Status Report

NASA Hubble Space Telescope Daily Report # 3547

By SpaceRef Editor
February 9, 2004
Filed under , ,

HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science




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_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

FGS 9969

FGS Astrometry of the Extrasolar Planet of Epsilon Eridani

We propose observations with HST/FGS in Position Mode to determine the
astrometric elements {perturbation orbit semimajor axis and
inclination} of the candidate extra-solar planet around the K2 V star
Epsilon Eridani that has been detected by Doppler spectroscopy. These
observations will also permit us to determine the actual mass of the
planet by providing the sin{i} factor which can not be determined with
the radial velocity method. High precision radial velocity {RV}
measurements spanning the years 1980.8–2000.0 for the nearby {3.22
pc} star Epsilon Eri show convincing variations with a period of ~ 7
yrs. These data represent a combination of six independent data sets
taken with four different telescopes. A least squares orbital solution
using robust estimation yields orbital parameters of period, P = 6.9
yrs, velocity K- amplitude = 19 m/s, eccentricity e = 0.6, projected
companion mass M_B sin{i} = 0.83 M_Jupiter. An estimate of the
inclination yields a perturbation semi-major axis, Alpha = 0arcs0022,
easily within the reach of HST/FGS astrometry.

ACS/WFC 9902

The Evolution of the Host Galaxies of Radio-Quiet Quasars

Study of the host galaxies and environments of high redshift AGN is
proving a valuable probe of current theories of how galaxies form and
evolve. Results from our NICMOS imaging program have indicated that
the hosts of z ~ 2 — 3 faint radio-quiet quasars {RQQ} have
luminosities only around local L*, making them similar to Lyman-break
field galaxies at the same redshifts, and to the low-z hosts RQQ
hosts. This is roughly consistent with theoretical predictions of
Kauffmann & Haehnelt {2000} for the hierarchical buildup of galaxy
hosts and their relation to their resident supermassive black holes.
The luminosity of the AGN in these RQQ is key to understanding this
relationship, however, and we are making a comprehensive archival HST
imaging study of the hosts of RQQs from low to high z at a range of
nuclear luminosities. At intermediate z, however, there are no studies
of the hosts of RQQs in the faint luminosity range that represents the
bulk of the quasar population. In the present proposal, we request
imaging at the same rest-wavelengths as our high-z sample of the hosts
of 10 similarly luminous RQQs at z ~ 0.9. These data will fill in an
important part of the parameter space defined by quasar luminosity and
redshift. Combined with existing HST data they will allow us to trace
the evolution of the hosts of RQQ and that of the relationship between
quasar luminosity and host galaxy luminosity.

ACS/WFC 9892

H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying
Star Formation in a Dusty Universe

Previous studies of nearby galaxies show large discrepancies between
different star formation {SF} indicators on large {>100 pc, or even
global} scales: the strikingly complex interplay of young stars, dust
and ionized gas are the primary cause of this variance. The few
galaxies in the HST Archive with both WFPC2 H-alpha and mid-UV {F255W
or F300W} imaging show this complex geometry extending down to <10 pc
scales. We propose a SNAPshot survey in the ACS/WFC H-alpha filter of
48 galaxies of all Hubble types, that are nearby but beyond the Local
Group, and that were previously imaged with WFPC2 in the mid-UV and in
F814W. We aim to provide a benchmark for understanding the SF
processes in both normal and star-bursting galaxies, at spatial
resolutions unattainable from the ground for a large and varied galaxy
sample. These data can be applied to a wide range of astrophysical
problems and will, therefore, be made public immediately. Our science
goals are to: {1} spatially resolve the dust clouds and filaments
which strongly affect mid-UV and H-alpha derived SF rates, {2} test
how the large-scale correlation between H-alpha and mid-UV flux breaks
down on pc scales, and {3} model the propagation of star formation by
comparing the SF over time scales of ~100 Myr {via mid-UV} and ~5 Myr
{via H-alpha}. This will {4} significantly improve our insight into,
and calibration of SF in UV-bright galaxies at high z, and into the
cosmic SF history.

