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#45844
Wed 02 Sep 2009 01:35:PM
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Joined: Feb 2001
Posts: 381,903
Launch Director
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OP
Launch Director
Joined: Feb 2001
Posts: 381,903 |
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #4922
PERIOD COVERED: 5am September 1 - 5am September 2, 2009 (DOY 244/09:00z-245/09:00z)
OBSERVATIONS SCHEDULED
ACS/WFC3 11882
CCD Hot Pixel Annealing
All the data for this program is acquired using internal targets (lamps)
only, so all of the exposures should be taken during Earth occultation
time (but not during SAA passages). This program emulates the ACS
pre-flight ground calibration and post-launch SMOV testing (program
8948), so that results from each epoch can be directly compared.
Extended Pixel Edge Response (EPER) and First Pixel Response (FPR) data
will be obtained over a range of signal levels for the Wide Field
Channel (WFC). The High Resolution Channel (HRC) visits have been
removed since it could not be repaired during SM4.
COS/FUV 11488
Internal FUV Wavelength Verification
This program will be executed after the uplink of the OSM1 position
updates derived from the determination of the wavelength-scale zero
points and desired spectral ranges for each grating in Activity COS29
(Program 11487 - COS FUV Internal/External Wavelength Scales). This
program will verify that the operational spectral ranges for each
grating, central wavelength, and FP-POS are those desired. Subsequent to
a successful verification, COS FUV ERO observations that require
accurate wavelength scales (if any) and FUV science can be enabled. An
internal wavelength calibration spectrum using the default PtNe lamp
(lamp 1) with each FUV grating at each central wavelength setting and
each FP-POS position will be obtained for the verification. Additional
exposures and waits between certain exposures will be required to avoid
- and to evaluate - mechanism drifts.
COS/FUV 11491
COS FUV External Flat Fields
Obtain external spectra of flat field targets at different positions
along the cross- dispersion direction of the FUV detector (and at a
variety of FP-POS positions) in order to obtain an FUV flat field. The
choices of gratings and positions of the target in the aperture have
been made in order to maximize the coverage on the detector in the
cross-dispersion direction and cover the entire region where science
spectra will fall.
COS/FUV 11897
FUV Spectroscopic Sensitivity Monitoring
The purpose of this proposal is to monitor sensitivity in each FUV
grating mode to detect any changes due to contamination or other causes.
COS/NUV 11896
NUV Spectroscopic Sensitivity Monitoring
The purpose of this proposal is to monitor sensitivity of each NUV
grating mode to detect any changes due to contamination or other causes.
FGS 11706
The Parallax of the Planet Host Star XO-3
We will use HST+FGS to measure the parallax of the transiting planet
host star XO 3. The resulting accurate distance measurement will provide
the most accurate radius determination to date for this massive
extrasolar planet (XO-3B), allowing us to critically test current giant
extrasolar planet structure models. These observations will also
constrain the amount of heating that may be produced inside XO-3B by
tides raised on the planet as it moves through its 3.2 d-eccentric (e ~
0.22) orbit.
FGS 11788
The Architecture of Exoplanetary Systems
Are all planetary systems coplanar? Concordance cosmogony makes that
prediction. It is, however, a prediction of extrasolar planetary system
architecture as yet untested by direct observation for main sequence
stars other than the Sun. To provide such a test, we propose to carry
out FGS astrometric studies on four stars hosting seven companions. Our
understanding of the planet formation process will grow as we match not
only system architecture, but formed planet mass and true distance from
the primary with host star characteristics for a wide variety of host
stars and exoplanet masses.
We propose that a series of FGS astrometric observations with
demonstrated 1 millisecond of arc per-observation precision can
establish the degree of coplanarity and component true masses for four
extrasolar systems: HD 202206 (brown dwarf+planet); HD 128311
(planet+planet), HD 160691 = mu Arae (planet+planet), and HD 222404AB =
gamma Cephei (planet+star). In each case the companion is identified as
such by assuming that the minimum mass is the actual mass. For the last
target, a known stellar binary system, the companion orbit is stable
only if coplanar with the AB binary orbit.
FGS 11789
An Astrometric Calibration of Population II Distance Indicators
In 2002, HST produced a highly precise parallax for RR Lyrae. That
measurement resulted in an absolute magnitude, M(V)= 0.61+/-0.11, a
useful result, judged by the over ten refereed citations each year
since. It is, however, unsatisfactory to have the direct,
parallax-based, distance scale of Population II variables based on a
single star. We propose, therefore, to obtain the parallaxes of four
additional RR Lyrae stars and two Population II Cepheids, or W Vir
stars. The Population II Cepheids lie with the RR Lyrae stars on a
common K-band Period-Luminosity relation. Using these parallaxes to
inform that relationship, we anticipate a zero-point error of 0.04
magnitude. This result should greatly strengthen confidence in the
Population II distance scale and increase our understanding of RR Lyrae
star and Pop. II Cepheid astrophysics.
