# Spherical harmonics

"Ylm" redirects here. For other uses, see YLM (disambiguation).
Visual representations of the first few real spherical harmonics. Blue portions represent regions where the function is positive, and yellow portions represent where it is negative. The distance of the surface from the origin indicates the value of ${\displaystyle Y_{\ell }^{m}(\theta ,\phi )}$ in angular direction ${\displaystyle (\theta ,\phi )}$.

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 that commonly occur in science. The spherical harmonics are a complete set of orthogonal functions on the sphere, and thus may be used to represent functions defined on the surface of a sphere, just as circular functions (sines and cosines) are used to represent functions on a circle 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 SO(3), the group of rotations in three dimensions, and thus play a central role in the group theoretic discussion of SO(3).

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. Functions that satisfy Laplace's equation are often said to be harmonic, hence the name spherical harmonics. The connection with spherical coordinates arises immediately if one uses the homogeneity to extract a factor of ${\displaystyle r^{\ell }}$ 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.

A specific set of spherical harmonics, denoted ${\displaystyle Y_{\ell }^{m}(\theta ,\varphi )}$ or ${\displaystyle Y_{\ell }^{m}({\mathbf {r} })}$, are called 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, e.g., the representation of multipole electrostatic and electromagnetic fields, computation of atomic orbital electron configurations, representation of gravitational fields, geoids, and the magnetic fields of planetary bodies and stars, and characterization of 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 at a point x associated to a set of point masses mi located at points xi 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 rr1 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 Pi are the Legendre polynomials, and they are a special case of spherical harmonics. Subsequently, in his 1782 memoire, 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 of Laplace's equation

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

By examining Laplace's equation in spherical coordinates, Thomson and Tait recovered Laplace's spherical harmonics. The term "Laplace's coefficients" was employed by William Whewell to describe the particular system of solutions introduced along these lines, whereas others reserved this designation for the zonal spherical harmonics that had properly been introduced by Laplace and Legendre.

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. 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 spherical harmonics are eigenfunctions of the square of the orbital angular momentum operator

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

and therefore they represent the different quantized configurations of atomic orbitals.

## Laplace's spherical harmonics

Real (Laplace) spherical harmonics Ym for = 0, …, 4 (top to bottom) and m = 0, …, (left to right). Zonal, sectoral, and tesseral harmonics are depicted along the left-most column, the main diagonal, and elsewhere, respectively. (The negative order harmonics ${\displaystyle Y_{\ell }^{-m}}$ would be shown rotated about the z axis by ${\displaystyle 90^{\circ }/m}$ with respect to the positive order ones.)

Laplace's equation imposes that the divergence of the gradient of a scalar field f is zero. 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:

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

The second equation can be simplified under the assumption that Y has the form Y(θ, φ) = Θ(θ) Φ(φ). Applying separation of variables again to the second equation gives way to the pair of differential equations

${\displaystyle {\frac {1}{\Phi }}{\frac {d^{2}\Phi }{d\varphi ^{2}}}=-m^{2}}$
${\displaystyle \lambda \sin ^{2}\theta +{\frac {\sin \theta }{\Theta }}{\frac {d}{d\theta }}\left(\sin \theta {\frac {d\Theta }{d\theta }}\right)=m^{2}}$

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± i m φ. 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 = ( + 1) for some non-negative integer with ≥ |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 Pm(cos θ) . Finally, the equation for R has solutions of the form R(r) = A r + B r − 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 , there are 2 + 1 independent solutions of this form, one for each integer m with m. These angular solutions 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 Ym is called a spherical harmonic function of degree and order m, Pm is an associated Legendre polynomial, N is a normalization constant, 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 , every solution Y(θ, φ) of the eigenvalue problem

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

is a linear combination of Ym. In fact, for any such solution, r Y(θ, φ) is the expression in spherical coordinates of a homogeneous polynomial that is harmonic (see below), and so counting dimensions shows that there are 2 + 1 linearly independent such polynomials.

The general solution to Laplace's equation in a ball centered at the origin is a linear combination of the spherical harmonic functions multiplied by the appropriate scale factor r,

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

where the fm are constants and the factors r Ym are known as solid harmonics. Such an expansion is valid in the ball

${\displaystyle r

### Orbital angular momentum

In quantum mechanics, Laplace's spherical harmonics are understood in terms of the orbital angular momentum[4]

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

The ħ is conventional in quantum mechanics; it is convenient to work in units in which ħ = 1. The spherical harmonics are eigenfunctions of the square of the orbital angular momentum

{\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}}}

Laplace's spherical harmonics are the joint eigenfunctions of the square of the orbital angular momentum and the generator of rotations about the azimuthal axis:

{\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 Hilbert space of functions f square-integrable with respect to the normal distribution on R3:

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

Furthermore, L2 is a positive operator.

