent of each other.^{[18]}^{[19]}
The normal distribution is a subclass of the elliptical distributions. The normal distribution is symmetric about its mean, and is nonzero over the entire real line. As such it may not be a suitable model for variables that are inherently positive or strongly skewed, such as the weight of a person or the price of a share. Such variables may be better described by other distributions, such as the lognormal distribution or the Pareto distribution.
The value of the normal distribution is practically zero when the value [math]\displaystyle{ x }[/math] lies more than a few standard deviations away from the mean (e.g., a spread of three standard deviations covers all but 0.27% of the total distribution). Therefore, it may not be an appropriate model when one expects a significant fraction of outliers—values that lie many standard deviations away from the mean—and least squares and other statistical inference methods that are optimal for normally distributed variables often become highly unreliable when applied to such data. In those cases, a more heavytailed distribution should be assumed and the appropriate robust statistical inference methods applied.
The Gaussian distribution belongs to the family of stable distributions which are the attractors of sums of independent, identically distributed distributions whether or not the mean or variance is finite. Except for the Gaussian which is a limiting case, all stable distributions have heavy tails and infinite variance. It is one of the few distributions that are stable and that have probability density functions that can be expressed analytically, the others being the Cauchy distribution and the Lévy distribution.
Symmetries and derivatives
The normal distribution with density [math]\displaystyle{ f(x) }[/math] (mean [math]\displaystyle{ \mu }[/math] and standard deviation [math]\displaystyle{ \sigma \gt 0 }[/math]) has the following properties:
 It is symmetric around the point [math]\displaystyle{ x=\mu, }[/math] which is at the same time the mode, the median and the mean of the distribution.^{[20]}
 It is unimodal: its first derivative is positive for [math]\displaystyle{ x\lt \mu, }[/math] negative for [math]\displaystyle{ x\gt \mu, }[/math] and zero only at [math]\displaystyle{ x=\mu. }[/math]
 The area bounded by the curve and the [math]\displaystyle{ x }[/math]axis is unity (i.e. equal to one).
 Its first derivative is [math]\displaystyle{ f'(x)=\frac{x\mu}{\sigma^2} f(x). }[/math]
 Its second derivative is [math]\displaystyle{ f''(x) = \frac{(x\mu)^2  \sigma^2}{\sigma^4} f(x). }[/math]
 Its density has two inflection points (where the second derivative of [math]\displaystyle{ f }[/math] is zero and changes sign), located one standard deviation away from the mean, namely at [math]\displaystyle{ x=\mu\sigma }[/math] and [math]\displaystyle{ x=\mu+\sigma. }[/math]^{[20]}
 Its density is logconcave.^{[20]}
 Its density is infinitely differentiable, indeed supersmooth of order 2.^{[21]}
Furthermore, the density [math]\displaystyle{ \varphi }[/math] of the standard normal distribution (i.e. [math]\displaystyle{ \mu=0 }[/math] and [math]\displaystyle{ \sigma=1 }[/math]) also has the following properties:
 Its first derivative is [math]\displaystyle{ \varphi'(x)=x\varphi(x). }[/math]
 Its second derivative is [math]\displaystyle{ \varphi''(x)=(x^21)\varphi(x) }[/math]
 More generally, its nth derivative is [math]\displaystyle{ \varphi^{(n)}(x) = (1)^n\operatorname{He}_n(x)\varphi(x), }[/math] where [math]\displaystyle{ \operatorname{He}_n(x) }[/math] is the nth (probabilist) Hermite polynomial.^{[22]}
 The probability that a normally distributed variable [math]\displaystyle{ X }[/math] with known [math]\displaystyle{ \mu }[/math] and [math]\displaystyle{ \sigma }[/math] is in a particular set, can be calculated by using the fact that the fraction [math]\displaystyle{ Z = (X\mu)/\sigma }[/math] has a standard normal distribution.
Moments
The plain and absolute moments of a variable [math]\displaystyle{ X }[/math] are the expected values of [math]\displaystyle{ X^p }[/math] and [math]\displaystyle{ X^p }[/math], respectively. If the expected value [math]\displaystyle{ \mu }[/math] of [math]\displaystyle{ X }[/math] is zero, these parameters are called central moments; otherwise, these parameters are called noncentral moments. Usually we are interested only in moments with integer order [math]\displaystyle{ \ p }[/math].
If [math]\displaystyle{ X }[/math] has a normal distribution, the noncentral moments exist and are finite for any [math]\displaystyle{ p }[/math] whose real part is greater than −1. For any nonnegative integer [math]\displaystyle{ p }[/math], the plain central moments are:^{[23]}
 [math]\displaystyle{ \operatorname{E}\left[(X\mu)^p\right] = \begin{cases} 0 & \text{if }p\text{ is odd,} \\ \sigma^p (p1)!! & \text{if }p\text{ is even.} \end{cases} }[/math]
Here [math]\displaystyle{ n!! }[/math] denotes the double factorial, that is, the product of all numbers from [math]\displaystyle{ n }[/math] to 1 that have the same parity as [math]\displaystyle{ n. }[/math]
The central absolute moments coincide with plain moments for all even orders, but are nonzero for odd orders. For any nonnegative integer [math]\displaystyle{ p, }[/math]
 [math]\displaystyle{ \begin{align} \operatorname{E}\left[X  \mu^p\right] &= \sigma^p (p1)!! \cdot \begin{cases} \sqrt{\frac{2}{\pi}} & \text{if }p\text{ is odd} \\ 1 & \text{if }p\text{ is even} \end{cases} \\ &= \sigma^p \cdot \frac{2^{p/2}\Gamma\left(\frac{p+1} 2 \right)}{\sqrt\pi}. \end{align} }[/math]
The last formula is valid also for any noninteger [math]\displaystyle{ p\gt 1. }[/math] When the mean [math]\displaystyle{ \mu \ne 0, }[/math] the plain and absolute moments can be expressed in terms of confluent hypergeometric functions [math]\displaystyle{ {}_1F_1 }[/math] and [math]\displaystyle{ U. }[/math]^{[24]}
 [math]\displaystyle{ \begin{align} \operatorname{E}\left[X^p\right] &= \sigma^p\cdot (i\sqrt 2)^p U\left(\frac{p}{2}, \frac{1}{2}, \frac{1}{2} \left( \frac \mu \sigma \right)^2 \right), \\ \operatorname{E}\left[X^p \right] &= \sigma^p \cdot 2^{p/2} \frac {\Gamma\left(\frac{1+p} 2\right)}{\sqrt\pi} {}_1F_1\left( \frac{p}{2}, \frac{1}{2}, \frac{1}{2} \left( \frac \mu \sigma \right)^2 \right). \end{align} }[/math]
These expressions remain valid even if [math]\displaystyle{ p }[/math] is not an integer. See also generalized Hermite polynomials.
Order  Noncentral moment  Central moment 

1  [math]\displaystyle{ \mu }[/math]  [math]\displaystyle{ 0 }[/math] 
2  [math]\displaystyle{ \mu^2+\sigma^2 }[/math]  [math]\displaystyle{ \sigma^2 }[/math] 
3  [math]\displaystyle{ \mu^3+3\mu\sigma^2 }[/math]  [math]\displaystyle{ 0 }[/math] 
4  [math]\displaystyle{ \mu^4+6\mu^2\sigma^2+3\sigma^4 }[/math]  [math]\displaystyle{ 3\sigma^4 }[/math] 
5  [math]\displaystyle{ \mu^5+10\mu^3\sigma^2+15\mu\sigma^4 }[/math]  [math]\displaystyle{ 0 }[/math] 
6  [math]\displaystyle{ \mu^6+15\mu^4\sigma^2+45\mu^2\sigma^4+15\sigma^6 }[/math]  [math]\displaystyle{ 15\sigma^6 }[/math] 
7  [math]\displaystyle{ \mu^7+21\mu^5\sigma^2+105\mu^3\sigma^4+105\mu\sigma^6 }[/math]  [math]\displaystyle{ 0 }[/math] 
8  [math]\displaystyle{ \mu^8+28\mu^6\sigma^2+210\mu^4\sigma^4+420\mu^2\sigma^6+105\sigma^8 }[/math]  [math]\displaystyle{ 105\sigma^8 }[/math] 
The expectation of [math]\displaystyle{ X }[/math] conditioned on the event that [math]\displaystyle{ X }[/math] lies in an interval [math]\displaystyle{ [a,b] }[/math] is given by
 [math]\displaystyle{ \operatorname{E}\left[X \mid a\lt X\lt b \right] = \mu  \sigma^2\frac{f(b)f(a)}{F(b)F(a)} }[/math]
where [math]\displaystyle{ f }[/math] and [math]\displaystyle{ F }[/math] respectively are the density and the cumulative distribution function of [math]\displaystyle{ X }[/math]. For [math]\displaystyle{ b=\infty }[/math] this is known as the inverse Mills ratio. Note that above, density [math]\displaystyle{ f }[/math] of [math]\displaystyle{ X }[/math] is used instead of standard normal density as in inverse Mills ratio, so here we have [math]\displaystyle{ \sigma^2 }[/math] instead of [math]\displaystyle{ \sigma }[/math].
Fourier transform and characteristic function
The Fourier transform of a normal density [math]\displaystyle{ f }[/math] with mean [math]\displaystyle{ \mu }[/math] and standard deviation [math]\displaystyle{ \sigma }[/math] is^{[25]}
 [math]\displaystyle{ \hat f(t) = \int_{\infty}^\infty f(x)e^{itx} \, dx = e^{i\mu t} e^{ \frac12 (\sigma t)^2} }[/math]
where [math]\displaystyle{ i }[/math] is the imaginary unit. If the mean [math]\displaystyle{ \mu=0 }[/math], the first factor is 1, and the Fourier transform is, apart from a constant factor, a normal density on the frequency domain, with mean 0 and standard deviation [math]\displaystyle{ 1/\sigma }[/math]. In particular, the standard normal distribution [math]\displaystyle{ \varphi }[/math] is an eigenfunction of the Fourier transform.
In probability theory, the Fourier transform of the probability distribution of a realvalued random variable [math]\displaystyle{ X }[/math] is closely connected to the characteristic function [math]\displaystyle{ \varphi_X(t) }[/math] of that variable, which is defined as the expected value of [math]\displaystyle{ e^{itX} }[/math], as a function of the real variable [math]\displaystyle{ t }[/math] (the frequency parameter of the Fourier transform). This definition can be analytically extended to a complexvalue variable [math]\displaystyle{ t }[/math].^{[26]} The relation between both is:
 [math]\displaystyle{ \varphi_X(t) = \hat f(t) }[/math]
Moment and cumulantgenerating functions
The moment generating function of a real random variable [math]\displaystyle{ X }[/math] is the expected value of [math]\displaystyle{ e^{tX} }[/math], as a function of the real parameter [math]\displaystyle{ t }[/math]. For a normal distribution with density [math]\displaystyle{ f }[/math], mean [math]\displaystyle{ \mu }[/math] and deviation [math]\displaystyle{ \sigma }[/math], the moment generating function exists and is equal to
 [math]\displaystyle{ M(t) = \operatorname{E}\left[e^{tX}\right] = \hat f(it) = e^{\mu t} e^{\sigma^2 t^2/2} }[/math]
The cumulant generating function is the logarithm of the moment generating function, namely
 [math]\displaystyle{ g(t) = \ln M(t) = \mu t + \tfrac 12 \sigma^2 t^2 }[/math]
Since this is a quadratic polynomial in [math]\displaystyle{ t }[/math], only the first two cumulants are nonzero, namely the mean [math]\displaystyle{ \mu }[/math] and the variance [math]\displaystyle{ \sigma^2 }[/math].
Some authors prefer to instead work with E[e^{itX}] = e^{iμt − σ2t2/2} and ln E[e^{itX}] = iμt − 1/2σ^{2}t^{2}.
Stein operator and class
Within Stein's method the Stein operator and class of a random variable [math]\displaystyle{ X \sim \mathcal{N}(\mu, \sigma^2) }[/math] are [math]\displaystyle{ \mathcal{A}f(x) = \sigma^2 f'(x)  (x\mu)f(x) }[/math] and [math]\displaystyle{ \mathcal{F} }[/math] the class of all absolutely continuous functions [math]\displaystyle{ f : \R \to \R \mbox{ such that }\mathbb{E}[f'(X)]\lt \infty }[/math].
