0 Assigned ID: 518 ----- Attempting Submission 1 (Fri Aug 17 23:57:20 GMT 2018) ----- H I Lyman alpha (1215.67 Ang; LyA) and O I (1302.2, 1304.9, 1306.0 Ang) are stellar emission lines in the COS FUV bandpass with great utility for stellar and exoplanet observations (e.g., chromosphere diagnosis and probing exoplanetary mass loss). However, emission from Earth's exosphere (airglow) entering through COS's large (2.5") aperture typically swamps the stellar LyA and O I signal in COS observations. Airglow subtraction is easily performed for STIS observations of these lines, because STIS employs a narrow slit and has spatial resolution in the cross-dispersion direction that simultaneously captures a spectrum of the airglow. Here we propose to apply proven airglow subtraction techniques homogeneously to the COS archive of F, G, K, and M dwarf spectra to extract true stellar LyA and O I spectra, increasing the number of stars with such spectra by a factor of 5. We will measure LyA and O I emission line fluxes and statistically compare fluxes and line kinematics to various stellar properties to uncover variations with mass and age. We will benchmark the airglow subtraction technique by comparing with STIS airglow-subtracted spectra for a subset of stars that have both COS G130M/G140L or STIS G140M/E140M/E140H spectra. We focus on stellar types that host exoplanets, because UV emission is an important for photochemistry in exoplanet atmospheres, but this program will produce legacy, user-friendly tools that will enable airglow subtraction on any COS spectrum. Planets and Planet Formation Stellar Physics 0 Legacy false false true false SUPPORTED