0Assigned ID: 6502
----- Attempting Submission 1 (Thu Apr 10 16:04:00 GMT 2025) -----Changed the NUV/E230M apertures to 6x0.2 to minimize slit losses (with approval from STIS User Support)914499571----- Attempting Submission 1 (Tue Aug 12 15:09:20 GMT 2025) -----
----- Attempting Submission 2 (Tue Nov 11 19:06:21 GMT 2025) -----
HST Phase II Proposal 18108 successfully submitted.
Receipt: # 18108-2
----- Attempting Submission 3 (Tue Nov 25 16:31:55 GMT 2025) -----
----- Attempting Submission 4 (Thu Dec 18 16:19:27 GMT 2025) -----
----- Attempting Submission 5 (Thu Feb 26 15:07:43 GMT 2026) -----Instrument's safety has been verified.Beyond hydrogen and helium: an exhaustive survey of escaping metals in ultra-hot Jupiters around bright, hot starsTwo decades ago, HST UV observations spearheaded the discovery of atmospheric escape from exoplanets, and it is now widely accepted that this process explains exoplanet population demographic features, the chemical composition of atmospheres in Solar System bodies, and resolves the curious lack of atmospheres in worlds orbiting M dwarfs. A wave of theoretical efforts to understand escape in hot exoplanets ensued, with the caveat that many efforts have assumed that atmospheres are composed of pure H+He. With the knowledge that this assumption limits our understanding of atmospheric escape, we hit a breaking point in our theoretical efforts: how do we best incorporate metals in our models? Our blindspot to the effects of metallicity has a downstream effect that limits our capacity to assess if smaller planets are able to retain their volatile-rich atmospheres, as they tend to be more metal-rich than larger exoplanets.
While hot Jupiters orbiting A-type stars are under no threat of losing significant fractions of their mass, they are the best targets to study atmospheric escape because they have the strongest and most detectable signals of exospheric metals in transmission spectroscopy. These signatures can only be observed by HST in the ultraviolet. The new observations we propose to observe will complement archival data from previous programs and yield an comprehensive survey that will measure the abundances of metals in their outflows and assess how efficiently these planets are evaporating. Our study exhausts the sample of known ultra-hot Jupiters orbiting bright A-type stars, the most extreme planets known to us.In this program, we aim to obtain exoplanet transit time-series observations of five ultrahot Jupiters orbiting bright, A-type stellar hosts. These hosts have strong continuum flux in the UV, allowing for precise measurements of atmospheric absorption during exoplanet transits. In fact, some of them are actually too bright to be observed with first-order spectroscopy or TIME-TAG mode. We describe each case below. We decided to use the widest slit available and supported for this program to minimize slit losses. For first-order spectra, we shall utilize 52x2'', which has the most stable spectrophotometric precision; for echelle observations, there are not many options and we shall use the usual 0.2x0.2'' to avoid order overlap.
WASP-189b and MASCARA-4b: FUV observations with G140L using the TIME-TAG mode produce heavy data loads, which will require special handling. NUV observations are too bright for TIME-TAG mode, even with E230H, and we choose ACCUM mode instead. We choose an exposure time > 120 s to allow for parallized memory buffer dumps and minimize overheads.
KELT-17b: FUV and NUV observations with G140L and E230M, respectively, can be executed in TIME-TAG mode, but produce heavy data, which will require special handling.
KELT-9b: FUV observations with G140L exceed global count rate limit of 30k cts/s, so we decided to use the echelle mode E140M. Observations are too bright for TIME-TAG mode and we choose ACCUM mode instead. We choose an exposure time > 120 s to allow for parallized memory buffer dumps and minimize overheads.
KELT-20b: NUV observations are too bright for TIME-TAG mode, even with E230H, and we choose ACCUM mode instead. We choose an exposure time > 120 s to allow for parallized memory buffer dumps and minimize overheads.
Observability:
- WASP-189: January-June
- MASCARA-4: All year round
- KELT-17: October-February
- KELT-9: All year round
- KELT-20: March-SeptemberOversight and leadership:
The Principal Investigator L. dos Santos has previously led four HST programs to pin down the high-energy environment and atmospheric escape rates of exoplanets and specializes in transmission spectroscopy techniques for transiting exoplanets, as well as modeling of planetary outflows. Dos Santos is the main developer of the p-winds code, and will oversee the entire program, including the observational, archival and theoretical efforts. Dos Santos will also develop the adaptions to the p-winds and ATES modeling codes necessary to achieve the goals of this program.
Data analysis effort:
M. Alam and J. Kirk have extensive experience in ground-based and space-based transmission spectroscopy techniques, and will provide support in analyzing the data. S. Vissapragada has led studies of metastable He narrowband photometry in hot Jupiters, and developed theoretical frameworks to interpret them in the context of atmospheric escape. P. McCreery has experience in fitting atmospheric escape models to transmission spectra using Gaussian Processes to eliminate systematic effects, and will contribute to the data analysis effort. L. Ramos-Rosado has an extensive experience with low- resolution transmission spectroscopy with STIS, and will contribute to the data analysis in the NUV continuum to search for cloud-precursor species. D. Sing is a world leader in characterizing exoplanets using ground- and space-based instruments, and is involved in several large programs to perform panchromatic exoplanet studies. D. Ehrenreich has an extensive experience on UV data analysis of planet-hosting stars, space- and ground-based transmission spectra. A. Deline specializes in data analysis of time-series observations of exoplanets using space-based instruments, such as HST and CHEOPS. J. Hoeijmakers is a leader in high-resolution transmission spectroscopy of exoplanets using the cross-correlation technique.
