0
Assigned ID: 910
----- Attempting Submission 1 (Fri Apr 10 22:05:22 GMT 2015) -----
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
* Visit 29: fixed wrong exposure labels (purely cosmetic), increased BUFFER-TIME of the G160M exposures to safeguard
against data loss, adjusted the exposure times to fit into the orbit, copied the correct ETC run ID into the
four G130M visits.
911473953
----- Attempting Submission 1 (Fri Jul 17 20:40:03 GMT 2015) -----
----- Attempting Submission 2 (Mon Jul 27 15:14:31 GMT 2015) -----
----- Attempting Submission 3 (Tue Jul 28 17:36:03 GMT 2015) -----
----- Attempting Submission 4 (Sat Sep 12 13:34:43 GMT 2015) -----
----- Attempting Submission 5 (Wed Nov 11 11:03:09 GMT 2015) -----
HST Phase II Proposal 14076 (14076.apt) successfully submitted.
Receipt: # 14076-5
----- Attempting Submission 6 (Wed Nov 11 11:25:18 GMT 2015) -----
----- Attempting Submission 7 (Mon Nov 16 15:12:57 GMT 2015) -----
----- Attempting Submission 8 (Mon Dec 21 16:38:17 GMT 2015) -----
----- Attempting Submission 9 (Wed Dec 23 17:20:14 GMT 2015) -----
For one of the COS visits, rather than using FP-POS, I use several central wavelengths to dither
in dispersion direction, which will do a similar job, and give seamless coverage.
An HST legacy ultraviolet spectroscopic survey of the 13pc white dwarf sample
Over 95% of all stars in the Galaxy will become white dwarfs, and this dominant population of stellar remnants plays a unique and central role for our understanding of the formation and evolution of stars, planetary systems, and the Galaxy itself. White dwarfs are fundamental for many areas of astrophysics, including post main-sequence mass loss, the local star formation history, the bulk composition of extra-solar planets, and the characterisation of dark energy.
Despite their fundamental importance for a wide range of astrophysical problems, our knowledge of the galactic white dwarf population is remarkably fragmentary: the only volume-limited and unbiased sample of white dwarfs contains 43 stars within d < 13 pc (of the Sun). This sample is dominated by cool and old stars, and an accurate determination of their temperatures, masses, and ages requires a detailed understanding of plasmas and convection at fluid-like densities.
Our team has carried out substantial theoretical and computational work on improved model atmospheres and all relevant input physics. The strongest effect of our new calculations on the emergent flux occurs at ultraviolet wavelengths, and we propose to obtain STIS and COS spectroscopy for all white dwarfs in the volume-limited 13pc sample to (1) test and calibrate our atmosphere models, which we will eventually apply to the ~200000 WDs discovered by Gaia, (2) turn the 13pc sample into the most accurate cosmic clocks reconstructing the local star formation history, and (3) probe in an unbiased way the frequency of rocky planet formation in the early ages of the Galaxy.
eThe aim of this proposal is to obtain HST STIS/COS spectra for all white dwarfs within 13pc that do not yet have high quality ultraviolet spectra. Many of these stars are cool, and are only detectable in the near-UV range with STIS/G230L. We use the 52x2 aperture to ensure the best spectrophotometric throughput. A small fraction is sufficiently hot to be observed with either COS/G140L, or COS/G130M/G160M. Where possible, we use the TIME-TAG mode.
A few targets need special considerations:
WD0727+482 (target #12, visit 13) is a white dwarf - white dwarf binary with a separation of 0.66".
This binary has been monitored for more than a decade with HST/FGS (PI Howard Bond), and we
would like to position both stars along the 52x2 long-slit, which needs a specific roll angle.
Four of our targets are part of wide common proper motion binaries / triples:
WD0208-501 = GJ86B (V=14): 2" separation from GJ86A (V=6.17, K0V) -> observed before with WFC3 and STIS/CCD. Offset acquisition necessary.
