0Assigned ID: 993
----- Attempting Submission 1 (Fri Apr 07 22:22:46 GMT 2017) -----Unschedulable Visit
Unschedulable Visit
Unschedulable Visit
Unschedulable Visit
ORBITAL VISIBILITY OVERRUN
Unschedulable Visit
ORBITAL VISIBILITY OVERRUN
Unschedulable Visit
ORBITAL VISIBILITY OVERRUN
Unschedulable Visit
Unschedulable Visit
ORBITAL VISIBILITY OVERRUNThis submission removes the repointings for visits 1, 2, 3, and 7 and increases the number of exposures per target.
The new observing pattern should just continue exposing on target, with no repointings or dither.
Pattern 1 (Line) is no longer used.
In preliminary reduction of visits 4-6 these were not found to improve performance and increased overhead.
No other changes were made.-342150615----- Attempting Submission 1 (Thu Jul 20 23:07:13 GMT 2017) -----
----- Attempting Submission 2 (Sat Sep 30 18:18:53 GMT 2017) -----
----- Attempting Submission 3 (Tue Aug 07 17:15:14 GMT 2018) -----
----- Attempting Submission 4 (Mon Sep 03 15:06:07 GMT 2018) -----
----- Attempting Submission 5 (Mon Dec 10 21:46:16 GMT 2018) -----Visit planner failed, likely due to prior complete observations. Resubmitting per B. Perriello.0Imaging the predicted asteroid belt analogue around Epsilon EridaniWe propose to take advantage of the STIS coronagraphic mode and advances in speckle subtraction techniques to probe for scattered light from Epsilon Eridani's predicted asteroid belt analog. This proposal tests for the presence of visible scattered light from a warm dust ring at 1 arcsecond with a 5e-5/as^2 contrast, predicted from observations of the 24 micron excess. Dust morphology and scattered light brightness (exozodi) present a significant challenge to future exoplanet imaging missions, and Epsilon Eridani is an excellent sunlike candidate for future exoplanet direct imaging missions due its easily accessible habitable zone.
Either a detection of scattered light from this circumstellar dust population or a non-detection will place valuable constraints on the dust composition, morphology, and transport mechanisms at work in the system and inform future direct imaging efforts of this nearby star system.We propose multi-roll, dithered, STIS Wedge A1.0 coronagraphic observations of Epsilon Eri and a calibration star, Delta Eridani. Extrapolating from known coronagraphic PSF wings and the count rates in the (partially-saturated) 12 second Wedge 1.0 eps Eri observation from proposal #8896, we estimate 2.3 second exposures will remain unsaturated near the inner-working angle of the wedge (0.5 arcsec). At this exposure time, six orbits will allow us to test for the predicted narrow warm belt, supplemented by two additional calibration star orbits. A different roll angle for each orbit, will minimize degeneracy between coronagraphic speckles and astrophysical sources while the calibration star will prevent self-subtraction of the expected face-on disk.
We will reduce the data using three approaches, classical and Karhunen-Lou've Image Plane (KLIP) (Soummer et al., 2012) PSF subtraction after alignment of images via radon transform, techniques previously demonstrated with the STIS BAR5 coronagraph (Debes & Ren (2017)) as well as reduction using g vectorized Nonnegative Matrix Factorization (Zhu 2016, Debes and Ren in Prep). KLIP reduction provides superior performance near the star, while classical subtraction reaches deeper contrasts at larger angles and NMF avoids over-subtraction of extended objects.
Consecutive orbits and dithering during each orbit are required to ensure accurate reference and speckle subtraction, and to reduce speckle noise due to instrument drift and pointing variations.
Reaching the contrasts proposed requires highly accurate PSF subtraction. Since the eps Eri system is nearly face-on, simply rolling on the star could lead to disk self-subtraction and a PSF calibration with a similar color is essential for accurate subtraction of the PSF wings (Schneider et al., 2014). We employ two orbits observing Delta Eridani, a K0 IV star of comparable color and similar magnitude and close (on-sky) proximity to eps Eri. This proximity will minimize speckle variations between the two targets by maintaining a similar spacecraft attitude.