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

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

for some real numbers m and λ. Here m must in fact be an integer, for Y must be periodic in the coordinate φ with period a number that evenly divides 2π. Furthermore, since

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

and each of Lx, Ly, Lz are self-adjoint, it follows that λ ≥ m2.

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

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

Then L+ and L commute with L2, and the Lie algebra generated by L+, L, Lz is the special linear Lie algebra, with commutation relations

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

Thus L+ : Eλ,mEλ,m+1 (it is a "raising operator") and L : Eλ,mEλ,m−1 (it is a "lowering operator"). In particular, Lk
+
: Eλ,mEλ,m+k
must be zero for k sufficiently large, because the inequality λ ≥ m2 must hold in each of the nontrivial joint eigenspaces. Let Y ∈ Eλ,m be a nonzero joint eigenfunction, and let k be the least integer such that

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

Then, since

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

it follows that

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

Thus λ = ℓ(ℓ+1) for the positive integer ℓ = m+k.

## Conventions

### Orthogonality and normalization

Several different normalizations are in common use for the Laplace spherical harmonic functions. Throughout the section, we use the standard convention that (see associated Legendre polynomials)

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

which is the natural normalization given by Rodrigues' formula.

In seismology[citation needed], the Laplace spherical harmonics are generally defined as (this is the convention used in this article)

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

while in quantum mechanics:[5][6]

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

which are orthonormal

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

where δij is the Kronecker delta and dΩ = sinθ dφ dθ. This normalization is used in quantum mechanics because it ensures that probability is normalized, i.e.

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

The disciplines of geodesy[citation needed] and spectral analysis use

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

which possess unit power

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

The magnetics[citation needed] community, in contrast, uses Schmidt semi-normalized harmonics

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

which have the normalization

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

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 (−1)m for m > 0, 1 otherwise, 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[7] 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.[citation needed]

### Real form

A real basis of spherical harmonics can be defined in terms of their complex analogues by setting

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

The Condon-Shortley phase convention is used here for consistency. The corresponding inverse equations are

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

The real spherical harmonics are sometimes known as tesseral spherical harmonics.[8] These functions have the same orthonormality properties as the complex ones above. The harmonics 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

${\displaystyle Y_{\ell m}={\begin{cases}\displaystyle {\sqrt {2}}{\sqrt {{(2\ell +1) \over 4\pi }{(\ell -|m|)! \over (\ell +|m|)!}}}P_{\ell }^{|m|}(\cos \theta )\sin |m|\varphi &{\mbox{if }}m<0\\\displaystyle {\sqrt {(2\ell +1) \over 4\pi }}P_{\ell }^{m}(\cos \theta )&{\mbox{if }}m=0\\\displaystyle {\sqrt {2}}{\sqrt {{(2\ell +1) \over 4\pi }{(\ell -m)! \over (\ell +m)!}}}P_{\ell }^{m}(\cos \theta )\cos m\varphi &{\mbox{if }}m>0\end{cases}}}$

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 (${\displaystyle l=1}$) are complex and mix axis directions, but the real versions are essentially just x, y and z.

## Spherical harmonics in Cartesian form

### The Herglotz generating function

If the quantum mechanical convention is adopted for the ${\displaystyle Y_{\ell }^{m}}$, then,

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

Here, ${\displaystyle {\mathbf {r} }}$ is the vector with components ${\displaystyle (x,y,z)}$, and

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

is a vector with complex coefficients. It suffices to take ${\displaystyle \lambda }$ as a real parameter. The essential property of ${\displaystyle {\mathbf {a} }}$ is that it is null:

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

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.[9] An immediate benefit of this definition is that if the c-number vector ${\displaystyle {\mathbf {r} }}$ is replaced by the quantum mechanical spin vector operator ${\displaystyle {\mathbf {J} }}$, 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):

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

and for m = 0:

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

Here

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

and

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

For ${\displaystyle m=0}$ this reduces to

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

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:

