Greater Collecting Area
Astronomers are in a constant search for light. The more light
an astronomer collects, the easier it is to determine the properties
of an object and to discover new phenomena.
In high-energy astronomy, astronomers gather light by counting
photons, which are particles of light. The limit to our knowledge
about the size, energy, or mass of an object depends
on how certain we are of the number of photons collected. The
relative uncertainty in the number of photons collected
decreases as the number of photons increases. Hence the
the more light we collect, the better we can know.
![Chandra X-ray Observatory](https://webarchive.library.unt.edu/eot2008/20090118032245im_/http://imagine.gsfc.nasa.gov/Images/satellites/chandra_sat.gif) Chandra X-ray Observatory |
In high-energy astronomy, astronomers collect photons using either
X-ray or gamma ray telescopes (as in the case of the Chandra X-ray Observatory or the X-ray Multiple-Mirror Mission) or large area
detectors (as in the case of the Rossi X-ray Timing Explorer).
| ![Rossi X-ray Timing Explorer](https://webarchive.library.unt.edu/eot2008/20090118032245im_/http://imagine.gsfc.nasa.gov/Images/xte/xte_artist.gif) Rossi X-ray Timing Explorer |
More photons means better images and better spectra.
Better images
because greater detail can be picked up as more photons create a
sharper image. Better spectra because weaker emission lines become more
evident as we detect more photons in them. But better images and
better spectra also need higher
resolution in the detector, in addition to greater collecting
area.
An artist's conception of an X-ray Binary
System. Collecting enough photons from a source such as this
can tell us whether it contains a black hole
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Larger collecting area
also means better light
curves. For bright
sources, large area means collecting more photons in a shorter amount
of time. Hence, we can detect phenomena that occur within a very
short time. With its large collecting area of 6250 cm2,
RXTE detected quasi-periodicities in
X-ray binaries down to
milliseconds, and provided evidence of the signature of material just
before if falls into a black
hole.
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Steps toward flying missions with larger collecting area are
constantly being taken. Launched in December 1999, the X-ray Multiple-Mirror
Mission uses compact X-ray optics to produce an effective collecting
area of 2500 cm2 at low X-ray energies. Among the many
types of objects it studies, XMM uses this collecting area to
study to the nature of the diffuse X-ray background, which ROSAT has
shown to be discrete sources, but whose nature is still largely a mystery.
| ![XMM](https://webarchive.library.unt.edu/eot2008/20090118032245im_/http://imagine.gsfc.nasa.gov/Images/satellites/xmm.jpg) XMM |
Another mission using larger collecting area is the Fermi Gamma Ray Space Telescope (Fermi), which will study objects emitting gamma-rays
having energies ranging from 10 MeV to 100 Gev. Fermi has
an effective collecting area of at least 8000 cm2, compared
to the EGRET instrument on the Gamma Ray Observatory, which has an
area of 1500 cm2. In addition, Fermi is able to view
4 times more of the sky at any one time than EGRET did. With its
large area and sensitivity,
Fermi is addressing the evolution of
supermassive black holes in the centers of
some galaxies, the
nature
of particle jets
emanating from these black holes, and search for
radiation from weakly interacting particles,
which may make up the dark matter in the universe.
| ![GLAST](https://webarchive.library.unt.edu/eot2008/20090118032245im_/http://imagine.gsfc.nasa.gov/Images/satellites/glast_v2.gif)
Fermi Gamma-Ray Space Telescope |
Updated: September 2008
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