Spherical Harmonics
In the early 2000's, people like Ravi Ramamoorthi^{2} and PeterPike Sloan^{4} introduced a new powerful and amazing tool to the Computer Graphics society: Spherical Harmonics (or SH).
Although Spherical Harmonics have always been around for quite some time, for example in the excellent 1992 paper from Westin et al. ^{1} (and well before that in quantum physics!),
they only piqued the public interest since their introduction as an efficient way of creating realistic and interactive indirect lighting rendering via Precomputed Radiance Transfer (PRT).
What are Spherical Harmonics?
Visual representations of the first 4 bands of real spherical harmonic functions. Blue portions are regions where the function is positive, and yellow portions represent regions where it is negative.
Image created by Iñigo Quilez.
According to wikipedia, SH are special functions defined on the surface of a sphere.
In computer graphics, we're using them as a tool to quickly and easily encode or decode a directional information. We use a specific set of spherical harmonics, denoted Y^m_l(\theta,\phi) called Laplace's spherical harmonics.
SH have interesting properties regarding their orthogonality, parity, symmetry and rotation that I will not cover here (cf. the wikipedia page for more info) as this page only is an overview. An excellent source of information is "Spherical Harmonics Lighting: the Gritty Details" by Robin Green ^{5} that actually covers the practical use of SH for Computer Graphics, it's a wellexplained extension of the original work done by PeterPike Sloan about Precomputed Radiance Transfer (PRT).
I will rather quickly talk about how to construct the SH coefficients and how to encode / decode / convolve signals using SH.
Generalities about SH orders
As can be seen in the inset on the right beautifully rendered by Iñigo Quilez (iQ), Spherical Harmonics are functions defined over the sphere. The SH functions are denoted Y^m_l(\theta,\phi) where l is the order of the function. Since SH define harmonic series, there are an infinite amount of possible orders.
For a given order l you have 2l+1 coefficients selected by the superscript m\in[l,+l]. It ensues that the indices and amount of coefficients for each order is then:
Order  Coefficient Indices  Coefficients Count  Total 

