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HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #5203
PERIOD
COVERED: 8:00pm October 11 - 7:59pm October 12, 2010 (DOY
285/00:00z-285/23:59z)
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
12464
- GSAcq(1,2,1) scheduled at 285/06:52:14z resulted in fine lock
backup (2,0,2) using FGS-2 due to scan step limit exceeded.
Observations possibly affected: ACS 39 Proposal ID#12210, WFC3 35
Proposal ID#11905
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSAcq
10
10
FGS
REAcq
05
05
OBAD
with Maneuver
08
08
SIGNIFICANT
EVENTS: (None)
OBSERVATIONS
SCHEDULED:
ACS/WFC
12210
SLACS
for the Masses: Extending Strong Lensing to Lower Masses and
Smaller
Radii
Strong
gravitational lensing provides the most accurate possible
measurement
of mass in the central regions of early-type galaxies
(ETGs).
We propose to continue the highly productive Sloan Lens ACS
(SLACS)
Survey for strong gravitational lens galaxies by observing a
substantial
fraction of 135 new ETG gravitational-lens candidates with
HST-ACS
WFC F814W Snapshot imaging. The proposed target sample has been
selected
from the seventh and final data release of the Sloan Digital
Sky
Survey, and is designed to complement the distribution of previously
confirmed
SLACS lenses in lens-galaxy mass and in the ratio of Einstein
radius
to optical half-light radius. The observations we propose will
lead
to a combined SLACS sample covering nearly two decades in mass,
with
dense mapping of enclosed mass as a function of radius out to the
half-light
radius and beyond. With this longer mass baseline, we will
extend
our lensing and dynamical analysis of the mass structure and
scaling
relations of ETGs to galaxies of significantly lower mass, and
directly
test for a transition in structural and dark-matter content
trends
at intermediate galaxy mass. The broader mass coverage will also
enable
us to make a direct connection to the structure of well-studied
nearby
ETGs as deduced from dynamical modeling of their line-of-sight
velocity
distribution fields. Finally, the combined sample will allow a
more
conclusive test of the current SLACS result that the intrinsic
scatter
in ETG mass-density structure is not significantly correlated
with
any other galaxy observables. The final SLACS sample at the
conclusion
of this program will comprise approximately 130 lenses with
known
foreground and background redshifts, and is likely to be the
largest
confirmed sample of strong-lens galaxies for many years to come.
COS/FUV
12212
What
are the Locations and Kinematics of Mass Outflows in AGN?
Mass
outflows of ionized gas in AGN, first revealed through blueshifted
UV
and X-ray absorption lines, are likely important feedback mechanisms
for
the enrichment of the IGM, self-regulation of black-hole growth, and
formation
of structure in the early Universe. To understand the origin,
dynamics,
and impact of the outflowing absorbers on their surroundings,
we
need to know their locations (radial positions and polar angles with
respect
to the AGN rotation axes) and kinematics (radial and transverse
velocities).
We will use COS high-resolution spectra of 11 Seyfert 1
galaxies
to derive velocity-dependent covering factors, ionic column
densities,
number densities (via metastable lines or variability), and
ionization
parameters (via photoionization models) of the UV absorbers,
and
thereby determine their radial locations as we have done for NGC
4151.
We will use absorption variability over time scales of up to ~20
years,
to determine transverse velocities and detect changes in radial
velocities.
We will use STIS G430M long-slit spectra and WFC3 [OIII]
images
to resolve the kinematics of the narrow-line region (NLR) and
determine
the inclinations of the AGN, to investigate the connection
between
nuclear absorption and NLR emission outflows and their
dependence
on polar angle.
COS/NUV/FUV
11742
Probing
HeII Reionization with GALEX-selected Quasar Sightlines and
HST/COS
We
propose spectroscopic observations with COS of eight z~3 QSOs that we
found
to be bright in the far ultraviolet. Our aim is to study
intergalactic
absorption caused by the onset of the He II Lyman forest.
Several
lines of evidence suggest that helium reionization occurred at
z~3.
Understanding this process is critical for a complete picture of
the
intergalactic medium and its evolution; it also gives clues to
hydrogen
reionization at z>6. The only direct means of assessing He II
reionization
is through far-UV observations of the He II Lyman alpha
forest.
Only 6 sightlines are known to date where this is feasible,
despite
extensive surveys. Our program is designed to double the number
of
available sightlines. To this effect, we cross- correlated all known
z>2.73
quasars with UV source lists from the GALEX satellite. The
selected
quasars were all significantly detected in the far UV by GALEX,
and
their UV colors are similar to those of already known quasars with
transparent
sightlines. Spectra obtained with COS will allow us to
compile
the first comprehensive sample of He II absorption spectra
probing
similar redshifts, enabling a systematic investigation of the He
II
reionization epoch and the spectral shape of the UV background.
STIS/CCD
11845
CCD
Dark Monitor Part 2
Monitor
the darks for the STIS CCD.
STIS/CCD
11847
CCD
Bias Monitor-Part 2
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.
