HST Daily Report # 3269
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3269
PERIOD COVERED: DOYs 361- 363
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 9468
ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7
We propose an ACS grism parallel survey to search for emission-line galaxies
toward 50 random lines of sight over the redshift interval 0 < z pl 7. We
request ACS parallel observations of duration more than one orbit at high
galactic latitude to identify ~ 300 HAlpha emission-line galaxies at 0.2 pl
z pl
0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3 pl z pl 1.68, and
pg
1000 Ly-alpha emission-line galaxies at 3 pl z pl 7 with total emission line
flux f pg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain direct
images with the F814W and F606W filters and dispersed images with the
WFC/G800L
grism at each position. The direct images will serve to provide a zeroth
order
model both for wavelength calibration of the extracted 1D spectra and for
determining extraction apertures of the corresponding dispersed images. The
primary scientific objectives are as follows: {1} We will establish a
uniform
sample of HAlpha and O II emission-line galaxies at z<1.7 in order to obtain
accurate measurements of co-moving star formation rate density versus
redshift
over this redshift range. {2} We will study the spatial and statistical
distribution of star formation rate intensity in individual galaxies using
the
spatially resolved emission-line morphology in the grism images. And {3} we
will
study high-redshift universe using Ly-alpha emitting galaxies identified at
z
pl 7 in the survey. The data will be available to the community immediately
as
they are obtained.
ACS 9647
CCD Daily Monitor Part I
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 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.
ACS 9656
Stability of the ACS CCD: geometry, flat fielding, photometry
A moderately crowded stellar field, located ~6′ West of the centre of the
cluster 47 Tuc, is observed repeatedly {every three weeks with the WFC,
every
other month with the HRC} in various filters, spending 1 orbit per epoch.
Different filters will be used every time, so that over the course of the
year
all filters will have been employed at least twice. The most common filters
will
be checked more frequently. The same field has been observed in the course
of
the SMOV phase and the positions and magnitudes of the most prominent stars
have
been accurately measured. Although the field is neither a proper
astrometric nor
a proper photometric standard one, the positions and magnitudes of the
objects
in it can be used to monitor any local and large scale variations in the
platescale and sensitivity of the detectors. It should be noted that for the
filters which have already been used during the SMOV phase it will be
sufficient
to take one single image, without CR-SPLIT, since the exposure time is
always
short {20-30 sec} and there will be so many stars that the few of them
which are
affected by cosmic rays can be discarded as outliers in the photometry. For
narrow and medium band filters not exercised on this target in the SMOV
phase,
however, a baseline will have to be set. This expenditure of time will apply
to
the current cycle only. At variance with the approach used in SMOV, there is
no
need for large telescope slews to place the same objects on opposite sides
of
the detectors, thence allowing the programme to remain compact and
efficient.
All exposure level parameters are set to their default values, except for
the
amplifier gain of the WFC exposures in the F606W band, which will be
collected
with the gain value of 2 for the WFC for compatibility with the SMOV
observations. The exposure time is typically 30 seconds for the WFC, 60 sec
for
the HRC. No attempt will be made to attain a predefined or the same
orientation
on the sky amongst different epochs. Typically, for the WFC, five exposures
will
be accommodated in one orbit. For the HRC, about 10 exposures can be fitted
within one orbit
ACS 9462
Systemic and Internal Proper Motions of the Magellanic Clouds from
Astrometry
with ACS
We request first epoch observations with ACS of Magellanic Cloud fields
centered
on background quasars. Second epoch observations will be requested ~ 5 years
later to allow the measurement of the systemic and internal proper motions
of
the Clouds with error <~0.05 mas/year. These motions are of fundamental
importance. The systemic motions of the LMC and SMC probe the gravitational
potential of the dark halo. The internal proper motion due to rotation can
be
exploited to yield a rotational parallax distance to the LMC; the first time
that this will be done for any galaxy. This is particularly important for
the
LMC because of its crucial role in the extragalctic distance ladder.
Previous
measurements of the proper motion of the LMC yield a systemic component
ranging
from 1.4 mas/year to 3.4 mas/year {differing by several times the quoted
errors}, with no useful determination of the internal motions. The main
problem
with measurements of the proper motion of the LMC has been the lack of a
sample
of background quasars to use as reference frame. We have recently been able
to
identify a sample of 54 quasars behind the Magellanic Clouds from their
variability characteristics in the MACHO database. With this sample and the
advent of ACS an accurate proper motion measurement has become possible for
the
very first time.