0  0  1  1² 
1  1 2 3  3  1 + 3 = 4 = 2² 
2  4 5 6 7 8  5  1 + 3 + 5 = 9 = 3² 
3  9 10 11 12 13 14 15  7  1 + 3 + 5 + 7 = 16 = 4² 
\dots  \dots  \dots  \dots 
N  2N+1  (N+1)^2 
We quickly see the amount of coefficients to properly represent each order grows quadratically.
[[File:SHSignalReconstruction.pngthumbright400pxEncoding of a signal in SH with increasing orders of approximation (from Robin Green).]]
Intuitively, we also can notice that the more coefficients we have, the more "directionalities" we can cover (i.e. the higher frequencies we can reach). Order 0 is a constant so it represents the "ambient term" — the average response of a signal — and has no specific direction. Coefficients for order 1 represent the response to a signal aligned with the X, Y and Z axes. At order 2, we start covering some diagonal directions and higher frequencies, and so on...
In fact, if we used an infinite sum of SH coefficients, we could encode or decode a signal perfectly. A great advantage of using SH is that we can recover a partial signal (i.e. a bandlimited signal) and we will obtain a lowfrequency representation of that signal, as opposed to wavelets that attempt to reconstruct all frequencies of a signal and can show highfrequency noise, a partial SHencoded signal will always be smooth.
It is common in realtime computer graphics to use only order 2 (9 coefficients) or order 3 (16 coefficients) at most, each coefficient being a RGB float3 triplet. SH are often used to encode irradiance, which is generally spatially varying pretty smoothly. Although it varies at higher frequency than irradiance, it is also possible to encode the radiance into SH.
Actually, both radiance and irradiance are related in terms of SH, as explained by this great 2001 paper from Ramamoorthi and Hanrahan^{2}.
It was shortly followed by another seminal paper called "An Efficient Representation for Irradiance Environment Maps"^{3} that extends on the first paper and shows that order 2 SH (9 coefficients) is often enough to properly represent the irradiance field surrounding an object since additional order disappear very quickly. We will come back to these papers later as I will show an extension on this irradiance estimate to introduce the Ambient Occlusion term.
Note
It is sometimes desirable to express a SH coefficient Y^m_l(\theta,\phi) by a single index Y_i(\theta,\phi) where i=l(l+1)+m. It can be noted that l(l+1) gives us the "central index" (If you refer to the pyramid of coefficient indices above, these are the bold indices 0, 2, 6, 12, 20, 30, etc.) for any given order l, then adding m will address the "left" or "right" coefficients depending on the sign of m. Inversely, when we want to retrieve l, m from i then l=\lfloor\sqrt{i}\rfloor and m=i  l(l+1).
Constructing the SH Coefficients
We're working with a ZUp orientation:
The expression of vector v in cartesian coordinates is v(\theta,\phi) = (\sin(\theta)\cos(\phi), \sin(\theta)\sin(\phi), \cos(\theta)).
The general spherical harmonics coefficients Y^m_l(\theta,\phi) are expressed as: Y^m_l(\theta,\phi) = K^m_l P^m_l(cos(\theta)) e^{im\phi}
Where K^m_l = \sqrt{ \frac{(2l+1)}{4\pi}\frac{(lm)!}{(l+m)!}} is a normalization factor and P^m_l(\theta,\phi) is the associated Legendre polynomial (shown on the right inset figure).
We're interested in the real form of spherical harmonics that is given by:
$$
Y^m_l(\theta,\phi) =
\begin{cases}
\sqrt{2} K^{m}_l P^{m}_l(cos(\theta)) \sin(m\phi) & \quad \text{if } m < 0\\
K^0_l P^0_l(cos(\theta)) & \quad \text{if } m = 0\\
\sqrt{2} K^m_l P^{ m }_l(cos(\theta)) cos(m\phi) & \quad \text{if } m > 0\\
\end{cases}
$$
Here is a code snippet (source Robin Green's "gritty details"^{5}) about how to build the SH functions:
// Renormalisation constant for SH function double K( int l, int m ) { double temp = ((2.0*l+1.0)*factorial(lm)) / (4.0*PI*factorial(l+m)); // Here, you can use a precomputed table for factorials return sqrt(temp); } // Evaluate an Associated Legendre Polynomial P(l,m,x) at x // For more, see “Numerical Methods in C: The Art of Scientific Computing”, Cambridge University Press, 1992, pp 252254 double P( int l, int m,double x ) { double pmm = 1.0; if ( m > 0 ) { double somx2 = sqrt((1.0x)*(1.0+x)); double fact = 1.0; for ( int i=1; i<=m; i++ ) { pmm *= (fact) * somx2; fact += 2.0; } } if( l == m ) return pmm; double pmmp1 = x * (2.0*m+1.0) * pmm; if ( l == m+1 ) return pmmp1; double pll = 0.0; for ( int ll=m+2; ll<=l; ++ll ) { pll = ( (2.0*ll1.0)*x*pmmp1(ll+m1.0)*pmm ) / (llm); pmm = pmmp1; pmmp1 = pll; } return pll; } // Returns a point sample of a Spherical Harmonic basis function // l is the band, range [0..N] // m in the range [l..l] // theta in the range [0..Pi] // phi in the range [0..2*Pi] double SH( int l, int m, double theta, double phi ) { const double sqrt2 = sqrt(2.0); if( m == 0 ) return K(l,0)*P(l,m,cos(theta)); else if( m > 0 ) return sqrt2*K(l,m)*cos(m*phi)*P(l,m,cos(theta)); else return sqrt2*K(l,m)*sin(m*phi)*P(l,m,cos(theta)); }
Analytical Expressions for the first SH Coefficients
