HST Daily Report # 3336

HUBBLE SPACE TELESCOPE

DAILY REPORT       # 3336

PERIOD COVERED: DOY 97

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.

WFPC2 9033

Measuring the mass distribution in the most distant, very X-ray luminous
galaxy
cluster known

We propose to obtain a mosaic of deep HST/WFPC2 images to conduct a weak
lensing
analysis of the mass distribution in the massive, distant galaxy cluster
ClJ1226.9+3332, recently discovered by us. At z=0.888 this exceptional
system is
more X-ray luminous and more distant than both MS1054.4-0321 and
ClJ0152.7-1357,
the previous record holders, thus providing yet greater leverage for
cosmological studies of cluster evolution. ClJ1226.9+3332 differs
markedly from
all other currently known distant clusters in that it exhibits little
substructure and may even host a cooling flow, suggesting that it could
be the
first cluster to be discovered at high redshift that is virialized. We
propose
joint HST and Chandra observations to investigate the dynamical state of
this
extreme object. This project will 1} take advantage of HST’s superb
resolution
at optical wavelengths to accurately map the mass distribution within 1.9
h^{-1}
50 Mpc via strong and weak gravitational lensing, and 2} use Chandra’s
unprecedented resolution in the X-ray waveband to obtain independent
constraints
on the gas and dark matter distribution in the cluster core, including
the
suspected cooling flow region. As a bonus, the proposed WFPC2
observations will
allow us to test the results by van Dokkum et al. {1998, 1999} on the
properties
of cluster galaxies {specifically merger rate and morphologies} at z~0.8
from
their HST study of MS1054.4-0321.

STIS/MA2 9096

Objective-Prism Spectroscopy of Massive Young Clusters.

The Space Telescope Imaging Spectrograph (MA2) was used to greatly
improve the
spatial information by obtaining STIS NUV-MAMA objective-prism
spectroscopy in
the 1300-3600 Angstrom range of three nearby extragalactic regions with a
total
of ~ 10 MYCs since most of the present knowledge of the UV spectral
properties
of massive young clusters {MYCs} is based on IUE data with marginal
spatial
resolution. Slitless techniques are seldom attempted on crowded clusters
due to
the overlap among different sources. It is planned to overcome that
problem by
observing with two different roll angles, using comparison UV and optical
images
from the HST archive.

HST 9382

A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO MgII-FeII Systems.

We have searched the first public release of SDSS QSO spectra for low-z
{z<1.65} metal absorption lines and found over 200 large rest equivalent width MgII-FeII systems. Previously, we empirically showed that such systems are good tracers of large neutral gas columns, with ~50% being classical damped Lyman alpha {DLA} systems {N_HI>=2*10^20 cm^-2}. Here we propose to follow up a
well-defined
subset of 79 of them to search for DLAs with 0.47

NICMOS 9423

NICMOS Observations of Transient Infrared Jets in the Galactic
Microquasar
GRS1915+105

We propose to use HST/NICMOS to make Target of Opportunity observations
of the
galactic microquasar GRS1915+105. This source possesses transient radio
jets
which exhibit apparent superluminal motions, and resolved infrared
emission
from
these jets has been observed in GRS1915+105 {Sams, Eckart, and Sunyaev,
1996;
Eikenberry and Fazio, 1996}. Because the jet ejection events are
correlated
with
X-ray outbursts, we will use observations of X-ray flares with the Rossi
X-Ray
Timing Explorer to trigger the HST observations. We will then monitor
GRS1915+105 periodically with NICMOS, obtaining relative astrometry,
photometry,
polarimetry, and grism spectroscopy of the jets and the parent object.
These
observations will allow us to greatly increase our understanding of the
jets’
radiative mechanisms and physical conditions, and their evolution with
time. We
require the capabilities of HST and NICMOS due to the small angular
separations
between the jets and the parent object {increasing from ~ 0.1 to ~ 0.8
arcsec
over the span of the TOO observations} and the high reddening towards
GRS1915+105 {A_V ~ 30 mag}.

ACS 9454

The Nature of the UV Continuum in LINERs: A Variability Test

LINERs may be the most common AGNs, and the signposts of accretion onto
the
massive black holes present in most galaxies. However, the LINER spectrum
is the
result of UV excitation, and, in at least some LINERs, a nuclear cluster
of hot
stars, rather than an AGN, dominates the energetics in the UV. Thus, it
is
still
unknown if the UV continuum, or the optical emission lines it excites,
have
anything to do with an AGN. The demographics and accretion physics of
low-luminosity AGNs hinge on this question. We propose to search for
variability
in a sample of 17 LINERs with compact UV nuclei. Variability can reveal
an AGN
component in the UV continuum, even when its light is not dominant. We
will
test
systematically the handful of non-definitive reports of UV variability,
and
potentially quantify the AGN contribution to the UV emission. Variability
in all
or most objects will be strong evidence that LINERs mark dormant AGNs in
most
galaxies. Alternatively, a general null detection of variability will
suggest
that, even in LINERs with additional AGN signatures, the UV continuum is
stellar
in origin. Contemporaneous monitoring with the VLA/VLBA of 11 objects
which
have
radio cores {five of which we already know are radio-variable} will
reveal the
relations between UV and radio variations. The UV-variable objects will
be
targeted for future, better-sampled, monitoring.

