HST Daily Report # 3295

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3295

PERIOD COVERED: DOY 36

OBSERVATIONS SCHEDULED

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 9374

The FUV Flux Irradiating the Surfaces of Protostellar Disks

We propose to use STIS to determine the Far-Ultraviolet {FUV} radiation
field in
3 proto-planetary disk systems. These systems: LkCa 15, GM Aur, and DM
Tau, are
among a handful of sources that can be subjected to detailed chemical
studies
with the current generation of millimeter-wave instruments. Such studies
have
found that the disks have a rich molecular chemistry, which appears to be
controlled by the FUV radiation field {Qi 2001; Dutrey et al 1997;
Kastner
et al
1997}. These observations will allow, for the first time, a firm
characterization of the FUV radiation field impinging on the surfaces of
circumstellar disks. Knowledge of the FUV field for each object will
allow for
theoretical chemical models to be created specific to each object and
compared
to observations. Since these objects will remain, for some time, the main
templates for chemical studies of extra-solar disks this project will
provide
the real UV data required to push theory forward. Given that molecules
are
excellent probes of their environment, the new information will place
better
constraints on the virtually unknown vertical structure of
proto-planetary
disks. This project is unique in scope and will increase our limited
understanding of disk chemical evolution, but also improve our knowledge
of
uncertain physical processes, such as the possible dissipation of outer
disks by
photo-evaporation and on the timescales of dust grain growth.

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 9426

Jupiter’s Ring Plane Crossing of 2002-2003

Jupiter’s ring system consists of three components: the main band, the
vertically-extended inner halo and the exterior gossamer rings. Each
component
illustrates aspects of dust dynamics within Jupiter’s inclined magnetic
field
and its strong plasma environment. We will image all three components
with ACS
during an unusual, extended period of edge-on viewing, December 2002
through
February 2003. For faint planetary rings, this geometry improves the
signal-to-noise ratio considerably and permits an unambiguous decoupling
of
radial and vertical structure. Although the Jovian rings have been
examined by
four spacecraft and from the ground, we are still lacking in a systematic
set of
data that can distinguish between the ring’s prominent dust population
and its
embedded macroscopic source bodies. We also do not know the size
distribution of
dust with sufficient accuracy to test rival theories of ring origin.
Observations of the system at a range of wavelengths and phase angles
with ACS
will finally make this determination possible. Coordinated observations
at the
W. M. Keck Telescope will extend our wavelength coverage well into the
IR.

ACS/WFC 9433

The Size Distribution of Kuiper Belt Bodies

The Kuiper Belt is a population of remnant planetesimals from the
formation of
the Solar System. Since the planetesimals in extrasolar systems are too
faint to
see with present or planned telescopes, the Kuiper Belt is our best
chance to
test models of accretional/collisional evolution against observations.
Current
ground-based observations of Kuiper Belt Objects {KBOs} are consistent
with a
pure power law size distribution N{D}propto D^-q, q~4.3. Current
accretion
models predict a break to a shallower slope q=3.5 for objects of diameter
D<~100
km. We will conduct a survey of 6 ACS/WFC fields to detect KBOs with
R<28.5, and
diameters as small as D~10 km. The number of KBOs at these small sizes,
unmeasurable from the ground, will test the existence of the predicted
break
with 95% confidence—we expect between 12 and 50 detections. A census of
small
KBOs is also important in confirming the idea that short-period comets
are
errant KBOs. With HST and ground- based followup, we can determine
orbital
parameters for the detected KBOs, and search for dynamical populations
which may
be deficient in D>100 km KBOs and hence not yet detected. In particular,
we
will
determine whether the current absence of objects with perihelia beyond 50
AU is
due to a truncation of the protoplanetary disk at some point in Solar
System
history, or just a failure to accrete D>150 km objects.

ACS 9463

Are OH/IR stars the youngest post-AGB stars? An ACS SNAPshot imaging
survey

Essentially all well-characterized preplanetary nebulae {PPNs}– 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
propose an ACS/SNAPshot imaging survey of a large, morphologically
unbiased
sample of these objects, selected using their IRAS 12-to-25micron colors.
Our
ground-based imaging study of OH/IR stars has revealed a few compact
bipolar
objects, supporting our hypothesis. However since most objects remain
unresolved, HST observations are needed to determine how and when the
bipolar
geometry asserts itself. 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 PPNs, are common or rare phenomena.