As indicated in the beginning of this page, most realtime applications only use a limited amount of SH orders (2, 3 or more rarely 4 orders) so we're usually dealing with at most 9 or 16 SH coefficients.
These coefficients have analytical expressions that we are now listing below (we dropped the \theta,\phi for conciseness):
Order l=0
Order l=1
Order l=2
Where: $$ \begin{cases} x = \sin(\theta)\cos(\phi)\\ y = \sin(\theta)\sin(\phi)\\ z = \cos(\theta)\\ \end{cases} $$
Common Usages for SH
Signal Encoding
A signal f(\theta,\phi) whose value is available for all directions can be encoded (or rather, projected) into SH coefficients by estimating the following integral:
To implement this integration numerically we can use the naïve pseudocode:
float EncodeSHCoeff( int l, int m ) { const int STEPS_PHI = 200; const int STEPS_THETA = 100; const float dPhi = 2*PI/STEPS_PHI; const float dTheta = PI/STEPS_THETA; float coeff = 0.0f; for ( int i=0; i < STEPS_PHI; i++ ) { float phi = i * dPhi; for ( int j=0; j < STEPS_THETA; j++ ) { float theta = (0.5f+j) * dTheta; float value = EstimateFunction( phi, theta ); float SHvalue = EstimateSH( l, m, phi, theta ) coeff += value * SHValue * sin( theta ) * dPhi * dTheta; } } return coeff; }
A better (and faster!) way to do that would be to use importance sampled Monte Carlo sampling. Please refer to Robin Green's paper for details about the technique.
We first need to generate an arbitrary set of samples on the sphere. We choose the samples so that they are uniformly distributed on the sphere, thus ensuring that each sample carries the same weight that will be \frac{4\pi}{N} where N is the amount of samples:
struct sample_t { float3 direction; float theta, phi; float* Ylm; }; // Fills an N*N*2 array with uniformly distributed samples across the sphere using jittered stratification void PreComputeSamples( int sqrt_n_samples, int n_bands, sample_t samples[], float ) { int i = 0; // array index double oneoverN = 1.0 / sqrt_n_samples; for ( int a=0; a < sqrt_n_samples; a++ ) { for ( int b=0; b < sqrt_n_samples; b++ ) { // Generate unbiased distribution of spherical coords double x = (a + random()) * oneoverN; // Do not reuse results double y = (b + random()) * oneoverN; // Each sample must be random! double theta = 2.0 * acos( sqrt( 1.0  x ) ); // Uniform sampling on theta double phi = 2.0 * PI * y; // Uniform sampling on phi // Convert spherical coords to unit vector samples[i].direction = float3( sin(theta)*cos(phi), sin(theta)*sin(phi), cos(theta) ); samples[i].theta = theta; samples[i].phi = phi; // precompute all SH coefficients for this sample for ( int l=0; l < n_bands; ++l ) { for ( int m=l; m<=l; ++m ) { int index = l*(l+1)+m; samples[i].Ylm[index] = EstimateSH( l, m, theta, phi ); } } ++i; } } }
We keep that nice array around because we will reuse it for as many encodings as we want by applying that now very straightforward pseudocode:
typedef double (*EstimateFunction)( double theta, double phi ); // Here, n_coeffs = n_bands*n_bands and n_samples = sqrt_n_samples*sqrt_n_samples void SHProject( EstimateFunction estimator, int n_samples, int n_coeffs, const sample_t samples[], double result[] ) { for ( i=0; i < n_coeff; ++i ) { result[i] = 0.0; // For each sample for ( int i=0; i < n_samples; ++i ) { double theta = samples[i].theta; double phi = samples[i].phi; for ( int n=0; n < n_coeff; ++n ) { result[n] += estimator( theta, phi ) * samples[i].Ylm[n]; } } // Divide the result by weight and number of samples double factor = 4.0*PI / n_samples; for ( i=0; i < n_coeff; ++i ) { result[i] = result[i] * factor; } }
Note
Projecting a function into SH coefficients is obviously not something we want to be doing every frame! The goal is to project once, and reuse the SH coefficients all around. The memory gain is enormous: for example imagine you want to encode a distant environment cube map into an order 2 SH to use it as the diffuse radiance source, then assuming you're dealing with a 256x256x6xRGB32F cube map, you start from a 256*256*6*16 = 6 solid Mega Bytes down to a mere 9*12 = 108 Bytes (9 float3 SH coefficients).
Of course, encoding with so little coefficients is sufficient enough for diffuse irradiance estimates and barely anything else, don't expect a great many deal of details out of that!
Signal Decoding
To reconstruct the bandlimited version of the original signal from a bunch of SH coefficients, you simply need to apply the inverse transform:
f(\theta,\phi) \; \simeq \; \displaystyle\sum_{l=0}^{N} \displaystyle\sum_{m=l}^{l} C_l^m Y_l^m(\theta,\phi) where N is the SH order
Note
we used the \simeq sign here because unless N=\infty we will only be able to reconstruct a bandlimited, lowfrequency version of the original signal.
Signal Convolution / Signal Product
This property is certainly the most important regarding SH.
In computer graphics it's often that we need to compute that kind of integral:
$$ \int\limits_\Omega{A(\boldsymbol\omega_i) B(\boldsymbol\omega_i) \; \mathrm{d\omega_i}} $$
Where:
 \Omega represents the set of all directions on the sphere
 A(\boldsymbol\omega_i) and B(\boldsymbol\omega_i) represent 2 arbitrary functions evaluated in direction \boldsymbol{\omega_i} that are convolved together
