In mathematics and physical science, spherical harmonics are special functions defined on the surface of a sphere. They are often employed in solving partial differential equations in many scientific fields. A list of the spherical harmonics is available in Table of spherical harmonics.

Since the spherical harmonics form a complete set of orthogonal functions and thus an orthonormal basis, each function defined on the surface of a sphere can be written as a sum of these spherical harmonics. This is similar to periodic functions defined on a circle that can be expressed as a sum of circular functions (sines and cosines) via Fourier series. Like the sines and cosines in Fourier series, the spherical harmonics may be organized by (spatial) angular frequency, as seen in the rows of functions in the illustration on the right. Further, spherical harmonics are basis functions for irreducible representations of SO(3), the group of rotations in three dimensions, and thus play a central role in the group theoretic discussion of SO(3).

Spherical harmonics originate from solving Laplace's equation in the spherical domains. Functions that are solutions to Laplace's equation are called harmonics. Despite their name, spherical harmonics take their simplest form in Cartesian coordinates, where they can be defined as homogeneous polynomials of degree ${\displaystyle \ell }$ in ${\displaystyle (x,y,z)}$ that obey Laplace's equation. The connection with spherical coordinates arises immediately if one uses the homogeneity to extract a factor of radial dependence ${\displaystyle r^{\ell ))$ from the above-mentioned polynomial of degree ${\displaystyle \ell }$; the remaining factor can be regarded as a function of the spherical angular coordinates ${\displaystyle \theta }$ and ${\displaystyle \varphi }$ only, or equivalently of the orientational unit vector ${\displaystyle \mathbf {r} }$ specified by these angles. In this setting, they may be viewed as the angular portion of a set of solutions to Laplace's equation in three dimensions, and this viewpoint is often taken as an alternative definition. Notice, however, that spherical harmonics are not functions on the sphere which are harmonic with respect to the Laplace-Beltrami operator for the standard round metric on the sphere: the only harmonic functions in this sense on the sphere are the constants, since harmonic functions satisfy the Maximum principle. Spherical harmonics, as functions on the sphere, are eigenfunctions of the Laplace-Beltrami operator (see the section Higher dimensions below).

A specific set of spherical harmonics, denoted ${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )}$ or ${\displaystyle Y_{\ell }^{m}({\mathbf {r} })}$, are known as Laplace's spherical harmonics, as they were first introduced by Pierre Simon de Laplace in 1782.^[1] These functions form an orthogonal system, and are thus basic to the expansion of a general function on the sphere as alluded to above.

Spherical harmonics are important in many theoretical and practical applications, including the representation of multipole electrostatic and electromagnetic fields, electron configurations, gravitational fields, geoids, the magnetic fields of planetary bodies and stars, and the cosmic microwave background radiation. In 3D computer graphics, spherical harmonics play a role in a wide variety of topics including indirect lighting (ambient occlusion, global illumination, precomputed radiance transfer, etc.) and modelling of 3D shapes.

History

Spherical harmonics were first investigated in connection with the Newtonian potential of Newton's law of universal gravitation in three dimensions. In 1782, Pierre-Simon de Laplace had, in his Mécanique Céleste, determined that the gravitational potential ${\displaystyle \mathbb {R} ^{3}\to \mathbb {R} }$ at a point x associated with a set of point masses m_i located at points x_i was given by

$${\displaystyle V(\mathbf {x} )=\sum _{i}{\frac {m_{i)){|\mathbf {x} _{i}-\mathbf {x} |)).}$$

Each term in the above summation is an individual Newtonian potential for a point mass. Just prior to that time, Adrien-Marie Legendre had investigated the expansion of the Newtonian potential in powers of r = |x| and r₁ = |x₁|. He discovered that if r ≤ r₁ then

$${\displaystyle {\frac {1}{|\mathbf {x} _{1}-\mathbf {x} |))=P_{0}(\cos \gamma ){\frac {1}{r_{1))}+P_{1}(\cos \gamma ){\frac {r}{r_{1}^{2))}+P_{2}(\cos \gamma ){\frac {r^{2)){r_{1}^{3))}+\cdots }$$

where γ is the angle between the vectors x and x₁. The functions ${\displaystyle P_{i}:[-1,1]\to \mathbb {R} }$ are the Legendre polynomials, and they can be derived as a special case of spherical harmonics. Subsequently, in his 1782 memoir, Laplace investigated these coefficients using spherical coordinates to represent the angle γ between x₁ and x. (See Applications of Legendre polynomials in physics for a more detailed analysis.)

In 1867, William Thomson (Lord Kelvin) and Peter Guthrie Tait introduced the solid spherical harmonics in their Treatise on Natural Philosophy, and also first introduced the name of "spherical harmonics" for these functions. The solid harmonics were homogeneous polynomial solutions ${\displaystyle \mathbb {R} ^{3}\to \mathbb {R} }$ of Laplace's equation

$${\displaystyle {\frac {\partial ^{2}u}{\partial x^{2))}+{\frac {\partial ^{2}u}{\partial y^{2))}+{\frac {\partial ^{2}u}{\partial z^{2))}=0.}$$

The 19th century development of Fourier series made possible the solution of a wide variety of physical problems in rectangular domains, such as the solution of the heat equation and wave equation. This could be achieved by expansion of functions in series of trigonometric functions. Whereas the trigonometric functions in a Fourier series represent the fundamental modes of vibration in a string, the spherical harmonics represent the fundamental modes of vibration of a sphere in much the same way. Many aspects of the theory of Fourier series could be generalized by taking expansions in spherical harmonics rather than trigonometric functions. Moreover, analogous to how trigonometric functions can equivalently be written as complex exponentials, spherical harmonics also possessed an equivalent form as complex-valued functions. This was a boon for problems possessing spherical symmetry, such as those of celestial mechanics originally studied by Laplace and Legendre.

