ABOUT ME
Hi hi! I am a Postdoctoral Researcher at the Max Planck Institute for Astronomy in Heidelberg, Germany. I work in the Planet and Star Formation department, on the Star Formation side of this group with particular focus on high-mass stars, their formation, accretion flows, evolution and lifetimes.
RESEARCH
Hierarchical flows from clouds to cores. Characterising the flow from pc to 1000 AU scales with ALMAGAL + IRAM 30m
In Prep • Expected 2026
Short summary of the paper. What the project studied, key methods, significance, etc.
From theory to observation: understanding filamentary flows in high-mass star-forming clusters.
A&A • 2025
Using multi-scale galactic MHD simulations, the study examined filamentary structures and star-forming clumps to measure flow rates along filaments, onto filaments, and radially around clumps. Flow patterns differed depending on feedback, with higher-feedback regions showing decreasing flows along filaments, while lower-feedback regions showed constant or increasing flows. Environmental inflows were sufficient to sustain filamentary flows. The flow rate measurement method produced results that closely matched the simulations, with significant overlap in both range and distribution.
Dynamical accretion flows: ALMAGAL: Flows along filamentary structures in high-mass star-forming clusters
A&A • 2024
Using ALMAGAL survey data, the study analyzed accretion flows along filaments in 100 high-mass star-forming regions, identifying 182 cores across four evolutionary stages. From 728 measured flow rates, the average accretion onto cores is ~10⁻⁴ M⊙ yr⁻¹, with rates increasing with evolutionary stage, distance from the core, and core mass. A clear ~M²ᐟ³ relationship between flow rate and core mass supports tidal-lobe accretion, highlighting how filamentary flows contribute to the growth of massive stars.
ATLASGAL - star forming efficiencies and the Galactic star formation rate
Monthly Notices • 2022
The ATLASGAL survey analyzed ~1000 embedded H II regions and found a broad correlation between clump mass and luminosity. Monte Carlo simulations of 200,000 clusters revealed that star formation efficiency (SFE) decreases with increasing clump mass—from ~20% in small clumps to ~8% in massive clumps—consistent with observations of nearby molecular clouds. Using this SFE trend and a 2 ± 1 Myr embedded phase, the study estimates the Galactic star formation rate at ~0.9 ± 0.45 M⊙ yr⁻¹, providing a direct method that avoids uncertainties in converting infrared luminosities to stellar mass.
Selected Publications
- Sawczuck et al. (2025). CASCADE: Filamentary accretion flows in Cygnus X DR20. Accepted by A&A.
- Schneider et al. (2025). Filamentary accretion flows in high-mass star-forming clouds. Accepted by A&A.
- Wells et al. (2025). From theory to observation: understanding filamentary flows in high-mass star-forming clusters. Accepted by A&A.
CURRICULUM VITAE
Coming soon
OUTREACH
Coming soon