NIC/NIC3 9865

The NICMOS Parallel Observing Program

We propose to continue managing the NICMOS pure parallel program.
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<z<1.9, which provides an excellent measure of current star
formation rate. We will also detect star-forming and active galaxies
in other redshift ranges using other emission lines. The grism
observations will produce by far the best available Halpha luminosity
functions over the crucial–but poorly observed–redshift range where
galaxies appear to have assembled most of their stellar mass. This key
process of galaxy evolution needs to be studied with IR data; we found
that observations at shorter wavelengths appear to have missed a large
fraction of the star-formation in galaxies, due to dust reddening. We
will also obtain deep F110W and F160W images, to examine the space
densities and morphologies of faint red galaxies. In addition to
carrying out the public parallels, we will make the fully reduced and
calibrated images and spectra available on-line, with some
ground-based data for the deepest parallel fields included.

ACS/WFC 9860

ESSENCE: Measuring the Dark Energy Equation of State

The accelerating universe appears to be dominated by a dark energy
with a significant negative pressure. The ratio of the pressure to
density of this mysterious energy {its equation of state} is an
observable which can differentiate between the proliferating candidate
theories. We propose to estimate the dark energy equation of state by
observing Type Ia supernovae at redshifts near z=0.7 with HST in
concert with the on-going ESSENCE NOAO Survey program that is
discovering and studying supernovae between 0.3<z<0.8. We show that an
interesting constraint on the equation of state can be made with
supernovae observed at modest redshifts given the current knowledge of
the matter density. We will follow 10 Type Ia supernovae discovered
from the ground and passed to HST without disrupting its schedule. The
full data set will constrain the equation of state to 10% and strictly
limit the range of possible dark energy models. In keeping with the
ESSENCE policy, these observations will available to the community


The role of dark matter and intracluster gas in galaxy formation and
cluster evolution

We propose a fully-sampled mosaic of 41 ACS images to survey galaxy
morphologies and measure weak lensing signals to the turn-around
radius in the X-ray luminous cluster, MS0451-03 {z=0.54}. The aim is
to isolate the physical processes which affect the evolution of
cluster galaxy morphologies in the context of well-defined dynamical
system. The study will be used in contrast to a successful campaign
undertaken in Cycle 9 on a optically-selected target. By comparing
morphologies with spectroscopic and Chandra X-ray data, we will
quantify the role of the intracluster medium and associated
substructures and establish the timescales and physical regions within
which the various environmental processes occur.


HST / Chandra Monitoring of a Dramatic Flare in the M87 Jet

As the nearest galaxy with an optical jet, M87 affords an unparalleled
opportunity to study extragalactic jet phenomena at the highest
resolution. During 2002, HST and Chandra monitoring of the M87 jet
have detected a dramatic flare in knot HST-1 located ~1" from the
nucleus. Its brightness has increased ten-fold in the optical band,
and continues to increase, and the X-rays show a similarly dramatic
outburst. In both bands this HST-1 now rivals the nucleus in
brightness. To our knowledge this is the first incidence of an optical
or X-ray outburst from a jet region which is spatially distinct from
the core source; this presents an unprecedented opportunity to study
the processes responsible for non-thermal variability and the X-ray
emission. We propose four epochs of HST/ACS monitoring during Cycle
12, as well as seven epochs of Chandra/ACIS observation {5ksec each}.
We also include a brief STIS observation that will be used with prior
STIS data to measure proper motions, and ACS polarimetry to map the
magnetic field structure. The results of this investigation are of key
importance not only for understanding the nature of the X-ray emission
of the M87 jet, but also for understanding flares in blazar jets,
which are highly variable, but where we have never before been able to
resolve the flaring region in the optical or X-rays. These
observations will allow us to test synchrotron emission models for the
X-ray outburst, constrain particle acceleration and loss timescales,
and study the jet dynamics associated with this flaring component.

NIC3 9824

NIC3 SNAPs of nearby galaxies imaged in the mid-UV: the remarkable
cool stellar population in late-type galaxies.

