In a full-sky cubic bispectrum estimator, pairwise Gaussian covariance within one triple gives a sum of Gaunt integrals with opposite indices. The spherical harmonic addition theorem turns their pair into the constant ; its integral against vanishes for . A zero temperature monopole removes . Thus only the six pairings connecting the two triples survive in the Gaussian variance; isotropic weights are essential for the cancellation.
Let denote the template at unit , and define . All sums below are over ordered triples of the retained multipoles, with the monopole removed and . A finite maximum multipole makes these expressions ordinary finite sums. Taking the expectation of the cubic numerator and using the template relation gives
Thus the full-sky cubic bispectrum estimator is unbiased for
The assumed template must have nonzero support, so . Using the Gaunt sum rule, write
The factor belongs to the ordered sum; an unordered triangle sum would instead use multiplicity factors for equal multipoles. This normalization is also the Gaussian Fisher information for the template amplitude.
For the cosmic variance, use the reality condition and Gaussian covariance
There are pairings of the six multipoles in the squared cubic numerator. Six pairings connect every factor in the first triple to a factor in the second. Each gives . The covariance phases cancel: nonzero Gaunt integrals have , and simultaneous reversal of the three indices multiplies the Gaunt integral by .
The other nine pairings contain one contraction within each triple. To see why their sums vanish, contract two legs of a Gaunt integral and use the spherical harmonic addition theorem:
The template and inverse-covariance weights are independent of , so they do not spoil this cancellation. The only possible surviving unpaired mode is the monopole, and removes it. This is monopole cancellation of internal cubic-estimator contractions. It explains why no linear correction is needed in this ideal full-sky isotropic problem; masks or anisotropic noise would spoil the argument.
The cubic numerator therefore has Gaussian variance . Dividing by gives
The result concerns the Gaussian-limit covariance. Non-Gaussian connected four- and six-point terms can change the variance at finite amplitude. Unbiasedness uses the assumed linear template relation for the observed three-point function.
A scalar cosmological perturbation at fixed wavevector carries no helicity or distinguished transverse direction. Its metric and scalar sources are unchanged by rotations around , and the scalar baryon peculiar velocity is longitudinal. With scalar initial conditions, rotational invariance of the linear evolution therefore makes a function only of . Expand it using the stated normalization, without an extra factor:
In the Thomson kernel, . The spherical harmonic addition theorem and Orthogonality of Legendre polynomials give
Only the monopole and quadrupole survive; the quadrupole's gives the angular scattering integral
This also explains why an isotropic distribution has zero net collision term.
The streaming term and the Legendre polynomial recurrence relation yield, after division by , . With , the velocity collision source is in the dipole equation; the gravitational gradient source is . Therefore the photon Boltzmann hierarchy is
Set the absent contribution to zero. This is algebraically the printed hierarchy. In particular,
Since , these collision terms damp the nonzero multipoles and drive the dipole to . The latter sign follows from the paper's velocity and conventions, not a reversed physical photon velocity.