After Sir William Herschel's discovery of infrared ,which showed that the Sun emits infrared light, astronomers tried to see if other objects in the universe gave out infrared waves. In 1856, astronomers used thermocouples (devices which convert heat into electric current) to detect infrared radiation from the Moon. Much later, in 1948 (decades before the first Moon landing), more sophisticated infrared studies of the Moon would show that its surface was covered with a fine powder. In the early 1900's, infrared radiation was successfully detected from the planets Jupiter and Saturn and from some bright stars such as Vega and Arcturus. However, the insensitivity of the early infrared instruments prevented the detection of other near-infrared sources. Work in infrared astronomy remained at a low level until breakthroughs in the development of new, sensitive infrared detectors were achieved in the 1960's. During the past few decades, infrared astronomy has become a major field of science due to the rapid advances in infrared detector technology. Many of these advances arose from U.S Department of Defense research into infrared array technology in the 1980's. Infrared light, having longer wavelengths and lower energy than visible light, does not have enough energy to interact with the photographic plates which are used in visible light astronomy. Instead infrared astronomers rely on electronic devices to detect radiation. Early infrared astronomers used thermocouples and thermopiles (a group of thermocouples combined in one cell). In the 1950's astronomers started to use Lead-sulphide (PbS) detectors to study infrared radiation in the 1 to 4 micron range. When infrared light in this range falls on a PbS cell it changes the resistance of the cell. This change in resistance can be measured and is related to the amount of infrared radiation which falls upon the cell. To increase the sensitivity of the PbS cell it was cooled to a temperature of 77 degrees Kelvin by placing it in a flask filled with liquid nitrogen. A major breakthrough came in 1961, with the development of the germanium bolometer. This instrument was hundreds of times more sensitive than previous detectors and was capable of detecting all infrared wavelengths. Basically, a cool thin strip of germanium is placed in a container which has a small opening in it. When infrared radiation comes through the opening and hits the germanium, it warms the metal and changes its conductivity (a measure of how much electrical current flows through an object). The change in conductivity can be measured and is directly proportional to the amount of infrared radiation entering the container. The germanium bolometer works best at an extremely low temperature (much lower than liquid nitrogen). The best way to cool the bolometer to such a low temperature is to surround it with liquid helium which cooled it to 4 degrees Kelvin. This is only a few degrees above absolute zero. To do this a metal Dewar (similar to a well insulated thermos flask) was developed which was able to hold the liquid helium in which the germanium bolometer was immersed. This type of infrared detector is sensitive to the entire range of infrared wavelengths. To study a particular wavelength of infrared emission from astronomical objects, astronomers place filters in front of the detectors, which filter out all but the desired wavelengths. Infrared detector technology continues to advance at a rapid rate. Astronomers now use InSb and HgCdTe detectors for the 1 to 5 micron range. These operate in a way similar to the PbS detectors but use materials which are much more sensitive to the infrared. The development of infrared array detectors in the 1980's caused another giant leap in the sensitivity of infrared observations. Basically a detector array is a combination of several single detectors. These arrays allow astronomers to produce images containing tens of thousands of pixels at the same time. Infrared arrays have been used on several infrared satellite missions. In 1983 the IRAS mission used an array of 62 detectors. Astronomers now commonly use 256x256 arrays (thats 65,536 detectors!). Due to these breakthroughs in infrared technology, infrared astronomy has developed more rapidly than any other field of astronomy and continues to bring us exciting new views of the universe. Infrared detectors attached to ground based telescopes can detect the near-infrared wavelengths which make it through our atmosphere. The best location for ground based infrared observatories is on a high, dry mountain, above much of the water vapor which absorbs infrared. At these high altitudes, astronomers can study infrared wavelengths centered at 1.25, 1.65, 2.2, 3.5, 4.75, 10.5, 19.5 and 35 microns. Telescopes as well as our atmosphere emit infrared radiation which can complicate the observation of cosmic sources. Infrared telescopes are designed to limit the the amount of this thermal emission from reaching the detectors. All