Update 8 Aug 2018:
DecreasingPlanets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARCIRCUMSTELLAR MATTERDISKEXTRA-SOLAR PLANETARY SYSTEMCoordinates from Simbad, APT keeps rounding J2000 coordinates, they should be:
ICRS coord. (ep=J2000) : 03 32 55.84496 -09 27 29.7312 (Optical) [ 1.84 1.75 90 ] A 2007A&A...474..653V.
Uncertainties from 007A&A...474..653V via Vizier.J2000J2000CALIBRATIONPOINT SPREAD FUNCTIONCoordinates from Simbad, APT keeps rounding J2000 coordinates, they should be:
ICRS coord. (ep=J2000) : 03 43 14.90088 -09 45 48.2084 (Optical) [ 2.54 1.93 79 ] A 2007A&A...474..653V
Uncertainties from 007A&A...474..653V via Vizier.J2000J2000STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0STIS/CCDImagingYesNoWEDGEA1.0POS-TARGDITHER0.01269Building on dither results from recent BAR5 studies to potentially improve KLIP post-processing by dithering perpendicular to the wedge's long axis.
Pattern is centered so no targ-pos offset is required.
It may be more efficient if the central point could be visited then each side of the line, since this would not require a repointing after acquisition.LINEfalsetrue30LINE1falseTiming link suitability includes constraints ([07 After 01 by 0.1 to 0.1 days] [01 After 06 by at most 30.0 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.Initial orientation unconstrained, each subsequent observations roll adds 15-25 degrees.
Repointings removed after preliminary analysis of visits 4-6 shows no improvement.154592761100041.31899999999999(Tic-Visit
:proposal-id 15217
:visit-id "01"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 13:35:52.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 185904
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "01"
:obset-id "01"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "01"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2812
:al-overhead-at-end 0
:internal-dur-at-end 395
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10Acq Exposure time calculation gives a 3x margin on saturation (occurs at 0.31 sec): http://etc.stsci.edu/etc/results/STIS.ta.1006837/
No ACQ-PEAK as advised by CS.SIZEAXIS2 is set to 110 to provide a 5.5 arcsec FOV (reduced from 190 or 10 arcsec to better sample the inner PSF following Su et al 2017's results showin the ring is likely to be between 0.5 as and 1 arcsecond from the star).
These exposures are balanced with 15 second "deep exposures" at the end of the sequence to place third STIS buffer dump at end of visit. Decreasing SIZEAXIS2 from 190 to 110 increased the number of exposures per pointing, allowing >10% increase in exposure time.
Deep exposures will saturate the core in that frame but maximizes the sensitivity for the number of frames available per orbit, we do not expect significant afterglow effects at levels below 50x full well (Instrument Science Report STIS 2015-06 (v1)).
