Target P2010-V1: There is no need or capability to test the scheduling of observations of moving targets in Phase I. This warning will go away the next time the proposal is loaded.1pm Sunday Jan 311175347877Assigned ID: 1264
----- Attempting Submission 1 (Sun Jan 31 21:16:00 GMT 2016) -----APT telles me to run the Visit Planner and, when I do, I get this message, telling me I cannot run the Visit Planner.
Diagnotics currently on your proposal
Warning (Visit Planner): Target P2010-V1: There is no need or capability to test the scheduling of observations of moving targets in Phase I. This warning will go away the next time the proposal is loaded.
Occurrence: #1 P2010-V1First submission for GO-14498.
We used a special ephemeris from JPL (solution #5) with an osculation epoch
of 12-Apr-2016 so that non-grav parameters aren't used.1174664357----- Attempting Submission 1 (Wed Mar 23 20:24:56 GMT 2016) -----Comet P/2010 V1 as a Natural Disintegration LaboratoryWe propose mid-cycle observations of short-period comet P/2010 V1, currently undergoing a spectacular disintegration. Observations already obtained under GO 14474 reveal multiple fragments undergoing rapid evolution, and motivate the additinal high resolution, time-resolved images proposed here. Science objectives are to determine the nature and cause of the breakup by studying the dynamics, and the photometric and morphological evolution of this body. Results will provide key constraints on existing breakup and disintegration models. Our HST data will constitute by far the best observational dataset ever obtained, with unprecedented spatial and temporal resolution.Our basic observing strategy is to take multiple long exposures (348-400 sec) using WFC3 and a wide bandpass filter (F350LP) for maximum sensitivity. We use F350LP because experience in previous HST programs shows that the F350LP count rate is 1.6 times higher for a target with a solar-type spectrum than other commonly used broadband filters (e.g. F606W). We also plan to dither the exposures to mitigate the effects from bad pixels, cosmic rays, and the inter-chip gap. The WFC3 Exposure Time Calculator indicates that, for a point source, solar-type spectrum, a signal-to-noise ratio of 6 is reached in 348 s at V = 26.5 in the F350LP filter (ETC request ID WFC3UVIS.im.765972; optimal extraction yields SNR=13). For example, on UT 2016 March 24, when heliocentric distance R = 1.57 AU, geocentric distance 0.78 AU and phase angle 31 deg, magnitude V = 26.5 corresponds to an object radius 30 m (geometric albedo 0.04 and C-type asteroid phase function assumed). These are upper limits to the point source thresholds because at least some of the fragments are embedded in their own dust comae. However, it is clear that HST offers unprecedented sensitivity to faint fragments. Our observations have the following main objectives, both of which build upon the unprecedented dataset we are acquiring under GO 14474. Five HST orbits, consecutive or as nearly consecutive as possible, will allow us to examine rotationally modulated brightness variations. Five orbits with HST will provide a timebase from which the best possible constraints on the importance of rotation can be obtained. The apparent rates of motion relative to sidereal are easily within Hubble|'s tracking capabilities. The rate of motion is also slow enough to keep a single pair of guide stars within the FGS pickles for an entire visibility window. The ephemeris uncertainties on the main components of P/2010 V1 (e.g. A, B, C, D) are sub-arcsecond. We will position the field so that D and the fragement-rich field in Figure (2) are well-placed but, because of the increasing separation of the components, will have to sacrifice the western-most component A. We understand that we will have essentially no control over the spacecraft roll angle.
We request 5 mid-cycle orbits within the April 1-15 window. Under GO 14474 we have schedule HST observations on January 26-28, February 11-13 and March 24. The March 24 observation is timed to coincide with the passage of Earth through the orbital plane of V1, providing a unique and projection-free determination of the out-of-plane velocity of the fragments, Unfortunately, because many fragments are likely aligned very closely with the plane, we expect substantial overlap and confusion with dust on this date and, for many fragments, the best astrometry will come only from the 2-week timebase separating the January and Febuary observations.Solar System12falsefalsefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMYESCOMETtestTYPE=COMET,Q=1.573112870680267E+00,E=4.905480395391478E-01,I=9.387268291468491E+00,O=3.782156311741634E+00,W=1.524172097988438E+02,T=17-MAR-2016:05:02:50,TTimeScale=TDB,EQUINOX=J2000,EPOCH=12-APR-2016:00:00:00,EpochTimeScale=TDBTYPE=POS_ANGLE,RAD=64.8,ANG=289.8,REF=NORTHEARTHWFC3/UVISImagingNoNoF350LPUsing ephemeris for target 14498-01-P2010-V-C-OFFSETephemeris data for target 14498-01-P2010-V-C-OFFSET does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 15.213 to 17.089. ephemeris interval: 16.060 to 18.060Timing link suitability includes constraints ([Sequence (01 02 03 04 05) within 1.0 days])The scheduling data was generated by CASM 24.0.CASM was run in Phase II mode.51/private/var/folders/tb/q3zsbl1j6d3gvdw7h3dn3qmj9fwgz5/T/OPVisit2009999166984631847.xml(Tic-Visit
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