Status Report

NASA Hubble Space Telescope Daily Report # 3523

By SpaceRef Editor

January 6, 2004

Filed under Hubble Space Telescope, Space Telescope Science Institute, US

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3523

PERIOD COVERED: DOYs 2-4/2004

OBSERVATIONS SCHEDULED

ACS 9984

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.

STIS/CCD 9981

The Ultra Deep Field – STIS parallels

We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS
area
around the UDF.

WFPC2 9980

The Ultra Deep Field – WFPC2 Parallels

The ACS Ultra Deep Field {UDF} is a survey carried out by using Director’s
Discretionary time. The main science drivers are galaxy evolution and
cosmology.
The primary instrument is the Advanced Camera for Surveys but WFPC2,
NICMOS, and
STIS will also be used in pure parallel mode. The data will be made public. The
UDF consists of a single ultra-deep field {410 orbits in total} within the
CDF-S
GOODS area. We request a modification of the default pure parallel programs.
Rather than duplicate the redder 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,
allowing determination of 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.

NIC3 9979

The Ultra Deep Field – NICMOS Parallels

This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep
Survey.
We will obtain a mix of F110W and F160W images along sight-lines within the
mosaiced ACS fields of the CDF-S GOODS and GEMS surveys, with these sight-lines
enabling an examination of the space density and morphologies of the reddest
galaxies.

ACS/CCD/WFC 9978

The Ultra Deep Field with ACS

The ACS Ultra Deep Field {UDF} is a survey carried out by using Director’s
Discretionary time. The main science driver are galaxy evolution and cosmology.
The primary instrument is the Advanced Camera for Surveys but WFPC2 and NICMOS
will also be used in parallel. The data will be made public. The UDF
consists of
a single ultra-deep field {410 orbits in total} within the CDF-S GOODS
area. The
survey will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W {150
orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V} exposures will be
one magnitude deeper than the equivalent HDF filters. The F775W {I} exposure
will be 1.5 magnitude deeper than the equivalent HDF exposure. The depth in
F775W and F850LP is optimized for searching very red objects – like z=6
galaxies
– at the detection limit of the F850LP image. The pointing will be RA{J2000}=3
32 40.0 and Decl.{J2000}=-27 48 00. These coordinates may change slightly
due to
guide star availability and implementation issues. We will attempt to
include in
the field both a spectroscopically confirmed z=5.8 galaxy and a
spectroscopically confirmed type Ia SN at z=1.3. The pointing avoids the gaps
with the lowest effective exposure on the Chandra ACIS image of CDFS. This
basic
structure of the survey represents a consensus recommendation of a Scientific
Advisory Committee to the STScI Director Steven Beckwith. A local Working Group
is looking in detail at the implementation of the survey.

FGS 9969

FGS Astrometry of the Extrasolar Planet of Epsilon Eridani

We propose observations with HST/FGS in Position Mode to determine the
astrometric elements {perturbation orbit semimajor axis and inclination} of the
candidate extra-solar planet around the K2 V star Epsilon Eridani that has been
detected by Doppler spectroscopy. These observations will also permit us to
determine the actual mass of the planet by providing the sin{i} factor
which can
not be determined with the radial velocity method. High precision radial
velocity {RV} measurements spanning the years 1980.8–2000.0 for the nearby
{3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs.
These data represent a combination of six independent data sets taken with four
different telescopes. A least squares orbital solution using robust estimation
yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19
m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83
M_Jupiter.
An estimate of the inclination yields a perturbation semi-major axis, Alpha =
0arcs0022, easily within the reach of HST/FGS astrometry.

WFPC2 9968

Fundamental properties of L-type dwarfs in binaries

We propose to characterize the physical properties of eight L-dwarfs in four
binary systems. Our goal is to obtain astrometric, photometric and
spectroscopic
measurements of each component that will yield basic information on their
atmospheric and dynamical properties. The high angular resolution of HST is
essential because all these systems have angular separations $le$0.5 arcsec.
They do not have bright enough stars nearby that can be used for natural guide
adaptive optics in ground-based telescopes. In Cycles~10 and 11 we propose to
obtain WFPC2 and STIS data, allowing the determination of parallax, proper
motion, position and spectral type for each component. In Cycle 12 we plan to
obtain additional WFPC2 images for follow-up of the orbital motion and
refinement of parallax and proper motion. We will also monitor possible
intrinsic photometric variability in two filters {F675W and F814W}. The STIS
observations will provide spectral types, gravity sensitive indicators, and
chromospheric activity {H$_ lpha$ emission} for each component. These 4 systems
will constitute benchmarks for determining dynamical masses of L dwarfs, and
inferring the age-mass-spectral type relationship of this new spectral class.

NIC/NIC3 9865

The NICMOS Parallel Observing Program

We propose to continue managing the NICMOS pure parallel program. Based on our
experience, we are well prepared to make optimal use of the parallel
opportunities. The improved sensitivity and efficiency of our observations will
substantially increase the number of line-emitting galaxies detected. As our
previous work has demonstrated, the most frequently detected line is Halpha at
0.7<z<1.9, which provides an excellent measure of current star formation rate.
We will also detect star-forming and active galaxies in other redshift ranges
using other emission lines. The grism observations will produce by far the best
available Halpha luminosity functions over the crucial–but poorly
observed–redshift range where galaxies appear to have assembled most of their
stellar mass. This key process of galaxy evolution needs to be studied with IR
data; we found that observations at shorter wavelengths appear to have missed a
large fraction of the star-formation in galaxies, due to dust reddening. We
will
also obtain deep F110W and F160W images, to examine the space densities and
morphologies of faint red galaxies. In addition to carrying out the public
parallels, we will make the fully reduced and calibrated images and spectra
available on-line, with some ground-based data for the deepest parallel fields
included.

ACS/WFC 9860

ESSENCE: Measuring the Dark Energy Equation of State

The accelerating universe appears to be dominated by a dark energy with a
significant negative pressure. The ratio of the pressure to density of this
mysterious energy {its equation of state} is an observable which can
differentiate between the proliferating candidate theories. We propose to
estimate the dark energy equation of state by observing Type Ia supernovae at
redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey
program that is discovering and studying supernovae between 0.3<z<0.8. We show
that an interesting constraint on the equation of state can be made with
supernovae observed at modest redshifts given the current knowledge of the
matter density. We will follow 10 Type Ia supernovae discovered from the ground
and passed to HST without disrupting its schedule. The full data set will
constrain the equation of state to 10% and strictly limit the range of possible
dark energy models. In keeping with the ESSENCE policy, these observations will
available to the community immediately.

STIS/CCD/MA1 9852

Whirling Dervish Dynamos: Magnetic Activity in CV Secondaries

The mass-losing secondary stars of cataclysmic variables {CVs} are the most
rapidly rotating cool dwarfs observable. Other rapid rotators show a maximal,
"saturated" level of magnetic activity {e.g., X-ray emission}, but there are
hints from contact binaries and young clusters that activity may be suppressed
at the highest rotation rates. CV secondaries are thus important probes of
magnetic dynamos at rotational extremes. Implications for CV evolution {e.g.,
the “period gap", accretion variability} may also be profound. Unfortunately,
study of CV secondaries is hampered by pesky accretion-related phenomena and
reflection effects. As a result, little systematic work has been done. To
explore activity in these stars, we therefore propose to study far-UV
spectra of
AM Her-type systems {which have no accretion disks} in deep photometric minima
in which accretion is shut off. Magnetic-related emission from the secondary
will be separated {in velocity} from residual accretion emission by
observations
near quadratures. Lower chromospheric irradiation due to the white dwarf
primary
will be removed by modeling, yielding the true level of magnetic activity
on the
secondary. We will compare the results to other dMe stars and draw implications
for magnetic dynamos and activity at rotational extremes, and for CV evolution
and behavior.

STIS/CCD/MA1 9848

A SNAPSHOT Survey of Sharp-Lined Early B-Type Stars

Although spectrum synthesis studies of the UV spectra of sharp-lined main
sequence B stars provide us with some our best determinations of the abundances
of the Fe group and neutron capture elements and the chemical evolution in our
galaxy and the Magellanic Clouds, the HST archive is virtually devoid of high
resolution spectra of the bright nearby B stars that have become to be regarded
as abundance standards. For example, there are NO observations of HR 1886, iota
Her, and tau Her, the sharpest-lined representatives {V sin i < 5 km/s} of
spectral classes B1 V, B3 IV-V and B5 IV, and only a few tiny spectral
intervals
of gamma Peg {B2 IV}. Information on the abundances of the Fe group is
important
for computing opacities for stellar evolution calculations and for determining
astrophysical f-values. There are no suitable galactic standards in the HST
database to compare with recent HST/STIS observations of B stars in the
Magellanic Clouds and the likely future observations of similar objects in M31
and other nearby galaxies. To correct this deficiency, we propose SNAPSHOT
observations with the STIS E140M and E230M gratings of 33 of the best bright
abundance standards in nearby clusters and the galactic field. Using this data
we will determine the abundances of the Fe group and heavy elements using the
technique of spectrum synthesis with LTE and NLTE treatments. We waive the
proprietary period.

