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What Are Clusters Made Of?
Cluster Mass Distributions, Dark Matter, and the Fate of the
Universe
Astrophysicists divide the universe up into two types of matter: "luminous
matter" -- stars and gas that shine of their own accord, and "dark
matter" that is detectable only through its gravitational effects on luminous
matter. One of the outstanding problems in modern cosmology is to measure the
total amount of material, both luminous and dark, since this determines the ultimate
fate of the expanding universe: if the mass density is above a certain `critical' value
the universe will eventually recollapse (perhaps as part of an eternal cycle of big
bangs and `big crunches'), if not it will expand forever. The sum of all the known
luminous matter adds up to less than 10f this critical density, but we know from
studies of our own, and other nearby, galaxies that there is more dark than
luminous matter in the universe. But how much more?
This is where the study of rich clusters of galaxies comes in. These
conglomerations of hundreds, or even thousands, of galaxies spread over millions
of light years are so large that the relative proportions of dark and luminous matter
are believed to be the same as the universe as a whole. Using X-ray observations,
we can measure the masses of both the hot gas (this pervasive medium lying
between the galaxies, and not the stars in the galaxies themselves, is the dominant
form of luminous mass in clusters) and dark matter.
The amount of hot gas in a cluster is simply related to the total X-ray luminosity
emitted (and collected by
telescopes on board orbiting X-ray observatories) -- the more hot gas there is,
the brighter in X-rays. Measuring the luminous matter is a fairly direct task.
The dark matter can be measured, or at least estimated, because clusters of galaxies
are approximately `relaxed' systems: these systems have been around long enough
to have attained a balance, an equilibrium, that depends only on the present-day
structure of the clusters and not how they were formed or on recent dynamical
processes. In the same way, the basic stable structure of the Earth's atmosphere
today depends only on the Earth's gravity, atmospheric composition, solar heating,
etc. and not on how the earth formed or what today's weather is like. And just as
the pressure in the Earth's atmosphere is in balance with the gravity of the Earth --
decreasing as one ascends to higher and higher altitudes -- so too is the hot X-ray
emitting cluster gas stratified in pressure in such a way as to be in balance with the
total gravity of the cluster. The pressure of the hot gas in clusters can be measured -
- it is simply related to the product of the hot gas mass density and temperature. The
density is inferred from the X-ray brightness (the higher the density of X-ray
emitting gas, the more intense the X-ray emission), while the temperature is
inferred from the X-ray spectrum (every temperature produces a characteristic
spectral shape).
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We then infer the total mass distribution from the measured pressure
profile by applying the condition of equilibrium. Not surprisingly -- based on what
we already know about individual galaxies -- we have found that most of the mass
in galaxy clusters consists of dark matter. The total mass in a rich cluster can exceed
1048 grams (as much as a million trillion Suns). However, there
have been a couple of surprising developments that have come out of our cluster
studies.
Surprising Developments
Modern physics `theories of everything' that attempt to unite the four forces in
nature predict that the total mass density in the universe should be just equal to the
`critical density' defined previously. This corresponds to roughly 90-99% of the
material being dark. While most of the matter in rich galaxy clusters is dark, we
find it is so only by about a three-to-one margin, not a ten- or hundred-to-one
margin, as expected. This means that if rich clusters are representative samples of
the universe -- and there's no reason to suppose otherwise -- then the universal
mass density is less than the critical value, and the universe will expand forever.
Another unexpected discovery is that for some (but not all) moderately rich clusters,
clusters with a few dozen galaxies, the dark matter fraction is higher -- around
90%. Why these clusters are different than poorer clusters may be telling us
something. The most straightforward explanation of this is that some of the
luminous matter (that is, the hot gas) has been expelled from these systems, and
therefore the relative proportion of dark matter is greater. While not as massive as
the richest clusters, the mass in these systems can exceed 1047
grams, and therefore expelling a large fraction of their hot gas requires a
tremendously violent and energetic process. As it turns out there is other X-ray
astrophysical evidence for such phenomena obtained from measuring the amount of
chemical pollutants in the hot cluster gas.
