Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5

Abstract

We present polarization maps of dust emission at 340 GHz in the luminous high-mass protocluster, W3 IRS5, observed with the Submillimeter Array. The projected magnetic fields appear fairly organized with a pinched morphology in the northern part and a concave shape in the southern part. We fit the polarization maps with a two-component magnetic field model: an hourglass model centered at the continuum peak, SMM2, and an empirical sphere centered at the O-type star, IRS7. Using the Davis-Chandrasekhar-Fermi method, we calculate a projected field strength of $B_\mathrm{pos} = 1.4 \; \mathrm{mG}$. Along with the Zeeman measurement, a total magnetic field strength of $B_\mathrm{tot} = 1.6 \; \mathrm{mG}$ is obtained. We find that the gravitational energy is the most dominant, followed by magnetic energy, and then turbulent energy. Small values of the virial parameter, $\alpha_\mathrm{vir} = 0.8$, and the ratio of timescales, $t_\mathrm{ff}/t_\mathrm{corss} = 0.6$, suggest an ongoing collapse. We also show collimated molecular outflows in the $\mathrm{CO \; (3-2)}$ and $\mathrm{SiO \; (8-7)}$ transitions. The morphology of magnetic fields and the surrounding \HII regions put forward a scenario for W3 IRS5. A gravitationally unstable dense core formed within a neutral gas ridge plowed by the expansions of W3 A and W3 B. The core began to contract, causing gravity to pull the magnetic field lines inward, which resulted in a pinched field morphology. Subsequent expansion of W3 F, ionized by IRS7, perturbed the magnetic field, creating concave patterns. The dynamical interactions among protostars led to misalignment of their outflows.