0Assigned ID: 7553
----- Attempting Submission 1 (Thu Apr 16 19:06:57 GMT 2026) -----
HST Phase I Proposal 7553 successfully submitted.
Receipt: # 7553-1
----- Attempting Submission 2 (Thu Apr 16 23:05:44 GMT 2026) -----Third submission updates all G280 visits using custom subarrays to collect a single bias exposure at the end of the visit on the same subarray, as recommended by Chapter 12.1 of the handbook and following recommendations by co-investigators.
A major change request for permission to use the BIAS target setting was opened alongside this resubmission.159632161----- Attempting Submission 1 (Mon Aug 17 18:49:21 GMT 2026) -----
HST Phase II Proposal 18422 successfully submitted.
Receipt: # 18422-1
----- Attempting Submission 2 (Tue Aug 18 16:01:53 GMT 2026) -----
HST Phase II Proposal 18422 successfully submitted.
Receipt: # 18422-2
----- Attempting Submission 3 (Tue Aug 18 19:17:30 GMT 2026) -----The Forest and the Trees: Revealing the Silicon Vapor-Aerosol Transition Through G280 and E230M SpectroscopyWe propose a survey of seven transiting hot to ultra-hot Jupiters (HD 209458 b, WASP-94 b, WASP-17 b, WASP-79 b, HAT-P-32 b, HAT-P-67 b, MASCARA-4 b) with HST WFC3/UVIS G280 and STIS E230M spectroscopy to characterize the solid-to-gas transition of silicon species in their upper atmospheres. Our survey will utilize the complementary potential of the WFC3/UVIS G280, which can detect aerosol coverage from UV-visible aerosol opacity and scattering, and the STIS E230M, which can unambiguously detect gas-phase species (i.e., SiO) from their forest of absorption lines. Our target list samples five targets in the equilibrium temperature range of 1600-1900 K where silicon gas and aerosols are predicted to coexist, as well two control targets at 1450 K (where aerosol coverage should be global) and 2250 K (where silicon should be globally vapor). We target planets with prior observations in G280 or E230M to efficiently complete complementary datasets using a minimal number of orbits. By constraining the aerosol coverage and reservoir of silicon vapor at the limbs of these targets, we will be able to test theories of silicate condensation and global reprocessing under different irradiation regimes.This program will acquire transmission spectra for seven hot Jupiters through either the HST WFC3/UVIS G280, or the STIS/NUV-MAMA E230M. Each target in this program has been selected for its temperature and for having a pre-existing transit spectroscopy dataset from one but not both of the instruments listed above. The combined spectroscopic information in these complementary G280+E230M datasets will allow robust constraints to be placed on the atmospheric abundance of SiO vapor and coverage by silicate grain aerosols.
Our HST WFC3/UVIS G280 observations target four exoplanets: HD-209458 b, WASP-94A b, WASP-79 b, and MASCARA-4 b. A total of 19 orbits across 4 visits are requested for these observations. All targets have one visit allocated. Each exposure places the target on Chip 2 of the WFC3/UVIS detector and reach between 103% and 105% full well saturation, as per WFC3 ISR 2010-10, the WFC3/UVIS detector remains linear well beyond saturation. We use Chip 2 as recommended by previous G280 observing programs (e.g. GO-16086, GO-17183) for its better sensitivity and more reliable calibration. This requires setting the Y POS TARG argument to -50" to center the target on Chip 2.
Every observation begins with an F300X image taken of the target which will enable wavelength calibration during analysis. Where possible, exposures with the G280 after the first orbit collect one more frame than the initial G280 exposures in Orbit 1 to maximize use of target visibility in each orbit. The G280 is a slitless observing mode, and therefore orient constraints are placed on our observations to prevent contamination of the target star's dispersed traces by those of near-field stars. Where necessary, FLASH is set to ensure a background of at least 20 e- that minimizes CTE.
We set SIZEAXIS1=2100 and SIZEAXIS2=600 to define a subarray that lets us minimize data volume and overheads, and ensure that buffer dumps occur during occultation of the target by Earth so that no orbit visibility is wasted. For one target (MASCARA-4 b) we further reduce the subarray to size 2050x500 due to its lower exposure time. We set CENTERAXIS1=2148 and CENTERAXIS2=1208 to center the subarray on the center of Chip 2. As we are using custom subarrays, we additionally request bias frames be taken at the end of each G280 visit, with parameters matching the subarrays of our exposures. These parameters are based on successful observations of transiting hot Jupiters carried out as part of HST-GO 16086 and 17183.
Our STIS/NUV-MAMA E230M observations target three exoplanets: WASP-17 b, HAT-P-32 b, and HAT-P-67A b. A total of 50 orbits across 10 visits are requested for these observations. Four visits each are allocated to WASP-17 b and HAT-P-32 b, while two are allocated to HAT-P-67A b. All visits start with a target acquisition image collected through the STIS/CCD with the MIRROR element and the F28X50LP aperture. Each E230M exposure is taken in TIME TAG mode using 80% of the buffer time recommended by the ETC, as recommended by STIS Instrument Handbook chapter 11.1.3. This results in a maximum of 30 buffer dumps during any one visit, which is at or below the 30-per-visit threshold which would require special handling of this program. Observations are centered on 2707 AA and use the square 0.2"x0.2" slit. E230M exposures are shorter in duration during the first orbit to accomodate the ACQ exposure. We have disabled automatic WAVECAL exposures for our E230M observations and instead schedule them manually to occur during occultation of the target star by Earth, ensuring that we make full use of available visibility. These parameters are based on successful observations of transiting hot Jupiters carried out as part of HST-GO 16086.