WFPC2 9809

Saturn’s rings and small moons on the eve of Cassini

We propose to continue our long-term survey of Saturn’s rings and small
moons to
obtain a coherent set of high resolution, multi-color WFPC2 images of
Saturn and
its rings during the final year before the arrival of the Cassini spacecraft at
Saturn in mid-2004. Our Cycle 6-11 programs {6806, 7427, 8398, 8660, 8802, and
9341} explored the rings from their nearly edge-on aspect {southern hemisphere
spring} to summer solstice in late 2002. We now propose to take advantage
of the
especially favorable viewing geometry of Cycle 12 to obtain UBVRI, F255W, and
methane-filter PC images of the rings, small moons, and planet at the lowest
phase angle {0.07 degrees} observable to date. A key goal is to measure for the
first time the expected sharp spike in the opposition brightness of the rings
and small moons, which will characterize the structure and particle properties
of the rings and the surfaces of the satellites. We will also follow the
chaotic
behavior of Prometheus and Pandora, two small moons which may be perturbing
each
other gravitationally. Here, our goals are to catch the satellites in the
act of
any new coupled motions and to determine the changes in semimajor axis,
eccentricity, and orbital inclination of the moons resulting from their most
recent large chaotic interaction in 2000. This will complete our continuous
WFPC2 coverage of these moons from 1994 until mid-2004, when Cassini’s cameras
will at long last surpass the capabilities of the HST. The Cycle 12
observations
will also enable us to determine zonal winds and regional variations in
Saturn’s
atmosphere prior to Cassini’s arrival.

NIC2 9801

Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey

Essentially all well-characterized preplanetary nebulae {PPNe}– objects in
transition between the AGB and planetary nebula evolutionary phases – are
bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical.
In order to understand the processes leading to bipolar mass-ejection, we need
to know at what stage of stellar evolution does bipolarity in the mass-loss
first manifest itself. We have recently hypothesized that most OH/IR stars
{evolved mass- losing stars with OH maser emission} are very young PPNe. We are
conducting a multiwavelength survey program of imaging and spectroscopic
observations of such objects, using a large, morphologically unbiased sample
selected using IRAS 12-to-25 micron colors. Our ongoing HST/SNAP imaging survey
of the optically bright half of this sample with WFPC2 and ACS is highly
successful: 19/32 objects observed are extended with bipolar/multipolar shapes
{remaining objects are unresolved}. Slightly more than 50% of our sample are
optically too faint or undetected but have strong near-IR counterparts — we
therefore propose a NICMOS SNAPshot imaging survey of these optically-faint
OH/IR stars. These observations are crucial for determining how and when the
bipolar geometry asserts itself. The results from our NICMOS survey {together
with the WFPC2/ACS survey} will allow us to draw general conclusions about the
onset of bipolar mass-ejection during late stellar evolution. Our complementary
program of interferometric mapping of the OH maser emission in our sources is
yielding kinematic information with spatial resolution comparable to that
in the
HST images. The HST/radio data will provide crucial input for theories of
post-AGB stellar evolution. In addition, these data will also indicate whether
the multiple concentric rings, "searchlight beams”, and truncated equatorial
disks recently discovered with HST in a few PPNe, are common or rare
phenomena.

STIS 9786

The Next Generation Spectral Library

We propose to continue the Cycle 10 snapshot program to produce a Next
Generation Spectral Library of 600 stars for use in modeling the integrated
light of galaxies and clusters. This program is using the low dispersion UV and
optical gratings of STIS. The library will be roughly equally divided among
four
metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar
{[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the entire
HR-diagram in each bin. Such a library will surpass all extant compilations and
have lasting archival value, well into the Next Generation Space Telescope era.
Because of the universal utility and community-broad nature of this venture, we
waive the entire proprietary period.

