Plasma line detected by Voyager 1 in the interstellar medium: Tips and traps for quasi-thermal noise spectroscopy

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Fig. 3.

Intensity of the line relative to the background as a function of its frequency, for the spectra acquired within the period shown in Fig. 1. The average power of the line of 14 ± 6% near 3 kHz increases to 20 ± 4% near 3.5 kHz, which is in agreement with Eq. (6).

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