STIS/CCD 11843
STIS CCD Performance Monitor
This activity measures the baseline performance and commandability of
the CCD subsystem. Only primary amplifier D is used. Bias and Flatfield
exposures are taken in order to measure bias level, read noise, CTE, and
gain. Numerous bias frames are taken to permit construction of
"superbias" frames in which the effects of read noise have been rendered
negligible. Full frame and binned observations are made, with binning
factors of 2 x 1, 1 x 2, 2 x 2. Bias frames are taken in subarray
readouts to check the bias level for ACQ and ACQ/PEAK observations. All
exposures are internals.
STIS/CCD 11844
CCD Dark Monitor Part 1
Monitor the darks for the STIS CCD.
STIS/CCD 11846
CCD Bias Monitor-Part 1
Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,
and 1x1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.
STIS/CCD 11850
CCD Sparse Field CTE Internal
CTE measurements are made using the "internal sparse field test", along
the parallel axis. The "Pos=" optional parameter, introduced during
Cycle 11, is used to provide off- center MSM positionings of some slits.
All exposures are internals.
STIS/CCD 11852
STIS CCD Spectroscopic Flats C17
Obtain pixel-to-pixel lamp flat fields for the STIS CCD in spectroscopic
mode.
STIS20 11402
STIS-20 NUV MAMA Dark Monitor
The STIS NUV-MAMA dark current is dominated by a phosphorescent glow
from the detector window. Meta-stable states in this window are
populated by cosmic ray impacts, which, days later, can be thermally
excited to an unstable state from which they decay, emitting a UV
photon. The equilibrium population of these meta-stable states is larger
at lower temperatures; so warming up the detector from its cold safing
will lead to a large, but temporary, increase in the dark current.
To monitor the decay of this glow, and to determine the equilibrium dark
current for Cycle 17, four 1380s NUV-MAMA ACCUM mode darks should be
taken each week during the SMOV period. Once the observed dark current
has reached an approximate equilibrium with the mean detector
temperature, the frequency of this monitor can be reduced to one pair of
darks per week.
WFC3/ACS/IR 11563
Galaxies at z~7-10 in the Reionization Epoch: Luminosity Functions to
<0.2L* from Deep IR Imaging of the HUDF and HUDF05 Fields
The first generations of galaxies were assembled around redshifts
z~7-10+, just 500-800 Myr after recombination, in the heart of the
reionization of the universe. We know very little about galaxies in this
period. Despite great effort with HST and other telescopes, less than
~15 galaxies have been reliably detected so far at z>7, contrasting with
the ~1000 galaxies detected to date at z~6, just 200-400 Myr later, near
the end of the reionization epoch. WFC3 IR can dramatically change this
situation, enabling derivation of the galaxy luminosity function and its
shape at z~7-8 to well below L*, measurement of the UV luminosity
density at z~7-8 and z~8-9, and estimates of the contribution of
galaxies to reionization at these epochs, as well as characterization of
their properties (sizes, structure, colors). A quantitative leap in our
understanding of early galaxies, and the timescales of their buildup,
requires a total sample of ~100 galaxies at z~7-8 to ~29 AB mag. We can
achieve this with 192 WFC3 IR orbits on three disjoint fields
(minimizing cosmic variance): the HUDF and the two nearby deep fields of
the HUDF05. Our program uses three WFC3 IR filters, and leverages over
600 orbits of existing ACS data, to identify, with low contamination, a
large sample of over 100 objects at z~7-8, a very useful sample of ~23
at z~8-9, and limits at z~10. By careful placement of the WFC3 IR and
parallel ACS pointings, we also enhance the optical ACS imaging on the
HUDF and a HUDF05 field. We stress (1) the need to go deep, which is
paramount to define L*, the shape, and the slope alpha of the luminosity
function (LF) at these high redshifts; and (2) the far superior
performance of our strategy, compared with the use of strong lensing
clusters, in detecting significant samples of faint z~7-8 galaxies to
derive their luminosity function and UV ionizing flux. Our recent z~7.4
NICMOS results show that wide-area IR surveys, even of GOODS-like depth,
simply do not reach faint enough at z~7-9 to meet the LF and UV flux
objectives. In the spirit of the HDF and the HUDF, we will waive any
proprietary period, and will also deliver the reduced data to STScI. The
proposed data will provide a Legacy resource of great value for a wide
range of archival science investigations of galaxies at redshifts z~2-9.
