  We present the statistical analysis of the spectral response of solar radio
type III bursts over the wide frequency range between 20 kHz and 410 MHz. For
this purpose, we have used observations that were carried out using both
spaced-based (Wind/Waves) and ground-based (Nan\c{c}ay Decameter Array and
Nan\c{c}ay Radioheliograph) facilities. In order to compare the flux densities
observed by the different instruments, we have carefully calibrated the data
and displayed them in Solar Flux Units. The main result of our study is that
type III bursts, in the metric to hectometric wavelength range, statistically
exhibit a clear maximum of their median radio flux density around 2 MHz.
Although this result was already reported by inspecting the spectral profiles
of type III bursts in the frequency range 20 kHz - 20 MHz, our study extends
such analysis for the first time to metric radio frequencies (i.e., from 20 kHz
to 410 MHz) and confirms the maximum spectral response around 2 MHz. In
addition, using a simple empirical model we show that the median radio flux $S$
of the studied dataset obeys the polynomial form $Y = 0.04 X^3 - 1.63 X^2 +
16.30 X -41.24$, with $X=\ln{(F_\text{MHz})}$ and with $Y=\ln{(S_\text{SFU})}$.
Using the Sittler and Guhathakurtha model for coronal streamers
\citep{Sit1999}, we have found that maximum of radio power falls therefore in
the range 4 to 10 $R_{\odot}$, depending on whether the type III emissions are
assumed to be at the fundamental or the harmonic.