WD0413-077 = 40 Eri B (V=9.5): 80" separation from 40 Eri A (V=4.4, K0.5V), has a fainter M-dwarf component, 40 Eri C (V=11.17, M5V) -> may need roll angle to avoid diffraction spikes
WD0426+588 = Stein 2051B (V=12.44): 7.4" separation from Stein 2051A (V=11.08, M4V) -> separation sufficiently small that it may cause trouble for STIS target acq.
WD1132-325 = vB4 (V=15), ~5" separation from GJ432A (V=5.98, K0V) -> separation sufficiently small that it may cause trouble for STIS target acq.
These targets are numbered as >#100, and the assiociated visits are AA and beyond.
HOT STARS
0
false
true
false
false
SUPPORTED
STAR
DA
NO
J2000
GALEX NUV=17.36+/-0.03
STAR
DC
NO
J2000
GALEX NUV=18.87+/-0.07
STAR
DZ
NO
J2000
GALEX NUV=18.19+/-0.04
STAR
DA
NO
J2000
GALEX NUV=15.07+/-0.01
STAR
DA
NO
J2000
GALEX NUV=17.03+/-0.02
STAR
DA
NO
J2000
GALEX NUV=22.08+/-0.40
STAR
DA
NO
J2000
GALEX FUV=11.422+/-0.003 GALEX NUV=12.985+/-0.003
STAR
DC
NO
J2000
GALEX NUV=16.24+/-0.02
STAR
DC
NO
J2000
STAR
DZ
NO
J2000
STAR
DA
NO
J2000
STAR
DA
NO
J2000
STAR
DA
NO
J2000
GALEX NUV=18.96+/-0.08
STAR
DA
NO
J2000
GALEX NUV=22.07+/-0.42
STAR
DA
NO
J2000
F(1800A)=1e-13erg/cm2/s/A (IUE SWP17286)
STAR
DC
NO
J2000
GALEX FUV=18.98+/-0.02 GALEX NUV=16.096+/-0.004
STAR
DC
NO
J2000
F(2800A)=8e-14erg/cm2/s/A (IUE: LWP08043)
STAR
DA
NO
J2000
GALEX FUV=21.24+/-0.24 GALEX NUV=16.21+/-0.01
STAR
DC
NO
J2000
F(1800A)=8e-14erg/cm2/s/A (IUE: SWP50283)
STAR
DA
NO
J2000
GALEX FUV=18.32+/-0.08 GALEX NUV=14.181+/-0.005
STAR
DA
NO
J2000
GALEX NUV=21.27+/-0.10
STAR
DA
NO
J2000
GALEX NUV = 22.2+/-0.2
STAR
DA
NO
J2000
F(1280A)=3.5e-12/erg/cm2/s/A (HST: GHRS Z19Z010EM)
STAR
DA
NO
J2000
GALEX FUV=13.608+/-0.005 GALEX NUV=13.383+/-0.003
STAR
DC
NO
2015/11/16: updated the proper motions.
J2000
GALEX NUV = 18.61+/-0.05
STAR
DA
NO
J2000
GALEX FUV=14.025+/-0.009 GALEX NUV=13.560+/-0.005
STAR
DB
NO
2015/12/21: the coordinates were swapped with those of WD1917+386 (target 28)
J2000
GALEX FUV=15.04+/-0.01 GALEX NUV=13.393+/-0.004
STAR
DC
NO
2015/12/21: the coordinates were swapped with those of WD1917-077 (target 27)
J2000
STAR
DA
NO
J2000
GALEX FUV=20.68+/-0.19 GALEX NUV=15.43+/-0.01
STAR
DC
NO
J2000
GALEX FUV=19.6+/-0.15 GALEX NUV=14.88+/-0.01
STAR
DZ
NO
J2000
GALEX NUV=23.3+/-0.3
STAR
DZ
NO
J2000
GALEX FUV=18.767+/-0.007 GALEX NUV=14.414+/-0.0006
STAR
K V-IV
NO
This object was generated by the target selector and retrieved from the SIMBAD database.
