HUBBLE SPACE TELESCOPE
DAILY REPORT # 3173
PERIOD COVERED: DOY 218
OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)
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.
STIS/CCD 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the
darks.
STIS/CCD 8904
Bias Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias
in
the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in
order
to build up high-S/N superbiases and track the evolution of hot columns.
STIS/MA1/MA2 8920
Cycle 10 MAMA Dark Measurements.
the MAMA detector dark noise, and is the primary means of checking on health
of
the MAMA detectors systems through frequent monitoring of the background
count
rate.
WFPC2 8934
WFPC2 Decontaminations and Associated Observations Pt. 3/3
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.
WFPC2 8938
WFPC2 CYCLE 9 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/CCD 9317
Pure Parallel Imaging Program: Cycle 10.
The Space Telescope Imaging Spectrograph (CCD) was used to perform the
default
archival pure parallel program for STIS during cycle 10.
GO 9344
The Asymmetric Atmosphere of Uranus
We propose to image Uranus as the planet plunges toward equinox in 2007.
Recent
HST images during this unique epoch {6818: Hammel, Lockwood, and Rages;
7429:
Tomasko and Karkoschka; 7885: Hammel, Karkoschka, and Marley} have
revealed: {i}
strongly wavelength-dependent latitudinal structure, {ii} the presence of
numerous visible-wavelength cloud features in the northern hemisphere, {iii}
zonal winds which may deviate from the smooth profile implied by the Voyager
observations in 1986, and, {iv} in the near-IR, discrete features northward
of
+25 degs that have the highest contrast ever seen for a Uranian cloud
{Karkoschka 1998, Science 393, 765-767; Hammel et al. 2001, Icarus 153,
229-235}. Specific scientific issues we will address with new observations
are:
whether the northern features are indicative of intrinsic change or result
simply from a change of viewing angle; the shape and stability of the zonal
wind
profile; and the source of the as-yet unexplained variations of the
atmospheric
reflectivity. When possible, observations will be coordinated with
ground-based
imaging, spectroscopy, and photometry. This period approaching equinox is
the
first opportunity {in the era of modern instrumentation} to examine the far
regions of the northern hemisphere on Uranus.
NICMOS 9360
Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample
We propose to carry out a NICMOS snapshot survey in the Paschen-alpha
{PAlpha}
emission line and H-band of the sample of galaxies being observed at 3.5 --
160
microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related
guaranteed
time survey of starburst galaxies. The PAlpha images, accessible only from
HST,
will be combined with groundbased HAlpha imaging to measure the extinction
in
the star-forming centers of these galaxies, and obtain robust, extinction-
corrected maps of the massive star formation rate {SFR}. The PAlpha data by
themselves will provide reliable `extinction- free' SFRs, and a
cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The
PAlpha--based SFR measurements will extend the SFR-vs.-gas density law
{Schmidt--law} to surface densities at least 30 times higher than what is
accessible using HAlpha--based SFR measurements alone, bridging the gap
between
normal galaxies and IR--luminous starbursts. Furthermore, the combination
of the
HST PAlpha images with the SIRTF images and spectra, as well as ancillary
ground--based UBVRIJHK images and GALEX UV images being obtained as part of
the
SINGS project, will provide a definitive study of the radiative transfer of
starlight and dust heating in star--forming galaxies. The processed NICMOS
images will be incorporated into the public SINGS Legacy Data Archive, to
enable
scores of follow-up studies by the astronomical community at large.
NICMOS 9386
Infrared Photometry of a Statistically Significant Sample of KBOs
While the discovery rate of Kuiper Belt objects is accelerating, the
physical
study of this new region of the solar system has been slowed by a lack of
basic
astrophysical data. Photometric observations of the majority of the more
than
400 known KBOs and Centaurs are rudimentary and incomplete, particularly in
the
infrared. The multicolor optical-infrared photometry that exists for a small
subset of KBOs often shows significant discrepancies between observations by
different observers. Their intrinsic faintness puts them at the practical
limits
of ground-based systems. In July 2001 we began what will be the largest
uniform
sample of optical photometry of KBOs with a WFPC2 SNAPSHOT program that will
perform accurate photometry at V, R, and I on a sample of up to 150 targets.
We
seek to greatly enhance the value of this survey by obtaining J and H
photometry
on the same sample using NICMOS. Combined optical and infrared broad band
photometry is a far more powerful tool for physical studies than is either
alone. Our sample includes objects that will be observed at thermal infrared
wavelengths by SIRTF and will be used with those data to derive the first
accurate diameters, albedos, and surface properties for a large sample of
KBOs.
ACS 9425
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.
ACS 9453
The Age of the Andromeda Halo
With the advent of the ACS, we can cross a critical threshold in the study
of
galaxy formation: For the first time, we can resolve the old main sequence
stars
in the Andromeda halo, and thus directly determine the ages of the halo
stars in
a giant galaxy other than our own. As the nearest giant galaxy, Andromeda
offers
the best testing ground for understanding galaxy formation and evolution.
