other ways-- ask to see a list. Spot modulation from lightcurves: lower limit on coverage fraction Probabilistic spectral decomposition from spectroscopy: posterior constraint on starspot coverage and contrast
from lightcurves: lower limit on coverage fraction Probabilistic spectral decomposition from spectroscopy: posterior constraint on starspot coverage and contrast Also: many other ways-- ask to see a list.
and contrast Observed spectrum = Photosphere Starspot spectrum + Simultaneously vary photospheric, starspot, and spectral calibration parameters in a big MCMC to get joint constraints. Czekala et al. 2015, Gully-Santiago et al. 2017
atmospheres? 1. Precise knowledge of total spot coverage and contrast (this workshop / this talk) 2. Precise knowledge of the planet mass (Natasha Batalha et al. 2019) 3. Precision instrumentation (e.g. JWST) 4. Precise ephemerides (e.g. Benneke et al. 2017) 5. Critically evaluated exoplanet atmosphere models (last slides of this talk)
atmospheres? 1. Precise knowledge of total spot coverage and contrast (this workshop / this talk) 2. Precise knowledge of the planet mass (Natasha Batalha et al. 2019) 3. Precision instrumentation (e.g. JWST) 4. Precise ephemerides (e.g. Benneke et al. 2017) 5. Critically evaluated exoplanet atmosphere models (last slides of this talk)
for accurate characterization of transiting exoplanet atmospheres. Caroline Morley, Mark Marley, and I are beginning an effort towards semi-empirical models of ultracool dwarfs, which will inform exoplanet atmosphere modeling. High resolution near infrared spectroscopy (e.g. IGRINS) can help with both of these goals.