Visit 0651001 requires 10281.6 seconds but separated by less than 8640.0 seconds from Visit 0651002 0 Assigned ID: 651 ----- Attempting Submission 1 (Fri Apr 10 18:30:37 GMT 2015) ----- HST Phase I Proposal 651 (kalas_fompol.apt) successfully submitted. Receipt: # 651-1 ----- Attempting Submission 2 (Fri Apr 10 23:00:49 GMT 2015) ----- In order to request consecutive orbits (and therefore achieve optimum PSF subtraction by minimizing thermal breathing) we make the AFTER time requirement very short. Reverted the proposal back to GO/SUPPORTED mode. -972206784 ----- Attempting Submission 1 (Thu Jul 23 13:23:34 GMT 2015) ----- ----- Attempting Submission 2 (Mon Sep 21 21:46:01 GMT 2015) ----- ----- Attempting Submission 3 (Thu Sep 24 19:20:52 GMT 2015) ----- HST Phase II Proposal 14154 (14154-bias.apt) successfully submitted. Receipt: # 14154-3 ----- Attempting Submission 4 (Thu Sep 24 20:21:01 GMT 2015) ----- David Golimowski added 4 internal orbits to obtain WFC1-2K subarray bias frames for science data calibration. These orbits are charged to the Cycle 23 ACS Calibration Program as approved by HSTMO. First imaging polarization study of Fomalhaut's 140 AU dust belt As one of the nearest exoplanetary systems with multiple dust structures and a candidate extrasolar planet on a highly eccentric orbit, Fomalhaut draws significant attention from observers and theorists alike. However, there is an unresolved debate concerning the fundamental 3D geometry of the system. This strongly impacts our knowledge of grain properties, such as the size distribution, and the question of spin-orbit alignment between the star, the dust belt, and Fomalhaut b. Here we propose the first optical polarization study of Fomalhaut's 140 AU dust belt, which is made feasible by the high-contrast, diffraction-limited imaging capability of ACS/WFC. As demonstrated with another dust belt system, HR 4796A, determining the Stokes parameters is a crucial diagnostic for scattering geometry and dust grain properties. Measuring the grain optical properties through polarization will not only resolve the spin-orbit debate for Fomalhaut, it will also permit a quantitative comparison to other dusty systems, from the primitive porous aggregates that comprise AU Mic's debris disk, to the highly processed interplanetary dust particles in our own solar system. These observations will obtain wide-field, high-contrast polarimetric imaging of Fomalhaut's dust belt. Our observing technique was validated in GO-9861 (PI Kalas). The bright star Beta Pictoris was placed near the 50 pixel wide WFC chip gap, and we obtained images at three roll angles (one orbit per angle, or ORIENT). We use the roll subtraction to estimate and subtract the stellar PSF. The absence of a coronagraph means that diffraction spikes and a bright pupil ghost dominate large portions of the field. The 14154 observations require specific spacecraft ORIENTs such that the pupil ghost does not overlap with the Fomalhaut's dust belt. Due to the ORIENT and sequence constraints, the scheduling windows are very few and very brief. We find a single opportunity in 2015 on October 11-12. Visit 01 has the first ORIENT for Fomalhaut, and Visit 02 and 03 are SAME AS Visit 01. Then Visit 04 has the PSF reference star Vega. A sequence of orbits is specified so that Visits 01,02,03,04 are executed consecutively. We need consecutive orbits to achieve PSF stability that is required for successful PSF subtraction. Ideally we would also have Visits 05,06,07 in the sequence, but a sequence of 7 orbits is difficult to schedule. Therefore for scheduling flexibility, we specify that Visit 05 should occur very soon after Visit 04, but it is not part of the Visit 01-04 sequence. However, Visits 05,06,07 have their own sequence so that they are executed consecutively in three orbits with no interruptions. The default aperture for a POL observation is pixel 3096,1024 on the WFC1 chip. This is the right half of the WFC1 chip and only half is necessary because of the 35" radius vignetting with POL observations. The default is to have a 2048x2048 subarray on WFC1. However, we want to place the star on the chip gap to mitigate saturation. Therefore we DO NOT want the default aperture and subarray for POL observations. We therefore specify for every exposure in every orbit a POS-TARG of x=0 arcsec, y=-11.25 arcsec from the WFC aperture (reference pixel 2072,200 on WFC1). This appears to be an allowed configuration in the APT and this should move the targets to the middle of the chip gap. CALIBRATION ORBITS: As per STScI policy, 4 internal orbits have been added to this proposal for the purpose of obtaining subarray bias frames that are contemporaneous with the science observations. These internal orbits will be charged to STScI's Cycle 23 ACS Calibration Program, not to GO 14154. The ACS Instrument Team at STScI is responsible for producing superbias reference files from the bias frames obtained in this GO proposal. EXTRA-SOLAR PLANETS 12 false false false false SUPPORTED STAR A0-A3 V-IV CIRCUMSTELLAR MATTER EXTRA-SOLAR PLANETARY SYSTEM This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR A0-A3 V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 ACS/WFC Imaging No Yes F606W ACS/WFC Imaging No Yes F606W /Users/golim/hst/acs/wfc/subarray/Cycle23/OP-cache/14154-bias-v01.xml Timing link suitability includes constraints ([Group (01 02 03 04 05 06 07 A4) Within 14.0 days] [Sequence (01 02 03 05 06 07) within 0.4 days] [01 After 04 by at most 0.1 days]) Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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