0 Assigned ID: 46 ----- Attempting Submission 1 (Sat Mar 30 14:19:45 GMT 2019) ----- HST Phase I Proposal 46 (2019-aumicimaging-apt) successfully submitted. Receipt: # 46-1 ----- Attempting Submission 2 (Mon Apr 01 21:31:59 GMT 2019) ----- HST Phase I Proposal 46 (2019-aumicimaging-apt) successfully submitted. Receipt: # 46-2 ----- Attempting Submission 3 (Wed Apr 03 10:43:24 GMT 2019) ----- HST Phase I Proposal 46 (2019-aumicimaging-apt) successfully submitted. Receipt: # 46-3 ----- Attempting Submission 4 (Thu Apr 04 19:04:00 GMT 2019) ----- Unschedulable Visit SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR Unschedulable Visit SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR Unschedulable Visit STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS 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 Unschedulable Visit SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR SUBARRAY OFF OF DETECTOR Unschedulable Visit Unschedulable Visit Unschedulable Visit Increased schedulability 1980640122 ----- Attempting Submission 1 (Wed Jul 24 17:17:46 GMT 2019) ----- ----- Attempting Submission 2 (Thu Jun 25 15:49:41 GMT 2020) ----- ----- Attempting Submission 3 (Fri May 13 17:14:00 GMT 2022) ----- Standard coronagraphy warnings, I think. Time Domain Coronagraphy: Diagnosing the Stripping of AU Mic's Debris Disk Boccaletti+ (2015) discovered features moving within the AU Mic debris disk at super-Keplerian tangential velocities in spatially resolved imagery of the AU Mic debris disk. To date, these are the only moving structures seen in spatially resolved imagery of debris disks. The surface brightness, number, morphology, and velocities of these moving features constrains their physical location and mass, and thus are critical quantities needed to constrain the origin of this phenomenon. We propose 7 orbits of HST/STIS time per cycle, for cycles 27,28,29, to determine: a) What is the surface brightness of all features, and how does the surface brightness and morphology of features change over time?; b) What is the detailed vertical motion of features, and does the amplitude of this motion depend on stellocentric separation?; and c) What is the motion of the newly found features (NW-gamma and NW-delta) on the NW-side of the disk? These data will be used to test hypotheses that predict features are caused by the stellar wind expelling grains originating from a parent body that orbits at 8+/-2 au (Sezestre+ 2017) or by interaction between the star's wind and repeated dust avalanche events (Chiang & Fung 2017). OVERALL PROGRAM This program will obtain two sets of visits of observations of AU Mic. The first set of 4 visits utilize Wedge A0.6 and Wedge A1.0 observations. All visits during this set MUST be executed in contiguous orbits. The second set of 3 visits utilize BAR5 observations. All visits during this set MUST be executed in contiguous orbits. VISITS AND EXPOSURE DETAILS 1) WEDGE-A OBSERVATION SET Guide Star Acquisitions: We require pointing and roll control with 2-FGS guiding. Single-FGS guiding does not offer sufficient target position stability for coronagraphy. Each visit (after its Guide Star acquisition) begins with a mode-2 target acquisition, is followed by a sequence of repetitive "short" exposures (by CR-SPLIT or exposure replication) at the WedgeA0.6 position followed by a sequence of repetitive "long" exposures (also by CR-SPLIT or exposure replication) at the Wedge A1.0 position. 1) Target Acquisitions. We expose our TA images to a SNR > appx 100 using the STIS ETC. While robust target acquisition is enabled with SNR 40, we also use the TA images as a pre mode-2 astrometric anchor to assess the "behind the wedge" target position to high precision (separate from "diffraction spike" analysis, for which higher SNR for precision centroiding is required. We also use these F25ND3 filtered imagesto photometrically obtain target:PSF template brightness ratios in the broad STIS passband. The STIS Target Acquisition ETC was used to determine the eposure times for all acquisition images. 2) The "short" exposure times are designed to reach 90% of full-well depth, with the target coronagraphically occulted, at the edge of the wedge 0.3" from the star. We scale, using the ETC, this from observations predicated upon an A0 star with V = 3.55 reach 90% full well from the PSF halo in 1 second based upon preious STIS coronagraphic observations allowing for up to as much of 1/2 pixel of possible target decentering in acquisition performance. We generally repeat these exposures to fill appx 35% of the target visibility interval after subtracting the time required for the preceding guide star and target acquisitions. 