Zerovariance limit
In the limit when [math]\displaystyle{ \sigma }[/math] tends to zero, the probability density [math]\displaystyle{ f(x) }[/math] eventually tends to zero at any [math]\displaystyle{ x\ne \mu }[/math], but grows without limit if [math]\displaystyle{ x = \mu }[/math], while its integral remains equal to 1. Therefore, the normal distribution cannot be defined as an ordinary function when [math]\displaystyle{ \sigma = 0 }[/math].
However, one can define the normal distribution with zero variance as a generalized function; specifically, as a Dirac delta function [math]\displaystyle{ \delta }[/math] translated by the mean [math]\displaystyle{ \mu }[/math], that is [math]\displaystyle{ f(x)=\delta(x\mu). }[/math] Its cumulative distribution function is then the Heaviside step function translated by the mean [math]\displaystyle{ \mu }[/math], namely
 [math]\displaystyle{ F(x) = \begin{cases} 0 & \text{if }x \lt \mu \\ 1 & \text{if }x \geq \mu \end{cases} }[/math]
Maximum entropy
Of all probability distributions over the reals with a specified finite mean [math]\displaystyle{ \mu }[/math] and finite variance [math]\displaystyle{ \sigma^2 }[/math], the normal distribution [math]\displaystyle{ N(\mu,\sigma^2) }[/math] is the one with maximum entropy.^{[27]} To see this, let [math]\displaystyle{ X }[/math] be a continuous random variable with probability density [math]\displaystyle{ f(x) }[/math]. The entropy of [math]\displaystyle{ X }[/math] is defined as^{[28]}^{[29]}^{[30]}
 [math]\displaystyle{ H(X) =  \int_{\infty}^\infty f(x)\ln f(x)\, dx }[/math]
where [math]\displaystyle{ f(x)\log f(x) }[/math] is understood to be zero whenever [math]\displaystyle{ f(x)=0 }[/math]. This functional can be maximized, subject to the constraints that the distribution is properly normalized and has a specified mean and variance, by using variational calculus. A function with three Lagrange multipliers is defined:
 [math]\displaystyle{ L=\int_{\infty}^\infty f(x)\ln f(x)\,dx\lambda_0\left(1\int_{\infty}^\infty f(x)\,dx\right)\lambda_1\left(\mu\int_{\infty}^\infty f(x)x\,dx\right)\lambda_2\left(\sigma^2\int_{\infty}^\infty f(x)(x\mu)^2\,dx\right)\,. }[/math]
At maximum entropy, a small variation [math]\displaystyle{ \delta f(x) }[/math] about [math]\displaystyle{ f(x) }[/math] will produce a variation [math]\displaystyle{ \delta L }[/math] about [math]\displaystyle{ L }[/math] which is equal to 0:
 [math]\displaystyle{ 0=\delta L=\int_{\infty}^\infty \delta f(x)\left(\ln f(x) 1+\lambda_0+\lambda_1 x+\lambda_2(x\mu)^2\right)\,dx }[/math]
Since this must hold for any small [math]\displaystyle{ \delta f(x) }[/math], the factor multiplying [math]\displaystyle{ \delta f(x) }[/math] must be zero, and solving for [math]\displaystyle{ f(x) }[/math] yields:
 [math]\displaystyle{ f(x)=\exp\left(1+\lambda_0+\lambda_1 x+\lambda_2(x\mu)^2\right)\,. }[/math]
The Lagrange constraints that [math]\displaystyle{ f(x) }[/math] is properly normalized and has the specified mean and variance are satisfied if and only if [math]\displaystyle{ \lambda_0 }[/math], [math]\displaystyle{ \lambda_1 }[/math], and [math]\displaystyle{ \lambda_2 }[/math] are chosen so that
 [math]\displaystyle{ f(x)=\frac{1}{\sqrt{2\pi\sigma^2}}e^{\frac{(x\mu)^2}{2\sigma^2}}\,. }[/math]
The entropy of a normal distribution [math]\displaystyle{ X \sim N(\mu,\sigma^2) }[/math] is equal to
 [math]\displaystyle{ H(X)=\tfrac{1}{2}(1+\ln 2\sigma^2\pi)\,, }[/math]
which is independent of the mean [math]\displaystyle{ \mu }[/math].
Other properties
 If the characteristic function [math]\displaystyle{ \phi_X }[/math] of some random variable [math]\displaystyle{ X }[/math] is of the form [math]\displaystyle{ \phi_X(t) = \exp Q(t) }[/math], where [math]\displaystyle{ Q(t) }[/math] is a polynomial, then the Marcinkiewicz theorem (named after Józef Marcinkiewicz) asserts that [math]\displaystyle{ Q }[/math] can be at most a quadratic polynomial, and therefore [math]\displaystyle{ X }[/math] is a normal random variable.^{[31]} The consequence of this result is that the normal distribution is the only distribution with a finite number (two) of nonzero cumulants.
 If [math]\displaystyle{ X }[/math] and [math]\displaystyle{ Y }[/math] are jointly normal and uncorrelated, then they are independent. The requirement that [math]\displaystyle{ X }[/math] and [math]\displaystyle{ Y }[/math] should be jointly normal is essential; without it the property does not hold.^{[32]}^{[33]}^{[proof]} For nonnormal random variables uncorrelatedness does not imply independence.
 The Kullback–Leibler divergence of one normal distribution [math]\displaystyle{ X_1 \sim N(\mu_1, \sigma^2_1) }[/math] from another [math]\displaystyle{ X_2 \sim N(\mu_2, \sigma^2_2) }[/math] is given by:^{[34]} [math]\displaystyle{ D_\mathrm{KL}( X_1 \parallel X_2 ) = \frac{(\mu_1  \mu_2)^2}{2\sigma_2^2} + \frac{1}{2}\left( \frac{\sigma_1^2}{\sigma_2^2}  1  \ln\frac{\sigma_1^2}{\sigma_2^2} \right) }[/math] The Hellinger distance between the same distributions is equal to [math]\displaystyle{ H^2(X_1,X_2) = 1  \sqrt{\frac{2\sigma_1\sigma_2}{\sigma_1^2+\sigma_2^2}} \exp\left(\frac{1}{4}\frac{(\mu_1\mu_2)^2}{\sigma_1^2+\sigma_2^2}\right) }[/math]
 The Fisher information matrix for a normal distribution w.r.t. [math]\displaystyle{ \mu }[/math] and [math]\displaystyle{ \sigma^2 }[/math] is diagonal and takes the form [math]\displaystyle{ \mathcal I (\mu, \sigma^2) = \begin{pmatrix} \frac{1}{\sigma^2} & 0 \\ 0 & \frac{1}{2\sigma^4} \end{pmatrix} }[/math]
 The conjugate prior of the mean of a normal distribution is another normal distribution.^{[35]} Specifically, if [math]\displaystyle{ x_1, \ldots, x_n }[/math] are iid [math]\displaystyle{ \sim N(\mu, \sigma^2) }[/math] and the prior is [math]\displaystyle{ \mu \sim N(\mu_0 , \sigma^2_0) }[/math], then the posterior distribution for the estimator of [math]\displaystyle{ \mu }[/math] will be [math]\displaystyle{ \mu \mid x_1,\ldots,x_n \sim \mathcal{N}\left( \frac{\frac{\sigma^2}{n}\mu_0 + \sigma_0^2\bar{x}}{\frac{\sigma^2}{n}+\sigma_0^2},\left( \frac{n}{\sigma^2} + \frac{1}{\sigma_0^2} \right)^{1} \right) }[/math]
 The family of normal distributions not only forms an exponential family (EF), but in fact forms a natural exponential family (NEF) with quadratic variance function (NEFQVF). Many properties of normal distributions generalize to properties of NEFQVF distributions, NEF distributions, or EF distributions generally. NEFQVF distributions comprises 6 families, including Poisson, Gamma, binomial, and negative binomial distributions, while many of the common families studied in probability and statistics are NEF or EF.
 In information geometry, the family of normal distributions forms a statistical manifold with constant curvature [math]\displaystyle{ 1 }[/math]. The same family is flat with respect to the (±1)connections [math]\displaystyle{ \nabla^{(e)} }[/math] and [math]\displaystyle{ \nabla^{(m)} }[/math].^{[36]}
Related distributions
Central limit theorem
The central limit theorem states that under certain (fairly common) conditions, the sum of many random variables will have an approximately normal distribution. More specifically, where [math]\displaystyle{ X_1,\ldots ,X_n }[/math] are independent and identically distributed random variables with the same arbitrary distribution, zero mean, and variance [math]\displaystyle{ \sigma^2 }[/math] and [math]\displaystyle{ Z }[/math] is their mean scaled by [math]\displaystyle{ \sqrt{n} }[/math]
 [math]\displaystyle{ Z = \sqrt{n}\left(\frac{1}{n}\sum_{i=1}^n X_i\right) }[/math]
Then, as [math]\displaystyle{ n }[/math] increases, the probability distribution of [math]\displaystyle{ Z }[/math] will tend to the normal distribution with zero mean and variance [math]\displaystyle{ \sigma^2 }[/math].
The theorem can be extended to variables [math]\displaystyle{ (X_i) }[/math] that are not independent and/or not identically distributed if certain constraints are placed on the degree of dependence and the moments of the distributions.
Many test statistics, scores, and estimators encountered in practice contain sums of certain random variables in them, and even more estimators can be represented as sums of random variables through the use of influence functions. The central limit theorem implies that those statistical parameters will have asymptotically normal distributions.
The central limit theorem also implies that certain distributions can be approximated by the normal distribution, for example:
 The binomial distribution [math]\displaystyle{ B(n,p) }[/math] is approximately normal with mean [math]\displaystyle{ np }[/math] and variance [math]\displaystyle{ np(1p) }[/math] for large [math]\displaystyle{ n }[/math] and for [math]\displaystyle{ p }[/math] not too close to 0 or 1.
 The Poisson distribution with parameter [math]\displaystyle{ \lambda }[/math] is approximately normal with mean [math]\displaystyle{ \lambda }[/math] and variance [math]\displaystyle{ \lambda }[/math], for large values of [math]\displaystyle{ \lambda }[/math].^{[37]}
 The chisquared distribution [math]\displaystyle{ \chi^2(k) }[/math] is approximately normal with mean [math]\displaystyle{ k }[/math] and variance [math]\displaystyle{ 2k }[/math], for large [math]\displaystyle{ k }[/math].
 The Student's tdistribution [math]\displaystyle{ t(\nu) }[/math] is approximately normal with mean 0 and variance 1 when [math]\displaystyle{ \nu }[/math] is large.
Whether these approximations are sufficiently accurate depends on the purpose for which they are needed, and the rate of convergence to the normal distribution. It is typically the case that such approximations are less accurate in the tails of the distribution.
A general upper bound for the approximation error in the central limit theorem is given by the Berry–Esseen theorem, improvements of the approximation are given by the Edgeworth expansions.
This theorem can also be used to justify modeling the sum of many uniform noise sources as Gaussian noise. See AWGN.
Operations and functions of normal variables
The probability density, cumulative distribution, and inverse cumulative distribution of any function of one or more independent or correlated normal variables can be computed with the numerical method of raytracing^{[38]} (Matlab code). In the following sections we look at some special cases.
Operations on a single normal variable
If [math]\displaystyle{ X }[/math] is distributed normally with mean [math]\displaystyle{ \mu }[/math] and variance [math]\displaystyle{ \sigma^2 }[/math], then
 [math]\displaystyle{ aX+b }[/math], for any real numbers [math]\displaystyle{ a }[/math] and [math]\displaystyle{ b }[/math], is also normally distributed, with mean [math]\displaystyle{ a\mu+b }[/math] and standard deviation [math]\displaystyle{ a\sigma }[/math]. That is, the family of normal distributions is closed under linear transformations.
 The exponential of [math]\displaystyle{ X }[/math] is distributed lognormally: [math]\displaystyle{ e^X \sim \ln(N(\mu, \sigma^2)) }[/math].
 The absolute value of [math]\displaystyle{ X }[/math] has folded normal distribution: [math]\displaystyle{ {{\left X \right \sim N_f(\mu, \sigma^2)}} }[/math]. If [math]\displaystyle{ \mu = 0 }[/math] this is known as the halfnormal distribution.
 The absolute value of normalized residuals, [math]\displaystyle{ X  \mu / \sigma }[/math], has chi distribution with one degree of freedom: [math]\displaystyle{ X  \mu / \sigma \sim \chi_1 }[/math].