${\displaystyle Y_{3}^{1}=-{\frac {1}{r^{3}}}\left[{\tfrac {7}{4\pi }}\cdot {\tfrac {3}{16}}\right]^{1/2}(5z^{2}-r^{2})(x+iy)=-\left[{\tfrac {7}{4\pi }}\cdot {\tfrac {3}{16}}\right]^{1/2}(5\cos ^{2}\theta -1)(\sin \theta e^{i\varphi })}$
${\displaystyle Y_{4}^{-2}={\frac {1}{r^{4}}}\left[{\tfrac {9}{4\pi }}\cdot {\tfrac {5}{32}}\right]^{1/2}(7z^{2}-r^{2})(x-iy)^{2}=\left[{\tfrac {9}{4\pi }}\cdot {\tfrac {5}{32}}\right]^{1/2}(7\cos ^{2}\theta -1)(\sin ^{2}\theta e^{-2i\varphi })}$

It may be verified that this agrees with the function listed here and here.

#### Real form

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:

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

and for 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 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 ${\displaystyle m=\pm \ell }$,

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

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

Main article: Parity (physics)

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 ${\displaystyle \{\theta ,\phi \}}$ to ${\displaystyle \{\pi -\theta ,\pi +\phi \}}$. The statement of the parity of spherical harmonics is then

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

(This can be seen as follows: The associated Legendre polynomials gives (−1)ℓ+m and from the exponential function we have (−1)m, giving together for the spherical harmonics a parity of (−1).)

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).

### 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,

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

where ${\displaystyle A_{mm'}}$ is a matrix of order ${\displaystyle (2\ell +1)}$ that depends on the rotation ${\displaystyle {\mathcal {R}}}$. However, this is not the standard way of expressing this property. In the standard way one writes,

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

where ${\displaystyle D_{mm'}^{(\ell )}({\mathcal {R}})^{*}}$ is the complex conjugate of an element of the Wigner D-matrix.

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 form a complete set of orthonormal functions and thus form an orthonormal basis of the Hilbert space of square-integrable functions. On the unit sphere, any square-integrable function 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 f can also be expanded in terms of the real harmonics Ym 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, but the benefit of the real expansion is that for real functions f the expansion coefficients become real.

## 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):

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

where

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

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

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

where

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

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 Sff(ℓ) and Sfg(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 Sff(ℓ) is related to the order of differentiability of f in the next section.

### Differentiability properties

One can also understand the differentiability properties of the original function f in terms of the asymptotics of Sff(ℓ). In particular, if Sff(ℓ) decays faster than any rational function of ℓ as ℓ → ∞, then f is infinitely differentiable. If, furthermore, Sff(ℓ) decays exponentially, then f is actually real analytic on the sphere.

The general technique is to use the theory of Sobolev spaces. Statements relating the growth of the Sff(ℓ) to differentiability are then similar to analogous results on the growth of the coefficients of Fourier series. Specifically, if

${\displaystyle \sum _{\ell =0}^{\infty }(1+\ell ^{2})^{s}S_{ff}(\ell )<\infty ,}$

then f is in the Sobolev space Hs(S2). In particular, the Sobolev embedding theorem implies that f is infinitely differentiable provided that

${\displaystyle S_{ff}(\ell )=O(\ell ^{-s})\quad {\rm {{as\ }\ell \to \infty }}}$

for all s.

## Algebraic properties

A mathematical result of considerable interest and use is called the addition theorem for spherical harmonics. This is a generalization of the trigonometric identity

${\displaystyle \cos(\theta '-\theta )=\cos \theta '\cos \theta +\sin \theta \sin \theta '}$

in which the role of the trigonometric functions appearing on the right-hand side is played by the spherical harmonics and that of the left-hand side is played by the Legendre polynomials.

Consider two unit vectors x and y, having spherical coordinates (θ,φ) and (θ′,φ′), respectively. The addition theorem states[10]

${\displaystyle P_{\ell }(\mathbf {x} \cdot \mathbf {y} )={\frac {4\pi }{2\ell +1}}\sum _{m=-\ell }^{\ell }Y_{\ell m}(\theta ',\varphi ')\,Y_{\ell m}^{*}(\theta ,\varphi ).}$

(1)

where P is the Legendre polynomial of degree ℓ. This expression is valid for both real and complex harmonics.[11] The result can be proven analytically, using the properties of the Poisson kernel in the unit ball, or geometrically by applying a rotation to the vector y so that it points along the z-axis, and then directly calculating the right-hand side.[12]

In particular, when x = y, this gives Unsöld's theorem[13]

${\displaystyle \sum _{m=-\ell }^{\ell }Y_{\ell m}^{*}(\theta ,\varphi )\,Y_{\ell m}(\theta ,\varphi )={\frac {2\ell +1}{4\pi }}}$

which generalizes the identity cos2θ + sin2θ = 1 to two dimensions.