ACS 9453
The Age of the Andromeda Halo
With the advent of the ACS, we can cross a critical threshold in the study
of
galaxy formation: For the first time, we can resolve the old main sequence
stars
in the Andromeda halo, and thus directly determine the ages of the halo
stars in
a giant galaxy other than our own. As the nearest giant galaxy, Andromeda
offers
the best testing ground for understanding galaxy formation and evolution.
Resolution of its halo will tell us about its spread in age and metallicity,
thus providing a formation history. Via extensive simulations, we
demonstrate
that we can unambiguously characterize the halo population via a deep
F606W/F814W color-magnitude diagram reaching below the main sequence
turnoff.
The data will distinguish whether the halo formed quickly or through
protracted
infall and merging episodes, and would detect even a few percent trace of
intermediate age stars. Our field was carefully chosen to meet two criteria:
an
optimal stellar density ensuring adequate statistics while avoiding
overcrowding, and the inclusion of an Andromeda globular cluster matched to
the
peak halo metallicity. We also propose very brief observations in the same
two
bands of five Galactic globular clusters spanning a wide metallicity range,
thus
establishing population templates in the ACS photometric system that will be
used to calibrate and interpret the Andromeda data.
ACS/WFC 9584
ACS Default {Archival} Pure Parallel Program II.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.
ACS/WFC 9419
The Complete IMF of a Massive Young Cluster
We propose to use the large improvement in sensitivity and wide-field
resolution
provided by ACS to obtain for the first time the complete ~ 0.1 M_Sun to ~
100
M_Sun IMF of a single massive young cluster. We will obtain BVI + nebular
deep
{V ~ 27} WFC photometry of six cluster and one background pointings and we
will
use the auto-parallel capacity of ACS to simultaneously acquire deep NUV+U+V
photometry of selected regions in the cluster. Special care has been taken
to
treat all the complications which arise in the reduction of data for the
purpose
of calculating the IMF of a young cluster. We have chosen as our object of
study
N11 in the LMC because it arguably provides the best combination of stellar
mass
range {> 40 O stars, with several O3 stars}, spatial resolution {1 WFC pixel
=
0.0125 pc}, low extinction {E{B-V} ~ 0.1}, crowding, background confusion,
and
nebular contamination in comparison to other Galactic and Local Group
clusters.
It also has the advantage of having two separate regions, one which has
already
stopped forming stars and another one which is still forming them, thus
allowing
us to search for differences in the IMF between those two cases. The ACS
data
will be complemented with IR ground-based observations obtained using Gemini
South, for which we already have been awarded time.
ACS/WFC/HRC 9075
Cosmological Parameters from Type Ia Supernovae at High Redshift.
The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble
diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as
a
record of the expansion history of the universe.
FGS 9348
The Distances to AM CVn stars
We propose to determine the parallaxes and proper motions of the five
brightest
of the seven known AM CVn systems using the HST Fine Guidance Sensors. AM
CVn
systems are binaries where mass is transferred from a completely
hydrogen-deficient, degenerate mass donor to a white dwarf primary through a
helium accretion disk. A better understanding of these systems is crucial
for a
number of reasons:, to study the late stages of binary evolution, to study
the
effect of chemical composition on the physics of accretion discs; , o to
estimate their contribution to the Supernovae Ia rate and , to estimate
their
contribution to the gravitational radiation background. All these studies
rely
critically on a determination of the distances to the currently known
systems.
With brightnesses in the range 13<V<17 and estimated distances <400pc they
are
ideal targets for the HST-FGS.
FGS/CAL 9602
Long Term Monitoring of FGS1r in Position Mode
It is known from our experience with FGS3, and later with FGS1r, that an FGS
on
orbit experiences long term evolution, presumably due to disorption of water
from the instrument’s graphite epoxy composites. This manifests principally
as a
change in the plate scale and secondarily as a change in the geometric
distortions. These effects are well modeled by adjustments to the rhoA and
kA
parameters which are used to transform the star selector servo angles into
FGS
{x, y} detector space coordinates. By observing the relative positions of
selected stars in a standard cluster at a fixed telescope pointing and
orientation, the evolution of rhoA and kA can be monitored and calibrated to
preserve the astrometric performance of FGS1r.
GTO/ACS 9290
The Nature of Galaxies at z > 4.