 The square of [math]\displaystyle{ X/\sigma }[/math] has the noncentral chisquared distribution with one degree of freedom: [math]\displaystyle{ X^2 / \sigma^2 \sim \chi_1^2(\mu^2 / \sigma^2) }[/math]. If [math]\displaystyle{ \mu = 0 }[/math], the distribution is called simply chisquared.
 The loglikelihood of a normal variable [math]\displaystyle{ x }[/math] is simply the log of its probability density function: [math]\displaystyle{ \ln p(x)= \frac{1}{2} \left(\frac{x\mu}{\sigma} \right)^2 \ln \left(\sigma \sqrt{2\pi} \right). }[/math] Since this is a scaled and shifted square of a standard normal variable, it is distributed as a scaled and shifted chisquared variable.
 The distribution of the variable [math]\displaystyle{ X }[/math] restricted to an interval [math]\displaystyle{ [a, b] }[/math] is called the truncated normal distribution.
 [math]\displaystyle{ (X  \mu)^{2} }[/math] has a Lévy distribution with location 0 and scale [math]\displaystyle{ \sigma^{2} }[/math].
Operations on two independent normal variables
 If [math]\displaystyle{ X_1 }[/math] and [math]\displaystyle{ X_2 }[/math] are two independent normal random variables, with means [math]\displaystyle{ \mu_1 }[/math], [math]\displaystyle{ \mu_2 }[/math] and standard deviations [math]\displaystyle{ \sigma_1 }[/math], [math]\displaystyle{ \sigma_2 }[/math], then their sum [math]\displaystyle{ X_1 + X_2 }[/math] will also be normally distributed,^{[proof]} with mean [math]\displaystyle{ \mu_1 + \mu_2 }[/math] and variance [math]\displaystyle{ \sigma_1^2 + \sigma_2^2 }[/math].
 In particular, if [math]\displaystyle{ X }[/math] and [math]\displaystyle{ Y }[/math] are independent normal deviates with zero mean and variance [math]\displaystyle{ \sigma^2 }[/math], then [math]\displaystyle{ X + Y }[/math] and [math]\displaystyle{ X  Y }[/math] are also independent and normally distributed, with zero mean and variance [math]\displaystyle{ 2\sigma^2 }[/math]. This is a special case of the polarization identity.^{[39]}
 If [math]\displaystyle{ X_1 }[/math], [math]\displaystyle{ X_2 }[/math] are two independent normal deviates with mean [math]\displaystyle{ \mu }[/math] and deviation [math]\displaystyle{ \sigma }[/math], and [math]\displaystyle{ a }[/math], [math]\displaystyle{ b }[/math] are arbitrary real numbers, then the variable [math]\displaystyle{ X_3 = \frac{aX_1 + bX_2  (a+b)\mu}{\sqrt{a^2+b^2}} + \mu }[/math] is also normally distributed with mean [math]\displaystyle{ \mu }[/math] and deviation [math]\displaystyle{ \sigma }[/math]. It follows that the normal distribution is stable (with exponent [math]\displaystyle{ \alpha=2 }[/math]).
 If [math]\displaystyle{ X_k \sim \mathcal N(m_k, \sigma_k^2) }[/math], [math]\displaystyle{ k \in \{ 0, 1 \} }[/math] are normal distributions, then their normalized geometric mean [math]\displaystyle{ \frac{1}{\int_{\R^n} X_0^{\alpha}(x) X_1^{1  \alpha}(x) \, \text{d}x} X_0^{\alpha} X_1^{1  \alpha} }[/math] is a normal distribution [math]\displaystyle{ \mathcal N(m_{\alpha}, \sigma_{\alpha}^2) }[/math] with [math]\displaystyle{ m_{\alpha} = \frac{\alpha m_0 \sigma_1^2 + (1  \alpha) m_1 \sigma_0^2}{\alpha \sigma_1^2 + (1  \alpha) \sigma_0^2} }[/math] and [math]\displaystyle{ \sigma_{\alpha}^2 = \frac{\sigma_0^2 \sigma_1^2}{\alpha \sigma_1^2 + (1  \alpha) \sigma_0^2} }[/math] (see here for a visualization).
Operations on two independent standard normal variables
If [math]\displaystyle{ X_1 }[/math] and [math]\displaystyle{ X_2 }[/math] are two independent standard normal random variables with mean 0 and variance 1, then
 Their sum and difference is distributed normally with mean zero and variance two: [math]\displaystyle{ X_1 \pm X_2 \sim \mathcal{N}(0, 2) }[/math].
 Their product [math]\displaystyle{ Z = X_1 X_2 }[/math] follows the product distribution^{[40]} with density function [math]\displaystyle{ f_Z(z) = \pi^{1} K_0(z) }[/math] where [math]\displaystyle{ K_0 }[/math] is the modified Bessel function of the second kind. This distribution is symmetric around zero, unbounded at [math]\displaystyle{ z = 0 }[/math], and has the characteristic function [math]\displaystyle{ \phi_Z(t) = (1 + t^2)^{1/2} }[/math].
 Their ratio follows the standard Cauchy distribution: [math]\displaystyle{ X_1/ X_2 \sim \operatorname{Cauchy}(0, 1) }[/math].
 Their Euclidean norm [math]\displaystyle{ \sqrt{X_1^2 + X_2^2} }[/math] has the Rayleigh distribution.
Operations on multiple independent normal variables
 Any linear combination of independent normal deviates is a normal deviate.
 If [math]\displaystyle{ X_1, X_2, \ldots, X_n }[/math] are independent standard normal random variables, then the sum of their squares has the chisquared distribution with [math]\displaystyle{ n }[/math] degrees of freedom [math]\displaystyle{ X_1^2 + \cdots + X_n^2 \sim \chi_n^2. }[/math]
 If [math]\displaystyle{ X_1, X_2, \ldots, X_n }[/math] are independent normally distributed random variables with means [math]\displaystyle{ \mu }[/math] and variances [math]\displaystyle{ \sigma^2 }[/math], then their sample mean is independent from the sample standard deviation,^{[41]} which can be demonstrated using Basu's theorem or Cochran's theorem.^{[42]} The ratio of these two quantities will have the Student's tdistribution with [math]\displaystyle{ n1 }[/math] degrees of freedom: [math]\displaystyle{ t = \frac{\overline X  \mu}{S/\sqrt{n}} = \frac{\frac{1}{n}(X_1+\cdots+X_n)  \mu}{\sqrt{\frac{1}{n(n1)}\left[(X_1\overline X)^2 + \cdots+(X_n\overline X)^2\right]}} \sim t_{n1}. }[/math]
 If [math]\displaystyle{ X_1, X_2, \ldots, X_n }[/math], [math]\displaystyle{ Y_1, Y_2, \ldots, Y_m }[/math] are independent standard normal random variables, then the ratio of their normalized sums of squares will have the Fdistribution with (n, m) degrees of freedom:^{[43]} [math]\displaystyle{ F = \frac{\left(X_1^2+X_2^2+\cdots+X_n^2\right)/n}{\left(Y_1^2+Y_2^2+\cdots+Y_m^2\right)/m} \sim F_{n,m}. }[/math]
 A quadratic form of a normal vector, i.e. a quadratic function [math]\displaystyle{ q = \sum x_i^2 + \sum x_j + c }[/math] of multiple independent or correlated normal variables, is a generalized chisquare variable.
Operations on the density function
The split normal distribution is most directly defined in terms of joining scaled sections of the density functions of different normal distributions and rescaling the density to integrate to one. The truncated normal distribution results from rescaling a section of a single density function.
Infinite divisibility and Cramér's theorem
For any positive integer [math]\displaystyle{ \text{n} }[/math], any normal distribution with mean [math]\displaystyle{ \mu }[/math] and variance [math]\displaystyle{ \sigma^2 }[/math] is the distribution of the sum of [math]\displaystyle{ \text{n} }[/math] independent normal deviates, each with mean [math]\displaystyle{ \frac{\mu}{n} }[/math] and variance [math]\displaystyle{ \frac{\sigma^2}{n} }[/math]. This property is called infinite divisibility.^{[44]}
Conversely, if [math]\displaystyle{ X_1 }[/math] and [math]\displaystyle{ X_2 }[/math] are independent random variables and their sum [math]\displaystyle{ X_1+X_2 }[/math] has a normal distribution, then both [math]\displaystyle{ X_1 }[/math] and [math]\displaystyle{ X_2 }[/math] must be normal deviates.^{[45]}
This result is known as Cramér's decomposition theorem, and is equivalent to saying that the convolution of two distributions is normal if and only if both are normal. Cramér's theorem implies that a linear combination of independent nonGaussian variables will never have an exactly normal distribution, although it may approach it arbitrarily closely.^{[31]}
Bernstein's theorem
Bernstein's theorem states that if [math]\displaystyle{ X }[/math] and [math]\displaystyle{ Y }[/math] are independent and [math]\displaystyle{ X + Y }[/math] and [math]\displaystyle{ X  Y }[/math] are also independent, then both X and Y must necessarily have normal distributions.^{[46]}^{[47]}
More generally, if [math]\displaystyle{ X_1, \ldots, X_n }[/math] are independent random variables, then two distinct linear combinations [math]\displaystyle{ \sum{a_kX_k} }[/math] and [math]\displaystyle{ \sum{b_kX_k} }[/math]will be independent if and only if all [math]\displaystyle{ X_k }[/math] are normal and [math]\displaystyle{ \sum{a_kb_k\sigma_k^2=0} }[/math], where [math]\displaystyle{ \sigma_k^2 }[/math] denotes the variance of [math]\displaystyle{ X_k }[/math].^{[46]}
Extensions
The notion of normal distribution, being one of the most important distributions in probability theory, has been extended far beyond the standard framework of the univariate (that is onedimensional) case (Case 1). All these extensions are also called normal or Gaussian laws, so a certain ambiguity in names exists.
 The multivariate normal distribution describes the Gaussian law in the kdimensional Euclidean space. A vector X ∈ R^{k} is multivariatenormally distributed if any linear combination of its components Σkj=1a_{j} X_{j} has a (univariate) normal distribution. The variance of X is a k×k symmetric positivedefinite matrix V. The multivariate normal distribution is a special case of the elliptical distributions. As such, its isodensity loci in the k = 2 case are ellipses and in the case of arbitrary k are ellipsoids.
 Rectified Gaussian distribution a rectified version of normal distribution with all the negative elements reset to 0
 Complex normal distribution deals with the complex normal vectors. A complex vector X ∈ C^{k} is said to be normal if both its real and imaginary components jointly possess a 2kdimensional multivariate normal distribution. The variancecovariance structure of X is described by two matrices: the variance matrix Γ, and the relation matrix C.
 Matrix normal distribution describes the case of normally distributed matrices.
 Gaussian processes are the normally distributed stochastic processes. These can be viewed as elements of some infinitedimensional Hilbert space H, and thus are the analogues of multivariate normal vectors for the case k = ∞. A random element h ∈ H is said to be normal if for any constant a ∈ H the scalar product (a, h) has a (univariate) normal distribution. The variance structure of such Gaussian random element can be described in terms of the linear covariance operator K: H → H. Several Gaussian processes became popular enough to have their own names:
 Gaussian qdistribution is an abstract mathematical construction that represents a qanalogue of the normal distribution.
 the qGaussian is an analogue of the Gaussian distribution, in the sense that it maximises the Tsallis entropy, and is one type of Tsallis distribution. This distribution is different from the Gaussian qdistribution above.
 The Kaniadakis κGaussian distribution is a generalization of the Gaussian distribution which arises from the Kaniadakis statistics, being one of the Kaniadakis distributions.
A random variable X has a twopiece normal distribution if it has a distribution
 [math]\displaystyle{ f_X( x ) = N( \mu, \sigma_1^2 ) \text{ if } x \le \mu }[/math]
 [math]\displaystyle{ f_X( x ) = N( \mu, \sigma_2^2 ) \text{ if } x \ge \mu }[/math]
where μ is the mean and σ_{1} and σ_{2} are the standard deviations of the distribution to the left and right of the mean respectively.
The mean, variance and third central moment of this distribution have been determined^{[48]}
 [math]\displaystyle{ \operatorname{E}( X ) = \mu + \sqrt{\frac 2 \pi } ( \sigma_2  \sigma_1 ) }[/math]
 [math]\displaystyle{ \operatorname{V}( X ) = \left( 1  \frac 2 \pi\right)( \sigma_2  \sigma_1 )^2 + \sigma_1 \sigma_2 }[/math]
 [math]\displaystyle{ \operatorname{T}( X ) = \sqrt{ \frac 2 \pi}( \sigma_2  \sigma_1 ) \left[ \left( \frac 4 \pi  1 \right) ( \sigma_2  \sigma_1)^2 + \sigma_1 \sigma_2 \right] }[/math]
where E(X), V(X) and T(X) are the mean, variance, and third central moment respectively.
