NASA Hubble Space Telescope Daily Report # 3382
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3382
PERIOD COVERED: DOY 162
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.
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.
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}.
WFPC2 9458
Probing the Formation & Evolution of M31’s Outer Disk and Halo
The fossil record of galaxy formation and evolution is imprinted on the
spatial
distribution, ages and metallicities of galactic stellar populations. The
observations proposed here build significantly upon our extensive
ground-based
and archival WFPC2 programs and aim to constrain the formation and evolution
of
our nearest large neighbour, M31. We propose deep imaging of 8 fields in the
outer disk and halo, several of which have been identified from our
panoramic
ground-based CCD survey {covering ~ 26 square degrees} to possess
significant
stellar density and/or potential metallicity variations. Deep
colour-magnitude
diagrams reaching ~2-3 magnitudes below the horizontal branch will be
constructed, allowing detailed characterization of the luminous evolved
stellar
populations via the red giant metallicity distribution, the luminous
asymptotic
giant branch, the horizontal branch morphology and the red clump, as well
as the
detection of a main-sequence that may be present from any younger
component. Our
primary goals are to: {i} quantify the stellar population variations
associated
with M31 halo substructure, including the newly- discovered giant stellar
stream, and {ii} derive stringent constraints on the age and metallicity of
stars in the far outer disk. These observations will directly address two
key
predictions of cold dark matter hierarchical galaxy formation models.
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 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
Survey
Fields
In anticipation of the allocation of ACS high-latitude imaging survey{s}, we
request a modification of the default pure parallel program for those WFPC2
parallels that fall within the ACS survey field. Rather than duplicate the
red
bands which will be done much better with ACS, we propose to observe in the
near-ultraviolet F300W filter. These data will enable study of the
rest-frame
ultraviolet morphology of galaxies at 0<z<1. We will determine the
morphological
k-correction, and the location of star formation within galaxies, using a
sample
that is likely to be nearly complete with multi-wavelength photometry and
spectroscopic redshifts. The results can be used to interpret observations
of
higher redshift galaxies by ACS.
NICMOS 9484
The NICMOS Parallel Observing Program
We propose to manage the default set of pure parallels with NICMOS. Our
experience with both our GO NICMOS parallel program and the public parallel
NICMOS programs in cycle 7 prepared us to make optimal use of the parallel
opportunities. The NICMOS G141 grism remains the most powerful survey tool
for
HAlpha emission-line galaxies at cosmologically interesting redshifts. It is
particularly well suited to addressing two key uncertainties regarding the
global history of star formation: the peak rate of star formation in the
relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star
formation missing from UV continuum-based estimates due to high extinction.
Our
proposed deep G141 exposures will increase the sample of known HAlpha
emission-
line objects at z ~ 1.3 by roughly an order of magnitude. We will also
obtain a
mix of F110W and F160W images along random sight-lines to examine the space
density and morphologies of the reddest galaxies. The nature of the
extremely
red galaxies remains unclear and our program of imaging and grism
spectroscopy
provides unique information regarding both the incidence of obscured star
bursts
and the build up of stellar mass at intermediate redshifts. In addition to
carrying
out the parallel program we will populate a public database with calibrated
spectra
and images, and provide limited ground- based optical and near-IR data for
the
deepest parallel fields.
STIS 9506
A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS
We propose a STIS G140L spectroscopic Snapshot program of bright {V<=16.5}
AGN
not previously observed in the UV to discover new high-column density {N_H
>=
10^15 cm^-2} LyAlpha absorbers in the local Universe {z <= 0.45}. Many more
of
these high column density systems are needed because: {1} They contribute
most
of the baryons to the local IGM; {2} They include systems for which valuable
metallicity and D/H measurements can be made with the Cosmic Origins
Spectrograph {COS}; {3} They include many of the “warm-hot” absorbers,
thought
to be a large baryon reservoir in the local Universe; and {4} They are most
likely to be “associated” with galaxy halos. Because of their low-z, many
of
these absorbers can be located relative to galaxies of known redshifts,
allowing
an immediate scientific return from these snapshots. Perhaps the most
important,
lasting results of this survey require higher resolution reobservations
with COS
by our GTO team. Using these snapshots to select the best targets, we will
obtain COS R~22, 000 spectra to determine the D/H and metallicity of
absorbers
in galaxy halos, groups, and voids. We will use pairs and “constellations”
of
AGN to determine absorber sizes, shapes, and covering factors. Candidate
“warm-hot” absorbers will be reobserved with COS to determine their
numbers
accurately and to assess their metallicity, sizes, and relationships to
galaxies
and galaxy groups.
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 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.
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.
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 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
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.
ACS/HRC/WFC 9728
Tracing the History of Cosmic Expansion to z~2 with Type Ia Supernovae
Type Ia supernovae {SNe Ia} provide the only direct evidence for an
accelerating
universe, an extraordinary result that needs the most rigorous test. The
case
for cosmic acceleration rests on the observation that SNe Ia at z = 0.5 are
about 0.25 mag fainter than they would be in a universe without
acceleration. A
powerful and straightforward way to assess the reliability of the SN Ia
measurement and the conceptual framework of its interpretation is to look
for
cosmic deceleration at z > 1. This would be a clear signature of a mixed
dark-matter and dark-energy universe. Systematic errors in the SNe Ia result
attributed to grey dust or cosmic evolution of the SN Ia peak luminosity
would
not show this change of sign. We have obtained a toehold on this putative
“epoch of deceleration” with SN 1997ff at z = 1.7, and 3 more at z > 1
from
our Cycle 11 program, all found and followed by HST. However, this is too
important a test to rest on just a few objects, anyone of which could be
subject
to a lensed line-of-sight or misidentification. Here we propose to extend
our
measurement with observations of twelve SNe Ia in the range 1.0 < z < 1.5 or
6
such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be discovered as a
byproduct from proposed Treasury and DD programs. These objects will provide
a
much firmer foundation for a conclusion that touches on important questions
of
fundamental physics.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.) None
COMPLETED OPS REQs:
16991-0 – FSW 2.3C EEPROM Installation @ 162/1243z
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS
GSacq 10 10
FGS REacq 7 7
FHST Update 20 20
LOSS of LOCK
SIGNIFICANT EVENTS:
On 162/11:49:27:00 commanding commenced for the installation of FSW2.3C
EEPROM
installation (OR 16991-0) on the first opportunity. EEPROM load was
completed at
162/11:55:13 and the memory dump and comparison completed at 162/12:35:30
with
FSW’s concurrence. BMIC enable (last step) was performed at
162/12:43:05. All
operations associated with the EEPROM installation proceeded nominally.
This
concludes a successful FSW2.3C Installation.
