Dynamics of the 6.7 and 12.2 GHz methanol masers around Cepheus A HW2

TL;DR

This study uses VLBI observations to map and analyze the dynamics of methanol masers around Cepheus A HW2, revealing infall motions and a likely shock interface in high-mass star formation.

Contribution

It provides detailed spatial and velocity mapping of methanol masers in Cepheus A HW2, proposing a new model of maser emission linked to infall and shock interfaces.

Findings

Maser spots form a filamentary structure over ~1350 AU.

Velocity field indicates infall, not rotation.

Maser emission likely arises in a shock interface.

Abstract

The 6.7 GHz methanol maser is exclusively associated with high-mass star formation. However, it remains unclear what structures harbour the methanol masers. Cepheus A is one of the closest regions of massive star formation, making it an excellent candidate for detailed studies. We determine the dynamics of maser spots in the high-mass star-forming region Cepheus A in order to infer where and when the maser emission occurs. Very long baseline interferometry (VLBI) observations of the 6.7 and 12.2 GHz methanol masers allows for mapping their spatial and velocity distribution. Phase-referencing is used to determine the astrometric positions of the maser emission, and multi-epoch observations can reveal 3D motions. The 6.7 GHz methanol masers are found in a filamentary structure over ~1350 AU, straddling the waist of the radio jet HW2. The positions agree well with previous observations of both the 6.7 and 12.2 GHz methanol masers. The velocity field of the maser spots does not show any sign of rotation, but is instead consistent with an infall signature. The 12.2 GHz methanol masers are closely associated with the 6.7 GHz methanol masers, and the parallax that we derive confirms previous measurements. We show that the methanol maser emission very likely arises in a shock interface in the equatorial region of Cepheus A HW2 and presents a model in which the maser emission occurs between the infalling gas and the accretion disk/process.