Infrared is usually divided into 3 spectral regions: near, mid and
far-infrared. The boundaries between the near, mid and far-infrared regions are
not agreed upon and can vary. The main factor that determines which wavelengths are
included in each of these three infrared regions is the type of detector
technology used for gathering infrared
Near-infrared observations have been made from ground based observatories
since the 1960's. They are done in much the same way as visible light
observations for wavelengths less than 1 micron, but require special infrared
detectors beyond 1 micron. Mid and far-infrared observations can only be made by
observatories which can get above our atmosphere. These observations require the
use of special
cooled detectors containing crystals like germanium whose electrical
resistance is very sensitive to heat.
Infrared radiation is emitted by any object that has a temperature
radiates heat). So, basically all celestial objects emit some infrared. The
wavelength at which an object radiates most intensely depends on its
temperature. In general, as the temperature of an object cools, it shows up more
prominently at farther infrared wavelengths. This means that some infrared
wavelengths are better suited for studying certain objects than others.
The rest of this article mainly discusses the technology of observing celestial objects using the principles of near-, mid- and far-infrared sensing. This illustrates the distance-travelling nature of infrared radiation, albeit in very small quantities, and the far-reaching importance of understanding infrared.
Visible (courtesy of Howard McCallon), near-infrared (2MASS), and mid-infrared (ISO) view of the Horsehead Nebula.
Image assembled by Robert Hurt.
As we move from the near-infrared into mid and far-infrared regions of
the spectrum, some celestial objects will appear while others will disappear
from view. For example, in the above image you can see how more stars
(generally cooler stars) appear as we go from the visible light image
to the near-infrared image. In the near-infrared, the dust also becomes
transparent, allowing us to see regions hidden by dust in the visible
image. As we go to the mid-infrared image, the cooler dust itself glows.
The table below highlights what we see in the different infrared spectral
WHAT WE SEE
Dust is transparent
comets and asteroids
Dust warmed by starlight
from cold dust
Central regions of galaxies
Very cold molecular clouds
Between about 0.7 to 1.1 microns we can use the same observing methods as are
used for visible light observations, except for observation by eye. The infrared
light that we observe in this region is not thermal (not due to heat radiation).
Many do not even consider this range as part of infrared astronomy. Beyond about
1.1 microns, infrared emission is primarily heat or thermal radiation.
As we move away from visible light towards longer wavelengths of light, we
enter the infrared region. As we enter the near-infrared region, the hot blue
stars seen clearly in visible light fade out and cooler stars come into view.
Large red giant stars and low mass red dwarfs dominate in the near-infrared. The
near-infrared is also the region where interstellar dust is the most transparent
to infrared light.
Visible (left) and Near-Infrared View of the Galactic Center
Visible image courtesy
of Howard McCallon. The infrared image is from the 2 Micron All Sky Survey (2MASS)
Notice in the above images how center of our galaxy, which is hidden by
thick dust in visible light (left), becomes transparent in the near-infrared
(right). Many of the hotter stars in the visible image have faded in the
near-infrared image. The near-infrared image shows cooler, reddish stars which
do not appear in the visible light view. These stars are primarily red dwarfs
and red giants.
Red giants are large reddish or orange stars which are running out of their
nuclear fuel. They can swell up to 100 times their original size and have
temperatures which range from 2000 to 3500 K. Red giants radiate most intensely
in the near-infrared region.
Red dwarfs are the most common of all stars. They are much smaller than our
Sun and are the coolest of the stars having a temperature of about 3000 K which
means that these stars radiate most strongly in the near-infrared. Many of these
stars are too faint in visible light to even be detected by optical telescopes,
and have been discovered for the first time in the near-infrared.
|As we enter the mid-infrared region of the spectrum, the cool stars
begin to fade out and cooler objects such as planets, comets and asteroids
come into view. Planets absorb light from the sun and heat up. They then
re-radiate this heat as infrared light. This is different from the visible
light that we see from the planets which is reflected sunlight. The
planets in our solar system have temperatures ranging from about 53 to 573
degrees Kelvin. Objects in this temperature range emit most of their light
in the mid-infrared. For example, the Earth itself radiates most strongly
at about 10 microns. Asteroids also emit most of their light in the
mid-infrared making this wavelength band the most efficient for locating
dark asteroids. Infrared data can help to determine the surface
composition, and diameter of asteroids.
An infrared view
of the Earth
IRAS mid-infrared view of Comet IRAS-Araki-Alcock
|Dust warmed by starlight is also very prominent in the
mid-infrared. An example is the zodiacal dust which lies in the plane of
our solar system. This dust is made up of silicates (like the rocks on
Earth) and range in size from a tenth of a micron up to the size of large
rocks. Silicates emit most of their radiation at about 10 microns. Mapping
the distribution of this dust can provide clues about the formation of our
own solar system. The dust from comets also has strong emission in the
Warm interstellar dust also starts to shine as we enter the mid-infrared
region. The dust around stars which have ejected material shines most brightly
in the mid-infrared. Sometimes this dust is so thick that the star hardly shines
through at all and can only be detected in the infrared. Protoplanetary disks,
the disks of material which surround newly forming stars, also shines brightly
in the mid-infrared. These disks are where new planets are possibly being
In the far-infrared, the stars have all vanished. Instead we now see
very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust
in our own galaxy, as well as in nearby galaxies, glow in far-infrared
light. In some of these clouds, new stars are just beginning to form.
Far-infrared observations can detect these protostars long before they
"turn on" visibly by sensing the heat they radiate as they contract."
IRAS view of infrared cirrus - dust heated by starlight
Michael Hauser (Space Telescope Science
the COBE/DIRBE Science Team, and NASA
|The center of our galaxy also shines brightly in the far-infrared
because of the thick concentration of stars embedded in dense clouds of
dust. These stars heat up the dust and cause it to glow brightly in the
infrared. The image (at left) of our galaxy taken by the COBE satellite,
is a composite of far-infrared wavelengths of 60, 100, and 240 microns.
|Except for the plane of our own Galaxy, the brightest far-infrared
object in the sky is central region of a galaxy called M82. The nucleus of
M82 radiates as much energy in the far-infrared as all of the stars in our
Galaxy combined. This far-infrared energy comes from dust heated by a
source that is hidden from view. The central regions of most galaxies
shine very brightly in the far-infrared. Several galaxies have active
nuclei hidden in dense regions of dust. Others, called starburst galaxies,
have an extremely high number of newly forming stars heating interstellar
dust clouds. These galaxies, far outshine all others galaxies in the
IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright