Further use of the data.
The full use of the data for scientific purposes requires the calibration of the intensity of the emission and the recording of timing information. A source of "white" noise is necessary in order to calibrate the intensity of the signal. The noise temperature of this noise source must be calibrated against a standard noise source such as the type 5722 current-saturated noise diodes. If available, an HP 461A wide band amplifier can be used as a noise source (with a step or variable attenuator). In order to calibrate the emission, the antenna must be disconnected from the input of the receiver and the noise source, conveniently attenuated, must the connected to the input of the receiver. The intensity of the noise can be varied using the step or variable attenuator. Make sure to record enough steps and cover from the galactic background level to the maximum deflection of Jupiter's emission. The noise temperature of the galactic background and those of Jupiter deflections can be determined by interpolation.
Radio station WWV timing signals can provide adequate timing information. WWV station transmit at the frequencies of 5, 10, 15, and 20 MHz.
The ability to identify the Jovian
emission and separate it from stations, static, or other types of interference
is an important consideration. The observer should constantly listen to
the audio output of the receiver. If the observer suspect that he/she is
receiving the emission, detuning the receiver a few kHz on either side
of the central frequency will help verify if what is being received is
a station or Jupiter. Radio stations are narrow band and should disappear,
Jupiter's emission is broad band and should continue to be received. Recording
of the receiver output in paper chart records provide a nice way of monitoring
the emission during the observation. The chart records can be used for
further data reduction and analysis, but their use is sometimes time consuming.
A personal computer with an A/D converter and chart recorder software will provide
a better way to display, monitor, store, retrieve, and process the information
(if further data reduction and analysis are to be made). Post- detection
time constants of about 1 second (sampling rate of 2 samples/sec) are adequate
for recording the envelope of both L and S bursts. Shorter time constants,
10-20 milliseconds or shorter, and faster sampling rates (50-100 samples/sec)
are necessary to resolve the faster S bursts.