of Contents]People old and young enjoy waxing nostalgic about and learning some of the history of early electronics.
Popular Electronics was published from October 1954 through April 1985. All copyrights (if any) are hereby acknowledged.
you have never paid much attention to the state of the art in telescopes, then you might believe
they consist of either the $99 Tasco jobs in Walmart's toy department or the 200" Hale atop
Mount Palomar. You might also think that objects which emit or reflect light in the visible
spectrum are the only things studied. You might not know that telescopes have been built to
detect frequencies ranging from HF all the way up into cosmic rays. Newer telescopes search
for gravity waves and even neutrino and 'dark matter' pseudo particles. You might not know that
there is a broad selection of optical telescopes for amateur and research grade telescopes and
that the line between amateur and research grade telescopes grows less distinct every year.
Even radio telescope equipment is beginning to hit the market. This article gives a nice intro
to the subject of radio telescopy; the basics haven't changed.
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How We Listen to Stars and
Long-range radar is used to track the Sputniks in their orbits. A typical transmission-response
pattern appears above the symbol for the International Geophysical Year.
Astronomers call this probable radio source "NGC 5128" - it is thought to be two galaxies
in collision. This photo was made with the 200-inch Palomar optical telescope.
Scientist measures and records radio observations of satellites at Lincoln Lab's new long-range
radar station, Lexington, Massachusetts.
The largest parabolic radio. telescope is at Jodrell Bank, England; a movable dish,
it is a 250-foot monster which has also been used in tracking the Russian Sputniks.
Radio and radar help astronomers search outer space
By Mike Bienstock
It wasn't very long ago that astronomy, like the mythical Cyclops, had only one eye
- the optical telescope. Astronomers expected that bigger and better giant "eyes" would unlock
the remaining closed doors of the universe. Everything, it seemed, was progressing quietly in
its well-ordered way.
Then a second eye was developed, that of radio astronomy. A whole
new universe opened - an incredible dimension they didn't know existed. Today radio astronomy
is flourishing like a lusty youngster; it may some day equal or even exceed in importance the
4000-year-old science of visual astronomy.
Another branch of the science is long-distance
radar, which is now coming into its own in tracking the Russian Sputniks. As a matter of fact,
some of the giant radio telescopes have had radar antennas installed in them for this job.
Radio astronomy is the science dealing with radio-frequency
emissions from the stars, a phenomenon never suspected until about 1930, when Karl Jansky, a
Bell Laboratories engineer, began to study and measure different kinds of static at frequencies
around 20 mc. Before long he realized that the hiss-type static which he encountered was being
emitted from definite points in space. Working in his own backyard observatory, Grote Reber,
another radio engineer and a radio amateur, confirmed Jansky's discovery. Using a small parabolic
antenna, he plotted the first radio star sky map.
Giant strides have been made from
these small beginnings. Dozens of radio telescopes are scattered across the earth, their sensitive
antennas constantly probing the heavens, recording the strange radio impulses. We now know that
three types of "stars" emit radio waves: huge hydrogen gas clouds, made up of such a thin diffusion
of atoms that they would be called vacuums on earth; novae, which are stars that have exploded
with awesome violence; and collisions of huge star clusters or universes called galaxies.
Heretofore, one of the stumbling blocks for astronomers had been the huge masses of
dust scattered about the galaxies which prevented light from more distant stars from being seen
on earth. Scientists could only guess what lay beyond them. Now, however, radio astronomy is
unlocking even this secret. By focusing on gas cloud signals coming from behind the dust pockets
(at a frequency of 1420 mc.) , astronomers have been able to "count" the number of stars beyond.
Mind you, they are not only counting the number of gas clouds whose radio emissions pass easily
through the dust but - mathematically - the actual number of "visual" stars. They have learned
that the greater the radio emission from an area, the greater the number of stars that are located
there. Sources of Emission.
Radio emission from gas clouds was first predicted
in 1944. It wasn't until 1955, however, that the signal was picked up on radioscopes. But since
then astronomers have made up for lost time. They have used the 1420-mc. signal, and shifts
in this frequency caused by the Doppler effect, to determine how fast and in which direction
the gas clouds are moving. Such data have allowed them to plot the movement of our own galaxy,
the Milky Way, as well as to gather more information on our expanding universe.
second most intense radio source, in the constellation of Cygnus, has been found to be from
two whole galaxies in collision about 200 light years away. Another is listed only as NGC 5128
by astronomers. Others are being charted.
Our own sun has been proving a fruitful source
of radio propagation. Although the study of the radio spectrum of the sun was begun only within
the past few years, it has been determined that a huge amount of radio energy comes from the
areas around large and active sunspots. This is in the 5-meter band. It is thought that the
flares, being highly ionized gas, may produce strong electric fields when given rotational motion,
which in turn may be the cause of the radio emissions.
