The Fundamental Plane (FP)
was discovered independently and simultaneously by
Djorgovski & Davis (1987) and Dressler et al. (1987b).
It is a relation between
,
,
and
,
and is linear in logarithmic space.
Since
,
the FP can also be expressed as a relation between
L,
,
and
,
or between
,
,
and L.
Djorgovski & Davis (1987) found a tight correlation for elliptical galaxies
between either a radius or the luminosity on the one hand, and a
linear combination of velocity dispersion and mean surface brightness on the
other hand.
They dubbed this relation the fundamental plane.
They found the best-fitting relation involving a radius to be
![]() |
(2.4) |
Dressler et al. (1987b), also known as the 7 Samurai,
found the same result, namely
that elliptical galaxies describe a plane in the 3-space of
or
.
They found the plane to be given by
![]() |
(2.5) |
Dressler et al.
also introduced a new photometric diameter
,
the diameter
within which the mean surface brightness is
,
in Johnson B.
They found
to correlate as well with
as any linear
combination of
and
,
and they where thus able to
reformulate the FP as the
-
relation,
.
However, they noted that the correlation
between
and a combination of
and
,
namely
,
had a small residual curvature.
Phillipps (1988) demonstrated theoretically that the relation
is expected for galaxies with r1/4 profiles and
around
in Johnson B.
He also showed, that for the range in
actually spanned by (giant) ellipticals,
the FP will be seen as a curved line in the
versus
plot.
Lucey, Bower, & Ellis (1991a)
were the first to demonstrate that
the residuals from the
-
relation were correlated with
.
They corrected for this by simply adding a linear term in
to the
-
relation.
JFK93
found for a sample of galaxies in the Coma cluster
that the
-
residuals showed the dependence on
that was predicted by Phillipps (1988), a dependence that has a quadratic term.
They concluded that
the FP is a true improvement of the
-
relation.
In accordance with this, they found the scatter of the
-
relation to be larger than for the FP,
namely 17% versus 11% for their sample.
In the following, we will mainly consider the FP, not the
-
relation.
Properties of E and S0 Galaxies in the Clusters HydraI and Coma
Master's Thesis, University of Copenhagen, July 1997
Bo Milvang-Jensen (milvang@astro.ku.dk)