The prevalence of spherical harmonics already in physics set the stage for their later importance in the 20th century birth of quantum mechanics. The (complex-valued) spherical harmonics ${\displaystyle S^{2}\to \mathbb {C} }$ are eigenfunctions of the square of the orbital angular momentum operator

$${\displaystyle -i\hbar \mathbf {r} \times \nabla ,}$$

Laplace's spherical harmonics

Laplace's equation imposes that the Laplacian of a scalar field f is zero. (Here the scalar field is understood to be complex, i.e. to correspond to a (smooth) function ${\displaystyle f:\mathbb {R} ^{3}\to \mathbb {C} }$.) In spherical coordinates this is:^[2]

$${\displaystyle \nabla ^{2}f={\frac {1}{r^{2))}{\frac {\partial }{\partial r))\left(r^{2}{\frac {\partial f}{\partial r))\right)+{\frac {1}{r^{2}\sin \theta )){\frac {\partial }{\partial \theta ))\left(\sin \theta {\frac {\partial f}{\partial \theta ))\right)+{\frac {1}{r^{2}\sin ^{2}\theta )){\frac {\partial ^{2}f}{\partial \varphi ^{2))}=0.}$$

Consider the problem of finding solutions of the form f(r, θ, φ) = R(r) Y(θ, φ). By separation of variables, two differential equations result by imposing Laplace's equation:

$${\displaystyle {\frac {1}{R)){\frac {d}{dr))\left(r^{2}{\frac {dR}{dr))\right)=\lambda ,\qquad {\frac {1}{Y)){\frac {1}{\sin \theta )){\frac {\partial }{\partial \theta ))\left(\sin \theta {\frac {\partial Y}{\partial \theta ))\right)+{\frac {1}{Y)){\frac {1}{\sin ^{2}\theta )){\frac {\partial ^{2}Y}{\partial \varphi ^{2))}=-\lambda .}$$

$${\displaystyle {\frac {1}{\Phi )){\frac {d^{2}\Phi }{d\varphi ^{2))}=-m^{2))$$

$${\displaystyle \lambda \sin ^{2}\theta +{\frac {\sin \theta }{\Theta )){\frac {d}{d\theta ))\left(\sin \theta {\frac {d\Theta }{d\theta ))\right)=m^{2))$$

for some number m. A priori, m is a complex constant, but because Φ must be a periodic function whose period evenly divides 2π, m is necessarily an integer and Φ is a linear combination of the complex exponentials e^{± imφ}. The solution function Y(θ, φ) is regular at the poles of the sphere, where θ = 0, π. Imposing this regularity in the solution Θ of the second equation at the boundary points of the domain is a Sturm–Liouville problem that forces the parameter λ to be of the form λ = ℓ (ℓ + 1) for some non-negative integer with ℓ ≥ |m|; this is also explained below in terms of the orbital angular momentum. Furthermore, a change of variables t = cos θ transforms this equation into the Legendre equation, whose solution is a multiple of the associated Legendre polynomial P^m
_ℓ(cos θ) . Finally, the equation for R has solutions of the form R(r) = A r^ℓ + B r^{−ℓ − 1}; requiring the solution to be regular throughout R³ forces B = 0.^[3]

Here the solution was assumed to have the special form Y(θ, φ) = Θ(θ) Φ(φ). For a given value of ℓ, there are 2ℓ + 1 independent solutions of this form, one for each integer m with −ℓ ≤ m ≤ ℓ. These angular solutions ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ are a product of trigonometric functions, here represented as a complex exponential, and associated Legendre polynomials:

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )=Ne^{im\varphi }P_{\ell }^{m}(\cos {\theta })}$$

which fulfill

$${\displaystyle r^{2}\nabla ^{2}Y_{\ell }^{m}(\theta ,\varphi )=-\ell (\ell +1)Y_{\ell }^{m}(\theta ,\varphi ).}$$

Here ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ is called a spherical harmonic function of degree ℓ and order m, ${\displaystyle P_{\ell }^{m}:[-1,1]\to \mathbb {R} }$ is an associated Legendre polynomial, N is a normalization constant,^[4] and θ and φ represent colatitude and longitude, respectively. In particular, the colatitude θ, or polar angle, ranges from 0 at the North Pole, to π/2 at the Equator, to π at the South Pole, and the longitude φ, or azimuth, may assume all values with 0 ≤ φ < 2π. For a fixed integer ℓ, every solution Y(θ, φ), ${\displaystyle Y:S^{2}\to \mathbb {C} }$, of the eigenvalue problem

$${\displaystyle r^{2}\nabla ^{2}Y=-\ell (\ell +1)Y}$$

${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$

${\displaystyle \mathbb {R} ^{3}\to \mathbb {C} }$

The general solution ${\displaystyle f:\mathbb {R} ^{3}\to \mathbb {C} }$ to Laplace's equation ${\displaystyle \Delta f=0}$ in a ball centered at the origin is a linear combination of the spherical harmonic functions multiplied by the appropriate scale factor r^ℓ,

$${\displaystyle f(r,\theta ,\varphi )=\sum _{\ell =0}^{\infty }\sum _{m=-\ell }^{\ell }f_{\ell }^{m}r^{\ell }Y_{\ell }^{m}(\theta ,\varphi ),}$$

where the ${\displaystyle f_{\ell }^{m}\in \mathbb {C} }$ are constants and the factors r^ℓ Y_ℓ^m are known as (regular) solid harmonics ${\displaystyle \mathbb {R} ^{3}\to \mathbb {C} }$. Such an expansion is valid in the ball

$${\displaystyle r<R={\frac {1}{\limsup _{\ell \to \infty }|f_{\ell }^{m}|^((1}/{\ell )))).}$$

For ${\displaystyle r>R}$, the solid harmonics with negative powers of ${\displaystyle r}$ (the irregular solid harmonics ${\displaystyle \mathbb {R} ^{3}\setminus \{\mathbf {0} \}\to \mathbb {C} }$) are chosen instead. In that case, one needs to expand the solution of known regions in Laurent series (about ${\displaystyle r=\infty }$), instead of the Taylor series (about ${\displaystyle r=0}$) used above, to match the terms and find series expansion coefficients ${\displaystyle f_{\ell }^{m}\in \mathbb {C} }$.

