Observational Studies of Massive Star Formation

This project will combine near infrared spectroscopy and radio continuum imaging. The spectroscopy allows the study of the molecular absorption lines, which give the structure of the cool gas very near to the star, and hydrogen and helium emission lines, which gives the velocity structure of any jet or wind present. These will be compared with the expected results from existing models for young protostars of this mass. Radio continuum data will also be used to study the jets. Continuum radio data will quantify the mass loss rate from the star. The high spatial resolution offered by radio imaging will be used to study the evolution, further constraining the emission mechanism present.This project will combine near infrared spectroscopy and radio continuum imaging. The spectroscopy allows the study of the molecular absorption lines, which give the structure of the cool gas very near to the star, and hydrogen and helium emission lines, which gives the velocity structure of any jet or wind present. These will be compared with the expected results from existing models for young protostars of this mass. Radio continuum data will also be used to study the jets. Continuum radio data will quantify the mass loss rate from the star. The high spatial resolution offered by radio imaging will be used to study the evolution, further constraining the emission mechanism present.