0Assigned ID: 782
----- Attempting Submission 1 (Fri Apr 08 20:19:20 GMT 2016) -----
HST Phase I Proposal 782 (K1GO24.p1.apt) successfully submitted.
Receipt: # 782-1
----- Attempting Submission 2 (Fri Apr 08 22:42:24 GMT 2016) -----
HST Phase I Proposal 782 (K1GO24.p1.apt) successfully submitted.
Receipt: # 782-2LONG SU LIKELY TO INTERSECT THE SAA
LONG SU LIKELY TO INTERSECT THE SAA
LONG SU LIKELY TO INTERSECT THE SAA
LONG SU LIKELY TO INTERSECT THE SAAResubmission.
We removed the single grism staring exposures at the beginning of each visit, to avoid persistence issues in the detector. I've updated the proposal description to reflect this.
Otherwise, this is the same as the previous version from early August.873233021----- Attempting Submission 1 (Thu Jul 21 15:57:47 GMT 2016) -----
HST Phase II Proposal 14664 (K1GO24.p2.apt) successfully submitted.
Receipt: # 14664-1
----- Attempting Submission 2 (Thu Jul 21 18:10:03 GMT 2016) -----
HST Phase II Proposal 14664 (K1GO24.p2.apt) successfully submitted.
Receipt: # 14664-2
----- Attempting Submission 3 (Tue Aug 02 06:45:34 GMT 2016) -----
----- Attempting Submission 4 (Wed Aug 24 20:04:52 GMT 2016) -----We are using WFC3/IR to observe an exoplanet target, and so each of our visits are 10 orbits long, which is within the 14 orbit limit fro exoplanet observations between SAA crossings.Phase-Resolved Emission Spectroscopy of the Transiting Brown Dwarf KELT-1b Using WFC3We propose to use 40 HST orbits to observe a spectroscopically-resolved orbital phase curve of the transiting brown dwarf KELT-1b from 1.15um to 1.65um using WFC3. KELT-1b is a 27MJ object on a short 1.217 day (29.2 hour) orbit around a bright (H=9.534) F5V star. This system is unique, in that it contains the only known highly irradiated brown dwarf on which it is possible to perform high precision atmospheric measurements. It thus gives us a chance to globally observe an irradiated atmosphere, when we know how that atmosphere should look in the absence of external irradiation. We intend to determine how irradiation affects the cloud properties and composition of KELT-1b's atmosphere, by comparing directly to observations of field brown dwarfs with a similar mass and age. We will also investigate the role surface gravity plays in setting the circulation and structure of hot Jupiter atmospheres, by comparing KELT-1b's high-gravity atmosphere to existing datasets for WASP-43b and WASP-103b. Finally, these observations will allow us to perform one of the first direct tests of brown dwarf surface gravity indicators. These observations will complement existing Spitzer observations of KELT-1b's phase curve at 3.6um and 4.5um, and an H-band eclipse spectrum that our group has already obtained from the ground.We will perform time-series spectroscopy using HST to measure a phase curve of KELT-1b. The observations will occur over four visits of 10 consecutive orbits each. We will use the WFC3 IR channel with the G141 grism to measure the planet-to-star flux ratio from 1.1 to 1.7 um during a complete orbit of the planet. The observations will be very similar to phase curve observations for WASP-43b for HST GO-13467.
The 10 orbits in each visit must be scheduled to avoid crossing the SAA.
I've labeled the visits according to what phases of the planetary orbit they cover. For example, "After transit to after eclipse" covers phases from just after a transit occurs to just after an eclipse completes.
The ephemeris we used in the phase 2 file is based on a transit measured during Spitzer observations from October 2015, which we used to determine a Tc closer to the current date and to refine the orbital period. The major difference from the discovery ephemeris is the orbital period is about 2 seconds shorter (updated period is 1.217494 days), which leads to transit predictions about 40 minutes earlier than the discovery ephemeris predicts.
The observations will be performed with the 256 x 256 subarray using SPARS10, NSAMP=15 (total time per exposure of 103 s) and the spatial scan mode with roundtrip scans to maximize the duty cycle (expected to be 80\%). We will use a scan rate of 0.097"/s, which will give peak counts of roughly 27K e-/pixel and a scan height of about 75 pixels. The peak counts is what is desired there, and sets the scan rate. We considered using SPARS5, but determined that we would end up losing too much on overhead compared to SPARS10. Following standard procedure, we will use an extra orbit at the beginning of each visit to allow the telescope and detector to settle. We will take a direct image with the F126N filter at the beginning of each orbit for wavelength calibration.
The phase constraints for each visit were chosen to ensure sufficient baseline before and after the transit and eclipse, and are not symmetric in orbital phase about the eclipses or transits (i.e., we're not starting around phase 0.25 or 0.75) in an attempt to have different parts of the orbital phase curve sampled with different detector systematics.
These phase contraints supersede the observing plan described in the proposal: they'll enforce the interleaving described in the proposal, but should allow easier scheduling than requiring the visits to be observed 36 HST orbits after one another.
If possible, we would like to have the two eclipse visits observed first ("After transit to after eclipse" and "Before eclipse to before transit").
We have not specified any orient ranges for the visits, just because the times these observations are possible is already pretty limited. In planning these observations, we have decided that the schedulabilty of the observations should outrank orientation and visibility constraints, so we've set the schedulabilty to 100, but once the observations are scheduled, if it is possible we would like to request the following:
There is a faint companion star 0.6 arcsec away from the target at a PA of 157.4 deg. If it's possible, we would like to orient the spacecraft so the the spatial scan is along this PA angle (towards or away, doesn't matter). I believe that along the PA angle would be orients of 292.17 or 112.17. An orient of 112.17 is only possible during the late Nov. 2016 visibility window. If the observations are scheduled during this date range, we'd prefer that orientation be used.
The actual orientation contraints are wider than this, to aid in scheduling. As it is, they should make it so that the companion star doesn't align closely with the target star along the dispersion direction. This is to allow the spectra of the target and the companion star to be separated.
Also, some of the data ranges allow for one more round-trip spatial scan exposure during an indivdual orbit. If these observations get scheduled for those longer visibility orbits, we'd appreciate if another scan could be added. Those dates are: Nov. 2016 and Dec. 2017.
That being said, the scientific goals of these observations will be possible without the orientation constraints or the extra scan, so it is not necessary to try and schedule specifically for any of these dates.Extrasolar Planets and Planet Formation12falsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETARY SYSTEMF3-F9NOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=9.682, H=9.534WFC3/IRSpectroscopicNoNoG141/tmp/OPVisit1985124230897697036.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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