All MFs can be expressed as integrals over the excursion set. While the first MF is simply given by the
volume integration of a Heaviside step function
normalized to the total volume
,
For a 3-D Gaussian random field, the average MFs per unit volume can be expressed analytically as follows:
where The above MFs can be indeed interpreted as well-known geometric quantities: the volume fraction
, the total surface area
, the integral mean curvature
, and the integral Gaussian
curvature, i.e., the Euler characteristic
. In our current definitions (see Equations (101
, 108
),
or Equations (102
, 115
)), one can easily show that
reduces simply to
. The
MFs were first introduced to cosmological studies by Mecke et al. [57
], and further details may
be found in [57, 32
]. Analytic expressions of MFs in weakly non-Gaussian fields are derived
in [52].
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