0Assigned ID: 5634
----- Attempting Submission 1 (Tue Mar 26 20:50:41 GMT 2024) -----Sensitive exposures should have an ETC run number provided.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
INEFFICIENT ORDERING OF FP-POS POSITIONS
Sensitive exposures should have an ETC run number provided.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
POS TARG OUTSIDE OF APERTURE NO ORIENT
POS TARG OUTSIDE OF APERTURE
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
Sensitive exposures should have an ETC run number provided.0----- Attempting Submission 1 (Wed Jul 10 10:28:39 GMT 2024) -----All exposures are repititions and we do not give ETC runs (but can point to previous exposures in the archive).
The offset exposures are meant to have the target outside the Field-of-view.A UV eclipse test for Callisto's atmosphere, plasma interaction and water oceanJupiter moon Callisto might have a subsurface ocean as well as the fourth densest atmosphere of all solar system moons. The primary O2 atmosphere was inferred indirectly through sensitive HST/COS observations of electron-excited UV oxygen emissions. Because the interaction of Callisto's atmosphere-ionosphere leads to a strong diversion of the magnetospheric electrons, the UV emissions were interpreted to be from photo-electrons. However, optical oxygen emissions were detected in 2021 when Callisto was in eclipse of Jupiter and thus must be excited by magnetospheric electrons and not photo-electrons. Archival COS observation of Callisto in sunlight can not resolve the question of the excitation, but interestingly they suggest O or H2O must be abundant in addition to O2.
After a 3-year period without eclipses, Callisto will be again eclipsed by Jupiter in the coming HST cycle. We propose sensitive COS observations of the diagnostic 1304 A and at 1356 A emissions from before ingress, through the eclipse passage until after egress. The changes in UV emissions over eclipse will reveal the excitation mechanism and provide constraints on the composition of the atmosphere. If the UV emissions disappear in eclipse, a strong plasma diversion and dense ionosphere are confirmed, which challenges the necessity of a subsurface ocean to explain magnetic induction.
ESA's JUpiter Icy Moon Explorer and NASA's Europa Clipper mission will carry out several flybys at Callisto. An improved understanding of the moon's atmosphere and ocean delivers important information for optimal science planning and addressing the habitability goals for these milestone missions.We observe Callist with 7 orbits to cover the complete transition from before ingress to after egress from eclipse.
1 visit with 2 orbits around ingress into eclipse,
1 visit with 3 orbits starting in eclipse and continuing to 1 hour after egress.
2 orbits for reference spectra at an offset from the target for background correction.
Crucially, the moment of going into and emerging from total umbral shadow should be within an exposure. For the egress visit, the first orbit should be at the egress and the second orbit/exposure will be ~1 hour after egress, as the time scale for recovery of a sublimated H2O component are on this order.
After a season without eclipses, Callisto is eclipsed again from August 2025. Optimally, the visits are scheduled as close in time as possible (same or consecutive eclipse passages).
For the offset, the aperture is placed 5" away along the detector y axis, identical for the large offsets used in GO 14755. The offset exposures can be taken when Callisto is eclipsed or in sunlight.
We do not set parameter to constrain exact geometries (like ingress) but will look into possible scheduling options case by case.The team is composed of experts on different parts of the project from planing of the observations to data analysis and modeling (DMSC) for the interpretation.
The PI Lorenz Roth has experience from leading 8 successful HST programs as PI. He has proven to lead the HST observing programs from the beginning to succesful publications, including programs with eclipse observations of Europa technically similar to the observations proposed here for Callisto. Joachim Saur is expert in the plasma interactions of the Jupiter moons with the magnetosphere and will provide input plasma sputtering processes for the surface and atmosphere. John Spencer, Nathaniel Cunningham, Joachim Saur, Kurt Retherford, and Carl Schmidt have furthermore extensive experience with HST and COS, inlcuding as PIs of several GO programs including Callisto observations. Shane Carberry Mogan and Andrew Poppe do DSMC modeling of Callisto's atmosphere (5+ papers).
The PI and three CoIs are members of the JUICE and Europa Clipper science teams.Solar System Astronomy6falsetruefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMYESSATELLITEJupiter moon CallistoSTD=JUPITERSTD=CALLISTONOT OCC OF CALLISTO-SUBJOVIAN BY JUPITER FROM EARTH,
SEP OF CALLISTO-SUBJOVIAN IO FROM EARTH GT 10",
SEP OF CALLISTO-SUBJOVIAN EUROPA FROM EARTH GT 10",
SEP OF CALLISTO-SUBJOVIAN GANYMEDE FROM EARTH GT 10",
CML OF CALLISTO-SUBJOVIAN FROM EARTH BETWEEN 330 30EARTHSOLAR SYSTEMYESSATELLITEOffset from Callisto for referenceSTD=JUPITERSTD=CALLISTONOT OCC OF CALLISTO-OFFSET BY JUPITER FROM EARTH,
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CML OF CALLISTO-OFFSET FROM EARTH BETWEEN 330 30EARTHSOLAR SYSTEMYESEuropa for acquistion for visit when Callisto is in eclipse at start.SATELLITEEuropa for acquisitionSTD=JUPITERSTD=EUROPANOT OCC OF EUROPA-ACQ BY JUPITER FROM EARTH,
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SEP OF EUROPA-ACQ CALLISTO FROM EARTH GT 10"EARTHCOS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291Using ephemeris for target 17739-01-CALLISTO-SUBJOVIANThe scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/williamj/hst/work/cycle32/OP-cache/17739-v01.xml(Tic-Visit
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