Chemical Abundances in Clusters: Star Formation and Supernova
History
Before stars or galaxies formed, the luminous matter in the universe consisted of
only the lightest and simplest elements -- mostly hydrogen and helium. Most of the
hot X-ray emitting gas we observe consists of this primordial material, but X-ray
spectroscopy reveals emission lines from other heavier elements, most universally
an iron line at 6.7 keV. Some clusters also show spectral emission lines from atoms
of oxygen, neon, magnesium, silicon, and sulfur. Where did these chemical
`pollutants' come from and how did they get out into the gas between the galaxies
in clusters?
The most common heavy elements are synthesized in nuclear reactions in the hot,
dense deep interiors of stars -- some elements steadily as part of a star's natural
slow evolution, others (including those we see in X-ray spectra of galaxy clusters)
in explosive events called supernovae. These heavy elements escape out of stars
through various means -- in supernovae the explosions themselves blow the star
apart. However, to get out into the cluster gas the material must escape not only
from a single star but out of the entire galaxy of stars. This can occur if many
supernovae explode in a sufficiently short period of time, leading to what is known
as a galactic wind.
The strength of any particular X-ray emission line is directly related to the
abundance of the element that produced that line, and by measuring all the heavy
elements in the spectrum we can estimate how many supernovae occurred. It turns
out that the number is unexpectedly high -- higher than one would predict based on
the stars we see. This has several consequences. Firstly, it means (again if clusters
are representative of other places in the universe) that there has been more massive
star formation (only stars at least eight times as massive as the sun explode as
supernovae) in the universe than was previous thought. The energy associated with
all of these supernovae is so great that it may have not only blown gas out of
individual galaxies, but out of some (but not the most massive) clusters as well --
thus offering an explanation for our detection that some clusters have higher dark
matter fractions than others, as discussed above.
Thus our observations that, except for the richest systems, clusters show a range of
relative proportions of dark and luminous matter; and, our measurement of large
amounts of heavy element enrichment of the gas between galaxies in all clusters
find a common explanation. At the time when the stars in cluster galaxies formed,
there must have been hundreds of billions of supernova explosions that expelled
material out of galaxies. And such powerful injections of heavy metals and energy
into the cluster gas both enriched it and, in some cases, expelled some fraction of
the material out of the clusters despite the fact that each one is about one thousand
times more massive than a typical galaxy consisting of ten billion stars.
What X-ray Missions Are Used in Cluster Research?
In order to carry out these areas of research, we need both images and spectra of the
X-ray emitting gas. Of course, we want the best spatial and spectral resolution to
give us the best possible observables and the most robust data to compare with
model predictions.
The best X-ray images, that is maps of X-ray emission, currently available come
from the ROSAT satellite. We use ROSAT observations to derive cluster gas mass
distributions.
The most useful spectra for cluster work come from the ASCA satellite, because
they yield the most detailed spectra over a wide range of X-ray energies. Our group
uses ASCA spectra to get the most accurate temperatures and elemental abundances.
We use a combination of the mass density (from ROSAT) and temperature (from
ASCA) profiles to find the pressure distribution and therefore the total cluster mass
distribution (dark and luminous matter).
What's In The Future?
New missions, such as CXO, and future missions, such as ASTRO-E and XMM, will improve the detail
and quality of cluster images and spectra. The major benefit of these increases in
capabilities will to be expand the number of clusters whose mass distributions and
elemental abundances are known, and to study clusters that are further away and
therefore younger. This will not only enable us to refine the above results, but to
explore systematic variations and address the questions of why only certain clusters
seem to have lost a lot of their hot gas. Looking back to earlier times will help us to
trace out the enrichment history and thus the evolution of, not only the clusters
themselves, but star formation in the universe as a whole.
Thank you to Michael Loewenstein (http://lheawww.gsfc.nasa.gov/users/loew/vita/mlcv.html) for contributing to this
article.
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