We have found evidence of a CNO/Fe excess in the integrated spectrum of 47 Tuc relative to a synthetic cluster built up of solar neighbourhood stellar spectra from Gunn & Stryker's library (GS, 1983). The 47 Tuc spectrum was synthesized between 3200 < λ < 9750å aided by the cluster color-magnitude diagram (Hesser et al. 1987) complemented with a low main sequence, which was simulated by a canonical initial mass function (IMF) of slope x = 2.8. If a flat IMF (Hesser et al. 1987) is attributed to stars earlier than M, then x ≍ 5 is necessary for lower masses. A similar synthesis procedure was previously applied to the Galactic open cluster M11 (Santos Jr. et al. 1990). The residuals from the spectral synthesis were analyzed between 3200 < λ < 5400å, where a blanketing stronger in 47 Tuc than in the solar model remained. This is the integrated version of blue/violet excesses found in 47 Tuc individual giants (Hesser et al. 1977). It is well known that 47 Tuc has lower [Fe/H] than the solar model, suggesting non-solar [CNO/Fe] as responsible for the blanketing. As the localized bands CN, C2 and CH are not enough to explain it, we have used 28 plausible diatomic molecular patterns (two examples are shown in Fig. 1) and a synthesis technique to suggest possible absorbers contributing to this blanketing. Fig. 2 presents the molecular model and the residuals shifted by a constant, where a NH localized band is clear. The CO molecule resulted the dominant distributed absorption (≍ 50% in flux of the total blanketing), followed by SiN (20%). Definite identifications of the absorbers need much higher resolution than that in GS's library (20-40å). On the other hand, the methods proved to be very efficient for analysing the 47 Tuc population by means of stellar synthesis and molecular synthesis.