Of the planets, Jupiter was the
first to be picked up on radioscopes; the signals are apparently due to large-scale atmospheric
disturbances. Venus was next to be detected. Radio-frequency measurements showed this planet
to have a temperature higher than that of boiling water. Optical measurements had shown only
half that temperature, but since Venus is covered by a layer of clouds, the optical measurements
only took the cloud surface into account. Mercury, Mars and Saturn are expected to be heard
from soon via their radio signals. And some cosmic static comes from "dark" areas, where stars
have never been seen.
Two Types of Scopes. The radiotelescope is usually one of two types,
the parabolic reflector (dish), and the interferometer. There are other types - helical, horn,
and combinations of two or more types. The first two, however, are most generally used.
Photo of Jupiter, showing the huge "Red Spot" in the upper left-hand segment; this largest
of planets is a radio source as well.
The 61-foot movable parabolic antenna at Stanford Research Institute in Menlo Park, California.
The largest "dish" is the one just completed and now being tested at Jodrell Bank in England.
This has a diameter of 250 feet, and is steerable, which will allow it to cover all of the visible
sky. It will complement the fixed 220-footer in operation there for many years. Work has also
begun on a 140-foot steerable dish at Green Bank, West Virginia, which will be the largest of
its type in the United States.
Another new scope is under construction at the University
of Michigan - this 85-foot dish will be completed in time to aid the International Geophysical
Year effort. Recently completed was a long-range radar station at Lexington, Mass. Built by
the Lincoln Laboratory, this radar has been used successfully to track the Sputniks. It is also
being used to check the radio effects of meteors and the aurora.
One of the largest
interferometers is near Sydney, Australia. This consists of an array of dipoles 1500 feet long.
Essentially, the job of the radio telescope is to focus the radio waves it receives
and feed them into a sensitive receiver. This is analogous to the action of the optical telescope.
The parabolic dish, either solid or made of wire screen or mesh, reflects incoming radio waves
to a focal point, where they are picked up by a rod or dipole and fed to a receiver. The signal
is amplified, then sent to a mechanical recorder, usually a pen tracing the signal on graph
The interferometer, on the other hand, works in a different manner. The typical
telescope of this sort consists of a flat array of dipoles. When they face directly toward the
emission source, the wavefront reaches all the dipoles at the same time. This is shown as a
signal of maximum strength. When the signal comes in at a slight angle, it reaches one dipole
earlier than the next, and the interference of the out-of-phase waves cuts the signal strength.
To improve resolution, interferometers are built with a second array of dipoles arranged at
right angles to the first array. Where the two signals of maximum strength intersect, they produce
a "pencil" beam which has the resolution of a huge parabolic antenna. Diffuse Definition.
Radio waves from space are relatively unaffected by daylight, cloud or fog, which is a tremendous
advantage over light waves for observation, but their long wavelength compared to light makes
it difficult to gain good resolution. The beam width depends on the ratio of the wavelength
to the diameter of the telescope. Therefore, in order to gain the resolution of even a small
optical telescope, the antenna of a radioscope would have to be thousands of miles long. For
that reason, radioscopes are able to define a radio source only diffusely, causing the observers
to concentrate on the shorter wavelength. But as the larger scopes are built, they will be able
to push their studies up into the longer wavelengths. There is no doubt that even more and possibly
greater surprises are awaiting them in this region.
With the earth trembling on the
threshold of space, it would not be out of place to predict that man may one day soon construct
even larger radio telescopes between orbiting space stations, or even on the moon itself. It
is impossible to guess what tremendous discoveries there will be, but one thing is certain -
radio astronomy will some day rank with optical astronomy as one of the most important of sciences.
Indeed, it may even outgrow its older brother in unlocking the secrets of the universe. It won't
be long now!
How a Radio Telescope WorksRadio telescopes are tuned to receive
certain radio frequencies and indicate the direction from which they come. The two most common,
the parabolic reflector (dish) and the interferometer, use two different methods to gain the
same end. Note that in the dish (Fig. 1) there is a single response pattern, a fairly wide one.
The dish is used just like an optical telescope: it "focuses" on a point as closely as possible
- by using the maximum response point "A" on the radio source. On the other hand, the interferometer
(Fig. 2) responds with a series of lobes as the angle of observation of the radio source changes,
alternately reinforcing and canceling. Using the angles between these peaks, such as between
"X" and "Y," the position of the radio source can be calculated with a somewhat better degree
of accuracy. Posted October 31, 2013