NIC3 9780

NIC3 Imaging of z~6 Candidates in a Deep ACS Parallel Field: Finding the
reionizing population and their LF

A fundamental cosmological question is when and how the universe was reionized.
It is now generally believed that the reionization ended by z=6. There is
evidence that QSO/AGN cannot provide enough photons to keep the universe
ionized
at that epoch. In Yan et al. {2003}, we presented a first statistically
significant sample of 6.0<z<6.5 galaxy candidates, 30 objects in total found in
a deep ACS/WFC parallel field by using the "drop-out" technique, and argued
that
the contamination due to possible contaminators was minimal. We concluded that
young, star-forming galaxies did exist in large number as expected from our
earlier work {Yan et al. 2002}, and that they could have contributed most
of the
reionizing photons. The candidates in our sample have a median magnitude of
AB=27.4 mag, beyond the spectroscopic capability of any existing
facilities. Any
effort of acquiring a large sample of galaxies around z=6 will have the vast
majority of candidates at such a faint brightness level. Thus near-IR
imaging is
the only practical way to further confirm the nature and the redshifts of these
candidates until the launch of the JWST in 2010. Here we propose to use the
NIC3
of the NICMOS to image 43% of our sample in the F110W and F160W bands to
unambiguously confirm their nature. We will image 13-14 of our candidates with
two NIC3 fields, and request 16 orbits of observation in total. With this data
set, we will be able to determine the surface density of galaxies at the
crucial
epoch around z=6, and derive photometric redshift for our candidates. Our
result
will set stringent limits to the faint-end slope of the luminosity function
{LF}
and the star formation rate at z=6, and thus provide essential constraints to a
series of questions regarding the reionization of the universe.

ACS/WFC 9751

Accurate Mass Determination of the Ancient White Dwarf ER 8 Through Astrometric
Microlensing

We propose to determine the mass of the very cool white dwarf ER 8 through
astrometric microlensing. We have predicted that ER 8 will pass very close to a
15th-mag background star in January 2006, with an impact parameter of less than
0.05 arcsec. As it passes in front, it will cause a deflection of the
background
star’s image by >8 milliarcsec, an amount easily detectable with HST/FGS. The
gravitational deflection angle depends only on the distances and relative
positions of the stars, and on the mass of the white dwarf. Since the distances
and positions can be determined precisely before the event, the astrometric
measurement offers a unique and direct method to measure the mass of the white
dwarf to high accuracy {<5%}. Unlike all other stellar mass determinations,
this
technique works for single stars {but only if they are nearby and of sufficient
mass}. The mass of ER 8 is of special interest because it is a member of the
Galactic halo, and appears to be the oldest known field white dwarf. This
object
can thus set a lower limit on the age of the Galactic halo, but since
white-dwarf cooling rates depend on their masses, the mass is a necessary
ingredient in the age determination. As a byproduct, we will obtain an accurate
parallax for ER 8, and thus its luminosity and {from its effective temperature}
its radius. Such quantities are at present rather poorly known for the coolest
white dwarfs, and will provide strong constraints on white-dwarf physics.

ACS/HRC/SBC 9745

From molecules to aerosols: observing the haze creation process during Titan’s
polar summer

Our Cycle 11 observations of Titan at southern summer solstice reveal
unexpected
complexity and an opportunity for science that has not previously been
possible.
Titan currently has a polar hood below 65 degrees S. The polar hood is dark in
the visible relative to the southern mid-latitudes, as is Titan’s northern
hemisphere. In the UV and near-IR, the hood is spectrally distinct from the
better-known north-south asymmetry, indicating a different formation mechanism.
The nature of the relation between the southern summer hood and the northern
spring equinox polar hood observed by Voyager is uncertain. We propose a set of
ultraviolet and supporting observations to demonstrate the nature of temporal
changes in the hood and to look for expected stratospheric absorbing
gasses. The
gasses are precursors to Titan’s aerosols; the polar hood may be an early stage
of aerosol evolution. Our observations will provide important constraints
on the
chemistry and dynamics of Titan’s stratosphere at summer solstice. The
chance to
follow-up our observations of the polar hood will allow us to assess the
processes and changes that are occurring now, so that Cassini observations of
the polar regions will not need to be interpreted in isolation from seasonal
context.

WFPC2 9712

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.