We propose a NIC3 H-band {F160W} SNAPshot survey of 48 nearby mid- to
late-type galaxies covering all inclinations. In Cycle 9 and 10, we
imaged ~100 galaxies in the mid-UV {F300W/F255W} and I-band {F814W}
with WFPC2, and obtained UBVR CCD surface photometry from the ground.
Early-mid-type galaxies show the usual small radial color-gradients,
where disks become somewhat bluer at larger radii. But, remarkably,
the majority of {lower luminosity, smaller and rounder} late-type
galaxies shows the opposite trend and becomes redder outwards in all
filters. While young UV/blue-bright stellar populations dominate their
inner morphology, most late-type galaxies must have a significant halo
or thick disk of older stars. Combining our proposed NIC3 H-band with
existing WFPC2 images will span the wavelength range 0.29-1.6 micron
at resolutions of 0.04-0.16" {FWHM}. This Panchromatic Nearby Galaxy
Atlas will be applicable to a wide range of problems, and will be made
public immediately. Our NIC3/F160W science goals are to: {1} Establish
the nature of the old outer stellar population. All target galaxies
have z<0.005, allowing us to resolve any luminous, cool supergiant
population. NIC3 is essential to make a pixel-to-pixel color-magnitude
study of the nature, distribution and uniformity of the outer stellar
populations, which will constrain dwarf galaxy formation theories. {2}
Determine galaxy structure at 5-20 pc resolution, tracing the old
stellar population and mass distribution compared to the star-forming
regions seen in the mid-UV. A range of inclinations is needed to
distinguish between old thick disks or halos in late-type galaxies.
{3} Make a multi-wavelength pixel-to-pixel decomposition to help
delineate the effects of dust, age, and metallicity. Since we must
cover a range of inclinations, NIC3 H-band is essential to map the
effects from dust, and see how these may affect the studies of {1} and


Observations of Intermediate Mass Black Hole Candidate Ultra-Luminous
X-ray Sources

Ultra-luminous X-ray {ULX} sources are off-nuclear point sources in
nearby normal galaxies. Variability observed on the timescale of days,
weeks, and years signals that ULXS are accreting sources, likely
harboring black holes. However, the observed X-ray luminosity of these
systems far exceeds the Eddington limit for a 10 Msun black hole; some
ULXs may be intermediate mass black holes. The identification and
study of optical counterparts with HST will be central to better
understanding these objects. We propose to obtain deep U-B-V-I
exposures of 4 extremely bright ULXs in nearby spirals: NGC 1313 X-1
and X-2, M81 X-9 {Holmberg II X-1}, and M74 X-1. Each has a 0.5”
Chandra position, and X-ray luminosity and spectral characteristics
consistent with expectations for intermediate mass black holes. We
will use the colors we obtain, the magnitudes we measure, and any
source variability {also, correlated optical-X-ray variability from
simultaneous Chandra snapshots} to constrain the nature of the donor
stars and the black holes {10 Msun or 100-1000 Msun}, and the
formation and evolution scenarios for each system.

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.


Search for Core-disrupting Wide-Angle Winds

We propose to obtain observations with STIS/FUV-MAMA of H$_2$
fluorescent lines along the cavity surrounding the star T Tau N. Since
H$_2$ fluorescent lines are direct tracers of shock-excitation in
low-mass star-forming regions, the high resolution achievable with
STIS will allow us to delineate the region of interaction between the
wind and the cloud, and to investigate the geometry of the outflow at
unprecedentedly close distances to its source, < 100 AU. Our
observations will allow us to confirm, map out, and provide
quantitative estimates of the off-axis {wide-angle} flow for the first
time. Understanding the geometry of the wind is crucial because {1} it
determines whether outflows can disrupt their natal cores, and {2} it
tests theories of jet production and collimation.


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.


STIS Observations of Orbital and Rotational Variations in the Unique
Post-Common Envelope System HS1136+6646

HS1136+6646 is a recently discovered close-binary system consisting of
a hot {Teff ~ 120, 000 K} DAO white dwarf and a K7V main sequence
companion. It is unique in being a relatively bright, nearby example
of both a very young post-common envelope system and a pre-cataclysmic
variable system. Although the K star component of HS1136+6646 has now
been well studied from the ground, the white dwarf can only be
effectively studied at UV wavelengths from space. We propose STIS
observations of HS1136+6646 which focus specifically on the nature of
the white dwarf, i.e., its mass, temperature, age, photospheric
composition and possible magnetic field. High-dispersion echelle
spectra, taken at quadrature of the 0.83607 day orbital period of the
system will provide an accurate determination of the gravitational
redshift of the white dwarf.


