Hubble Space Telescope Daily Report #3362
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3362
PERIOD COVERED: DOY 133
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 9334
Dynamical Masses of White Dwarfs from Resolved Sirius-Like Binaries
In Cycle 8 we initiated a WFPC2 snapshot survey for resolved,
“Sirius-like”
systems containing hot white-dwarf companions of cooler main-sequence
stars. Out
of 17 systems observed to date, 8 have been resolved with WFPC2 by using
UV
filters. Two of the resolved systems—56 Persei and Zeta Cygni—have
predicted
or known orbital periods short enough that dynamical masses can be
determined
for the white dwarfs within reasonable times. These would thus add to the
extremely small number of white dwarfs presently having accurately and
directly
measured masses. We propose to image them annually in the UV with WFPC2.
In
addition, we will observe Zeta Cyg with FGS in order to measure the
absolute
motion of the optical component, needed for the mass solution. We also
propose
to observe Sirius itself with WFPC2 over the next 3 Cycles. The resulting
astrometric data will not only greatly improve the precision of the
binary
orbit
and the dynamical mass measurements for both the main-sequence and
white-dwarf
components, but will also test definitively for the claimed presence of a
third
body in this famous system.
GO 9367
Unique Opportunities to Search for the Optical Counterparts to High-Z
Damped
LyAlpha Systems
The galaxies responsible for damped LyAlpha absorption in QSO spectra are
difficult
to observe against the strong background QSO emission. We propose to
detect
even low luminosity
galaxies associated with QSO absorption line systems out to redshifts as
high as
z = 1.8 by observing them in the shadow cast by an even higher redshift
damped
LyAlpha absorber. As a result the galaxy will be observed free of
contamination
by the background AGN and of the uncertainties which arise when image
processing
techniques are required to remove the AGN emission. We propose two
approaches.
In the first we will attempt to detect a z = 1.8634 system seen in the
optical
spectrum of a high-z BL Lac object in the shadow of two higher-redshift
systems
seen in the same optical spectrum. In the second only the higher redshift
shadowing LyAlpha system is seen in the optical spectrum and the presence
of the
lower- redshift systems at z = 0.713 and z = 1.0466 are inferred from the
presence of strong MgII, SiII and FeII absorption lines.
ACS/HRC 9391
High-Resolution Imaging of Pluto’s Surface
We will collect a series of observations with the ACS/HRC from which we
will
derive a two-color global map of Pluto’s surface. We will image Pluto at
F435W
and F555W, wavelengths that have been extensively studied from the ground
over
the past 50 years. The maps will provide albedos with accurate error
determinations down to 52 degrees South latitude. These observations will
provide a second epoch of HST mapping of the active surface of Pluto as
it
continues to recede from the Sun and will provide an important context
for
other
detailed studies of Pluto.
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.
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 9488
Cosmic Shear – with ACS Pure Parallel Observations
The ACS, with greater sensitivity and sky coverage, will extend our
ability to
measure the weak gravitational lensing of galaxy images caused by the
large
scale distribution of dark matter. We propose to use the ACS in pure
parallel
{non- proprietary} mode, following the guidelines of the ACS Default Pure
Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have
measured cosmic shear at arc-min angular scales. The MDS image
parameters, in
particular the galaxy orientations and axis ratios, are such that any
residual
corrections due to errors in the PSF or jitter are much smaller than the
measured signal. This situation is in stark contrast with ground-based
observations. We have also developed a statistical analysis procedure to
derive
unbiased estimates of cosmic shear from a large number of fields, each of
which
has a very small number of galaxies. We have therefore set the stage for
measurements with the ACS at fainter apparent magnitudes and smaller, 10
arc-second scales corresponding to larger cosmological distances. We will
adapt
existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to
work
with the ACS. The analysis would also yield an online database similar to
that
in archive.stsci.edu/mds/
STIS 9507
STIS/UV snapshot survey of bright AGN
We propose a UV spectroscopic snapshot survey of bright AGN, quadrupling
the
number of Seyferts UV spectra and adding dozens of new quasars, aimed at
the
following goals: beginenumerate em Finding the relationship between the
intrinsic luminosity of the AGN and the maximum velocity {and width} of
the
outflow emanating from it, and determining the frequency of outflows in
low-z
AGN as a function of luminosity. em Surveying IGM absorption line systems
in
numerous new sight-lines. em Identifying promising targets for
observations
with
the future highly sensitive Cosmic Origin Spectrograph. endenumerate A
35-minute
snapshot with exposures in either the G140L or G230L will yield spectra
with a
minimum S/N > 15 per resolution element at all wavelengths for all our
potential
targets. This will allow us to be sensitive to absorption lines to a
limiting
equivalent width of 0.3 Angstrom at the 3 Sigma level. In order to
facilitate
rapid observational followup, we waive the data proprietary period
entirely.
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 9612
STIS CCD Hot Pixel Annealing Cycle 11
The effectiveness of the CCD hot pixel annealing process is assessed by
measuring the dark current behavior before and after annealing and by
searching
for any window contamination effects. In addition CTE performance is
examined by
looking for traps in a low signal level flat. Follows on from proposal
8906.
STIS 9613
STIS CCD Spectroscopic Flats C11
Obtain CCD flats on the STIS CCD in spectroscopic mode.
STIS 9614
STIS CCD Imaging Flats C11
Investigate flat-field stability over a monthly period.
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 9661
ACS Polarization Calibration
This proposal aims to calibrate the polarization modes most heavily used
in
Cycle 11. We need L-flat observations, observations of a polarized star
and an
unpolarized star, and an observation of an extended polarized source.
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 9688
Connecting the X-Ray and UV Ionized Absorbers in MRK 279
We propose a deep X-ray/UV spectroscopy campaign on the bright Seyfert 1
galaxy
MRK 279, using Chandra LETGS, HST/STIS, and FUSE. Our main scientific
goal
is to
study the AGN outflow seen as an ionized absorber in this galaxy,
focusing on
the crucial connection between the X-ray and UV manifestations of the
outflows.
We will map the ionization and velocity structure, measure the elemental
abundances and then determine the mass and kinetic luminosity flux of the
outflow- all stepping stones for studying the importance of outflows in
the
evolution of AGN and their host galaxies. In addition we will use the
LETGS
data
to determine the existence of relativistic CNO emission lines in the
spectrum.
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.
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.
WFPC2 9710
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTAR 9033: Solar Array Section 3 anomaly re-occurrence. Through
examination of EPS
daily plots, a temporary re-occurrence of the SA
Section 3 (-E SPA) anomaly from
Day 036 where part of a SA “circuit” shorted to
structure ground. The Day 126
event occurred while in trickle-charge and was
sustained for approximately 18
seconds. As with the Day 036 event (HSTAR 8923),
structure current was present
with a peak of 1.6 Amps as was the indicated
increase in Section 3 current reading.
Following the 18 second event, the structure
current
and SA Section 3 current
returned to normal. Under investigation.
COMPLETED OPS REQs: None
OPS NOTES EXECUTED:
1108-2 Perform Observation Re-Dumps on the Partial Obs. Level @
133/1322z,
134/0009z
SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 08 08FGS REacq 08 08 FHST Update 17 17 LOSS of LOCK
SIGNIFICANT EVENTS: None