HR637
HD13445
J2000
J2000
STAR
DC
Offset values based on Cycle 19 WFC3 images taken 31 March 2012, and extrapolated for orbital estimates based on MC simulations; J Farihi July 2015.
GJ86B
J2000
STAR
DA
NO
J2000
GALEX FUV=11.54+/-0.005 GALEX NUV=11.75+/-0.005
STAR
DC
NO
J2000
GALEX NUV=14.960+/-0.0008
STAR
DC
K V-IV
NO
HD100623
STAR
DC
NO
GJ432B
VB4
J2000
STIS/FUV-MAMA
Spectroscopic
No
No
E140H
1234
STIS/FUV-MAMA
Spectroscopic
No
No
E140H
1416
STIS/FUV-MAMA
Spectroscopic
No
No
E140H
1598
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
1763
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2013
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2263
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2513
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F814W
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F814W
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1577
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F814W
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1577
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
COS/FUV
Spectroscopic
No
No
G140L
1105
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
POS-TARG
DITHER
0.173
LINE
0.112
false
false
81.785
4
23.884
WFC3-UVIS-DITHER-BOX
1
false
POS-TARG
DITHER
0.567
LINE
0.567
false
false
143.130102
4
26.6
STIS-CCD-BOX
4
false
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 14076
:visit-id "01"
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(Tic-Obset
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3403
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
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:visit-id "02"
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:data-volume 365712
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(Tic-Obset
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(Tic-Orbit
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:si-vis-utilization 2889
:al-overhead-at-end 0
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:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3222
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true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
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:proposal-version -1
:trans-version "20150609"
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(Tic-Obset
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:pcs-mode "FGS"
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(Tic-Orbit
:proposal-id 14076
:visit-id "03"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2880
:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3213
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 14076
:visit-id "04"
:proposal-version -1
:trans-version "20150609"
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:number-of-orbits 2
:saa-model "31"
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(Tic-Obset
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(Tic-Orbit
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:dark-offset NIL
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)
(Tic-Orbit
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:orbit-number 2
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:si-vis-utilization 2991
:al-overhead-at-end 0
:internal-dur-at-end 388
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3213
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)
true
2
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
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:proposal-version -1
:trans-version "20150609"
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:data-volume 713632
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(Tic-Obset
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(Tic-Orbit
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:pcs-time 333
:si-vis-utilization 2877
:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3210
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 14076
:visit-id "06"
:proposal-version -1
:trans-version "20150609"
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
:saa-model "24"
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)
(Tic-Obset
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)
(Tic-Orbit
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:orbit-number 1
:pcs-time 333
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:al-overhead-at-end 0
:internal-dur-at-end 440
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3556
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
1444554373000
213.61971164008577
(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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)
true
2
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
11/11/2015: this visit was problematic because of the total number of buffer dumps. Given up on the TIME-TAG mode would impact the potential scientific return. The best choice seems to be to split the E140M and E230M observations into two separate visits, reducing the number of buffer dumps per visit, while keeping the TIME-TAG mode. This results in a small loss of on-target time, but given that this is a bright target, the loss in S/N is negligible. Visit 08 is now only the E140M observation, and the new visit 47 contains the E230M observations.
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11/11/2015: For the E140M observations in Visit 08, the ETC simulation gives a "countrate entire detector" of 11381, i.e. a buffer time of 175sec. The IUE spectrum of WD0310-688 (SWP15471) suggests that the WD model used for the ETC simulation overpredicts the flux by ~20%. Allowing an additional 20% safety margin ontop of the model prediction, we end with a BUFFER-TIME of 145sec, or a total of 20 buffer dumps in this visit, including the WAVECALs.
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
This is a close white dwarf + white dwarf binary, with a projected orbital separation of ~0.7", and a period of ~19 years. This binary is monitored with HST/FGS for more than a decade (PI Howard Bond). The aim of this visit should be observe both white dwarfs simultanesoulsy by acquiring the binary along the cross-dispersion direction on the 52x2 slit.