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.

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.

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 9605

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD

STIS 9607

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 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.

STIS/CCD 9622

CCD Full-Field Sensitivity Monitor C11

Measure a photometric standard star field in Omega Cen in 50CCD mode once
per
year to monitor CCD sensitivity over the whole field of view. Keep the
spacecraft orientation within a suitable range {+/- 5 degrees} to keep
the same
stars in the same part of the CCD for every measurement. This test will
give a
direct transformation of the 50CCD magnitudes to the Johnson-Cousins
system for
red sources. These transformations should be accurate to 1%. The
stability of
these transformations will be measured to the sub-percent level. These
observations also provide a check of the astrometric and PSF stability of
the
instrument over its full field of view.

STIS 9625

STIS NUV-MAMA Cycle 11 Flats

This program will obtain NUV-MAMA observations of the STIS internal
Deuterium
lamp to construct an NUV flat applicable to all NUV modes

ACS 9673

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

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.

ACS 9681

Probing the Structure of the Narrow-Line Region in Seyfert Galaxies with
CXO
Imaging Spectroscopy

One of the most striking aspects of the Seyfert phenomenon is the conical
structure of the Narrow Emission Line Regions {NLRs} which, in the
Unified
Model, is the result of collimation of the ionizing radiation. Recent HST
imaging spectroscopy shows evidence of accelerating mass outflows and
rich
dynamics. The handful of sources with known extended NLRs that have been
imaged
to date with CXO reveal tantalizing insights into an NLR/X-Ray
connection. Here
we propose to obtain 20 ksec images of the 8 next best targets. All of
these
Seyferts show [OIII] emission on scale > few arcsec, hence easily
resolvable by
CXO. Our prime goal is to address whether there is indeed a correlation
between
the extended x-ray structure and other properties of the NLR.

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 9706

STIS Pure Parallel Imaging Program: Cycle 10

FLIGHT OPERATIONS SUMMARY:

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

Four Structure Currents mnemonics (CSTRUCCP, CSTRUCCR, CSFSCUR,
CSFSCUR1),
2 primary and
2 redundant, flagged OOL high @ 036/12:25:27Z. Currents returned to
normal at entry
orbit night. Structure Currents flagged OOL high again the next orbit
coincident with
-E Trim Relay opening. See HSTAR 8923. The anomalous current is
believed
to be caused
by a short of a SA string to structure. Preliminary assessment by the
Tiger team indicates
no health and safety risk to the vehicle. Battery charging and load
share
are nominal with
little to no impact observed during the full trickle charge periods. All
other subsystems
reported nominal operations.

At 036/23:37Z the anomalous structure current was not present during the
Trickle
Charge period, indicating the fault has cleared. Preliminary analysis
indicates
the fault cleared at the opening of the -E SPA.

HSTAR 8923: Four Structure Current mnemonics (2 primary, 2 redundant)
flagged OOL
high @ 036/12:25:22Z. CSTRUCCP = 1.4 Amp. (yellow high limit 1.2 Amp.),
CSTRUCCR = 1.2 Amp.
(yellow high limit 1.0 Amp.), CSFSCUR = 1.4 Amp. (red high limit 1.2
Amp.),
and
CSFSCUR1 = 1.2 (red high limit 1.0 Amp.) CSTRUCCP toggled in-and-out of
limits while
the other three mnemonics were continuously OOL until LOS @
036/12:39:00Z. At AOS
(036/12:57:39Z), all mnemonics were in bounds. At 036/14:06:17Z all four
mnemonics
flagged again until LOS @ 036/14:21:30Z. At AOS (036/14:33:30Z) all
mnemonics were
in bounds. Vehicle was in orbit day in both cases.

COMPLETED OPS REQs: None

OPS NOTES EXECUTED: None

                         SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq             8                          8
FGS REacq             10                        10
FHST Update           16                        16
LOSS of LOCK

SIGNIFICANT EVENTS: See above information from System Engineering flash
reports
and HSTAR 8923.