0 Assigned ID: 520 ----- Attempting Submission 1 (Fri Mar 06 16:07:49 GMT 2020) ----- SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR 0 ----- Attempting Submission 1 (Fri Jun 26 22:20:16 GMT 2020) ----- The SUBARRAY OFF OF DETECTOR warnings are due to the centering on the wedge and combined roll angle subtraction strategy. These warnings should not affect our proposed scientific objectives. Debris disks are readily detectable tracers of embedded planetary systems; however, their complex internal structures are often challenging to interpret as most debris disks do not harbor known exoplanets. The prototypical debris disk around Beta Pic and its two relatively short-period super-Jupiter planets offer a unique laboratory for studying planet-disk interactions. Five mechanisms have been identified through models in which Beta Pic b may shape the complex disk structure and may perturb planetesimals into an inclined orbit, giving rise to the secondary disk discovered with HST. Structures shaped by the planet's resonances can introduce large-scale azimuthal asymmetries in the disk that orbit on timescales similar to that of the planet (~18 yr). With STIS images from 1997 and 2012 a uniquely long baseline is available for identifying the temporal evolution of the disk, which is predicted to evolve on comparable Keplerian timescales. We propose to revisit and continue monitoring the Beta Pic disk with STIS to characterize the temporal evolution of the disk. By repeating the earlier observations we will detect variations as small as 1% at 0.5". In comparison, models of radiation-pressure driven small grains freed from planetesimals trapped in resonance with the planet predict variations up 300% in this component. We will identify disk structures and dust grain populations that are a result of interactons with the two giant planets, directly testing models explaining the disks' complex structure. These observations will provide an entirely new set of constraints on the 3D structure and dynamics of the only known disk/planet system where such measurements are possible. The proposed observations aim to obtain a STIS coronagraphic image of the Beta Pictoris debris disk with two goals: The primary goal is to compare the disk surface brightness distribution to 1997 and 2012 STIS observations of the same disk, to identify or constrain changes in the disk structure. The secondary goal is to image the disk at a smaller inner working angle (stellocentric angular distance 0.3") than imaged before to explore the inner disk structure. The surface brightness variations and inner disk structure is particularly interesting in this system, where a giant planet has been directly imaged. The planet's projected separation in 2021-2022 is about 0.35-0.43" from the star. The 1997 data was obtained with STIS using positions along both WedgeA and WedgeB. We will observe the target star and a PSF star at four positions and different orientations. This data set will allow PSF subtraction both through roll (self)subtraction and through PSF subtraction, thus allowing two alternate reduction methods. The combination of the data sets will provide an optimal spatial coverage and can correct for the field lost due to wedge obscuration and diffraction spike contamination. Based on the comparison of the reduced 1997 and 2012 data and a set of PSF stars from other programs we identified that the following strategy provides the best quality data and best comparison to the earlier data sets: We will observe the two targets using three single-orbit visits (01, 02, 03) that are linked both in time and orientation angles. The three visits must be scheduled "back-to-back" in sequential visibility periods, each uninterrupted by Earth occultation -- hence the AFTER scheduling requirements of 0.5 to 1.5 orbit (start-to-start) times on Visits 02 and 03. In Visit 01 we observe our science target (Beta Pic). In Visit 02 we will observe our PSF calibration target (Alpha Pic). The Alpha Pic visit (02) MUST be scheduled in time in between Visits 01 and 03. In Visit 03 we again observe Beta Pic, but at an orientation angle differing by +33.5 deg from the absolute orientation specified for Visit 01. We begin each Visit with an on-board autonomous coronagraphic target acquisition. Target acquisition exposure times were chosen to provide SNR ~ 100 in the central pixel of the target acq images. In all cases we use the F25ND5 filter due to the brightness of our target stars. First orbit: We will observe Beta Pic at four wedge-occulted locations: WedgeA06, WedgeA1.0, WedgeB1.0, and a position POSTARGETED (by -7.4", 0.0") to a narrow position on the mid-line of WedgeB. (This latter position is symmetrically equivalent to the WedgeA0.6 aperture position, but no such aperture is currently defined, therefore we POSTARG from a standard aperture position on WedgeB.) We will obtain a series of short exposures