0 Assigned ID: 3172 ----- Attempting Submission 1 (Fri Mar 25 09:47:44 GMT 2022) ----- HST Phase I Proposal 3172 successfully submitted. Receipt: # 3172-1 ----- Attempting Submission 2 (Fri Mar 25 23:43:48 GMT 2022) ----- corrected wavecal aperture -2129114670 ----- Attempting Submission 1 (Sat Jul 02 16:20:21 GMT 2022) ----- ----- Attempting Submission 2 (Thu Nov 17 14:12:01 GMT 2022) ----- Observing the Overlooked Double Lyman-alpha Transit of HD 189733 b to Break Mass Loss Rate Degeneracies Lyman-alpha transits provide a window into atmospheric escape, a process that has observably shaped the exoplanet population. However, mass loss estimates from these observations are highly model dependent. A recently predicted feature of hot Jupiter transits could begin dismantling this model dependence: the delayed transit of the outflow tail. These transits have been hiding in plain sight, just slightly beyond the primary transits sampled by past Lyman-alpha transit observations. Critically, the plasma causing this delayed transit will have reached ionization equilibrium. Knowing the plasma's ionization state eliminates a confounding factor from the interpretation of the transit signal, enabling a stronger link between the the observations and the rate and efficiency of the planet's mass loss. This program will observe the delayed transit from the outflow tail of HD 189733 b, a planet with a well-established primary Lyman-alpha transit. The outcome will be an improved measurement of HD 189733 b's mass loss rate and efficiency, with broader implications for mass loss across the population of exoplanets. We will conduct all observations with STIS G140M/1222, a configuration with extensive heritage that limits contamination by geocoronal Lya airglow. HD 189733 has already been extensively observed in Lya with this mode. To measure the tail transit, we will stagger two five-orbit visits. To guard against evolution in the out-of-transit Lya flux between these sets, we will conduct two-orbit pre-transit visits approximately 24 or 48~h (again, timing limited by SAA passages) ahead of each 5-orbit transit visit. Dr. R. O. Parke Loyd has extensive experience in the reduction and analysis of HST data, with a numer of publications on the analysis of UV data of exoplanet atmospheric escape (JKulow et al. 2014, Loyd et al. 2017) and setllar activity (Loyd et al. 2014, 2016, 2018a,b). Dr. Loyd will carry out data reduction for the program. Drs. James Owen and Ruth Murray-Clay are experts in modeling exoplanetary escape (e.g., Owen and Alvarez, 2016; Murray-Clay et al., 2009, McCann et al. 2019). Dr. Owen modeled the atmospheric escape of the planets for which we propose observations and is responsible for an early prediction of the exoplanet radius gap (Owen and Wu, 2013). 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