One of the main practical uses of the Gaussian law is to model the empirical distributions of many different random variables encountered in practice. In such case a possible extension would be a richer family of distributions, having more than two parameters and therefore being able to fit the empirical distribution more accurately. The examples of such extensions are:
 Pearson distribution — a fourparameter family of probability distributions that extend the normal law to include different skewness and kurtosis values.
 The generalized normal distribution, also known as the exponential power distribution, allows for distribution tails with thicker or thinner asymptotic behaviors.
Statistical inference
Estimation of parameters
It is often the case that we do not know the parameters of the normal distribution, but instead want to estimate them. That is, having a sample [math]\displaystyle{ (x_1, \ldots, x_n) }[/math] from a normal [math]\displaystyle{ \mathcal{N}(\mu, \sigma^2) }[/math] population we would like to learn the approximate values of parameters [math]\displaystyle{ \mu }[/math] and [math]\displaystyle{ \sigma^2 }[/math]. The standard approach to this problem is the maximum likelihood method, which requires maximization of the loglikelihood function:
 [math]\displaystyle{ \ln\mathcal{L}(\mu,\sigma^2) = \sum_{i=1}^n \ln f(x_i\mid\mu,\sigma^2) = \frac{n}{2}\ln(2\pi)  \frac{n}{2}\ln\sigma^2  \frac{1}{2\sigma^2}\sum_{i=1}^n (x_i\mu)^2. }[/math]
Taking derivatives with respect to [math]\displaystyle{ \mu }[/math] and [math]\displaystyle{ \sigma^2 }[/math] and solving the resulting system of first order conditions yields the maximum likelihood estimates:
 [math]\displaystyle{ \hat{\mu} = \overline{x} \equiv \frac{1}{n}\sum_{i=1}^n x_i, \qquad \hat{\sigma}^2 = \frac{1}{n} \sum_{i=1}^n (x_i  \overline{x})^2. }[/math]
Then [math]\displaystyle{ \ln\mathcal{L}(\hat{\mu},\hat{\sigma}^2) }[/math] is as follows:
 [math]\displaystyle{ \ln\mathcal{L}(\hat{\mu},\hat{\sigma}^2) = (n/2) [log(2 \pi \hat{\sigma}^2)+1] }[/math]
Sample mean
Estimator [math]\displaystyle{ \textstyle\hat\mu }[/math] is called the sample mean, since it is the arithmetic mean of all observations. The statistic [math]\displaystyle{ \textstyle\overline{x} }[/math] is complete and sufficient for [math]\displaystyle{ \mu }[/math], and therefore by the Lehmann–Scheffé theorem, [math]\displaystyle{ \textstyle\hat\mu }[/math] is the uniformly minimum variance unbiased (UMVU) estimator.^{[49]} In finite samples it is distributed normally:
 [math]\displaystyle{ \hat\mu \sim \mathcal{N}(\mu,\sigma^2/n). }[/math]
The variance of this estimator is equal to the μμelement of the inverse Fisher information matrix [math]\displaystyle{ \textstyle\mathcal{I}^{1} }[/math]. This implies that the estimator is finitesample efficient. Of practical importance is the fact that the standard error of [math]\displaystyle{ \textstyle\hat\mu }[/math] is proportional to [math]\displaystyle{ \textstyle1/\sqrt{n} }[/math], that is, if one wishes to decrease the standard error by a factor of 10, one must increase the number of points in the sample by a factor of 100. This fact is widely used in determining sample sizes for opinion polls and the number of trials in Monte Carlo simulations.
From the standpoint of the asymptotic theory, [math]\displaystyle{ \textstyle\hat\mu }[/math] is consistent, that is, it converges in probability to [math]\displaystyle{ \mu }[/math] as [math]\displaystyle{ n\rightarrow\infty }[/math]. The estimator is also asymptotically normal, which is a simple corollary of the fact that it is normal in finite samples:
 [math]\displaystyle{ \sqrt{n}(\hat\mu\mu) \,\xrightarrow{d}\, \mathcal{N}(0,\sigma^2). }[/math]
Sample variance
The estimator [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] is called the sample variance, since it is the variance of the sample ([math]\displaystyle{ (x_1, \ldots, x_n) }[/math]). In practice, another estimator is often used instead of the [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math]. This other estimator is denoted [math]\displaystyle{ s^2 }[/math], and is also called the sample variance, which represents a certain ambiguity in terminology; its square root [math]\displaystyle{ s }[/math] is called the sample standard deviation. The estimator [math]\displaystyle{ s^2 }[/math] differs from [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] by having (n − 1) instead of n in the denominator (the socalled Bessel's correction):
 [math]\displaystyle{ s^2 = \frac{n}{n1} \hat\sigma^2 = \frac{1}{n1} \sum_{i=1}^n (x_i  \overline{x})^2. }[/math]
The difference between [math]\displaystyle{ s^2 }[/math] and [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] becomes negligibly small for large n's. In finite samples however, the motivation behind the use of [math]\displaystyle{ s^2 }[/math] is that it is an unbiased estimator of the underlying parameter [math]\displaystyle{ \sigma^2 }[/math], whereas [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] is biased. Also, by the Lehmann–Scheffé theorem the estimator [math]\displaystyle{ s^2 }[/math] is uniformly minimum variance unbiased (UMVU),^{[49]} which makes it the "best" estimator among all unbiased ones. However it can be shown that the biased estimator [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] is better than the [math]\displaystyle{ s^2 }[/math] in terms of the mean squared error (MSE) criterion. In finite samples both [math]\displaystyle{ s^2 }[/math] and [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] have scaled chisquared distribution with (n − 1) degrees of freedom:
 [math]\displaystyle{ s^2 \sim \frac{\sigma^2}{n1} \cdot \chi^2_{n1}, \qquad \hat\sigma^2 \sim \frac{\sigma^2}{n} \cdot \chi^2_{n1}. }[/math]
The first of these expressions shows that the variance of [math]\displaystyle{ s^2 }[/math] is equal to [math]\displaystyle{ 2\sigma^4/(n1) }[/math], which is slightly greater than the σσelement of the inverse Fisher information matrix [math]\displaystyle{ \textstyle\mathcal{I}^{1} }[/math]. Thus, [math]\displaystyle{ s^2 }[/math] is not an efficient estimator for [math]\displaystyle{ \sigma^2 }[/math], and moreover, since [math]\displaystyle{ s^2 }[/math] is UMVU, we can conclude that the finitesample efficient estimator for [math]\displaystyle{ \sigma^2 }[/math] does not exist.
Applying the asymptotic theory, both estimators [math]\displaystyle{ s^2 }[/math] and [math]\displaystyle{ \textstyle\hat\sigma^2 }[/math] are consistent, that is they converge in probability to [math]\displaystyle{ \sigma^2 }[/math] as the sample size [math]\displaystyle{ n\rightarrow\infty }[/math]. The two estimators are also both asymptotically normal:
 [math]\displaystyle{ \sqrt{n}(\hat\sigma^2  \sigma^2) \simeq \sqrt{n}(s^2\sigma^2) \,\xrightarrow{d}\, \mathcal{N}(0,2\sigma^4). }[/math]
In particular, both estimators are asymptotically efficient for [math]\displaystyle{ \sigma^2 }[/math].
Confidence intervals
By Cochran's theorem, for normal distributions the sample mean [math]\displaystyle{ \textstyle\hat\mu }[/math] and the sample variance s^{2} are independent, which means there can be no gain in considering their joint distribution. There is also a converse theorem: if in a sample the sample mean and sample variance are independent, then the sample must have come from the normal distribution. The independence between [math]\displaystyle{ \textstyle\hat\mu }[/math] and s can be employed to construct the socalled tstatistic:
 [math]\displaystyle{ t = \frac{\hat\mu\mu}{s/\sqrt{n}} = \frac{\overline{x}\mu}{\sqrt{\frac{1}{n(n1)}\sum(x_i\overline{x})^2}} \sim t_{n1} }[/math]
This quantity t has the Student's tdistribution with (n − 1) degrees of freedom, and it is an ancillary statistic (independent of the value of the parameters). Inverting the distribution of this tstatistics will allow us to construct the confidence interval for μ;^{[50]} similarly, inverting the χ^{2} distribution of the statistic s^{2} will give us the confidence interval for σ^{2}:^{[51]}
 [math]\displaystyle{ \mu \in \left[ \hat\mu  t_{n1,1\alpha/2} \frac{1}{\sqrt{n}}s, \hat\mu + t_{n1,1\alpha/2} \frac{1}{\sqrt{n}}s \right], }[/math]
 [math]\displaystyle{ \sigma^2 \in \left[ \frac{(n1)s^2}{\chi^2_{n1,1\alpha/2}}, \frac{(n1)s^2}{\chi^2_{n1,\alpha/2}} \right], }[/math]
where t_{k,p} and χ 2
k,p are the pth quantiles of the t and χ^{2}distributions respectively. These confidence intervals are of the confidence level 1 − α, meaning that the true values μ and σ^{2} fall outside of these intervals with probability (or significance level) α. In practice people usually take α = 5%, resulting in the 95% confidence intervals.
Approximate formulas can be derived from the asymptotic distributions of [math]\displaystyle{ \textstyle\hat\mu }[/math] and s^{2}:
 [math]\displaystyle{ \mu \in \left[ \hat\mu  z_{\alpha/2}\frac{1}{\sqrt n}s, \hat\mu + z_{\alpha/2}\frac{1}{\sqrt n}s \right], }[/math]
 [math]\displaystyle{ \sigma^2 \in \left[ s^2  z_{\alpha/2}\frac{\sqrt{2}}{\sqrt{n}}s^2, s^2 + z_{\alpha/2}\frac{\sqrt{2}}{\sqrt{n}}s^2 \right], }[/math]
The approximate formulas become valid for large values of n, and are more convenient for the manual calculation since the standard normal quantiles z_{α/2} do not depend on n. In particular, the most popular value of α = 5%, results in z_{0.025} = 1.96.
Normality tests
Normality tests assess the likelihood that the given data set {x_{1}, ..., x_{n}} comes from a normal distribution. Typically the null hypothesis H_{0} is that the observations are distributed normally with unspecified mean μ and variance σ^{2}, versus the alternative H_{a} that the distribution is arbitrary. Many tests (over 40) have been devised for this problem. The more prominent of them are outlined below:
Diagnostic plots are more intuitively appealing but subjective at the same time, as they rely on informal human judgement to accept or reject the null hypothesis.
 Q–Q plot, also known as normal probability plot or rankit plot—is a plot of the sorted values from the data set against the expected values of the corresponding quantiles from the standard normal distribution. That is, it is a plot of point of the form (Φ^{−1}(p_{k}), x_{(k)}), where plotting points p_{k} are equal to p_{k} = (k − α)/(n + 1 − 2α) and α is an adjustment constant, which can be anything between 0 and 1. If the null hypothesis is true, the plotted points should approximately lie on a straight line.
 P–P plot – similar to the Q–Q plot, but used much less frequently. This method consists of plotting the points (Φ(z_{(k)}), p_{k}), where [math]\displaystyle{ \textstyle z_{(k)} = (x_{(k)}\hat\mu)/\hat\sigma }[/math]. For normally distributed data this plot should lie on a 45° line between (0, 0) and (1, 1).
Goodnessoffit tests:
Momentbased tests:
 D'Agostino's Ksquared test
 Jarque–Bera test
 Shapiro–Wilk test: This is based on the fact that the line in the Q–Q plot has the slope of σ. The test compares the least squares estimate of that slope with the value of the sample variance, and rejects the null hypothesis if these two quantities differ significantly.
Tests based on the empirical distribution function:
 Anderson–Darling test
 Lilliefors test (an adaptation of the Kolmogorov–Smirnov test)
Bayesian analysis of the normal distribution
Bayesian analysis of normally distributed data is complicated by the many different possibilities that may be considered:
 Either the mean, or the variance, or neither, may be considered a fixed quantity.
 When the variance is unknown, analysis may be done directly in terms of the variance, or in terms of the precision, the reciprocal of the variance. The reason for expressing the formulas in terms of precision is that the analysis of most cases is simplified.
 Both univariate and multivariate cases need to be considered.
