Infrared
Astronomy
Star-Forming Region
The Flame Nebula, also called NGC 2024,
is a region of dust and gas in the constellation Orion. Some of the dust and
gas is in the process of condensing into stars. This photograph was taken in
the infrared range of electromagnetic radiation. Infrared radiation has
wavelenghts slightly longer than those of visible light.
Infrared Astronomy, the detection and study
of infrared radiation emanating from objects in outer space. Infrared radiation
is another form of electromagnetic energy, similar to visible light and radio
waves, but differing by its wavelength (or frequency); all such waves travel at
the speed of light in a vacuum. Infrared wavelengths begin around 0.0007 mm
just beyond the reddest light that the human eye can detect, this is called the
“near” infrared, and grow in size to about 0.35 mm in the “far” infrared.
Wavelengths larger than this belong to the sub-millimeter, microwave, and radio
parts of the electromagnetic spectrum.
Infrared observations are important
in astrophysics for several reasons. Infrared radiation penetrates more easily
through the vast stretches of interstellar gas and dust clouds than does
visible and ultraviolet light, revealing regions hidden to normal telescopes.
Young stars are surrounded by a cocoon of gas and dust which can make them
invisible, but their heat warms the dust grains and produces infrared radiation
which escapes to reveal their presence. Infrared radiation is also called
“thermal” or heat radiation. Many molecules, such as carbon monoxide (CO) and
hydrogen (H2), and tiny solid particles known as dust grains, are
best studied at infrared wavelengths. Finally, the expansion of the universe
changes (or redshifts) the visible light emitted by the most distant galaxies
into red and infrared light.
II
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INFRARED TELESCOPES AND DETECTORS
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Infrared Telescope
Infrared telescopes detect radiation
that has wavelengths longer than the light that humans can see. Infrared
radiation enters the telescope and reflects off of a large mirror on the bottom
of the telescope, then off of a smaller mirror. Detectors and instruments
beneath the mirrors record the radiation. Infrared telescopes must be kept at
very low temperatures to prevent their own heat from producing infrared
radiation that could interfere with observations.
Infrared telescopes look similar
to normal optical telescopes. Light is collected and focused by a large curved
mirror onto a smaller secondary mirror and then into the scientific instrument
(camera or spectrometer) for analysis. Most often, the secondary mirror is very
small and gold-coated because gold offers better reflectance in the infrared
than the normal aluminized mirrors do. The secondary mirror is mechanized so
that it can tilt back and forth rapidly, up to 20 times per second, allowing
the detector in the science instrument to compare the signals from the source
plus sky background and the sky background alone. This technique is called
“chopping” and is very effective for detecting a faint signal against a very
strong background. Infrared telescopes have an open structure, without the
black tubes or baffles common to normal telescopes, since these emit infrared
radiation. For an infrared telescope in space the baffles can be cooled to
reduce infrared emissions. One of the largest telescopes dedicated to
ground-based infrared astronomy is the 152-inch (3.8-m) United Kingdom Infrared
Telescope (UKIRT) at the Mauna Kea Observatory in Hawaii, but many other
telescopes possess infrared instruments, especially for near-infrared work. In
recent years, infrared astronomy has been revolutionized by the introduction of
tiny imaging devices called “infrared arrays” making it possible to take
pictures at these invisible wavelengths and display them on computer screens.
Everything that is warm
emits infrared radiation. A star like the Sun emits most of its radiant energy
as visible (yellow) light. Redder and cooler stars at half the Sun’s
temperature have a peak emission at near-infrared wavelengths. Merely warm
objects, like telescopes and Earth’s atmosphere, don’t emit light but they give
off profuse amounts of infrared radiation with a peak emission around a
wavelength of 0.01 mm. Since they are much closer to the infrared camera or
detector, these sources of infrared radiation swamp any signals from distant
planets, stars, and galaxies. Likewise, the optical and mechanical parts of the
scientific instrument will emit strong infrared radiation. The solution to this
problem is to cool the detector, and all the optics, inside a vacuum chamber.
Temperatures around that of liquid nitrogen (77 degrees Kelvin (K) above
absolute zero) are needed for near-infrared detection whereas temperatures near
liquid helium (only 4 K) are required for far-infrared detectors.
To eliminate the large,
unwanted background of infrared radiation it would be necessary to cool down
the entire telescope and remove Earth’s atmosphere. For a space-based
telescope, however, there is no atmosphere and no problem of condensation and
ice formation if the telescope itself is cooled. Ground-based infrared
telescopes need to be located at very high, dry, and cold sites like Mauna Kea,
Hawaii, to minimize the thermal background. This is effective for near-infrared
work. Far-infrared observations are best done from space or from high-flying
airplanes.
III
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THE INFRARED UNIVERSE
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Orion Nebula in Infrared
This image of the Orion Nebula was taken
in infrared radiation—radiation with wavelengths longer than visible light—and
given false visible colors. The Orion Nebula is a cloud of gas and dust that surrounds
new stars. The young stars light up the nebula and cause it to glow.
Infrared radiation emanating
from the outer planets and their moons reveals much about their temperatures
and compositions. Jupiter emits more infrared radiation than expected from
absorption of sunlight, indicating that it has an internal source of heat
energy. Infrared observations of Jupiter’s moon Io show thermal hot spots
caused by the active volcanoes on its surface.
