0 Assigned ID: 4550 ----- Attempting Submission 1 (Wed May 24 19:49:34 GMT 2023) ----- HST Phase I Proposal 4550 successfully submitted. Receipt: # 4550-1 ----- Attempting Submission 2 (Wed May 24 20:35:15 GMT 2023) ----- ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser Corrected the CENTERAXIS1 value for each F300X exposure to match each G280 exposure for the three remaining visits. 1305362115 ----- Attempting Submission 1 (Thu Sep 14 08:49:36 GMT 2023) ----- ----- Attempting Submission 2 (Tue Feb 11 08:48:13 GMT 2025) ----- We have chosen not to preflash given advice from the CS. We requre subarrays for these observations as has been done in previous UVIS measurements for exoplanetss Upon Reflection: Unveiling a Cloud Transition with a High-Precision Reflected Light Spectrum Measuring reflected light of exoplanets in the optical gives us a unique view of the stellar radiation backscattered by the atmosphere or surface. Unlike transmission and emission spectra, reflected light is uniquely sensitive to the properties of aerosols and ultimately reveals how much energy is absorbed by the planet contributing to its overall energy budget and climate. Yet, few measurements of reflected light have been made, with only two published results of spectroscopic albedo measurements probing the wavelength dependence of scattered light. Here we propose to utilize the spectroscopic capabilities of WFC3's UVIS G280 grism to measure the reflected light from 350-800nm of Saturn-mass exoplanet WASP-69b, which will make it the coolest object studied with reflected light spectroscopy. We will: 1) obtain a benchmark high-precision exoplanet reflected light spectrum, 2) extend the temperature phase space of exoplanets probed in reflected light to uncharted parameter space, and 3) uniquely complement existing JWST observations by providing information that could unveil key transitions in cloud physics regimes. WASP-69b has an equilibrium temperature of 990K, putting it in a regime where a dominant cloud transition process analogous to the L/T transition on Brown Dwarfs may be occurring. Results from this program will not only allow us to begin unveiling these key cloud processes, but will also kick-start investigations needed to enable successful direct imaging missions (Nancy Grace Roman Space Telescope, HWO) whose goals are to study reflected light spectroscopy of exoplanet atmospheres. We will perform five secondary eclipse observations of the hot Jupiter WASP-69b using WFC3/UVIS G280. Each visit consists of four HST orbits each with 20 exposures of 73 seconds. The first orbit will contain an additional exposure for the F300X filter image to accurately obtain the posiion of the star in the subarray for wavelength calibration. Each visit is phase constrained to an eclipse event for zero phase 2457176.17789 with a period of 3.86814 starting between 0.4680437856150214 and 0.47163437150097404 (calculated using Pandexo). Eaxh exposure is performed in a subarry with a postarge of -50 so that the target is positioned in the center of chip2, and size axis[1,2] = 2050, 450 and center axis[1,2] = 2048, 1208. Subarrays are used to increase the efficiency of observations and reduce the number of buffer dumps which should occur during Earth occultation events. There are no orient constraints palced on these observations. The team has extensive experience analyzing HST time-series data, and modeling/interpretation of exoplanet spectra, including significant knowledge of clouds and exoplanet model development (see PICASO/Virga). M. Marley, L. Mayorga, and N. Batalha are leaders in the field of reflected light for solar system and exoplanet targets and developing models to interpret exoplanet atmospheres. H. Wakeford is the leading expert in the WFC3-UVIS G280 grism for exoplanet time-series observations and L. Alderson has expertise in exoplanet observations and data reduction. N. Lewis is an expert in 1D and 3D models of exoplanetary atmospheres in particular the consideration of dynamics and chemical regimes. D. Powell and S. Moran are leading experts in cloud modeling. J. Birkby is an expert in high resolution spectroscopy which can be paired with low resolution spectra. T. Greene, T. Bell, and E. Schlawin are experts in observations with JWST obsevations of WASP-69b which are highly complimentary to this program. This team is led by N. Batalha and H. Wakeford. Exoplanets and Exoplanet Formation 6 false false false false false false AVAILABLE STAR EXTRA-SOLAR PLANET EXTRA-SOLAR PLANETARY SYSTEM K III-I NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Spectroscopic No No G280 WFC3/UVIS Imaging No No F300X The scheduling data was generated by CASM 33.0. 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