 Either conjugate or improper prior distributions may be placed on the unknown variables.
 An additional set of cases occurs in Bayesian linear regression, where in the basic model the data is assumed to be normally distributed, and normal priors are placed on the regression coefficients. The resulting analysis is similar to the basic cases of independent identically distributed data.
The formulas for the nonlinearregression cases are summarized in the conjugate prior article.
Sum of two quadratics
Scalar form
The following auxiliary formula is useful for simplifying the posterior update equations, which otherwise become fairly tedious.
 [math]\displaystyle{ a(xy)^2 + b(xz)^2 = (a + b)\left(x  \frac{ay+bz}{a+b}\right)^2 + \frac{ab}{a+b}(yz)^2 }[/math]
This equation rewrites the sum of two quadratics in x by expanding the squares, grouping the terms in x, and completing the square. Note the following about the complex constant factors attached to some of the terms:
 The factor [math]\displaystyle{ \frac{ay+bz}{a+b} }[/math] has the form of a weighted average of y and z.
 [math]\displaystyle{ \frac{ab}{a+b} = \frac{1}{\frac{1}{a}+\frac{1}{b}} = (a^{1} + b^{1})^{1}. }[/math] This shows that this factor can be thought of as resulting from a situation where the reciprocals of quantities a and b add directly, so to combine a and b themselves, it is necessary to reciprocate, add, and reciprocate the result again to get back into the original units. This is exactly the sort of operation performed by the harmonic mean, so it is not surprising that [math]\displaystyle{ \frac{ab}{a+b} }[/math] is onehalf the harmonic mean of a and b.
Vector form
A similar formula can be written for the sum of two vector quadratics: If x, y, z are vectors of length k, and A and B are symmetric, invertible matrices of size [math]\displaystyle{ k\times k }[/math], then
 [math]\displaystyle{ \begin{align} & (\mathbf{y}\mathbf{x})'\mathbf{A}(\mathbf{y}\mathbf{x}) + (\mathbf{x}\mathbf{z})' \mathbf{B}(\mathbf{x}\mathbf{z}) \\ = {} & (\mathbf{x}  \mathbf{c})'(\mathbf{A}+\mathbf{B})(\mathbf{x}  \mathbf{c}) + (\mathbf{y}  \mathbf{z})'(\mathbf{A}^{1} + \mathbf{B}^{1})^{1}(\mathbf{y}  \mathbf{z}) \end{align} }[/math]
where
 [math]\displaystyle{ \mathbf{c} = (\mathbf{A} + \mathbf{B})^{1}(\mathbf{A}\mathbf{y} + \mathbf{B} \mathbf{z}) }[/math]
The form x′ A x is called a quadratic form and is a scalar:
 [math]\displaystyle{ \mathbf{x}'\mathbf{A}\mathbf{x} = \sum_{i,j}a_{ij} x_i x_j }[/math]
In other words, it sums up all possible combinations of products of pairs of elements from x, with a separate coefficient for each. In addition, since [math]\displaystyle{ x_i x_j = x_j x_i }[/math], only the sum [math]\displaystyle{ a_{ij} + a_{ji} }[/math] matters for any offdiagonal elements of A, and there is no loss of generality in assuming that A is symmetric. Furthermore, if A is symmetric, then the form [math]\displaystyle{ \mathbf{x}'\mathbf{A}\mathbf{y} = \mathbf{y}'\mathbf{A}\mathbf{x}. }[/math]
Sum of differences from the mean
Another useful formula is as follows: [math]\displaystyle{ \sum_{i=1}^n (x_i\mu)^2 = \sum_{i=1}^n (x_i\bar{x})^2 + n(\bar{x} \mu)^2 }[/math] where [math]\displaystyle{ \bar{x} = \frac{1}{n} \sum_{i=1}^n x_i. }[/math]
With known variance
For a set of i.i.d. normally distributed data points X of size n where each individual point x follows [math]\displaystyle{ x \sim \mathcal{N}(\mu, \sigma^2) }[/math] with known variance σ^{2}, the conjugate prior distribution is also normally distributed.
This can be shown more easily by rewriting the variance as the precision, i.e. using τ = 1/σ^{2}. Then if [math]\displaystyle{ x \sim \mathcal{N}(\mu, 1/\tau) }[/math] and [math]\displaystyle{ \mu \sim \mathcal{N}(\mu_0, 1/\tau_0), }[/math] we proceed as follows.
First, the likelihood function is (using the formula above for the sum of differences from the mean):
 [math]\displaystyle{ \begin{align} p(\mathbf{X}\mid\mu,\tau) &= \prod_{i=1}^n \sqrt{\frac{\tau}{2\pi}} \exp\left(\frac{1}{2}\tau(x_i\mu)^2\right) \\ &= \left(\frac{\tau}{2\pi}\right)^{n/2} \exp\left(\frac{1}{2}\tau \sum_{i=1}^n (x_i\mu)^2\right) \\ &= \left(\frac{\tau}{2\pi}\right)^{n/2} \exp\left[\frac{1}{2}\tau \left(\sum_{i=1}^n(x_i\bar{x})^2 + n(\bar{x} \mu)^2\right)\right]. \end{align} }[/math]
Then, we proceed as follows:
 [math]\displaystyle{ \begin{align} p(\mu\mid\mathbf{X}) &\propto p(\mathbf{X}\mid\mu) p(\mu) \\ & = \left(\frac{\tau}{2\pi}\right)^{n/2} \exp\left[\frac{1}{2}\tau \left(\sum_{i=1}^n(x_i\bar{x})^2 + n(\bar{x} \mu)^2\right)\right] \sqrt{\frac{\tau_0}{2\pi}} \exp\left(\frac{1}{2}\tau_0(\mu\mu_0)^2\right) \\ &\propto \exp\left(\frac{1}{2}\left(\tau\left(\sum_{i=1}^n(x_i\bar{x})^2 + n(\bar{x} \mu)^2\right) + \tau_0(\mu\mu_0)^2\right)\right) \\ &\propto \exp\left(\frac{1}{2} \left(n\tau(\bar{x}\mu)^2 + \tau_0(\mu\mu_0)^2 \right)\right) \\ &= \exp\left(\frac{1}{2}(n\tau + \tau_0)\left(\mu  \dfrac{n\tau \bar{x} + \tau_0\mu_0}{n\tau + \tau_0}\right)^2 + \frac{n\tau\tau_0}{n\tau+\tau_0}(\bar{x}  \mu_0)^2\right) \\ &\propto \exp\left(\frac{1}{2}(n\tau + \tau_0)\left(\mu  \dfrac{n\tau \bar{x} + \tau_0\mu_0}{n\tau + \tau_0}\right)^2\right) \end{align} }[/math]
In the above derivation, we used the formula above for the sum of two quadratics and eliminated all constant factors not involving μ. The result is the kernel of a normal distribution, with mean [math]\displaystyle{ \frac{n\tau \bar{x} + \tau_0\mu_0}{n\tau + \tau_0} }[/math] and precision [math]\displaystyle{ n\tau + \tau_0 }[/math], i.e.
 [math]\displaystyle{ p(\mu\mid\mathbf{X}) \sim \mathcal{N}\left(\frac{n\tau \bar{x} + \tau_0\mu_0}{n\tau + \tau_0}, \frac{1}{n\tau + \tau_0}\right) }[/math]
This can be written as a set of Bayesian update equations for the posterior parameters in terms of the prior parameters:
 [math]\displaystyle{ \begin{align} \tau_0' &= \tau_0 + n\tau \\[5pt] \mu_0' &= \frac{n\tau \bar{x} + \tau_0\mu_0}{n\tau + \tau_0} \\[5pt] \bar{x} &= \frac{1}{n}\sum_{i=1}^n x_i \end{align} }[/math]
That is, to combine n data points with total precision of nτ (or equivalently, total variance of n/σ^{2}) and mean of values [math]\displaystyle{ \bar{x} }[/math], derive a new total precision simply by adding the total precision of the data to the prior total precision, and form a new mean through a precisionweighted average, i.e. a weighted average of the data mean and the prior mean, each weighted by the associated total precision. This makes logical sense if the precision is thought of as indicating the certainty of the observations: In the distribution of the posterior mean, each of the input components is weighted by its certainty, and the certainty of this distribution is the sum of the individual certainties. (For the intuition of this, compare the expression "the whole is (or is not) greater than the sum of its parts". In addition, consider that the knowledge of the posterior comes from a combination of the knowledge of the prior and likelihood, so it makes sense that we are more certain of it than of either of its components.)
The above formula reveals why it is more convenient to do Bayesian analysis of conjugate priors for the normal distribution in terms of the precision. The posterior precision is simply the sum of the prior and likelihood precisions, and the posterior mean is computed through a precisionweighted average, as described above. The same formulas can be written in terms of variance by reciprocating all the precisions, yielding the more ugly formulas
 [math]\displaystyle{ \begin{align} {\sigma^2_0}' &= \frac{1}{\frac{n}{\sigma^2} + \frac{1}{\sigma_0^2}} \\[5pt] \mu_0' &= \frac{\frac{n\bar{x}}{\sigma^2} + \frac{\mu_0}{\sigma_0^2}}{\frac{n}{\sigma^2} + \frac{1}{\sigma_0^2}} \\[5pt] \bar{x} &= \frac{1}{n}\sum_{i=1}^n x_i \end{align} }[/math]
With known mean
For a set of i.i.d. normally distributed data points X of size n where each individual point x follows [math]\displaystyle{ x \sim \mathcal{N}(\mu, \sigma^2) }[/math] with known mean μ, the conjugate prior of the variance has an inverse gamma distribution or a scaled inverse chisquared distribution. The two are equivalent except for having different parameterizations. Although the inverse gamma is more commonly used, we use the scaled inverse chisquared for the sake of convenience. The prior for σ^{2} is as follows:
 [math]\displaystyle{ p(\sigma^2\mid\nu_0,\sigma_0^2) = \frac{(\sigma_0^2\frac{\nu_0}{2})^{\nu_0/2}}{\Gamma\left(\frac{\nu_0}{2} \right)}~\frac{\exp\left[ \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right]}{(\sigma^2)^{1+\frac{\nu_0}{2}}} \propto \frac{\exp\left[ \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right]}{(\sigma^2)^{1+\frac{\nu_0}{2}}} }[/math]
The likelihood function from above, written in terms of the variance, is:
 [math]\displaystyle{ \begin{align} p(\mathbf{X}\mid\mu,\sigma^2) &= \left(\frac{1}{2\pi\sigma^2}\right)^{n/2} \exp\left[\frac{1}{2\sigma^2} \sum_{i=1}^n (x_i\mu)^2\right] \\ &= \left(\frac{1}{2\pi\sigma^2}\right)^{n/2} \exp\left[\frac{S}{2\sigma^2}\right] \end{align} }[/math]
where
 [math]\displaystyle{ S = \sum_{i=1}^n (x_i\mu)^2. }[/math]
Then:
 [math]\displaystyle{ \begin{align} p(\sigma^2\mid\mathbf{X}) &\propto p(\mathbf{X}\mid\sigma^2) p(\sigma^2) \\ &= \left(\frac{1}{2\pi\sigma^2}\right)^{n/2} \exp\left[\frac{S}{2\sigma^2}\right] \frac{(\sigma_0^2\frac{\nu_0}{2})^{\frac{\nu_0}{2}}}{\Gamma\left(\frac{\nu_0}{2} \right)}~\frac{\exp\left[ \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right]}{(\sigma^2)^{1+\frac{\nu_0}{2}}} \\ &\propto \left(\frac{1}{\sigma^2}\right)^{n/2} \frac{1}{(\sigma^2)^{1+\frac{\nu_0}{2}}} \exp\left[\frac{S}{2\sigma^2} + \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right] \\ &= \frac{1}{(\sigma^2)^{1+\frac{\nu_0+n}{2}}} \exp\left[\frac{\nu_0 \sigma_0^2 + S}{2\sigma^2}\right] \end{align} }[/math]
The above is also a scaled inverse chisquared distribution where
 [math]\displaystyle{ \begin{align} \nu_0' &= \nu_0 + n \\ \nu_0'{\sigma_0^2}' &= \nu_0 \sigma_0^2 + \sum_{i=1}^n (x_i\mu)^2 \end{align} }[/math]
or equivalently
 [math]\displaystyle{ \begin{align} \nu_0' &= \nu_0 + n \\ {\sigma_0^2}' &= \frac{\nu_0 \sigma_0^2 + \sum_{i=1}^n (x_i\mu)^2}{\nu_0+n} \end{align} }[/math]
Reparameterizing in terms of an inverse gamma distribution, the result is:
 [math]\displaystyle{ \begin{align} \alpha' &= \alpha + \frac{n}{2} \\ \beta' &= \beta + \frac{\sum_{i=1}^n (x_i\mu)^2}{2} \end{align} }[/math]
With unknown mean and unknown variance
For a set of i.i.d. normally distributed data points X of size n where each individual point x follows [math]\displaystyle{ x \sim \mathcal{N}(\mu, \sigma^2) }[/math] with unknown mean μ and unknown variance σ^{2}, a combined (multivariate) conjugate prior is placed over the mean and variance, consisting of a normalinversegamma distribution. Logically, this originates as follows:
 From the analysis of the case with unknown mean but known variance, we see that the update equations involve sufficient statistics computed from the data consisting of the mean of the data points and the total variance of the data points, computed in turn from the known variance divided by the number of data points.
