0Assigned ID: 2059
----- Attempting Submission 1 (Fri Apr 09 17:46:37 GMT 2021) -----STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME
STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUMEModified the PHASE constraint of Visit S2 to have a better phase coverage of the exoplanet transit.1627698703----- Attempting Submission 1 (Thu Jul 29 16:24:33 GMT 2021) -----
HST Phase II Proposal 16724 successfully submitted.
Receipt: # 16724-1
----- Attempting Submission 2 (Thu Jul 29 16:30:00 GMT 2021) -----
----- Attempting Submission 3 (Tue Nov 09 19:52:41 GMT 2021) -----
----- Attempting Submission 4 (Tue Jan 18 16:27:27 GMT 2022) -----
----- Attempting Submission 5 (Mon Aug 29 18:38:57 GMT 2022) -----
----- Attempting Submission 6 (Sat Jan 07 19:37:41 GMT 2023) -----The heavy data volume warning has already been dealt with in the past.Hydrodynamic atmospheric escape in a benchmark ultra-hot JupiterHydrodynamic atmospheric escape is thought to be the main avenue for early evolution in exoplanets ranging from gas giants to terrestrial worlds, as shown by demographic studies resulting from the Kepler survey. However, with only three exoplanets to date that display smoking gun evidence of hydrodynamic escape, most modeling efforts to understand this process have been limited to semi-arbitrary assumptions and artificial test cases. This has a downstream effect that limits our capacity to assess if sub-Jovian planets are able to retain their volatile-rich atmospheres. While hot Jupiters are under no threat of losing significant fractions of their mass, they are the best targets to study hydrodynamic escape because they have detectable signals of exospheric metals in transmission spectroscopy. These signatures can only be observed by HST in the ultraviolet. In this program, we propose to observe the transmission spectrum of the ultra-hot Jupiter WASP-76b. We predict that this planet is losing mass at a rate 10 times larger than that of HD 209458b, and we can detect escape of Mg and Fe at more than 5-sigma confidence in high resolution. We further predict that the escaping material fills the Roche lobe of the planet and is in a state of geometric blow-off. Our results will automatically yield a precise near-UV transmission spectrum of WASP-76 b, a crucial measurement to probe opacity sources in its stratosphere and rainout of metallic species.We shall observe two transits of the ultra-hot Jupiter WASP-76b using STIS/NUV-MAMA. The objective is to detect metals escaping from the planet, and producing in-transit absorption in emission lines between 2400 and 2900 angstrom. This program is time sensitive because it can only be executed when the planet transits. Thus, we set a periodic time constraint. It is imperative to observe as many orbits as possible in a visit to cover the entirety of the transit, as well as obtain out-of-transit baseline observations. UV observations are limited to a maximum of five orbits, so we set the phase constraints to allow five consecutive orbits per visit. There are multiple observing opportunities between early November 2021 and mid-February 2022, as well as the last months of Cycle 29.
We will use the E230M grating centered at 2707 angstrom with the square 0.2x0.2 slit aiming for the best spectrophotometric stability. We will use the TIME-TAG mode to allow us to break down each exposure into sub-exposures, which in turn is necessary to obtain a precise time series of fluxes. The ETC recommends a buffer time of 265 s, but at this value we would require special handling for the program because the number of buffer dumps exceeds 30. No further acquisition exposures are necessary in consecutive orbits within the same visit.
Each orbit was set to execute one peakup exposure before the science exposure. WASP-76 is too bright for a peakup using the MIRROR, so we use instead the G430L element; the aperture 31X0.05NDB is necessary to avoid saturation in comparison with other apertures. The wavelength calibration was set to happen after the science exposure in order to spend as much time as possible on target. Due to the position of our target in the sky, the available visibility is around 1700 s per orbit. In order to allow us to have as much time as possible on target, we set the schedulability to 30%.The Principal Investigator L. dos Santos has previously led two HST programs to pin down the high-energy environment and atmospheric escape rates of young exoplanets (GO-15934 and GO-16085), and specializes in atmospheric spectroscopy techniques for transiting exoplanets. In total, our team has published more than 20 first-author papers about evaporating exoplanets based on HST data. D. Ehrenreich and V. Bourrier detected and interpreted the evaporation of the warm Neptune GJ 436 b, a key result that fostered the field of UV characterization of exoplanets with HST. J. Seidel and J. Hoeijmakers are experts in studying the atmospheres of hot Jupiters using high-resolution spectroscopy. M. Lendl has an extensive experience with photometric measurements to characterize hot Jupiters and their atmospheres. 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. J. D. 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. Vidotto specializes 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. V. Parmentier and J. Wardenier are leading the global climate modeling of WASP-76 b. M. Alam specializes in visible and near-infrared characterization of the lower atmosphere of exoplanets, and has extensively worked on removing stellar activity effects from HST transmission spectra. J. Teske is a leading expert in determining the chemical abundances of planet-hosting stars using high-resolution spectra.Exoplanets and Exoplanet FormationStellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARF3-F9NOCoordinates updated to ICRS reference frame, epoch J2000.WASP-76J2000J2000STIS/NUV-MAMASpectroscopicNoNoE230M2707STIS/NUV-MAMASpectroscopicNoNoE230M2707The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode./private/var/folders/0q/ph_vqx8j58s5t8b4smvzpcf80002vw/T/OPVisit12714966991915608567.xml164196446700068.43297927144931(Tic-Visit
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