Orbital angular momentum

In quantum mechanics, Laplace's spherical harmonics are understood in terms of the orbital angular momentum^[5]

$${\displaystyle \mathbf {L} =-i\hbar (\mathbf {x} \times \mathbf {\nabla } )=L_{x}\mathbf {i} +L_{y}\mathbf {j} +L_{z}\mathbf {k} .}$$

$${\displaystyle {\begin{aligned}\mathbf {L} ^{2}&=-r^{2}\nabla ^{2}+\left(r{\frac {\partial }{\partial r))+1\right)r{\frac {\partial }{\partial r))\\&=-{\frac {1}{\sin \theta )){\frac {\partial }{\partial \theta ))\sin \theta {\frac {\partial }{\partial \theta ))-{\frac {1}{\sin ^{2}\theta )){\frac {\partial ^{2)){\partial \varphi ^{2))}.\end{aligned))}$$

$${\displaystyle {\begin{aligned}L_{z}&=-i\left(x{\frac {\partial }{\partial y))-y{\frac {\partial }{\partial x))\right)\\&=-i{\frac {\partial }{\partial \varphi )).\end{aligned))}$$

These operators commute, and are densely defined self-adjoint operators on the weighted Hilbert space of functions f square-integrable with respect to the normal distribution as the weight function on R³:

$${\displaystyle {\frac {1}{(2\pi )^{3/2))}\int _{\mathbb {R} ^{3))|f(x)|^{2}e^{-|x|^{2}/2}\,dx<\infty .}$$

If Y is a joint eigenfunction of L² and L_z, then by definition

$${\displaystyle {\begin{aligned}\mathbf {L} ^{2}Y&=\lambda Y\\L_{z}Y&=mY\end{aligned))}$$

$${\displaystyle \mathbf {L} ^{2}=L_{x}^{2}+L_{y}^{2}+L_{z}^{2))$$

Denote this joint eigenspace by E_λ,m, and define the raising and lowering operators by

$${\displaystyle {\begin{aligned}L_{+}&=L_{x}+iL_{y}\\L_{-}&=L_{x}-iL_{y}\end{aligned))}$$

${\displaystyle {\mathfrak {sl))_{2}(\mathbb {C} )}$

$${\displaystyle [L_{z},L_{+}]=L_{+},\quad [L_{z},L_{-}]=-L_{-},\quad [L_{+},L_{-}]=2L_{z}.}$$

$${\displaystyle L_{+}^{k}Y=0.}$$

$${\displaystyle L_{-}L_{+}=\mathbf {L} ^{2}-L_{z}^{2}-L_{z))$$

$${\displaystyle 0=L_{-}L_{+}^{k}Y=(\lambda -(m+k)^{2}-(m+k))Y.}$$

The foregoing has been all worked out in the spherical coordinate representation, ${\displaystyle \langle \theta ,\varphi |lm\rangle =Y_{l}^{m}(\theta ,\varphi )}$ but may be expressed more abstractly in the complete, orthonormal spherical ket basis.

Harmonic polynomial representation

The spherical harmonics can be expressed as the restriction to the unit sphere of certain polynomial functions ${\displaystyle \mathbb {R} ^{3}\to \mathbb {C} }$. Specifically, we say that a (complex-valued) polynomial function ${\displaystyle p:\mathbb {R} ^{3}\to \mathbb {C} }$ is homogeneous of degree ${\displaystyle \ell }$ if

$${\displaystyle p(\lambda \mathbf {x} )=\lambda ^{\ell }p(\mathbf {x} )}$$

${\displaystyle \lambda \in \mathbb {R} }$

${\displaystyle x\in \mathbb {R} ^{3))$

${\displaystyle p}$

$${\displaystyle \Delta p=0,}$$

${\displaystyle \Delta }$

${\displaystyle \ell }$

$${\displaystyle \mathbf {A} _{\ell }=\left\((\text{harmonic polynomials ))\mathbb {R} ^{3}\to \mathbb {C} {\text{ that are homogeneous of degree ))\ell \right\}.}$$

For example, when ${\displaystyle \ell =1}$, ${\displaystyle \mathbf {A} _{1))$ is just the 3-dimensional space of all linear functions ${\displaystyle \mathbb {R} ^{3}\to \mathbb {C} }$, since any such function is automatically harmonic. Meanwhile, when ${\displaystyle \ell =2}$, we have a 5-dimensional space:

$${\displaystyle \mathbf {A} _{2}=\operatorname {span} _{\mathbb {C} }(x_{1}x_{2},\,x_{1}x_{3},\,x_{2}x_{3},\,x_{1}^{2}-x_{2}^{2},\,x_{1}^{2}-x_{3}^{2}).}$$

For any ${\displaystyle \ell }$, the space ${\displaystyle \mathbf {H} _{\ell ))$ of spherical harmonics of degree ${\displaystyle \ell }$ is just the space of restrictions to the sphere ${\displaystyle S^{2))$ of the elements of ${\displaystyle \mathbf {A} _{\ell ))$.^[6] As suggested in the introduction, this perspective is presumably the origin of the term “spherical harmonic” (i.e., the restriction to the sphere of a harmonic function).

