0 Assigned ID: 4582 ----- Attempting Submission 1 (Wed May 24 20:16:35 GMT 2023) ----- Could not find ephemeris for target 17417-01-QUAOAR Could not find ephemeris for target 17417-02-QUAOAR Resubmission of the Program 17417 Phase II proposal. Removed the patterns for each visit from the Noninterruptable sequence containers. Edit 10/31/23: Placing all exposures into Non-interruptable sequences, as per recommendation by L. Dressel. Edit 03/14/24: Expanded BETWEENs for Visit 1 and 2 to accomodate scheduling needs, as per request by A. Armstrong. I've also performed a bright object check and modified BETWEENs to prevent imaging of target while near bright stars. Edit 03/28/24: Relaxed timing constraints for Visits 3, 4, and 5, as per request by A. Armstrong. BETWEENs now avoid bright field stars to optimize image quality. Edit 08/15/24: Reworked timing constraints for Visits 3-5 with new constraints placed by RGM. Science constraints are shown by the phase requirements. BETWEENs are purely for avoiding bright background stars that could diminish image quality. -957711386 ----- Attempting Submission 1 (Tue Sep 12 21:39:18 GMT 2023) ----- ----- Attempting Submission 2 (Thu Sep 14 17:48:13 GMT 2023) ----- ----- Attempting Submission 3 (Tue Oct 31 22:28:26 GMT 2023) ----- ----- Attempting Submission 4 (Thu Mar 14 20:10:12 GMT 2024) ----- ----- Attempting Submission 5 (Thu Mar 28 14:39:56 GMT 2024) ----- ----- Attempting Submission 6 (Thu Aug 15 21:51:44 GMT 2024) ----- Visit planner won't update for Visits 1 and 2. Both are already executed, so not important. Exploring the Dynamics of Quaoar's Rings Recent stellar occultations have revealed a pair of enigmatic rings around the dwarf planet Quaoar. These narrow rings, which lie well outside Quaoar's Roche limit are extremely interesting targets for study into ring formation, evolution, and ring particle interactions. Quaoar and its moon Weywot, are, unfortunately, not well enough characterized to study the dynamics of the newly discovered ring system. In this 5 orbit program, we propose to study the orbit of Weywot to constrain the dynamics of Quaoar's rings. By using state-of-the-art non-Keplerian orbit fitting techniques, the additional astrometric observations obtained in this program will strongly constrain Weywot's orbit and orbital precession, as well as Quaoar's mass and shape. This will enable further study of Quaoar's rings, allowing the system to act as a touchstone for future studies of rings around TNOs. Our proposal uses a novel observing strategy to ensure the most efficient use of HST time, while still allowing us to accomplish our goals. Our observations call for 5 single-orbit visits to image the Quaoar-Weywot binary system using the WFC3/UVIS instrument. During each visit, images will be acquired using the UVIS2-C512C-SUB aperture, paired with the F350LP filter to optimize astrometric precision. Exposure times are chosen to optimize SNR and schedulability, with 8 dithered images taken during each visit. This allows us to remain robust to unlucky cosmic ray hits. Each visit has been scheduled to best achieve the goals of our program. We request that Visit 01 is scheduled as soon as possible in the cycle, at times which best optimize target visibility. Visit 02 should take place ~90 days later, again at times of maximum visibility. Lastly, we request Visits 03-05 are scheduled as late as possible in the cycle. These should be taken in a sequence with 2-4 days between each visit. While these scheduling constraints are quite stringent, this observing cadence allows us to optimize our use of precious HST time. If the scheduling requirements are too onerous, we are happy to work with schedulers to relax these requirements as needed. Once each visit has a planned window/schedule, we will be able to check whether any bright objects are too close to our target, as we have done in previous programs. Reduced gyro operations will not significantly affect the execution of this program, apart from potentially requiring a rescheduling of observations due to reductions in observing windows. As needed, we can flexibly reschedule observations without significantly harming the goals of this program. Reduced spatial scan speed will not prohibit observations of our target as the maximum needed spatial scan speed is ~5 arcseconds/hour, well within the limits of reduced gyro operations. PI Proudfoot is a graduate student that has expertise in all areas of this proposal. He is an expert in non-Keplerian orbit fitting and HST image analysis. He is one of the main developers of MultiMoon, the non-Keplerian orbit fitting tool that forms much of the core of this proposal. He is also the developer of the PSF fitting tools that will be extensively used for this project. In addition, he is an expert in Bayesian parameter inference and orbital dynamics of TNO moons. Co-I Ragozzine is PI Proudfoot's graduate faculty advisor. He is also an expert in TNO moon orbit fitting, with extensive experience in detecting non-Keplerian effects caused by massive moons (like those of Haumea). He has been PI of multiple HST programs focusing on understanding the formation, evolution, and physical characteristics of TNOs. Co-I Grundy is a major expert in HST