CChanged roll restrictions slightly (largest change is no more than 5 degrees) to incorporate comparison star and pointing uncertainty. Also, changed 'target' to the the center point between WASP-19 and a comparison star rather than WASP-19. Changed the x POS TARG for the spectral locations so that the centroid between WASP-19 and the comparison star now falls approximately at pixel 512. Changed a little in the observing description regarding date constraints. Changed the ACQ time slightly after noticing mild bleeding in previous observations. -1668186406 ----- Attempting Submission 2 (Thu Jun 27 09:14:01 GMT 2013) ----- ----- Attempting Submission 3 (Thu Jul 11 16:04:10 GMT 2013) ----- Characterization of extrasolar planets has accelerated rapidly thanks to low-density transiting hot Jupiters, which have large signals in transmission and secondary eclipse and enable the study of atmospheres in new and extreme conditions. Despite this, such observations are limited since they cannot directly be linked to physical atmospheric processes. Phase curves are crucial because they provide information about the circulation in a planetary atmosphere by constraining the day-night temperature contrast and horizontal wind speeds. The only existing exoplanet phase curves are photometric. We propose to measure the first spectroscopic phase curve, to probe the 3D atmospheric thermal, chemical and wind structure. Unlike previous work, this will constrain degeneracies between atmospheric opacities and temperatures. We will target WASP-19b, an ideal candidate with a short orbital period, large expected signal and constrained composition. We propose to measure the first near-IR phase curve using WFC3, to probe down to 0.4 bar, a previously unobserved regime and the deepest currently possible for thermal phase curves. WASP-19b is at the critical temperature where thermal redistribution could become less efficient. Deep-atmosphere observations, where advection should dominate, will provide the best constraints (Showman & Guillot, 2002) and will also reach down to the optical photosphere for transmission spectroscopy. The proposed observations will extend our knowledge to 3D circulation, and constrain physical processes in a previously unobserved altitude regime in an important object near the thermal redistribution efficiency limit. They are only achievable with the HST. This program uses the WFC3 instrument to perform precision photometry over the course of half an orbit of an exoplanet. The aim is to measure the change in brightness of the tidally-locked planet over the course of its orbit to determine how the planet's temperature varies across its surface. The target will be observed in 3 separate visits each containing 5 orbits. Each visit will be offset from the others in phase so that the gaps for Earth occultation occur in different phases of the planet's orbit for each visit. This will ensure that we obtain as complete coverage as possible over the duration of the phase curve. The first orbit of each visit will not be used for analysis due to the systematics introduced by the HST settling into its new pointing position. This is a well known phenomenon, and all other similar transiting HST programs have adopted this strategy. We will use the G141 grism to cover the wavelength range 1.1-1.6 microns and will adopt exposure times of 47 seconds. We wil use the 512 subarray to reduce overheads but still have a large enough FOV to encompass a comparison star, which will help us to correct for visit-long systematic trends. Each orbit contains 29 exposures (apart from the first orbit). We will use the new spatial scan mode which will lengthen the spectrum along the y-axis of the detector during an exposure. This avoids saturation and permits relativly long exposures, greatly increasing the efficiency. We will observe both WASP-19 and a comparison star simultaneously with a roll angle requirement to avoid overlapping spectra. There is an additional roll angle requirement in place due to a third star close to the comparison star. Our target for the observation is the center of the field between our science target (WASP-19) and the comparison star. This will be centred in the middle of the detector, meaning that each of the two stars we wish to observe will be in a different half of the detector. This strategy enables two different possilbe roll ranges 180 degres apart and eases scheduling. We have placed a constraint that we want to observe the target between November 2013 and June 2014. Out of this time, we would strongly prefer the period from February 2014 to June 2014. This is to enable ground-based monitoring of the star from the CTIO to characterise and remove contamination from stellar variability in the signal. WASP-19 is observable from the CTIO from November 2013 to June 2014, but the CTIO observing semester only actually starts in February 2014. We have put in a director's discretionary proposal to enable the observations to start sooner. If that proposal is accepted, then we can hopefully use the whole range between November 2013 to June 2014. Aside from this, each visit is phase constrained to start around a certain point in the planet's orbit. EXTRA-SOLAR PLANETS Default false false false false false SUPPORTED STAR EXTRA-SOLAR PLANETARY SYSTEM G V-IV Center point between WASP-19 and a comparison star. J2000 WFC3/IR Spectroscopic No No G141 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.770/0.787. The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1373558458279 /private/var/folders/89/xrgtq0854tsgshs0g8nzygxc0003rb/T/OPVisit3641269912369348463.xml It is essential that the 5 orbits be scheduled in a continuous block. (Tic-Visit :proposal-id 13431 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "11-Jul-2013 17:00:51.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 2962880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13431 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13431 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3017 :al-overhead-at-end 0 :internal-dur-at-end 728 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13431 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3155 :al-overhead-at-end 0 :internal-dur-at-end 723 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13431 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3155 :al-overhead-at-end 0 :internal-dur-at-end 723 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13431 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3155 :al-overhead-at-end 0 :internal-dur-at-end 723 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13431 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3155 :al-overhead-at-end 0 :internal-dur-at-end 727 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) true 5 0 Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.071/0.088. The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1373558505945 /private/var/folders/89/xrgtq0854tsgshs0g8nzygxc0003rb/T/OPVisit2828764545662262857.xml It is essential that the 5 orbits be scheduled in a continuous block. 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Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.203/0.220. The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1373558551943 /private/var/folders/89/xrgtq0854tsgshs0g8nzygxc0003rb/T/OPVisit8655388154589173330.xml It is essential that the 5 orbits be scheduled in a continuous block. 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Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time. Extra exposure to force buffer dump into occultation time.