0Assigned ID: 738
----- Attempting Submission 1 (Fri Apr 05 20:47:53 GMT 2019) -----
HST Phase I Proposal 738 (KELT-9b_emission_WFC3_v1.apt) successfully submitted.
Receipt: # 738-1
----- Attempting Submission 2 (Fri Apr 05 22:29:26 GMT 2019) -----
HST Phase I Proposal 738 (KELT-9b_emission_WFC3_v1.apt) successfully submitted.
Receipt: # 738-2
----- Attempting Submission 3 (Fri Apr 05 22:38:49 GMT 2019) -----Exposure 9 was missing POS TARG keyword in previous version.1083699004----- Attempting Submission 1 (Wed Jul 24 21:16:44 GMT 2019) -----
----- Attempting Submission 2 (Sun Aug 11 11:19:11 GMT 2019) -----
HST Phase II Proposal 15820 (KELT-9b_emission_WFC3_resubmitted_1.pdf.apt) successfully submitted.
Receipt: # 15820-2
----- Attempting Submission 3 (Sun Aug 11 11:27:07 GMT 2019) -----Measuring the first [Fe/H] of an exoplanetUltra-hot Jupiters are planets whose day-sides, hotter than 2,200 K, offer the opportunity to study the physics and chemistry of planetary atmospheres in a regime that is not accessible in the solar system or in other exoplanets. At such temperatures, molecules begin to dissociate and atoms become ionized, which gives rise to opacity sources such as H- or metal lines, that are more common in stars than planets. Indeed, recent observations at high resolution (R>100,000) from the ground revealed lines from metals in the atmosphere of the hottest planet of this category: KELT-9b (4,000 K). The most prominent lines belong to neutral and ionized iron. However, this kind of observations suffer from the contamination of Earth atmosphere, resulting in the loss of the planetary continuum. This is what prevented previous authors from measuring [Fe/H] for this exoplanet. With 6 HST orbits, we will observe the secondary eclipse of KELT-9b to: (1) provide the first direct detection of H-, responsible for generating the continuum in UHJ spectra, and constrain the overall metal enrichment of the exoplanet through the strength of this feature; (2) use the measured continuum level to calibrate ground-based high-resolution observations and provide the first measurement of [Fe/H] in an exoplanet.We propose to collect WFC3 spectra during one eclipse of KELT-9b (Hmag = 7.492), covered with a single HST visit. To properly sample the in-transit and out-of-transit baseline requires 6 consecutive orbits. These orbits need to be consecutive in order to sample the eclipse event. Two orbits will occur before eclipse, three during eclipse/ingress/egress and one after eclipse. The star is bright, thus we will increase the duty cycle by employing bi-directional spatial scans at 0.4380 arcsecs/sec. We will use a 512x512 subarray in SPARS25 mode with NSAMP = 5. The total scan length spans 334.973 pixels leaving enough space on the detector for background correction. A total of 19 frames will be obtained in each orbit (18 for the first orbit). Each orbit will be preceeded by one F164N direct image for the wavelength calibration and as sanity check for telescope pointing. The last exposure of each sequence for obits >=2 is performed with a forward scan only, to maximize the duty cycle. We offset the telescope in the Y direction with the POS TARG keyword to accomodate the spectrum in the center of the subarray (and avoid bleeding outside of the detector). We expect peak counts of 30360 electrons. With PANDEXO, we compute that we will reach an uncertainty of 26 ppm in 15 spectral bins on the eclipse depth after discarding the first orbit, as is customary with HST WFC3 transit/eclipse observations.
Estimated impact of reduced-gyro mode: this program should not be deeply affected by the reduced-gyro mode. The period of the eclipse is short, hopefully mitigating the reduced schedulability. Our serpentine spatial scan-rate is comfortably lower than the maximum 1 arcsec/sec allowed. No roll angle constraints are set for our program.Our team is comprised of experts in all of the aspects required for this project, including eclipse spectroscopy of exoplanets (Bean, Dwsert, Mansfield, Arcangeli), high-resolution cross-correlation spectroscopy (Pino, Hoeijmakers), modeling of day-side spectroscopy and climate of ultra hot Jupiters (Parmentier, Line, Komacek), joint interpretation of low- to high-resolution specrtoscopic data (Pino, Line, Desert).Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARA0-A3 V-IVEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Hmag = 7.492WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.It is essential that the 6 HST orbits are scheduled in a continuous block, to properly sample the eclipse event.
We have defined each HST orbit within a non-interruptible sequence, to ensure that all exposures defined within the sequence are taken during the same HST orbit.
We have defined phase constraints to cover the eclipse event, with the requirement that at least two orbits occur before the eclipse, and one after.157325842600071.0(Tic-Visit
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