HST Daily Report # 3351
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3351
PERIOD COVERED: DOY 118
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
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.
NICMOS 9386
Infrared Photometry of a Statistically Significant Sample of KBOs
of the solar system has been slowed by a lack of basic astrophysical
data.
Photometric observations of the majority of the more than 400 known KBOs
and
Centaurs are rudimentary and incomplete, particularly in the infrared.
The
multicolor optical-infrared photometry that exists for a small subset of
KBOs
often shows significant discrepancies between observations by different
observers. Their intrinsic faintness puts them at the practical limits of
ground-based systems. In July 2001 we began what will be the largest
uniform
sample of optical photometry of KBOs with a WFPC2 SNAPSHOT program that
will
perform accurate photometry at V, R, and I on a sample of up to 150
targets. We
seek to greatly enhance the value of this survey by obtaining J and H
photometry
on the same sample using NICMOS. Combined optical and infrared broad band
photometry is a far more powerful tool for physical studies than is
either
alone. Our sample includes objects that will be observed at thermal
infrared
wavelengths by SIRTF and will be used with those data to derive the first
accurate diameters, albedos, and surface properties for a large sample of
KBOs.
ACS 9401
The ACS Virgo Cluster Survey
We propose the most comprehensive imaging survey to date of low-redshift,
early-type galaxies. Our goal is to exploit the exceptional imaging
capabilities
of the ACS by acquiring deep images — in the SDSS g^ and z^ bandpasses
— for
163 E, S0, dE, dE, N and dS0 galaxies in Virgo, the nearest rich cluster.
This
extraordinary dataset would likely constitute one of the principal
legacies of
HST, and would have widespread applications for many diverse areas of
astrophysics. Our immediate scientific objectives are threefold: {1}
measure
metallicities, ages and radii for the many thousands of globular clusters
{GCs}
in these galaxies, and use this information to derive the protogalactic
mass
spectrum of each galaxy; {2} measure the central luminosity and color
profile of
each galaxy, and use this information to carry out a completely
independent
test
of the merging hierarchy inferred from the GCs, with the aid of N-body
codes
that simulate the merger of galaxies containing massive black holes; and
{3}
calibrate the z^ -band SBF method, measure Virgo’s 3-D structure, and
carry out
the definitive study of the GC luminosity function’s precision as a
standard
candle. Our proposed Virgo Cluster Survey will yield a database of
unprecedented
depth, precision and uniformity, and will enable us to study the record
of
galaxy and cluster formation in a level of detail which will never be
possible
with more distant systems.
STIS 9437
Quantitative Constraints for Massive Star Evolution Models with Rotation
Rotation is now recognized as an important physical component in
understanding
massive stars. Theory suggests that rotation affects the lifetimes,
chemical
yields, stellar evolution tracks, and the supernova and compact remnant
properties {Heger & Langer 2000, Maeder & Meynet 2000}. In a Cycle 7
program, we
proved that rotational mixing occurs in massive main sequence stars {Venn
et al.
2001}. In this proposal, we want to quantitatively test model predictions
and
constrain the theory for a better understanding of massive star
evolution. We
are requesting HST STIS observations of the BIII 2066 Angstrom resonance
line of
seven massive stars in three young clusters carefully selected from IUE
analyses. These stars show traces of boron depletion, but without
nitrogen
enrichment; rotation is the only theory able to explain this abundance
pattern.
These new abundances will allow us to test rotating model predictions:
that
mixing strength increases with stellar age, mass, and rotation rate. They
will
also help to quantitatively constrain the rotational mixing efficiencies
in
massive stars. One very high S/N spectrum of a moderately boron-depleted
star is
also requested. We wish to measure its 11B/10B ratio, which is predicted
to
change as boron is depleted in the rotating models. This ratio will
further
confirm rotational effects and observationally constrain the 10B{p,
Alpha}
thermonuclear reaction rate, which is presently highly uncertain.
ACS/STIS 9451
ACS Imaging and STIS Spectroscopy of Binary Brown Dwarfs
We have compiled a sample of 9 spatially resolved binary brown dwarfs {18
objects}, and now propose ACS imaging and STIS spectroscopic follow-up
observations. While theoretical models on the interplay of chemical and
physical
processes governing brown dwarf atmospheres have reached a high level of
sophistication, interpretation of observational data remains difficult.
As
brown
dwarfs never stabilize themselves on the hydrogen main sequence, there is
always
an ambiguity between the temperature or luminosity of any brown dwarf and
its
mass or age. The individual components of brown dwarf binaries, however,
are
expected to be coeval and have the same underlying chemical composition.
This
provides crucial constraints on any model, thus greatly reducing the
number of
the free parameters. The aim is to obtain photometric and spectroscopic
data to
probe the physical and chemical properties of the brown dwarf
atmospheres, as
well as second epoch astrometric data to characterize th e orbital
motion. The
study will provide important feedback on theoretical model atmospheres
and
evolutionary tracks for brown dwarfs. As such, it will be an important
step
towards a better understanding of objects with spectral properties
intermediate
between those of giant planets and late-type stars.
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.
WFPC2 9589
WFPC2 Decontaminations and Associated Observations Pt. 1/3
photometric stability check, focus monitor, pre- and post-decon internals
{bias,
intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and
internal UV
flat check.
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
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/CAL 9609
CCD Read Noise Monitor
This proposal measures the read noise of all the amplifiers {A, B, C, D}
on the
STIS CCD using pairs of bias frames. Full frame and binned observations
are
made
in both Gain 1 and Gain 4, with binning factors of 1×1, 1×2, 2×1 and 2×2.
All
exposures are internals. Pairs of visits are scheduled for monthly
execution.
STIS 9613
STIS CCD Spectroscopic Flats C11
Obtain CCD flats on the STIS CCD in spectroscopic mode.
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 9659
Bias and dark dependence on CCD gains
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.
STIS 9708
STIS Pure Parallel Imaging Program: Cycle 11
WFPC2 9709
POMS Test Proposal: WFII parallel archive proposal
Proposal 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.) None
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 7 7
FGS REacq 7 7
FHST Update 20 20
LOSS of LOCK
SIGNIFICANT EVENTS:
Continue upgrade to STScI main routers with Giga-bit Ethernet adapters 6
–
10 pm local.
Upgrade gear from 155Mb ATM to Giga-bit Ethernet. Install Giga-bit
Ethernet modules in
both main and backup core routers. Interruptions should be no more that
15 – 20 minutes
and may occur several times between 6 and 10 pm local.