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 9703

Coronographic Search for Planets around Nearby Stars

We will use the HRC coronagraph to search for planets, disks, and exo-zodiacal
dust around nearby stars. We have selected the following stars: alpha Cen A and
B, tau Ceti, and epsilon Eridani. The observations of each star will be
taken at
two or more epochs. The observations will be broken into a sequence of short
exposures and taken at different roll angles to compensate for "telescope
breathing" during the orbit. As a further precaution, the observations will be
scheduled after the closest possible nearby pointing in order to minimize
thermal changes in the OTA during the first orbit of observations. After
matching phases, the PSFs from one star will be subtracted from the other
star.

NICMOS/STIS CCD 9405

The Origin of Gamma-Ray Bursts

The rapid and accurate localization of gamma-ray bursts {GRBs} promised by a
working HETE-2 during the coming year may well revolutionize our ability to
study these enigmatic, highly luminous transients. We propose a program of HST
and Chandra observations to capitalize on this extraordinary opportunity. We
will perform some of the most stringent tests yet of the standard model, in
which GRBs represent collimated relativistic outflows from collapsing massive
stars. NICMOS imaging and STIS CCD spectroscopy will detect broad atomic
features of supernovae underlying GRB optical transients, at luminosities more
than three times fainter than SN 1998bw. UV, optical, and X-ray spectroscopy
will be used to study the local ISM around the GRB. Chandra spectroscopy will
investigate whether the GRB X-ray lines are from metals freshly ripped from the
stellar core by the GRB. HST and CTIO infra-red imaging of the GRBs and their
hosts will be used to determine whether `dark’ bursts are the product of
unusually strong local extinction; imaging studies may for the first time
locate
the hosts of `short’ GRBs. Our early polarimetry and late-time broadband
imaging
will further test physical models of the relativistic blast wave that produces
the bright GRB afterglow, and will provide unique insight into the influence of
the GRB environment on the afterglow.

NICMOS 8790

NICMOS Post-SAA calibration – CR Persistence Part 1.

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.

ACS/WFC 10086

The Ultra Deep Field with ACS

STIS/CCD 10085

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during cycle 12.

WFPC2 10074

WFPC2 Cycle 12 UV Earth Flats

Monitor flat field stability. This proposal obtains sequences of earth streak
flats to improve the quality of pipeline flat fields for the WFPC2 UV filter
set. These Earth flats will complement the UV earth flat data obtained during
cycles 8-11.

WFPC2 10069

WFPC2 CYCLE 12 Supplemental Darks, Part 1/3

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

WFPC2 10067

WFPC2 Cycle 12 Decontaminations and Associated Observations

This proposal is for the monthly WFPC2 decons. Also included are instrument
monitors tied to decons: photometric stability check, focus monitor, pre- and
post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,
VISFLAT sweep, and internal UV flat check.

ACS/HRC/WFC 10059

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.

ACS/WFC 10046

CCD Hot Pixel Annealing

Hot pixel annealing will be performed once every 4 weeks. The CCD TECs will be
turned off and heaters will be activated to bring the detector temperatures to
about +20C. This state will be held for approximately 12 hours, after which the
heaters are turned off, the TECs turned on, and the CCDs returned to normal
operating condition. To assess the effectiveness of this procedure, a bias and
two dark images will be taken after the annealing procedure for both WFC and
HRC. The HRC darks are taken in parallel with the WFC darks.

STIS/CCD 10038

CTE measurement and photometric accuracy for extended sources

This is a follow-up study to proposal 8839 to study STIS CTE calibration for
extended objects. This takes images of galaxies to measure the effects of
CTE on
the isophotes of galaxies. The aim is to image small {2-3"} extended sources in
a suitably rich galaxy cluster. The target, A1689, has been observed by
WFPC2 in
the WF2 and WF4 chips {in Feb 2000}, so that cross-instrument comparison
will be
straightforward. One orbit is needed per amplifier, i.e. two orbits total.

STIS/CCD 10019

CCD Bias Monitor – Part 1

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/CCD 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)

HSTAR 9261: GS Acquisition (2,1,1) @ 002/09:16Z failed to FL backup. No
flags were set indicating SRLE. Under investigation.

COMPLETED OPS REQs: None

OPS NOTES EXECUTED: None

SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 20 20 FGS REacq 21 21 FHST Update 53 53 LOSS of LOCK

SIGNIFICANT EVENTS: None