I have removed 2 exposures from each orbit and set the schedulability parameter to 100%. There is no visibility overrun for either visit according to APT. -621170463 ----- Attempting Submission 2 (Fri Dec 07 10:41:13 GMT 2012) ----- The First Transmission Spectrum of an Eccentric Cool Jupiter The techniques of transmission/emission spectroscopy are at the forefront of the characterization of exoplanetary atmospheres, allowing for a direct determination of elemental abundances, chemistry and temperature-pressure profiles. Hot Jupiters have dominated such studies due to their large spectroscopic signals. Despite this well-studied sample of similar exoplanets, the measured spectra exhibit surprising diversity, a fact which remains poorly understood. Since the hotter gas giants are well-observed, advancing our understanding of exoplanetary atmospheres requires the multi-wavelength detection of transits for exoplanets residing in cooler temperature regimes. We propose the very first transit observations, from the optical to the near-infrared, of a moderately-irradiated (~650-960 K), Jupiter-like exoplanet residing on an eccentric orbit (e=0.346): HAT-P-17b. Besides being in a previously unobserved temperature regime, its eccentric orbit allows the atmosphere of HAT-P-17b to periodically cross the condensation curves of sodium and potassium, implying that these alkali metals exist in the gas phase at periapsis and condense out into clouds/hazes at apoapsis. Furthermore, the range of temperatures allow for the carbon budget to be based on comparable amounts of CO and CH4. Our proposed observations will determine if the spectral features of K I, Na I, CH4 and H2O are present or absent from the optical to the near-infrared, thereby allowing us to constrain elemental abundances and atmospheric temperatures. This first dataset of a unique transition object will provide an insightful compliment to existing transmission observations of hot Jupiters. This program uses the STIS and WFC3 instruments to perform precision photometry during transit events. With the STIS instrument, we will observe the target during one transit, with the visit containing five orbits. We will use the STIS G750L grating to cover the wavelength range between 5300-10200 Å and use the 52”x2” slit to minimize slit losses. We will adopt exposure times of 140 seconds, with a sub-array size of 128, which is chosen to provide a sufficient time sampling of the HST orbital-phase trend such that it can be modeled and removed successfully. There will not be any gaps for buffer dumps. For each orbit, we will take 17 exposures of 140 seconds each, with 21 second overheads. We have set Wavecal=No for all STIS observations (as in previous similar programs such as GO 11740) such that the duty cycle and photometric precision is maximized. The zeropoint of the wavelength calibration will be determined from the stellar spectrum itself. We have also scheduled an explicit wavecal exposure after the HST is occulted by the Earth. For each exposure, S/N levels per resolution element of 500 at 7500Å will be reached for the G750L. The visit using WFC3/G141 will also observe one transit, with the visit containing 5 oribts. We will use the 256 sub-array to reduce the observational overheads. We will also use the new line scan mode which will lengthen the spectrum along the slit during an exposure. This avoids saturation and permits relatively long exposures (66 seconds), greatly increasing the efficiency. By degrading the S/N estimates of the ETC by a factor of sqrt(2) these exposure times give a S/N per resolution element of 2100. Each visit contains 5 orbits, which ensures high S/N transmission spectra are obtained. For each visit, there are three out-of-transit orbits, and two orbits occur during transit. The first orbit of each visit will likely not be used for primary analysis in the transit light curve, as the telescope thermally relaxes into its new pointing position during that time. This is a well known phenomenon, and all other similar transiting HST programs have adopted this strategy. Therefore, two of the out-of-transit orbits will be used to determine the baseline flux. Set Wavecal=No for the STIS observations (as in previous similar programs such as GO 11740) such that the duty cycle and photometric precision is maximized. EXTRA-SOLAR PLANETS 12 false 0.0 0.0 false false false false AVAILABLE STAR G V-IV K V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/CCD Spectroscopic No No G750L 7751 WFC3/IR Spectroscopic No No G141 /private/var/folders/fh/fho5qAVMEDWyN1p2kkC5Dk++0zA/-Tmp-/OPVisit6714871220722814962.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. HAT-P-17 STIS G750L. It is essential that the five orbits be scheduled in a coninuous block. 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CASM was run in Phase II mode. HAT-P-17 WFC G141. It is essential that the five orbits be scheduled in a coninuous block. (Tic-Visit :proposal-id 12956 :visit-id "02" :proposal-version -1 :trans-version "20121031" :date "07-Dec-2012 10:17:06.0" :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 1309792 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12956 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12956 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2645 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12956 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2709 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12956 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2709 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12956 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2709 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12956 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2709 :al-overhead-at-end 0 :internal-dur-at-end 470 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) true 5 0