Verifying the White Dwarf Mass-Radius Relation with Sirius B

We propose timely STIS observations of Sirius B, that will provide
fundamental astrophysical data on this very important, but difficult
to study, white dwarf. High quality spectra of the Balmer line region
will provide accurate, modern measurements of its gravitational
redshift, effective temperature, surface gravity and absolute flux.
From these measurements, precise determinations of the spectroscopic
mass and radius can be made, that will approach a 1% uncertainty. At
this level, it will be possible to: 1} directly compare the
spectroscopic and astrometric masses at a comparable level of
accuracy, 2} precisely test the theoretical mass-radius relation for a
1 solar mass white dwarf, 3} distinguish between thick and thin H
layer masses and 4} confirm the widely used method of estimating white
dwarf masses from the Balmer lines. The only existing Balmer line
observations of Sirius B are those of Greenstein et al. {1971} from
the days of photographic plates. The increasing separation of the
components now permits STIS observations at a time when new
astrometric and far UV observations are available.


Investigating the Powering Sources of Expanding Supergiant Shells in
the Nearby Dwarf Galaxy IC 2574

Using the unique resolving capability of the Hubble Space Telescope
{HST} and the wide-field imaging capabilities of the ACS, we propose
to perform a stellar population study of two prominent supergiant
shells {SGS} in the nearby dwarf galaxy IC2574. By constructing the
star formation history for those SGSs we will for the first time be
able to test if past star formation created these impressive
structures, as suggested by theory. We have carefully selected 2 SGSs;
one is young {age: few 10^7yr, exhibiting a prominent central stellar
association and the other is older {few 10^8yr}, with no obvious
optical counterpart. The aim of this proposal is to determine the age
and SF history of the central stellar associations of both SGSs by B,
V, and I band imaging using HST’s ACS. A primary goal is the
comparison of the stellar ages with the age estimates from the HI
kinematics. Using color magnitude diagrams, we will also estimate how
many stars have evolved off the main sequence and exploded as SN,
giving an estimate for the total mechanical energy deposited. A
comparison with the values derived in other wavelengths is not only
important for understanding these particular SGSs but will also set
strong timing as well as energy constraints on the physical mechanisms
which lie at the origin of SGSs in general.

NIC2 9752

A Search for the Exciting Sources in OMC-1 through NICMOS Polarization

Orion contains the site of the nearest region of massive star
formation to the Sun; only here can this pivotal process in galactic
evolution be studied at the highest resolution. There are 10^5 solar
luminosities of radiation emitted from the Orion Molecular Cloud
{OMC-1}, possibly from a young massive star or protostar, or possibly
from several, less luminous sources. Either way, the powering
source{s} in the closest site of massive star formation has still not
yet been identified. Here we propose to apply a new tool to determine
which, of several prospective sources, might prove to be the heart of
OMC-1. The sources cannot be seen directly because they lie in, or
behind, a warm, dense molecular cloud. However, their presence can be
inferred in polarized light, through the manner in which light is
scattered off neighboring clouds. Heretofore, the spatial resolution
has not been adequate to identify the locations of individual stars.
We propose to use the NICMOS polarizers combined with the high spatial
resolution of HST to achieve this, in spite of the high density of
candidate objects in the core of Orion. The demands of accurately
measuring the polarization vectors of small, diffuse objects relative
to the surrounding background from dust-scattered light requires the
high Strehl ratio and stable point-spread function only achievable
from space.

ACS/HRC 9747

An Imaging Survey of the Statistical Frequency of Binaries Among
Exceptionally-Young Dynamical Families in the Main Asteroid Belt

We propose an ambitious SNAPSHOT program to determine the frequency of
binaries among two very young asteroid families in the Main Belt, with
potentially profound implications. These families {of C- and S-type}
have recently been discovered {Nesvorny et al. 2002, Nature 417, 720},
through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY
ago in catastrophic impact events. This is the first time such
precise and young ages have been assigned to a family. Main-belt
binaries are almost certainly produced by collisions, and we would
expect a young family to have a significantly higher frequency of
binaries than the background, because they may not yet have been
destroyed by impact or longer-term gravitational instabilities. In
fact, one of the prime observables from such an event should be the
propensity for satellites. This is the best way that new numerical
models for binary production by collisions {motivated largely by our
ground-based discoveries of satellites among larger asteroids}, can be
validated and calibrated. HST is the only facility that can be used to
search for binaries among such faint objects {V>17.5}. We will also
measure two control clusters, one being an "old" family, and the other
a collection of background asteroids that do not have a family
association, and further compare with our determined value for the
frequency of large main-belt binaries {2%}. We request visits to 180
targets, using ACS/HRC.

