Astronomers around the world use radio telescopes to observe the naturally occurring radio emissions from well beyond Earth. They come from stars, planets, galaxies, clouds of dust and molecules of gas. Most of us are familiar with visible-light astronomy and what it reveals about these objects. “Visible” or “optical” light is what we see with our eyes, however, visible lightVisible LightThe wavelengths of electromagnetic radiation that are visible to the naked eye. doesn’t tell the whole story about an object. To get a complete understanding of a distant quasarQuasarAn apparently small (at least to observers on Earth) yet immensely powerful cosmic object. Some quasars (quasi-stellar objects, or QSOs) are strong radio sources. Radio-emitting quasars were the first to be discovered. These are some of the most distant objects in the Universe, and are believed to be fueled by supermassive black holes residing in ancient galaxies. or a planet, for example, astronomers study it in as many wavelengths as possible, including the radio range.
There’s a hidden universe out there, radiating at wavelengths and frequencies we can’t see. Each object in the cosmos gives off unique patterns of radio emissions that allow astronomers to get the whole picture of a distant object. Radio astronomers study emissions from gas giant planets, blasts from the hearts of galaxies, or even precisely ticking signals from a dying star.
Today, radio astronomy is a major branch of astronomy and reveals otherwise-hidden characteristics of everything in the universe.
What ARE Radio Waves?
Our eyes are built to see the cosmos in visible light. However, objects in the universe radiate many other types of light, across what’s called the “electromagnetic spectrum”. Light travels through space in waves, like ripples in a pond. Each ripple has a peak and a trough, which is called a cycle. An object emitting radio waves gives off many cycles in a very short period of time. During each cycle, the wave moves a short distance, which is called its wavelength.
Radio Frequencies and Astronomy by the Numbers
For radio emissions of all kinds, the number of cycles per second is called a frequencyFrequencyA measure of wave vibrations per unit time. Typically measured in hertz, or cycles per second. In radio astronomy, high frequency corresponds to shorter wavelengths, like submillimeter waves detected by ALMA. Lower frequency refer to longer waves, like centimeter waves detected by the VLA. . One cycle per second is called one hertzHertzA unit of measurement of a wave's frequency. Hertz are measured by the number of oscillations that occur per second. 1 Hertz (Hz) = 1 cycle or oscillation/second.. A thousand cycles per second is a kilohertz; a gigahertz is a billion cycles per second. Radio astronomers are most interested in objects that emit in the frequency range between 3 kilohertz and 300 gigahertz. It’s easier to think of these in terms of wavelengths, however, which range from a very large 100-kilometer radio wave to a very small one-millimeter wave. The largest wavelengths require arrays of telescopes to detect, while the smallest ones may only require a few (or only one) telescope.
Doing Radio Astronomy
The radio portion of the electromagnetic spectrum comes from energetic objects and processes in the universe. Because different wavelengths are given off by different objects, radio astronomers use a variety of methods and instruments to detect them. One type of instrument is a large dish that looks similar to a satellite TV dish. It’s called a radio telescope. While single-dish discoveries are often made, the observatories of NRAO usually link many dishes together in giant arrays to gather detailed radio images of distant objects.
Since we are a visual species, seeing or “imaging” is an important part of all astronomy, regardless of the type of light being studied. While radio telescopes don’t take pictures in the same way that visible-light telescopes do, the signals they detect are converted into data that can be used to make radio images. Radio astronomy data streams are brought together and processed in a supercomputer. The output can be turned into images that are colored in different ways to show characteristics of the object such as its temperature, “clumpiness”, or the strength of radio emissions from different regions. The resulting images let scientists and the public see the otherwise invisible radio objects.