Infall Motions in the Hot Core Associated with the Hypercompact H ii Region G345.0061+01.794 B

Abstract

We report high angular resolution observations, made with the Atacama Large Millimeter Array in band 6, of high excitation molecular lines of ${\mathrm{CH}}_{3}\mathrm{CN}$ and SO _2 and of the H29 α radio recombination line toward the G345.0061+01.794 B HC H ii region in order to investigate the physical and kinematical characteristics of its surroundings. Emission was detected in all observed components of the J = 14 →13 rotational ladder of ${\mathrm{CH}}_{3}\mathrm{CN}$ and in the 30 _4,26 –30 _3,27 , and 32 _4,28 –32 _3,29 lines of SO _2 . The peak of the velocity-integrated molecular emission is located ∼0.″4 northwest of the peak of the continuum emission. The first-order moment images and channel maps show a velocity gradient of 1.1 km s ^−1 arcsec ^−1 across the source and a distinctive spot of blueshifted emission toward the peak of the zero-order moment. The rotational temperature is found to decrease from 252±24 K at the peak position to 166±16 K at its edge, indicating that our molecular observations are probing a hot molecular core that is internally excited. The emission in the H29 α line arises from a region of 0.″65 in size, where its peak coincides with that of the dust continuum. We model the kinematical characteristics of the “central blue spot” feature as due to infalling motions, suggesting a central mass of 172.8±8.8 M _⊙ . Our observations indicate that this HC H ii region is surrounded by a compact structure of hot molecular gas, which is rotating and infalling toward a central mass, that is most likely confining the ionized region. The observed scenario is reminiscent of a “butterfly pattern” with an approximately edge-on torus and ionized gas roughly parallel to its rotation axis.

Keywords

• Star formation
• Radio astronomy
• H II regions
• Molecular clouds
• Molecular gas