The characteristics of the three different principal data sets that have been extensively analyzed in a search for g-modes (Tenerife, ACRIM, and Stanford) are reviewed, and the results claimed from the analysis are examined. It is noted that discrepancies betwen observers suggest that, though they have probably been detected, the solar g-modes have not yet been measured or classified. There is general agreement about the existence of signals, embedded in noise, in the low-frequency range where g-modes are expected to occur. The situation appears to be quite different from that for p-modes (e.g., lower frequencies and poorer SNR). It is concluded that, given the planned SOHO helioseismology experiments and earth-based networks of helioseismological instruments, there is real hope for success in the future.