NASA Hubble Space Telescope Daily Report # 3372

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3372

PERIOD COVERED: DOY 148

OBSERVATIONS SCHEDULED

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.

STIS/CCD/MA1 9357

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 propose to carry out a
STIS UV
spectroscopic snapshot survey of CVs that fully exploits the diagnostic
potential of these objects for our understanding of accretion physics.
This
survey will provide an 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 parameterized 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 at least double, if not triple, the number of
high-quality accretion disc / wind outflow / accreting white dwarf
spectra, and
we waive our proprietary rights to permit a timely use of this database.

GO 9367

Unique Opportunities to Search for the Optical Counterparts to High-Z
Damped
LyAlpha Systems

The galaxies responsible for damped LyAlpha absorption in QSO spectra are
difficult to observe against the strong background QSO emission. We
propose to
detect even low luminosity galaxies associated with QSO absorption line
systems
out to redshifts as high as z = 1.8 by observing them in the shadow cast
by an
even higher redshift damped LyAlpha absorber. As a result the galaxy will
be
observed free of contamination by the background AGN and of the
uncertainties
which arise when image processing techniques are required to remove the
AGN
emission. We propose two approaches. In the first we will attempt to
detect a z
= 1.8634 system seen in the optical spectrum of a high-z BL Lac object in
the
shadow of two higher-redshift systems seen in the same optical spectrum.
In the
second only the higher redshift shadowing LyAlpha system is seen in the
optical
spectrum and the presence of the lower- redshift systems at z = 0.713 and
z =
1.0466 are inferred from the presence of strong MgII, SiII and FeII
absorption
lines.

NICMOS 9375

The Host Galaxies of Time Delay Lenses: , An Independent Route to the
Hubble
Constant

Because of its importance in setting the distance scale, the time scale
and in
estimating cosmological parameters from the CMB, astronomy needs an
estimate of
the Hubble constant independent of the local distance scale and its
systematic
problems. This can be achieved using gravitational lenses with time delay
measurements given enough constraints on the gravitational potential of
the
lens. We will use deep NICMOS observations of the lensed quasar host
galaxies in
7 gravitational lenses with time delay measurements to obtain the
necessary
constraints, determine the dark matter distribution and estimate H_0.
Analysis
of the existing images and the well-developed theory for analyzing
Einstein
ring
images of host galaxies suggest the new data will break the familiar
degeneracies between lens mass distributions and the Hubble constant. We
also
request 30 ksec Chandra ACIS images for each of the 2 systems lacking
them
{B1608+656 and B1600+434} to measure the mass in nearby or surrounding
groups
and clusters.

ACS/HRC 9391

High-Resolution Imaging of Pluto’s Surface

We will collect a series of observations with the ACS/HRC from which we
will
derive a two-color global map of Pluto’s surface. We will image Pluto at
F435W
and F555W, wavelengths that have been extensively studied from the ground
over
the past 50 years. The maps will provide albedos with accurate error
determinations down to 52 degrees South latitude. These observations will
provide a second epoch of HST mapping of the active surface of Pluto as
it
continues to recede from the Sun and will provide an important context
for
other
detailed studies of Pluto.

ACS 9476

Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster
Sample

The study of distant cluster galaxies requires two key ingredients: {1}
deep
high-resolution imaging, to constrain galaxy structure; and {2} 8m-class
spectroscopy, to measure stellar content, star-formation rates, dynamics,
and
cluster membership. We will reach both conditions with the addition of
HST/ACS
imaging to our suite of VLT {36 nights} and NTT {20 nights} observations
of 10
confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey
{EDisCS}.
The proposed HST/ACS data will complement our existing optical/IR imaging
and
spectroscopy with quantitative measures of cluster galaxy morphologies
{i.e.
sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and
with
measurements of cluster masses via weak lensing. Major advantages unique
to the
EDisCS project include: {i} uniform selection of clusters; {ii} large
enough
sample sizes to characterize the substantial cluster-to-cluster variation
in
galaxy populations; {iii} large quantities of high quality data from 8m
telescopes; {iv} uniform measurements of morphologies, spectroscopic and
photometric redshifts, SEDs, star-formation/AGN activities, and internal
kinematics; {v} optical selection of clusters to complement the X-ray
selection
of almost all high-z clusters in the ACS GTO programs; {vi} forefront
numerical
simulations designed specifically to allow physical interpretation of
observed
differences between the high-z and local clusters.