ground based infrared detectors are cooled to extremely low temperatures to reduce their emission. In addition, astronomers making ground based observations measure both the emission from the sky and from object that they are observing. They then subtract the sky's emission from the infrared emission of a celestial object to get an accurate measurement. In the mid-1960's, the first infrared survey of the sky was made at the Mount Wilson Observatory using liquid nitrogen cooled PbS detectors which were most sensitive at 2.2 microns. The survey covered approximately 75 percent of the sky and found about 20,000 infrared sources. Many of these sources were stars which had never been seen before in visible light. These stars were much cooler than our Sun and had surface temperatures of 1,000 degrees to 2,000 degrees Kelvin. Our Sun has a surface temperature of about 6,000 degrees Kelvin. The brightest 5,500 of these sources made up the first catalog of infrared stars. A partial infrared survey of the southern sky was also made in 1968 at the Mount John Observatory in New Zealand. New observatories, specializing in infrared astronomy, became possible in the 1960's due to advances in infrared detectors. The largest group of infrared telescopes can be found on top of Mauna Kea (a dormant volcano) on the island of Hawaii. At an elevation of 13,796 ft., * the Mauna Kea Observatories , which were founded in 1967, are well above much of the infrared absorbing water vapor. The Mauna Kea Observatories Photo courtesy of Richard Wainscoat, Institute for Astronomy, University of Hawaii By the early 1970s, it was found that the centers of most galaxies emit strongly in the infrared, including our own galaxy, the Milky Way. Quasars and other active galaxies were also found to be strong infrared emitters. All of this new information came from near-infrared observations which could be made from the ground. Today, most of the larger ground based telescopes have been modified to accommodate infrared detectors. Many ground based infrared telescopes are now using adaptive optics to create very sharp images. Adaptive optics removes the blurring of an astronomical image due to turbulence in earth's atmosphere. In addition to absorbing most of the infrared radiation from cosmic sources, the Earth's atmosphere itself radiates in the infrared which interferes with infrared observations. This is why it is best to get above as much of the atmosphere as possible to observe in the infrared. To do this, infrared detectors have been placed on balloons, rockets and airplanes, allowing astronomers to study longer infrared wavelengths. Even though these methods can only observe a small part of the sky for short periods of time, they have contributed much to infrared astronomy. The first cooled telescopes were those placed on rockets which could observe the sky for several minutes before reentry. The first infrared all sky map resulted from a series of rocket flights by the Air Force Cambridge Research Laboratory. This project, called Hi Star, surveyed the cosmos at wavelengths of 4, 10 and 20 microns. Although the total observation time accumulated by these flights was only about 30 minutes, they successfully detected 2363 reliable infrared sources which were published in the AFCRL Infrared Sky Survey. About 70% of these sources matched sources found by the Mount Wilson 2.2 micron survey. Rockets also found bright infrared emission from HII regions (regions of ionized hydrogen) and the center of our galaxy. Helium filled, mylar balloons have carried infrared telescopes up to altitudes as high as 25 miles. In 1963, a germanium bolometer was attached to a balloon to make infrared observations of Mars. Beginning in 1966, the Goddard Institute of Space Sciences used balloons to survey the sky at 100 microns. Their program led to the discovery of about 120 bright infrared sources near the plane of our galaxy. Infrared telescopes onboard aircraft such as the * Kuiper Airborne Observatory were used to discover the rings of Uranus in 1977. The KAO has been used to gather infrared astronomical data for over 20 years and can fly at an altitude of 41,000 feet which is above 99 percent of the Earth's water vapor. In addition to being able to study additional infrared wavelengths, airborne observatories can detect fainter infrared objects which cannot be observed well from the ground (such as interstellar clouds). The Kuiper Airborne Observatory Plans are being made by NASA for a new airborne observatory. * SOFIA - The Stratospheric Observatory For Infrared Astronomy will be an optical/infrared/sub-millimeter telescope mounted in a Boeing 747 and is expected to be fully operational by the year 2001. In the 1970s, astronomers around the world began to consider the possibility of placing an infrared telescope on a satellite in orbit around the Earth. This telescope would be above the Earth's atmosphere and could view the sky at the far-infrared wavelengths which were