 From the analysis of the case with unknown variance but known mean, we see that the update equations involve sufficient statistics over the data consisting of the number of data points and sum of squared deviations.
 Keep in mind that the posterior update values serve as the prior distribution when further data is handled. Thus, we should logically think of our priors in terms of the sufficient statistics just described, with the same semantics kept in mind as much as possible.
 To handle the case where both mean and variance are unknown, we could place independent priors over the mean and variance, with fixed estimates of the average mean, total variance, number of data points used to compute the variance prior, and sum of squared deviations. Note however that in reality, the total variance of the mean depends on the unknown variance, and the sum of squared deviations that goes into the variance prior (appears to) depend on the unknown mean. In practice, the latter dependence is relatively unimportant: Shifting the actual mean shifts the generated points by an equal amount, and on average the squared deviations will remain the same. This is not the case, however, with the total variance of the mean: As the unknown variance increases, the total variance of the mean will increase proportionately, and we would like to capture this dependence.
 This suggests that we create a conditional prior of the mean on the unknown variance, with a hyperparameter specifying the mean of the pseudoobservations associated with the prior, and another parameter specifying the number of pseudoobservations. This number serves as a scaling parameter on the variance, making it possible to control the overall variance of the mean relative to the actual variance parameter. The prior for the variance also has two hyperparameters, one specifying the sum of squared deviations of the pseudoobservations associated with the prior, and another specifying once again the number of pseudoobservations. Each of the priors has a hyperparameter specifying the number of pseudoobservations, and in each case this controls the relative variance of that prior. These are given as two separate hyperparameters so that the variance (aka the confidence) of the two priors can be controlled separately.
 This leads immediately to the normalinversegamma distribution, which is the product of the two distributions just defined, with conjugate priors used (an inverse gamma distribution over the variance, and a normal distribution over the mean, conditional on the variance) and with the same four parameters just defined.
The priors are normally defined as follows:
 [math]\displaystyle{ \begin{align} p(\mu\mid\sigma^2; \mu_0, n_0) &\sim \mathcal{N}(\mu_0,\sigma^2/n_0) \\ p(\sigma^2; \nu_0,\sigma_0^2) &\sim I\chi^2(\nu_0,\sigma_0^2) = IG(\nu_0/2, \nu_0\sigma_0^2/2) \end{align} }[/math]
The update equations can be derived, and look as follows:
 [math]\displaystyle{ \begin{align} \bar{x} &= \frac 1 n \sum_{i=1}^n x_i \\ \mu_0' &= \frac{n_0\mu_0 + n\bar{x}}{n_0 + n} \\ n_0' &= n_0 + n \\ \nu_0' &= \nu_0 + n \\ \nu_0'{\sigma_0^2}' &= \nu_0 \sigma_0^2 + \sum_{i=1}^n (x_i\bar{x})^2 + \frac{n_0 n}{n_0 + n}(\mu_0  \bar{x})^2 \end{align} }[/math]
The respective numbers of pseudoobservations add the number of actual observations to them. The new mean hyperparameter is once again a weighted average, this time weighted by the relative numbers of observations. Finally, the update for [math]\displaystyle{ \nu_0'{\sigma_0^2}' }[/math] is similar to the case with known mean, but in this case the sum of squared deviations is taken with respect to the observed data mean rather than the true mean, and as a result a new interaction term needs to be added to take care of the additional error source stemming from the deviation between prior and data mean.
The prior distributions are
 [math]\displaystyle{ \begin{align} p(\mu\mid\sigma^2; \mu_0, n_0) &\sim \mathcal{N}(\mu_0,\sigma^2/n_0) = \frac{1}{\sqrt{2\pi\frac{\sigma^2}{n_0}}} \exp\left(\frac{n_0}{2\sigma^2}(\mu\mu_0)^2\right) \\ &\propto (\sigma^2)^{1/2} \exp\left(\frac{n_0}{2\sigma^2}(\mu\mu_0)^2\right) \\ p(\sigma^2; \nu_0,\sigma_0^2) &\sim I\chi^2(\nu_0,\sigma_0^2) = IG(\nu_0/2, \nu_0\sigma_0^2/2) \\ &= \frac{(\sigma_0^2\nu_0/2)^{\nu_0/2}}{\Gamma(\nu_0/2)}~\frac{\exp\left[ \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right]}{(\sigma^2)^{1+\nu_0/2}} \\ &\propto {(\sigma^2)^{(1+\nu_0/2)}} \exp\left[ \frac{\nu_0 \sigma_0^2}{2 \sigma^2}\right]. \end{align} }[/math]
Therefore, the joint prior is
 [math]\displaystyle{ \begin{align} p(\mu,\sigma^2; \mu_0, n_0, \nu_0,\sigma_0^2) &= p(\mu\mid\sigma^2; \mu_0, n_0)\,p(\sigma^2; \nu_0,\sigma_0^2) \\ &\propto (\sigma^2)^{(\nu_0+3)/2} \exp\left[\frac 1 {2\sigma^2}\left(\nu_0\sigma_0^2 + n_0(\mu\mu_0)^2\right)\right]. \end{align} }[/math]
The likelihood function from the section above with known variance is:
 [math]\displaystyle{ \begin{align} p(\mathbf{X}\mid\mu,\sigma^2) &= \left(\frac{1}{2\pi\sigma^2}\right)^{n/2} \exp\left[\frac{1}{2\sigma^2} \left(\sum_{i=1}^n(x_i \mu)^2\right)\right] \end{align} }[/math]
Writing it in terms of variance rather than precision, we get:
 [math]\displaystyle{ \begin{align} p(\mathbf{X}\mid\mu,\sigma^2) &= \left(\frac{1}{2\pi\sigma^2}\right)^{n/2} \exp\left[\frac{1}{2\sigma^2} \left(\sum_{i=1}^n(x_i\bar{x})^2 + n(\bar{x} \mu)^2\right)\right] \\ &\propto {\sigma^2}^{n/2} \exp\left[\frac{1}{2\sigma^2} \left(S + n(\bar{x} \mu)^2\right)\right] \end{align} }[/math]
where [math]\displaystyle{ S = \sum_{i=1}^n(x_i\bar{x})^2. }[/math]
Therefore, the posterior is (dropping the hyperparameters as conditioning factors):
 [math]\displaystyle{ \begin{align} p(\mu,\sigma^2\mid\mathbf{X}) & \propto p(\mu,\sigma^2) \, p(\mathbf{X}\mid\mu,\sigma^2) \\ & \propto (\sigma^2)^{(\nu_0+3)/2} \exp\left[\frac{1}{2\sigma^2}\left(\nu_0\sigma_0^2 + n_0(\mu\mu_0)^2\right)\right] {\sigma^2}^{n/2} \exp\left[\frac{1}{2\sigma^2} \left(S + n(\bar{x} \mu)^2\right)\right] \\ &= (\sigma^2)^{(\nu_0+n+3)/2} \exp\left[\frac{1}{2\sigma^2}\left(\nu_0\sigma_0^2 + S + n_0(\mu\mu_0)^2 + n(\bar{x} \mu)^2\right)\right] \\ &= (\sigma^2)^{(\nu_0+n+3)/2} \exp\left[\frac{1}{2\sigma^2}\left(\nu_0\sigma_0^2 + S + \frac{n_0 n}{n_0+n}(\mu_0\bar{x})^2 + (n_0+n)\left(\mu\frac{n_0\mu_0 + n\bar{x}}{n_0 + n}\right)^2\right)\right] \\ & \propto (\sigma^2)^{1/2} \exp\left[\frac{n_0+n}{2\sigma^2}\left(\mu\frac{n_0\mu_0 + n\bar{x}}{n_0 + n}\right)^2\right] \\ & \quad\times (\sigma^2)^{(\nu_0/2+n/2+1)} \exp\left[\frac{1}{2\sigma^2}\left(\nu_0\sigma_0^2 + S + \frac{n_0 n}{n_0+n}(\mu_0\bar{x})^2\right)\right] \\ & = \mathcal{N}_{\mu\mid\sigma^2}\left(\frac{n_0\mu_0 + n\bar{x}}{n_0 + n}, \frac{\sigma^2}{n_0+n}\right) \cdot {\rm IG}_{\sigma^2}\left(\frac12(\nu_0+n), \frac12\left(\nu_0\sigma_0^2 + S + \frac{n_0 n}{n_0+n}(\mu_0\bar{x})^2\right)\right). \end{align} }[/math]
In other words, the posterior distribution has the form of a product of a normal distribution over [math]\displaystyle{ p(\mu\sigma^2) }[/math] times an inverse gamma distribution over [math]\displaystyle{ p(\sigma^2) }[/math], with parameters that are the same as the update equations above.
Occurrence and applications
The occurrence of normal distribution in practical problems can be loosely classified into four categories:
 Exactly normal distributions;
 Approximately normal laws, for example when such approximation is justified by the central limit theorem; and
 Distributions modeled as normal – the normal distribution being the distribution with maximum entropy for a given mean and variance.
 Regression problems – the normal distribution being found after systematic effects have been modeled sufficiently well.
Exact normality
Certain quantities in physics are distributed normally, as was first demonstrated by James Clerk Maxwell. Examples of such quantities are:
 Probability density function of a ground state in a quantum harmonic oscillator.
 The position of a particle that experiences diffusion. If initially the particle is located at a specific point (that is its probability distribution is the Dirac delta function), then after time t its location is described by a normal distribution with variance t, which satisfies the diffusion equation [math]\displaystyle{ \frac{\partial}{\partial t} f(x,t) = \frac{1}{2} \frac{\partial^2}{\partial x^2} f(x,t) }[/math]. If the initial location is given by a certain density function [math]\displaystyle{ g(x) }[/math], then the density at time t is the convolution of g and the normal probability density function.
Approximate normality
Approximately normal distributions occur in many situations, as explained by the central limit theorem. When the outcome is produced by many small effects acting additively and independently, its distribution will be close to normal. The normal approximation will not be valid if the effects act multiplicatively (instead of additively), or if there is a single external influence that has a considerably larger magnitude than the rest of the effects.
 In counting problems, where the central limit theorem includes a discretetocontinuum approximation and where infinitely divisible and decomposable distributions are involved, such as
 Binomial random variables, associated with binary response variables;
 Poisson random variables, associated with rare events;
 Thermal radiation has a Bose–Einstein distribution on very short time scales, and a normal distribution on longer timescales due to the central limit theorem.
Assumed normality
I can only recognize the occurrence of the normal curve – the Laplacian curve of errors – as a very abnormal phenomenon. It is roughly approximated to in certain distributions; for this reason, and on account for its beautiful simplicity, we may, perhaps, use it as a first approximation, particularly in theoretical investigations.—(Pearson 1901 )
There are statistical methods to empirically test that assumption; see the above Normality tests section.
 In biology, the logarithm of various variables tend to have a normal distribution, that is, they tend to have a lognormal distribution (after separation on male/female subpopulations), with examples including:
 Measures of size of living tissue (length, height, skin area, weight);^{[52]}
 The length of inert appendages (hair, claws, nails, teeth) of biological specimens, in the direction of growth; presumably the thickness of tree bark also falls under this category;
 Certain physiological measurements, such as blood pressure of adult humans.
 In finance, in particular the Black–Scholes model, changes in the logarithm of exchange rates, price indices, and stock market indices are assumed normal (these variables behave like compound interest, not like simple interest, and so are multiplicative). Some mathematicians such as Benoit Mandelbrot have argued that logLevy distributions, which possesses heavy tails would be a more appropriate model, in particular for the analysis for stock market crashes. The use of the assumption of normal distribution occurring in financial models has also been criticized by Nassim Nicholas Taleb in his works.
