Unveiling the nightside of ultra-short period ultra-hot Jupiter TOI-2109b

0 Assigned ID: 4238 ----- Attempting Submission 1 (Wed May 24 03:20:34 GMT 2023) ----- LONG SU LIKELY TO INTERSECT THE SAA 0 ----- Attempting Submission 1 (Thu Sep 14 20:11:44 GMT 2023) ----- ----- Attempting Submission 2 (Mon Apr 01 20:50:03 GMT 2024) ----- ----- Attempting Submission 3 (Thu Apr 04 20:33:15 GMT 2024) ----- Double the period and halve the phase. Unveiling the nightside of ultra-short period ultra-hot Jupiter TOI-2109b TOI-2109b is an ultra-hot Jupiter on a 16-hour orbit recently discovered by TESS. It has a measured dayside temperature of 3631K which makes it the second hottest exoplanet ever discovered. The extremely hot dayside and short period make it the perfect target for immediate follow-up phase curve observation. We propose to measure two full phase curves including two eclipses each visit with WFC3/G141 to obtain longitudinally resolved emission spectra from the day to night side of the planet. This dataset will allow us to measure the planet's nightside spectrum and constrain the day-to-night heat circulation. We expect to detect strong hydrogen dissociation/recombination effects and increases H- abundance. TOI-2109b will fill the ultra-hot Jupiter population gap between KELT-9b and the rest of the planets in the ~3500K temperature range. We request two sets of 15 continuous orbits for the phase curve observation. The two visits will cover the HST phase gaps from Earth occultation. The first visit has a more flexible starting phase window of 48 mins, but the second visit should cover the HST phase gaps from earth occultation during the first visit. This is need for the science goals of measuring the complete planet phase curve and nightside emission. We request that two 15-orbit visits be performed. Due to problems encountered with APT when trying to specify 15-orbit visits, for the purpose of Phase 2 we have split each 15-rbit visit into three 5-orbit "segment1, segment2, segment3". We request that these visits be performed back-to-back, to achieve a single 15-orbit visit: i.e. visit1 = "visit1_segment1" + "visit1_segment2" + "visit1_segment3" Guangwei Fu is an expert in the analysis of HST WFC3 and STIS transmission and emission observations, including population-wide surveys with such data. He is is PI of 2 recent HST programs and Co-I in 5 upcoming JWST programs. Co-I Dr. Wong is an expert in phase curve observations. He has published multiple papers analyzing TESS and Spitzer phase curves. Co-I Dr. Shporer is an expert in transiting exoplanets phase curve observation and modeling. Co-I Prof. Komacek is an expert in ultra-hot Jupiter GCM modeling. Co-I Dr. Kitzmann is an expert in modeling ultra-hot Jupiter atmospheres. Co-I Dr. Deming is the Ph.D. advisor for Guangwei Fu and an expert in observing transiting exoplanets. He was P.I. for two large HST exoplanet programs using WFC3 in Cycles 18 and 23. Co-I Prof. Sing is an expert in the analysis and interpretation of HST exoplanet datasets, including population- wide surveys with such data. Prof. Sing is also an expert in calculating atmosphere models to interpret HST observations, particularly with the ATMO code. Prof. Sing has been PI of several HST programs, including small, large, and Treasury programs. Co-I Dr. Lothringer is an expert in both observing with HST, as well as atmosphere modeling and retrieval with PHOENIX. Dr. Lothringer has extensive experience studying the highly irradiated class of ultra-hot Jupiters and is PI of 4 recent HST programs and 2 upcoming JWST programs. Co-I Dr. Mansfield is an expert in exoplanet atmosphere observations. She has published mutiple studies with HST and Spitzer. Co-I Dr.Tan is an expert in modeling ultra-hot Jupiter atmospheres. Exoplanets and Exoplanet Formation 6 false false false false false false SUPPORTED STAR EXTRA-SOLAR PLANET G III-I This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/IR Spectroscopic No No G141 1712262506301 The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. 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