NIC1 9737

A NICMOS direct imaging search for giant planets around the seven
single white dwarfs in the Hyades

We propose to use the NIC1 camera on HST to search for massive giant
planets around the known seven single white dwarfs in the nearby
Hyades cluster at sub-arcsec separations. At an age of 625 Myr, the
white dwarfs had protogenitor masses of about 3 solar masses, and
massive gaseous giant planets should have formed in the massive
circumstellar disks around these ex Herbig A0 stars, probably at
orbital separations similar or slightly larger than that of Jupiter {5
AU} in our own solar system. Such planets would have survived the
post-Main Sequence mass loss of the parent star, and would have
migrated outward adiabatically by a factor 4.5, equal to the ratio of
initial to final stellar mass {3Mo/0.66Mo}, due to conservation of
orbital angular momentum during the mass loss {AGB and PN} phase. Thus
the orbital separation NOW would be 4.5 x 5 AU = 22.5 AU, which at the
distance of the Hyades {45 pc} corresponds to 0.50 arcsec. Simulations
with TinyTim then show that giant planets at this separation with
masses in the range 6-12 Jupiter masses and apparent J and H
magnitudes in the range 20.5-23.3 mag {from Baraffe or Burrows models}
can be spatially resolved around the Hyades white dwarfs. Their J and
H brightnesses are known to be 15 +/- 0.5 mag, implying a median
star-planet brightness ratio of 1000:1 {7.5 mag}. This combination of
dynamic range and orbital separation is observable with NICMOS, by
subtracting images taken at two roll angles. Therefore, the proposed
near-IR diffraction-limited observations in the F110W and F160W
filters promise to resolve giant planets around low-mass stars for the
first time. If successful, the observations would also prove that
giant planets do form around early-type stars more massive than the

NIC3 9735

ACS, NICMOS, and STIS Observations of Three Ongoing Mergers

We propose to make ACS {U, B, V, I, H_alpha}, NICMOS {J, H, K}, and
STIS {long-slit H_alpha} observations of NGC 520, NGC 2623, and NGC
3256, three merging galaxies in the middle of the Toomre Sequence and
currently in the throes of violent relaxation. Two of these {NGC 2623
and NGC 3256} are the most IR luminous galaxies in the sequence.
Hence, these ongoing mergers are ideal candidates for studying the
triggering mechanism responsible for the formation of stars and star
clusters. The ACS observations will allow us to age date the star
clusters, and reliably distinguish clusters from stars based on their
apparent sizes. They will also be used in conjunction with
ground-based measurements of the stellar velocity dispersion to
determine dynamical masses of the clusters and hence address the
question of whether the IMF is truncated. The NICMOS observations will
allow us to penetrate the dust and answer several fundamental
questions such as: What fraction of the young clusters are hidden by
dust? How do these clusters form and evolve? The STIS observations
will allow us to study the kinematics of the young cluster system and
measure the pressure and shock properties which may be triggering the
formation of the clusters. A better understanding of how mergers form
tremendous numbers of clusters and stars in the local universe will
help shed light on processes that were crucial during galaxy assembly
in the high-z universe.

NIC2 9726

A NICMOS search for obscured supernovae in starburst galaxies

Recent near-IR monitoring campaigns were successful in detecting
obscured supernovae {SNe} in starburst galaxies. The inferred SN rate
is much higher than that obtained in previous optical campaigns, but
it is still significantly lower than expected by the high level star
formation of these systems. One possible explanation for the shortage
of SNe is that most of them occur in the nuclear region, where the
limited angular resolution of groundbased observations prevents their
detection. We propose NICMOS SNAP observations of a sample of
starburst galaxies already observed once by NICMOS, with the goal of
exploiting its sensitivity and angular resolution to detect nuclear
obscured SNe which might have been missed by groundbased surveys.
These observation will allow to assess the real SN rate in starbust
galaxies and deliver a sample of SN occurring in the extreme
environment of galactic nuclei. We expect to detect more than 55 SNe
{if the whole sample is observed}. If the number of SNe detected in
the program is much lower than expected it would prompt for a revision
of our understanding of the relation between the star formation rate
and the SN rate.


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.