 Measurement errors in physical experiments are often modeled by a normal distribution. This use of a normal distribution does not imply that one is assuming the measurement errors are normally distributed, rather using the normal distribution produces the most conservative predictions possible given only knowledge about the mean and variance of the errors.^{[53]}
 In standardized testing, results can be made to have a normal distribution by either selecting the number and difficulty of questions (as in the IQ test) or transforming the raw test scores into output scores by fitting them to the normal distribution. For example, the SAT's traditional range of 200–800 is based on a normal distribution with a mean of 500 and a standard deviation of 100.
 Many scores are derived from the normal distribution, including percentile ranks (percentiles or quantiles), normal curve equivalents, stanines, zscores, and Tscores. Additionally, some behavioral statistical procedures assume that scores are normally distributed; for example, ttests and ANOVAs. Bell curve grading assigns relative grades based on a normal distribution of scores.
 In hydrology the distribution of long duration river discharge or rainfall, e.g. monthly and yearly totals, is often thought to be practically normal according to the central limit theorem.^{[54]} The blue picture, made with CumFreq, illustrates an example of fitting the normal distribution to ranked October rainfalls showing the 90% confidence belt based on the binomial distribution. The rainfall data are represented by plotting positions as part of the cumulative frequency analysis.
Methodological problems and peer review
John Ioannidis argued that using normally distributed standard deviations as standards for validating research findings leave falsifiable predictions about phenomena that are not normally distributed untested. This includes, for example, phenomena that only appear when all necessary conditions are present and one cannot be a substitute for another in an additionlike way and phenomena that are not randomly distributed. Ioannidis argues that standard deviationcentered validation gives a false appearance of validity to hypotheses and theories where some but not all falsifiable predictions are normally distributed since the portion of falsifiable predictions that there is evidence against may and in some cases are in the nonnormally distributed parts of the range of falsifiable predictions, as well as baselessly dismissing hypotheses for which none of the falsifiable predictions are normally distributed as if were they unfalsifiable when in fact they do make falsifiable predictions. It is argued by Ioannidis that many cases of mutually exclusive theories being accepted as validated by research journals are caused by failure of the journals to take in empirical falsifications of nonnormally distributed predictions, and not because mutually exclusive theories are true, which they cannot be, although two mutually exclusive theories can both be wrong and a third one correct.^{[55]}
Computational methods
Generating values from normal distribution
In computer simulations, especially in applications of the MonteCarlo method, it is often desirable to generate values that are normally distributed. The algorithms listed below all generate the standard normal deviates, since a N(μ, σ^{2}) can be generated as X = μ + σZ, where Z is standard normal. All these algorithms rely on the availability of a random number generator U capable of producing uniform random variates.
 The most straightforward method is based on the probability integral transform property: if U is distributed uniformly on (0,1), then Φ^{−1}(U) will have the standard normal distribution. The drawback of this method is that it relies on calculation of the probit function Φ^{−1}, which cannot be done analytically. Some approximate methods are described in (Hart 1968 ) and in the erf article. Wichura gives a fast algorithm for computing this function to 16 decimal places,^{[56]} which is used by R to compute random variates of the normal distribution.
 An easytoprogram approximate approach that relies on the central limit theorem is as follows: generate 12 uniform U(0,1) deviates, add them all up, and subtract 6 – the resulting random variable will have approximately standard normal distribution. In truth, the distribution will be Irwin–Hall, which is a 12section eleventhorder polynomial approximation to the normal distribution. This random deviate will have a limited range of (−6, 6).^{[57]} Note that in a true normal distribution, only 0.00034% of all samples will fall outside ±6σ.
 The Box–Muller method uses two independent random numbers U and V distributed uniformly on (0,1). Then the two random variables X and Y [math]\displaystyle{ X = \sqrt{ 2 \ln U} \, \cos(2 \pi V) , \qquad Y = \sqrt{ 2 \ln U} \, \sin(2 \pi V) . }[/math] will both have the standard normal distribution, and will be independent. This formulation arises because for a bivariate normal random vector (X, Y) the squared norm X^{2} + Y^{2} will have the chisquared distribution with two degrees of freedom, which is an easily generated exponential random variable corresponding to the quantity −2 ln(U) in these equations; and the angle is distributed uniformly around the circle, chosen by the random variable V.
 The Marsaglia polar method is a modification of the Box–Muller method which does not require computation of the sine and cosine functions. In this method, U and V are drawn from the uniform (−1,1) distribution, and then S = U^{2} + V^{2} is computed. If S is greater or equal to 1, then the method starts over, otherwise the two quantities [math]\displaystyle{ X = U\sqrt{\frac{2\ln S}{S}}, \qquad Y = V\sqrt{\frac{2\ln S}{S}} }[/math] are returned. Again, X and Y are independent, standard normal random variables.
 The Ratio method^{[58]} is a rejection method. The algorithm proceeds as follows:
 Generate two independent uniform deviates U and V;
 Compute X = √8/e (V − 0.5)/U;
 Optional: if X^{2} ≤ 5 − 4e^{1/4}U then accept X and terminate algorithm;
 Optional: if X^{2} ≥ 4e^{−1.35}/U + 1.4 then reject X and start over from step 1;
 If X^{2} ≤ −4 lnU then accept X, otherwise start over the algorithm.
 The two optional steps allow the evaluation of the logarithm in the last step to be avoided in most cases. These steps can be greatly improved^{[59]} so that the logarithm is rarely evaluated.
 The ziggurat algorithm^{[60]} is faster than the Box–Muller transform and still exact. In about 97% of all cases it uses only two random numbers, one random integer and one random uniform, one multiplication and an iftest. Only in 3% of the cases, where the combination of those two falls outside the "core of the ziggurat" (a kind of rejection sampling using logarithms), do exponentials and more uniform random numbers have to be employed.
 Integer arithmetic can be used to sample from the standard normal distribution.^{[61]} This method is exact in the sense that it satisfies the conditions of ideal approximation;^{[62]} i.e., it is equivalent to sampling a real number from the standard normal distribution and rounding this to the nearest representable floating point number.
 There is also some investigation^{[63]} into the connection between the fast Hadamard transform and the normal distribution, since the transform employs just addition and subtraction and by the central limit theorem random numbers from almost any distribution will be transformed into the normal distribution. In this regard a series of Hadamard transforms can be combined with random permutations to turn arbitrary data sets into a normally distributed data.
Numerical approximations for the normal cumulative distribution function and normal quantile function
The standard normal cumulative distribution function is widely used in scientific and statistical computing.
The values Φ(x) may be approximated very accurately by a variety of methods, such as numerical integration, Taylor series, asymptotic series and continued fractions. Different approximations are used depending on the desired level of accuracy.
 (Zelen Severo ) give the approximation for Φ(x) for x > 0 with the absolute error ε(x) < 7.5·10^{−8} (algorithm 26.2.17): [math]\displaystyle{ \Phi(x) = 1  \varphi(x)\left(b_1 t + b_2 t^2 + b_3t^3 + b_4 t^4 + b_5 t^5\right) + \varepsilon(x), \qquad t = \frac{1}{1+b_0x}, }[/math] where ϕ(x) is the standard normal probability density function, and b_{0} = 0.2316419, b_{1} = 0.319381530, b_{2} = −0.356563782, b_{3} = 1.781477937, b_{4} = −1.821255978, b_{5} = 1.330274429.
 (Hart 1968 ) lists some dozens of approximations – by means of rational functions, with or without exponentials – for the erfc() function. His algorithms vary in the degree of complexity and the resulting precision, with maximum absolute precision of 24 digits. An algorithm by (West 2009 ) combines Hart's algorithm 5666 with a continued fraction approximation in the tail to provide a fast computation algorithm with a 16digit precision.
 (Cody 1969 ) after recalling Hart68 solution is not suited for erf, gives a solution for both erf and erfc, with maximal relative error bound, via Rational Chebyshev Approximation.
 (Marsaglia 2004 ) suggested a simple algorithm^{[note 1]} based on the Taylor series expansion [math]\displaystyle{ \Phi(x) = \frac12 + \varphi(x)\left( x + \frac{x^3} 3 + \frac{x^5}{3 \cdot 5} + \frac{x^7}{3 \cdot 5 \cdot 7} + \frac{x^9}{3 \cdot 5 \cdot 7 \cdot 9} + \cdots \right) }[/math] for calculating Φ(x) with arbitrary precision. The drawback of this algorithm is comparatively slow calculation time (for example it takes over 300 iterations to calculate the function with 16 digits of precision when x = 10).
 The GNU Scientific Library calculates values of the standard normal cumulative distribution function using Hart's algorithms and approximations with Chebyshev polynomials.
 (Dia 2023 ) proposes the following approximation of [math]\displaystyle{ 1\Phi }[/math] with a maximum relative error less than [math]\displaystyle{ 2^{53} }[/math] [math]\displaystyle{ \left(\approx 1.1 \times 10^{16}\right) }[/math] in absolute value: for [math]\displaystyle{ x \ge 0 }[/math][math]\displaystyle{ \begin{aligned} 1\Phi\left(x\right) & = \left(\frac{0.39894228040143268}{x+2.92678600515804815}\right) \left(\frac{x^2+8.42742300458043240 x+18.38871225773938487}{x^2+5.81582518933527391 x+8.97280659046817350} \right) \\ & \left(\frac{x^2+7.30756258553673541 x+18.25323235347346525}{x^2+5.70347935898051437 x+10.27157061171363079}\right) \left(\frac{x^2+5.66479518878470765 x+18.61193318971775795}{x^2+5.51862483025707963 x+12.72323261907760928}\right) \\ & \left( \frac{x^2+4.91396098895240075 x+24.14804072812762821}{x^2+5.26184239579604207 x+16.88639562007936908}\right) \left( \frac{x^2+3.83362947800146179 x+11.61511226260603247}{x^2+4.92081346632882033 x+24.12333774572479110}\right) e^{\frac{x^2}{2}} \end{aligned} }[/math] and for [math]\displaystyle{ x\lt 0 }[/math],
[math]\displaystyle{ 1\Phi\left(x\right) = 1\left(1\Phi\left(x\right)\right) }[/math]
Shore (1982) introduced simple approximations that may be incorporated in stochastic optimization models of engineering and operations research, like reliability engineering and inventory analysis. Denoting p = Φ(z), the simplest approximation for the quantile function is: [math]\displaystyle{ z = \Phi^{1}(p)=5.5556\left[1 \left( \frac{1p} p \right)^{0.1186}\right],\qquad p\ge 1/2 }[/math]
This approximation delivers for z a maximum absolute error of 0.026 (for 0.5 ≤ p ≤ 0.9999, corresponding to 0 ≤ z ≤ 3.719). For p < 1/2 replace p by 1 − p and change sign. Another approximation, somewhat less accurate, is the singleparameter approximation: [math]\displaystyle{ z=0.4115\left\{ \frac{1p} p + \log \left[ \frac{1p} p \right]  1 \right\}, \qquad p\ge 1/2 }[/math]
The latter had served to derive a simple approximation for the loss integral of the normal distribution, defined by [math]\displaystyle{ \begin{align} L(z) & =\int_z^\infty (uz)\varphi(u) \, du=\int_z^\infty [1\Phi (u)] \, du \\[5pt] L(z) & \approx \begin{cases} 0.4115\left(\dfrac p {1p} \right)  z, & p\lt 1/2, \\ \\ 0.4115\left( \dfrac {1p} p \right), & p\ge 1/2. \end{cases} \\[5pt] \text{or, equivalently,} \\ L(z) & \approx \begin{cases} 0.4115\left\{ 1\log \left[ \frac p {1p} \right] \right\}, & p \lt 1/2, \\ \\ 0.4115 \dfrac{1p} p, & p\ge 1/2. \end{cases} \end{align} }[/math]
This approximation is particularly accurate for the right fartail (maximum error of 10^{−3} for z≥1.4). Highly accurate approximations for the cumulative distribution function, based on Response Modeling Methodology (RMM, Shore, 2011, 2012), are shown in Shore (2005).
Some more approximations can be found at: Error function. In particular, small relative error on the whole domain for the cumulative distribution function [math]\displaystyle{ \Phi }[/math] and the quantile function [math]\displaystyle{ \Phi^{1} }[/math] as well, is achieved via an explicitly invertible formula by Sergei Winitzki in 2008.