For example, for any ${\displaystyle c\in \mathbb {C} }$ the formula

$${\displaystyle p(x_{1},x_{2},x_{3})=c(x_{1}+ix_{2})^{\ell ))$$

${\displaystyle \ell }$

${\displaystyle \mathbb {R} ^{3}\to \mathbb {C} }$

${\displaystyle x_{3))$

${\displaystyle p}$

${\displaystyle (r,\theta ,\varphi )}$

${\displaystyle r=1}$

$${\displaystyle p(\theta ,\varphi )=c\sin(\theta )^{\ell }(\cos(\varphi )+i\sin(\varphi ))^{\ell },}$$

$${\displaystyle p(\theta ,\varphi )=c\left({\sqrt {1-\cos ^{2}(\theta )))\right)^{\ell }e^{i\ell \varphi }.}$$

${\displaystyle P_{\ell }^{\ell ))$

${\displaystyle Y_{\ell }^{\ell }(\theta ,\varphi ).}$

Conventions

Orthogonality and normalization

Several different normalizations are in common use for the Laplace spherical harmonic functions ${\displaystyle S^{2}\to \mathbb {C} }$. Throughout the section, we use the standard convention that for ${\displaystyle m>0}$ (see associated Legendre polynomials)

$${\displaystyle P_{\ell }^{-m}=(-1)^{m}{\frac {(\ell -m)!}{(\ell +m)!))P_{\ell }^{m))$$

In acoustics,^[8] the Laplace spherical harmonics are generally defined as (this is the convention used in this article)

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )={\sqrt ((\frac {(2\ell +1)}{4\pi )){\frac {(\ell -m)!}{(\ell +m)!))))\,P_{\ell }^{m}(\cos {\theta })\,e^{im\varphi ))$$

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )=(-1)^{m}{\sqrt ((\frac {(2\ell +1)}{4\pi )){\frac {(\ell -m)!}{(\ell +m)!))))\,P_{\ell }^{m}(\cos {\theta })\,e^{im\varphi ))$$

where ${\displaystyle P_{\ell }^{m))$ are associated Legendre polynomials without the Condon–Shortley phase (to avoid counting the phase twice).

In both definitions, the spherical harmonics are orthonormal

$${\displaystyle \int _{\theta =0}^{\pi }\int _{\varphi =0}^{2\pi }Y_{\ell }^{m}\,Y_{\ell '}^{m'}{}^{*}\,d\Omega =\delta _{\ell \ell '}\,\delta _{mm'},}$$

$${\displaystyle \int {|Y_{\ell }^{m}|^{2}d\Omega }=1.}$$

The disciplines of geodesy^[11] and spectral analysis use

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )={\sqrt (((2\ell +1)}{\frac {(\ell -m)!}{(\ell +m)!))))\,P_{\ell }^{m}(\cos {\theta })\,e^{im\varphi ))$$

which possess unit power

$${\displaystyle {\frac {1}{4\pi ))\int _{\theta =0}^{\pi }\int _{\varphi =0}^{2\pi }Y_{\ell }^{m}\,Y_{\ell '}^{m'}{}^{*}d\Omega =\delta _{\ell \ell '}\,\delta _{mm'}.}$$

The magnetics^[11] community, in contrast, uses Schmidt semi-normalized harmonics

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )={\sqrt {\frac {(\ell -m)!}{(\ell +m)!))}\,P_{\ell }^{m}(\cos {\theta })\,e^{im\varphi ))$$

which have the normalization

$${\displaystyle \int _{\theta =0}^{\pi }\int _{\varphi =0}^{2\pi }Y_{\ell }^{m}\,Y_{\ell '}^{m'}{}^{*}d\Omega ={\frac {4\pi }{(2\ell +1)))\delta _{\ell \ell '}\,\delta _{mm'}.}$$

In quantum mechanics this normalization is sometimes used as well, and is named Racah's normalization after Giulio Racah.

It can be shown that all of the above normalized spherical harmonic functions satisfy

$${\displaystyle Y_{\ell }^{m}{}^{*}(\theta ,\varphi )=(-1)^{-m}Y_{\ell }^{-m}(\theta ,\varphi ),}$$

where the superscript * denotes complex conjugation. Alternatively, this equation follows from the relation of the spherical harmonic functions with the Wigner D-matrix.

Condon–Shortley phase

One source of confusion with the definition of the spherical harmonic functions concerns a phase factor of ${\displaystyle (-1)^{m))$, commonly referred to as the Condon–Shortley phase in the quantum mechanical literature. In the quantum mechanics community, it is common practice to either include this phase factor in the definition of the associated Legendre polynomials, or to append it to the definition of the spherical harmonic functions. There is no requirement to use the Condon–Shortley phase in the definition of the spherical harmonic functions, but including it can simplify some quantum mechanical operations, especially the application of raising and lowering operators. The geodesy^[12] and magnetics communities never include the Condon–Shortley phase factor in their definitions of the spherical harmonic functions nor in the ones of the associated Legendre polynomials.^[13]