The Morphological, Photometric, and Spectroscopic Properties of Intermediate
Redshift Cluster. New and fundamental constraints on the evolutionary state
of
high redshift clusters will be made by obtaining deep, multiband images
{SDSS g,
r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the
range
0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM,
will
be performed over the central 750 kpc region of each system galaxy.
HST 9382
A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO
MgII-FeII Systems.
We have searched the first public release of SDSS QSO spectra for low-z
{z<1.65}
metal absorption lines and found over 200 large rest equivalent width
MgII-FeII
systems. Previously, we empirically showed that such systems are good
tracers of
large neutral gas columns, with ~50% being classical damped Lyman alpha
{DLA}
systems {N_HI>=2*10^20 cm^-2}. Here we propose to follow up a well-defined
subset of 79 of them to search for DLAs with 0.47<z<1.60. Only QSOs brighter
than g’=19 were selected. The QSO emission and DLA absorption redshifts were
constrained to virtually eliminate data loss due to intervening Lyman limit
absorption. Consequently, we expect to discover ~40 new DLAs, which is a
three-fold increase in this redshift interval. This will significantly
improve
our earlier low-z DLA statistical results on their incidence, cosmological
mass
density, and N_HI distribution. The results will also allow us to better
quantify the empirical DLA — metal-line correlation. With this improved
understanding, the need for follow-up UV spectroscopy will lessen and, with
the
release of the final database of SDSS QSO spectra {an ~25-fold increase},
the
number of low-z DLAs could be increased arbitrarily. Thus, the power of the
large and statistically-sound SDSS database in combination with a proven
technique for finding low-z DLAs will, over the next few years, essentially
solve the problem of making an accurate determination of the cosmic
evolution of
the neutral gas component down to z~0.4.
NICMOS 9636
Cycle 11 NICMOS dark current, shading profile, and read noise monitoring
program
The purpose of this proposal is to monitor the dark current, read noise, and
shading profile for all three NICMOS detectors throughout the duration of
Cycle
11. This proposal is a continuation of PID 9321 which covers the period
between
the end of SMOV3B and the onset of Cycle 11.
NICMOS 8790
NICMOS Post-SAA calibration – CR Persistence Part 1.
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.
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 9607
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 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9631
Faint Standard Extension {FASTEX}
Fainter standard stars are needed for the flux calibration of COS, for the
prism
modes on ACS, and for astronomical community, in general. The bright object
safety limit for COS is 1.25 ct/s per pixel, while the total countrate
limit per
FUV detector segment is 20000/s. In addition, the GALEX project {see
Appendix}
requires more secondary standards in the flux range of the two fainter
original
FASTEX stars. Customarily, one NASA project provides observing time in
support
of other NASA projects. The existing observations of the two fainter FASTEX
standards, WD0947+857 and WD1657+343, have the most CTE losses in the G430L
data
and are still a bit marginal on S/N. Since the stellar models are normalized
to
V, good spectrophotometry to 5500A is important. All five targets will be
observed at the new G430L aperture to minimize CTE loss and at the original
aperture to constrain CTE models. Combined with additional planned cal data
for
stars of intermediate flux, the CTE model for spectra can be tuned to cover
the
full range of signal levels.
STIS 9632
Measuring Proper Motions in the Very Fast Outflow of the Carbon star, V
Hydra
This proposal will look at V Hydra
STIS 9633
STIS parallel archive proposal – Nearby Galaxies – Imaging and Spectroscopy
Using parallel opportunities with STIS which were not allocated by the TAC,
we
propose to obtain deep STIS imagery with both the Clear {50CCD} and
Long-Pass
{F28X50LP} filters in order to make color-magnitude diagrams and luminosity
functions for nearby galaxies. For local group galaxies, we also include
G750L
slitless spectroscopy to search for e.g., Carbon stars, late M giants and
S-type
stars. This survey will be useful to study the star formation histories,
chemical evolution, and distances to these galaxies. These data will be
placed
immediately into the Hubble Data Archive.
STIS 9692
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle 10.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle 10.