12 Sep 2015:
J. Farihi has updated the roll angle so that there is a good chance to get both stars on the STIS slit; Ed Nelan and Gail Schaefer have provided a detailed, month by month ephemeris for the binary over cycle 23. The only viable scheduling period is during a 10 day window in January(!).
ORIENT required to avoid diffraction spikes of primary. Target is expected at PA=335.9 deg on 2016 Jan 12 (middle of 10-day window), and thus optimal slit alignment is 335.9 deg, and U3 axis at 20.9 deg or 200.9 deg
11 Nov 2015: Removed "on hold" flag, as Jay already implemented the PA constraints.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
11/11/2015: changed label of the visit and exposures in the visit, as there was a typo in the WD number.
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This is a HOPR repeat of failed visit 19.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
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11/11/2015: The buffer time estimated from the ETC is ~120s, which is only 20% above the minimum buffer time for uninterrupted observations. I re-ran the ETC calculation, and check the available IUE spectra (LWR06454, LWR06455, LWP27752), which are consistent with the model used as ETC input, maybe even a few % lower. Thus, let's stick to the TIME-TAG mode, as we should have 20% headroom.
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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11/11/2015: The central wavelength of the second E230M observation was switched to 2707A. Exposure times were adjusted to free up ~180sec for an Auto-WAVECAL for the second
central wavelength.
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
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Had the wrong target (WD1917+386)
Had the wrong target (WD1917+386)
Had the wrong target (WD1917+386)
The scheduling data was generated by CASM 23.2.
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true
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To get a gap-free spectrum over the entire range covered by the G160M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G160M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G160M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G160M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G130M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G130M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G130M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
To get a gap-free spectrum over the entire range covered by the G130M grating, we use four different central wavelength, all with FP-POS=1 (instead of one central wavelength with four FP-POS settings, which would still leave a gap).
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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true
1
0
The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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true
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The scheduling data was generated by CASM 23.2.
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true
2
0
The scheduling data was generated by CASM 23.2.
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true
3
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
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true
1
0
The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
ORIENT required to avoid diffraction spikes of primary. Target is expected at PA=81.3 deg from primary and thus optimal slit alignment is -8.7 deg, and U3 axis at 36.3 deg or 216.3 deg.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
ORIENT required to avoid diffraction spikes of primary. Target is expected at PA=98.8 deg from primary and thus optimal slit alignment is 8.8 deg, and U3 axis at 53.8 deg or 233.8 deg.
11/11/2015: The central wavelength of the second E230M observation was switched to 2707A. Exposure times were adjusted to free up ~180sec for an Auto-WAVECAL for the second
central wavelength. Removed "on hold" flag, as the PA constraint is now implemented.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
11/11/2015: removed "on hold" flag, as John Subasavage confirmed that we are in good shape with the coordinates / proper motions for WD0426+588.
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The scheduling data was generated by CASM 23.2.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
ORIENT required to avoid target lying near diffraction spikes an bleeding columns of primary. Target is expected at PA=127.3 deg from primary, and thus optimal U3 alignment is (+221 deg) 348.3 deg or 168.3 deg.
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
ORIENT required to avoid diffraction spikes of primary. Target is expected at PA=127.3 deg from primary and thus optimal slit alignment is 37.3 deg, and U3 axis at 82.3 deg or 262.3 deg
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The scheduling data was generated by CASM 23.2.
CASM was run in Phase II mode.
11/11/2015: this is a new visit containing the E230M observations of WD0310-688, previously part of Visit 08, that were split off to keep the total number of buffer tumps per visit below 30.
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11/11/2015: E230M @ 1978A: the ETC simulation gives a "countrate entire detector" of 11972 cts/s, i.e. a buffer time of 167sec. The IUE spectrum of WD0310-688 (LWP11954) suggests that the WD model used for the ETC simulation overpredicts the flux by ~20%. Allowing an additional 20% safety margin ontop of the model prediction gives BUFFER-TIME=140sec.
11/11/2015: E230M @ 2707: as above. Total countrate=15571 cts/s => BUFFER-TIME=128sec, allowing for 20% margin, we adopt 108sec.