NASA Hubble Space Telescope Daily Report # 3371
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3371
PERIOD COVERED: DOY 147
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 9184
A Survey for Missing Baryons in Highly Ionized Intergalactic Gas at Low
Redshift.
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe six
additional low-z QSOs with the STIS FUV E140M echelle mode {7 km s^-1
resolution}. Combined with archival data, this will increase the sample
redshift
path by a factor of ~7 compared to the published data. With the echelle
data, we
will {1} measure the number of O VI absorbers per unit redshift {dN/dz}
and
their minimum cosmological mass density with a limiting equivalent width
of
W_Lambda ~50 mAngstrom , {2} examine whether the O VI absorption arises
in
photoionized, collisionally ionized, or multiphase gas, and {3} study the
dependence of the O VI system properties on environment. In addition to
testing
this prediction regarding the location of the missing baryons, the data
will
have applications to many other topics such as low-z LyAlpha absorbers
and the
physical properties and abundances of gas in the Milky Way halo.
WFPC2 9342
Confirmation of Black Hole, Planetary, and Binary Microlensing Events
We propose WFPC2 images of five MACHO Project microlensing events in
order to
confirm our microlensing models which indicate that these events were
caused by
black holes and stars with extra-solar planets. Our microlensing parallax
fits
for MACHO-96-BLG-5 and MACHO-97-BLG-6 indicate that the lenses are likely
to be
black holes of ~ 40M{sun} and ~ 8M{sun}, respectively, and we can test
these
models by comparing the amount of stellar blended predicted by the model
with
the blended determined from the WFPC2 images. For the large mass black
hole
candidate MACHO-96-BLG-5, we propose a time series of observations to
follow the
declining magnification of ~ 0.4 mag over the next several years as
predicted by
the microlensing model. For the two extra-solar planet candidates
reported by
the Microlensing Planet Search {MPS} Collaboration, MACHO-97-BLG-41 and
MACHO-98-BLG-35, we propose to test the planetary microlensing models by
determining the amount of blending between each source star and its
neighbors.
Our observations of MACHO-97-BLG-41, will serve as a first epoch for the
possible observation of this triple lens system moving away from the
source
star. Finally, we propose to image binary lensing event MACHO-98-SMC-1 to
test
our ability to determine the location of the lens systems for such
events.
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<z<1.60. Only QSOs
brighter
than g’=19 were selected. The QSO emission and DLA absorption redshifts
were
constrained to virtually eliminate data loss due to intervening Lyman
limit
absorption. Consequently, we expect to discover ~40 new DLAs, which is a
three-fold increase in this redshift interval. This will significantly
improve
our earlier low-z DLA statistical results on their incidence,
cosmological mass
density, and N_HI distribution. The results will also allow us to better
quantify the empirical DLA — metal-line correlation. With this improved
understanding, the need for follow-up UV spectroscopy will lessen and,
with the
release of the final database of SDSS QSO spectra {an ~25-fold increase},
the
number of low-z DLAs could be increased arbitrarily. Thus, the power of
the
large and statistically-sound SDSS database in combination with a proven
technique for finding low-z DLAs will, over the next few years,
essentially
solve the problem of making an accurate determination of the cosmic
evolution of
the neutral gas component down to z~0.4.
SNAP/STIS 9434
A SNAPSHOT Survey of the Hot Interstellar Medium
We propose to obtain SNAPSHOT STIS echelle observations of key tracers of
hot
interstellar gas {CIV, NV and SiIV} for selected FUSE Team OVI survey
targets
with known UV fluxes. By taking advantage of the SNAPSHOT observing mode
we
will
efficiently obtain a large number of spectra suitable for the study of
the
highly ionized hot component of the interstellar medium {ISM}. Our goals
are to
explore the physical conditions in and distribution of such gas, as well
as to
explore the nature of the interfaces between the hot ISM and the other
interstellar gas phases. Using inter–comparisons of the various ionic
ratios
for CIV, NV, OVI and SiIV, we will be able to discriminate between the
various
models for the production of the highly ionized gas in the Galactic ISM.
The
survey will also enable detailed studies of regions already known to
contain hot
gas through X-ray emission measurements {e.g., SNRs and radio loops}. The
proposed SNAPSHOT observations will extend our previous Cycle 9 survey
{which
was compromised by the STIS side 1 failure}, and should roughly double
the
number of stars for which high quality STIS observations of the important
hot
gas tracers are available, enabling us to derive a truly global view of
the hot
ISM.
ACS 9468
ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7
We propose an ACS grism parallel survey to search for emission-line
galaxies
toward 50 random lines of sight over the redshift interval 0 < z pl 7. We
request ACS parallel observations of duration more than one orbit at high
galactic latitude to identify ~ 300 HAlpha emission-line galaxies at
0.2 pl
z pl
0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3 pl z pl 1.68, and
pg
1000 Ly-alpha emission-line galaxies at 3 pl z pl 7 with total emission
line
flux f pg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain
direct
images with the F814W and F606W filters and dispersed images with the
WFC/G800L
grism at each position. The direct images will serve to provide a zeroth
order
model both for wavelength calibration of the extracted 1D spectra and for
determining extraction apertures of the corresponding dispersed images.
The
primary scientific objectives are as follows: {1} We will establish a
uniform
sample of HAlpha and O II emission-line galaxies at z<1.7 in order to
obtain
accurate measurements of co-moving star formation rate density versus
redshift
over this redshift range. {2} We will study the spatial and statistical
distribution of star formation rate intensity in individual galaxies
using the
spatially resolved emission-line morphology in the grism images. And {3}
we
will
study high-redshift universe using Ly-alpha emitting galaxies identified
at z
pl 7 in the survey. The data will be available to the community
immediately as
they are obtained.
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.
STIS 9505
The Evolution of Molecular Clouds.
The combined STIS, FUSE and ground-based results will yield information
needed
to understand the role of ablation in the evolution of the central
clouds.
ACS 9583
The Great Observatories Origins Deep Survey: Imaging with ACS
We propose a Treasury program of ACS imaging as part of the Great
Observatories
Origins Deep Survey {GOODS}, covering 320{square}’, or 32* the area of
the two
original WFPC2 HDFs, to within 0.5–0.8 mag of their depth in four ACS
bands,
BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep
Field
South, are the premier deep survey areas from X– ray to radio
wavelengths. ACS
data will provide unique angular resolution, sensitivity, and wavelength
coverage to close the gap between the deepest Chandra and SIRTF
observations.
Supported by extensive imaging and spectroscopy from the VLT, Keck,
Subaru,
NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data
set will
make it possible to map the evolution of the Hubble sequence with
redshift,
reconstruct the history of galaxy mass assembly, star formation and
nuclear
activity from the epoch of reionization to the present, trace the growth
of
density perturbations via cosmic shear, and, with properly phased z–band
observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the
cosmic
acceleration and the presence of dark energy. All HST, SIRTF, Chandra,
and
supporting GOODS data are non– proprietary, with science–quality images
and
catalogs released on a timescale of months. This will constitute the
deepest,
largest, and most uniform panchromatic data set ever assembled to study
the
distant universe.
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.
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.
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 10 10FGS REacq 5 5 FHST Update 18 18 LOSS of LOCK
SIGNIFICANT EVENTS:
HST FSW 2.3c Ops Acceptance Test Part 1 of 2 scheduled 148/10:00Z –
149/01:00Z with
GDOC, HITT, SE, and VEST using CCS "B" String 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.