Cannot find file /Users/dave/Dropbox/Cycle_30_midcycle_2_Didymos/midcycle2_DART.pdf0Assigned ID: 3884
----- Attempting Submission 1 (Mon Feb 13 15:21:39 GMT 2023) -----
HST Phase I Proposal 3884 successfully submitted.
Receipt: # 3884-1
----- Attempting Submission 2 (Tue Feb 14 15:40:36 GMT 2023) -----This is the initial submission for this mid-cycle continuation of our Didymos monitoring, with similar observing strategy as our earlier programs 17289 and 17293. We'd like the 15 orbits scheduled as close together as possible near April 1. The timing constraints are tight, but can be relaxed, and also the exposure times can be reduced as needed for scheduling. A slight dithering is applied in between groups of 5 visits as small POS TARGs. We are available to our Program Coordinator to continue tweaking this program as needed for quick implementation. -- Max Mutchler1764861179----- Attempting Submission 1 (Wed Mar 22 14:39:23 GMT 2023) -----Evolution of the DART Dimorphos Debris FieldDeep HST images of the NASA DART asteroid target Didymos/Dimorphos reveal the unexpected existence of a swarm of at least 40 discrete, co-moving objects. These are interpreted as boulders lifted from the asteroid surface by the DART impact, with sizes up to 8 m. Depending on the size distribution, large particles like those observed may dominate the ejected mass, so that it is important to characterize their properties (especially size), their number, and their dynamics. We propose deep observations with HST and WFC3 in order to obtain additional observations before the boulder swarm fades to invisibility. Using the enlarged data arc provided by the new observations, we will estimate the ejection speeds and directions and compare with independent measurements and models of the small particle ejection. The observations are urgent because the target is rapidly fading as it recedes from the Sun and Earth and because the boulders are already very faint. The proposed measurements maximally capitalize on the resolution and sensitivity of HST. Results will be of value for the practical understanding of impact physics, for the interpretation of natural impacts like those already detected in P/2010 A2 and 596 Scheila, and to set the scene for ESA's imminent HERA mission to Didymos/Dimorphos.We request 15 orbits with WFC3 and F350LP on or near April 1. This number of orbits will provide detections of 8 - 12 boulders and give unique and irreplaceable information on the dynamics of the largest bodies ejected by the DART impact. More boulders could be imaged, but only at the cost of a much larger orbit allocation that would be incompatible with the mid-cycle limit and also disproportionate to the extra science gained. The ejection velocity field obtained from the observations will be compared with the known impact and ejecta directions from the DART impact mission. The orbits should ideally be close together but need not be contiguous. The observation would be conducted as follows. The F350LP filter is a long-pass filter with very broad spectral coverage (FWHM > 4000 A), providing maximum sensitivity to continuum sources. It has become the standard filter for numerous Hubble GO observations of faint solar system targets, from asteroids and comet nuclei to Kuiper belt objects. Our plan is to obtain dithered images (to escape the effects of bad pixels and the inter-chip gap) with six images per orbit having exposure times of 200s each. To maximize observing efficiency and, bearing in mind the known sky area occupied by the co-movers, we will use a 2k x 2k WFC3 CCD readout, providing a 80 x 80 arcsec field of view. The target fades progressively as it recedes from the Earth and Sun. We used the WFC3 Exposure Time Calculator to find that the brightest co-mover would be detected at optimum SNR (signal-to-noise ratio) = 5.3 on UT 2023 April 1, given 15 orbits of HST with WFC3 and F350LP. A composite from these 15 orbits will reveal the largest and brightest 8 - 12 of the 38 detected boulders at signal-to-noise > 3 and give valuable (+/- 0.04 arcsec) astrometry for each. This is a large enough sample and good enough accuracy to meaningfully probe the ejection dynamics of the boulders as a group. Therefore, we request 15 orbits with WFC3 and F350LP on or near April 1, with earlier observations providing better sensitivity and substantially later ones degrading the number of boulders to be detected. In summary, our request is for 15 orbits with WFC3 and F350LP, as close as possible to UT 2023 April 1. The ephemeris uncertainties are < 1 arcsec and have no impact on the planned observations. The non-sidereal rates of Didymos as observed from HST are < 65 arcsec/hour on UT 2023 April 1 and fall well within HSTs tracking capabilities (which are limited by linear interpolation from the ephemeris). The elongation of Didymos is 107 degrees on April 1, falling into the HST solar exclusion zone of 55 degrees by UT 2023 July 6. It remains too close to the Sun to observe until 2024 Jan 28, by which time both rH and delta are too large for the boulders to be imaged. Equivalent Cycle 31 observations therefore cannot be proposed. There is no observationally favorable, comparably close pass to Earth by Didymos until 2062 and therefore the proposed observations cannot be repeated in the forseeable future. Scheduling of these observations and characterization of the ejecta in the remainder of Cycle 30 will allow us to be ready for the next stage of the Didymos/Dimorphos investigation, expected to unfold with the upcoming launch of the ESA HERA mission in late 2024.PI Jewitt is experienced in the study of solar system bodies with HST and other telescopes. CoI Kim is an expert in the modeling of dust dynamics, needed to interpret the trail dynamics. CoI Li is experienced in digital imaging analysis. CoI Mutchler is an expert in matching the capabilities of HST/WFC3 to the scientific study of challenging non-sidereal targets. CoI Agarwal is experienced in the study of low speed macroscopic objects in spacecraft data.Solar System Astronomy3falsefalsefalsefalsefalsetruefalsefalseSUPPORTEDSOLAR SYSTEMNOASTEROIDBinary asteroid (65803) Didymos impacted by DART spacecraftTYPE=ASTEROID,A=1.642514363757057,E=0.3832947329867846,I=3.414168800300961
,O=72.99221760945375,W=319.5559920731379,M=38.72558818260499,EQUINOX=J2000,EPOCH=12-JAN-2023:12:00:00,EpochTimeScale=TDB,R0=1.
,A1=0.,A2=-1.042309691002E-14,A3=0.
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 422320
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17297
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17297
:visit-id "14"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2333
:al-overhead-at-end 0
:internal-dur-at-end 498
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2782
:pcs-gap 0
)true10Using ephemeris for target 17297-15-DIDYMOSephemeris data for target 17297-15-DIDYMOS does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 22.213 to 24.182. ephemeris interval: 23.059 to 25.060Timing link suitability includes constraints ([Group (01 02 03 04 05 06 07 08 09 10 11 12 13 14 15) Within 1.5 days])The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 17297
:visit-id "15"
:proposal-version -1
:trans-version "20220630"
:date "22-Mar-2023 10:33:49.0"
: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 422320
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17297
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17297
:visit-id "15"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2333
:al-overhead-at-end 0
:internal-dur-at-end 498
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2782
:pcs-gap 0
)true10