In the expansion (1), the left-hand side P(x·y) is a constant multiple of the degree ℓ zonal spherical harmonic. From this perspective, one has the following generalization to higher dimensions. Let Yj be an arbitrary orthonormal basis of the space H of degree ℓ spherical harmonics on the n-sphere. Then ${\displaystyle Z_{\mathbf {x} }^{(\ell )}}$, the degree ℓ zonal harmonic corresponding to the unit vector x, decomposes as[14]

${\displaystyle Z_{\mathbf {x} }^{(\ell )}({\mathbf {y} })=\sum _{j=1}^{\dim(\mathbf {H} _{\ell })}{\overline {Y_{j}({\mathbf {x} })}}\,Y_{j}({\mathbf {y} })}$

(2)

Furthermore, the zonal harmonic ${\displaystyle Z_{\mathbf {x} }^{(\ell )}({\mathbf {y} })}$ is given as a constant multiple of the appropriate Gegenbauer polynomial:

${\displaystyle Z_{\mathbf {x} }^{(\ell )}({\mathbf {y} })=C_{\ell }^{((n-1)/2)}({\mathbf {x} }\cdot {\mathbf {y} })}$

(3)

Combining (2) and (3) gives (1) in dimension n = 2 when x and y are represented in spherical coordinates. Finally, evaluating at x = y gives the functional identity

${\displaystyle {\frac {\dim \mathbf {H} _{\ell }}{\omega _{n-1}}}=\sum _{j=1}^{\dim(\mathbf {H} _{\ell })}|Y_{j}({\mathbf {x} })|^{2}}$

where ωn−1 is the volume of the (n−1)-sphere.

### Clebsch–Gordan coefficients

The Clebsch–Gordan coefficients are the coefficients appearing in the expansion of the product of two spherical harmonics in terms of spherical harmonics itself. A variety of techniques are available for doing essentially the same calculation, including the Wigner 3-jm symbol, the Racah coefficients, and the Slater integrals. Abstractly, the Clebsch–Gordan coefficients express the tensor product of two irreducible representations of the rotation group as a sum of irreducible representations: suitably normalized, the coefficients are then the multiplicities.

## Visualization of the spherical harmonics

Schematic representation of ${\displaystyle Y_{\ell m}}$ on the unit sphere and its nodal lines. ${\displaystyle {\text{Re}}[Y_{\ell m}]}$ is equal to 0 along m great circles passing through the poles, and along ℓ−m circles of equal latitude. The function changes sign each time it crosses one of these lines.
3D color plot of the spherical harmonics of degree n = 5. Note that n = ℓ.

The Laplace spherical harmonics ${\displaystyle Y_{\ell }^{m}}$ can be visualized by considering their "nodal lines", that is, the set of points on the sphere where ${\displaystyle {\text{Re}}[Y_{\ell }^{m}]=0}$, or alternatively where ${\displaystyle {\text{Im}}[Y_{\ell }^{m}]=0}$. Nodal lines of ${\displaystyle Y_{\ell }^{m}}$ are composed of circles: some are latitudes and others are longitudes. One can determine the number of nodal lines of each type by counting the number of zeros of ${\displaystyle Y_{\ell }^{m}}$ in the latitudinal and longitudinal directions independently. For the latitudinal direction,[clarification needed] the real and imaginary components of the associated Legendre polynomials each possess ℓ−|m| zeros, whereas for the longitudinal direction, the trigonometric sin and cos functions possess 2|m| zeros.[clarification needed]

When the spherical harmonic order m is zero (upper-left in the figure), the spherical harmonic functions do not depend upon longitude, and are referred to as zonal. Such spherical harmonics are a special case of zonal spherical functions. When ℓ = |m| (bottom-right in the figure), there are no zero crossings in latitude, and the functions are referred to as sectoral. For the other cases, the functions checker the sphere, and they are referred to as tesseral.