ACS/WFPC2 9488

Cosmic Shear – with ACS Pure Parallel Observations

The ACS, with greater sensitivity and sky coverage, will extend our
ability to measure the weak gravitational lensing of galaxy images
caused by the large scale distribution of dark matter. We propose to
use the ACS in pure parallel {non- proprietary} mode, following the
guidelines of the ACS Default Pure Parallel Program. Using the HST
Medium Deep Survey WFPC2 database we have measured cosmic shear at
arc-min angular scales. The MDS image parameters, in particular the
galaxy orientations and axis ratios, are such that any residual
corrections due to errors in the PSF or jitter are much smaller than
the measured signal. This situation is in stark contrast with
ground-based observations. We have also developed a statistical
analysis procedure to derive unbiased estimates of cosmic shear from a
large number of fields, each of which has a very small number of
galaxies. We have therefore set the stage for measurements with the
ACS at fainter apparent magnitudes and smaller, 10 arc-second scales
corresponding to larger cosmological distances. We will adapt existing
MDS WFPC2 maximum likelihood galaxy image analysis algorithms to work
with the ACS. The analysis would also yield an online database similar
to that in


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.

ACS/WFC 10089

Hubble Heritage Image of the Light Echo around V838 Monocerotis

We will obtain a spectacular color image of the light echo around V838

STIS/CCD 10085

STIS Pure Parallel Imaging Program: Cycle 12

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

WFPC2 10084

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 10082

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans

WFPC2 10070

WFPC2 CYCLE 12 Supplemental Darks Part 2/3

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


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/WFC 10056

Extreme Red Stars

ACS provides unprecedented sensitivity in the far red, this coupled
with recent astronomical pushes to ever cooler objects {e.g. new
classifications for L and T stellar dwarfs, and extremely high
redshift galaxies} increases the need for extending the photometric
calibration to include such objects. We propose observations of 2
stellar objects for which STIS spectra will exist, as well as NICMOS
grism. The two targets include a late M dwarf and a T dwarf. The M
dwarf provides a temporal check with WFC and new constraint for the
HRC. The T dwarf provides new results for the WFC.

ACS/HRC 10050

ACS Earth Flats

High signal sky flats will be obtained by observing the bright Earth
with the HRC and WFC. These observations will be used to verify the
accuracy of the flats currently used by the pipeline and will provide
a comparison with flats derived via other techniques: L-flats from
stellar observations, sky flats from stacked GO observations, and
internal flats using the calibration lamps. Weekly coronographic
monitoring is required to assess the changing position of the spots.

STIS/CCD 10019

CCD Bias Monitor – Part 1

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/CCD 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.


Focus Monitor

The focus of HST is measured from WFPC2/PC and ACS/HRC images of
stars. Multiple exposures are taken in parallel over an orbit to
determine the influence of breathing on the derived mean focus.
Observations are taken of clusters with suitable orientations to
ensure stars appear in all fields.


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

HSTAR 9317: GS Acquisition (1,2,2) @ 039/20:04:36Z resulted in FL
backup (1,0,1) due to SSLEX on FGS 2. Prior FHST FM Updates @
039/19:46:03Z and 19:48:48Z showed good attitude error vector. Under

HSTAR 9318: GS Acquisition (2,3,3) @ 040/06:44:20Z resulted in FL
backup using FGS 2 due to SSLE (QF3SSLEX) on FGS 3. Prior FHST FM
Updates @ 040/06:38:50Z and 06:41:35Z showed good attitude error
vector. Subsequent GS Acquisition (2,3,3) @ 040/07:20:00Z, with
different GS ID, was successful at AOS. Under investigation.

17087-1 Command Generator FSW Parameter Patch @ 040/00:47:18z

1196-0 Limits Changes to NMEBTMP2 and EFHST18T @ 037/15:15z
1197-0 Adjust ACS Error Count Limit @ 037/16:03z
1160-2 Default Configuration for TMDIAG’s @ 040/00:51:45z

                            SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq                35                        35
FGS REacq                14                        14
FHST Update              58                        58


Successfully completed Command Generator Slew Parameter change
040/00:44Z – 00:47Z (OR 17087-1 with attached script). First Type 2
slew, utilizing the updated parameters, occurred @ 040/01:38Z.
On-orbit slew duration matched the duration projected within the .RSM
report and the slew executed as expected. RWA speeds and torques were
all nominal during the slew. Trending of vehicle Type 2 slews will
continue over the next several days to verify slew, RWA, and HGA
performance. First occurrence of a HGA transition from spline to
ephemeris track, during a Type 2 slew, occurs @ 042/08:06Z, will be
monitored in real-time to verify no HGA high torque error are

SpaceRef staff editor.