Assigned ID: 159
----- Attempting Submission 1 (Thu Feb 25 18:52:33 GMT 2010) -----
HST Phase I Proposal 159 (HST_WASP12.apt) successfully submitted.
----- Attempting Submission 2 (Fri Feb 26 18:07:09 GMT 2010) ---------- Attempting Submission 1 (Thu Jul 08 20:33:59 GMT 2010) -----The effect of radiation forcing on an exoplanet atmosphereWe propose to determine the effects of radiation forcing by the stellar primary on the atmosphere of the hot-Jupiter exoplanet WASP-12b using WFC3 near-IR spectroscopy. We will accomplish this by obtaining a completely unique data set consisting of the emission spectra sequence from the dayside, terminator, and nightside regions of the exoplanet’s atmosphere. In addition we will obtain the terminator region transmission spectrum; the combination of emission and transmission spectra will be used to help resolve the temperature/composition ambiguity present in interpreting emission spectra. The wavelength range we have selected, 1.1 to 1.7 microns, includes features from H2O, CH4, and CO2 – all of which have been detected in this wavelength range in the hot-Jupiter XO-1b with Hubble. The molecules H2O, CH4, and CO2 have been detected in three hot-Jupiter exoplanets to date; we expect to use these molecules as probes of the temperature and composition of the atmosphere of WASP-12b in the dayside, terminator, and nightside regions and thus determine the role of powerful radiation forcing on this exoplanet.Visits = 3
The visits have an individual science objective and a combined one.
(1) For the combined science objective, we include the observation of a calibrator source (HD 258439) at the end of each exoplanet host system observation (WASP-12). The science and calibrator observations should be executed as a continuous series of either 7 or 4 orbits in total. The objective is to obtain the best possible spectro-photometric calibration of the exoplanet host system in respect to the calibrator source which will enable a completely unique "following around the orbit" of an exoplanet and thus deriving the longitudinal spectroscopic changes of the atmosphere.
(2) for the individual science case, the exoplanet host system is followed constinuously over 5 or 2 orbits at different orbital phases in three visits. The visits are scheduled such that the third orbit is covering the secondary or primary eclipse event for the visits consisting in total of 7 orbits (5 on the exoplanet system). The visit covering 4 orbits is sceduled such that the 2 exoplanet orbits cover the epoch in between transit and secondary eclipse.
The observations always start with the exoplanet orbits and in the first orbit, a direct image is taken to establish wavelength calibration for the later G141 GRISM observations with WFC3. All remaining time on the exoplanet host system is filled with 7.6 s exposures using the G141 grism on NICMOS (SPARS10 sequence; NSAMPLE = 2). The immediately following orbits on the calibrator start also with a direct image followed by the same fast sequence of spectra taking (over two orbits) with G141.
To optimize the ability to decorrelate the observed flux for instrument changes, all observations need to be conducted at the same role angle. Additionally, there should be no role angle moves during a visit (also not in the repointing to the calibrator source).Visits = 3
The visits have an individual science objective and a combined one.
(1) For the combined science objective, we include the observation of a calibrator source (HD 258439) at the end of each exoplanet host system observation (WASP-12). The science and calibrator observations should be executed as a continuous series of either 7 or 4 orbits in total. The objective is to obtain the best possible spectro-photometric calibration of the exoplanet host system in respect to the calibrator source which will enable the extraction of the nightside and terminator region exoplanet emission spectrum.
(2) for the individual science case, the exoplanet host system is followed continuously over 5 or 2 orbits at different orbital phases in three visits. The visits are scheduled such that the third orbit is covering the secondary or primary eclipse event for the visits consisting in total of 7 orbits (5 on the exoplanet system). The visit covering 4 orbits is sceduled such that the 2 exoplanet orbits cover the 90/270 degree orbital phase angle position (epoch in between transit and secondary eclipse).
The observations always start with the exoplanet orbits and in the first orbit, a direct image is taken to establish wavelength calibration for the later G141 GRISM observations with WFC3. All remaining time on the exoplanet host system is filled with 7.6 s exposures using the G141 grism on NICMOS (SPARS10 sequence; NSAMPLE = 2). The immediately following orbits on the calibrator start also with a direct image followed by the 8 RAPID G141 exposures.
We request no role angle moves during a visit (also not in the repointing to the calibrator source), to optimize the stability.EXTRA-SOLAR PLANETS12false0.00.0falsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMThis object was generated by the targetselector and retrieved from the SIMBAD database.H = 10.227; J = 10.477; K = 10.188J200006 30 32.7940+29 40 20.29J2000STARA0-A3 V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.H = 9.114; J = 9.114; K = 9.104J200006 30 53.8035+29 25 23.61J2000WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141/private/var/folders/RC/RC7wfml9FQycwu13ilKJQk++OeY/-Tmp-/OPVisit1620608214030839790.xmlPhase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.815/0.850.Timing link suitability includes constraints ([Group (01 02 03) Within 5.0 days])The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.Primary Eclipse sequence for WASP-12 (5 orbits), which will be immediately followed by the calibrator source HD 258439 (2 orbits; no interupt - 7 orbits in total).(Tic-Visit
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)true70/Users/pderoo/Documents/paperassen/proposals/HST_2010_wasp12/PhaseII/OP-cache/apt_12230_stsci_revision4-v03.xmlPhase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.160/0.220.Timing link suitability includes constraints ([Group (01 02 03) Within 5.0 days])The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.Phase Curve sequence for WASP-12 (2 orbits), which will be immediately followed by the calibrator source HD 258439 (2 orbits; no interupt - 4 orbits in total).
NOTE: This visit is scheduled to be observed around phase 0.25. An equivalent observation is to observe around 0.75! We could however not give multiple options in the phasing requirements. If necessary, the phasing can be adjusted to be between 0.66 and 0.72 (see first image in WAVE_CAL_WASP-12).(Tic-Visit
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