More general spherical harmonics of degree ℓ are not necessarily those of the Laplace basis ${\displaystyle Y_{\ell }^{m}}$, and their nodal sets can be of a fairly general kind.[15]

## List of spherical harmonics

Analytic expressions for the first few orthonormalized Laplace spherical harmonics that use the Condon-Shortley phase convention:

${\displaystyle Y_{0}^{0}(\theta ,\varphi )={1 \over 2}{\sqrt {1 \over \pi }}}$
${\displaystyle Y_{1}^{-1}(\theta ,\varphi )={1 \over 2}{\sqrt {3 \over 2\pi }}\,\sin \theta \,e^{-i\varphi }}$
${\displaystyle Y_{1}^{0}(\theta ,\varphi )={1 \over 2}{\sqrt {3 \over \pi }}\,\cos \theta }$
${\displaystyle Y_{1}^{1}(\theta ,\varphi )={-1 \over 2}{\sqrt {3 \over 2\pi }}\,\sin \theta \,e^{i\varphi }}$
${\displaystyle Y_{2}^{-2}(\theta ,\varphi )={1 \over 4}{\sqrt {15 \over 2\pi }}\,\sin ^{2}\theta \,e^{-2i\varphi }}$
${\displaystyle Y_{2}^{-1}(\theta ,\varphi )={1 \over 2}{\sqrt {15 \over 2\pi }}\,\sin \theta \,\cos \theta \,e^{-i\varphi }}$
${\displaystyle Y_{2}^{0}(\theta ,\varphi )={1 \over 4}{\sqrt {5 \over \pi }}\,(3\cos ^{2}\theta -1)}$
${\displaystyle Y_{2}^{1}(\theta ,\varphi )={-1 \over 2}{\sqrt {15 \over 2\pi }}\,\sin \theta \,\cos \theta \,e^{i\varphi }}$
${\displaystyle Y_{2}^{2}(\theta ,\varphi )={1 \over 4}{\sqrt {15 \over 2\pi }}\,\sin ^{2}\theta \,e^{2i\varphi }}$

## Higher dimensions

The classical spherical harmonics are defined as functions on the unit sphere S2 inside three-dimensional Euclidean space. Spherical harmonics can be generalized to higher-dimensional Euclidean space Rn as follows.[16] Let P denote the space of homogeneous polynomials of degree ℓ in n variables. That is, a polynomial P is in P provided that

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

Let A denote the subspace of P consisting of all harmonic polynomials; these are the solid spherical harmonics. Let H denote the space of functions on the unit sphere

${\displaystyle S^{n-1}=\{\mathbf {x} \in \mathbf {R} ^{n}\,\mid \,|x|=1\}}$

obtained by restriction from A.

The following properties hold:

• The sum of the spaces H is dense in the set of continuous functions on Sn−1 with respect to the uniform topology, by the Stone-Weierstrass theorem. As a result, the sum of these spaces is also dense in the space L2(Sn−1) of square-integrable functions on the sphere. Thus every square-integrable function on the sphere decomposes uniquely into a series a spherical harmonics, where the series converges in the L2 sense.
• For all f ∈ H, one has
${\displaystyle \Delta _{S^{n-1}}f=-\ell (\ell +n-2)f.}$
where ΔSn−1 is the Laplace–Beltrami operator on Sn−1. This operator is the analog of the angular part of the Laplacian in three dimensions; to wit, the Laplacian in n dimensions decomposes as
${\displaystyle \nabla ^{2}=r^{1-n}{\frac {\partial }{\partial r}}r^{n-1}{\frac {\partial }{\partial r}}+r^{-2}\Delta _{S^{n-1}}={\frac {\partial ^{2}}{\partial r^{2}}}+{\frac {n-1}{r}}{\frac {\partial }{\partial r}}+r^{-2}\Delta _{S^{n-1}}}$
• It follows from the Stokes theorem and the preceding property that the spaces H are orthogonal with respect to the inner product from L2(Sn−1). That is to say,
${\displaystyle \int _{S^{n-1}}f{\bar {g}}\,d\Omega =0}$
for f ∈ H and g ∈ Hk for k ≠ ℓ.
• Conversely, the spaces H are precisely the eigenspaces of ΔSn−1. In particular, an application of the spectral theorem to the Riesz potential ${\displaystyle \Delta _{S^{n-1}}^{-1}}$ gives another proof that the spaces H are pairwise orthogonal and complete in L2(Sn−1).
• Every homogeneous polynomial P ∈ P can be uniquely written in the form
${\displaystyle P(x)=P_{\ell }(x)+|x|^{2}P_{\ell -2}+\cdots +{\begin{cases}|x|^{\ell }P_{0}&\ell {\rm {\ even}}\\|x|^{\ell -1}P_{1}(x)&\ell {\rm {\ odd}}\end{cases}}}$
where Pj ∈ Aj. In particular,
${\displaystyle \dim \mathbf {H} _{\ell }={\binom {n+\ell -1}{n-1}}-{\binom {n+\ell -3}{n-1}}.}$

