Massive Star Formation Starts in Sub-virial Dense Clumps Unless Resisted by Strong Magnetic Fields

TL;DR

This study statistically constrains the initial dynamical state of high-mass star-forming regions, revealing they are sub-virial and often collapsing unless supported by strong magnetic fields, challenging existing theoretical models.

Contribution

It provides the first statistical evidence that high-mass starless clumps are sub-virial and highlights the importance of magnetic fields in supporting these regions against collapse.

Findings

Most HMSCs are sub-virial with Mach number <5.

Nearly all HMSCs are gravitationally bound with virial parameter <2.

Magnetic field strengths are correlated with density and are sufficient to support against collapse.

Abstract

The initial conditions are critical for understanding high-mass star formation, but are not well observed. Built on our previous characterization of a Galaxy-wide sample of 463 candidate high-mass starless clumps (HMSCs), here we investigate the dynamical state of a representative subsample of 44 HMSCs (radii 0.13-1.12 pc) using GBT NH3 (1,1) and (2,2) data from the Radio Ammonia Mid-Plane Survey (RAMPS) pilot data release. By fitting the two NH3 lines simultaneously, we obtain velocity dispersion, gas kinetic temperature, NH3 column density and abundance, Mach number, and virial parameter. Thermodynamic analysis reveals that most HMSCs have Mach number $<$5, inconsistent to what have been considered in theoretical models. All but one (43/44) of the HMSCs are gravitationally bound with virial parameter $\alpha_{\mathrm{vir}} < 2$. Either these massive clumps are in collapsing or magnetic field strengths of 0.10-2.65 mG (average 0.51 mG) would be needed to support them against collapsing. The estimated B-field strength correlates tightly with density, $B_{\rm est}/{\rm mG}=0.269\,(n_{\rm H_2}/10^4\,{\rm cm^{-3}})^{0.61}$, with a similar power-law index as found in observations, but a factor of 4.6 higher in strength. For the first time, the initial dynamical state of high-mass formation regions has been statistically constrained to be sub-virial, in contradictory to theoretical models in virial equilibrium, and in agreement with the lack of observed massive starless cores. The findings urge future observations to quantify the magnetic field support in the prestellar stage of massive clumps, which are rarely explored so far, towards a full understanding of the physical conditions that initiate massive star formation.