Added SCHED 100 % to give sufficient flexibility to have a chance of scheduling.
----- Submission 46 (Fri May 14 23:37:31 GMT 2004) -----
----- Submission 1 (Fri Apr 22 22:57:24 GMT 2005) -----
----- Submission 2 (Mon Apr 25 15:55:11 GMT 2005) -----
Phase II Proposal 10165 (10165-Submission-002) successfully submitted.
----- Submission 3 (Mon Apr 25 15:56:22 GMT 2005) -----
Visit planner cannot be used on moving Solar System targets.
Non-interruptible sequence recommended by our Program Coordinator. Required for science goals.
Determination of orbits and colors for two new binaries in the Koronis asteroid family
We propose to measure color and orbital properties of two asteroid binaries in the Koronis family discovered in our SNAP-9747 survey. The best previously studied asteroid binary system, Ida/Dactyl, is also in the Koronis family. Differential space weathering measured on the Ida and Dactyl surfaces has been a powerful constraint on models of satellite formation mechanisms and satellite survivability. HST offers the unique opportunity for similar measurements of these much smaller, main-belt binaries. The new satellites are believed to have formed through different collisional mechanisms than Ida/Dactyl.
Further, with a set of 4 relative position measurements for each of the two systems, added to the discovery snapshots, we will determine and compare the densities of the primaries with Ida (a large, 31.5 km, asteroid with density 2.6+-0.5 g/cm^3, measured by the Galileo flyby). In contrast, (17246) and (22899) are 4.5 km bodies that are likely to have been restructured since the family-forming event by subsequent collisions. As all are members of the same family, differences in density would constrain bulk composition and internal structure (e.g. shard vs. rubble-pile). Hence, these measurements are likely to further elucidate the mechanisms for formation of satellites.
Each of 8 visits is an identical single orbit sequence of images in four filters with dithers. Dithers are larger than system size but small enough to execute quickly. A skewed box is used to reduce probability of multiple images of the system being influenced by a column defect.
The 3 images per orbit with F775W are spaced for overall light curve monitoring
during the orbit.
Summed S/N expected in satellite of order 55 in each filter in each visit. The
visits are spaced in time for optimal period determination, around the time of opposition.
As described in Phase-I, we expect that visits 3, 4, 7 & 8 may need their timing requirements adjusted slightly based on data acquired in visits 1, 2, 5, & 6.
SOLAR SYSTEM
12
false
0.0
false
false
false
false
false
SUPPORTED
SOLAR SYSTEM
satellite is 2.5 mag fainter
ASTEROID
Minor Planet (17246) 2000 GL74
TYPE=ASTEROID,A=2.8417325,E=0.0216704,I=2.4533,O=34.59017,W=214.88074,M=287.10964,EQUINOX=J2000,EPOCH=14-JUL-2004:00:00:00
SOLAR SYSTEM
satellite is 2.5mag fainter
ASTEROID
Minor Planet (22899) 1999 TO14
TYPE=ASTEROID,A=2.844071,E=0.085052,I=2.87792,O=136.15296,W=217.72689,M=38.104,EQUINOX=J2000,EPOCH=14-JUL-2004:00:00:00
ACS/HRC
Imaging
No
No
F850LP
ACS/HRC
Imaging
No
No
F775W
ACS/HRC
Imaging
No
No
F435W
ACS/HRC
Imaging
No
No
F550M
ACS/HRC
Imaging
No
No
F850LP
ACS/HRC
Imaging
No
No
F435W
ACS/HRC
Imaging
No
No
F550M
ACS/HRC
Imaging
No
No
F775W
POS-TARG
DITHER
0.15
LINE
0.098
false
false
63.5
4
19.89
ACS-HRC-DITHER-BOX
1
false
Earlier within the timing window is preferred.
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