An orthogonal basis of spherical harmonics in higher dimensions can be constructed inductively by the method of separation of variables, by solving the Sturm-Liouville problem for the spherical Laplacian

${\displaystyle \Delta _{S^{n-1}}=\sin ^{2-n}\phi {\frac {\partial }{\partial \phi }}\sin ^{n-2}\phi {\frac {\partial }{\partial \phi }}+\sin ^{-2}\phi \Delta _{S^{n-2}}}$

where φ is the axial coordinate in a spherical coordinate system on Sn−1. The end result of such a procedure is[17]

${\displaystyle Y_{l_{1},\dots l_{n-1}}(\theta _{1},\dots \theta _{n-1})={\frac {1}{\sqrt {2\pi }}}e^{il_{1}\theta _{1}}\prod _{j=2}^{n-1}{}_{j}{\bar {P}}_{l_{j}}^{l_{j-1}}(\theta _{j})}$

where the indices satisfy |ℓ1| ≤ ℓ2 ≤ ... ≤ ℓn−1 and the eigenvalue is −ℓn−1(ℓn−1 + n−2). The functions in the product are defined in terms of the Legendre function

${\displaystyle {}_{j}{\bar {P}}_{L}^{l}(\theta )={\sqrt {{\frac {2L+j-1}{2}}{\frac {(L+l+j-2)!}{(L-l)!}}}}\sin ^{\frac {2-j}{2}}(\theta )P_{L+{\frac {j-2}{2}}}^{-(l+{\frac {j-2}{2}})}(\cos \theta )}$

## Connection with representation theory

The space H of spherical harmonics of degree ℓ is a representation of the symmetry group of rotations around a point (SO(3)) and its double-cover SU(2). Indeed, rotations act on the two-dimensional sphere, and thus also on H by function composition

${\displaystyle \psi \mapsto \psi \circ \rho }$

for ψ a spherical harmonic and ρ a rotation. The representation H is an irreducible representation of SO(3).

The elements of H arise as the restrictions to the sphere of elements of A: harmonic polynomials homogeneous of degree ℓ on three-dimensional Euclidean space R3. By polarization of ψ ∈ A, there are coefficients ${\displaystyle \psi _{i_{1}\dots i_{\ell }}}$ symmetric on the indices, uniquely determined by the requirement

${\displaystyle \psi (x_{1},\dots ,x_{n})=\sum _{i_{1}\dots i_{\ell }}\psi _{i_{1}\dots i_{\ell }}x_{i_{1}}\cdots x_{i_{\ell }}.}$

The condition that ψ be harmonic is equivalent to the assertion that the tensor ${\displaystyle \psi _{i_{1}\dots i_{\ell }}}$ must be trace free on every pair of indices. Thus as an irreducible representation of SO(3), H is isomorphic to the space of traceless symmetric tensors of degree ℓ.

More generally, the analogous statements hold in higher dimensions: the space H of spherical harmonics on the n-sphere is the irreducible representation of SO(n+1) corresponding to the traceless symmetric ℓ-tensors. However, whereas every irreducible tensor representation of SO(2) and SO(3) is of this kind, the special orthogonal groups in higher dimensions have additional irreducible representations that do not arise in this manner.

The special orthogonal groups have additional spin representations that are not tensor representations, and are typically not spherical harmonics. An exception are the spin representation of SO(3): strictly speaking these are representations of the double cover SU(2) of SO(3). In turn, SU(2) is identified with the group of unit quaternions, and so coincides with the 3-sphere. The spaces of spherical harmonics on the 3-sphere are certain spin representations of SO(3), with respect to the action by quaternionic multiplication.

