0 Assigned ID: 576 ----- Attempting Submission 1 (Fri Mar 06 17:20:55 GMT 2020) ----- HST Phase I Proposal 576 successfully submitted. Receipt: # 576-1 ----- Attempting Submission 2 (Fri Mar 06 18:53:06 GMT 2020) ----- HST Phase I Proposal 576 successfully submitted. Receipt: # 576-2 LONG SU LIKELY TO INTERSECT THE SAA LONG SU LIKELY TO INTERSECT THE SAA Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Orbit number missing (probably due to addition of this sub-exposure after previous Orbit Planner processing). To learn more about orbit numbers, please read the full error text in the Diagnostic Report. Phase II, Submission Version 1. Ignoring SAA warnings for this 23-orbit phase curve observation. Error describing missing orbit number is incorrect. This is a known issue in APT. 1758523611 ----- Attempting Submission 1 (Tue Jun 30 14:43:44 GMT 2020) ----- Ignoring SAA warnings for this 23-orbit phase curve observation. Error describing missing orbit number is incorrect. This is a known issue in APT. Exoplanets on highly eccentric orbits offer unique insights into how planetary atmospheres respond to extreme variations in stellar forcing. By tracking the reradiation of heat during the planet's closest approach to its host star (periapse passage), we can test how a planet's atmosphere responds to extreme radiative forcing, and directly measure the radiative timescales that remain ambiguous for planets on circular orbits. We propose to observe with HST/WFC3 a partial-orbit spectroscopic phase curve of the highly-eccentric transiting exoplanet, HAT-P-2b. The planet's dayside temperature changes from being a typical Hot-Jupiter (1300~K) at apoapse, with no thermal inversion expected, to that of an Ultra-Hot-Jupiter (2400~K) at periapse, at which temperature thermal inversions are expected. Therefore, this target offers an opportunity to explore the transition between Hot- and Ultra-Hot-Jupiters. This WFC3 phase curve observation, will start before transit, continue through periapse passage, and end after secondary eclipse. The wavelength range offered by WFC3 will probe deep atmospheric pressure levels, where dynamical processes become relevant in shaping the observed spatial and temporal flux variations. The spectroscopic phase curve observation through periapse passage will be the key to constraining the timescales of atmospheric response, and to measure changes in the atmospheric vertical structure and opacities in this atmosphere. Our investigation will disentangle the contributions of radiative, dynamical, and chemical processes at work in strongly irradiated atmospheres, enabling it to become a model for the broader class of Hot and Ultra-Hot Jupiters. We will observe a partial phase curve of HAT-P-2b, starting 2-3 HST orbits before primary transit and ending 2-3 orbits after secondary eclipse. The observing start window is relatively lax (75 minutes) to enable as many observing opportunities as possible. The first orbit of Visit 01 consists of a direct image, a non-scanned spectrum to measure the spectra of any potentially-overlapping background stars, and the standard spatially-scanned spectra. The orient constraints are such that they avoid overlapping spectra with a faint source seen in the 2MASS image. The remaining 22 orbits are identicle, consisting of a direct image and 14 spatially-scanned spectra (7 in each direction), and have been separated into 2 visits to keep the total number of non-destructive reads below 400 per visit. Visit 2 should immediately follow Visit 1. The scan rate has been set to accumulate a maximum fluence of 42,500 electrons/pixel. The total scan length (400 pixels) fits comfortably within the 512x512 subarray. There is unused time at the end of each HST orbit for gyro bias updates. We will work with the STScI schedulers to plan the observation around SAA crossings. In order to make a precise measurement, we note that SAA crossings must only impact the latter half of an HST orbit and cannot coincide with in-transit or in-eclipse orbits. PI Desert is an expert on exoplanet atmospheres. Co-I Line will apply 1D Bayesian retrieval methods (Line et al. 2013, Line et al. 2014) to the measured time-dependent emission spectra to constrain atmospheric chemical abundances, metallicities, and the thermal structure. Co-Is Line, Fortney will lead atmospheric retrievals of the spectrophotometric data to constrain chemical abundances, metallicities, and the presence of clouds or hazes \citep{Line2013b,Line2014-C/O}. Co-Is Parmentier, Lewis, Kataria will generate 3D general circulation planet models for comparison to the acquired data. Co-I Lewis has developed a suite of 3D general circulation models that realistically couples radiative, dynamical, and equilibrium chemistry processes (Lewis et al. 2014). These simulations assume a range of atmospheric compositions, including atmospheres with and with TiO/VO that would result in the formation of atmospheric temperature inversions on the dayside of the planet. These models can also consider cases in which the assumption of pseudo-synchronous rotation. does not apply, thus allowing the planet to rotate at a rate that is significantly faster or slower than the assumed nominal value. Lewis will also develop new models that include a range of C/O ratios. Co-I Arcangeli, Stevenson, Bean, Kreidberg are expert in spectroscopic phase curves. CoI Todorov, Baxter are experts in Spitzer observations, useful for the combination HST and Spitzer. CoI Khorshid, Jacobs will help with the data analysis and interpretation of teh WFC3 data. Exoplanets and Exoplanet Formation 6 false false false false false false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 WFC3/IR Spectroscopic No No G141 1604494301501 /solaris/user1/williamj/hst/work/cycle28/OP-cache/16194-v01.xml Timing link suitability includes constraints ([Sequence (01 02) within 1.5 days]) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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