NASA Hubble Space Telescope Daily Report # 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 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 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 two
attempts to achieve
FLDV on FGS 1. OTA SE, in review of TC error log
from PTAS run of SA223N SMS,
found FGS 1 took two attempts before achieving FLDV
for this re-acquisition.
The 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.