Challenges in probing turbulent and magnetic support in cores: the W43-MM1 protocluster case study
Abstract
Context . Estimating the level of nonthermal support in cores is both challenging yet crucial for constraining the earliest stages of star formation and improving our understanding of the underlying physical processes. Aims . We aim to quantify the kinetic and magnetic support operating within the cores of the high-mass protocluster W43-MM1, and to test the simple assumptions behind the approximated virial theorem, which is used to interpret observations. Methods . We used ALMA 12 m molecular line observations of DCN (3–2), 13 CS (5–4), and CH 3 CN (5 3 –4 3 ) to estimate the kinetic support. The plane-of-sky magnetic field strength ( B POS ) was derived from ALMA 12 m dust-polarization observations using the Davis-Chandrasekhar-Fermi (DCF) method. The B POS estimates were obtained in areas with a diameter of ∼12 500 au (∼2.3″, the three-beam scale of polarimetric observations), which ensures statistically meaningful measurements for the DCF analysis. These values were then extrapolated to core scales (∼2500 au) using the density–field strength relation. Results . We derived kinetic support estimates for 45 cores (21 prestellar and 24 protostellar), of which 21 also have magnetic field support estimates. The velocity dispersions range from 0.34 to 4.48 km s −1 . The three-beam scale B POS values span 1.1–22.5 mG, which extrapolate to 1.1–49.3 mG at the core scale. Using the virial theorem, we find 16 out of the subset of 24 cores with turbulence alone (∼70%) to be stable against gravitational collapse. From the subset of 21 cores with both estimates, ten cores (∼50%) appear to be magnetically supported against gravity when considering magnetic fields alone. Combining both estimates, 18 cores (∼85%) are found with α vir,B > 1. These numbers are unexpectedly high, especially for protostellar cores that are expected to be undergoing collapse. Conclusions . We conclude that the contamination of the measured linewidths by organized motions (of order 1–3 km s −1 and consistent with previous observational studies), together with the omission of surface terms in the observational virial theorem, prevents us from accurately measuring the nonthermal support in cores. This highlights that any simplified framework of a virial analysis can introduce significant biases when assessing the physical support mechanisms within cores.
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BibTeX
@article{valeillemanet2026challenges,
title = {{Challenges in probing turbulent and magnetic support in cores: the W43-MM1 protocluster case study}},
author = {M Valeille-Manet and F Louvet and F Motte and A.M Stutz and C Arce-Tord and P.C Cortés and M Fernandez-Lopez and N.A Sandoval-Garrido and P Sanhueza and R.H Álvarez-Gutiérrez and S Chevalier and A Ginsburg and A Koley and P Saha and S Savorgnano and R Veyry},
journal = {Astronomy \& Astrophysics - A\&A},
year = {2026},
month = sep,
doi = {10.1051/0004-6361/202659121},
eprint = {2607.10029},
archivePrefix = {arXiv},
url = {https://hal.science/hal-05762871v1},
note = {CC BY},
}
RIS
TY - JOUR
TI - Challenges in probing turbulent and magnetic support in cores: the W43-MM1 protocluster case study
AU - M Valeille-Manet
AU - F Louvet
AU - F Motte
AU - A.M Stutz
AU - C Arce-Tord
AU - P.C Cortés
AU - M Fernandez-Lopez
AU - N.A Sandoval-Garrido
AU - P Sanhueza
AU - R.H Álvarez-Gutiérrez
AU - S Chevalier
AU - A Ginsburg
AU - A Koley
AU - P Saha
AU - S Savorgnano
AU - R Veyry
PY - 2026
DA - 2026/09/24
JO - Astronomy & Astrophysics - A&A
DO - 10.1051/0004-6361/202659121
UR - https://hal.science/hal-05762871v1
AB - Context . Estimating the level of nonthermal support in cores is both challenging yet crucial for constraining the earliest stages of star formation and improving our understanding of the underlying physical processes. Aims . We aim to quantify the kinetic and magnetic support operating within the cores of the high-mass protocluster W43-MM1, and to test the simple assumptions behind the approximated virial theorem, which is used to interpret observations. Methods . We used ALMA 12 m molecular line observations of DCN (3–2), 13 CS (5–4), and CH 3 CN (5 3 –4 3 ) to estimate the kinetic support. The plane-of-sky magnetic field strength ( B POS ) was derived from ALMA 12 m dust-polarization observations using the Davis-Chandrasekhar-Fermi (DCF) method. The B POS estimates were obtained in areas with a diameter of ∼12 500 au (∼2.3″, the three-beam scale of polarimetric observations), which ensures statistically meaningful measurements for the DCF analysis. These values were then extrapolated to core scales (∼2500 au) using the density–field strength relation. Results . We derived kinetic support estimates for 45 cores (21 prestellar and 24 protostellar), of which 21 also have magnetic field support estimates. The velocity dispersions range from 0.34 to 4.48 km s −1 . The three-beam scale B POS values span 1.1–22.5 mG, which extrapolate to 1.1–49.3 mG at the core scale. Using the virial theorem, we find 16 out of the subset of 24 cores with turbulence alone (∼70%) to be stable against gravitational collapse. From the subset of 21 cores with both estimates, ten cores (∼50%) appear to be magnetically supported against gravity when considering magnetic fields alone. Combining both estimates, 18 cores (∼85%) are found with α vir,B > 1. These numbers are unexpectedly high, especially for protostellar cores that are expected to be undergoing collapse. Conclusions . We conclude that the contamination of the measured linewidths by organized motions (of order 1–3 km s −1 and consistent with previous observational studies), together with the omission of surface terms in the observational virial theorem, prevents us from accurately measuring the nonthermal support in cores. This highlights that any simplified framework of a virial analysis can introduce significant biases when assessing the physical support mechanisms within cores.
SN - 0004-6361
SN - 1432-0746
ER -