  To discover Earth analogs around other stars, next generation spectrographs
must measure radial velocity (RV) with 10 cm/s precision. To achieve 10cm/s
precision, however, the effects of telluric contamination must be accounted
for. The standard approaches to telluric removal are: (a) observing a standard
star and (b) using a radiative transfer code. Observing standard stars,
however, takes valuable observing time away from science targets. Radiative
transfer codes, meanwhile, rely on imprecise line data in the HITRAN database
(typical line position uncertainties range from a few to several hundred m/s)
and require difficult-to-obtain measurements of water vapor column density for
best performance. To address these issues, we present SELENITE: a
SELf-calibrating, Empricial, Light-Weight liNear regressIon TElluric model for
high-resolution spectra. The model exploits two simple observations: (a) water
tellurics grow proportionally to precipitable water vapor and therefore
proportionally to each other and (b) non-water tellurics grow proportionally to
airmass. Water tellurics can be identified by looking for pixels whose growth
correlates with a known calibration water telluric and modelled by regression
against it, and likewise non-water tellurics with airmass. The model doesn't
require line data, water vapor measurements and additional observations (beyond
one-time calibration observations), achieves fits with a reduced chi squared of
1.17 on B stars and 2.95 on K dwarfs, and leaves residuals of 1% (B stars) and
1.1% (K dwarfs) of continuum. Fitting takes seconds on laptop PCs: SELENITE is
light-weight enough to guide observing runs.
