Visit 0000001 requires 10281.6 seconds but separated by less than 4320.0 seconds from Visit 00000020Assigned ID: 870
----- Attempting Submission 1 (Fri Apr 11 21:30:08 GMT 2014) -----
HST Phase I Proposal 870 (kalas_fom_c22.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 23:54:19 GMT 2014) -----This is the usual warning error because we are requesting consecutive orbits and hence the short time requested between observations of the science target and the PSF reference star.I checked the phase2 file (2014-09-05) for final submission to scheduling.
The only change I made was to reduce the integration times for Fomalhaut exposures 6,7,8 so that they are exactly the same in Visits 2-5 and Visits 7-10.
This leads to ~10 extra seconds of unused orbit visibility and should create no scheduling problem.-283175507----- Attempting Submission 3 (Fri Sep 05 15:12:40 GMT 2014) -----Scattered light imaging of Fomalhaut's ice line belt to understand dynamical upheavals in planetary systemsThe dynamical history of the solar system in the first gigayear is thought to be complex and violent, with fossil evidence pointing to events such as the Late Heavy Bombardment and the formation of the Moon via a giant impact. The study of extrasolar planetary systems has also revealed tracers of vigorous dynamical evolution, such as the existence of hot Jupiters and cases of highly eccentric planet orbits. The closest planetary system with evidence of complex dynamics is Fomalhaut at 7.7 pc. Fomalhaut has two dusty debris belts - the cold belt at 140 AU imaged with HST and other facilities, and a warmer, ice-line belt at 8-12 AU which has not been resolved yet. Fomalhaut b has a highly eccentric orbit with periastron occurring a century ago at ~10 AU, and which is currently located at ~125 AU on its way to apastron at ~300 AU. Fomalhaut b may have been recently scattered outward by a more massive planet near the ice line belt, or inward by an outer planet close to the cold belt. If the dynamical upheaval occurred in the ~10 AU region, then the ice-line belt could have an asymmetric morphology. We propose a STIS imaging program optimized for detecting the ice line belt in scattered light for the first time. Concurrently, we will obtain deeper images with STIS to detect Fomalhaut b in 2015. This astrometric point is extremely valuable in constraining Fomalhaut b's orbital elements. In particular, its periastron distance and coplanarity with the belts are crucial elements in determining the likely location and mechanism for the system's dynamical upheaval.Our goal is to detect dust scattered light from Fomalhaut's ice line belt at ~10 AU radius (1.3") and detect Fomalhaut b at 13.6" projected radius.
ICE LINE BELT: For the purpose of planning the observations, we assume the ice line belt is a narrow width structure located somewhere in the range between 8 and 10 AU radius, with an inclination to the line of sight and position angle identical to that of the 140 AU belt. The maximum that the HST roll angle orientation can be changed is 30 deg. This will lead to significant self-subtraction of the belt and therefore requires a PSF reference star. We will use WEDGEB1.0 for the ice-line belt imaging.
We also use a subarray of size 230 pixels to minimize readout time overhead.
FOMALHAUT b: Within each orbit (one visit = one orbit), after WEDGEB1.0 exposures, we move to WEDGEB2.5 for deeper exposures (30 seconds) aimed at detecting Fomalhaut b. Knowledge of previous Fomalhaut STIS data allows us to orient the telescope such that Fomalhaut b will land in an azimuthal region that is relatively clean from residual scattered light artifacts. To improve observing efficiency we use a subarray size of 700 pixels. Since the wedge midline is at Y=305, we request the available but not supported CENTERAXIS2=350, which was used in GO-12923.
ORBIT STRATEGY: Accurate PSF subtraction requires that the PSF star is observed in a consecutive orbit with the Fomalhaut observations. However, only 4-5 orbits can be scheduled in a continuous sequence. Therefore we plan on two sequences of four orbits on Fomalhaut and one orbit on the PSF reference Vega. Initially we wished to insert the PSF observation in the middle of each 4-orbit Fomalhaut sequence. However, due to scheduling constraints, the observations of the PSF star was moved to the beginning of each sequence. The problem was that the PSF star in the middle of the sequence resulted in a wasted orbit (no data taken) due to the time it takes to slew the telescope between Vega and Fomalhaut.
ORIENTs: Due to scheduling constraints, the initial absolute ORIENT for the Fomalhaut sequence was limited to ORIENT=15 degrees, and the maximum ORIENT FROM that is feasible is 26 degrees.DEBRIS DISKSDefaultfalsefalsefalsefalsefalseAVAILABLESTARA0-A3 V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARA0-A3 V-IVNot sure if the GSC1 Plate reference frame continues to be necessary. This was how Fomalhaut was handled in previous Cycles. This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/CCDImagingYesNoWEDGEA2.5STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA2.5STIS/CCDImagingYesNoWEDGEA1.0Timing link suitability includes constraints ([Sequence (01 02 03 04 05) within 0.3 days])The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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