You may not use the exact name of a given Standard Target unless you are observing it directly.Thank you!867686264Assigned ID: 770
----- Attempting Submission 1 (Fri Apr 11 20:26:35 GMT 2014) -----We are observing Haumea directly, so this error about using the exact name does not apply. (Presumably, APT
is a bit confused about direct observations of moving objects.)Resubmission after discussion with Linda Dressler and Alison Vick about avoiding CTE issues by pre-FLASHing and using a Box-Dither instead of a Line-Dither.
Minor changes that should not affect scheduling.-1896905183----- Attempting Submission 1 (Thu Jul 24 18:20:26 GMT 2014) -----
HST Phase II Proposal 13873 (haumea13873v0.apt) successfully submitted.
----- Attempting Submission 2 (Thu Jul 24 19:35:46 GMT 2014) -----
----- Attempting Submission 3 (Thu Nov 06 20:55:06 GMT 2014) -----The Intriguing Formation of Haumea's SatellitesThe dwarf planet Haumea is arguably the most intriguing Kuiper Belt Object in the outer solar system. Orbited by two satellites, Haumea is also the progenitor of the only collisional family in the Kuiper belt and provides unique insights on the physics of KBO collisions, tides, surfaces, and interiors. A self-consistent theory for Haumea's formation remains elusive, but is clearly connected to unanswered questions about the outer solar system. Precise physical and orbital characteristics of Haumea's satellites can distinguish between several proposed histories. When 2010 HST data was added to the initial orbital solution from Ragozzine & Brown 2009 (RB09), degeneracies between the non-Keplerian effects from satellite masses and from Haumea's non-spherical gravity began to break (Cuk, Ragozzine, Nesvorny 2013). By obtaining three single-orbit visits in Cycle 22, HST will double its observational baseline, which provides very significant improvement in inference of the most interesting system properties. This small investment benefits multiple sicence goals: robust satellite mass and Haumea J2 measurements to distinguish between formation models; crucial support for Haumea-inner-satellite mutual events through 2020; tying down the unusually rapid rotation of outer satellite; and providing context for New Horizons' visit to Pluto. Observations from the ground cannot reasonably provide the same scientific benefit since close-in (~0.25") resolved astrometry and photometry are required. This proposal provides low-risk, high-return scientific insight into the formation of this intriguing object with implications for understanding the outer solar system.Astrometric and photometric observations of the dwarf planet Haumea and its two satellites Hi'iaka and Namaka.
The goal is to obtain precise astrometry and high-cadence photometry of the satellites of Haumea. During the observing season, Haumea is located near 14h and +17d. The observing sequence will follow the successful observations of Program 12004.
The observations are designed to maximize overall signal-to-noise (by maximizing total exposure time), while taking multiple observations to produce a high-cadence light curve. We would like as many 40-second observations per orbit as possible. In order to minimize overheads, we're using the 512K subarray of WFC3/UVIS. The target should be centered in a region of good pixels near the center of the subarray.
The observations are time-sensitive: observing when the satellites are near Haumea, but definitely not within its PSF, contains the most information and has the highest scientific value. This limits the useful observation time to ~20% of the total time, spread over tens of observation periods. It turned out to be most straightforward to enter this in as a large number of BETWEEN requirements. We also require 30 days between each observation to obatin independent information. As necessary, we will interact directly with scheduling to make the observations both plausible and valuable.SOLAR SYSTEM12falsefalse0.00.0falsefalsefalseSUPPORTEDSOLAR SYSTEMUsing Haumea as a standard target.
During this cycle of observations, the rough RA and Dec are 14h and 17d.DWARF-PLANET(136108) Dwarf Planet HaumeaSTD=HAUMEAEARTHWFC3/UVISImagingNoNoF350LPPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falseUsing ephemeris for target 13873-01-HAUMEAephemeris data for target 13873-01-HAUMEA does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 14.213 to 16.090. ephemeris interval: 14.304 to 16.306The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.C:\Users\dragozzine\AppData\Local\Temp\OPVisit5708829862467828575.xmlEach visit is 1 orbit long with 4 sets of 7 observations each, with a dither in between, and each observation lasting about 40 seconds. The number of observations calls for the use of the 512x512 subarry on WFC3. The goal is precise astrometry and photometry of moving object Haumea.
To optimize the information content, I have identified when the satellites are visible and non-overlapping and current orbital solutions are weak. The easiest way to define this was as ~50 between requirements with 1-3 day durations. We can iterate with the schedulers to make this work.(Tic-Visit
:proposal-id 13873
:visit-id "01"
:proposal-version -1
:trans-version "20140605"
:date "06-Nov-2014 15:47:41.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 128144
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
:proposal-id 13873
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
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(Tic-Orbit
:proposal-id 13873
:visit-id "01"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2862
:al-overhead-at-end 0
:internal-dur-at-end 177
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3222
:pcs-gap 0
)true10Using ephemeris for target 13873-02-HAUMEAephemeris data for target 13873-02-HAUMEA does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 14.213 to 16.090. ephemeris interval: 14.304 to 16.306The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.C:\Users\dragozzine\AppData\Local\Temp\OPVisit4102276663242301082.xmlEach visit is 1 orbit long with 4 sets of 7 observations each, with a dither in between, and each observation lasting about 40 seconds. The number of observations calls for the use of the 512x512 subarry on WFC3. The goal is precise astrometry and photometry of moving object Haumea.
To optimize the information content, I have identified when the satellites are visible and non-overlapping and current orbital solutions are weak. The easiest way to define this was as ~50 between requirements with 1-3 day durations. We can iterate with the schedulers to make this work.(Tic-Visit
:proposal-id 13873
:visit-id "02"
:proposal-version -1
:trans-version "20140605"
:date "06-Nov-2014 15:47:56.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 128144
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13873
:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13873
:visit-id "02"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2862
:al-overhead-at-end 0
:internal-dur-at-end 177
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3222
:pcs-gap 0
)true10Using ephemeris for target 13873-03-HAUMEAephemeris data for target 13873-03-HAUMEA does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 14.213 to 16.090. ephemeris interval: 14.304 to 16.306The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.C:\Users\dragozzine\AppData\Local\Temp\OPVisit2046787421223332772.xmlEach visit is 1 orbit long with 4 sets of 7 observations each, with a dither in between, and each observation lasting about 40 seconds. The number of observations calls for the use of the 512x512 subarry on WFC3. The goal is precise astrometry and photometry of moving object Haumea.
To optimize the information content, I have identified when the satellites are visible and non-overlapping and current orbital solutions are weak. The easiest way to define this was as ~50 between requirements with 1-3 day durations. We can iterate with the schedulers to make this work.(Tic-Visit
:proposal-id 13873
:visit-id "03"
:proposal-version -1
:trans-version "20140605"
:date "06-Nov-2014 15:47:58.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 128144
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13873
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13873
:visit-id "03"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2862
:al-overhead-at-end 0
:internal-dur-at-end 177
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3222
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)true10