Interstellar atoms and molecules
Pulsars, quasars, radio galaxies
Cosmic microwave background
Slide 49
Jansky's vertically polarized beam antenna was built in 1931 to study the direction of thunderstorms, which were suspected to cause signal-to-noise problems in Bell Lab’s initial transoceanic radio-telephone circuits.
In addition to detecting lightning, Jansky detected a signal that that appeared 4 minutes earlier each day and was strongest when Sagittarius was high in the sky.
The center of the Galaxy is in the direction of Sagittarius, so Jansky concluded that he was detecting radio waves from an astronomical source
Slide 50
Grote Reber read about Jansky's discovery.
In 1937, Reber built his own 32-foot-diameter parabolic dish antenna in his backyard in Wheaton, Illinois to seek cosmic radio emissions.
Slide 51
Grote Reber’s telescope
In the spring of 1939, he was able to detect cosmic radio emissions with his equipment. In 1941, he made the first survey of the sky at radio wavelengths (160MHz).
Slide 52
On display at Greenbank Radio Observatory
Greenbank, WV
Slide 53
Radio, millimeter, and submillimeter astronomy
The place of radio, millimeter, and submillimeter astronomy the study of astronomy
The parts of a radio telescope and how it works
The two big challenges of radio astronomy overcome by radio astronomers
Tiny signal strength of radio signals
Low angular resolution
Next generation radio, millimeter, and submillimeter telescopes
Slide 54
Antenna
Collects the radiation
Focuses the radiation on the receiver horn
Receiver
Horn
Amplifies the signal
Converts the radio-frequency signal to signals (current/voltage) we can record and analyze
Steering gear
Moves the telescope as it tracks the observed object
Slide 55
Parts of a radio telescope
Antenna
Receiver
Antenna
Receiver
Steering gear
Parkes 64-meter radio telescope
Slide 56
Film clip of Parkes Radio Telescope
from
“The Dish”
Slide 57