Daily 3580

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3580

PERIOD COVERED: DOY 89

OBSERVATIONS SCHEDULED

ACS 9475

ACS coronagraphic survey for debris disks around nearby stars

We propose a comprehensive imaging survey of nearby stars that will
realize the full potential of the ACS coronagraph to map debris disks,
the extrasolar analogs of our Kuiper Belt. Most debris disks are
detected only by excess thermal emission at far-infrared wavelengths.
Because they have a factor of 100 less dust cross section than the
young debris disks around HR 4796A and beta Pic, they are undetectable
by present techniques. In simulations of disk detectability, Kalas and
Jewitt {1996} determined that detecting the scattered light from the
disk requires at least two orders of magnitude of supression of the
central PSF than is attainable from the ground. The ACS coronagraph
finally provides this increase in sensitivity, surpassing the WFPC2
sensitivity to faint nebulosity near bright stars by at least three
orders of magnitude. Mapping the debris around stars is particularly
important for the indirect detection of planet-mass objects. Dynamical
models have shown that unseen perturbers dynamically modify the
radial, azimuthal and vertical structure of debris disks. These data
will provide the critical high-resolution mapping of debris disks.

ACS/HRC 9747

An Imaging Survey of the Statistical Frequency of Binaries Among
Exceptionally-Young Dynamical Families in the Main Asteroid Belt

We propose an ambitious SNAPSHOT program to determine the frequency of
binaries among two very young asteroid families in the Main Belt, with
potentially profound implications. These families {of C- and S-type}
have recently been discovered {Nesvorny et al. 2002, Nature 417, 720},
through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY
ago in catastrophic impact events. This is the first time such
precise and young ages have been assigned to a family. Main-belt
binaries are almost certainly produced by collisions, and we would
expect a young family to have a significantly higher frequency of
binaries than the background, because they may not yet have been
destroyed by impact or longer-term gravitational instabilities. In
fact, one of the prime observables from such an event should be the
propensity for satellites. This is the best way that new numerical
models for binary production by collisions {motivated largely by our
ground-based discoveries of satellites among larger asteroids}, can be
validated and calibrated. We will also measure two control clusters,
one being an "old" family, and the other a collection of background
asteroids that do not have a family association, and further compare
with our determined value for the frequency of large main-belt
binaries {2%}. We request visits to 180 targets, using ACS/HRC.

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 9788

A Narrow-band Snapshot Survey of Nearby Galaxies

We propose to use ACS/WFC to conduct the first comprehensive HST
narrow-band {H-alpha + [N II]} imaging survey of the central regions
of nearby bulge-dominated disk {S0 to Sbc} galaxies. This survey will
cover, at high angular resolution extending over a large field, an
unprecedented number of galaxies representing many different
environments. It will have important applications for many
astrophysical problems of current interest, and it will be an
invaluable addition to the HST legacy. The observations will be
conducted in snapshot mode, drawing targets from a complete sample of
145 galaxies selected from the Palomar spectroscopic survey of nearby
galaxies. Our group will use the data for two primary applications.
First, we will search for nuclear emission-line disks suitable for
future kinematic measurements with STIS, in order to better constrain
the recently discovered relations between black hole mass and bulge
properties. Preliminary imaging of the type proposed here must be
done, sooner or later, if we are to make progress in this exciting new
field. Second, we will investigate a number of issues related to
extragalactic star formation. Specifically, we will systematically
characterize the properties of H II regions and super star clusters on
all galactic scales, from circumnuclear regions to the large-scale
disk.

ACS/WFC/WFPC2 9822

The COSMOS 2-Degree ACS Survey

We will undertake a 2 square degree imaging survey {Cosmic Evolution
Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS
equatorial field. This wide field survey is essential to understand
the interplay between Large Scale Structure {LSS} evolution and the
formation of galaxies, dark matter and AGNs and is the one region of
parameter space completely unexplored at present by HST. The
equatorial field was selected for its accessibility to all
ground-based telescopes and low IR background and because it will
eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS
instrument. The imaging will detect over 2 million objects with I 27
mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and
extremely red galaxies out to z ~ 5. COSMOS is the only HST project
specifically designed to probe the formation and evolution of
structures ranging from galaxies up to Coma-size clusters in the epoch
of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The
size of the largest structures necessitate the 2 degree field. Our
team is committed to the assembly of several public ancillary datasets
including the optical spectra, deep XMM and VLA imaging, ground-based
optical/IR imaging, UV imaging from GALEX and IR data from SIRTF.
Combining the full-spectrum multiwavelength imaging and spectroscopic
coverage with ACS sub-kpc resolution, COSMOS will be Hubble's ultimate
legacy for understanding the evolution of both the visible and dark
universe.

