0 Assigned ID: 461 ----- Attempting Submission 1 (Fri Apr 07 09:56:33 GMT 2017) ----- HST Phase I Proposal 461 (Mg_W33_W94_Cy25.apt) successfully submitted. Receipt: # 461-1 ----- Attempting Submission 2 (Fri Apr 07 17:59:10 GMT 2017) ----- NB: To improve the transit light curve coverage, and obtain the WAVE exposures during the Earth occultation, we put the keyword WAVE=NO for all ACCUM exposures and for each HST orbit we added explicit WAVE exposures, that should be obtained during the Earth occultation. Second submission with an updated (slightly improved) value for T0c of WASP-33. 1131184192 ----- Attempting Submission 1 (Tue Jul 11 10:59:35 GMT 2017) ----- HST Phase II Proposal 15139 (15139.apt) successfully submitted. Receipt: # 15139-1 ----- Attempting Submission 2 (Wed Jul 12 07:45:57 GMT 2017) ----- Metals from deep atmosphere to exosphere in hot-Jupiters With STIS/UV observations we detected magnesium atoms at high altitude in the atmosphere of the hot-Jupiter HD209458b, probing lower regions in the atmosphere than previously done with Lyman-alpha observations (Vidal-Madjar et al. 2013). With the present program, we will search for magnesium and other heavy species in escaping atmospheres of 2 giant planets orbiting hot A and F-type stars: WASP-94Ab and WASP-33b.The observations will provide unprecedented information on the physical conditions (velocity, temperature, and density) in the upper atmosphere of these two hot-Jupiters. Targets have been selected for the expected high significance level of the atmospheric detections (>10 sigma). These exoplanets present favorable configuration for upper atmosphere observations because of the combination of high escape rates and large spatial extensions of the magnesium clouds surrounding them. The atmospheric signatures of the magnesium and other metals are therefore expected to be easily detectable. Moreover, the two selected exoplanets have highly different equilibrium temperatures, below and above the MgSiO3 condensation temperature. Consequently, because the metals observed in the escaping flow originate from deeper in the atmosphere where haze can condensate, the observations will constrain the physical processes taking place in the clouds that cannot be observed directly. We plan to execute 2 visits for each of the 2 exoplanets, each visit consisting of 5 consecutive HST orbits. All observations will be done with the STIS E230M echelle grating. The phase constraints will provide one to two HST orbits before the planetary transit, to measure the baseline stellar flux. With transit durations of 2.2 and 3.6 hours, we will obtain 1.5 to 2 HST orbits during the transit. The last orbit after the transit will be used to search for the presence of a comet-like tail, expected from the strong radiation pressure of the host stars. WASP-33 is too bright for a Time-tag exposure, we adopt ACCUM exposure of 400 seconds, as already done in our HST program ID#11576. This will provide 7 exposures per orbit, and enough individual exposures to allow efficient modeling and removal of the HST orbital phase trend (Vidal-Madjar et al. 2013). Although WASP-94 should allow for Time-Tag exposure with a buffer-time of 400 s, this would imply a too large number of buffer dumps. Therefore we chose to also adopt ACCUM exposure of 400 seconds fro WASP-94 as for WASP-33. To have the WAVE exposures obtained during the Earth occultation, we put the keyword WAVE=NO for all ACCUM exposures and added explicit WAVE exposures, that should be obtained during the Earth occultation. Planets and Planet Formation 6 false false true false false false false SUPPORTED STAR F3-F9 NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR A4-A9 V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. HD15082 J2000 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 The scheduling data was generated by CASM 25.2. 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