The data are likely to remain the deepest IR/optical images until JWST
is launched, and will provide sources for spectroscopic followup by
JWST, ALMA and EVLA.
WFC3/IR 11915
IR Internal Flat Fields
This program is the same as 11433 (SMOV) and depends on the completion
of the IR initial alignment (Program 11425). This version contains three
instances of 37 internal orbits: to be scheduled early, middle, and near
the end of Cycle 17, in order to use the entire 110-orbit allocation.
In this test, we will study the stability and structure of the IR
channel flat field images through all filter elements in the WFC3-IR
channel. Flats will be monitored, i.e. to capture any temporal trends in
the flat fields and delta flats produced. High signal observations will
provide a map of the pixel-to-pixel flat field structure, as well as
identify the positions of any dust particles.
WFC3/IR/S/C 11929
IR Dark Current Monitor
Analyses of ground test data showed that dark current signals are more
reliably removed from science data using darks taken with the same
exposure sequences as the science data, than with a single dark current
image scaled by desired exposure time. Therefore, dark current images
must be collected using all sample sequences that will be used in
science observations. These observations will be used to monitor changes
in the dark current of the WFC3-IR channel on a day-to-day basis, and to
build calibration dark current ramps for each of the sample sequences to
be used by GOs in Cycle 17. For each sample sequence/array size
combination, a median ramp will be created and delivered to the
calibration database system (CDBS).
WFC3/UVIS 11714
Snapshot Survey for Planetary Nebulae in Local Group Globular Clusters
Planetary nebulae (PNe) in globular clusters (GCs) raise a number of
interesting issues related to stellar and galactic evolution. The number
of PNe known in Milky Way GCs, four, is surprisingly low if one assumes
that all stars pass through a PN stage. However, it is likely that the
remnants of stars now evolving in galactic GCs leave the AGB so slowly
that any ejected nebula dissipates long before the star becomes hot
enough to ionize it. Thus there should not be ANY Pne in Milky Way
GCs--but there are four! It has been suggested that these Pne are the
result of mergers of binary stars within GCs, i.e., that they are
descendants of blue stragglers. The frequency of occurrence of Pne in
external galaxies poses more questions, because it shows a range of
almost an order of magnitude.
I propose a Snapshot survey aimed at discovering Pne in the GC systems
of Local Group galaxies outside the Milky Way. These clusters, some of
which may be much younger than their counterparts in our galaxy, might
contain many more Pne than those of our own galaxy. I will use the
standard technique of emission-line and continuum imaging, which easily
discloses Pne. This proposal continues a WFPC2 program started in Cycle
16, but with the more powerful WFC3. As a by-product, the survey will
also produce color-magnitude diagrams for numerous clusters for the
first time, reaching down to the horizontal branch.
WFC3/UVIS 11905
WFC3 UVIS CCD Daily Monitor
The behavior of the WFC3 UVIS CCD will be monitored daily with a set of
full-frame, four-amp bias and dark frames. A smaller set of 2Kx4K
subarray biases are acquired at less frequent intervals throughout the
cycle to support subarray science observations. The internals from this
proposal, along with those from the anneal procedure (11909), will be
used to generate the necessary superbias and superdark reference files
for the calibration pipeline (CDBS).
WFC3/UVIS 11908
Cycle 17: UVIS Bowtie Monitor
Ground testing revealed an intermittent hysteresis type effect in the
UVIS detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially found via an unexpected bowtie-shaped feature in flatfield
ratios, subsequent lab tests on similar e2v devices have since shown
that it is also present as simply an overall offset across the entire
CCD, i.e., a QE offset without any discernable pattern. These lab tests
have further revealed that overexposing the detector to count levels
several times full well fills the traps and effectively neutralizes the
bowtie. Each visit in this proposal acquires a set of three 3x3 binned
internal flatfields: the first unsaturated image will be used to detect
any bowtie, the second, highly exposed image will neutralize the bowtie
if it is present, and the final image will allow for verification that
the bowtie is gone.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
of potential non-nominal performance that will be investigated.)
HSTARS:
12001 - GSAcq 1,2,1 scheduled from 244/21:59:48 - 244/22:06:30, failed due to
Search Radius Limit Exceeded on FGS-1.
Observations affected: COS 40 & 41 Proposal ID# 11897,
WFC3 22 proposal ID# 11908.
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 8 7
FGS REAcq 5 5
OBAD with Maneuver 8 8
SIGNIFICANT EVENTS: (None)
David Cottle
UBB Owner & Administrator
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