Real form

A real basis of spherical harmonics ${\displaystyle Y_{\ell m}:S^{2}\to \mathbb {R} }$ can be defined in terms of their complex analogues ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ by setting

$${\displaystyle {\begin{aligned}Y_{\ell m}&={\begin{cases}{\dfrac {i}{\sqrt {2))}\left(Y_{\ell }^{m}-(-1)^{m}\,Y_{\ell }^{-m}\right)&{\text{if))\ m<0\\Y_{\ell }^{0}&{\text{if))\ m=0\\{\dfrac {1}{\sqrt {2))}\left(Y_{\ell }^{-m}+(-1)^{m}\,Y_{\ell }^{m}\right)&{\text{if))\ m>0.\end{cases))\\&={\begin{cases}{\dfrac {i}{\sqrt {2))}\left(Y_{\ell }^{-|m|}-(-1)^{m}\,Y_{\ell }^{|m|}\right)&{\text{if))\ m<0\\Y_{\ell }^{0}&{\text{if))\ m=0\\{\dfrac {1}{\sqrt {2))}\left(Y_{\ell }^{-|m|}+(-1)^{m}\,Y_{\ell }^{|m|}\right)&{\text{if))\ m>0.\end{cases))\\&={\begin{cases}{\sqrt {2))\,(-1)^{m}\,\Im [{Y_{\ell }^{|m|))]&{\text{if))\ m<0\\Y_{\ell }^{0}&{\text{if))\ m=0\\{\sqrt {2))\,(-1)^{m}\,\Re [{Y_{\ell }^{m))]&{\text{if))\ m>0.\end{cases))\end{aligned))}$$

${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$

${\displaystyle Y_{\ell m}:S^{2}\to \mathbb {R} }$

$${\displaystyle Y_{\ell }^{m}={\begin{cases}{\dfrac {1}{\sqrt {2))}\left(Y_{\ell |m|}-iY_{\ell ,-|m|}\right)&{\text{if))\ m<0\\[4pt]Y_{\ell 0}&{\text{if))\ m=0\\[4pt]{\dfrac {(-1)^{m)){\sqrt {2))}\left(Y_{\ell |m|}+iY_{\ell ,-|m|}\right)&{\text{if))\ m>0.\end{cases))}$$

The real spherical harmonics ${\displaystyle Y_{\ell m}:S^{2}\to \mathbb {R} }$ are sometimes known as tesseral spherical harmonics.^[14] These functions have the same orthonormality properties as the complex ones ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ above. The real spherical harmonics ${\displaystyle Y_{\ell m))$ with m > 0 are said to be of cosine type, and those with m < 0 of sine type. The reason for this can be seen by writing the functions in terms of the Legendre polynomials as

$${\displaystyle Y_{\ell m}={\begin{cases}\left(-1\right)^{m}{\sqrt {2)){\sqrt ((\dfrac {2\ell +1}{4\pi )){\dfrac {(\ell -|m|)!}{(\ell +|m|)!))))\;P_{\ell }^{|m|}(\cos \theta )\ \sin(|m|\varphi )&{\text{if ))m<0\\[4pt]{\sqrt {\dfrac {2\ell +1}{4\pi ))}\ P_{\ell }^{m}(\cos \theta )&{\text{if ))m=0\\[4pt]\left(-1\right)^{m}{\sqrt {2)){\sqrt ((\dfrac {2\ell +1}{4\pi )){\dfrac {(\ell -m)!}{(\ell +m)!))))\;P_{\ell }^{m}(\cos \theta )\ \cos(m\varphi )&{\text{if ))m>0\,.\end{cases))}$$

The same sine and cosine factors can be also seen in the following subsection that deals with the Cartesian representation.

See here for a list of real spherical harmonics up to and including ${\displaystyle \ell =4}$, which can be seen to be consistent with the output of the equations above.

Use in quantum chemistry

As is known from the analytic solutions for the hydrogen atom, the eigenfunctions of the angular part of the wave function are spherical harmonics. However, the solutions of the non-relativistic Schrödinger equation without magnetic terms can be made real. This is why the real forms are extensively used in basis functions for quantum chemistry, as the programs don't then need to use complex algebra. Here, it is important to note that the real functions span the same space as the complex ones would.

For example, as can be seen from the table of spherical harmonics, the usual p functions (${\displaystyle \ell =1}$) are complex and mix axis directions, but the real versions are essentially just x, y, and z.

Spherical harmonics in Cartesian form

The complex spherical harmonics ${\displaystyle Y_{\ell }^{m))$ give rise to the solid harmonics by extending from ${\displaystyle S^{2))$ to all of ${\displaystyle \mathbb {R} ^{3))$ as a homogeneous function of degree ${\displaystyle \ell }$, i.e. setting

$${\displaystyle R_{\ell }^{m}(v):=\|v\|^{\ell }Y_{\ell }^{m}\left({\frac {v}{\|v\|))\right)}$$

${\displaystyle R_{\ell }^{m))$

${\displaystyle \ell }$

${\displaystyle SO(3)}$

${\displaystyle R_{\ell }^{m))$

The Herglotz generating function

If the quantum mechanical convention is adopted for the ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$, then

$${\displaystyle e^{v{\mathbf {a} }\cdot {\mathbf {r} ))=\sum _{\ell =0}^{\infty }\sum _{m=-\ell }^{\ell }{\sqrt {\frac {4\pi }{2\ell +1))}{\frac {r^{\ell }v^{\ell }{\lambda ^{m))}{\sqrt {(\ell +m)!(\ell -m)!))}Y_{\ell }^{m}(\mathbf {r} /r).}$$

${\displaystyle \mathbf {r} }$

${\displaystyle (x,y,z)\in \mathbb {R} ^{3))$

${\displaystyle r=|\mathbf {r} |}$

$${\displaystyle {\mathbf {a} }={\mathbf {\hat {z)) }-{\frac {\lambda }{2))\left({\mathbf {\hat {x)) }+i{\mathbf {\hat {y)) }\right)+{\frac {1}{2\lambda ))\left({\mathbf {\hat {x)) }-i{\mathbf {\hat {y)) }\right).}$$

${\displaystyle \mathbf {a} }$

${\displaystyle \mathbf {a} =[{\frac {1}{2))({\frac {1}{\lambda ))-\lambda ),-{\frac {i}{2))({\frac {1}{\lambda ))+\lambda ),1].}$

The essential property of ${\displaystyle \mathbf {a} }$ is that it is null:

$${\displaystyle \mathbf {a} \cdot \mathbf {a} =0.}$$

It suffices to take ${\displaystyle v}$ and ${\displaystyle \lambda }$ as real parameters. In naming this generating function after Herglotz, we follow Courant & Hilbert 1962, §VII.7, who credit unpublished notes by him for its discovery.

