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

We present the core mass function (CMF) of massive star-forming clump G33.92+0.11 using 1.3 mm observations obtained with Atacama Large Millimeter/submillimeter Array (ALMA). With a resolution 1000 au, this is one highest CMF measurements to date. The corrected by flux and number incompleteness obtain sample that complete for gas masses $M\gtrsim2.0\ M_\odot$. resulting well represented power-law ($dN/d\log M\propto M^\Gamma$), whose slope determined two different approaches: $i)$ least-squares fitting functions flux- number-corrected CMF, $ii)$ comparing observed simulated samples similar incompleteness. provide prescription quantify correct flattening bias affecting fits in first approach, which caused small-sample or edge effects when data either classical histograms kernel density estimate, respectively. slopes from both approaches are good agreement each other, $\Gamma=-1.11_{-0.11}^{+0.12}$ being our adopted value. Although appears be slightly flatter than Salpeter $\Gamma=-1.35$ stellar initial (IMF), we find Monte Carlo simulations statistically indistinguishable representation IMF. Our results consistent idea form IMF inherited at least high latter high-enough resolution.