for the 0.6" wedge locations to avoid the saturation close to the wedge. We obtain a combination of short and long exposures at the 1.0" locations to probe the disk close to the wedge and also at large separations. Absolute Orientation: 59.05 degree Second Orbit: Carry out the same observing sequence as in Orbit 1 on the PSF star Alpha Pictoris. This star is slightly brighter, so exposures are shorter to avoid saturation. In this visit we observe our PSF template calibration star. In order to minimize variations in PSF structure from thermal driven changes in OTA wavefront errors, we constrain the orientation of this calibration target which is nearby in the sky to our science target (similar spacecraft attitude and sun angle) to be in between the orientations of Visit 01 and 03. NOTE TO OUR PC: Ideally, we would like this Visit scheduled with an Orientation of 75.8 deg if possible, but any orientation within the specified range is acceptable. Third Orbit: Repeat the observations of Beta Pic (1st orbit) but at a different spacecraft orientation. Orientation: Visit 1 +33.5 degree. EXPOSURE TIMES: Individual coronagraphic exposure times (Ex. Time / # CR Splits) have been carefully chosen at all wedge positions based upon prior coronagraphic imaging so as not to saturate at the smallest IWA for each wedge position while also providing > appx 70% full well depth. NOTE TO OUR PC: Please do *NOT* allow "automatic" adjustment of any exposure times in our coronagraphic exposures to fill any (small) "dead time" in the orbits WEDGE B POSITION: At the end of each visibiliy period we image along the B wedge using a POSTARG offset from Wedge1.0B. In doing so we do NOT specify an "available" engineering mode parameter CENTERAXIS2 (though we use "supported" mode SIZEAXIS2 sub-array readout specifications here and elsewhere) on these POSTARGED exposures on the recommendation of our CS. We REQUEST that when an SMS (or precursor input product) is generated, this be verified that the subarray for this position is indeed centeed on the target in the Y axis direction. ORIENTATIONS: The observations are sensitive to the roll angles: the right angles will ensure that the disk is optimally placed between the wedges and the diffraction spikes at both orientations and minimize the spatial coverage lost due to obscuration. DISK AND SPACECRAFT ORIENTATIONS: The "northern" semi-major axis of the nearly-edge on Beta Pic disk is at a celestial position angle of appx 30.8 deg. (The inner disk itself is warped and PAs varying by a few degrees appear in the literature, depending upon how and at what distances measures have been made. For our observation planning we adopt 30.8 deg). In Visit 01 we select an absolute ORIENTATION angle of 59.05 deg to rotate the disk 16.75 deg counter-clockwise with respect to the mid-line of the A-wedge. In Visit 03 we specify a +33.5 deg ORIENT FROM w.r.t. the absolute orientation of 59.05 deg (corresponding to an absolute orientation of 92.55 deg). NOTE TO OUR PC: Our goal here is to simultaneously: (a) have the +/- roll offsets w.r.t nominal U3, so that in Visit 01 and 03 the disk major axis is equally rotated in opposite directions with symmetric displacements w.r.t. the mid-line of the A wedge, while ALSO (b) providing the largest roll difference (+33.5 deg informed by the roll range report) for which the mid-range of the absolute orientations of Visits 01 and 03 would align the disk major axis with the mid-line of the A-wedge (conceptually, at 75.8 deg). This is key to optimizing the science return for this program. If a suitable GS pair cannot be found to enable this geometry, we would later suggest possible specific alternates depending upon schedualbility with more restrictive differential roll ranges with trades in science return. EXTRA SHORT EXPOSURES AT THE END OF VISIT 02: Based on our experience we expect the IWA to be determined by the slight positional difference between the PSF star and the target star. Our PSF star is brighter than the target star, thus requiring somewhat shorter exposures, leaving an extra 2.5 minutes at the end of Visit 02. We plan to use this time to obtain short exposures of the PSF at two additional positions along the Y axis - the combination of the three (total) positions will allow us to find the best positional match for the target star which should help providing a better PSF subtraction than possible with regular pointing technique. This will potentially further enhance the data and only uses some of the remaining visibility. If really necessary, these exposures (02.012-02.013) can be removed. The three orbits must be executed back-to-back to minimize the changes in the instrumental PSF and the spacecraft/instrument state. Our team includes expertise in high-contrast disk and exoplanet observations, as well as leading theorists specializing in disk models. Members of our team proposed