STIS/NUV-MAMA observations are limited to no more than five consecutive orbits. For two of our targets this is sufficient to capture pre- and post-transit baseline flux as well as the full transit. However, HAT-P-67A b has a transit duration of 6.989 hours and there is no configuration of orbits that can capture the full transit and adequate baseline flux. We therefore set two different phase constraints on each visit, with one visit beginning before and ending during transit, while the other visit begins during and ends after transit. Combining these visits will enable us to recover the full transit of HAT-P-67A b. As requested in the Phase I APT, these two observations are constrained to occur within 30 days of each other to minimize degradation of the transmission spectrum due to stellar activity.V. Abby Boehm (PI, Cornell University) is an expert in data reduction for time-series observations of transiting exoplanets. Boehm has extensive experience with HST WFC3/UVIS G280 exoplanet studies and is a lead developer for an open-source pipeline for G280 data reduction.
Elijah Mullens (Co-PI, Cornell University) is an expert in exoplanet atmospheric modeling and retrievals. He has conducted multiple analyses of JWST and HST transmission and emission spectra with a focus on characterizing disequilibrium chemistry and aerosol properties.
Nikole Lewis (Co-I, Cornell University) is an expert in high-precision spectroscopic and photometric time-series analysis with HST and JWST as well as exoplanet atmospheric theory and modeling.
Joshua Lothringer (Co-I, Space Telescope Science Institute) is an expert in exoplanet atmospheric modeling and retrievals. He has particular experience with the ultra-hot Jupiter population and with NUV observations of such planets. He is also an HST/STIS instrument scientist.
Jason Dittmann (Co-I, University of Florida) is experienced in transit observations of exoplanets from both space- and ground-based platforms at high and low spectral resolution. He also has direct experience with HST/STIS data products.
Sarah Rugheimer (Co-I, University of Edinburgh) is an expert in habitable worlds and studying extreme environments like ultra-hot Jupiters. She helped develop the code utilized to reanalyze the archival HST/STIS spectroscopy of WASP-178b to detect SiO molecular absorption.
Sarah Moran (Co-I, Space Telescope Science Institute) is an expert in exoplanet atmospheric modeling and laboratory experiments. In particular, her expertise covers the chemistry and aerosol behavior of exoplanet atmospheres and how these lend themselves to the interpretation of both JWST and HST data.
Leonardo Dos Santos (Co-I, Space Telescope Science Institute) is an expert in observations and modeling of atmospheric escape in transiting exoplanets. He is the PI of several observing programs with HST and Keck to characterize the upper atmospheres of gas giants and Neptune-sized exoplanets. He is also the developer of the open-source code p-winds, which is widely utilized in the literature.
Lili Alderson (Co-I, Cornell University) is an expert in reducing, analysing and interpreting transiting exoplanet atmospheres with space telescopes.
Ailsa Campbell (Co-I, University of Bristol) is experienced in the data reduction of HST WFC3/UVIS G280 time series observations of transiting exoplanets.
Hannah Wakeford (Co-I, University of Bristol) is an expert in high-precision spectroscopic and photometric time-series analysis with HST and JWST, pioneering the use of the G280 grism for exoplanet time series analysis. She is also an expert in exoplanet aerosols and the impact of Si chemistry on the spectra.
Munazza Alam (Co-I, Space Telescope Science Institute) is an expert in reducing and analyzing time-series exoplanet observations from HST, JWST, and large ground-based telescopes. On the HST side, she has experience working with STIS and was a member of the STScI WFC3 instrument team. On the JWST side, she serves as the Deputy Lead of the JWST Time-Series Observations Coordination Team at STScI, and is the BOTS pipeline lead on the STScI NIRSpec instrument team.
Katy Chubb (Co-I, University of Bristol) is an expert in computing molecular opacities and running atmospheric retrievals, primarily using ARCiS.
Carlos Gascon (Co-I, Space Telescope Science Institute) is an expert in characterizing exoplanet atmospheres via transmission spectroscopy with both Hubble and JWST.
Esther Wang (Co-I, University of Bern) is an expert in NUV transmission spectroscopy with HST/STIS. She developed and applied an in-band/out-of-band statistical framework to detect SiO molecular absorption in HST/STIS E230M spectra. She has experience with E230M systematics modelling and high-resolution molecular detection methodology, and is also developing high-resolution atmospheric retrieval code.
Ryan MacDonald (Co-I, University of St. Andrews) is an expert in exoplanet atmosphere modelling and Bayesian retrievals of HST and JWST spectra.
Ryan Challener (Co-I, Cornell University) is an expert in 1D, 2D, and 3D characterization of exoplanet atmospheres, including applications to eccentric objects.Exoplanets and Exoplanet Formation6falsetruefalsefalsefalsefalsefalseAVAILABLESTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.WASP-94J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.WASP-17J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.WASP-79J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000STAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.HAT-P-67J2000J2000STARA4-A9 V-IVEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
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As requested in the Phase I APT, this visit is to occur within 30 days of Visit 14 (HAT-P-67 E230M Transit 2 of 2) to minimize degradation of the transmission spectrum due to stellar activity. This visit and Visit 14 have different phase constraints to ensure sufficient phase coverage is acquired to complete the full transit of HAT-P-67 b.(Tic-Visit
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