Status Report

NASA Hubble Space Telescope Daily Report # 3437

By SpaceRef Editor
September 2, 2003
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HUBBLE SPACE TELESCOPE

DAILY REPORT # 3437

PERIOD COVERED: DOY 240

OBSERVATIONS SCHEDULED

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 9984

Cosmic Shear With ACS Pure Parallels

Small distortions in the shapes of background galaxies by foreground
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_m0.5, 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.

ACS/HRC/WFC 9731

Kepler’s Supernova Remnant: an Imaging Study of the Blast Wave –
Circumstellar Medium Interaction

Kepler’s SNR {SN 1604 AD} is the prime example of a young Galactic SNR
where the blast wave is running into the wind of the progenitor star.
The interaction between the blast wave and the inhomogeneous
circumstellar medium gives rise to knots, evolving on a time scale of
years, that dominate the optical emission from the remnant. Also
visible in the optical are fainter Balmer line filaments that exhibit
a range of geometries – from normal sheet-like filaments to more
diffuse clumps of emission, the latter unique to this remnant. We
propose to image Kepler’s SNR through several narrowband filters using
ACS/WFC and WFPC2. The morphology and ionization structure of the
knots will be obtained from H-alpha, [S II], and [O III] images. We
will also obtain a [N II] image, which is known to be strong and
spatially variable in the remnant. The proposed H-alpha images will be
deep enough so that the physical scales and structure of the Balmer
dominated non-radiative shocks can be investigated. Our data will be a
critical part of multiwavelength studies of Kepler’s SNR. They will
complement Chandra and XMM X-ray data and VLA radio data, and provide
a significant advance in understanding the processes of magnetic field
amplification and cosmic ray acceleration in SNRs as well as the
evolution and dynamics of the blast wave – circumstellar medium
interaction.

ACS/WFC/HRC 9771

The local Hubble flow and the density field within 6 Mpc

Great progress has been made recently in accurate distance
measurements of nearby galaxies beyond the Local Group based on the
luminosity of the tip of the red giant branch {TRGB}. Over the last
three years, snapshot surveys with HST have provided us with the TRGB
distances for more than a hundred nearby galaxies obtained with an
accuracy of about 10%. The local velocity field within 5 Mpc exhibits
a significant anisotropy which disagrees with a spherical
Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms
deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter
can only realize such low dispersions with a combination of a low mean
density of matter and a substantial component with negative pressure.
There may be a constraint on the equation of state w=-p/rho. Our
observations will concentrate on 116 galaxies whose expected distances
lie within 4 – 6 Mpc, allowing us to trace a Dark Matter distribution
in the Local Volume with twice the information currently available.
The program is a good one for SNAP mode because the order and rate
that the observations are made are not very important, as long as
there is good completion over several years.

NIC1/NIC2/STIS/CCD/WFPC2 9738

Spectroscopy and Polarimetry of Mars at Closest Approach

We plan a coordinated program of spectroscopy, imaging, and
spectropolarimetry of Mars during the August 2003 opposition to study
the composition and physical state of surface materials and airborne
aerosols. The observations include {a} Moderate spectral resolution
290 to 570 nm STIS long-slit push-broom imaging spectroscopy of Mars,
to constrain the properties of airborne aerosol particles and to
search for and globally map iron-bearing minerals that are diagnostic
of specific past climatic conditions; {b} WFPC2 UV-VIS images designed
primarily to quantify the effects of ice and dust aerosols on our STIS
spectra; {c} NICMOS near-IR images to search for and globally map the
presence of hydrated surface minerals; and {d} ACS multispectral
polarizer images to provide critical phase function measurements
needed to constrain the physical properties of the Martian surface
layer. The observations are timed to take advantage of the closest
approach of Mars to Earth for the next several hundred years. Images
and spectra will be acquired at a spatial scale comparable to existing
spacecraft orbital spectroscopy data {~10 km/pixel} and in wavelength
regions not sampled by past or current Mars spacecraft
instrumentation. These observations also provide complementary
scientific and calibration measurements in support of current and
future NASA and ESA Mars exploration missions.

NICMOS 8791

NICMOS Post-SAA calibration – CR Persistence Part 2

A new procedure proposed to alleviate the CR-persistence problem of
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.

NICMOS 9636

Cycle 11 NICMOS dark current, shading profile, and read noise monitoring
program

The purpose of this proposal is to monitor the dark current, read
noise, and shading profile for all three NICMOS detectors throughout
the duration of Cycle 11. This proposal is a continuation of PID 9321
which covers the period between the end of SMOV3B and the onset of
Cycle 11.

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,
and 1×1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.

STIS 9633

STIS parallel archive proposal – Nearby Galaxies – Imaging and
Spectroscopy

Using parallel opportunities with STIS which were not allocated by the
TAC, we propose to obtain deep STIS imagery with both the Clear
{50CCD} and Long-Pass {F28X50LP} filters in order to make
color-magnitude diagrams and luminosity functions for nearby galaxies.
For local group galaxies, we also include G750L slitless spectroscopy
to search for e.g., Carbon stars, late M giants and S-type stars. This
survey will be useful to study the star formation histories, chemical
evolution, and distances to these galaxies. These data will be placed
immediately into the Hubble Data Archive.

