NASA Hubble Space Telescope Daily Report # 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 0.3<z<0.8. 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
0.7<z<1.9, 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 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/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.