for, reduced, analyzed, and published the most recent epoch of STIS imaging on the proposed target, which we propose here to repeat. Prof. Daniel Apai is an expert on studies of extrasolar planets and planet-forming environments. Apai led eight HST proposals as PI and has published a comprehensive paper on HST/STIS observatoins of the Beta Pictoris system, the target of this proposal. Dr. Glenn Schneider is an expert in HST high-contrast imaging and coronagraphy: observational methodology, data reduction and PSF subtraction techniques, image post-processing and enhancement, and interpretation and modeling as applied to protoplanetary, transition and debris disks. For more than two decades he has led (PIed) or actively engaged in numerous highly successful HST/GO, GTO, AR and CAL programs (https://tinyurl.com/GSCHNEIDER-HST-PROPS) particularly germane to this debris disk (DD) investigation. He has authored or coauthored over 90 papers in the refereed literature on HST coronagraphy, dusty circumstellar disks, and planet-forming/hosting environments (https://tinyurl.com/GSCHNEIDER-PUBS). Dr. Christopher Stark is an Associate Scientist at STScI and has experience observing debris disks, analyzing high contrast imaging data sets, studying disk composition and dust grain optical properties, and modeling disk-planet dynamical interactions. Mr. Kevin Wagner is a PhD candidate at The University of Arizona (anticipated defense in 2020). Mr. Wagner's research focuses on studying exoplanets and planet formation through high-contrast imaging and spectroscopy. Mr. Wagner has experience planning, reducing, and analyzing high-contrast imaging data (e.g., Wagner et al. 2018, ApJL, 863, L8), and in interpreting planet-disk interactions (e.g., Wagner et al. 2019, ApJ, 882, 20) and disk variability (e.g., Wagner et al. 2015, ApJ, 798, 94). Prof. Mark Wyatt is an expert in debris disk modelling and variability studies. Professor Wyatt has contributed to numberous successful HST programs, including past studies of the Beta Pictoris, and has developed specifically tuned models to that system. Exoplanets and Exoplanet Formation 6 false false false false false false 0.0 0.0 false SUPPORTED STAR A4-A9 V-IV Beta Pictoris, debris disk: semi-major axis P.A.: +30.8 degree (E of N) A6V J2000 J2000 B=4.03 CALIBRATION POINT SPREAD FUNCTION PSF calibrator for Beta Pictoris HD50241 J2000 J2000 B=3.48 STIS/CCD Imaging Yes No WEDGEB1.0 STIS/CCD Imaging Yes No WEDGEB1.0 STIS/CCD Imaging Yes No WEDGEB1.0 Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1593025101190 Timing: Must be executed in sequential orbit immediately prior to Visit 02 with only intervening inter-visit Earth occultation. Orientation: Absolute Orientation 59.05 degrees only. (Tic-Visit :proposal-id 16174 :visit-id "01" :proposal-version -1 :trans-version "20200518" :date "24-Jun-2020 11:58:19.0" :trans-errors '(:WARNINGS 8 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 343296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16174 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16174 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2927 :al-overhead-at-end 0 :internal-dur-at-end 324 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) false 1 0 Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days] [03 After 02 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1593022885624 Timing: Must be executed in sequential orbit immediately after Visit 01 with only intervening inter-visit Earth occultation. Orientation: Absolute Orientation between 65.8 and 85.8 degrees; optimal absolute orientation: 75.8 (Tic-Visit :proposal-id 16174 :visit-id "02" :proposal-version -1 :trans-version "20200518" :date "24-Jun-2020 11:21:24.0" :trans-errors '(:WARNINGS 11 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 370112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16174 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16174 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3024 :al-overhead-at-end 0 :internal-dur-at-end 345 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) false 1 0 Timing link suitability includes constraints ([03 After 02 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1593025104516 Timing: Must be executed in sequential orbit immediately after Visit 03 with only intervening inter-visit Earth occultation. Orientation: Relative Orientation 33.5 degrees from Visit 1 orientation. (Tic-Visit :proposal-id 16174 :visit-id "03" :proposal-version -1 :trans-version "20200518" :date "24-Jun-2020 11:58:23.0" :trans-errors '(:WARNINGS 9 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 343296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16174 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16174 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2927 :al-overhead-at-end 0 :internal-dur-at-end 321 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) false 1 0