The high-density, turbulent, and overall extreme environment of the Central Molecular Zone (CMZ) can be used to probe disk scales in conditions similar to the star forming environment at cosmic noon (z~2). Multiple high-mass star-forming regions in the CMZ represent different stages of star formation. In young star clusters such as the Arches and Quintuplet clusters, there is evidence of a top-heavy IMF. Peering into early stages of star formation in the CMZ can help us understand if the IMF varies depending on the local environment and thus is shallower in the early universe.
We present ~500 AU resolution 3 mm and 1 mm ALMA observations of protostellar cores in the giant molecular cloud Sagittarius B2 (Sgr B2). This cloud accounts for over half of the total Star Formation Rate in the CMZ, despite containing ~10% of the mass and <1% of the volume. Previous observations of this region detected ~150 sources down to 8 solar masses. With a tenfold increase in resolution, we detect ~370 cores down to ~1 solar masses. A fifth of the new detections come from low-resolution detections fragmenting into multiple objects. We determine that the observed sources are most consistent with stage I YSOs that are warmer than in the rest of the Galaxy.