Stars of lower mass than
the Sun are less luminous and much cooler. They emit most of their energy at
infrared wavelengths. While these red dwarf stars are much more plentiful than
the rare and short-lived high-mass stars, the very lowest mass objects—called brown
dwarfs—have been hard to find because they are so faint at visible light
wavelengths. Infrared astronomy has played a key role in the search for these
objects which lie on the boundary between true stars and giant Jupiter-like
planets.
Although interstellar space is a
vacuum, it is not completely empty. Tiny solid particles called dust grains can
be found around and between the stars. These particles are formed from heavier
elements (like silicon and iron) produced deep inside an earlier generation of massive
stars. Dust grains absorb ultraviolet and visible light, making the most
distant stars appear redder and fainter, while also heating the dust slightly
above the temperature of space and causing it to glow at far-infrared
wavelengths. Dust obscures our view of distant parts of our own Milky Way
Galaxy, including the center of the galaxy. The central regions can only be
observed at infrared and radio wavelengths. Recent ground-based and space-based
observations of the center of the galaxy have revealed for the first time clear
evidence of dynamic motion around a massive, invisible source believed to be a
black hole with a mass over one million times that of the Sun. Dust also
obscures our view of young, recently-formed stars. As a cloud of gas and dust
contracts to form a star it tends to flatten into a disk due to rotation.
Eventually the disk might dissipate or it may allow planets to form. The disk
both hides the starlight and is heated by it. Infrared observations reveal the
hidden source and provide knowledge of how stars and planetary systems form.
Spiral galaxies similar to our
own contain lots of dust and star-forming regions making them difficult to
study except with infrared instruments. Some classes of galaxies are
exceptionally luminous in the infrared because they have so much dust and have
absorbed so much ultraviolet energy from the central sources within the nucleus
of the galaxy. Distant galaxies are fainter and redder than nearby ones. The
reddening in this case is not caused by intergalactic dust but by the expansion
of the universe discovered by Edwin Hubble. Traveling at 186,000 mi every
second (300,000 km/s), it takes light billions of years to reach us from the
most distant galaxies, and therefore we see these galaxies as they were when
they were young and not as they are now. During this time space itself has
expanded and the wavelength of the radiation has been stretched or “redshifted”
by such a large amount that the galaxy is no longer readily detectable at
visible light wavelengths because all its energy is now in the infrared.
IV
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HISTORY AND CURRENT RESEARCH
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Saturn’s Atmosphere
This infrared photo of the planet Saturn
has been color coded to indicate the cloud level in Saturn’s atmosphere. Violet
and blue represent areas in which Saturn’s atmopshere is clear down to the main
cloud layer. Green and yellow show layers of haze above the main cloud layer
(yellow represents thicker haze). Red and orange indicate the highest level of
clouds, thicker than the haze. White areas are areas of the atmosphere with
high levels of water vapor. The bright dots at the upper right and lower left
of the picture are Saturn’s satellites Tethys and Dione, respectively. The
Hubble Space Telescope took this image in 1998.
Modern infrared astronomy began
in the 1950s when simple photoelectric detectors made from lead sulphide became
available and were used to survey the sky at infrared wavelengths for new
sources. Later, germanium detectors were used to open up the study of much
longer infrared wavelengths with the aid of rocket, balloon, and airplane
surveys. In the late 1970s, several large ground-based telescopes dedicated to
infrared astronomy were built which included the 3.8-m United Kingdom Infrared
Telescope (UKIRT) and the National Aeronautics and Space Administration (NASA)
3-m Infrared Telescope Facility (IRTF) both on Mauna Kea, Hawaii, at 14,000 ft
above sea level. With the launch of the Infrared Astronomical Satellite (IRAS),
by the United States, the United Kingdom, and The Netherlands in 1983, infrared
astronomy took another leap forward. This mission surveyed the entire sky at
wavelengths of 12, 25, 60, and 100 microns (1 micron is a millionth of a meter)
until its onboard supply of liquid helium ran out. A short time later infrared
astronomy was revolutionized by the first introduction of devices that could
take infrared images. The advent of sensitive infrared cameras inspired many
traditional observatories to convert for infrared work, especially in the near
infrared where city lights don’t cause problems and the thermal background from
the telescope is minimal.
Uranus and Its Rings
The planet Uranus rotates on an axis
that is tilted nearly horizontal. Other planets in the solar system have axes
that are more vertical. This infrared image taken by the Hubble Space Telescope
shows Uranus's rings orbiting in the plane of the planet's tipped equator. The
colors are not real and are used to bring out details such as clouds in the
atmosphere and the shape of the rings. The white disks are moons.
Infrared astronomy from space
received two boosts when the Infrared Space Observatory (ISO) was launched in
December 1995 and when the Hubble Space Telescope was refurbished in 1997 with
NICMOS, the Near Infrared Camera and Multi-Object Spectrograph. Both of these
missions used infrared array detectors. Another important satellite which used
infrared techniques for part of its mission was the Cosmic Background Explorer
(COBE). The Spitzer Space Telescope, launched in 2003, is the largest and most
sensitive infrared space telescope ever launched.
Future infrared missions include
SOFIA, the Stratospheric Observatory for Infrared Astronomy. SOFIA is a
modified Boeing 747 with a 2.5-m telescope on board, due for commissioning in
2004.
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