University of Chicago

The Thomson scattering cross section depends on polarization as (see e.g. [Chandrasekhar] 1960)

where ( ) are the incident (scattered) polarization directions. Heuristically, the incident light sets up oscillations of the target electron in the direction of the electric field vector , i.e. the polarization. The scattered radiation intensity thus peaks in the direction normal to, with polarization parallel to, the incident polarization. More formally, the polarization dependence of the cross section is dictated by electromagnetic gauge invariance and thus follows from very basic principles of fundamental physics.

If the incoming radiation field were isotropic, orthogonal polarization
states from incident directions separated by would balance so
that the outgoing radiation would remain unpolarized. Conversely,
if the incident radiation field possesses a *quadrupolar* variation
in intensity or temperature (which possess intensity peaks at
separations), the result is a *linear* polarization of the scattered
radiation (see Fig. 1).
A reversal in sign of the temperature fluctuation corresponds to a
rotation of the polarization, which reflects the spin-2
nature of polarization.

Fig. 1: Thomson scattering of radiation with a quadrupole anisotropy generates linear polarization. Blue colors (thick lines) represent hot and red colors (thin lines) cold radiation.

In terms of a multipole decomposition of the radiation field into spherical
harmonics, , the five quadrupole moments are
represented by , .
The orthogonality of the spherical harmonics guarantees that no other moment
can generate polarization from Thomson scattering.
In these spherical coordinates, with the north pole at , we call
a N-S (E-W) polarization component *Q*>0 (*Q*<0) and a NE-SW (NW-SE) component
*U*>0 (*U*<0).
The polarization amplitude and angle clockwise from north are

Alternatively, the Stokes parameters *Q* and *U* represent the diagonal and
off diagonal components of the symmetric, traceless, intensity
matrix
in
the polarization plane spanned by ( , ),

where are the Pauli matrices and circular polarization is assumed absent.

If Thomson scattering is rapid, then the randomization of photon directions
that results destroys any quadrupole anisotropy and polarization.
The problem of understanding the polarization pattern of the CMB thus reduces
to understanding the quadrupolar temperature fluctuations at *last*
scattering.

Temperature perturbations have 3 geometrically distinct sources: the scalar (compressional), vector (vortical) and tensor (gravitational wave) perturbations. Formally, they form the irreducible basis of the symmetric metric tensor. We shall consider each of these below and show that the scalar, vector, and tensor quadrupole anisotropy correspond to respectively. This leads to different patterns of polarization for the three sources as we shall discuss in §3.

** Next:** Scalar Perturbations