3) Following the short exposures we execute a Type-2 slew (by a change in instrument aperture to Wedge1.0) for the "long" exposure imaging. Sub-Array Readouts. For most coronagraphic exposures we use subarray readouts (SIZEAXIS2) symmetrically centered on the target to fully read-out the region along the wedge (Axis2, image Y axis) to the edge of the FOV at the small end of the wedge taper, and symmetrically on the diametrically opposing side. For WedgeA1.0 the max SIZEAXIS2 (without displacing with an |unsupported| CENTERAXIS2) is 427 pixels. This implies that the A1.0 position is 10.82 from the edge of the FOV (whole sub-array centered on target symmetrically 21.65 along the wedge). For WedgeA0.6 is (without displacing with an |unsupported| CENTERAXIS2) is 137 pixels. This implies that the A0.6 position is 3.47 from the edge of the FOV (whole sub-array centered on target symmetrically 6.95 along the wedge). VISIT LINKAGES (RELATIVE ORIENTATION CONSTRAINTS AND INTERLEAVED PSF OBSERVATIONS) ============================================================ We place an absolute orient request on VISIT 2 that constrain the AU Mic disk to align perpendicular to the long axis of occulting Wedge A. We place relative orient constraints on VISIT 1 (-30 to -20 degrees from VISIT 2) and on VISIT4 (20 to 30 degrees from VISIT 2). No relative orient constraints are placed on VISIT 3, where the PSF star is observed. We require all 4 visits within this observation group be executed in contiguous orbits. 2) BAR5 OBSERVATION SET Guide Star Acquisitions: We require pointing and roll control with 2-FGS guiding. Single-FGS guiding does not offer sufficient target position stability for coronagraphy. Each visit (after its Guide Star acquisition) begins with a mode-2 target acquisition, is followed by a sequence of repetitive "short" exposures (by CR-SPLIT or exposure replication) at the nominal BAR5 position. To mitigate against target centering uncertainties behind BAR5, we also include one sequence of repetitive exposures with the target offset by 0.25 pixels ABOVE the nominal center of BAR5 and one sequence of repetitive exposures with the target offset by 0.25 pixels BELOW the nominal center of BAR5 (i.e. an effective dither about the center position of BAR5). We achieve this dither pattern by using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = + 0.0024921 arcsec and y = + 0.0122491 for the PLUSDITHER position, and x = - 0.0024921 arcsec and y = - 0.0122491 for the MINUSDITHER position). 1) Target Acquisitions. We expose our TA images to a SNR > appx 100 using the STIS ETC. While robust target acquisition is enabled with SNR 40, we also use the TA images as a pre mode-2 astrometric anchor to assess the "behind the wedge" target position to high precision (separate from "diffraction spike" analysis, for which higher SNR for precision centroiding is required. We also use these F25ND3 filtered imagesto photometrically obtain target:PSF template brightness ratios in the broad STIS passband. The STIS Target Acquisition ETC was used to determine the eposure times for all acquisition images. VISIT LINKAGES (RELATIVE ORIENTATION CONSTRAINTS AND INTERLEAVED PSF OBSERVATIONS) ============================================================ We place an absolute orient request on VISIT 6 that constrains the AU Mic disk to align perpendicular to the long axis of occulting BAR5. We place relative orient constraints on VISIT 5 (-6.5 to -6.5 degrees from VISIT 6) and on VISIT 7 (6.5 to 6.5 degrees from VISIT 6). We require all 3 visits within this observational be executed in contiguous orbits. -------- Realtime Justification -------- We have no real-time requirments. ------ Calibration Justification ------- We ask for no SPECIAL calibrations for this proposal (and called none out in Phase 1). We did not because we ASSUME that STScI will acquire GAIN=4 (supported mode) bias, DARK, and flat-field frames (and derived hot/bad pixel maps) as part of their Cycle 28 calibration plan in support of approved Cycle 28 science programs. If this is NOT the case then we must obtain GAIN=4 calibration reference bias/dark data as part of our program using NON-POINTED (internal) orbits only. If STScI does not include acquiring for broader purposes the reference data we need, then we will need to add those internal calibrations to this program AFTER the Phase 2 deadline. PI John Wisniewski has 10+ years of expertise in high contrast imaging of protoplanetary and debris disks using ground-based and HST instrumentation (including coronagraphs on STIS, ACS, and NICMOS). Wisniewski is PI of GO-15219, which is the immediate precursor project of our proposed program. Co-I Glenn Schneider is a leading expert in HST high-contrast coronagraphy: observational methodology, data reduction & PSF subtraction techniques, image post-processing and enhancement, interpretation and modeling as applied to exoplanetray systems (EDS) science inclusive of protoplanetray, transition and debris disks. For more than two decades he has led (PI'ed) or actively engaged in numerous highly successful HST GO, GTO, AR and CAL programs particular germane to this proposal. He has authored or coauthored over 86 papers in the refereed literature on HST coronagraphy and dusty circumstellar planet-forming/hosting environments. Co-I Carol Grady is an expert in the reduction and analysis of STIS coronagraphic imagery and with high-contrast imaging in the NIR from the ground as part of the SEEDS and post-SEEDS teams. Co-I Anthony Boccaletti is leading high contrast imaging of AU Mic from the ground using VLT/SPHERE, and is the lead author of the studies reporting the discovery and follow-up of outward moving features in its disk (Boccaletti+ 2015; Boccaletti+ 2018). Co-Is John Debes and Dean Hines have long-term expertise in reducing and analyzing coronagraphic imagery of debris disks from HST's STIS and NICMOS instruments. Co-I Chris Stark is a theorist with broad interest and expertise in the early evolution of planetary systems (including our own), and debris disks. Co-Is Jean-Charles Augereau, Thomas Henning, and Elie Sezestre are key members of the VLT/SPHERE team that have been tracing the morphological evolution of the AU Mic's spatially resolved disk. They all have substantial observational and theoretical expertise in analyzing and interpreting spatially resolved imagery of debris disks. Planets and Planet Formation 6 false false false false false false false AVAILABLE STAR CIRCUMSTELLAR MATTER M V-IV Coordinates are from GSC2.3.2. J2000 J2000 STAR M V-IV Coordinates from GSC2.3.2. J2000 J2000 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No WEDGEA0.6 STIS/CCD Imaging Yes No WEDGEA1.0 Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit5758497743454206487.