STIS 9507
STIS/UV snapshot survey of bright AGN
We propose a UV spectroscopic snapshot survey of bright AGN, quadrupling the
number of Seyferts UV spectra and adding dozens of new quasars, aimed at the
following goals: beginenumerate em Finding the relationship between the
intrinsic luminosity of the AGN and the maximum velocity {and width} of the
outflow emanating from it, and determining the frequency of outflows in
low-z
AGN as a function of luminosity. em Surveying IGM absorption line systems in
numerous new sight-lines. em Identifying promising targets for observations
with
the future highly sensitive Cosmic Origin Spectrograph. endenumerate A
35-minute
snapshot with exposures in either the G140L or G230L will yield spectra with
a
minimum S/N > 15 per resolution element at all wavelengths for all our
potential
targets. This will allow us to be sensitive to absorption lines to a
limiting
equivalent width of 0.3 Angstrom at the 3 Sigma level. In order to
facilitate
rapid observational followup, we waive the data proprietary period entirely.
STIS/CCD 9066
Closing in on the Hydrogen Reionization Edge of the Universe.
The Space Telescope Imaging Spectrograph (CCD) was used in parallel
constrain
the Hydrogen reionization edge in emission that marks the transition from a
neutral to a fully ionized IGM at a predicted redshifts.
STIS/CCD 9164
Helical Flows and Rotation in Protostellar Jets.
The Space Telescope Imaging Spectrograph (CCD) was used to study the
velocity
structure of protostellar jets transverse to the jet flow axis. HST
resolution
would allow the search for rotation, e.g. a helical flow pattern, around the
axis of an optical jet. Such a detection would provide strong evidence that
jets
act as outflowing channels for angular momentum, thus allowing infalling
material to fully accrete onto the protostar.
STIS/CCD 9136
T Tauri Star Coronagraphic Survey: A PMS Protoplanetary Disk Census.
The Space Telescope Imaging Spectrograph (CCD) was used to observe pre-main
sequence solar-mass stars, the T Tauri stars that Millimeter and IR studies
suggest at least 50 percent have circumstellar disks similar to the disk
from
which our planetary system formed. High spatial resolution, high dynamic
range
imaging of such systems will map the spatial distribution of material
around the
star, constraining the disk sizes and inclinations, and provide a first
assessment of when structure in the disk, such as cleared central zones and
annuli, which has been linked to planet formation, develops.
STIS/CCD/MA1 9184
A Survey for Missing Baryons in Highly Ionized Intergalactic Gas at Low
Redshift.
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to observe
six
additional low-z QSOs with the STIS FUV E140M echelle mode {7 km s^-1
resolution}. Combined with archival data, this will increase the sample
redshift
path by a factor of ~7 compared to the published data. With the echelle
data, we
will {1} measure the number of O VI absorbers per unit redshift {dN/dz} and
their minimum cosmological mass density with a limiting equivalent width of
W_Lambda ~50 mAngstrom , {2} examine whether the O VI absorption arises in
photoionized, collisionally ionized, or multiphase gas, and {3} study the
dependence of the O VI system properties on environment. In addition to
testing
this prediction regarding the location of the missing baryons, the data will
have applications to many other topics such as low-z LyAlpha absorbers and
the
physical properties and abundances of gas in the Milky Way halo.
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 analyze 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.
STIS/FUV 9412
The Physical Parameters of the Hottest, Most Luminous Stars as a Function of
Metallicity
We have obtained excellent, new ground-based blue optical and HAlpha spectra
of
a sample of very early-type stars in the Magellanic Clouds in order to
measure
their physical properties, for comparison with the extensive data that
exists
for higher-metallicity Galactic stars. Our aim is to understand how
effective
temperatures depend upon metallicity {necessary in determining IMFs}, and to
explore the astrophysically interesting regime of stars of extreme
temperatures,
masses, and luminosities. In order to do this, we need to measure the
stellar
wind terminal velocities for our stars, necessary to constrain the stellar
models. These can only be measured with STIS/FUV on HST. In addition, we
will
obtain higher spatial resolution data on the HAlpha line for stars for which
nebular contamination is significant in our ground-based data. We also
include
several R136 stars with excellent STIS/CCD data but which lack UV line
measures.
These new HST data will provide important information about the strengths of
stellar winds at extreme luminosities and the calibration of the Wind
Momentum-
Luminosity Relationship at lower metallicities. This proposal was highly
rated
in Cycle 9, but only 4 snapshots were obtained. We have completed the
analysis
of these plus additional data from the archives, but need spectra of the
remaining objects if we are to answer the questions we pose.
WFPC2 9699
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
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.
WFPC2 9593
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt1/3
This dark calibration program obtains 3 dark frames every day to provide
data
for monitoring and characterizing the evolution of hot pixels.
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 19 19
FGS REacq 23 23
FHST Update 57 57
LOSS of LOCK
SIGNIFICANT EVENTS: None
