0
Assigned ID: 215
----- Attempting Submission 1 (Thu Apr 07 12:58:31 GMT 2016) -----
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/PEAKXD.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
ORBITAL VISIBILITY OVERRUN
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
Hi Amber,
I have (re)set the COS/G130M exposures to a 1291A central wavelength in the four repeat visits.
Boris
1177181546
----- Attempting Submission 1 (Thu Jul 21 22:03:32 GMT 2016) -----
----- Attempting Submission 2 (Sat Jul 23 18:20:59 GMT 2016) -----
----- Attempting Submission 3 (Wed Aug 10 19:13:41 GMT 2016) -----
----- Attempting Submission 4 (Mon Aug 15 12:14:58 GMT 2016) -----
----- Attempting Submission 5 (Mon Oct 03 11:08:00 GMT 2016) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 6 (Mon Jan 30 09:25:09 GMT 2017) -----
----- Attempting Submission 7 (Mon Feb 13 22:07:08 GMT 2017) -----
Your proposal could not be saved.
Submission aborted.
Your proposal could not be saved.
Submission aborted.
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 8 (Fri Apr 14 15:55:30 GMT 2017) -----
Regarding any coordinate accuracy warnings, we have done > 100 COS visits with catalog-informed coordinates + proper motions,
which proved to be good enough that we don't need an ACQ/SEARCH.
The new APT version complains about a few visibility overruns, of a few seconds . I didn't fix those for now,
as they were fine previously - OK?
An Ultraviolet Spectral Legacy of Polluted White Dwarfs
Polluted white dwarfs represent the best path to empirically measure the bulk chemical compositions and limiting masses of extrasolar planetesimals. A wealth of data now firmly link metal-enriched white dwarfs with circumstellar debris that derives from rocky planetary building blocks or fragments of larger parent bodies.
Ultraviolet spectroscopy is the only way to detect critical elements such as carbon and oxygen, and the small handful of stars studied in this way have yielded spectacular results. Our recent HST successes demonstrate the power of this technique, and we wish to take the next logical step with a large survey.
In the same way that planetary scientists utilize diverse meteorite classes to understand the formation and composition of the terrestrial planets, we need a statistical census of extrasolar planetesimal compositions to fully understand their physical and chemical role as exoplanet precursors. A large (N ~ 40) dataset of detailed metal abundances in polluted white dwarfs is essential to our understanding of the assembly and chemistry of Earth-like exoplanets.
We propose to observe a brightness-limited sample of metal-rich white dwarfs, by selecting 31 targets that can be observed in a single COS / STIS visit, and thereby making the most efficient use of HST time for any sample of this size. This will increase the number of polluted white dwarfs observed in the far ultraviolet by a factor of five, and thereby perform the most robust and statistically meaningful study that is currently possible.
This is a legacy that HST should leave to future planet formation modelers and cosmochemists, and it requires the ultraviolet capacity of HST.
We will obtain far-ultraviolet spectroscopy of 27 metal-polluted white dwarfs, with the aim to measure photospheric abundances, and infer the bulk composition of exo-planetesimals. The bulk of the observations will be done with COS/G130M, with a few targets done with STIS/E140M.
We have compiled the most accurate effective temperatures and surface gravities from the literature, computed model spectra for each star, and scaled the model spectra to match the GALEX NUV/FUV fluxes. These scaled models were then used for all ETC simulations, paying particular attention to any possible violations of the bright object limits. BOP does flag up a few possible problems, but those are related to the fact that BOP assumes a steeper O5V spectrum.
We used APOP and PPMXL to obtain coordinates and proper motions. We have gathered extensive experience from > 100 COS observations that these coordinates are sufficiently accurate that we can skip the ACCUM/SEARCH pattern during the acquisition.