Essentially all the properties of the spherical harmonics can be derived from this generating function.^[15] An immediate benefit of this definition is that if the vector ${\displaystyle \mathbf {r} }$ is replaced by the quantum mechanical spin vector operator ${\displaystyle \mathbf {J} }$, such that ${\displaystyle {\mathcal {Y))_{\ell }^{m}({\mathbf {J} })}$ is the operator analogue of the solid harmonic ${\displaystyle r^{\ell }Y_{\ell }^{m}(\mathbf {r} /r)}$,^[16] one obtains a generating function for a standardized set of spherical tensor operators, ${\displaystyle {\mathcal {Y))_{\ell }^{m}({\mathbf {J} })}$:

$${\displaystyle e^{v{\mathbf {a} }\cdot {\mathbf {J} ))=\sum _{\ell =0}^{\infty }\sum _{m=-\ell }^{\ell }{\sqrt {\frac {4\pi }{2\ell +1))}{\frac {v^{\ell }{\lambda ^{m))}{\sqrt {(\ell +m)!(\ell -m)!))}{\mathcal {Y))_{\ell }^{m}({\mathbf {J} }).}$$

The parallelism of the two definitions ensures that the ${\displaystyle {\mathcal {Y))_{\ell }^{m))$'s transform under rotations (see below) in the same way as the ${\displaystyle Y_{\ell }^{m))$'s, which in turn guarantees that they are spherical tensor operators, ${\displaystyle T_{q}^{(k)))$, with ${\displaystyle k={\ell ))$ and ${\displaystyle q=m}$, obeying all the properties of such operators, such as the Clebsch-Gordan composition theorem, and the Wigner-Eckart theorem. They are, moreover, a standardized set with a fixed scale or normalization.

Separated Cartesian form

The Herglotzian definition yields polynomials which may, if one wishes, be further factorized into a polynomial of ${\displaystyle z}$ and another of ${\displaystyle x}$ and ${\displaystyle y}$, as follows (Condon–Shortley phase):

$${\displaystyle r^{\ell }\,{\begin{pmatrix}Y_{\ell }^{m}\\Y_{\ell }^{-m}\end{pmatrix))=\left[{\frac {2\ell +1}{4\pi ))\right]^{1/2}{\bar {\Pi ))_{\ell }^{m}(z){\begin{pmatrix}\left(-1\right)^{m}(A_{m}+iB_{m})\\(A_{m}-iB_{m})\end{pmatrix)),\qquad m>0.}$$

$${\displaystyle r^{\ell }\,Y_{\ell }^{0}\equiv {\sqrt {\frac {2\ell +1}{4\pi ))}{\bar {\Pi ))_{\ell }^{0}.}$$

$${\displaystyle A_{m}(x,y)=\sum _{p=0}^{m}{\binom {m}{p))x^{p}y^{m-p}\cos \left((m-p){\frac {\pi }{2))\right),}$$

$${\displaystyle B_{m}(x,y)=\sum _{p=0}^{m}{\binom {m}{p))x^{p}y^{m-p}\sin \left((m-p){\frac {\pi }{2))\right),}$$

$${\displaystyle {\bar {\Pi ))_{\ell }^{m}(z)=\left[{\frac {(\ell -m)!}{(\ell +m)!))\right]^{1/2}\sum _{k=0}^{\left\lfloor (\ell -m)/2\right\rfloor }(-1)^{k}2^{-\ell }{\binom {\ell }{k)){\binom {2\ell -2k}{\ell )){\frac {(\ell -2k)!}{(\ell -2k-m)!))\;r^{2k}\;z^{\ell -2k-m}.}$$

${\displaystyle m=0}$

$${\displaystyle {\bar {\Pi ))_{\ell }^{0}(z)=\sum _{k=0}^{\left\lfloor \ell /2\right\rfloor }(-1)^{k}2^{-\ell }{\binom {\ell }{k)){\binom {2\ell -2k}{\ell ))\;r^{2k}\;z^{\ell -2k}.}$$

The factor ${\displaystyle {\bar {\Pi ))_{\ell }^{m}(z)}$ is essentially the associated Legendre polynomial ${\displaystyle P_{\ell }^{m}(\cos \theta )}$, and the factors ${\displaystyle (A_{m}\pm iB_{m})}$ are essentially ${\displaystyle e^{\pm im\varphi ))$.

Examples

Using the expressions for ${\displaystyle {\bar {\Pi ))_{\ell }^{m}(z)}$, ${\displaystyle A_{m}(x,y)}$, and ${\displaystyle B_{m}(x,y)}$ listed explicitly above we obtain:

$${\displaystyle Y_{3}^{1}=-{\frac {1}{r^{3))}\left[{\tfrac {7}{4\pi ))\cdot {\tfrac {3}{16))\right]^{1/2}\left(5z^{2}-r^{2}\right)\left(x+iy\right)=-\left[{\tfrac {7}{4\pi ))\cdot {\tfrac {3}{16))\right]^{1/2}\left(5\cos ^{2}\theta -1\right)\left(\sin \theta e^{i\varphi }\right)}$$

$${\displaystyle Y_{4}^{-2}={\frac {1}{r^{4))}\left[{\tfrac {9}{4\pi ))\cdot {\tfrac {5}{32))\right]^{1/2}\left(7z^{2}-r^{2}\right)\left(x-iy\right)^{2}=\left[{\tfrac {9}{4\pi ))\cdot {\tfrac {5}{32))\right]^{1/2}\left(7\cos ^{2}\theta -1\right)\left(\sin ^{2}\theta e^{-2i\varphi }\right)}$$