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (1-4) uses WedgeA. These visits (1-4) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from -30 deg to -20 degrees from Visit 2, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to -30 degrees from the preferred absolute orient of 83.7 degrees in Visit 2. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 2 deviates from 83.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 1. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 1, 2, or 4. 1602377504000 53.69999999999999 (Tic-Visit :proposal-id 16205 :visit-id "01" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:23.0" :trans-errors '(:WARNINGS 13 :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 47360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. For long exposures at WedgeA1.0 go > 10x deeper in each that will fit into remainer ofvisibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. This setup for the "long" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. 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 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit2616929700696309655.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (1-4) uses WedgeA. These visits (1-4) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable absolute orientation to range from 73.7 deg to 93.7 degrees, to allow a sufficiently large scheduling window. NOTE TO PC: AU Mic's disk has a PA of 128.7 degrees. Our science is optimized if we can achieve an absolute orient that places the major axis of AU Mic's disk perpendicular to the long axis of WEDGEA. We need our absolute orient to be as close as possible to (128.7 degrees + 315 degrees = 83.7 degrees; or equivalently ok 128.7 degrees + 135 degrees = 263.7 degrees). We ask that you please try to identify scheduling windows that enable us to get as close as possible to either of these absolute orientations. These orientiations place the circumstellar disk axis perpendicular to the long-axis of WEDGEA. We have allowed a +/-10 degree window about this strong preference to aid scheduled and GS acquisition. Relative Timing: This visit (2) MUST immediately follow Visit 1 and immediately preceed Visit 3 in back-to-back orbits. 1602383223000 73.0 (Tic-Visit :proposal-id 16205 :visit-id "02" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:25.0" :trans-errors '(:WARNINGS 13 :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 47360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. For long exposures at WedgeA1.0 go > 10x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. This setup for the "long" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([03 After 02 by 0.0 to 0.1 days] [04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit15859039178492022456.xml PSF (HD191849). PSF calibration target for AU MIC. V = 7.97. B-V = +1.46. This set of visits (1-4) uses WedgeA. These visits (1-4) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: NOTE TO OUR PC: Our PSF star visit (#3) has no absolute or relative orientation constraints. However, all other things being equal, when scheduled, we would request that both be observed with roll angles as close to Visit 2 as possible. This is not a hard requirement and we do not constrain, but a request this if possible to optimize the science return through likely better PSF calibration. Relative Timing: This visit (3) MUST immediately follow visit 2 and immediately precede visit 4. I.e., They should be executed sequentially in "back-to-back" orbits. 1602388592000 73.0 (Tic-Visit :proposal-id 16205 :visit-id "03" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:26.0" :trans-errors '(:WARNINGS 16 :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 54656 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2852 :al-overhead-at-end 0 :internal-dur-at-end 359 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) true 1 0 SNR = 100, V = 7.97, sp = M0Ve, Exptime rounded to nearest 0.1 second SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. V = 7.97 so saturation in 34.0s. So 90% full well in appx 30.6s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. V = 7.97 so saturation in 34.0s. So 90% full well in appx 30.6s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. V = 6.26 so saturation in 12.1s. So 90% full well in appx 10.9s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. For long exposures at WedgeA1.0 go <=20x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. This setup for the "long" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit5254828326996166373.