 \boldsymbol{\omega_i} is the unit integration vector (i.e. the incoming direction)
 \mathrm{d\omega_i} is the solid angle (a scalar!) in the incoming direction
Well, assuming you managed to encode A(\boldsymbol\omega_i) into SH coefficients a_l^m and similarly you obtained the b_l^m SH coefficients corresponding to the B(\boldsymbol\omega_i) signal then the integral in terms of SH simply is:
So we basically reduced a difficult integral computation into a simple dot product!
Note the exact equal sign only stands because we have an infinite number of SH coefficients here. With a finite number, say 9 or 16, we can only obtain an incomplete, bandlimited version of the signal...
Irradiance Estimate Example
The integration of radiance into diffuse irradiance over the hemisphere is given by:
Where:
 L(\mathbf n,\boldsymbol{\omega_i}) is the radiance arriving in incoming direction \boldsymbol{\omega_i}
 E(\mathbf n) is the irradiance perceived in direction \mathbf{n}
 \mathbf n is the surface normal direction
 \lfloor (\mathbf\omega_i\cdot\mathbf n)\rfloor represents the dot product clamped over the upper hemisphere
Assuming you have a SH representation of the surrounding radiance, for example coming from a cube map, then it is easy to analytically compute the SH coefficients for the clamped cosine.
This is exactly the purpose of the 2001 paper by Ramamoorthi et al.^{2} that we will discuss below
Precomputed Radiance Transfer Example
Another example is the surface radiance estimate:
Where:
 L(\boldsymbol{\omega_i}) is the radiance arriving in incoming direction \boldsymbol{\omega_i}
 L(\boldsymbol{\omega_o}) is the radiance leaving in outgoing direction \boldsymbol{\omega_o}
 f_r( \boldsymbol{\omega_o}, \boldsymbol{\omega_i} ) is the surface's BRDF
 \Omega^+ represents the upper hemisphere of directions (so there is no need for the clamped dot product here!)
Again, assuming you have a SH representation of the surrounding radiance (e.g. coming from a cube map or some indirect lighting computation) that we will call L_l^m and also a SH representation of the BRDF and cosine term that we will call T_l^m, the encoded "transfer function", then the outgoing radiance simply is:
Once again we warn about the exact equal sign. In practice, the radiance environment and "BRDF+cosine term" transfer functions are encoded with only a few SH coefficients and can thus only represent very lowfrequency environments.
This is why the SH PRT technique is generally only used to encode slowly varying transfer functions like the diffuse BRDF \frac{\rho}{\pi} where \rho represents the surface's reflectance.
Anyway, you can immediately see the beauty and strong interest SH can bring to the table: you can precompute a (distant) lighting environment in term of SH and place any object within that environment, assuming you know the transfer function for every part of the object you want to light.
For example:
 If the transfer function simply is the BRDF \times cosine term as mentioned above, then your object will simply be directly lit by the environment as is normally the case with standard lighting
 But the interesting part is that, since the transfer function could be anything, it may as well be the BRDF \times cosine term plus what the object perceives of its environment: you would then obtain the direct lighting plus the indirect lighting!
This is illustrated by the image on the right where we increase the realism of the scene's lighting. What's even better is that we can completely change the surrounding lighting environment on the fly at any time for absolutely no cost at all!
You can see an example of that technique applied in my St Jean cathedral project (requires WebGL!).
In this example, I stored 2 bands (order 1 = 4 coefficients) of the precomputed radiance transfer coefficients for every vertex of the model.
Note
Although it seems cool to do that, it's pretty heavy for real game scenes that now use tens of millions of vertices, it's also pretty long to precompute since you must raytrace the scene from every vertex and finally, it's limited to a static environment...
Signal Triple Product
Sometimes we will want to perform another very important operation that takes 2 SH representations of a signal as input and outputs a new SH representation as output: that is called the "triple product".
A basic example would be:
 You have the SH coefficients A_i for the (dynamic) ambient lighting in your environment (e.g. the unoccluded sky light)
 You also have the precomputed SH coefficients B_i representing (static) local shadowing of the environment (e.g. you're inside a room and the environment is only perceived through a door)
 And you want to dynamically obtain the SH coefficients C_i for the "shadowed ambient lighting" (e.g. the occluded sky light that you perceive through the door)
This is a rather complicated operation involving the transfer matrix:
$$
\mathbf{M_{ij}} \; = \; \int\limits_{\Omega} {B(\boldsymbol{\omega_i}) Y_i({\omega_i}) Y_j({\omega_i}) \; \mathrm{d\omega_i}}
$$
Then:
The main problems are:

