HST Daily Report # 3360 (part 2)
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.
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.
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.
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.
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 9606
CCD Dark Monitor-Part 2
Monitor the darks for the STIS CCD.
STIS 9631
Faint Standard Extension {FASTEX}
Fainter standard stars are needed for the flux calibration of COS, for
the
prism
modes on ACS, and for astronomical community, in general. The bright
object
safety limit for COS is 1.25 ct/s per pixel, while the total countrate
limit per
FUV detector segment is 20000/s. In addition, the GALEX project {see
Appendix}
requires more secondary standards in the flux range of the two fainter
original
FASTEX stars. Customarily, one NASA project provides observing time in
support
of other NASA projects. The existing observations of the two fainter
FASTEX
standards, WD0947+857 and WD1657+343, have the most CTE losses in the
G430L
data
and are still a bit marginal on S/N. Since the stellar models are
normalized to
V, good spectrophotometry to 5500A is important. All five targets will be
observed at the new G430L aperture to minimize CTE loss and at the
original
aperture to constrain CTE models. Combined with additional planned cal
data for
stars of intermediate flux, the CTE model for spectra can be tuned to
cover the
full range of signal levels.
STIS 9339
Physical Parameters of the Erupting Luminous Blue Variable NGC 2363-V1
In 1996, we reported the discovery of a bright variable star in the giant
extragalactic H , ii region NGC 2363. Subsequent photometry and high
quality
HST/STIS spectroscopy of this star, NGC 2363-V1, revealed that we are
witnessing
a significant event in the evolution of a massive star, namely a major
eruption
of a Luminous Blue Variable {LBV}. A quantitative analysis of the STIS
datasets
gathered in 1997 and 1999 allowed us to determine the luminosity, mass
loss
rate, wind terminal velocity, surface temperature and even Fe content of
this
erupting LBV. Because such events are rare, continuous monitoring of the
physical parameters of NGC 2363- V1 over the course of its present
eruption
will
provide an invaluable set of constraints for theoretical models. We
therefore
propose to obtain high quality STIS spectra of this star once a year for
the
next three observing Cycles.
STIS 9708
STIS Pure Parallel Imaging Program: Cycle 11
This is the default archival pure parallel program for STIS during cycle
11.
STIS 9441
Zinc Abundances in Damped Ly-Alpha Systems at z < 0.5: A Missing Link in
the
Chemical History of Galaxies
The evolution of metallicity in damped Lyman alpha {DLA} quasar
absorption
systems is an important constraint on the global star formation history
of the
universe, but remains a big puzzle at present. The H I column density
weighted
mean metallicity in DLAs is expected to rise to solar values at low
redshifts,
based on cosmic chemical evolution models, because the mass-weighted mean
metallicity of local galaxies is near- solar. However, current DLA
abundance
studies are highly uncertain and cannot distinguish between evolution and
no
evolution in the mean metallicity at redshifts 0.4 < z < 3.5. The
existing data
are particularly incomplete because no Zn measurements exist for z < 0.4,
and
only 2 exist for z < 0.5, which spans the past 35-45 % of the age of the
universe. To pin down the cosmic age-metallicity relation all the way to
the
present epoch, we propose to measure Zn abundances in five DLAs at 0.1 <
z <
0.5. We propose to use HST STIS because it is the only existing
instrument that
can measure the necessary UV lines. Our observations will clearly
distinguish
between no metallicity evolution vs. the predicted evolution. Our data
will
also
provide Cr measurements, which will help to estimate the dust abundance.
The
proposed observations are crucial for tying together the absorption and
emission
histories of gas and stars in galaxies and for clarifying the relation of
DLAs
to present-day galaxies.
