0 Assigned ID: 2930 ----- Attempting Submission 1 (Thu Mar 24 01:27:23 GMT 2022) ----- HST Phase I Proposal 2930 successfully submitted. Receipt: # 2930-1 ----- Attempting Submission 2 (Thu Mar 24 02:07:58 GMT 2022) ----- HST Phase I Proposal 2930 successfully submitted. Receipt: # 2930-2 ----- Attempting Submission 3 (Thu Mar 24 15:52:37 GMT 2022) ----- HST Phase I Proposal 2930 successfully submitted. Receipt: # 2930-3 ----- Attempting Submission 4 (Thu Mar 24 23:10:39 GMT 2022) ----- Spectroscopic characterization of transiting exoplanets with HST has led to a sea of change in our understanding of extra-solar atmospheres, from ultra-hot Jovians to temperate super-Earth worlds. Transmission spectra are sensitive to molecular and atomic absorbers, clouds/hazes, molecular weight, and average temperature at high altitudes along the limbs of the planet. Much of the theoretical and observational focus has been on understanding/interpreting the atmospheric properties that can be informed by optical/near-IR spectra--primarily due to the nominal observing mode/capabilities of HST and Spitzer. However, recent advances in HST observing modes and data processing (e.g., WFC3/UVIS-G280) have enabled simultaneous broadband NUV-to-Optical spectroscopy of transiting planets. However, there has been little theoretical development in understanding just how diagnostic NUV spectra, and their combination with longer wavelengths, can be. NUV spectra, owing to large refractory, gaseous opacities, are thought to be diagnostic of the onset of condensate cloud formation, vertical mixing, and refractory composition in planetary atmospheres. Our proposed theoretical work will develop a foundation for understanding the exoplanet atmospheric processes that benefit from NUV observations. We will develop an atmospheric population synthesis framework, leveraging state-of-the-art radiative convective models, to generate predictive atmospheric process hypotheses that can be tested with NUV observations and directly compared to publish datasets. This theoretical foundation will have implications for over a dozen planets over a dozen NUV HST programs and beyond. Our team brings together individuals with a variety of expertice in modeling and observing exoplanet atmospheres with HST, from the UV to infrared, as well as instrumentation experience. Our team is currently collaborating on/developing a dedicated UV NASA MIDEX mission to survey the UV spectra of transiting exoplanet systems and the stars that they orbit. Prof. Michael Line (PI) is an expert in modeling exoplanet atmospheres and has developed a bulk of the theoretical methodologies and concepts used to interpret transiting exoplanet observations with HST. This includes the development of the CHIMERA/ScCHIMERA atmospheric retrieval/1D-RCE modeling frameworks and subsequent innovations. Line also has experience in both HST and ground-based observational planning and analysis. Line will lead the modeling development/analysis. Dr. Joshua D. Lothringer is an expert in observing and modeling exoplanets, particularly ultra-hot Jupiters using the PHOENIX 1D-RCE model and the PETRA retrieval suite. He is PI or co-I of several HST proposals, including an AR program. Lothringer will co-lead the radiative convective modeling analysis with the PHOENIX retrieval code as well as colate the NUV spectra from various in-house programs. Dr. Travis Barman is a senior expert on both theoretical and observational aspects of exoplanets having modeled and observed directly imaged and transiting exoplanets for over two decades. As a lead developer of the PHOENIX model atmosphere code, Dr. Barman is responsible for maintaining and expanding its abilities to predict and interpret the atmospheric properties of exoplanets and the stars they orbit. Barman will work with Lothringer and Line in what physical processes need be included in the modeling frameworks. Dr. David Sing has 15 years of experience observing exoplanet atmospheres with the transit method. These observations span the FUV to near- IR with experience including serving as PI of the PanCET project which the largest transiting exoplanet program on HST to date and has produced many of the highest impact findings in the field. Sing will provide NUV transit spectra from his numerous HST programs. Prof. Evgenya Shkolnik is a leader in the field of stellar activity of planet hosts and magnetic and tidal star-planet interactions, working in these areas for over 20 years. She has extensive experience with monitoring stellar upper-atmospheric activity from the ground in the optical through the infrared, and from space in the ultraviolet (UV) through X-ray emission using the Hubble Space Telescope (HST), the Galaxy Evolution Explorer (GALEX), XMM-Newton, and ROSAT. She is also the PI of the SPARCS cubesat, a dedicated stellar UV flux monitoring mission. Shkolnik will provide insight into the influence of stellar effects on the physical processesin the upper atmospheres of the planets. Dr. Mark Swain was a pioneer in infrared transit spectroscopy of molecules in exoplanet atmospheres using the Hubble Space Telescope. He has extensive experience in infrared instrumentation, technology development, and served as the integration and test lead for the Keck Interferometer. Swain is currently the PI for the CASE Explorer Mission of Opportunity, the use participation in the ESA Ariel, a dedicated transit spectroscopy survey mission. Dr. David Ardila is an expert in UV diagnostics on star formation and stellar atmospheres. He has extensive NASA spacecraft development experience. He has served as instrument scientist for Astrophysics and Earth Science concepts, including SPARCS. He leads JPL's Strategic UV Initiative, to develop technology for UV spectroscopy applications. Dr. Kevin Stevenson is an expert in HST and Spitzer observations and data analysis accross the UV to mid-IR. He has led one of the largest Spitzer programs (660 hrs) and is also the Co-PI of the JWST Transiting Exoplanet Community Early Release Science Program. Stevenson will provide expertice on the synergies between UV and near-to-mid-IR observations. Ms. Lindsey wiser is a 2nd year PhD student with Dr. Line. She is currently working on radiative-convective grid modeling based fitting of HST WFC3 G141+Spitzer IRAC data. Wiser will work with Line to produce the population level models and subsequent observational diagnostics. 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