We don't want to store a matrix for every vertex in the scene! (although the matrix is very sparse, storing SH coefficients for every vertex is already heavy!)

We don't want to perform a matrix multiplication for every vertex either!

Computing the matrix coefficients can be pretty involved as it features some funny stuff like ClebschGordan coefficients and Wigner 3j symbols...
So basically, this technique is pretty heavy and shouldn't be used very often, certainly not at every vertex of a scene!
You can find the code to compute the tripleproduct of 2 sets of SH coefficients in the excellent 2006 paper by John Snyder.
Here is the HLSL version of that code cleaned up for only 9 coefficients:
// Performs the SH triple product r = a * b // From John Snyder (appendix A8) // void SHProduct( const in float4 a[9], const in float4 b[9], out float4 r[9] ) { float4 ta, tb, t; const float C0 = 0.282094792935999980; const float C1 = 0.126156626101000010; const float C2 = 0.218509686119999990; const float C3 = 0.252313259986999990; const float C4 = 0.180223751576000010; const float C5 = 0.156078347226000000; const float C6 = 0.090111875786499998; // [0,0]: 0, r[0] = C0*a[0]*b[0]; // [1,1]: 0,6,8, ta = C0*a[0]+C1*a[6]C2*a[8]; tb = C0*b[0]+C1*b[6]C2*b[8]; r[1] = ta*b[1]+tb*a[1]; t = a[1]*b[1]; r[0] += C0*t; r[6] = C1*t; r[8] = C2*t; // [1,2]: 5, ta = C2*a[5]; tb = C2*b[5]; r[1] += ta*b[2]+tb*a[2]; r[2] = ta*b[1]+tb*a[1]; t = a[1]*b[2]+a[2]*b[1]; r[5] = C2*t; // [1,3]: 4, ta = C2*a[4]; tb = C2*b[4]; r[1] += ta*b[3]+tb*a[3]; r[3] = ta*b[1]+tb*a[1]; t = a[1]*b[3]+a[3]*b[1]; r[4] = C2*t; // [2,2]: 0,6, ta = C0*a[0]+C3*a[6]; tb = C0*b[0]+C3*b[6]; r[2] += ta*b[2]+tb*a[2]; t = a[2]*b[2]; r[0] += C0*t; r[6] += C3*t; // [2,3]: 7, ta = C2*a[7]; tb = C2*b[7]; r[2] += ta*b[3]+tb*a[3]; r[3] += ta*b[2]+tb*a[2]; t = a[2]*b[3]+a[3]*b[2]; r[7] = C2*t; // [3,3]: 0,6,8, ta = C0*a[0]+C1*a[6]+C2*a[8]; tb = C0*b[0]+C1*b[6]+C2*b[8]; r[3] += ta*b[3]+tb*a[3]; t = a[3]*b[3]; r[0] += C0*t; r[6] += C1*t; r[8] += C2*t; // [4,4]: 0,6, ta = C0*a[0]C4*a[6]; tb = C0*b[0]C4*b[6]; r[4] += ta*b[4]+tb*a[4]; t = a[4]*b[4]; r[0] += C0*t; r[6] = C4*t; // [4,5]: 7, ta = C5*a[7]; tb = C5*b[7]; r[4] += ta*b[5]+tb*a[5]; r[5] += ta*b[4]+tb*a[4]; t = a[4]*b[5]+a[5]*b[4]; r[7] += C5*t; // [5,5]: 0,6,8, ta = C0*a[0]+C6*a[6]C5*a[8]; tb = C0*b[0]+C6*b[6]C5*b[8]; r[5] += ta*b[5]+tb*a[5]; t = a[5]*b[5]; r[0] += C0*t; r[6] += C6*t; r[8] = C5*t; // [6,6]: 0,6, ta = C0*a[0]; tb = C0*b[0]; r[6] += ta*b[6]+tb*a[6]; t = a[6]*b[6]; r[0] += C0*t; r[6] += C4*t; // [7,7]: 0,6,8, ta = C0*a[0]+C6*a[6]+C5*a[8]; tb = C0*b[0]+C6*b[6]+C5*b[8]; r[7] += ta*b[7]+tb*a[7]; t = a[7]*b[7]; r[0] += C0*t; r[6] += C6*t; r[8] += C5*t; // [8,8]: 0,6, ta = C0*a[0]C4*a[6]; tb = C0*b[0]C4*b[6]; r[8] += ta*b[8]+tb*a[8]; t = a[8]*b[8]; r[0] += C0*t; r[6] = C4*t; // entry count=13 // **multiplications count=120** // **addition count=74** }
About Distant Radiance and Irradiance Environments
So let's delve deeper into Ramamoorthi's paper^{2} that establishes the relationship between radiance and irradiance in terms of SH coefficients.
Estimating the lambertian BRDF SH coefficients
Ramamoorthi states that irradiance E(\mathbf n ) reflected by a diffuse Lambertian surface is written:
Where:
 E(\mathbf n) represents the irradiance estimate along normal direction \mathbf n
 L(\boldsymbol{\omega_i}) represents the radiance along incoming direction \boldsymbol{\omega_i}
 \Omega(\mathbf n) is the set of all possible directions over the sphere centered about normal vector \mathbf n
We can write radiance and irradiance in terms of SH coefficients as:
Where \theta_n, \phi_n are the spherical coordinates of the normal vector n.
We saw earlier that the SH product allowed us to estimate integrals like (1) above: assuming A(\theta_i) = \lfloor(\mathbf n \cdot \boldsymbol{\omega_i})\rfloor = \lfloor\cos(\theta_i)\rfloor is representing the transfer function defined over the entire sphere (with clamping so it's 0 in the lower hemisphere) then:
Notice here that we don't use the azimuthal dependence on \phi since the cosine lobe is symmetrical about the vertical axis z: we call this special kind of SH, those with m=0, the Zonal Harmonics (or ZH). They are defined by a single index l defining the order of the ZH. The coefficients are given by:
$$ \begin{equation} A_l \, = \, \int\limits_0^{2\pi} \int\limits_0^\pi \lfloor\cos(\theta_i)\rfloor Y_l^0(\theta_i) \sin(\theta_i) \; \mathrm{d\theta_i} \; \mathrm{d\phi_i}\\ = 2\pi \int\limits_0^{\frac{\pi}{2}} \cos(\theta_i) Y_l^0(\theta_i) \sin(\theta_i) \; \mathrm{d\theta_i} \qquad (4) \quad\\ \end{equation} $$ (notice we changed the integration interval and got rid of the floor operator)
Now if we expand Y_l^0(\theta) in terms of Legendre polynomials we get:
$$
Y_l^0(\theta) \, = \, \sqrt{\frac{2l+1}{4\pi}} \, P_l(\cos(\theta))
$$
We can then rewrite (4) as:
$$
A_l \, = \, 2\pi \sqrt{\frac{2l+1}{4\pi}} \int\limits_0^{\frac{\pi}{2}} P_l(\cos(\theta_i)) \cos(\theta_i) \sin(\theta_i) \; \mathrm{d\theta_i} \qquad (5)
$$
Letting u=\cos(\theta_i) and noting that \cos(\theta_i)=P_1(\cos(\theta_i)) (or P_1(u)=u now), we obtain:
$$
A_l \, = \, 2\pi \sqrt{\frac{2l+1}{4\pi}} \int\limits_0^1 P_l(u) P_1(u) \; \mathrm{du} \qquad (6)
$$
Notice once again the integration interval changed: it was reversed because of the minus sign coming with the fact that \mathrm{du}=\sin(\theta_i) \mathrm{d\theta_i}.
Performing a numerical integration of the first 20 ZH orders, we can plot the values of the Lambertian BRDF coefficients A_l (from Ramamoorthi):
Ramamoorthi notices that:

for l=1 : \qquad A_1 = \sqrt{\pi/3}

for l>1, \; odd : \quad A_l = 0

for l \; even : \quad A_l = 2\pi\sqrt{\frac{2l+1}{4\pi}} \frac{(1)^{l/21}}{(l+2)(l1)} \left(\frac{l!}{2^l(l!/2)^2}\right) and decreases very rapidly (A_l \propto l^{2})
Rewriting the diffuse reflection in terms of SH
We can now write the SH version of the diffuse reflection integral (1) from the previous section:
I skipped the description of the full rotation of the incoming lighting but it now comes into play as the expression R^l_{m,m'}(\theta_n) \sin(m \phi_n) where R^l_{m,m'}(\theta_n) represents a (2l+1)\times(2l+1) matrix that tells us how a SH transforms under rotation about the Y axis, i.e., how to rewrite a rotated SH as a linear combination of all the SH of the same order.
This matrix is further simplified by the fact that the transfer function A = \cos(\theta_n) has no azimuthal dependence so terms with m'\neq0 will vanish.
It can be shown that: $$ R^l_{m,0}(\theta_n) sin(m \phi_n) \, = \, \sqrt{\frac{4\pi}{2l+1}} Y_l^m(\theta_n, \phi_n) $$
So we can finally rewrite equation (7) as: $$ E(\theta_n, \phi_n) \; = \; \displaystyle\sum_{l,m} \sqrt{\frac{4\pi}{2l+1}} \, A_l \, L_l^m \, Y_l^m(\theta_n, \phi_n) \qquad (8) $$
And since we know from equation (3) that: $$ E(\theta_n, \phi_n) \; = \; \displaystyle\sum_{l,m} E_l^m \, Y_l^m(\theta_n, \phi_n) $$
We can finally write: $$ E_l^m \, = \, \sqrt{\frac{4\pi}{2l+1}} \, A_l \, L_l^m $$
For convenience, we put: $$ \hat{A}_l \, = \, \sqrt{\frac{4\pi}{2l+1}} \, A_l $$
And thus: $$ E_l^m \, = \, \hat{A}_l \, L_l^m $$
This result is very interesting since it implies that if you have a valid encoding of the surrounding radiance environment (e.g. from a cube map) in the form of the SH coefficients L_l^m then you can easily obtain the diffuse irradiance SH coefficients E_l^m, that is the radiance convolved by the diffuse Lambertian reflectance operator that is represented here by the \hat{A}_l Zonal Harmonics coefficients.
Also, due to the rapidly decreasing amplitude of \hat{A}_l coefficients, Ramamoorthi states that only a small number SH orders are necessary to properly encode the irradiance. Usually, order 2 (9 coefficients) is enough for most purposes.
Using the result for realtime diffuse irradiance estimation
The first few terms of \hat{A_l} are: $$ \hat{A_0} = \sqrt{4\pi} \, \sqrt{\frac{\pi}{4}} = \pi\\ \hat{A_1} = \sqrt{\frac{4\pi}{3}} \, \sqrt{\frac{\pi}{3}} = \frac{2\pi}{3} = 2.094395\\ \hat{A_2} = \sqrt{\frac{4\pi}{5}} \, \sqrt{\frac{5\pi}{4}} \frac{1}{4} = \frac{\pi}{4} = 0.785398\\ \hat{A_3} = 0\\ \hat{A_4} = \sqrt{\frac{4\pi}{9}} \, \frac{\sqrt{9\pi}}{48} = \frac{\pi}{24} = 0.130900\\ \hat{A_5} = 0\\ \hat{A_6} = \sqrt{\frac{4\pi}{13}} \, \frac{\sqrt{13\pi}}{128} = \frac{\pi}{64} = 0.049087\\ $$
We also gave the analytical SH functions up to order 2 earlier.
Thus, to estimate: $$ E(\mathbf n) \; = \; \displaystyle\sum_{l,m} \hat{A_l} \, L_l^m \, Y_l^m(\mathbf n) $$
We only need to apply the following HLSL code:
// Evaluates the irradiance perceived in the provided direction // Analytic method from http://www1.cs.columbia.edu/~ravir/papers/envmap/envmap.pdf eq. 13 // float3 EvaluateSHIrradiance( float3 _Direction, float3 _SH[9] ) { const float c1 = 0.42904276540489171563379376569857; // 4 * Â2.Y22 = 1/4 * sqrt(15.PI) const float c2 = 0.51166335397324424423977581244463; // 0.5 * Â1.Y10 = 1/2 * sqrt(PI/3) const float c3 = 0.24770795610037568833406429782001; // Â2.Y20 = 1/16 * sqrt(5.PI) const float c4 = 0.88622692545275801364908374167057; // Â0.Y00 = 1/2 * sqrt(PI) float x = _Direction.x; float y = _Direction.y; float z = _Direction.z; return max( 0.0, (c1*(x*x  y*y)) * _SH[8] // c1.L22.(x²y²) + (c3*(3.0*z*z  1)) * _SH[6] // c3.L20.(3.z²  1) + c4 * _SH[0] // c4.L00 + 2.0*c1*(_SH[4]*x*y + _SH[7]*x*z + _SH[5]*y*z) // 2.c1.(L22.xy + L21.xz + L21.yz) + 2.0*c2*(_SH[3]*x + _SH[1]*y + _SH[2]*z) ); // 2.c2.(L11.x + L11.y + L10.z) }
Extension to account for the Ambient Occlusion term
So all is well, we can now estimate the diffuse radiance reflection easily and when it comes to integrating the ambient occlusion (AO) term to modulate the indirect lighting, people usually simply apply AO * DiffuseIrradiance. Here, we show a more accurate way to estimate the irradiance by accounting for ambient occlusion as well.
To illustrate the concept of Ambient Occlusion, I like to imagine a "cone of vision" from the point of view of the surface that represents the set of directions in which the light can reach the surface without any occlusion from the surrounding environment:
In this figure we see the "bent normal" which is oriented toward the direction of least occlusion as well as the "ambient cone" whose halfangle \theta_{AO} \, = \, \frac{\pi}{2} \, AO lets a reduced amount light be perceived by the surface.
So basically, when AO = 1 the cone is fully open and we fallback to the full hemisphere irradiance estimate. When AO = 0, the cone is fully closed and no light is perceived nor reflected by the surface.
It is often not clear what is the distance we need to trace from a surface to estimate it is "not occluded". When unspecified, the distance should be infinite and the perceived environment will be an infinitely distant environment like the ambient sky.
But when we're dealing with some closed models then we need to specify a finite distance otherwise the model would be completely occluded (AO=0) and the ambient occlusion would serve no purpose. In fact, AO is always used to only modulate indirect lighting — sometimes called "ambient lighting" — and it's completely wrong to use it to modulate direct lighting (unless it's called something else, like a cavity map) and thus the distance at which to estimate the AO should be closely related to the distance at which you sample the indirect lighting.
It's important to notice that AO is not something that exists when you deal with actual path tracing as it's intrinsically embedded into the global illumination computation. AO is only a trick that is used for realtime graphics, a way to precompute the "amount of rays" a surface perceives to gather indirect lighting...
Estimating the new Diffuse Reflectance Terms
If we come back to equation (6) from earlier: $$ A_l \, = \, 2\pi \sqrt{\frac{2l+1}{4\pi}} \int\limits_0^1 P_l(u) P_1(u) \; \mathrm{du} $$
We can notice that the integration boundaries are 0 and 1 that respectively correspond to \cos(\pi/2) \text{ and } \cos(0) because we integrate over the entire upper hemisphere of directions.
All we have to do is restrict the integration bounds and integrate from \cos(\theta_{AO}) to 1 instead:
We can do this analytically for the first few coefficients using the first Legendre polynomials given by Wikipedia:
For the rest of the discussion, we'll let t=\cos(\theta_{AO}).
 Order 0 
Carrying the integration of (9) for order 0 gives us:
Thus:
 Order 1 
Carrying the integration of (9) for order 1 gives us:
Thus: $$ \hat{A_1}'(\theta_{AO}) = \sqrt{\frac{4\pi}{3}} \, \left[\sqrt{\frac{\pi}{3}} \left(1  t^3\right)\right] = \frac{2\pi}{3} \left(1t^3\right) $$
 Order 2 
Carrying the integration of (9) for order 2 gives us:
Thus:
Discussion
You can see here the effect of Ambient Occlusion on diffuse lambertian reflectance coefficients.
The black curve is the numerical integration of the coefficients up to order 20 (order is represented horizontally).
The Red, Green and Blue dots are the values analytically computed for orders 0, 1 and 2 using the above integrals:
It is interesting to note a few things about the Red, Green and Blue coefficients:
 They are not at all negligible
 They don't simply vanish proportionally to the AO factor as a simple multiplication would imply
 Their relative importance changes with the AO value: we can see the blue coefficient rises up before decreasing again, indicating an increase in the importance of 2^{nd} order SH terms
 Contrary to what Ramammorthi found, the coefficients for odd orders no longer vanish which means that the sharper the cone gets, the more the directional terms become important.
It's also quite natural to think that the more directional the cone gets, the more we're going to end up sampling radiance instead of irradiance...
As for the general shape of the black curve, we notice that the numerical integration yields some kind of attenuated sine wave whose amplitude and frequency decreases along with the AO factor.
It made me curious about the fact there must exist a "continuous Legendre polynomial" that can be evaluated at noninteger degree and indeed it does exist and it is called the Legendre Function.
It involves:

