![]() | Annu. Rev. Astron. Astrophys. 1994. 32:
319-70 Copyright © 1994 by Annual Reviews. All rights reserved |
2.3. The Correlation Function
It is conventional in CMB work to expand the temperature fluctuations in spherical harmonics
![]() | (3) |
and work in terms of the multipole moments
am. One
can define the sky correlation function
![]() | (4) |
where the average is taken over the (observed) sky with the separation
angle 21 held
fixed. Using the properties of
Y
m the
correlation function
Csky(
21) (hereafter we will drop the
subscript "sky") is
![]() | (5) |
where we have introduced the rotationally symmetric quantity
a2
m
|a
m|2. The
a
2
are not to be confused with
(2
+ 1)
C
(see
later) which is
often used to define the power spectrum of fluctuations in a Gaussian
theory. At this point we have made no assumption about the underlying
theory of fluctuations or the model of structure formation - the
a
2
are purely measured quantities on the sky. [Note that other authors'
definitions of various quantities can differ from ours by
4
,
(2
+ 1), or similar
factors.] The COBE team
(C. Bennett et al 1992,
Kogut et al 1993,
Fixsen et al 1994,
Bennett et al 1994)
quote results for the first two moments, i.e.
a
T0 /
(4
) for
= 1, 2,
![]() | (6) |
A common way of comparing theory and experiment is through the
am. Of
course an actual measurement of a temperature difference on
the sky involves finite resolution and specific measurement strategies
modifying Equation 5. These are usually included in the theoretically
predicted correlation function through a window or filter function,
W
,
described in Section 4.2.