Below 1.3 mHz the solar background level increases as well as the energy of the solar acoustic modes decreases. This situation yields the detection of low degree p-modes extremely difficult because the signal to background ratio is very small (S/B ll 1). Yet, these modes are of paramount importance to be able to infer the structure of the solar core. On the other hand, the extrapolation of the linewidths of p-modes of higher frequency seem to tell us that these modes live for many months thus allowing an improvement of the S/B ratio as the length of the observations increases; however, not much better of what we have now will be possible. Therefore techniques to search for small signals amongst noise have to be used. Here, we present the actual status of the search and the preliminary results so far obtained.