STIS 9786

The Next Generation Spectral Library

We propose to continue the Cycle 10 snapshot program to produce a Next
Generation Spectral Library of 600 stars for use in modeling the
integrated light of galaxies and clusters. This program is using the
low dispersion UV and optical gratings of STIS. The library will be
roughly equally divided among four metallicities, very low {[Fe/H] lt
-1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and
super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in
each bin. Such a library will surpass all extant compilations and have
lasting archival value, well into the Next Generation Space Telescope
era. Because of the universal utility and community-broad nature of
this venture, we waive the entire proprietary period.

STIS/CCD 10000

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during cycle
12.

STIS/CCD/MA1 9724

Towards a global understanding of accretion physics – Clues from an UV
spectroscopic survey of cataclysmic variables

Accretion inflows and outflows are fundamental phenomena in a wide
variety of astrophysical environments, such as Young Stellar Objects,
galactic binaries, and AGN. Observationally, cataclysmic variables
{CVs} are particularly well suited for the study of accretion
processes. We are currently carrying out a Cycle 11 STIS UV
spectroscopic snapshot survey of CVs to fully exploit the diagnostic
potential of these objects for our understanding of accretion physics.
While the data obtained so far are of excellent quality, the number of
targets that will be observed in Cycle 11 is too small for a
statistically significant analysis {only 19 objects out of our 149
accepted Cycle 11 snapshot targets have been observed at the time of
writing}. We propose here to extend this survey into Cycle 12,
building a homogenous database of accretion disc and wind outflow
spectra covering a wide range of mass transfer rates and binary
inclinations. We will analyze these spectra with state-of-the-art
accretion disc model spectra {SYNDISK}, testing our current knowledge
of the accretion disc structure, and, thereby, providing new insight
into the so far not well understood process of viscous dissipation. We
will use our parameterised wind model PYTHON for the analysis of the
radiation driven accretion disc wind spectra, assessing the
fundamental question whether the mass loss rate correlates with the
disc luminosity. In addition, our survey data will identify a number
of systems in which the white dwarf significantly contributes to the
UV flux, permitting an analysis of the impact of mass accretion on the
evolution of these compact stars. This survey will triple the number
of currently available high-quality accretion disc / wind outflow /
accreting white dwarf spectra, and we waive our proprietary rights to
permit a timely use of this database.

WFPC2 9595

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3

This dark calibration program obtains 3 dark frames every day to
provide data for monitoring and characterizing the evolution of hot
pixels.

WFPC2 9709

POMS Test Proposal: WFII parallel archive proposal

This is the generic target version of the WFPC2 Archival Pure Parallel
program. The program will be used to take parallel images of random
areas of the sky, following the recommendations of the 2002 Parallels
Working Group.

WFPC2 9710

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.)

HSTAR 9130: GS Acquisition (2,3,2) @ 240/20:48:18Z
result GS. Under backup on F acquisition 8 for
8, FGS re-acquisitions 8 for 8, FHST updates 11 for 11, no LOLs.

SIGNIFICANT EVENTS:

Completed CCS Release 4.0.3/CCS Release 5.0.3 Online Data Archive
Compare testing 239/10:15Z 15:18Z. It was noted did not have any
telemetry data from previous tests in the real-time, recorder, and
merged areas with the same time frame on both strings. Plots were
pulled with different time frames but with the same mnemonic
(TDMMNFC). It was also noted that on the Sun String (D), the plots
and reports were running anywhere from 4 55 seconds quicker that on
the SGI String (B). Both strings were showing the same data on the
quick plots and reports.

Completed Command Timing testing 239/11:25Z 21:05Z using CCS C
String with CCS Release 4.0.3. All objectives were met, except for
one exception. TDRSS remains nominal, GSTDN remains nominal, JSC1
(single stage commanding) results were consistent with previous
testing, meaning that fluctuations in the EDRs continue to appear.
Fluctuations were in the 12 15 % range. JSC2 (two-stage commanding)
remains nominal, with the two runs that were performed. Parameters
UPLKVER, UPLKNVER, and PROP were changed as in previous testing in JSC
(ON1) and JSC(ON2) to the following: UPLKVER = 1.1, UPLKNVER = 1.6,
and PROP = 2.5. More detailed analysis of the results will take place
early next week.

Completed Engineering Data Products testing on Day 239 using CCS D
String with CCS Release 5.0.3. Historical requests were submitted on
D String. The data source specified was real-time because there
were no merged data available on the D String. Plots and reports
were generated for a 24-hour time span and compared against plots and
reports generated on the B String (CCS Release 4.0.3) for the same
time period. One difference was noted with the ESTR-2 telemetry
mnemonics due to the fact the ESTR-2 telemetry was active on B
String and inactive on D String. The comparison revealed no other
differences for either the plots or the reports. The processing time
was significantly faster on the D String. The reports and plots
were generated in approximately 5 7 minutes on D String and 16
19 minutes on the B String.

Completed CCS Release 4.0.3 SDH/HSTPS-SM Verification testing
240/11:00Z 16:10Z. Test was a success with one issue. The SDH/HSTPS
ingested various science dumps, both PN and non-PN encoded. During PN
& non-PN NSSC-1 Status Buffer dumps, CCS displayed an even error
message stating Bad line count received. Source ID=0. Received
value = 50 . After a re-cycle of the CCSPSS, the messages never
displayed again during a repeat of the dumps. TSAR 2593 was written
and the SOC will investigate.

Completed ANCC HSTUPS Software Release 14 testing 24013:30Z 18:10Z.
All test objectives were met and the test was successful. Able to
send new TDRS Support Request (additions) and Replacement Requests
(time adjustment of already defined supports).

SpaceRef staff editor.