0Assigned ID: 1168
----- Attempting Submission 1 (Fri Apr 07 23:49:04 GMT 2017) -----
HST Phase I Proposal 1168 (HST_uvspec.pdf.apt) successfully submitted.
Receipt: # 1168-1
----- Attempting Submission 2 (Fri Apr 07 23:53:38 GMT 2017) -----ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUNRevised observing program.
Changes:
- STIS G430L science exposures placed at E1 position
- STIS G430L science exposures use full array
- STIS G230L exposure times reduced to accomodate additional overheads715404556----- Attempting Submission 1 (Wed Jul 19 22:39:49 GMT 2017) -----
----- Attempting Submission 2 (Wed May 09 20:12:19 GMT 2018) -----We request pushing the last wavecal of each visit into occultation in order to maximize on-target science exposures, having received approval by the PC. Our program described here is designed to have the wavecal exposure begin right at the start of occultation.An observational test of the dynamical instability hypothesis in the Solar SystemRecent theories of solar system evolution describe a period of chaotic dynamical restructuring that greatly altered the orbital architecture of the giant planets. A key prediction of these models is that the Jupiter Trojans originated in the outer Solar System and were scattered inward during this period of dynamical instability and captured into resonance. Therefore, understanding the composition of Trojans serves as a crucial observational test of these models. While optical spectroscopy has so far not revealed any spectral features, the bimodality in visible color indicates that Trojans are comprised of two subpopulations. In the context of dynamical instability models, both of these groups must originate in the outer Solar System. We have hypothesized that the color bimodality is due to differential sublimation loss of volatile ices and irradiation, with retention or depletion of hydrogen sulfide ice being the determining factor in the surface color. Laboratory spectra of irradiated ice samples analogous to our proposed volatile ice mixtures display an intriguing collection of absorption features in the ultraviolet. The experimental spectra corresponding to the two Trojan color groups show distinct shapes at these wavelengths. We propose using STIS to obtain UV spectra of the brightest 3 Trojans in each color subpopulation. Finding spectral features in this data that match the laboratory spectra would not only confirm our hypothesis for the Trojan color bimodality, but also directly validate dynamical instability models of solar system evolution.We plan on observing six Trojans near opposition at UV wavelengths using the STIS instrument. The targets are the brightest objects within each of the two attested Trojan color subpopulations: less-red (LR: 1437 Diomedes, 3451 Mentor, 659 Nestor) and red (R: 624 Hektor, 911 Agamemnon, 1143 Odysseus). Two spectral settings will be used to provide continuous low resolution wavelength coverage from 160 to 570 nm: MAMA/G230L grism and CCD/G430L grism, utilizing the 52x0.2 slit.
The objective of our observations is to probe the 200-550 nm region for several diagnostic absorption features that are predicted by laboratory experiments and theoretical work modeling the surfaces of these objects within the framework of current dynamical instability models of solar system evolution. We constructed synthetic spectra of LR and R Trojans using the results of laboratory experiments in order to estimate the necessary sensitivity and exposure times needed to discern the predicted absorption features. Our observations are designed to achieve a signal-to-noise per resolution element of 2-3 and 8-10 at 250 nm and 375 nm in the G230L and G430L grisms, respectively.
To successfully observe the objects in our target list at the required sensitivity (and accounting for additional overhead for instrumental setup, spectral setting changes, guide star acquisition, target acquisition, readout, etc.), 7 orbits are needed: two orbits for the faintest target (659 Nestor) and one orbit each for the other 5 Trojans. We have ensured that none of our observations exceed the MAMA buffer imposed limit of 65536 counts/pix or the CCD full well limits. None of our targets require more than the 30 minute limit of total CCD/G430L observing time imposed on mixed STIS MAMA/CCD visits.
In order to efficiently achieve the necessary sensitivity, while allowing for flexibility in scheduling, we propose to observe each target when it is within 0.4-0.5 mag of its maximum brightness during Cycle 25. CCD subarray readout and MAMA binning are utilized to increase science exposure time.Solar SystemPlanets and Planet Formation6falsetruefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMNOASTEROIDASTEROID 1437TYPE=ASTEROID,A=5.159533988224353,E=0.04337508653727421,I=20.52304023492648,O=315.8382440061976,W=129.8928448172086,M=237.2093229761014,EQUINOX=J2000,EPOCH=02-JUL-2006:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMNOASTEROIDASTEROID 3451TYPE=ASTEROID,A=5.112538606970747,E=0.07273377412577345,I=24.6919631935671,O=179.7350158862094,W=131.3185979626035,M=31.88554467267942,EQUINOX=J2000,EPOCH=24-AUG-2011:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMNOASTEROIDASTEROID 659TYPE=ASTEROID,A=5.188694498473398,E=0.1155298393340581,I=4.52091114237396,O=350.8633704121841,W=342.4576456464608,M=81.15977816176995,EQUINOX=J2000,EPOCH=15-OCT-2010:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMNOASTEROIDASTEROID 624TYPE=ASTEROID,A=5.230512653197949,E=0.0228792278641838,I=18.18760284338413,O=342.8071355844293,W=184.8732525052816,M=186.8097363865895,EQUINOX=J2000,EPOCH=27-NOV-2007:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMNOASTEROIDASTEROID 911TYPE=ASTEROID,A=5.25843204129491,E=0.06674871651864867,I=21.78111098287296,O=338.0213980243912,W=79.93752395121545,M=322.9676482457472,EQUINOX=J2000,EPOCH=12-JAN-2009:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMNOASTEROIDASTEROID 1143TYPE=ASTEROID,A=5.257989356782309,E=0.09124805333240484,I=3.135184279117223,O=221.2969502080842,W=235.1547662909868,M=272.3700881440353,EQUINOX=J2000,EPOCH=13-FEB-2009:00:00:00,EpochTimeScale=TDBEARTHSTIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300Using ephemeris for target 15249-01-1437ephemeris data for target 15249-01-1437 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 18.077 to 19.121. ephemeris interval: 18.120 to 20.122The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode./private/var/folders/9v/xf2tslcn5dndy9m1t750wb300000gq/T/OPVisit549778224653485512.xml(Tic-Visit
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