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P. B. Keegstra1, C. L. Bennett2,
G. F. Smoot3, K. M. Gorski4,
G. Hinshaw2, L. Tenorio5
1Hughes STX Corporation
2Laboratory for Astronomy and Solar Physics,
NASA/Goddard Space Flight Center
3Lawrence Berkeley Laboratory, University of California,
Berkeley
4Theoretical Astrophysics Center, Denmark and
Warsaw University Observatory, Poland
5Universidad Carlos III de Madrid, Spain
Generalized spherical harmonics are an extension of ordinary spherical harmonics, intended for expansion of functions whose transformation properties at each point on the sphere are more complex than just scalars. The general form
has three indices , m, and n where
and
(Gel'fand et al. 1963).
The forms appropriate for expanding complex Stokes
parameters
and
are (Sazhin & Korolëv 1985)
Since and
are real and
, the two expansions
are degenerate, and we may restrict our consideration
to the first form.
Thus, for the DMR case we need only consider
generalized spherical harmonics with n=2,
which we will henceforth refer to as
.
The are complex expansion coefficients, analogues of
the
of ordinary spherical harmonic expansions of
scalar quantities. Like them, the
for a given
transform among themselves in a coordinate transformation,
but the absolute sum
is invariant.
Following recent work by Zaldarriaga & Seljak (1997)
and Kamionkowski et al. (1997), we can partition
the independent real parameters per value of
into those associated with even-parity solutions and odd-parity
solutions, called E-like and B-like respectively by Zaldarriaga
& Seljak. The formula appropriate for the phase convention used
here is
Figure: Geometry for definitions
of and
(Kosowsky 1996).
Original PostScript figure (48kB).
Generalized spherical harmonics obey a sum rule
analogous to a familiar one for ordinary spherical harmonics,
but it includes an explicit phase factor which depends
on the orientation of the two lines of sight.
That phase factor depends on the angle which
carries the reference direction for line of sight
into the reference direction for line of sight
.
The geometry of
and
is illustrated
in Figure 1.
,
which has the following geometric interpretation.
The reference direction is rotated by
into the great circle from
to
,
translated to
, and then rotated through
to bring it
into alignment with the reference direction at
.
(
is the angle between
and
).
With that definition of , the sum rule relating generalized
spherical harmonics along two lines of sight to
the angle
between those lines of sight is
If this phase factor is included in the definition
of the spherical average
over all directions and
separated
by an angle
where ,
then this allows us to define rotationally invariant
analogues
to the power spectra
:
Additionally, we can construct analogous sums
of and
,
which we denote as
and
respectively.
These
are the appropriate quantities to use for
comparison to theoretical treatments of polarization.
The partitioning into
and
is
pertinent since Zaldarriaga & Seljak (1996)
and Kamionkowski et al. (1996) both show that
scalar perturbations cannot produce a nonzero
.
It is interesting to note that ,
which implies that correlations between physical polarization
signals vanish at the antipodes.
The National Aeronautics and Space Administration (NASA)/Goddard Space Flight Center (GSFC) is responsible for the design, development, and operation of the Cosmic Background Explorer ( COBE ). Scientific guidance is provided by the COBE Science Working Group. GSFC is also responsible for the development of analysis software and for the production of the mission data sets.
Fruitful discussions with M. Jacobsen, University of Maryland Department of Mathematics, and B. Summey, Hughes STX, are gratefully acknowledged.
Gel'fand, I. M., Minlos, R. A., & Shapiro, Z. Y. 1963, Representations of the Rotation and Lorentz Groups and their Applications (New York: Pergamon Press)
Kamionkowski, M., Kosowsky, A., & Stebbins, A. 1997, Phys. Rev. Lett., 78, 2038
Kosowsky, A. 1996, Ann. Phys., 246, 49
Sazhin, M. V., & Korolëv, V. A. 1985, Sov. Astron. Lett., 11, 204
Zaldarriaga, M., & Seljak, U. 1997, Phys. Rev. D, in press
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