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/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 9592

WFPC2 CYCLE 11 Standard Darks

This dark calibration program obtains dark frames every week in order to
provide
data for the ongoing calibration of the CCD dark current rate, and to
monitor
and characterize the evolution of hot pixels. Over an extended period
these
data
will also provide a monitor of radiation damage to the CCDs.

WFPC2 9594

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3

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

WFPC2 9596

WFPC2 CYCLE 11 INTERNAL MONITOR

This calibration proposal is the Cycle 11 routine internal monitor for
WFPC2, to
be run weekly to monitor the health of the cameras. A variety of internal
exposures are obtained in order to provide a monitor of the integrity of
the CCD
camera electronics in both bays {gain 7 and gain 15}, a test for quantum
efficiency in the CCDs, and a monitor for possible buildup of
contaminants on
the CCD windows.

WFPC2/ACS 9601

WFPC2-ACS Photometric Cross-Calibration

This proposal is aimed at providing photometric zeropoint
cross-calibration
between the commonly used WFPC2 photometric filter sets and those that
will be
used for ACS programs. The proposal includes observations of globular
clusters
spanning a wide range in metallicity, including NGC 2419 and 47 Tuc. In
addition, we will obtain WFPC2 observations of the primary ACS standard
star.
This program will produce a valuable tie-in between the WFPC2, ACS and
Sloan
filter photometric systems.

STIS 9606

CCD Dark Monitor-Part 2

STIS 9608

CCD Bias Monitor – Part 2

high-S/N superbiases and track the evolution of hot columns.

STIS 9615

Cycle 11 MAMA Dark Monitor

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.

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.

WFPC2 9634

POMS Test Proposal: WFII targeted parallel archive proposal

The parallel opportunities available with WFPC2 in the neighborhood of
bright
galaxies are treated in a slightly different way from the normal pure
parallels.
Local Group galaxies offer the opportunity for a closer look at young
stellar
populations. Narrow-band images in F656N can be used both to identify
young
stars via their emission lines, and to map the gas distribution in
star-forming
regions. Thus, the filter F656N is added to the four standard filters.
Near
more
distant galaxies, up to about 10 Mpc, we can map the population of
globular
clusters; for this purpose, F300W is less useful, and only F450W, F606W,
and
F814W will be used.

NICMOS 9637

NICMOS Focus Stability

The purpose of this activity is to determine if the best focus determined
in
SMOV is stable. This program will execute in approximately one month
intervals
starting about 1 month after the last execution of proposal 8980.

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 9673

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 9702

NICMOS Parallel Thermal Background

NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to
establish the stability of the HST+NCS+Instrument thermal emission. This
data
will be compared against the already available Camera 3 measurements in
F222M
which show an increased thermal background.

STIS 9706

STIS Pure Parallel Imaging Program: Cycle 10

This is the default archival pure parallel program for STIS during cycle
10.

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 paralell 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.) None

COMPLETED OPS REQs: NONE

OPS NOTES EXECUTED: NONE

                        SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq            09                        09
FGS REacq            06                        06
FHST Update          18                        18
LOSS of LOCK

SIGNIFICANT EVENTS:

FOT real-time spacecraft operations continue from the GSFC MOR, pending
study
of recent SIMOR commercial power loss event.

Successfully completed CCS Command Test 097/10:52Z – 14:20Z using CCS “A”
String with
CCS Release 4.0.2 and PRD S07102.  Testing was executed from the SMOR
using
CCS “A”
String with the SOC in Building x (x=removed for publication).  All
objectives were met
with CCS generating appropriate error messages, when expected.

Successfully completed CCS 4.0.2 HSTSIM/CCSPSS Verification testing
097/14:23Z – 17:34Z
using CCS “A” String with CCS Release 4.0.2 and PRD S07102.  CCS was able
to properly
handle 0.5, 4, and 32 kbps telemetry formats transmitted from the HSTSIM
and CCSPSS.
Also, able to properly transmit commands to the HSTSIM and CCSPSS and
update the CDI
counter as well as transmit loads for the 486 and NSSC-1 and receive 486,
NSSC-1 memory,
and SSR engineering and science playbacks.  4 and 32 kbps telemetry
formats
transmitted
from the HSTSIM and CCSPSS, a 486 hardware “I” Channel dump via PDI, and
SSR engineering
and science playbacks were also properly handled with CCS in a SM
configuration.