Su et al., The Inner 25 Au Debris Distribution in the Eri System. The Astronomical Journal 153 (5): 226. https://doi.org/10.3847/1538-3881/aa696b.Timing link suitability includes constraints ([03 After 02 by 0.1 to 0.1 days] [02 After 07 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.154593905300056.31899999999999(Tic-Visit
:proposal-id 15217
:visit-id "02"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 13:40:17.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 185904
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:visit-id "02"
:obset-id "02"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "02"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2812
:al-overhead-at-end 0
:internal-dur-at-end 395
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10same as visit 1.Timing link suitability includes constraints ([03 After 02 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.154594477400071.31899999999999(Tic-Visit
:proposal-id 15217
:visit-id "03"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 14:46:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 185904
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "03"
:obset-id "03"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "03"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2812
:al-overhead-at-end 0
:internal-dur-at-end 395
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10same as visit 1.Timing link suitability includes constraints ([05 After 04 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.This sequence of roll angles (04)-(06) can be scheduled either before or after the first 4, but simply should have the same angular seperations relative to (01) thru (03) and the same separation of days between them. The separation was chosen to keep a feature orbiting at the target separation small - shorter separations would be preferred.154338751000026.31899999999999(Tic-Visit
:proposal-id 15217
:visit-id "04"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 15:36:25.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 182000
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "04"
:obset-id "04"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "04"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2872
:al-overhead-at-end 0
:internal-dur-at-end 365
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true11Timing link suitability includes constraints ([05 After 04 by 0.1 to 0.1 days] [08 After 05 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.This sequence of roll angles (04)-(06) can be scheduled either before or after the first 4, but simply should have the same angular seperations relative to (01) thru (03) and the same separation of days between them. (There does not appear to be a way to relate the two sets of visits in a reversable manner in APT but that would be OK for scheduling.) The time separation between sets was chosen to keep a feature orbiting at the target separation (3.0AU) from orbiting more than 1.5 pixels and shorter separations would be preferred.154339323100011.318999999999988(Tic-Visit
:proposal-id 15217
:visit-id "05"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 15:36:44.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 182000
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "05"
:obset-id "05"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "05"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2872
:al-overhead-at-end 0
:internal-dur-at-end 365
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true11Timing link suitability includes constraints ([01 After 06 by at most 30.0 days] [06 After 08 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.This sequence of roll angles (04)-(06) can be scheduled either before or after the first 4, but simply should have the same angular seperations relative to (01) thru (03) and the same separation of days between them. (There does not appear to be a way to relate the two sets of visits in a reversable manner in APT but that would be OK for scheduling.) The separation was chosen to keep a feature orbiting at the target separation (3.0AU) from orbiting more than 1.5 pixels and shorter separations would be preferred.1543404672000356.31899999999996(Tic-Visit
:proposal-id 15217
:visit-id "06"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 15:37:00.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 182000
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "06"
:obset-id "06"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "06"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2872
:al-overhead-at-end 0
:internal-dur-at-end 365
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true11Timing link suitability includes constraints ([07 After 01 by 0.1 to 0.1 days] [02 After 07 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.Orientation unconstrained. Directly follows first three epsilon eridani orbits in order to minimize changes in telescope state.154593337700049.0(Tic-Visit
:proposal-id 15217
:visit-id "07"
:proposal-version -1
:trans-version "20181130"
:date "10-Dec-2018 15:03:08.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 193712
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "07"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2807
:al-overhead-at-end 0
:internal-dur-at-end 403
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true10Exposure time of 0.1 second with ND3 filter gives SNR=345 and the time to saturation is 0.25, a 2.5x margin, acquition exposure time calculator run using Pickles K0IV star: http://etc.stsci.edu/etc/results/STIS.ta.1012385/Exposure time rescaled from Eps Eri using the 20% increased flux from Delta Eri.
Deep (~15 sec) exposure at the end of each set to match Eps Eri.
Auto-adjusted last frame of central pointing to fill out exposure time.Timing link suitability includes constraints ([08 After 05 by 0.1 to 0.1 days] [06 After 08 by 0.1 to 0.1 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.Orientation unconstrained. Directly follows second three epsilon eridani orbits in order to minimize changes in telescope state.154339899000020.884552178857092(Tic-Visit
:proposal-id 15217
:visit-id "08"
:proposal-version -1
:trans-version "20181130"
:date "08-Dec-2018 22:57:42.0"
:trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 187856
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15217
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15217
:visit-id "08"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2846
:al-overhead-at-end 0
:internal-dur-at-end 367
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3145
:pcs-gap 0
)true11Exposure time of 0.1 second with ND3 filter gives SNR=345 and the time to saturation is 0.25, a 2.5x margin, acquition exposure time calculator run using Pickles K0IV star: http://etc.stsci.edu/etc/results/STIS.ta.1012385/