NASA Hubble Space Telescope Daily Report # 3452
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3452
PERIOD COVERED: DOY 265
OBSERVATIONS SCHEDULED
ACS 9658
ACS Earth Flats
This program will obtain sequences of flat field images by observing
the bright Earth. Several UV filters from the interim calibration
program {9564} require additional exposures to obtain the required
illumination. A few UV filters from this program will be repeated to
monitor for changes in the flat fields and to verify the interim
results. Since no streaks are observed in the UV, the wavelength
coverage is extended to longer wavelengths in order to explore the
severity of streaks in the flats from clouds in the FOV. We have added
exposures for the HRC in the visible filters to verify the results
derived from the L-flat campaign and to explore the severity of
streaks. We have also added exposures on WFC using the minimum
exposure time and using filters which will not saturate the brightest
WFC pixel by more than 10 times the full well.
ACS 9675
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
development of hot pixels and test for any source of noise in ACS CCD
detectors. This programme will be executed once a day for the entire
lifetime of ACS.
ACS 9760
ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at
z = 1.5
We are presently carrying out the deepest redshift survey ever
ACS 9984
Cosmic Shear With ACS Pure Parallels
Small distortions in the shapes of background galaxies by foreground
ACS/HRC/WFC 9793
The Grism-ACS Program for Extragalactic Science {GRAPES}
We propose an ACS grism spectroscopic survey with a wide component and
ACS/WFC 10055
ACS Polarization Calibration
This proposal aims to address several specific issues for the
NIC/NIC3 9865
The NICMOS Parallel Observing Program
We propose to continue managing the NICMOS pure parallel program.
NIC1/NIC2/NIC3 8792
NICMOS Post-SAA calibration – CR Persistence Part 3
A new procedure proposed to alleviate the CR-persistence problem of
NIC2 9801
Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey
Essentially all well-characterized preplanetary nebulae {PPNe}–
STIS 9606
CCD Dark Monitor-Part 2
Monitor the darks for the STIS CCD.
STIS 9608
CCD Bias Monitor – Part 2
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1,
STIS 9615
Cycle 11 MAMA Dark Monitor
This test performs the routine monitoring of the MAMA detector dark
STIS 9973
Intensive Coverage of the Eta Carinae Event in 2003
For a variety of reasons, HST can provide a very special and unique
STIS/CCD 10000
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during
STIS/CCD 10025
STIS CCD Spectroscopic Dispersion Monitor
Obtain a wavecal deep enough to constrain wavelength and spatial
WFPC2 9589
WFPC2 Decontaminations and Associated Observations Pt. 1/3
This proposal is for the monthly WFPC2 decons. Also included are
WFPC2 9595
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3
This dark calibration program obtains 3 dark frames every day to
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
COMPLETED OPS REQs:NONE
OPS NOTES EXECUTED:
911-0 Limit Management During WFPCII Decontamination (M001) @ 265/23:32z
SIGNIFICANT EVENTS:
Completed SM-4 Aft Flight Deck Telemetry Test, Dry Run # 2 265/11:00Z
undertaken {the Gemini Deep Deep Survey}. Spectra of extraordinary
quality have been taken in order to obtain redshifts in the so-called
“redshift desert” at 1
mass provide a powerful method of directly measuring the amount and
distribution of dark matter. Several groups have recently detected
this weak lensing by large-scale structure, also called cosmic shear.
The high resolution and sensitivity of HST/ACS provide a unique
opportunity to measure cosmic shear accurately on small scales. Using
260 parallel orbits in Sloan textiti {F775W} we will measure for the
first time: beginlistosetlength sep0cm setlengthemsep0cm setlength
opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the
skewness of the shear distribution, and em the magnification effect.
endlist Our measurements will determine the amplitude of the mass
power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20,
and the mass density Omega_m with s/n=4. They will be done at small
angular scales where non-linear effects dominate the power spectrum,
providing a test of the gravitational instability paradigm for
structure formation. Measurements on these scales are not possible
from the ground, because of the systematic effects induced by PSF
smearing from seeing. Having many independent lines of sight reduces
the uncertainty due to cosmic variance, making parallel observations
ideal.
an ultradeep single ACS field. The wide component covers the
well-imaged GOODS Chandra Deep Field south and the deepest field will
be the Ultra Deep field to be observed in cycles 11 and 12. The Grism
ACS Program for Extra-galactic Science {GRAPES} will: {1} Probe the
reionization epoch by robustly determining the luminosity function of
Lyman-alpha emitters, Lyman break galaxies and low luminosity AGNs at
z~6, and thus the sources of ionizing photons at the end of the “dark
ages”. A similar census of ionizing photon sources at z=4-6 needed to
maintain the ionized state of the IGM will also be achieved. {2} Study
galaxy formation and evolution by finding galaxies in a contiguous
redshift range between z=4-7 and evolution of black holes through a
census of low-luminosity AGNs. {3} Study star-formation and galaxy
assembly at its peak at z=1-2 by identifying star-forming galaxies by
their emission lines, old galaxies by the 4000 AA break and any
combination of new and old populations showing both lines and breaks.