STIS/ACS 9384
Ozone, Condensates, and Dust in the Martian Atmosphere
We propose to utilize the unique UV capabilities of STIS and ACS/HRC in
order to
study the spatial and seasonal variations in ozone, condensates, and dust
in the
Martian atmosphere. The data obtained will be critical in addressing
recent
breakthroughs in understanding the basic radiative, transport, and
microphysical
processes that provide for both long-term and short-term balance within
the
global Mars climate system. The proposal includes both Cycle 11 & 12
observations in order to span the classic dust storm season on Mars and
provide
the first good opportunity for HST to synoptically observe a dusty
atmosphere on
the planet. The UV observations will complement broad-band visible and IR
observations that will be made during the Mars Global Surveyor Extended
Mission
and will provide support for the future UV observations of MARCI on the
2005
Mars Reconnaissance Orbiter.
STIS/MA1 9466
SBS 1150+599: A Population III Planetary Nebula?
SBS 1150+599 is a puzzling emission-line object. Optical spectra reveal
only
strong Balmer, He II and Ne V lines, along with a hot, featureless
continuum. We
have recently partially resolved the HAlpha emission in a ground-based
image,
and believe the object to be a new halo planetary nebula, one of only
handful
known in the Milky Way. If correct, its lack of significant O III and
other
forbidden emission means that SBS 1150+599 has the lowest metallicity of
any
known planetary nebula. Our estimate of the oxygen abundance places it 40
times
lower than that of K 648 in the globular cluster M15, the previous record
holder, and would make it one of the most metal-poor objects in the
Galaxy. We
propose obtaining ACS images of SBS 1150+599 to confirm that it is a
planetary
nebula and to determine its morphology. Planetary nebulae in old
populations may
occur due to binary-star merging, and the morphology may test this
hypothesis.
We will also study the UV spectrum of SBS 1150+599 using STIS to confirm
the O/H
value and estimate carbon and nitrogen abundances unobtainable in the
optical.
WFPC2 9336
Expansion distances to the symbiotic Miras He 2-104 and He 2-147
We propose to measure the expansion parallax of the nebulae around the
binary
symbiotic Miras He 2-104 {the Southern Crab} and He 2-147 by means of
high
resolution WFPC2/F658N images to be taken at two different epochs. Given
the
large outward velocities of these nebulae inferred from ground-based
spectroscopy, their apparent expansion can be measured by HST imaging
over
timescales of only 2-3 years. For He 2-104 we have already obtained
“Epoch 1”
HST images {cf. STScI-PRC- PR99-32}. Combining the angular and radial
velocity
expansions will straightforwardly yield the distance to the proposed
targets.
Knowledge of the distance to these nebulae will provide a solid
contribution to
a variety of research fields such as {a} the energetics of nuclear
burning in
symbiotic binaries containing a Mira, {b} the pulsation mode of binary
Miras,
and {c} the viability of Mira symbiotics as supersoft X-ray sources and
potential progenitors of Type Ia supernovae. HST high resolution imaging
of the
nebulae combined with ground-based spectroscopy will also address the
still
debated issue of the formation of bipolar nebulae by collimated outflows
from
evolved stars.
WFPC2 9710
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
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.
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
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.) None
COMPLETED OPS REQs:
16970-2 Battery 2 Capacity test script @ 129/1931z
OPS NOTES EXECUTED:
0900-1 COMMAND PROBLEM @ 129/1303z
0900-1 COMMAND PROBLEM @ 132/0330z
1108-2 Perform Observation Re-Dumps on the Partial Obs. Level @129/1445z,
130/0001z,130/0003z, 130/1141z, 130/1143z, 130/1146z, 130/1150z,
130/1153z,130/1148z, 130/1315z, 130/1318z, 130/2233z, 130/2235z,
130/2238z,130/2239z, 131/1307z, 131/1309z, 131/1311z, 131/1313z,131/2039z
1110-0 S/W Dump of HST486 Memory @ 130/1305z
1111-0 Change Limits MAMA1 Threshold Voltage @ 130/1622z
0910-2 SI Console response to MCE Resets after FSW 4.8 is activated @ 130/1546z
0916-0 Tabulation of Slew Attitude Error (Miss-distance) @ 132/0152z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS
GSacq 21 21
FGS REacq 28 28
FHST Update 41 41
LOSS of LOCK
SIGNIFICANT EVENTS: None