Resolution of its halo will tell us about its spread in age and metallicity,
thus providing a formation history. Via extensive simulations, we
demonstrate
that we can unambiguously characterize the halo population via a deep
F606W/F814W color-magnitude diagram reaching below the main sequence
turnoff.
The data will distinguish whether the halo formed quickly or through
protracted
infall and merging episodes, and would detect even a few percent trace of
intermediate age stars. Our field was carefully chosen to meet two criteria:
an
optimal stellar density ensuring adequate statistics while avoiding
overcrowding, and the inclusion of an Andromeda globular cluster matched to
the
peak halo metallicity. We also propose very brief observations in the same
two
bands of five Galactic globular clusters spanning a wide metallicity range,
thus
establishing population templates in the ACS photometric system that will be
used to calibrate and interpret the Andromeda data.
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.
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.
NICMOS 9485
Completing A Near-Infrared Search for Very Low Mass Companions to Stars
within
10 pc of the Sun
Most stars are fainter and less massive than the Sun. Nevertheless, our
knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is
quite limited. Unknown are the true luminosity function {LF}, multiplicity
fraction, mass function, and mass-luminosity relation for red and brown
dwarfs,
though they dominate the Galaxy in both numbers and total mass. The best way
to
constrain these relations is a search for faint companions to nearby stars.
Such
a search has several advantages over field surveys, including greater
sensitivity to VLM objects and the availability of precise parallaxes from
which
luminosities and masses can be derived. We propose to complete our
four-filter
NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma
detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10
and
100 AU that are at least 9 mag fainter than the empirical end of the main
sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When
completed, our search will be the largest, most sensitive, volume-limited
search
for VLM companions ever undertaken. Our four-filter search will permit
unambiguous identification of VLM-companion candidates for follow-up
observation. Together with IR speckle and deep imaging surveys, our program
will
firmly establish the LF for VLM companions at separations of 1-1000 AU and
the
multiplicity fraction of all stars within 10 pc.
ACS/CAL 9558
ACS weekly Test
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 9564
ACS Cycle 11: UV Earth Flats
This proposal will obtain sequences of UV flats by observing the bright
Earth.
The HRC UV filters were chosen for modes which were not obtained in the lab.
Since the UV transmission is likely to vary as a function of position on the
Pol_UV filters and on the coronograph, and since this behavior is currently
unconstrained by measurement, a good estimate for the missing UV flats
cannot be
made. Although POL_UV and CORON transmissions change little at long
wavelengths,
the UV transmission may change by amounts larger than can be estimated in
the
absence of actual UV transmission measurements
ACS 9565
ACS Post-SMOV UV Contamination Monitor
This programme continues the UV sensitivity monitoring campaign {ACS SMOV
proposal 9010} of the HRC and SBC after the end of the SMOV period.
ACS 9567
SBC Dark Current
Dark current measurements will be made for the ACS SBC once a week.
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.
WFPC2 9676
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:
HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)
HSTARS: None
COMPLETED OPS REQs: None
OPS NOTES EXECUTED:
1004-2 Update Pressure-Based Battery Capacity Equations
0911-0 Limit Management During WFPC2 Decontamination (M001)
0911-0 Limit Management During WFPC2 Decontamination (M001)
0900-1 COMMAND PROBLEM
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 9 9
FGS REacq 6 6
FHST Update 20 20
LOSS of LOCK
Operations Notes:
1. First command (NOOP) sent to HST via the IP command path @ 218/14:36:07z.
2. ESB code 103 is "Block load interrupted a block load" due to the command
dropout on day 219 (CDS # 30839).
SIGNIFICANT EVENTS:
HST On-Orbit Checkout of real-time WSC interface scheduled daily 217 - 224
with GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS "G" String with
CCS Release 4.0.1 and PRD D06100R2. The purpose of this testing is
to verify CCS Release 4.0.1 (IP) capability to interface through the
IP Packet Filters to WSC for real-time telemetry and commands.
HST On-Orbit Checkout of real-time DSMC interface test scheduled
219/13:22Z - 13:31Z, 1506Z - 15:15Z, and 16:51Z - 17:06Z with NCC GTD,
WSC TC, GDOC, HITT, I&C, and CCS using CCS "G" String with Release 4.0.1
and PRD D06100R2. The purpose of this testing is verify CCS Release
4.0.1 (IP) is capable of interfacing through the IP Packet Filters
to the DSMC for ODMs and GCMRs.
HST CCS 4.0.1 Case 17, NSSC-1 and SI Operations Regression test
scheduled 219/11:00Z - 20:00Z with GDOC, IDOC, HITT, SE, and VEST
using CCS "B" String with CCS Release 4.0.1 and PRD D06100R2. The
purpose of this testing is to verify the CCS Release 4.0.1 supports
normal NSSC-1 and SI commanding in an operational scenario.
