Magnetic geometry of M dwarfs in the southern PLATO field

M dwarfs are the most abundant stars in the Galaxy and exhibit diverse magnetic behaviours. While understanding their large-scale magnetic fields is essential for investigating stellar dynamos and assessing the impact of magnetic activity on planetary environments, their magnetic properties and long-term variability remain poorly characterised. Our aim was to characterise the large-scale magnetic fields of six M dwarfs in the southern field, with rotation periods ranging from approximately 1 to 17 days and masses between 0.26 and 0.64 M_⊙. Five of these stars are partially convective, while one is fully convective. These targets extend the mass–rotation diagram into previously unsampled regions. PLATO We analysed light curves to determine accurate rotation periods and optimise phase coverage for our spectropolarimetric observations. SPIRou data were reduced to obtain least-squares deconvolution (LSD) profiles and longitudinal field measurements, while synthetic spectra fitting yielded small-scale field strengths. We then applied ZDI to reconstruct the large‑scale magnetic topologies of the six targets. TESS We report a wide diversity of magnetic topologies among the six M dwarfs, with three main results: (1) Rapidly rotating (P_ < 2 d) early M dwarfs can generate dipole-dominated magnetic fields of moderate intensity, similar to those of less massive mid-M dwarfs; (2) Rapidly rotating mid-M dwarfs can generate non-axisymmetric large-scale magnetic fields featuring a significant toroidal component; (3) We report a moderately rotating (P_ ∼ 17 d) early M dwarf featuring a surprisingly weak large-scale magnetic field. rot rot Our findings further highlight the diversity of magnetic field configurations among M dwarfs, including in previously unexplored regions of parameter space. Long-term monitoring of our sample is crucial in order to distinguish persistent features from variability-driven excursions and to characterise the long-term evolution of their surface magnetic fields. Complementary photometry, including flare and spot‑induced variability analyses, will be essential to link surface activity with magnetic properties. PLATO