Theoretical analysis effort:
V. Bourrier developed empirical and analytical tools to analyze and interpret observations of atmospheric escape from exoplanets, including the 3D upper atmosphere particle dynamics code EVE (Bourrier & Lecavelier des Etangs 2013; Bourrier et al. 2016; Allart et al. 2018). A. Vidotto and A. Allan specialize in simulating the space weather and stellar wind interactions of exoplanet upper atmospheres using hydrodynamical models, whose work has extensively been used to interpret HST observations. J. Seidel is an expert in studying the atmospheres of hot Jupiters using high-resolution spectroscopy and modeling planetary winds. J. Lothringer is an expert in both observing exoplanet atmospheres with HST, as well as atmosphere modeling with PHOENIX with extensive experience studying ultra-hot Jupiters. A. Oklopcic will contribute to the interpretation of the data using Parker-wind models in combination with CLOUDY models to simulate outflows in exoplanets. A. Garcia Munoz specializes in simulating outflows in hot exoplanets, and will contribute to development of new theoretical tools to interpret the archival and new observations we propose.Exoplanets and Exoplanet Formation0falsetruefalsefalsetruefalsefalsefalsefalsefalseSUPPORTEDEXT-STARA4-A9 V-IVEXTRA-SOLAR PLANETARY SYSTEMNOThis 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.J2000J2000EXT-STARA0-A3 V-IVEXTRA-SOLAR PLANETARY SYSTEMNOThis 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.J2000J2000EXT-STARA4-A9 V-IVEXTRA-SOLAR PLANETARY SYSTEMNOThis 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.J2000J2000EXT-STARA0-A3 V-IVEXTRA-SOLAR PLANETARY SYSTEMNOThis 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.J2000J2000EXT-STARA0-A3 V-IVEXTRA-SOLAR PLANETARY SYSTEMNOThis 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.J2000J2000STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoE230H2862STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoE230M2707The scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.Ephemeris from Lendl+2020. Transit midpoint uncertainty by January 2026 is << 1 minute.
In the FUV, the current strategy is to use G140L. But we can also consider going for E140M; ETC results for comparison are here: STIS.sp.2023891 (G140L results are in STIS.sp.2022820).1771821419000279.0(Tic-Visit
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ETC sim for 52x0.5'' aperture: STIS.sp.2022821 (SNR~57 at 1425 A)ETC sim for 52x2'' aperture: STIS.sp.2022820 (SNR~61 at 1425A)
ETC sim for 52x0.5'' aperture: STIS.sp.2022821 (SNR~57 at 1425 A)ETC sim for 52x2'' aperture: STIS.sp.2022820 (SNR~61 at 1425A)
ETC sim for 52x0.5'' aperture: STIS.sp.2022821 (SNR~57 at 1425 A)ETC sim for 52x2'' aperture: STIS.sp.2022820 (SNR~61 at 1425A)
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ETC sim for 52x0.5'' aperture: STIS.sp.2022821 (SNR~57 at 1425 A)ETC sim for 52x2'' aperture: STIS.sp.2022820 (SNR~61 at 1425A)
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)false50Star is too bright for TIME-TAG mode, even when using E230H. We decide to go with E230M to increase the wavelength range of the observation and set mode to ACCUM. We shall use a minimum exposure time of 120 s to allow for parallel buffer dumps, which maximizes the time on object. The count rate in the brightest pixel is only 3.85 cts/s, so one exposure of 120 s yields 462 cts, which is well below the MAMA saturation limit of 65,536 counts per pixel.Star is too bright for TIME-TAG mode, even when using E230H. We decide to go with E230M to increase the wavelength range of the observation and set mode to ACCUM. We shall use a minimum exposure time of 120 s to allow for parallel buffer dumps, which maximizes the time on object. The count rate in the brightest pixel is only 3.85 cts/s, so one exposure of 120 s yields 462 cts, which is well below the MAMA saturation limit of 65,536 counts per pixel.Star is too bright for TIME-TAG mode, even when using E230H. We decide to go with E230M to increase the wavelength range of the observation and set mode to ACCUM. We shall use a minimum exposure time of 120 s to allow for parallel buffer dumps, which maximizes the time on object. The count rate in the brightest pixel is only 3.85 cts/s, so one exposure of 120 s yields 462 cts, which is well below the MAMA saturation limit of 65,536 counts per pixel.Star is too bright for TIME-TAG mode, even when using E230H. We decide to go with E230M to increase the wavelength range of the observation and set mode to ACCUM. We shall use a minimum exposure time of 120 s to allow for parallel buffer dumps, which maximizes the time on object. The count rate in the brightest pixel is only 3.85 cts/s, so one exposure of 120 s yields 462 cts, which is well below the MAMA saturation limit of 65,536 counts per pixel.Star is too bright for TIME-TAG mode, even when using E230H. We decide to go with E230M to increase the wavelength range of the observation and set mode to ACCUM. We shall use a minimum exposure time of 120 s to allow for parallel buffer dumps, which maximizes the time on object. The count rate in the brightest pixel is only 3.85 cts/s, so one exposure of 120 s yields 462 cts, which is well below the MAMA saturation limit of 65,536 counts per pixel.Ephemeris from Lendl+2020. Transit midpoint uncertainty by January 2026 is << 1 minute.(Tic-Visit
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