ACS 9480

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 ideal.

ACS 9482

ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES}

Ly-alpha line emission is an efficient tool for identifying young
galaxies at
high redshift, because it is strong in galaxies with young stars and
little or
no dust — properties expected in galaxies undergoing their first burst
of
star- formation. Slitless spectroscopy with the ACS Wide-Field Camera and
G800L
grism allows an unmatched search efficiency for such objects over the
uninterrupted range 4 <~ z <~ 7. We propose the ACS Pure Parallel
Ly-alpha
Emission Survey {“APPLES”}, to exploit this unique HST capability and
so
obtain the largest and most uniform sample of high redshift Ly-alpha
emitters
yet. Parallel observations will allow this survey to be conducted with
minimal
impact on HST resources, and we will place reduced images and extracted
spectra
in the public domain within three months of observation. We aim to find ~
1000
Ly-alpha emitters, 5 times the biggest current sample of Ly-alpha
emitters.
This
unprecedented sample will provide robust statistics on the populations
and
evolution of Ly-alpha emitters between redshifts 4–7; a robust
measurement of
the reionization redshift completely independent of the Gunn-Peterson
trough;
spatial clustering information for Ly-alpha emitters which would let us
probe
their bias function and hence halo mass as a function of redshift; many
galaxies
at redshift exceeding 6; and lower redshift serendipitous discoveries.

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 archive.stsci.edu/mds/

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.

STIS 9604

STIS CCD Performance Monitor

This activity measures the baseline performance and commandability of the
CCD
subsystem. Only primary amplifier D is used. Bias and Flat Field
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, 4 x
1,
and 4
x 2. Dark images are taken in 2×2 binning mode; 1×1 binning darks are
being
taken in the nominal CCD Dark Monitor. Bias frames are taken in subarray
readouts to check the bias level for ACQ and ACQ/PEAK observations. All
exposures are internals.

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 9615

Cycle 11 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
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.

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.

ACS 9674

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.

NICMOS 9693

NICMOS Coronagraphic Performance Assessment

This test defines a coherent program designed to quantitatively measure
and map
out the diffractive and scattered energy rejection of occulted targets to
improve the target/background contrast ratios by use of the NICMOS
coronagraph.
The performance levels of system will be assessed while exploring the
observational parameter spaces and execution strategies which undoubtedly
will
be proposed for use in HST Cycle 11. This test is constructed in four
parts
with
different, but complementary, Taken together they will provide critical
information needed to re-evaluate the coronagraphic systemic performance
from
which flight {and possibly ground} S/W updates, and advisories to
observers
defining Phase 2 proposals will be issued.

STIS 9708

STIS Pure Parallel Imaging Program: Cycle 11

This is the default archival pure parallel program for STIS during cycle
11.

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.

FLIGHT OPERATIONS SUMMARY:

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

HSTAR 9046: GS Acquisition (2,3,2) @ 148/09:40:13Z failed to RGA control
during ZOE due
to SRLE on primary FGS 2. Under investigation.

COMPLETED OPS REQs:NONE

OPS NOTES EXECUTED:
1114-0 Change Limits MAMA2 Threshold Voltage @ 148/23:16z

                            SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq                09                        08              See
Hstar # 9046
FGS REacq                07                        07
FHST Update              18                        18
LOSS of LOCK

SIGNIFICANT EVENTS:

HST FSW 2.3c Ops Acceptance Test Part 2 of 2 scheduled 148/10:00Z –
149/01:00Z with GDOC,
HITT, SE, and VEST using CCS "B" and "C" Strings with CCS Release 4.0.2.2
and PRD O06100R1T.
The purpose of the testing is to verify installation and back out
procedures for the RAM
version of FSW 2.3c and EEPROM installation procedure work in an
operational scenario.