Figure 6: Spectra of foregrounds at the Tenerife frequencies. We represent the cross-correlation coefficients as a function of frequency for , and ((a), (b), and (c), resp.). From top to bottom, we plot the r.m.s. contribution from synchrotron, free-free, and dust to theTenerife data. In solid black and red, we show standard and best-fit models of the electromagnetic spectrum for each galactic emission. The models for dust are rescaled to fit the data. Details on the best-fit models can be found in the text.