0 Assigned ID: 3753 ----- Attempting Submission 1 (Fri Mar 25 23:53:53 GMT 2022) ----- HST Phase I Proposal 3753 successfully submitted. Receipt: # 3753-1 ----- Attempting Submission 2 (Fri Mar 25 23:57:39 GMT 2022) ----- HST Phase I Proposal 3753 successfully submitted. Receipt: # 3753-2 0 ----- Attempting Submission 1 (Thu Jul 14 06:57:21 GMT 2022) ----- Constraining the mass loss in evaporating planets by catching the second tail Highly irradiated gas-giant exoplanets vigorously lose their atmospheres. This makes them excellent laboratories for extreme atmospheric physics - where we can study the effect of high levels of irradiation and stellar wind. Despite decades of observations with HST, the scientific value of the Lyman-alpha detections remains surprisingly under-exploited. In particular, the observations have not yet been able to precisely quantify planetary mass-loss rates. To address the gap between Lyman-alpha models and observations, a new observational pathway has been proposed to untangle the web of parameter interdependency. Originally identified in the 3D radiative-hydrodynamic simulations, this method requires measuring the second Lyman-alpha transits that are predicted to occur for hot Jupiters after the main transit. Second Lyman-alpha transits have never yet been probed or observed, despite this theoretical prediction. By measuring the time-delay of the secondary transit, the strength of the acceleration mechanism and the inertia of the outflowing gas can be measured, which is set by the mass loss rate. Thus, a measurement of a hot Jupiter's secondary transit will allow us to break the degeneracies that have plagued interpretation of Lyman-alpha transits, bringing firm physical constraints which will finally allow us to observationally, qualitatively constrain the mass-loss rate of an exoplanet. Our program will observe the HD209458 system three times, covering the nominal exoplanet transit in one visit, and then covering ten hours of post-transit time at subsequent transit events. Each observation will consist of 5 HST orbits which overlap in planet orbital phase by approximately 1.5 orbits. Combined, they will cover the entire planet transit plus any post-transit tail, caused by material escaping from the atmosphere and trailing behind the planet. The aim of the proposal is to measure the length of this post-transit tail. The transit duration of HD209458b is 3.05 hours, corresponding to 2 and 2.5 orbits. Visit 1, a 5-orbit sequence, will therefore capture the entire nominal transit, if there is no post-transit tail. We require observations before the transit to establish a pre-transit baseline. Visits 2 and 3 are also 5 orbits long, and will measure any extended egress (as is the case for many other exoplanets). Because we can accomodate ~ 30 mins of timing uncertainty, we set the phase requirements to +- 0.25 hours. We planned our observations so that the first orbit of each visit has an ACQ and ACQ-PEAKUP exposure, followed by a science exposure and wavelength calibration. Subsequent orbits only have a science exposure and a wavelength calibration exposure, with no ACQ or ACQ-PEAKUP. Because the few minutes' difference in orbital visibility due to precession has minimal impact on our science, we change the schedulability parameter from 30 to 90 to make scheduling easier. If possible, we kindly ask the Program Coordinator to expand our science observations to fill up the entire orbital visibility for the orbits that are actually scheduled. We do not forsee major impacts from reduced gyro mode. Dr. Spake is an expert in the analysis and interpretation of transiting exoplanets with space-based observatories, leading 3 successful HST proposals, 1 JWST proposal, and 1 Spitzer proposal. She has also led successful ground-based proposals to measure the tails of escaping exoplanet atmospheres. Dr. Owen is an expert in exoplanet atmospheric theorist and in analytic modeling of escaping atmospheres. Dr. Knutson is an expert on exoplanet atmosphere modeling and observations. Dr. Vissapragada is an expert on modeling and observations of escaping exoplanet atmospheres. Dr. Hillenbrand is an expert in ground-based observations and data analysis from the x-ray to millmeter wavelengths and in particular has expertise in stellar wind phenomena. Dr. Loyd is an expert in space weather and its effect on exoplanetary atmospheres, including the effects of stellar flares and atmospheric blow-off. He has led an HST proposal to obtain measurements of these processes on Neptune-sized planets. Co-I Schreyer is a graduate student working with Dr. Owen. Co-I Zhang is a graduate student working with Dr. Knutson. 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