Target EUROPA-45: 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.
Target EUROPA-135: 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.
Target EUROPA-225: 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.
Target EUROPA-315: 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.0Assigned ID: 3624
----- Attempting Submission 1 (Fri Mar 25 22:07:08 GMT 2022) -----All four warnings are due to my target being a moving target, which does not require testing the scheduling of observations in phase I.Resubmitting with shortened exposure times for the second orbit of visit 05, so that all science expsoures are now 200 seconds. This change is to aid in scheduling.135986882----- Attempting Submission 3 (Thu Oct 20 16:38:19 GMT 2022) -----
----- Attempting Submission 4 (Fri Jan 05 23:34:00 GMT 2024) -----
----- Attempting Submission 5 (Mon Jan 08 20:24:32 GMT 2024) -----I ran it only for visit 05, because it was failing for the other (completed visits).Europa's UV absorptions: oceanic or exogenic origins?Recently resurfaced terrain on Europa may contain compositional fingerprints of the internal ocean, providing a window into its chemistry and habitability. However, understanding the relationship between the surface and subsurface chemistries relies on distinguishing endogenic species from those produced via the exogenic bombardment of the surface with Jovian magnetospheric particles. Over the past 20+ years, numerous studies have sought to disentangle the two, but have been stymied by either a lack of spectral features across the wavelengths explored, a lack of sufficient spatial resolution to discern geology from background magnetospheric patterns, or both. High-spatial-resolution observations in the mid-UV would provide a singular opportunity to build our understanding of these contributions to Europa's surface, which will soon be visited by two Flagship-class spacecraft missions--NASA's Europa Clipper and ESA's JUICE. Two of Europa's fewer than ten compositionally diagnostic absorption features (other than those of water ice) lie at mid-UV wavelengths, including the only feature indicative of the plausibly endogenic SO2 and a feature newly discovered this year that could indicate endogenic salt or an exogenic radiolytic product. We propose a simple slit-scanning program with STIS in G230L to map these features at the high spatial resolution necessary to determine their origins. As neither spacecraft mission carries instrumentation spanning these wavelengths, HST provides the only opportunity to map Europa across this critical wavelength range, thereby enhancing the scientific return of the upcoming missions.Using STIS, we plan to create a uniform dataset of spatially resolved UV (G230L) spectra of the surface of Europa. We plan to replicate previously successful G430L and G750L Europa programs as closely as possible. Four separate phases of Europa will be observed to allow complete longitudinal coverage. Four observations spaced 90 degrees apart ensure that the worst resolution along the equator will be degraded by only ~40% relative to the sub-observer point. The past programs on which we base our observations used the 0.1" slit and stepped it across the surface in 0.06" increments over four Europa phases, for a total of 15 overlapping slit positions per phase. We propose to execute an analogous program in G230L to achieve the same spatial resolution and global coverage at UV wavelengths, thereby resolving any correlations of the UV absorption features with geology.
To ensure that our planned exposures will obtain the signal-to-noise ratio (SNR) necessary to achieve our science goals, we scale from the existing archival G230L observations of Europa. We set our SNR requirements based on our science goal of mapping the 230-nm feature, which is weaker than the SO2 absorption and falls in a noisier portion of the spectrum. Spectra that meet this requirement will thus be more than adequate to map the SO2 absorption. Based on the variability in the 230-nm band strength that we observe in the existing G230L data, we estimate a need to detect absorptions with an equivalent width of 3 nm to 5 sigma in order to adequately measure the geographic distribution. As the G230L spectra provide ~275 points across the 40-nm FWHM of the absorption feature, this equates to a required SNR of ~4 per pixel. Using 800-second exposures in the 0.2" slit, the existing G230L spectra achieved a SNR of 10 per pixel across the 230-nm region. Scaling directly from this measurement, we can achieve a SNR of 5 per pixel (half that of the current observations and beyond our calculated requirement of 4 per pixel) using the 0.1" slit, at least 200-second integrations, and 2-pixel extractions (resulting in the same effective pixel scale as the past G430L observations).
We plan our program in 4 two-orbit visits (one visit per phase; two orbits to map the entire disk each time). We break up the slit-scan of the disk each visit into two separate patterns: a 7-slit pattern covering slightly less than half of the disk to be executed in the first orbit of a visit, which has less science time due to target acquisition, and a 9-slit pattern covering slightly more than half of the disk to be executed in the second orbit of a visit. In the exposure sequence corresponding to each pattern within the visits, we specify the necessary target offsets, such that the 7-slit pattern begins at the edge of the disk and the 9-slit pattern begins where the 7-slit pattern left off, thereby completing coverage of the disk over the 16 total slit positions. To maximize time dedicated to science exposures, we place the necessary wavecals at the end of each orbit, so that they are pushed into occultation.
In the event of reduced-gyro operations, the main impacts to this program are expected to be reduced schedulability, as these observations are already time-constrained, and increased overheads for target acquisition, resulting in reduced science exposure times.Our team has extensive experience in Europa spectroscopy from the UV through infrared and in STIS spatially resolved slit spectroscopy. We recently published the first spatially resolved visible wavelength observations of Europa (using HST STIS), spatially resolved STIS observations of Ganymede, as well as the existing HST STIS UV observations of Europa.Solar System Astronomy6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMYESCentered near phase = 45 degrees (45 W longitude)SATELLITESATELLITE EUROPASTD=JUPITERSTD=EUROPANOT OCC OF EUROPA-45 BY JUPITER FROM EARTH,
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)false20Using ephemeris for target 17142-05-EUROPA-45-2ephemeris data for target 17142-05-EUROPA-45-2 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 22.269 to 25.152. ephemeris interval: 24.152 to 26.152The scheduling data was generated by CASM 32.1.CASM was run in Phase II mode./private/var/folders/46/4jpf0wpx40jbz16h87362w240001d2/T/OPVisit17170633950655723671.xmlTiming windows are chosen such that Europa's angular size is near its maximum of ~1 arcsecond, in order to maximize spatial resolution, which is key to our science goals.(Tic-Visit
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:visit-id "02"
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:date "20-Oct-2022 12:36:30.0"
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