data reduction and analysis for TNO binaries. He has led several programs focusing on characterization of individual TNB systems. He maintains an extensive online catalog of TNO binaries. Co-I Spencer is an graduate student member of Co-I Ragozzine's group and is also a developer of MultiMoon. Solar System Astronomy 6 false false false false false false false false SUPPORTED SOLAR SYSTEM DWARF-PLANET The dwarf planet Quaoar TYPE=ASTEROID,A=43.35621062592979,E=0.03993647193741599,I=7.9912917217563 ,O=189.0992394650243,W=158.6070723684032,M=293.8106399929501,EQUINOX=J2000,EPOCH=25-MAY-2023:00:00:00,EpochTimeScale=TDB EARTH WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F350LP WFC3/UVIS Imaging No No F350LP POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false The first visit to image Quaoar. This visit will act as an anchor to ensure all subsequent visits are as constraining as possible. In this visit, observation timing is optimized to ensure the highest chance of detection. This should be scheduled as early in the Cycle as possible. 1716314435000 256.07903976387036 (Tic-Visit :proposal-id 17417 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "11-Jun-2024 12:23:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 36624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17417 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17417 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :al-overhead-at-end 0 :internal-dur-at-end 77 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0 The second visit to image Quaoar. This should take place about 30 days after Visit 1. This observation allows for maximum separation of possible period aliases. 1719067763000 220.94774307756887 (Tic-Visit :proposal-id 17417 :visit-id "02" :proposal-version -1 :trans-version "20240604" :date "11-Jun-2024 12:23:51.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 36624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17417 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17417 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2622 :al-overhead-at-end 0 :internal-dur-at-end 77 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0 Using ephemeris for target 17417-03-QUAOAR ephemeris data for target 17417-03-QUAOAR does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 24.112 to 25.213. ephemeris interval: 24.213 to 26.213 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/tm/bvd5g5k95vq10v9nl69qpjj80000gn/T/OPVisit5684431381872138856.xml The third visit to image Quaoar. Taken at particular orbital phase. Betweens represent times when nearby bright objects are too close to Quaoar for good imaging. (Tic-Visit :proposal-id 17417 :visit-id "03" :proposal-version -1 :trans-version "20240604" :date "15-Aug-2024 16:20:29.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 36624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17417 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 17417 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17417 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2478 :al-overhead-at-end 0 :internal-dur-at-end 77 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0 Using ephemeris for target 17417-04-QUAOAR ephemeris data for target 17417-04-QUAOAR does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 24.112 to 25.213. ephemeris interval: 24.213 to 26.213 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/tm/bvd5g5k95vq10v9nl69qpjj80000gn/T/OPVisit10984648127728549476.xml The fourth visit to image Quaoar. Taken at particular orbital phase. Betweens represent times when nearby bright objects are too close to Quaoar for good imaging. (Tic-Visit :proposal-id 17417 :visit-id "04" :proposal-version -1 :trans-version "20240604" :date "15-Aug-2024 17:43:02.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 36624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17417 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 17417 :visit-id "04" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17417 :visit-id "04" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2478 :al-overhead-at-end 0 :internal-dur-at-end 77 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0 Using ephemeris for target 17417-05-QUAOAR ephemeris data for target 17417-05-QUAOAR does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 24.112 to 25.213. ephemeris interval: 24.213 to 26.213 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. /private/var/folders/tm/bvd5g5k95vq10v9nl69qpjj80000gn/T/OPVisit11938230844304740269.xml The fifth visit to image Quaoar. Taken at particular orbital phase. Betweens represent times when nearby bright objects are too close to Quaoar for good imaging. (Tic-Visit :proposal-id 17417 :visit-id "05" :proposal-version -1 :trans-version "20240604" :date "15-Aug-2024 17:43:04.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 36624 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17417 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 17417 :visit-id "05" :obset-id "A5" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17417 :visit-id "05" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2478 :al-overhead-at-end 0 :internal-dur-at-end 77 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 1 0