### Generalizations

The angle-preserving symmetries of the two-sphere are described by the group of Möbius transformations PSL(2,C). With respect to this group, the sphere is equivalent to the usual Riemann sphere. The group PSL(2,C) is isomorphic to the (proper) Lorentz group, and its action on the two-sphere agrees with the action of the Lorentz group on the celestial sphere in Minkowski space. The analog of the spherical harmonics for the Lorentz group is given by the hypergeometric series; furthermore, the spherical harmonics can be re-expressed in terms of the hypergeometric series, as SO(3) = PSU(2) is a subgroup of PSL(2,C).

More generally, hypergeometric series can be generalized to describe the symmetries of any symmetric space; in particular, hypergeometric series can be developed for any Lie group.[18][19][20][21]

## Notes

1. ^ A historical account of various approaches to spherical harmonics in three-dimensions can be found in Chapter IV of MacRobert 1967. The term "Laplace spherical harmonics" is in common use; see Courant & Hilbert 1962 and Meijer & Bauer 2004.
2. ^ The approach to spherical harmonics taken here is found in (Courant & Hilbert 1966, §V.8, §VII.5).
3. ^ Physical applications often take the solution that vanishes at infinity, making A = 0. This does not affect the angular portion of the spherical harmonics.
4. ^ Edmonds 1957, §2.5
5. ^ Messiah, Albert (1999). Quantum mechanics : two volumes bound as one (Two vol. bound as one, unabridged reprint ed.). Mineola, NY: Dover. ISBN 9780486409245.
6. ^ al.], Claude Cohen-Tannoudji, Bernard Diu, Franck Laloë; transl. from the French by Susan Reid Hemley ... [et (1996). Quantum mechanics. Wiley-Interscience: Wiley. ISBN 9780471569527.
7. ^ Heiskanen and Moritz, Physical Geodesy, 1967, eq. 1-62
8. ^ Watson & Whittaker 1927, p. 392.
9. ^ See, e.g., Appendix A of Garg, A., Classical Electrodynamics in a Nutshell (Princeton University Press, 2012).
10. ^ Edmonds, A. R. Angular Momentum In Quantum Mechanics. Princeton University Press. p. 81.
11. ^ This is valid for any orthonormal basis of spherical harmonics of degree ℓ. For unit power harmonics it is necessary to remove the factor of 4π.
12. ^ Watson & Whittaker 1927, p. 395
13. ^ Unsöld 1927
14. ^ Stein & Weiss 1971, §IV.2
15. ^ Eremenko, Jakobson & Nadirashvili 2007
16. ^
17. ^ Higuchi, Atsushi (1987). "Symmetric tensor spherical harmonics on the N-sphere and their application to the de Sitter group SO(N,1)". Journal of Mathematical Physics. 28 (7). Bibcode:1987JMP....28.1553H. doi:10.1063/1.527513.
18. ^ N. Vilenkin, Special Functions and the Theory of Group Representations, Am. Math. Soc. Transl.,vol. 22, (1968).
19. ^ J. D. Talman, Special Functions, A Group Theoretic Approach, (based on lectures by E.P. Wigner), W. A. Benjamin, New York (1968).
20. ^ W. Miller, Symmetry and Separation of Variables, Addison-Wesley, Reading (1977).
21. ^ A. Wawrzyńczyk, Group Representations and Special Functions, Polish Scientific Publishers. Warszawa (1984).

## References

Cited references
General references
• E.W. Hobson, The Theory of Spherical and Ellipsoidal Harmonics, (1955) Chelsea Pub. Co., ISBN 978-0-8284-0104-3.
• C. Müller, Spherical Harmonics, (1966) Springer, Lecture Notes in Mathematics, Vol. 17, ISBN 978-3-540-03600-5.
• E. U. Condon and G. H. Shortley, The Theory of Atomic Spectra, (1970) Cambridge at the University Press, ISBN 0-521-09209-4, See chapter 3.
• J.D. Jackson, Classical Electrodynamics, ISBN 0-471-30932-X
• Albert Messiah, Quantum Mechanics, volume II. (2000) Dover. ISBN 0-486-40924-4.
• Press, WH; Teukolsky, SA; Vetterling, WT; Flannery, BP (2007), "Section 6.7. Spherical Harmonics", Numerical Recipes: The Art of Scientific Computing (3rd ed.), New York: Cambridge University Press, ISBN 978-0-521-88068-8
• D. A. Varshalovich, A. N. Moskalev, V. K. Khersonskii Quantum Theory of Angular Momentum,(1988) World Scientific Publishing Co., Singapore, ISBN 9971-5-0107-4