Toward a Self-calibrating, Empirical, Light-weight Model for Tellurics in High-resolution Spectra

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Abstract To discover Earth analogs around other stars, next generation spectrographs must measure radial velocity with 10 cm s−1 precision. Since even microtellurics can induce RV errors of up to 50 cm s−1, achieving 10 cm s−1 precision requires precise modeling of telluric absorption features. The standard approaches to telluric modeling 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, may omit microtelluric features, which are an important contributor to the RV error budget at 10 cm s−1. To address these issues, we present a telluric model of the self-calibrating, empirical, light-weight linear regression telluric (SELENITE) 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 modeled by regression against it, and likewise non-water tellurics with airmass. The model does not require line data, water vapor measurements, or additional observations (beyond one-time calibration observations), achieves fits with a 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.