0Assigned ID: 959
----- Attempting Submission 1 (Fri Apr 05 23:35:35 GMT 2019) -----
HST Phase I Proposal 959 (hst27.apt) successfully submitted.
Receipt: # 959-1
----- Attempting Submission 2 (Fri Apr 05 23:50:09 GMT 2019) -----
HST Phase I Proposal 959 (hst27.apt) successfully submitted.
Receipt: # 959-2
----- Attempting Submission 3 (Fri Apr 05 23:55:13 GMT 2019) -----
HST Phase I Proposal 959 (hst27.apt) successfully submitted.
Receipt: # 959-3
----- Attempting Submission 4 (Fri Apr 05 23:57:29 GMT 2019) -----Do we need an X offset for the scanning? I've heard some other programs have them, but wasn't aware of any charge transfer efficiency issues with the WFC3 IR detector.
Removed BEFORE constraints on all visits - they weren't needed and were there by mistake.783324432----- Attempting Submission 1 (Tue Jul 23 19:50:39 GMT 2019) -----
----- Attempting Submission 2 (Wed Jul 24 17:12:11 GMT 2019) -----Searching for Secondary Atmospheres in a System of Benchmark WorldsWe are moving from an era of exoplanet discovery into an era of exoplanet characterization, but small, potentially-rocky planets orbiting bright, nearby stars that are suitable for atmospheric characterization studies are relatively scarce. Here we propose to obtain time series spectroscopy using WFC3/IR to test for detectable atmospheric signatures of the three recently-discovered small planets (R=0.7, 1.3, and 1.4 Rearth) orbiting the nearby (10.6 pc), bright (H = 7.4) M3 dwarf L 98-59, the second closest transiting multiplanet system. The equilibrium temperatures for the outer two planets are close to or less than the H2 molecular escape temperature, raising the possibility of hydrogen-dominated atmospheres. We propose to obtain one transit for each of the outer two planets to test for hydrogen-dominated atmospheres. For the innermost sub-Earth-sized planet, due to its low expected gravity, a hydrogen atmosphere would be highly vulnerable to atmospheric escape. However, a water-dominated atmosphere is much more resilient, so we propose five transits of the innermost planet to test for a cloud-free water-dominated atmosphere. The host star is particularly quiet with no detected flares or rotational modulation, allowing a comparison between small planets orbiting an active late M-dwarf (TRAPPIST-1) and those around a quiet early M-dwarf (L 98-59), and pave the path for atmospheric characterization of the L 98-59 planets with JWST.The program will obtain time series spectroscopy of each of the three planets in the L98-59 planetary system. We will use WFC3's G141 grism and the 512x512 subarray. We will cover 5 transits of planet b, 1 transit of planet c, and 1 transit of planet d. Each transit is covered by a single visit, and each visit consists of four sequential orbits to obtain quasi-continuous coverage of the transits. The actual planet transits will occur in the third orbit of each visit, with two pre-transit orbits and one post-transit orbit. We will use the first orbit of each visit in our construction of the out-of-transit baseline flux if instrument systematics allow. Each orbit begins with a direct image of the target with the F130N filter for wavelength calibration. The remainder of each orbit will consist of MULTIACCUM exposures with the NSAMP = 4, SPARS25 readout pattern. To keep the fluence near 30,000 photoelectrons, we will use spatial scan mode with a 0.496 arcsec/sec scan rate, yielding a total scan height of 285.3 pixels), as recommended by Pandexo. To maximize the duty cycle of the observations (~60%), we will alternate between forward and reverse scanning along the detector.The proposed investigation relies on the precise planning of exoplanet transit observations with HST and the careful reduction and analysis of WFC3 data. Dr. Knicole Colon, Dr. Laura Kreidberg and Dr. Avi Mandell have expertise in these tasks. These investigators have all been PIs of successful HST observing campaigns in past cycles, which have in turn led to numerous publications based on the HST data collected (e.g., Kreidberg et al. 2014a,b, 2015, 2018a,b). Drs. Colon and Kreidberg were the PI and Co-PI on HST GO-15255 and led the planning and implementation of WFC3 transit observations of KELT-11b. Drs. Kreidberg led the reduction and analysis of those WFC3 transit observations.
Dr. Barclay, Dr. Mullally, Dr. Schlieder and Dr. Youngblood have expertise in stellar and exoplanet characterization using a variety of photometric and spectroscopic tools. Dr. Kostov was the lead author on the L 98-59 discovery paper and has experience modeling transits.
Dr. Kopparapu, Dr Hu and Dr. Lopez have expertise in interpreting exoplanet transmission spectroscopy, and will lead the theoretical modeling aspects of the proposal.
Dr Lopez is an expert in formation, evolution, and interior models of exoplanets, which will be applied to this investigations to interpret the findings from HST.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.158122752500017.022883491768113(Tic-Visit
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