Daily 3534
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3534
PERIOD COVERED: DOY 19
OBSERVATIONS SCHEDULED
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 10050
ACS Earth Flats
High signal sky flats will be obtained by observing the bright Earth
with the HRC and WFC. These observations will be used to verify the
accuracy of the flats currently used by the pipeline and will provide
a comparison with flats derived via other techniques: L-flats from
stellar observations, sky flats from stacked GO observations, and
internal flats using the calibration lamps. Weekly coronographic
monitoring is required to assess the changing position of the spots.
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/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/HRC/WFC 9919
The Morphological, Photometric, and Spectroscopic Properties of
Intermediate Redshift Cluster Galaxies:
New and fundamental constraints on the evolutionary state of high
redshift clusters will be made by obtaining deep, multiband images
{SDSS r, i, z} over the central 1.5 Mpc regions of seven distant
clusters in the range 0.76 z 1.27. The ACS data will allow us to
{1} definitively establish the morphological composition and star
formation rates as functions of clustercentric radius, local density,
x-ray luminosity {obtained from accompanying Chandra, and XMM data},
{2} explore the relationship between substructure, kinematics, and
morphology, {3} strongly constrain the galaxy merger frequency and the
origins of elliptical and S0 galaxies, {4} measure the mass
distribution independently from the light {via gravitational lensing}
enabling comparisons with kinematically derived masses, and {5} study
the evolution of the structure of the brightest cluster members. The
clusters selected for this program already have extensive
spectroscopic observations and NIR imaging is either in hand or
underway from approved ground based programs. To date, the lower part
of this redshift range has only been marginally studied with HST. Our
sample includes the two most distant, spectroscopically confirmed
superclusters and will significantly increase the baseline over which
evolutionary effects can be studied. The data will also be used to
identify very high-z galaxies via their unique spectral properties.
ACS/HRC/WFC/STIS/CCD 9836
The role of dark matter and intracluster gas in galaxy formation and
cluster evolution
We propose a fully-sampled mosaic of 41 ACS images to survey galaxy
morphologies and measure weak lensing signals to the turn-around
radius in the X-ray luminous cluster, MS0451-03 {z=0.54}. The aim is
to isolate the physical processes which affect the evolution of
cluster galaxy morphologies in the context of well-defined dynamical
system. The study will be used in contrast to a successful campaign
undertaken in Cycle 9 on a optically-selected target. By comparing
morphologies with spectroscopic and Chandra X-ray data, we will
quantify the role of the intracluster medium and associated
substructures and establish the timescales and physical regions within
which the various environmental processes occur.
ACS/WFC 9789
The Distance to the Pleiades
Despite its fundamental importance to stellar astrophysics, the
distance to the Pleiades open cluster remains in great dispute.
Main-sequence fitting results in a distance of 132.3 +/- 1.9 pc, while
the Hipparcos average parallax for Pleaides member stars gives a
distance of 116.4 +/- 2.9 pc. If the Hipparcos distance is to be
believed, our current understanding of stellar astrophysics is
dramatically incomplete. On the other hand, it has been proposed that
the Hipparcos parallax measurement to the Pleiades suffers systematic
uncertainties which result in the discrepancy with the main-sequence
fitting technique. The question will remain open until an independent
distance measurement to the Pleiades cluster is performed. We will use
ACS imaging to determine the parallax to the Pleiades to an accuracy
of about 1.5%. This will resolve the current controversy over the
distance to the cluster once and for all.
ACS/WFC 9860
ESSENCE: Measuring the Dark Energy Equation of State
The accelerating universe appears to be dominated by a dark energy
with a significant negative pressure. The ratio of the pressure to
density of this mysterious energy {its equation of state} is an
observable which can differentiate between the proliferating candidate
theories. We propose to estimate the dark energy equation of state by
observing Type Ia supernovae at redshifts near z=0.7 with HST in
concert with the on-going ESSENCE NOAO Survey program that is
discovering and studying supernovae between 0.3z0.8. We show that an
interesting constraint on the equation of state can be made with
supernovae observed at modest redshifts given the current knowledge of
the matter density. We will follow 10 Type Ia supernovae discovered
from the ground and passed to HST without disrupting its schedule. The
full data set will constrain the equation of state to 10% and strictly
limit the range of possible dark energy models. In keeping with the
ESSENCE policy, these observations will available to the community
immediately.
