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The presence of a volume density gradient in molecular clumps allow them toraise their star formation rate compared to what they would experience weretheir gas uniform in density. This higher star formation rate yields in turn ahigher value for the star formation efficiency per freefall time that wemeasure. The measured star formation efficiency per freefall time$\epsilon_{\rm ff, meas}$ of clumps is therefore plagued by a degeneracy, astwo factors contribute to it: one is the density gradient of the clump gas, theother is the intrinsic star formation efficiency per freefall time$\epsilon_{\rm ff, int}$ with which the clump would form stars should there beno gas density gradient. This paper presents a method allowing one to recoverthe intrinsic efficiency of a centrally-concentrated clump. It hinges on therelation between the surface densities in stars and gas measured locally fromclump center to clump edge. Knowledge of the initial density profile of theclump gas is not required. A step-by-step description of the method is providedas a tool in hand for observers. Once $\epsilon_{\rm ff, int}$ has beenestimated, it can be compared with its measured, clump-averaged, counterpart$\epsilon_{\rm ff, meas}$ to quantify the impact that the initial gas densityprofile of a clump has had on its star formation history.

Molecular clumps disguising their star formation efficiency per freefall time: What we can do not to be fooled