Following the Phase I time allocation, we have slightly revised our target list based on more detailed simulations, which results in the removal of the following Phase I targets:
WD0408-041
WD0415-105
WD1011+570
WD1150-153
WD1350-162
WD1709+230
WD2144-079
WD2229+235
WD2253+803
The reason for withdrawing these targets is that either updated temperature measurements make them less likely to produce high-quality data, or that deeper exposures compared to previous COS observations would have less impact due to the decreasing COS sensitivity. We have (a) increased the exposure time for a few of the remaining targets, and (b) added the following fivenew targets
WD0106-358
WD0437+138
WD0536-479
WD0842+572
WD1644+198
Extrasolar Planets and Planet Formation
Stellar Physics
6
false
true
false
false
false
false
AVAILABLE
STAR
DA
NO
Teff=16600K
HS0047+1903
J2000
GALEX FUV=1990microJy GALEX NUV=1780microJy
STAR
DA
NO
Teff=15700K
HE0106-3253
J2000
GALEX FUV=3050microJy GALEX NUV=2750microJy
STAR
DA
NO
Teff=29000K
GD683
J2000
GALEX FUV=26633microJy GALEX NUV=13767microJy (these values are corrected for the non-linearity)
STAR
DB
NO
Teff=18700K
HE0110-5630
J2000
GALEX FUV=2190microJy GALEX NUV=2670microJy
STAR
DB
NO
Teff=16600K
G274-39
J2000
GALEX FUV=1880microJy GALEX NUV=3070microJy
STAR
DA
NO
Teff=13500K
PG
J2000
GALEX FUV=1450microJy GALEX NUV=1790microJy
STAR
DB
NO
Teff=15120K
LP475-242
J2000
GALEX FUV=2440microJy GALEX NUV=4176microJy
STAR
DA
NO
Teff=22810K
EC05365-4749
J2000
GALEX FUV=6180microJy GALEX NUV=4129microJy
STAR
DA
NO
Teff=18000K
SDSSJ084602.45+570328.5
J2000
GALEX FUV=854microJy GALEX NUV=825microJy
STAR
DA
NO
Teff=22400K
PG
J2000
GALEX FUV=2330microJy GALEX NUV=1780microJy
STAR
DB
NO
Teff=14900K
GD128
J2000
GALEX FUV=950microJy GALEX NUV=1740microJy
STAR
DA
NO
Teff=23000K
SDSSJ114404.74+052951.6
J2000
GALEX FUV=880microJy GALEX NUV=640microJy
STAR
DA
NO
Teff=20400K STIS not COS
G238-44
J2000
GALEX FUV=33700microJy GALEX NUV=35000microJy
STAR
DB
NO
Teff=18200K
HE1349-2305
J2000
GALEX FUV=880microJy GALEX NUV=1160microJy
STAR
DB
NO
Teff=14000K
PG
J2000
GALEX FUV=0microJy GALEX NUV=1570microJy
STAR
DA
NO
Teff=21450K
PG
J2000
GALEX FUV=0microJy GALEX NUV=0microJy
STAR
DB
NO
Teff=20800K
SDSSJ153725.71+515126.9
J2000
GALEX FUV=650microJy GALEX NUV=730microJy
STAR
DA
NO
Teff=22800K
SDSSJ155720.77+091624.6
J2000
GALEX FUV=220microJy GALEX NUV=190microJy
STAR
DA
NO
Teff=17400K
PG
J2000
GALEX FUV=3430microJy GALEX NUV=2840microJy
STAR
DB
NO
Teff=15190K
PG1644+199
J2000
GALEX FUV=2004microJy GALEX NUV=3330microJy
STAR
DA
NO
Teff=20000K STIS not COS
G186-31
J2000
GALEX FUV=0microJy GALEX NUV=24200microJy
STAR
DA
NO
Teff=13200K
HS2132+0941
J2000
GALEX FUV=950microJy GALEX NUV=1170microJy
STAR
DA
NO
Teff=17300K STIS not COS
G93-48
J2000
GALEX FUV=2450microJy GALEX NUV=30500microJy
STAR
DB
NO
Teff=15200K
EGGR906
J2000
GALEX FUV=830microJy GALEX NUV=1510microJy
STAR
DA
NO
Teff=20300K
GD237
J2000
GALEX FUV=2930microJy GALEX NUV=2450microJy
STAR
DB
NO
Teff=19000K
PG
J2000
GALEX FUV=2750microJy GALEX NUV=3000microJy
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
The scheduling data was generated by CASM 25.0.
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false
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The scheduling data was generated by CASM 25.0.
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Repeat of Visit 08, with the central wavelength at 1291A instead of 1327A.
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The scheduling data was generated by CASM 25.0.
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The scheduling data was generated by CASM 25.0.
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The scheduling data was generated by CASM 25.0.
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The scheduling data was generated by CASM 25.0.
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The scheduling data was generated by CASM 25.0.
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3
0
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false
1
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This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
The scheduling data was generated by CASM 25.0.
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Repeat of Visit 17, with the central wavelength at 1291A instead of 1327A.
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false
1
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This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
This target has no GALEX fluxes, we rely on the WD model predictions for the UV, which are way below any safety threshold.
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false
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The scheduling data was generated by CASM 25.0.
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The scheduling data was generated by CASM 25.0.
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false
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The scheduling data was generated by CASM 25.0.
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false
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false
1
1
The scheduling data was generated by CASM 25.0.
CASM was run in Phase II mode.
Repeat of Visit Y7, with the central wavelength at 1291A instead of 1327A.
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false
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