Daily 3431

HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3431

PERIOD COVERED: DOY 232

OBSERVATIONS SCHEDULED

ACS 9658

ACS Earth Flats

This program will obtain sequences of flat field images by observing
the bright Earth. Several UV filters from the interim calibration
program {9564} require additional exposures to obtain the required
illumination. A few UV filters from this program will be repeated to
monitor for changes in the flat fields and to verify the interim
results. Since no streaks are observed in the UV, the wavelength
coverage is extended to longer wavelengths in order to explore the
severity of streaks in the flats from clouds in the FOV. We have added
exposures for the HRC in the visible filters to verify the results
derived from the L-flat campaign and to explore the severity of
streaks. We have also added exposures on WFC using the minimum
exposure time and using filters which will not saturate the brightest
WFC pixel by more than 10 times the full well.

ACS 9675

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 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.

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. HST is the only facility that can be used to search
for binaries among such faint objects {V>17.5}. 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 9853

A Search for Young Binary Brown Dwarfs: Constraining Formation
Scenarios and Masses Through Multiplicity

We propose to use the Advanced Camera for Surveys / High Resolution
Camera to conduct a direct imaging multiplicity survey of 34 young
brown dwarfs in the nearest regions of recent star formation, the T
association Taurus-Auriga and the OB association Upper Scorpius. The
determined multiplicity fraction, the separation distribution, and the
mass ratio distribution will offer stringent observational constraints
on proposed brown dwarf formation scenarios. Moreover, the small
semi-major axes of known field and open cluster brown dwarf binaries
suggest the exciting possibility of our identifying several very close
binaries {< 15 AU}. Continued monitoring of these systems would yield,
on a decade timescale, the first dynamical mass estimates of T Tauri
brown dwarfs. With masses intermediate between those of stars and
planets, brown dwarfs offer our best hope of relating the reasonably
well understood processes of star formation to the less well
understood processes of planet formation.

ACS/HRC 9990

Investigating the multiplicity of the L dwarf LHS 102B

Cycle 11 NICMOS images of LHS 102B {Program 9485} suggest that the L
dwarf is a close visual binary separated by about 88 milliarcsec,
which corresponds to an apparent physical separation of 0.85 AU. We
will image this L dwarf with the HRC approximately one year after the
NICMOS observations to confirm this probable binarity and to
investigate the nature of another faint object located within 2 arcsec
of LHS 102B.

ACS/WFC 9991

The Orbit of a Newly Discovered Transneptunian Binary

We have recently discovered a binary companion to the transneptunian
object {TNO} 1999 RZ253. We are requesting rapid followup observations
during cycle 12 to make observations sufficient for a preliminary
characterization of the orbital period, semimajor axis, eccentricity,
and inclination. In particular, it is urgent to determine if this
object is a candidate for observable mutual events in the near future,
a possibility that would greatly add to its scientific interest. The
study of TNBs is in a stage of explosive growth, fueled in large part
by the capabilities of HST that we seek to exploit.

ACS/WFC/HRC 9771

The local Hubble flow and the density field within 6 Mpc

Great progress has been made recently in accurate distance
measurements of nearby galaxies beyond the Local Group based on the
luminosity of the tip of the red giant branch {TRGB}. Over the last
three years, snapshot surveys with HST have provided us with the TRGB
distances for more than a hundred nearby galaxies obtained with an
accuracy of about 10%. The local velocity field within 5 Mpc exhibits
a significant anisotropy which disagrees with a spherical
Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms
deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter
can only realize such low dispersions with a combination of a low mean
density of matter and a substantial component with negative pressure.
There may be a constraint on the equation of state w=-p/rho. Our
observations will concentrate on 116 galaxies whose expected distances
lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution
in the Local Volume with twice the information currently available.
The program is a good one for SNAP mode because the order and rate
that the observations are made are not very important, as long as
there is good completion over several years.

FGS 9881

Dynamical Masses and Radii of Four White Dwarf Stars

The cool white dwarf stars WD1639+153 and WD1818+126 were recently
resolved by HST FGS1r to be double degenerate binary systems with
projected separations of 112 mas and 174 mas respectively. At a
distance of less than 50 pc they may both have periods shorter than
about 20 years, making them ideal candidates for follow up studies for
dynamical mass determinations. This will increase the number of white
dwarfs with dynamical mass measurements from the current 4 up to 8.
Continued observations of these white dwarfs along with nearby field
stars with the FGS will accurately determine the orbital elements and
parallax of each system. The mass and radius of all four white dwarfs
can be determined to an unprecedented 1%, making it possible to test
and calibrate the theoretical white dwarf mass radius relation at the
cool end of the cooling curve for the DA and DC subclasses. Since the
components of the binary are coeval, once the mass and radius, and
hence the cooling age of each star is known, it will be possible to
estimate the relation between the initial mass and final mass for all
four white dwarfs. We are requesting a total of 4 HST orbits per year
for the next three cycles to initiate the process that will result in
a determination of the mass and radius of the four white dwarfs.