FGS 9879

An Astrometric Calibration of the Cepheid Period-Luminosity Relation

We propose to measure the parallaxes of 10 Galactic Cepheid variables.
There is no other instrument on or off the earth that can consistently
deliver HST FGS level of precision for critical parallaxes. When these
parallaxes {with 1-sigma precisions of 10% or better} are added to our
recent HST FGS parallax determination of delta Cep {Benedict et al
2002}, we anticipate determining the Period-Luminosity relation zero
point with a 0.03 mag precision. In addition to permitting the test of
assumptions that enter into other Cepheid distance determination
techniques, this calibration will reintroduce Galactic Cepheids as a
fundamental step in the extragalactic distance scale ladder. A
Period-Luminosity relation derived from solar metallicity Cepheids can
be applied directly to extragalactic solar metallicity Cepheids,
removing the need to bridge with the Large Magellanic Cloud and its
associated metallicity complications.

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
0.7z1.9, 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.

NIC1 9833

T Dwarf Companions: Searching for the Coldest Brown Dwarfs

Faint companions to known stars have historically led to the discovery
of new classes of stellar and substellar objects. Because these
discoveries are typically limited by the flux ratio of the components
in the system, the intrinsically faintest companions are most
effectively identified around the intrinsically faintest primaries. We
propose to use NICMOS to image a sample of 22 of the coolest known
{T-type} brown dwarfs in the Solar Neighborhood in order to search for
fainter and cooler brown dwarf companions. The high spatial resolution
of the NIC 1 detector enables us to distinguish binary systems with
apparent separations greater than 0"08, or physical separations
greater than 1.2 AU at the nominal distances of the objects in our
sample. Furthermore, the substantial sensitivity of NICMOS imaging
allows us to probe companion masses of 5-50 Jupiter masses and
companion effective temperatures of 250-1300 K in a maximally
efficient manner. Based on work to date, we expect that roughly 20% of
the objects in our sample will be binary, and that one or two of these
will likely harbor a significantly fainter secondary. Hence, we expect
to find a companion cooler than any currently known brown dwarf, a
potential prototype for the next spectral class. In addition, our
investigation will add substantially to the sample of known binary
brown dwarfs, allowing improved statistical analyses of the binary
fraction, separation distribution, and mass ratio distribution of
these systems, key quantities for probing brown dwarf formation. We
will also identify optimal substellar systems for astrometric mass
measurements, a critical check for theoretical models of brown dwarfs
and extrasolar planets.

NIC1/NIC2/NIC3 8792

NICMOS Post-SAA calibration - CR Persistence Part 3

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.

NIC3 9999

The COSMOS 2-Degree ACS Survey NICMOS Parallels

The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a
companion to program 9822.

STIS/CCD 10018

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS/CCD 10020

CCD Bias Monitor - Part 2

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,
and 1x1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.

STIS/CCD 10085

STIS Pure Parallel Imaging Program: Cycle 12

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

STIS/MA1 10034

Cycle 12 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.

WFPC2 10068

WFPC2 CYCLE 12 Standard Darks

This dark calibration program obtains dark frames every week in order
to provide data for the ongoing calibration of the CCD dark current
rate, and to monitor and characterize the evolution of hot pixels.
Over an extended period these data will also provide a monitor of
radiation damage to the CCDs.

WFPC2 10070

WFPC2 CYCLE 12 Supplemental Darks Part 2/3

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

WFPC2 10072

WFPC2 CYCLE 12 INTERNAL MONITOR

This calibration proposal is the Cycle 12 routine internal monitor for
WFPC2, to be run weekly to monitor the health of the cameras. A
variety of internal exposures are obtained in order to provide a
monitor of the integrity of the CCD camera electronics in both bays
{gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a
monitor for possible buildup of contaminants on the CCD windows.

WFPC2 10084

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 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.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.) None

COMPLETED OPS REQs:
17115-1 Load Updated Battery Reconditioning MACRO @090/0047z

OPS NOTES EXECUTED:
1213-1 Tracking waiver during Battery 2 capacity test (On going through
end of Batt#2 Test)

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 12 12
FGS REacq 02 02
FHST Update 27 27
LOSS of LOCK

SIGNIFICANT EVENTS:

Started commanding for Battery 2, Two-stage Capacity Testing @
090/01:17Z with the set-up portion of the script (OR 17017-1). SA
Section 2 was connected to Diode Bus C on first opportunity @
090/03:06Z with discharge expected to continue for approximately 54
hours. As of 090/05:00Z, Battery 2 discharge continuing nominally.
Switched from High-rate to Low-rate discharge @ 090/10:03Z.
Following completion of discharge at approximately 092/09:30Z, Battery
2 will be placed back online. At approximately 093/14:19Z, Battery 2
will placed back in FSW 6-battery system.

Ops Note 1213: Tracking waiver during Battery 2 Capacity Test.
Project has strong desire to capture all telemetry (real-time and
recorded) during the Battery 2 Capacity Test. In order to mitigate
data loss due to tracking mode changes, FDF and I&C Systems have
waived the tracking requirement during the battery discharge period.
Resume tracking one Battery 2 discharge is terminated.

Command Timing test scheduled 090/12:00Z - 22:00Z with GDOC, SOC,
HITT, and CCS using CCS "H" String with CCS Release 5.0.3.1 and PRD
O06300ST. The purpose of this testing is to check command timing for
CCS Release 5.0.3.1 with historical, baselined numbers for a standard
configuration with S-Channel data and other loads.