Directly convolving a modeled transmission spectrum biases low-resolution exoplanet retrievals; the correct approach is to convolve the stellar flux spectra and then take the ratio, and HR and LR helium observations are complementary.
Giant Tidal Tails of Helium Escaping the Hot Jupiter HAT-P-32 b
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abstract
Capturing planets in the act of losing their atmospheres provides rare opportunities to probe their evolution history. Such analysis has been enabled by observations of the helium triplet at 10833 \AA, but past studies have focused on the narrow time window right around the planet's optical transit. We monitored the hot Jupiter HAT-P-32 b using high-resolution spectroscopy from the Hobby-Eberly Telescope covering the planet's full orbit. We detected helium escaping HAT-P-32 b at a $14\sigma$ significance, with extended leading and trailing tails spanning a projected length over 53 times the planet's radius. These tails are among the largest known structures associated with an exoplanet. We interpret our observations using three-dimensional hydrodynamic simulations, which predict Roche Lobe overflow with extended tails along the planet's orbital path.
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Toward a unified framework for helium observations and interpretation of atmospheric escape
Directly convolving a modeled transmission spectrum biases low-resolution exoplanet retrievals; the correct approach is to convolve the stellar flux spectra and then take the ratio, and HR and LR helium observations are complementary.