difficult to detect on Earth. It could view a large area of the sky and observe regions for a longer period of time. By 1977, an international collaboration was formed by the Netherlands, United States and Great Britain to develop IRAS - The Infrared Astronomical Satellite. The American team built the telescope, detectors and cooling system. The British built the satellite ground station and control center and the Dutch team built the spacecraft which included the on-board computers and pointing system. It takes a great deal of effort to build an infrared space telescope. After many years of hard work and after overcoming several complications, IRAS was successfully launched on January 25, 1983. The telescope was housed in a dewar, filled with 127 gallons of liquid helium and contained 62 detectors. The entire telescope was cooled to a temperature of just a few degrees above absolute zero because otherwise the telescope itself would emit infrared radiation (heat) which would interfere with the observations. A space infrared telescope must be cooler than the objects in space that it will observe. IRAS in orbit - Artist Rendition The IRAS mission would last as long as the liquid helium did. For the next ten months, IRAS scanned more than 96 percent of the sky four times, providing the first high sensitivity all sky map at wavelengths of 12, 25, 60 and 100 microns. IRAS increased the number of cataloged astronomical sources by about 70%, detecting about 350,000 infrared sources. IRAS discoveries included a disk of dust grains around the star Vega, six new comets, and very strong infrared emission from interacting galaxies as well as wisps of warm dust called infrared cirrus which could be found in almost every direction of space. IRAS also revealed for the first time the core of our galaxy, the Milky Way. Several successful infrared satellite missions were launched after IRAS. During July and August of 1985, an infrared telescope was flown onboard the Space Shuttle's Spacelab 2 to complement observations made by the IRAS mission. This mission produced a high quality map of about 60% of the plane of our galaxy. The Space Shuttle With Skylab 2 In November 1989, NASA launched the * COBE satellite to study both infrared and microwave characteristics of the cosmic background radiation (the remains of the extreme heat that was created by the Big Bang). Over a ten month period, COBE mapped the brightness of the entire sky at several infrared wavelengths and discovered that the cosmic background radiation is not entirely smooth, showing extremely small variations in temperature. These variations may have led to the formation of galaxies. * The Infrared Telescope in Space (IRTS), launched In March 1995, was Japan's first infrared satellite mission. During its 28 day mission, IRTS surveyed about 7% of the sky with four instruments: A Near and Mid Infrared Spectrometer which covered wavelengths of 1.4 to 4 microns and 4.5 to 11 microns respectively, a Far Infrared Line Mapper which studied Oxygen and Carbon spectral lines at 63 and 158 microns, and a Far infrared Photometer which studied the sky at four bands centered at 150, 250, 400, and 700 microns. This data should add to our knowledge of cosmology, interstellar matter, late type stars and interplanetary dust. The European Space Agency launched the * Infrared Space Observatory (ISO) in November 1995. ISO, which observed at wavelengths between 2.5 and 240 microns, not only covered a much wider wavelength range than IRAS but was also thousands of times more sensitive than IRAS and viewed infrared sources with much better resolution. ISO took data for about 2.5 years (3 times times longer than IRAS). It ceased operations in April 1998 when its supply liquid helium ran out. ISO contained instruments which measured details of both the shorter and longer wavelength regions of the infrared spectrum, an infrared camera which had two infrared arrays, and a photometer. Unlike IRAS, which was an infrared survey mission, ISO is operated like a ground based observatory, having astronomers submit observing proposals to study specific astronomical objects in detail. As hundreds of astronomers from several countries study the data from ISO, important * new discoveries about our universe are expected to emerge. ISO has already detected dry ice in interstellar dust and hydrocarbons in some nebulae. The Midcourse Space Experiment (MSX) was launched in April 1996 and lasted until end of helium in Feb 1997. During its 10 months of operation, MSX gathered a vast amount of data at 4.2 - 26 microns. MSX studied the infrared emission from the gas and dust which permeates the universe. MSX had 30 times the spatial resolution as IRAS and surveyed areas of the sky which were missed by IRAS. * Link to an outside web site Last Updated: January 20, 1998 Discovery | What is Infrared | Importance | Infrared Universe | Recent Discoveries | Future Missions | Gallery | Activities | Infrared Links | Outreach Centers