A very interesting branch of mathematics called Fractional calculus, that allows us to take fractional powers of the differentiation operator.
For example imagine f^\frac{1}{2}(x) to be the "half differential operator" then applying twice gives f^\frac{1}{2}( f^\frac{1}{2}(x) ) = \frac{d}{dx} f(x) = f'(x) 
The gamma function which is the natural extension of the factorial operator x! to the set of complex numbers
Using the new results
As Ramamoorthi puts it, starting from equation (8): $$ E(\theta_n, \phi_n) \; = \; \displaystyle\sum_{l,m} \sqrt{\frac{4\pi}{2l+1}} \, A_l \, L_l^m \, Y_l^m(\theta_n, \phi_n) $$
And using the analytical expressions for Y_l^m(\theta_n, \phi_n), we can expand the complete expression:
E(\mathbf{n}) \, = \, \left( \hat{A'_0}(AO) \; \frac{1}{2}\sqrt{\frac{1}{\pi}} \right) \; L_0^0 \quad +
\quad \left( \hat{A'_1}(AO) \; \frac{1}{2}\sqrt{\frac{3}{\pi}} \, y \right) \; L_1^{1} \quad + \quad \left( \hat{A'_1}(AO) \; \frac{1}{2}\sqrt{\frac{3}{\pi}} \, z \right) \; L_1^0 \quad + \quad \left( \hat{A'_1}(AO) \; \frac{1}{2}\sqrt{\frac{3}{\pi}} \, x \right) \; L_1^1 \quad +
\quad \left( \hat{A'_2}(AO) \; \frac{1}{2}\sqrt{\frac{15}{\pi}} \, xy \right) \; L_2^{2} \quad + \quad \left( \hat{A'_2}(AO) \; \frac{1}{2}\sqrt{\frac{15}{\pi}} \, yz \right) \; L_2^{1} \quad + \quad \left( \hat{A'_2}(AO) \; \frac{1}{4}\sqrt{\frac{5}{\pi}} \, \left(3z^21\right) \right) \; L_2^0 \quad + \quad \left( \hat{A'_2}(AO) \; \frac{1}{2}\sqrt{\frac{15}{\pi}} \, zx \right) \; L_2^1 \quad + \quad \left( \hat{A'_2}(AO) \; \frac{1}{4}\sqrt{\frac{15}{\pi}} \, \left(x^2  y^2\right) \right) \; L_2^2
Each individual c_l^m term can be obtained as: $$ c_0^0 = \hat{A'_0}(AO) \times Y_0^0 = \left[\pi \left(1t^2\right)\right] \times \left[\frac{1}{2}\sqrt{\frac{1}{\pi}}\right] = \frac{1}{2}\sqrt{\pi} \left(1t^2\right) $$
Where c_1 = \sqrt{\frac{\pi}{3}} \left(1t^3\right).
Where c_2 = \frac{1}{16} \sqrt{5\pi} \left[3\left(1t^4\right)2\left(1t^2\right)\right].
Finally, we can write the new and improved HLSL code using a few extra instructions:
// Evaluates the irradiance perceived in the provided direction, also accounting for Ambient Occlusion // Details can be found at http://wiki.nuaj.net/index.php?title=SphericalHarmonicsPortal // Here, _CosThetaAO = cos( PI/2 * AO ) and represents the cosine of the halfcone angle that drives the amount of light a surface is perceiving // float3 EvaluateSHIrradiance( float3 _Direction, float _CosThetaAO, float3 _SH[9] ) { float t2 = _CosThetaAO*_CosThetaAO; float t3 = t2*_CosThetaAO; float t4 = t3*_CosThetaAO; float ct2 = 1.0  t2; float c0 = 0.88622692545275801364908374167057 * ct2; // 1/2 * sqrt(PI) * (1t^2) float c1 = 1.02332670794648848847955162488930 * (1.0t3); // sqrt(PI/3) * (1t^3) float c2 = 0.24770795610037568833406429782001 * (3.0 * (1.0t4)  2.0 * ct2); // 1/16 * sqrt(5*PI) * [3(1t^4)  2(1t^2)] const float sqrt3 = 1.7320508075688772935274463415059; float x = _Direction.x; float y = _Direction.y; float z = _Direction.z; return max( 0.0, c0 * _SH[0] // c0.L00 + c1 * (_SH[1]*y + _SH[2]*z + _SH[3]*x) // c1.(L11.y + L10.z + L11.x) + c2 * (_SH[6]*(3.0*z*z  1.0) // c2.L20.(3z²1) + sqrt3 * (_SH[8]*(x*x  y*y) // sqrt(3).c2.L22.(x²y²) + 2.0 * (_SH[4]*x*y + _SH[5]*y*z + _SH[7]*z*x))) // 2sqrt(3).c2.(L22.xy + L21.yz + L21.zx) ); }
Here is a demonstration of the new result as a sidebyside comparison of a simple sphere illuminated by the Ennis environment: on the left I'm simply doing AO*irradiance while on the right I'm using the new irradiance estimate accounting for the AOguided aperture angle.
Tangent space irradiance estimates
In the presentation "Adding RealTime, PointBased Global Illumination to Video Games: Lessons Learned" (2010), Michael Bunnel talks about computing 3 irradiance values per sample point (i.e. per vertex) and an additional value through the surface for translucency using a variant on the HL2 tangentspace basis but with vectors at 45° from the surface normal:
// Reflection vectors in tangent space are constant // (45º from normal and 180º, 60º, and 60º around normal vector) const float3 r1 = float3(0.7071, 0, 0.7071); const float3 r2 = float3(0.35355, 0.61237, 0.7071); const float3 r3 = float3(0.35355, 0.61237, 0.7071);
This allows to only transport 4 values from vertex to pixel shader and to save a lot of interpolators as opposed to transporting the 9 * float3 for the entire SH coefficients (that would require 7 * float4 interpolators which is far too much!).
Then, in the pixel shader, you simply interpolate the irradiance value depending on the orientation of the normal in the surface's tangent space.
If we look at the basis from the top, we see that each of the 3 vectors covers a 120° sector:
But from the side, we see that each of the 3 vectors covers a 90° sector:
In any case, we notice that it might be interesting once again to restrict the angle of the cone we use to estimate the irradiance:
Moreover, we know that:

The maximum cone angle shouldn't be more than 60°

Exceeding a 45° angle then we start sampling radiance in directions that can be below the surface

If we're given the bent normal and an Ambient Occlusion value, then we should also be careful to account for the fact that radiance outside the bent AO cone will not be available
So we need to somehow account for all of these indications to use the best possible direction and cone angle when we estimate irradiance for each of the 3 principal directions.
Todo
@TODO: Find a proper solution for this problem!
Precious References

(1992) "Predicting Reflectance Functions from Complex Surfaces" Stephen Westin et al. ↩

(2001) "On the relationship between radiance and irradiance: determining the illumination from images of a convex Lambertian object" Ravi Ramamoorthi and Pat Hanrahan ↩↩↩↩

(2001) "An Efficient Representation for Irradiance Environment Maps" Ravi Ramamoorthi and Pat Hanrahan ↩

(2002) "Precomputed Radiance Transfer for RealTime Rendering in Dynamic, LowFrequency Lighting Environments" PeterPike Sloan et al. ↩

(2003) "Spherical Harmonics Lighting: the Gritty Details" Robin Green ↩↩

(2006) "Code Generation and Factoring for Fast Evaluation of Loworder Spherical Harmonic Products and Squares" John Snyder ↩

(2008) "Stupid Spherical Harmonics Tricks" PeterPike Sloan et al. ↩

(2010) "Adding RealTime, PointBased Global Illumination to Video Games: Lessons Learned" by Michael Bunnel ↩