![]() | Annu. Rev. Astron. Astrophys. 2003. 41:
191-239 Copyright © 2003 by Annual Reviews. All rights reserved |
If elliptical galaxies were perfectly homologous stellar systems
with identical stellar populations, then the
"central" velocity dispersion
o,
stellar mass M and half-light (effective) radius
Re would be related by the virial theorem,
o2
=
(M /
Re) =
(LV /
Re)(M / LV) with constant
.
Instead, non-homology and/or stellar population variations conspire
to place elliptical galaxies on a nearby fundamental plane
o2
(LV
/ Re)[Re0.22
o0.49], implying that
(M /
LV)
Re0.22
o0.49
M0.24
Re-0.02
LV0.32 Re-0.03
(Dressler et al. 1987;
Djorgovski & Davis
1987).
The width of the fundamental plane is remarkably small
(Renzini & Ciotti
1993).
In projection the fundamental plane indicates that
the binding energy per unit mass decreases with
stellar (or galactic) mass,
o2
M0.32
(Faber et al. 1997),
i.e., hot interstellar gas is less bound in low mass ellipticals.
This regularity in the global properties of elliptical galaxies
is useful in interpreting the X-ray
emission from the hot interstellar gas they contain.
The internal structure is also quite uniform among
massive E galaxies. For those with de Vaucouleurs (r1/4)
stellar profiles the stellar distribution is
completely determined by the optical half-light radius
Re and the total stellar mass M*t.
Provided the dark halos consist of cold, non-interacting
particles, the halo density profile is determined by
its virial mass, Mdh, the mass enclosing a cosmic
overdensity of ~ 100 relative to the critical density
c
= 3H02 /
8
G
in a flat
CDM
universe with
M = 0.3
(Eke, Navarro, &
Frenk 1998;
Bullock et al. 2000).
If elliptical galaxies formed by mergers in galaxy groups, as generally
believed, then the hot gas they
contain must be understood in this evolutionary context.
The r1/4 stellar
density profile in ellipticals and the high incidence
(
50 percent)
of counter-rotating or kinematically independent
stellar cores are natural consequences of hierarchical mergers
(Hernquist & Barnes
1991;
Bender 1996).
While many massive E galaxies currently reside in the
dense cores of rich galaxy clusters, the orbital velocities
of cluster member galaxies are too high for efficient mergers.
In spite of these regularities,
giant elliptical galaxies come in two flavors
depending on their mass or optical luminosity.
Low luminosity ellipticals have power law central stellar density
profiles, disky isophotes, and oblate symmetry consistent
with their moderate rotation. Ellipticals of high luminosity
have flatter stellar cores within a break radius rb
(typically a few percent of Re),
boxy isophotes, and have aspherical
structures caused by anisotropic stellar velocities,
not by rotation which is generally small
(Kormendy & Bender
1996;
Faber et al. 1997;
Lauer et al. 1998).
Nevertheless, many of the most luminous E0 and E1 galaxies are
thought to be intrinsically spherical to a reasonable approximation
(Merritt & Tremblay
1996)
and these galaxies are among the most luminous in X-rays.
The transition from power-law to core ellipticals
occurs gradually over
-20
MV
- 22 where both
types coexist on the same fundamental plane. Finally, optical spectra of
ellipticals often show evidence of a (sub)population of younger stars,
particularly in ellipticals with power-law profiles (e.g.
Trager et al. 2000;
Terlevich & Forbes
2002).
The X-ray luminosities Lx of elliptical galaxies
correlate with LB in a manner that
also exhibits a transition with increasing mass
(Canizares et al. 1987;
Donnelly et al. 1990;
White & Sarazin
1991;
Fabbiano, Kim &
Trinchieri 1992;
Eskridge, Fabbiano, &
Kim 1995a,
b,
c;
Davis & White 1996;
Brown & Bregman 1998;
Beuing et al. 1999).
For elliptical galaxies of low luminosity
(i.e. LB
LB,
crit = 3 × 109
LB,
)
O'Sullivan et al. (2001)
find that the bolometric X-ray and optical luminosities
are approximately proportional,
Lx
LB.
The X-ray emission from these galaxies is apparently dominated by
low-mass X-ray binary stars with a different (typically harder) spectrum
than that of the interstellar gas
(Brown & Bregman
2001).
The brightest stellar X-ray sources can be
individually resolved with Chandra (e.g.
Sarazin, Irwin &
Bregman 2000;
Blanton, Sarazin, &
Irwin 2001a).
However, the X-ray emission from
more luminous ellipticals (LB
LB,
crit) varies approximately as
Lx
LB2
(O'Sullivan et
al. 2001),
clearly indicating a non-stellar origin,
i.e., the hot gas. As shown in Figure 1,
the scatter about this correlation is enormous,
Lx varies by almost two orders of magnitude
for galaxies with similar LB.
![]() |
Figure 1. A plot of the bolometric X-ray
luminosity and B-band optical luminosity for elliptical galaxies
(RC3 type T |
The large scatter in the
Lx
LB2
correlation has received much attention but
an explanation in terms of some specific environmental
or intrinsic property of the galaxies has been elusive (e.g.
Eskridge, Fabbiano, &
Kim 1995a,
b,
c).
White and Sarazin
(1991) and
Henriksen &
Cousineau (1999)
find that ellipticals
having other massive galaxies nearby have systematically
lower Lx / LB while
Brown & Bregman
(2000)
find a positive correlation with Lx /
LB and the local density of galaxies.
Pellegrini (1999)
presented evidence that
ellipticals with power law profiles have much smaller
range in Lx / LB, as might be
expected if a larger fraction of
Lx in these galaxies has a stellar origin
(Irwin & Sarazin
1998).
Power law ellipticals tend to be non-central in groups/clusters and
therefore tidally subordinate with some exceptions.
More luminous group-centered, group-dominant ellipticals
typically have much larger Lx / LB,
enhanced by an additional contribution of circumgalactic or intragroup
hot gas
(Helsdon et al. 2001;
Matsushita 2001).
The possible influence of galactic rotation and
(oblate) flattening on Lx / LB have
been explored with limited success
(Nulsen et al. 1984;
Kley & Mathews
1995;
Brighenti & Mathews
1996;
Pellegrini, Held &
Ciotti 1997;
D'Ercole & Ciotti
1998).
While there is some evidence that
Lx / LB is several times lower in
flattened and rotating ellipticals, this cannot explain
the much larger scatter observed. In the evolutionary scheme of
Ciotti et al. (1991)
the scatter results from a transition from early
Type Ia driven winds to cooling inflows, but this
scenario (discussed below) produces too much iron in the hot gas
(Loewenstein &
Mathews 1991).
Mathews and Brighenti
(1998)
showed that ellipticals with larger Lx also have more
extended hot gas,
Lx / LB
(Rex / Re)0.60±0.20,
where Rex is the half-brightness radius for
the X-ray image which can extend out to
~ 10Re or beyond. This correlation (see also
Fukugita & Peebles
1999
and Matsushita 2001)
may result from the tidal competition for diffuse baryonic gas among
elliptical-dominated galaxy groups as they formed
with different degrees of relative isolation.
Ram pressure stripping must also influence Lx /
LB for E galaxies in richer clusters (e.g.
Toniazzo & Schindler
2001).