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.

NIC1/NIC2 10063

NICMOS Focus and PAM Grid Tilt Tests

The purpose of this proposal is to determine if the focus has changed
during the safing of NICMOS during the recent shutdown of the NCS, as
well as to determine if the tilt of the PAM needs to be corrected. The
program consists of: Visit 01: Focus sweep using NIC2 Visit 02: Focus
sweep using NIC1 Visit 03: Uplink of PAM settings {on hold pending
evaluation of visit 1 and 2} Visit 04: Focus sweep using NIC3 {on hold
pending evaluation of visit 1 and 2} Visit 05: PAM X/Y grid tilt for
NIC1 {on hold pending evaluation of visit 1 and 2} Visit 06: PAM X/Y
grid tilt for NIC2 {on hold pending evaluation of visit 1 and 2} Visit
07: Uplink of PAM X/Y parameters {on hold pending execution of visit 5
and 6} After the focus sweeps with NIC1 and NIC2, the focus parameters
will be evaluated together with a rough estimate of the coma. The
results of this evaluation may lead to a decision to perform a focus
sweep with NIC3 and/or a measurement of the PAM tilt grid. No
measurement of the PAM tilt grid are planned for NIC3. The focus
sweeps are based on the normal focus monitoring proposal 9637. The
tilt grid measurements are based proposal 8977 {NIC1} and 9645 {NIC2}.

NIC3/NIC2/NIC3 10064

Mini-SMOV NICMOS dark current, shading profile, and read noise program

The purpose of this proposal is to study the dark current, read noise,
and shading profile for all three NICMOS detectors after the NICMOS
starts operating due to safing. This proposal is a version of the
NICMOS monitoring program.

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.

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 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 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.

STIS/CCD 10000

STIS Pure Parallel Imaging Program: Cycle 12

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

STIS/CCD/MA1 9894

UV Spectroscopic Observations of Luminous Narrow-line Seyfert 1 Galaxies

Narrow-line Seyfert 1 galaxies {NLS1s} have remarkably different
properties than Active Galactic Nuclei with broad optical lines. The
most promising explanation for this behavior is that NLS1s have a
higher accretion rate relative to Eddington {L/M} than do broad-line
Seyferts. Despite uniformity in optical line properties, detailed
analysis reveals a divergence of the UV emission line properties that
can be traced differences in the shape of the continuum. A link with
similarly divergent X-ray properties suggests that there may be
variations in L/M even among NLS1s. To test this scenario, we propose
UV spectroscopic of two X-ray extreme NLS1s. These observations offer
the opportunity to advance our understanding in the scatter in the
relationship between line width and black hole mass, to understand
physics of gas in AGN optical and UV emission-line regions, and to
understand recently-discovered peculiar line-less high-z quasars that
may be the early universe counterpart of luminous NLS1s.

WFPC2 9595

WFPC2 CYCLE 11 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.

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.

FLIGHT OPERATIONS SUMMARY:

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

HSTAR 9118:  GS Re-acquisition (2,1,1) @ 227/20:53:03Z required tw
attempts to achieve                        FLDV on review of TC error
log from PTAS run of SA223N SMS,              took two attempts before
achieving FLDV for this re-acquisition.                    first
attempt resulted in FGS 1 SSLEX. Under investigation.


COMPLETED OPS REQs:
17031-0  Adjust NCS PID Control Setpoints @ 232/20:08z

OPS NOTES EXECUTED: NONE

                           SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq               09                        09
FGS REacq               02                        02
FHST Update             32                        32
LOSS of LOCK


SIGNIFICANT EVENTS:

Successfully adjusted NCS PID control setpoints @ 232/20:08Z to change
the detector temperature.  The Prime (dewar, NOT active), and the
Alternate (weighted average neon, ACTIVE) control points were set to
77.25 K and 72.45 K, respectively (OR 17031).  The Compressor speed
under PID control dropped just noticeably in speed to affect the
commanded increase in control point temperature.  MNCOINTRL
successfully achieved 72.45 K at 232/20:17Z and system operation
appears to be continuing nominally.

Completed CCS Release 5.0.3 Events Analyzer Comparison Test on Day 230
and 231 using CCS "D" and "B" Strings.  The first part of the test
ingesting real-time data was mostly successful, except for several
data drops on the "D" String while a science data playback was being
transmitted from the HST through the CCS and HSTPS systems using
Packet Filter 1.  The second part of the test using the PSSs as data
sources was also mostly successful.  There were several command data
drops from both the "B" and "D" Strings using Packet Filter 15.  This
happened when sending FIVEBLCKs and NSSC-1 FSW loads.  Lastly, the new
"Key Monitor" was tried out on "D" String Test mode.  Issue 19 was
added to the CCS 5.0.3 Test Matrix to have CCS Development/Response
Team copy the canned request job to the Test side of "D" String.