0Assigned ID: 267
----- Attempting Submission 1 (Thu Apr 06 18:48:31 GMT 2017) -----
HST Phase I Proposal 267 (wasp80b.apt) successfully submitted.
Receipt: # 267-1
----- Attempting Submission 2 (Fri Apr 07 22:34:39 GMT 2017) -----
HST Phase I Proposal 267 (wasp80b.apt) successfully submitted.
Receipt: # 267-2ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUNPhase-II corrected from a problem on the XY PosTarget for Visit-01
Changed from SCHED30 to SCHED100
Updated T02070481101----- Attempting Submission 2 (Tue May 15 15:29:27 GMT 2018) -----
HST Phase II Proposal 15131 (wasp80b_phaseII.apt) successfully submitted.
Receipt: # 15131-2
----- Attempting Submission 3 (Fri May 18 19:14:22 GMT 2018) -----
HST Phase II Proposal 15131 (wasp80b_phaseII.apt) successfully submitted.
Receipt: # 15131-3
----- Attempting Submission 4 (Mon Jun 04 10:25:16 GMT 2018) -----There are 16 seconds visibility overrun for the first orbit of each visit.The first near-infrared reflectance spectrum of an exoplanetAmongst the important results that came out in the field of exoplanetology is that clouds and hazes in exoplanet atmospheres seem to be ubiquitous. Their presence provides important information on the chemistry and composition of atmospheres, and have major impact on planets' energy budgets and evolutions. Aerosols are also important observationally because they prevent probing deeper atmospheric composition, and they have been the common interpretation in a long list of published featureless transmission spectra. However, none of these indirect detections can definitely confirm or deny the presence of aerosols; thus, we propose a program that will change our view on aerosols by looking at their reflectivity.
Theoretical models and laboratory experiments have long speculated on the origins and properties of aerosols in exoplanet atmospheres. More recent studies have shown that photochemical hazes can be very reflective in the near-Infrared (NIR) for planets cooler than 900 K. We propose to tackle this revolutionizing idea by pioneering an observational program that will both test these new models and provide a novel way to study atmospheres of exoplanets.
We will look for reflective hazes in the NIR with WFC3 and deliver the first geometric albedo spectrum (Ag) of an exoplanet: WASP-80b. We will measure expected reflectivity (Ag=0.5) at high level of confidence (7-Sigma), and put stringent limits on haze models. This program will provide a pathway towards the study of exoplanets around low mass-stars through their reflectivity, which is urgent since these will be the golden targets for JWST. Only HST can provide the required precision for such an experiment.We propose to obtain time-series spectroscopy of the planet Wasp-80b (Hmag=8.5) during secondary eclipse using HST/WFC3, in order to measure its wavelength dependent spectrum of the planet.
We will observe five secondary eclipses of the planet (5 visits), containing each 4 consecutive HST orbits,
We will use the WFC3/IR instrument with the G141 grism to measure the spectrum of the planet from 1.1-1.7~\micron. We will use the 256 x 256 subarray with SAMP-SEQ=SPARS10, NSAMP=15 (total time per exposure of 103 s) and the spatial scan mode with bi-directional scans to maximize the duty cycle (expected to be 73\%). We will use a scan rate of 0.22''/s, which will give peak counts of roughly 22~ke$^{-}$/pixel and a scan height of about 190 pixels. The scan will fit comfortably in the 256 subarray and leave plenty of empty detector space to estimate the background.
A total of 19 exposures will be obtained in each orbit (18 for the first orbit of each visit, allowing for a F139M direct image for the wavelength calibration), and one orbit during each visit will occur during the secondary eclipse, and the remaining 3 orbits will be outside eclipse and used for normalization of the light curve.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETThis object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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