Introduction: Why the LMC Matters for Hot Core Studies
The MAGellanic Outflow And Chemistry Survey (MAGOS) targets the Large Magellanic Cloud (LMC) to probe hot cores around massive protostellar objects under subsolar metallicity. The LMC’s proximity offers a unique laboratory to study how chemistry and early star formation unfold when heavy elements are less abundant than in the Milky Way. By surveying a diverse sample of protostellar candidates, MAGOS seeks to map molecular inventories, temperature structures, and outflow dynamics that shape stellar birth in metal-poor environments.
Survey Overview: 30 Massive Protostellar Candidates
The project observes 30 luminous protostellar objects in the LMC, aiming to identify bona fide hot cores—compact, warm regions rich in complex organic molecules and distinct spectral lines. The selection emphasizes high-mass star formation, where feedback processes such as jets and outflows interact with the surrounding cloud. MAGOS combines high-sensitivity spectroscopy with spatially resolved mapping to disentangle core emission from surrounding envelope and outflow contributions.
Key Findings: Chemistry in a Subsolar Environment
Early results highlight several themes relevant to star formation under subsolar metallicity. First, hot-core–like chemistry is detectable despite lower overall dust and metal abundances, indicating robust pathways for complex molecule formation even when elemental reservoirs are constrained. Second, the relative abundances of certain carbon- and nitrogen-bearing species shift compared with Galactic hot cores, suggesting metallicity-dependent chemistry that influences the thermal balance and ionization structure of these regions. Third, localized heating from protostellar activity appears to drive rich organic chemistry, with molecular tracers revealing temperature gradients consistent with compact, warm cores embedded in cooler envelopes.
Outflows, Temperatures, and Molecular Inventories
Outflow activity is a common feature in the MAGOS targets, providing clues about accretion processes and feedback. By mapping line emission from molecules such as CO, HCN, and several complex organics, the study constrains gas temperatures and densities within the hot cores. The results point to a nuanced interplay between heating mechanisms and chemical evolution: strong UV fields and shocks from outflows can both enhance certain molecular pathways and destroy more delicate species, shaping the observable inventory.
Implications for Star Formation Theory
These findings have broad implications for how we model high-mass star formation in metal-poor galaxies. The presence of hot-core–like chemistry at subsolar metallicity supports the universality of certain chemical processes, while observed abundance shifts call for metallicity-aware astrochemical networks. Understanding these differences helps refine predictions for planet-forming potential, dust evolution, and the initial mass function in environments akin to the early universe.
Future Directions: Expanding MAGOS and Beyond
As MAGOS continues, deeper observations and higher-resolution mapping will sharpen core demographics and chemical timelines. Complementary theoretical work, including updated reaction networks tailored to subsolar conditions, will be essential to interpret the observed molecular inventories. The survey also sets the stage for comparisons with other low-metallicity systems, building a broader framework for how environment shapes chemistry and star formation across galaxies.
Conclusion
MAGOS demonstrates that hot-core chemistry thrives in the LMC’s subsolar milieu, offering crucial benchmarks for star formation theories in metal-poor environments. The survey’s integrated view of chemistry, dynamics, and temperature structure informs our understanding of how massive stars form and how their natal clouds evolve under diverse cosmic conditions.