ACS/WFC/WFPC2 9810
Accurate and Robust Calibration of the Extragalactic Distance Scale
with the Maser Galaxy NGC4258
The extragalactic distance scale {EDS} is defined by a comparison of
Cepheid Period-Luminosity {PL} relations for nearby galaxies and the
LMC, whose uncertain distance is thereby the SOLE anchor. Studies of
maser sources orbiting the central black hole in the galaxy NGC4258
have provided the most accurate extragalactic distance ever {7.2+/-
0.5Mpc}. Since this distance is well determined and based on GEOMETRIC
arguments, NGC4258 can provide a much needed new anchor for the EDS.
We propose multi-epoch BVIH observations of NGC4258 in order to
discover about 100 Cepheids and to characterize their light curves
with 2-3 times greater accuracy than was previously possible with
WFPC2. At 90 orbits {48 in Cycle 12; 42 in Cycle 13}, this is a
relatively large program. However, the result will have a major impact
on the EDS, and substantial attention must be paid to characterization
and minimization of systematic errors, as from metallicity, crowding,
and blending. The resulting dataset will be the most complete for
Cepheids in any galaxy yet studied with HST. In an ongoing NASA-funded
program {OSS-SARA}, we are using new analysis techniques and radio
data to reduce uncertainty in the geometric distance to 3% {0.07
mag}. With this improved geometric distance and the BVIH data, we will
be able to calculate the zero point of the PL relation ROBUSTLY to 4%
{0.09 mag}.
ACS/WFC/WFPC2 9825
An ACS/WFC H-alpha Survey of the Orion Nebula
We propose to survey nearly 500 square arcminutes of the Orion Nebula
in H-alpha using the ACS/WFC, increasing the sky coverage by an order
of magnitude over the sum of all previous HST observations. This
survey will, for the first time, sample the majority of young stars
and circumstellar environments in the extended Trapezium cluster of 2,
000 low-mass stars. Our primary goal is to determine the survival rate
and statistical properties of protoplanetary disks in the type of
radiation field and dynamical environment in which most stars are
born. The survey will be used to search for new silhouette disks,
bright proplyds, microjets, large-scale outflows, and to characterize
the properties of these objects as a function of location in the
nebula. We will determine accurate proper motions in regions where
previous HST data exist. However, 90% of our fields will be observed
with HST for the first time. This survey will provide the first
complete census of pre-main sequence objects and outflows in an HII
region and will constrain the extent of hazards to planet formation in
such environments. The images will also provide a legacy for future
stellar and nebular variability studies and proper motion measurements
by providing a first epoch data base.
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.
NIC3 9998
NICMOS Cycle 12 Grism Calibration and Standard Stars to 2.5microns
This is the grism calibration proposal.
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 10033
MAMA Sensitivity and Focus Monitor Cycle 12
Monitor sensitivity of each MAMA grating mode to detect any change due
to contamination or other causes. Also monitor the STIS focus in a
spectroscopic and an imaging mode.
STIS/CCD 10017
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD.
STIS/CCD 10019
CCD Bias Monitor - Part 1
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 10069
WFPC2 CYCLE 12 Supplemental Darks, Part 1/3
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 10082
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans
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.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.)
HSTAR 9291: During ZOE, GS Acquisition (1,2,1) @ 019/12:03:39Z
resulted in FL back up (1,0,1). Under investigation.
HSTAR 9292: GS Acquisition (3,2,3) @ 019/20:12:42Z resulted in FL
backup using FGS 2 due to SSLE (QF3SSLEX) on FGS 3. Prior FHST FM
Updates @ 019/19:35:15Z and 19:38:00Z showed good attitude error
vector. FHST Map @ 019/20:32:08Z showed 3-axis (RSS) error value ~
11.00 arcsec. Subsequent GS Reacquisition (3,2,3) @ 019/21:29:47Z
resulted in FL backup. Under investigation.
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 11 11
FGS REacq 3 3
FHST Update 24 24
LOSS of LOCK
SIGNIFICANT EVENTS:
HST Command Timing test scheduled 020/12:00Z - 22:00Z with GDOC, SOC,
HITT, and CCS using CCS "D" String with CCS Release 5.0.3.1 and PRD
O06300ST. The purpose of this testing is to check the command time
for CCS Release 5.0.3.1 with historical, baselined numbers.
|