Real forms

Using the equations above to form the real spherical harmonics, it is seen that for ${\displaystyle m>0}$ only the ${\displaystyle A_{m))$ terms (cosines) are included, and for ${\displaystyle m<0}$ only the ${\displaystyle B_{m))$ terms (sines) are included:

$${\displaystyle r^{\ell }\,{\begin{pmatrix}Y_{\ell m}\\Y_{\ell -m}\end{pmatrix))={\sqrt {\frac {2\ell +1}{2\pi ))}{\bar {\Pi ))_{\ell }^{m}(z){\begin{pmatrix}A_{m}\\B_{m}\end{pmatrix)),\qquad m>0.}$$

$${\displaystyle r^{\ell }\,Y_{\ell 0}\equiv {\sqrt {\frac {2\ell +1}{4\pi ))}{\bar {\Pi ))_{\ell }^{0}.}$$

Special cases and values

1. When ${\displaystyle m=0}$, the spherical harmonics ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ reduce to the ordinary Legendre polynomials:
   $${\displaystyle Y_{\ell }^{0}(\theta ,\varphi )={\sqrt {\frac {2\ell +1}{4\pi ))}P_{\ell }(\cos \theta ).}$$

   
2. When ${\displaystyle m=\pm \ell }$,
   $${\displaystyle Y_{\ell }^{\pm \ell }(\theta ,\varphi )={\frac {(\mp 1)^{\ell )){2^{\ell }\ell !)){\sqrt {\frac {(2\ell +1)!}{4\pi ))}\sin ^{\ell }\theta \,e^{\pm i\ell \varphi },}$$

   
   or more simply in Cartesian coordinates,
   $${\displaystyle r^{\ell }Y_{\ell }^{\pm \ell }({\mathbf {r} })={\frac {(\mp 1)^{\ell )){2^{\ell }\ell !)){\sqrt {\frac {(2\ell +1)!}{4\pi ))}(x\pm iy)^{\ell }.}$$

   
3. At the north pole, where ${\displaystyle \theta =0}$, and ${\displaystyle \varphi }$ is undefined, all spherical harmonics except those with ${\displaystyle m=0}$ vanish:
   $${\displaystyle Y_{\ell }^{m}(0,\varphi )=Y_{\ell }^{m}({\mathbf {z} })={\sqrt {\frac {2\ell +1}{4\pi ))}\delta _{m0}.}$$

   

Symmetry properties

The spherical harmonics have deep and consequential properties under the operations of spatial inversion (parity) and rotation.

Parity

The spherical harmonics have definite parity. That is, they are either even or odd with respect to inversion about the origin. Inversion is represented by the operator ${\displaystyle P\Psi (\mathbf {r} )=\Psi (-\mathbf {r} )}$. Then, as can be seen in many ways (perhaps most simply from the Herglotz generating function), with ${\displaystyle \mathbf {r} }$ being a unit vector,

$${\displaystyle Y_{\ell }^{m}(-\mathbf {r} )=(-1)^{\ell }Y_{\ell }^{m}(\mathbf {r} ).}$$

In terms of the spherical angles, parity transforms a point with coordinates ${\displaystyle \{\theta ,\varphi \))$ to ${\displaystyle \{\pi -\theta ,\pi +\varphi \))$. The statement of the parity of spherical harmonics is then

$${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )\to Y_{\ell }^{m}(\pi -\theta ,\pi +\varphi )=(-1)^{\ell }Y_{\ell }^{m}(\theta ,\varphi )}$$

Parity continues to hold for real spherical harmonics, and for spherical harmonics in higher dimensions: applying a point reflection to a spherical harmonic of degree ℓ changes the sign by a factor of (−1)^ℓ.

Rotations

Consider a rotation ${\displaystyle {\mathcal {R))}$ about the origin that sends the unit vector ${\displaystyle \mathbf {r} }$ to ${\displaystyle \mathbf {r} '}$. Under this operation, a spherical harmonic of degree ${\displaystyle \ell }$ and order ${\displaystyle m}$ transforms into a linear combination of spherical harmonics of the same degree. That is,

$${\displaystyle Y_{\ell }^{m}({\mathbf {r} }')=\sum _{m'=-\ell }^{\ell }A_{mm'}Y_{\ell }^{m'}({\mathbf {r} }),}$$

${\displaystyle A_{mm'))$

${\displaystyle (2\ell +1)}$

${\displaystyle {\mathcal {R))}$

$${\displaystyle Y_{\ell }^{m}({\mathbf {r} }')=\sum _{m'=-\ell }^{\ell }[D_{mm'}^{(\ell )}({\mathcal {R)))]^{*}Y_{\ell }^{m'}({\mathbf {r} }),}$$

${\displaystyle D_{mm'}^{(\ell )}({\mathcal {R)))^{*))$

${\displaystyle \mathbf {r} '}$

${\displaystyle \phi _{0))$

$${\displaystyle Y_{\ell }^{m}({\mathbf {r} }')=Y_{\ell }^{m}({\mathbf {r} })e^{im\phi _{0)).}$$

The rotational behavior of the spherical harmonics is perhaps their quintessential feature from the viewpoint of group theory. The ${\displaystyle Y_{\ell }^{m))$'s of degree ${\displaystyle \ell }$ provide a basis set of functions for the irreducible representation of the group SO(3) of dimension ${\displaystyle (2\ell +1)}$. Many facts about spherical harmonics (such as the addition theorem) that are proved laboriously using the methods of analysis acquire simpler proofs and deeper significance using the methods of symmetry.