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (1-4) uses WedgeA. These visits (1-4) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from 20 deg to 30 degrees from Visit 2, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to +30 degrees from the preferred absolute orient of 83.7 degrees in Visit 2. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 2 deviates from 83.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 4. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 1, 2, or 4. Relative Timing: This visit (4) MUST immediately follow Visit 3. I.e., They should be executed sequentially in "back-to-back" orbits. 1602394661000 92.30000000000001 (Tic-Visit :proposal-id 16205 :visit-id "04" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:28.0" :trans-errors '(:WARNINGS 13 :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 47360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated (8x) with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. Use this for the "short" exposures, repeated with multiple CR Splits. This setup for the "short" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "short" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 137, appropriate for the WedgeA0.6 position. SCALABLE BENCHMARK: We expect full-well at r=0.3" from wings of stellar PSF in 1 second for V=3.55. AU MIC is V = 8.61 so saturation in 50.6s. So 90% full well in appx 45.5s. For long exposures at WedgeA1.0 go > 10x deeper in each that will fit into remainer of visibility period CR-SPLIT at least 3 times - and trim exposure time to fit in visibility window. This setup for the "long" exposures replicates the setup used for GO-12228 for this target and WEDGE observations. SCALABLE PARAMETER FOR SUB-ARRAY Readout: SIZEAXIS2 = 20 is 1" in full extent (r = 0.5") For these "long" exposures we will image perpendicular to the wedge (symmetrically) centered on the target to the maximum extent permitted by the limits of the FOV (edge of the detector) on the "small" side of the Wedge A taper. Thus, for these short exposures we use SIZEAXIS12 = 427, appropriate for the WedgeA1.0 position. Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit10181477772473521957.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from -6.5 deg to -6.5 degrees from Visit 6, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to -6.5 degrees from the preferred absolute orient of 353.7 degrees in Visit 6. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 6 deviates from 353.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 5. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 5,6, or 7. 1629022998000 9.5 (Tic-Visit :proposal-id 16205 :visit-id "05" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:30.0" :trans-errors '(:WARNINGS 0 :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 214256 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "05" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2706 :al-overhead-at-end 0 :internal-dur-at-end 377 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days] [07 After 06 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit15853675312211461464.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable absolute orientation to range from 343.7 deg to 15.7 degrees, to allow a sufficiently large scheduling window. NOTE TO PC: AU Mic's disk has a PA of 128.7 degrees. Our science is optimized if we can achieve an absolute orient that places the major axis of AU Mic's disk perpendicular to the long axis of BAR5. We need our absolute orient to be as close as possible to (128.7 degrees + 45 degrees = 173.7 degrees; or equivalently ok 128.7 degrees + 225 degrees = 353.7 degrees). We ask that you please try to identify scheduling windows that enable us to get as close as possible to either of these absolute orientations. These orientiations place the circumstellar disk axis perpendicular to the long-axis of BAR5, while allowing schedulability and avoiding the disk falling along diffraction spikes. We have allowed a +25 and -25 degree window about this strong preference to aid scheduled and GS acquisition. Relative Timing: This visit (6) MUST immediately follow Visit 5 and immediately preceed Visit 7 in back-to-back orbits. 1629028715000 16.0 (Tic-Visit :proposal-id 16205 :visit-id "06" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:34.0" :trans-errors '(:WARNINGS 0 :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 214256 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2706 :al-overhead-at-end 0 :internal-dur-at-end 377 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. Timing link suitability includes constraints ([07 After 06 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit11615303182376817434.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from +6.5 deg to +6.5 degrees from Visit 6, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to +6.5 degrees from the preferred absolute orient of 353.7 degrees in Visit 6. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 6 deviates from 353.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 7. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 5,6, or 7. Relative Timing: This visit (7) MUST immediately follow Visit 6. I.e., They should be executed sequentially in "back-to-back" orbits. 