Program: GN-2013A-Q-109

Magnetospheric observational proxies are used for indirect detection of magnetic fields in hot, massive stars via UV, optical, and X-ray spectral lines. With the increasing sensitivity and quality of infrared spectrographs, we need to develop a similar diagnostic in this wavelength range, not only for known massive stars, but also for populations of stars located in highly obscured regions, where UV and optical spectra are not easily available. We propose to use high quality J, H, and K-band spectroscopy from the GNIRS spectrograph to study a hot, massive star with a known magnetic field. By searching for variability in primarily hydrogen recombination lines, we will identify suitable lines for indirect magnetic detections. In addition to providing a tool for detection of magnetism in massive stars, we will further exploit these data to study magnetospheric kinematics, constrain the geometry of the ionized gas, as well as determine its physical properties.