{4} Allow the deepest unbiased spectroscopy yet, for identification of
objects to I=27. {5} Enhance the value of multiwavelength data in the
UDF and GOODS field to the astronomical community.
polarization calibration: {1} variations in calibration with position
on the detector {field dependence}, {2} dependence on telescope
roll-angle relative to the target, {3} orientation of the polarizer
axes, and {4} geometric distortion contributed by the polarizers.
Based on our experience, we are well prepared to make optimal use of
the parallel opportunities. The improved sensitivity and efficiency of
our observations will substantially increase the number of
line-emitting galaxies detected. As our previous work has
demonstrated, the most frequently detected line is Halpha at
0.7
NICMOS. Dark frames will be obtained immediately upon exiting the SAA
contour 23, and every time a NICMOS exposure is scheduled within 50
minutes of coming out of the SAA. The darks will be obtained in
parallel in all three NICMOS Cameras. The POST-SAA darks will be
non-standard reference files available to users with a USEAFTER
date/time mark. The keyword ‘USEAFTER=date/time’ will also be added to
the header of each POST-SAA DARK frame. The keyword must be populated
with the time, in addition to the date, because HST crosses the SAA ~8
times per day so each POST-SAA DARK will need to have the appropriate
time specified, for users to identify the ones they need. Both the raw
and processed images will be archived as POST-SAA DARKSs. Generally we
expect that all NICMOS science/calibration observations started within
50 minutes of leaving an SAA will need such maps to remove the CR
persistence from the science images. Each observation will need its
own CRMAP, as different SAA passages leave different imprints on the
NICMOS detectors.
objects in transition between the AGB and planetary nebula
evolutionary phases – are bipolar, whereas the mass-loss envelopes of
AGB stars are strikingly spherical. In order to understand the
processes leading to bipolar mass-ejection, we need to know at what
stage of stellar evolution does bipolarity in the mass-loss first
manifest itself. We have recently hypothesized that most OH/IR stars
{evolved mass- losing stars with OH maser emission} are very young
PPNe. We are conducting a multiwavelength survey program of imaging
and spectroscopic observations of such objects, using a large,
morphologically unbiased sample selected using IRAS 12-to-25 micron
colors. Our ongoing HST/SNAP imaging survey of the optically bright
half of this sample with WFPC2 and ACS is highly successful: 19/32
objects observed are extended with bipolar/multipolar shapes
{remaining objects are unresolved}. Slightly more than 50% of our
sample are optically too faint or undetected but have strong near-IR
counterparts — we therefore propose a NICMOS SNAPshot imaging survey
of these optically-faint OH/IR stars. These observations are crucial
for determining how and when the bipolar geometry asserts itself. The
results from our NICMOS survey {together with the WFPC2/ACS survey}
will allow us to draw general conclusions about the onset of bipolar
mass-ejection during late stellar evolution. Our complementary program
of interferometric mapping of the OH maser emission in our sources is
yielding kinematic information with spatial resolution comparable to
that in the HST images. The HST/radio data will provide crucial input
for theories of post-AGB stellar evolution. In addition, these data
will also indicate whether the multiple concentric rings, “searchlight
beams”, and truncated equatorial disks recently discovered with HST
in a few PPNe, are common or rare phenomena.
and 1×1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.
noise. This proposal will provide the primary means of checking on
health of the MAMA detectors systems through frequent monitoring of
the background count rate. The purpose is to look for evidence of
change in dark indicative of detector problem developing.
data set when Eta Car experiences its next spectroscopic event in
mid-2003. Explaining the phenomenon is only part of the motivation.
This star and its ejecta have unique characteristics that make them
important for several branches of astrophysics; and when a
spectroscopic event occurs, it’s like varying the parameters in an
experiment {or rather, set of experiments}. The 2003 event may be the
only chance in the forseeable future to obtain such a data set,
especially with HST. Eta Carinae has extreme parameters; it is
mysterious in surprisingly basic ways; and HST/STIS can gather useful
data on it at a terrific rate. As we explain below, the proposed data
set will be valuable in several independent ways: It will help solve a
specific set of current problems, it will constitute a large and
unique archival data base for both stellar and nebular astrophysics,
and it will be well-suited for educational uses.
cycle 12.
distortion maps without overusing the calibration lamp – to supplement
the Cycle 11 9617 program.
instrument monitors tied to decons: photometric stability check, focus
monitor, pre- and post-decon internals {bias, intflats, kspots, &
darks}, UV throughput check, VISFLAT sweep, and internal UV flat
check.
provide data for monitoring and characterizing the evolution of hot
pixels.
reports of potential non-nominal performance that will be
investigated.)
911-0 Limit Management During WFPCII Decontamination (M001) @ 265/13:52z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 07 07
FGS REacq 05 05
FHST Update 15 15
LOSS of LOCK
– 18:30Z using CCS “B” String with CCS Release 4.0.3 and PRD S07200.
Data source was PSS in Building 25 with Release 3.2.9.1. Testing was
not successful in verifying the SOC scenario files. Mnemonics DDIU2REQ
and DDIU5REQ could not be set in the simulator database to be
automated when transitioning between TN and D/E formats. These
mnemonics need to be set for the battery pressures to display the
correct calibration curves. However, the test went very smoothly and
all scenario files were executed correctly with only this one
exception.
