HST Daily Report # 3339

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3339

PERIOD COVERED: DOY 100

OBSERVATIONS SCHEDULED

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.

WF/PC-2 9069

Proper Motions in Extragalactic Optical Jets.

parameter in our understanding of these objects. We would like to build
on our
successful HST proper motion measurements in M87, and propose similar
measurements in four other optical jets.

STIS/CCD/MA1 9357

Towards a global understanding of accretion physics –, Clues from an UV
spectroscopic survey of cataclysmic variables

Accretion inflows and outflows are fundamental phenomena in a wide
variety of
astrophysical environments, such as Young Stellar Objects, galactic
binaries,
and AGN. Observationally, cataclysmic variables {CVs} are particularly
well
suited for the study of accretion processes. We propose to carry out a
STIS UV
spectroscopic snapshot survey of CVs that fully exploits the diagnostic
potential of these objects for our understanding of accretion physics.
This
survey will provide an homogenous database of accretion disc and wind
outflow
spectra covering a wide range of mass transfer rates and binary
inclinations. We
will analyse these spectra with state-of-the-art accretion disc model
spectra
{SYNDISK}, testing our current knowledge of the accretion disc structure,
and,
thereby, providing new insight into the so far not well understood
process of
viscous dissipation. We will use our parameterised wind model PYTHON for
the
analysis of the radiation driven accretion disc wind spectra, assessing
the
fundamental question whether the mass loss rate correlates with the disc
luminosity. In addition, our survey data will identify a number of
systems in
which the white dwarf significantly contributes to the UV flux,
permitting an
analysis of the impact of mass accretion on the evolution of these
compact
stars. This survey will at least double, if not triple, the number of
high-quality accretion disc / wind outflow / accreting white dwarf
spectra, and
we waive our proprietary rights to permit a timely use of this database.

ACS 9363

Ultra Low Surface Brightness Galaxies

Extremely low surface brightness galaxies have been detected in the Virgo
cluster, which are 2 magnitudes fainter than any previously known in that
cluster or even in the Local Group. ACS images of three of these should
resolve
stars at the giant branch tip, and allow us to determine distances, mean
metal
abundance of the stars, and rough ages. Confirmation of the nature of
these
galaxies will provide evidence that dark matter halos are pervasive in
the
universe, extending to galaxies with stellar densities 6 times lower than
currently known. These resolved stars would be the most distant yet
observed
accurately by HST.

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.

STIS 9509

Probing the Distance and Structure of the LMC Using Eclipsing Binaries:
STIS

The distance to the LMC is crucial to calibrating the Cosmic Distance
Scale but
remains controversial and uncertain despite the efforts of many
investigators.
We have shown that the analysis of eclipsing binary {EB} systems has the
potential to resolve this controversy. We have determined accurate
distances to
three eclipsing binaries in the LMC. Two EBs in the LMC bar, HV 2274 and
EROS
1044, yield a consistent distance of 46.0+/-1.2 kpc for the bar itself. A
third
system, HV 982, is located at a greater distance {50.2+/-1.2 kpc}, which
is
similar to that of the nearby SN 1987A {51.4+/-1.2 kpc}. These results
may
suggest a significant depth to the LMC populations but a larger stellar
sample
is needed to verify this. The distances of the program stars were derived
from
ground-based light curves, HST or CTIO radial velocity data, and HST
UV/optical
spectrophotometry. We propose HST/STIS low-resolution spectra of seven
LMC EBs
for which we already have radial velocity and light curves. This will
permit us
to complete the analysis and derive accurate {to ~3%} individual
distances.
HST/STIS spectroscopy {covering 115-800nm} is a key dataset because it
provides
Teff, Fe/H, and A_lambda. The ensemble of targets, in addition to nailing
down
the distance to the LMC, will provide fundamental stellar properties and
a
detailed probe of the structure and spatial extent of this important
galaxy, in
particular its line-of-sight depth.

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 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.

ACS 9649

ACS internal CTE monitor

The charge transfer efficiency {CTE} of the ACS CCD detectors will
decline as
damage due to on-orbit radiation exposure accumulates. This degradation
will be
closely monitored at regular intervals, because it is likely to determine
the
useful lifetime of the CCDs. All the data for this program is acquired
using
internal targets {lamps} only, so all of the exposures should be taken
during
Earth occultation time {but not during SAA passages}. This program
emulates the
ACS pre-flight ground calibration and post-launch SMOV testing {program
8948},
so that results from each epoch can be directly compared. Extended Pixel
Edge
Response {EPER} and First Pixel Response {FPR} data will be obtained over
a
range of signal levels for both the Wide Field Channel {WFC}, and the
High
Resolution Channel {HRC}.

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/WFC 9682

The Physics of Relativistic Jets: Deep Chandra and HST Observations of
Two
Newly
Discovered Jets

We propose deep observations of two X-ray-bright jets newly discovered in
our
A02 Survey, both with optical counterparts in our HST images. The targets
were
selected because of their interesting physical properties. Our goals are
to
obtain high-quality x-ray and optical images to study the jet
morphologies and
determine the x-ray and optical spectra. Both the morphologies and
spectra will
test the origin of x-rays, whether they are from inverse Compton on
microwave
background phtons vs direct synchrotron emission, allowing us to
determine the
jet physical parameters {Lorentz factors, particle distributions, and
beaming}
at different locations in the jet. This has important implications on the
modes
of energy transport and dissipation in relativistic jets.

ACS/WFC/HRC 9696

Hubble Heritage observations of NGC 3370

Hubble Heritage proposes to observe NGC 3370 in conjunction with GO
program
9351
{PI Adam Riess} to use the combined data to produce a three color image.

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

WFPC2 9709

POMS Test Proposal: WFII parallel archive proposal

used to take paralell images of random areas of the sky, following the
recommendations of the 2002 Parallels Working Group.

WFPC2 9710

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

ACS/WFC 9715

Short ACS/WFC Darks and Bias Analysis

The current ACS/WFC bias correction is not optimal. Small residuals are
due to
the random offset between the bias level in the active area and in the
overscan
region selected as reference. In addition in science and dark frames the
bias
level of amplifier B shows a bimodal distribution which is however not
observed
in bias frames. The use of normal bias frames to correct B amp images can
result
in a bias jump between amp A and B. Since bias frames are readout with a
clocking pattern slightly different from the dark and science ones we
propose to
investigate if short darks {0.5sec} can be used as replacement of bias
frames.

FLIGHT OPERATIONS SUMMARY:

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

COMPLETED OPS REQs: NONE

OPS NOTES EXECUTED: NONE

                              SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq                  7                          7
FGS REacq                  9                          9
FHST Update                19                        19
LOSS of LOCK

SIGNIFICANT EVENTS: FOT real-time spacecraft operations continue from the
GSFC MOR,
pending study of SIMOR commercial power loss event. Expect return to
SIMOR
today on evening shift. HST-FSB3 Server remains inoperative.