Spherical harmonics expansion

The Laplace spherical harmonics ${\displaystyle Y_{\ell }^{m}:S^{2}\to \mathbb {C} }$ form a complete set of orthonormal functions and thus form an orthonormal basis of the Hilbert space of square-integrable functions ${\displaystyle L_{\mathbb {C} }^{2}(S^{2})}$. On the unit sphere ${\displaystyle S^{2))$, any square-integrable function ${\displaystyle f:S^{2}\to \mathbb {C} }$ can thus be expanded as a linear combination of these:

$${\displaystyle f(\theta ,\varphi )=\sum _{\ell =0}^{\infty }\sum _{m=-\ell }^{\ell }f_{\ell }^{m}\,Y_{\ell }^{m}(\theta ,\varphi ).}$$

This expansion holds in the sense of mean-square convergence — convergence in L² of the sphere — which is to say that

$${\displaystyle \lim _{N\to \infty }\int _{0}^{2\pi }\int _{0}^{\pi }\left|f(\theta ,\varphi )-\sum _{\ell =0}^{N}\sum _{m=-\ell }^{\ell }f_{\ell }^{m}Y_{\ell }^{m}(\theta ,\varphi )\right|^{2}\sin \theta \,d\theta \,d\varphi =0.}$$

The expansion coefficients are the analogs of Fourier coefficients, and can be obtained by multiplying the above equation by the complex conjugate of a spherical harmonic, integrating over the solid angle Ω, and utilizing the above orthogonality relationships. This is justified rigorously by basic Hilbert space theory. For the case of orthonormalized harmonics, this gives:

$${\displaystyle f_{\ell }^{m}=\int _{\Omega }f(\theta ,\varphi )\,Y_{\ell }^{m*}(\theta ,\varphi )\,d\Omega =\int _{0}^{2\pi }d\varphi \int _{0}^{\pi }\,d\theta \,\sin \theta f(\theta ,\varphi )Y_{\ell }^{m*}(\theta ,\varphi ).}$$

If the coefficients decay in ℓ sufficiently rapidly — for instance, exponentially — then the series also converges uniformly to f.

A square-integrable function ${\displaystyle f:S^{2}\to \mathbb {R} }$ can also be expanded in terms of the real harmonics ${\displaystyle Y_{\ell m}:S^{2}\to \mathbb {R} }$ above as a sum

$${\displaystyle f(\theta ,\varphi )=\sum _{\ell =0}^{\infty }\sum _{m=-\ell }^{\ell }f_{\ell m}\,Y_{\ell m}(\theta ,\varphi ).}$$

The convergence of the series holds again in the same sense, namely the real spherical harmonics ${\displaystyle Y_{\ell m}:S^{2}\to \mathbb {R} }$ form a complete set of orthonormal functions and thus form an orthonormal basis of the Hilbert space of square-integrable functions ${\displaystyle L_{\mathbb {R} }^{2}(S^{2})}$. The benefit of the expansion in terms of the real harmonic functions ${\displaystyle Y_{\ell m))$ is that for real functions ${\displaystyle f:S^{2}\to \mathbb {R} }$ the expansion coefficients ${\displaystyle f_{\ell m))$ are guaranteed to be real, whereas their coefficients ${\displaystyle f_{\ell }^{m))$ in their expansion in terms of the ${\displaystyle Y_{\ell }^{m))$ (considering them as functions ${\displaystyle f:S^{2}\to \mathbb {C} \supset \mathbb {R} }$) do not have that property.

Spectrum analysis

Power spectrum in signal processing

The total power of a function f is defined in the signal processing literature as the integral of the function squared, divided by the area of its domain. Using the orthonormality properties of the real unit-power spherical harmonic functions, it is straightforward to verify that the total power of a function defined on the unit sphere is related to its spectral coefficients by a generalization of Parseval's theorem (here, the theorem is stated for Schmidt semi-normalized harmonics, the relationship is slightly different for orthonormal harmonics):

$${\displaystyle {\frac {1}{4\,\pi ))\int _{\Omega }|f(\Omega )|^{2}\,d\Omega =\sum _{\ell =0}^{\infty }S_{f\!f}(\ell ),}$$

$${\displaystyle S_{f\!f}(\ell )={\frac {1}{2\ell +1))\sum _{m=-\ell }^{\ell }|f_{\ell m}|^{2))$$

is defined as the angular power spectrum (for Schmidt semi-normalized harmonics). In a similar manner, one can define the cross-power of two functions as

$${\displaystyle {\frac {1}{4\,\pi ))\int _{\Omega }f(\Omega )\,g^{\ast }(\Omega )\,d\Omega =\sum _{\ell =0}^{\infty }S_{fg}(\ell ),}$$

$${\displaystyle S_{fg}(\ell )={\frac {1}{2\ell +1))\sum _{m=-\ell }^{\ell }f_{\ell m}g_{\ell m}^{\ast ))$$

is defined as the cross-power spectrum. If the functions f and g have a zero mean (i.e., the spectral coefficients f₀₀ and g₀₀ are zero), then S_ff(ℓ) and S_fg(ℓ) represent the contributions to the function's variance and covariance for degree ℓ, respectively. It is common that the (cross-)power spectrum is well approximated by a power law of the form

$${\displaystyle S_{f\!f}(\ell )=C\,\ell ^{\beta }.}$$

When β = 0, the spectrum is "white" as each degree possesses equal power. When β < 0, the spectrum is termed "red" as there is more power at the low degrees with long wavelengths than higher degrees. Finally, when β > 0, the spectrum is termed "blue". The condition on the order of growth of S_ff(ℓ) is related to the order of differentiability of f in the next section.

Differentiability properties