History
Development
Some authors^{[64]}^{[65]} attribute the credit for the discovery of the normal distribution to de Moivre, who in 1738^{[note 2]} published in the second edition of his The Doctrine of Chances the study of the coefficients in the binomial expansion of (a + b)^{n}. De Moivre proved that the middle term in this expansion has the approximate magnitude of [math]\displaystyle{ 2^n/\sqrt{2\pi n} }[/math], and that "If m or 1/2n be a Quantity infinitely great, then the Logarithm of the Ratio, which a Term distant from the middle by the Interval ℓ, has to the middle Term, is [math]\displaystyle{ \frac{2\ell\ell}{n} }[/math]."^{[66]} Although this theorem can be interpreted as the first obscure expression for the normal probability law, Stigler points out that de Moivre himself did not interpret his results as anything more than the approximate rule for the binomial coefficients, and in particular de Moivre lacked the concept of the probability density function.^{[67]}
In 1823 Gauss published his monograph "Theoria combinationis observationum erroribus minimis obnoxiae" where among other things he introduces several important statistical concepts, such as the method of least squares, the method of maximum likelihood, and the normal distribution. Gauss used M, M′, M′′, ... to denote the measurements of some unknown quantity V, and sought the most probable estimator of that quantity: the one that maximizes the probability φ(M − V) · φ(M′ − V) · φ(M′′ − V) · ... of obtaining the observed experimental results. In his notation φΔ is the probability density function of the measurement errors of magnitude Δ. Not knowing what the function φ is, Gauss requires that his method should reduce to the wellknown answer: the arithmetic mean of the measured values.^{[note 3]} Starting from these principles, Gauss demonstrates that the only law that rationalizes the choice of arithmetic mean as an estimator of the location parameter, is the normal law of errors:^{[68]} [math]\displaystyle{ \varphi\mathit{\Delta} = \frac h {\surd\pi} \, e^{\mathrm{hh}\Delta\Delta}, }[/math] where h is "the measure of the precision of the observations". Using this normal law as a generic model for errors in the experiments, Gauss formulates what is now known as the nonlinear weighted least squares method.^{[69]}
Although Gauss was the first to suggest the normal distribution law, Laplace made significant contributions.^{[note 4]} It was Laplace who first posed the problem of aggregating several observations in 1774,^{[70]} although his own solution led to the Laplacian distribution. It was Laplace who first calculated the value of the integral ∫ e^{−t2} dt = √π in 1782, providing the normalization constant for the normal distribution.^{[71]} Finally, it was Laplace who in 1810 proved and presented to the Academy the fundamental central limit theorem, which emphasized the theoretical importance of the normal distribution.^{[72]}
It is of interest to note that in 1809 an IrishAmerican mathematician Robert Adrain published two insightful but flawed derivations of the normal probability law, simultaneously and independently from Gauss.^{[73]} His works remained largely unnoticed by the scientific community, until in 1871 they were exhumed by Abbe.^{[74]}
In the middle of the 19th century Maxwell demonstrated that the normal distribution is not just a convenient mathematical tool, but may also occur in natural phenomena:^{[75]} The number of particles whose velocity, resolved in a certain direction, lies between x and x + dx is [math]\displaystyle{ \operatorname{N} \frac{1}{\alpha\;\sqrt\pi}\; e^{\frac{x^2}{\alpha^2}} \, dx }[/math]
Naming
Today, the concept is usually known in English as the normal distribution or Gaussian distribution. Other less common names include Gauss distribution, LaplaceGauss distribution, the law of error, the law of facility of errors, Laplace's second law, and Gaussian law.
Gauss himself apparently coined the term with reference to the "normal equations" involved in its applications, with normal having its technical meaning of orthogonal rather than usual.^{[76]} However, by the end of the 19th century some authors^{[note 5]} had started using the name normal distribution, where the word "normal" was used as an adjective – the term now being seen as a reflection of the fact that this distribution was seen as typical, common – and thus normal. Peirce (one of those authors) once defined "normal" thus: "...the 'normal' is not the average (or any other kind of mean) of what actually occurs, but of what would, in the long run, occur under certain circumstances."^{[77]} Around the turn of the 20th century Pearson popularized the term normal as a designation for this distribution.^{[78]}
Many years ago I called the Laplace–Gaussian curve the normal curve, which name, while it avoids an international question of priority, has the disadvantage of leading people to believe that all other distributions of frequency are in one sense or another 'abnormal'.—(Pearson 1920 )
Also, it was Pearson who first wrote the distribution in terms of the standard deviation σ as in modern notation. Soon after this, in year 1915, Fisher added the location parameter to the formula for normal distribution, expressing it in the way it is written nowadays: [math]\displaystyle{ df = \frac{1}{\sqrt{2\sigma^2\pi}} e^{(x  m)^2/(2\sigma^2)} \, dx. }[/math]
The term "standard normal", which denotes the normal distribution with zero mean and unit variance came into general use around the 1950s, appearing in the popular textbooks by P. G. Hoel (1947) Introduction to Mathematical Statistics and A. M. Mood (1950) Introduction to the Theory of Statistics.^{[79]}
See also
 Bates distribution – similar to the Irwin–Hall distribution, but rescaled back into the 0 to 1 range
 Behrens–Fisher problem – the longstanding problem of testing whether two normal samples with different variances have same means;
 Bhattacharyya distance – method used to separate mixtures of normal distributions
 Erdős–Kac theorem – on the occurrence of the normal distribution in number theory
 Full width at half maximum
 Gaussian blur – convolution, which uses the normal distribution as a kernel
 Modified halfnormal distribution^{[80]} with the pdf on [math]\displaystyle{ (0, \infty) }[/math] is given as [math]\displaystyle{ f(x)= \frac{2\beta^{\frac{\alpha}{2}} x^{\alpha1} \exp(\beta x^2+ \gamma x )}{\Psi{\left(\frac{\alpha}{2}, \frac{ \gamma}{\sqrt{\beta}}\right)}} }[/math], where [math]\displaystyle{ \Psi(\alpha,z)={}_1\Psi_1\left(\begin{matrix}\left(\alpha,\frac{1}{2}\right)\\(1,0)\end{matrix};z \right) }[/math] denotes the Fox–Wright Psi function.
 Normally distributed and uncorrelated does not imply independent
 Ratio normal distribution
 Reciprocal normal distribution
 Standard normal table
 Stein's lemma
 SubGaussian distribution
 Sum of normally distributed random variables
 Tweedie distribution – The normal distribution is a member of the family of Tweedie exponential dispersion models.
 Wrapped normal distribution – the Normal distribution applied to a circular domain
 Ztest – using the normal distribution
Notes
 ↑ For example, this algorithm is given in the article Bc programming language.
 ↑ De Moivre first published his findings in 1733, in a pamphlet Approximatio ad Summam Terminorum Binomii (a + b)^{}n in Seriem Expansi that was designated for private circulation only. But it was not until the year 1738 that he made his results publicly available. The original pamphlet was reprinted several times, see for example (Walker 1985 ).
 ↑ "It has been customary certainly to regard as an axiom the hypothesis that if any quantity has been determined by several direct observations, made under the same circumstances and with equal care, the arithmetical mean of the observed values affords the most probable value, if not rigorously, yet very nearly at least, so that it is always most safe to adhere to it." — (Gauss 1809 )
 ↑ "My custom of terming the curve the Gauss–Laplacian or normal curve saves us from proportioning the merit of discovery between the two great astronomer mathematicians." quote from (Pearson 1905 )
 ↑ Besides those specifically referenced here, such use is encountered in the works of Peirce, Galton ((Galton 1889 )) and Lexis (( Lexis 1878 ), (Rohrbasser Véron )) c. 1875.^{[citation needed]}
References
Citations
 ↑ Norton, Matthew; Khokhlov, Valentyn; Uryasev, Stan (2019). "Calculating CVaR and bPOE for common probability distributions with application to portfolio optimization and density estimation". Annals of Operations Research (Springer) 299 (1–2): 1281–1315. doi:10.1007/s10479019033731. http://uryasev.ams.stonybrook.edu/wpcontent/uploads/2019/10/Norton2019_CVaR_bPOE.pdf. Retrieved 20230227.
 ↑ Normal Distribution, Gale Encyclopedia of Psychology
 ↑ (Casella Berger )
 ↑ Lyon, A. (2014). Why are Normal Distributions Normal?, The British Journal for the Philosophy of Science.
 ↑ Jorge, Nocedal; Stephan, J. Wright (2006). Numerical Optimization (2nd ed.). Springer. pp. 249. ISBN 9780387303031.
 ↑ ^{6.0} ^{6.1} "Normal Distribution". https://www.mathsisfun.com/data/standardnormaldistribution.html.
 ↑ (Stigler 1982 )
 ↑ (Halperin Hartley )
 ↑ (McPherson 1990 )
 ↑ (Bernardo Smith )
 ↑ Scott, Clayton; Nowak, Robert (August 7, 2003). "The Qfunction". Connexions. http://cnx.org/content/m11537/1.2/.
 ↑ Barak, Ohad (April 6, 2006). "Q Function and Error Function". Tel Aviv University. http://www.eng.tau.ac.il/~jo/academic/Q.pdf.
 ↑ Weisstein, Eric W.. "Normal Distribution Function". http://mathworld.wolfram.com/NormalDistributionFunction.html.
 ↑ Abramowitz, Milton; Stegun, Irene Ann, eds (1983). "Chapter 26, eqn 26.2.12". Handbook of Mathematical Functions with Formulas, Graphs, and Mathematical Tables. Applied Mathematics Series. 55 (Ninth reprint with additional corrections of tenth original printing with corrections (December 1972); first ed.). Washington D.C.; New York: United States Department of Commerce, National Bureau of Standards; Dover Publications. pp. 932. LCCN 6512253. ISBN 9780486612720. http://www.math.sfu.ca/~cbm/aands/page_932.htm.
 ↑ Vaart, A. W. van der (19981013). Asymptotic Statistics. Cambridge University Press. doi:10.1017/cbo9780511802256. ISBN 9780511802256. http://dx.doi.org/10.1017/cbo9780511802256.
 ↑ Cover, Thomas M.; Thomas, Joy A. (2006). Elements of Information Theory. John Wiley and Sons. p. 254. ISBN 9780471748816. https://archive.org/details/elementsinformat00cove.
 ↑ Park, Sung Y.; Bera, Anil K. (2009). "Maximum Entropy Autoregressive Conditional Heteroskedasticity Model". Journal of Econometrics 150 (2): 219–230. doi:10.1016/j.jeconom.2008.12.014. http://www.wise.xmu.edu.cn/Master/Download/..%5C..%5CUploadFiles%5Cpapermasterdownload%5C2009519932327055475115776.pdf. Retrieved 20110602.
 ↑ Geary RC(1936) The distribution of the "Student's ratio for the nonnormal samples". Supplement to the Journal of the Royal Statistical Society 3 (2): 178–184
 ↑ Lukacs, Eugene, Wikidata Q55897617
 ↑ ^{20.0} ^{20.1} ^{20.2} (Patel Read )
 ↑ (Fan 1991 )
 ↑ (Patel Read )
 ↑ Papoulis, Athanasios. Probability, Random Variables and Stochastic Processes (4th ed.). p. 148.
 ↑ Winkelbauer, Andreas (2012). "Moments and Absolute Moments of the Normal Distribution". arXiv:1209.4340 [math.ST].
 ↑ (Bryc 1995 )
 ↑ (Bryc 1995 )
 ↑ (Cover Thomas )
 ↑ Williams, David (2001). Weighing the odds : a course in probability and statistics (Reprinted. ed.). Cambridge [u.a.]: Cambridge Univ. Press. pp. 197–199. ISBN 9780521006187. https://archive.org/details/weighingoddscour00will.
 ↑ Smith, José M. Bernardo; Adrian F. M. (2000). Bayesian theory (Reprint ed.). Chichester [u.a.]: Wiley. pp. 209, 366. ISBN 9780471494645. https://archive.org/details/bayesiantheory00bern_963.
 ↑ O'Hagan, A. (1994) Kendall's Advanced Theory of statistics, Vol 2B, Bayesian Inference, Edward Arnold. ISBN 0340529229 (Section 5.40)
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External links
 Hazewinkel, Michiel, ed. (2001), "Normal distribution", Encyclopedia of Mathematics, Springer Science+Business Media B.V. / Kluwer Academic Publishers, ISBN 9781556080104, https://www.encyclopediaofmath.org/index.php?title=p/n067460
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