Parts of a radio telescope
Receivers
Primary antenna
Secondary
reflector
Hat Creek Radio Observatory
Steering gear
Slide 58
Parts of a radio telescope
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 59
Antenna surface errors
The surface error (accuracy of antenna surface and shape) should be less than 1/20 wavelength to keep losses to less than 30%
This results in much more stringent requirements for
sub-millimeter telescopes than for radio telescopes.
Slide 60
Antenna surface errors
1/20l=0.05mm
Millimeter
1/20l=0.015mm
Sub-millimeter
Smoother
Smooth
Smoothest
NRAO 12 meter (1mm-3mm)
Kitt Peak
JCMT (0.3mm-2.0mm)
Mauna Kea
1/20l=0.15mm
Radio
VLBA (3mm-3m)
Mauna Kea
Slide 61
Antenna surface errors
This image was taken during the SMT reflector's holographic testing showing that the deviations of the reflector are nearing the targeted 0.015 microns (about the thickness of a human hair)
Slide 62
Parts of a radio telescope
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 63
Receivers
Horn
Purpose of the horn is to collect the radiation directed to it from the antenna.
Amplifier
Increases the amplitude of the signal
Mixer
Used to change the frequency to a more easily used frequency
Slide 64
Receivers
Store data
Radio
Amplifier
mixer (mix to
baseband freq)
Convert to
desired form to record/analyze
Store data
Millimeter
Convert to
desired form to record/analyze
Submillimeter
Store data
Convert to
desired form to record/analyze
Mixer
(mix to lower freq)
Horn
Slide 65
Reasons to use a mixer