In the present work we used a grid of photoionization models combined with stellar population synthesis models to derive reliable Ionization Correction Factors ( ICFs ) for the sulphur in star-forming regions .
These models cover a large range of nebular parameters and yielding ionic abundances in consonance with those derived through optical and infrared observational data of star-forming regions .
From our theoretical ICFs , we suggested an \alpha value of 3.27 \pm 0.01 in the classical Stasińska formulae .
We compared the total sulphur abundance in the gas phase of a large sample of objects by using our Theoretical ICF and other approaches .
In average , the differences between the determinations via the use of the different ICFs considered are similar to the uncertainties in the S/H estimations .
Nevertheless , we noted that for some objects it could reach up to about 0.3 dex for the low metallicity regime .
Despite of the large scatter of the points , we found a trend of S/O ratio to decrease with the metallicity , independently of the ICF used to compute the sulphur total abundance .