1629034433000 22.5 (Tic-Visit :proposal-id 16205 :visit-id "07" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 11:55:38.0" :trans-errors '(:WARNINGS 0 :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 214256 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2706 :al-overhead-at-end 0 :internal-dur-at-end 377 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. Timing link suitability includes constraints ([56 After 55 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit11891107763988162756.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from -6.5 deg to -6.5 degrees from Visit 6, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to -6.5 degrees from the preferred absolute orient of 353.7 degrees in Visit 6. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 6 deviates from 353.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 5. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 5,6, or 7. (Tic-Visit :proposal-id 16205 :visit-id "55" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 12:02:56.0" :trans-errors '(:WARNINGS 0 :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 189088 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "55" :obset-id "55" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "55" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2424 :al-overhead-at-end 0 :internal-dur-at-end 368 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. Timing link suitability includes constraints ([56 After 55 by 0.0 to 0.1 days] [57 After 56 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit535687145512857590.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable absolute orientation to range from 343.7 deg to 15.7 degrees, to allow a sufficiently large scheduling window. NOTE TO PC: AU Mic's disk has a PA of 128.7 degrees. Our science is optimized if we can achieve an absolute orient that places the major axis of AU Mic's disk perpendicular to the long axis of BAR5. We need our absolute orient to be as close as possible to (128.7 degrees + 45 degrees = 173.7 degrees; or equivalently ok 128.7 degrees + 225 degrees = 353.7 degrees). We ask that you please try to identify scheduling windows that enable us to get as close as possible to either of these absolute orientations. These orientiations place the circumstellar disk axis perpendicular to the long-axis of BAR5, while allowing schedulability and avoiding the disk falling along diffraction spikes. We have allowed a +25 and -25 degree window about this strong preference to aid scheduled and GS acquisition. Relative Timing: This visit (6) MUST immediately follow Visit 5 and immediately preceed Visit 7 in back-to-back orbits. (Tic-Visit :proposal-id 16205 :visit-id "56" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 12:13:05.0" :trans-errors '(:WARNINGS 0 :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 189088 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "56" :obset-id "56" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "56" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2424 :al-overhead-at-end 0 :internal-dur-at-end 368 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. Timing link suitability includes constraints ([57 After 56 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/48/gyq3l4d578d1z_kzqh9zdgrw0000gq/T/OPVisit7903549774308815990.xml AU MIC (V=8.61, B-V = + 1.45). This set of visits (5-7) uses BAR5. These visits (5-7) MUST be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We have set the allowable orientation to range from +6.5 deg to +6.5 degrees from Visit 6, to allow a sufficiently large scheduling window. NOTE TO PC: Our science is optimized if we can achieve an orient as close as possible to +6.5 degrees from the preferred absolute orient of 353.7 degrees in Visit 6. We ask that you please try to identify scheduling windows that enable us to get as close as possible to this orientation. IF the absolute orient of Visit 6 deviates from 353.7 degrees, PLEASE ask us for guidance as to the orientation range we prefer for Visit 7. We absolutely do NOT want the disk major axis (128.7 degrees) to align with the STIS diffration spikes in Visits 5,6, or 7. Relative Timing: This visit (7) MUST immediately follow Visit 6. I.e., They should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 16205 :visit-id "57" :proposal-version -1 :trans-version "20211222" :date "13-May-2022 12:03:01.0" :trans-errors '(:WARNINGS 0 :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 189088 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16205 :visit-id "57" :obset-id "57" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16205 :visit-id "57" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2424 :al-overhead-at-end 0 :internal-dur-at-end 368 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3180 :pcs-gap 0 ) true 1 0 SNR = 100, V = 8.61, sp = M1Ve, Exptime rounded to nearest 0.1 second NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures. NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture), and attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = -0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 237 to yield a 6" round FOV. SCALABLE BENCHMARK: We scale our exposure times from GO-12923. We expect that 16.7 seconds per exposure will yield 75% to saturation in the brightest pixel. Our exposures are thus comprised of CR-SPLITS in integral units of 16.7 second exposures.