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We present the core mass function (CMF) of the massive star-forming clumpG33.92+0.11 using 1.3 mm observations obtained with the Atacama LargeMillimeter/submillimeter Array (ALMA). With a resolution of 1000 au, this isone of the highest resolution CMF measurements to date. The CMF is corrected byflux and number incompleteness to obtain a sample that is complete for gasmasses $M\gtrsim2.0\ M_\odot$. The resulting CMF is well represented by apower-law function ($dN/d\log M\propto M^\Gamma$), whose slope is determinedusing two different approaches: $i)$ by least-squares fitting of power-lawfunctions to the flux- and number-corrected CMF, and $ii)$ by comparing theobserved CMF to simulated samples with similar incompleteness. We provide aprescription to quantify and correct a flattening bias affecting the slope fitsin the first approach, which is caused by small-sample or edge effects when thedata is represented by either classical histograms or a kernel densityestimate, respectively. The resulting slopes from both approaches are in goodagreement each other, with $\Gamma=-1.11_{-0.11}^{+0.12}$ being our adoptedvalue. Although this slope appears to be slightly flatter than the Salpeterslope $\Gamma=-1.35$ for the stellar initial mass function (IMF), we find fromMonte Carlo simulations that the CMF in G33.92+0.11 is statisticallyindistinguishable from the Salpeter representation of the stellar IMF. Ourresults are consistent with the idea that the form of the IMF is inherited fromthe CMF, at least at high masses and when the latter is observed at high-enoughresolution.

A Core Mass Function Indistinguishable from the Salpeter Stellar Initial Mass Function Using 1000 au Resolution ALMA Observations