WFC3/IR
12224
Measuring
the Stellar Populations of Individual Lyman Alpha Emitters
During
the Epoch of Peak Star Formation
Selecting
galaxies by their strong Lyman-alpha emission provides a
powerful
means of probing the reionization epoch and the faint/low-mass
galaxies
that dominate star formation at high redshift. Yet, our
understanding
of high-redshift Lyman-alpha emitters (LAEs) has lagged
behind
that of other well-studied populations (e.g., Lyman break
galaxies)
due to their continuum faintness and the shifting of
age/mass-sensitive
features into the near-IR where the high terrestrial
background
inhibits deep observations. All existing studies of LAEs at
z>2
have used stacked optical and/or Spitzer infrared data to discern
their
median properties, but the actual distributions of ages,
reddenings,
and stellar masses for these populations are poorly
characterized.
To fill this glaring gap in the observations and advance
our
understanding of this important population, we propose WFC3/IR+F160W
imaging
of fields where we have conducted a survey of low redshift
(z~1.9)
Lyman-alpha emitters (LAEs), in order to measure their ages and
stellar
masses at an epoch where such observations directly probe the
age-sensitive
Balmer/4000 AA breaks. The targeted sample will include
45-50
spectroscopically confirmed LAEs at z=1.7-2.1 and roughly twice as
many
candidates, making it the largest sample of homogeneously selected
LAEs
with individual measurements of the ages, masses, and dust
extinction.
With these data we will (1) carefully take into account the
age-dependence
of the extinction curve to make robust comparisons
between
LAEs and continuum-selected galaxies at the same redshifts; (2)
combine
clustering and stellar mass measurements to infer the duty
cycles
of LAEs and determine if they are triggered in the presence of
large-scale
structures; and (3) quantify the importance of the LAE phase
at
different galaxy luminosity and mass scales, over a large dynamic
range
in these properties. An economical investment of just 12 orbits
will
allow us to accomplish these goals, and remains the only hope of
efficiently
studying such low luminosity high-redshift galaxies in the
near-IR
prior to the JWST-era.
WFC3/IR
12286
Hubble
Infrared Pure Parallel Imaging Extragalactic Survey (HIPPIES)
WFC3
has demonstrated its unprecedented power in probing the early
universe.
Here we propose to continue our pure parallel program with
this
instrument to search for LBGs at z~6--8. Our program, dubbed as the
Hubble
Infrared Pure Parallel Imaging Extragalactic Survey ("HIPPIES"),
will
carry on the HST pure parallel legacy in the new decade. We request
205
orbits in Cycle-18, which will spread over ~ 50 high Galactic
latitude
visits (|b|>20deg) that last for 3 orbits and longer, resulting
a
total survey area of ~230 square arcmin. Combining the WFC3 pure
parallel
observations in Cycle-17, HIPPIES will complement other
existing
and forthcoming WFC3 surveys, and will make unique
contributions
to the study in the new redshift frontier because of the
randomness
of the survey fields. To make full use of the parallel
opportunities,
HIPPIES will also take ACS parallels to study LBGs at
z~5--6.
Being a pure parallel program, HIPPIES will only make very
limited
demand on the scarce HST resources, but will have potentially
large
scientific returns. As in previous cycle, we waive all proprietary
data
rights, and will make the enhanced data products public in a timely
manner.
(1)
The WFC3 part of HIPPIES aims at the most luminous LBG population at
z~8
and z~7. As its survey fields are random and completely
uncorrelated,
the number counts of the bright LBGs from HIPPIES will be
least
affected by the "cosmic variance", and hence we will be able to
obtain
the best constraint on the bright-end of the LBG luminosity
function
at z~8 and 7. Comparing the result from HIPPIES to the
hydrodynamic
simulations will test the input physics and provide insight
into
the nature of the early galaxies. (2) The z~7--8 candidates from
HIPPIES,
most of which will be the brightest ones that any surveys would
be
able to find, will have the best chance to be spectroscopically
confirmed
at the current 8--10m telescopes. (3) The ACS part of HIPPIES
will
produce a significant number of candidate LBGs at z~5 and z~6 per
ACS
field. Combining with the existing, suitable ACS fields in the HST
archive,
we will be able to utilize the random nature of the survey to
quantify
the
cosmic variance and to measure the galaxy bias at z~5--6, and
therefore
the galaxy halo masses at these redshifts. (4) We will also
find
a large number of extremely red, old galaxies at intermediate
redshifts,
and the fine spatial resolution offered by the WFC3 will
enable
us constrain their formation history based on the study of their
morphology,
and hence shed light on their connection to the very early
galaxies
in the universe.
WFC3/IR
12307
A
public SNAPSHOT Survey of Gamma-ray Burst Host Galaxies
We
propose to conduct a public infrared survey of the host galaxies of
Swift
selected gamma-ray bursts (GRBs) at z<3. By obtaining deep,
diffraction
limited imaging in the IR we will complete detections for
the
host galaxies, and in concert with our extensive ground based
afterglow
and host programmes will compile a detailed catalog of the
properties
of high-z galaxies selected by GRBs. In particular these
observations
will enable us to study the colours, luminosities and
morphologies
of the galaxies. This in turn informs studies of the nature
of
the progenitors and the role of GRBs as probes of star formation
across
cosmic history. Ultimately it provides a product of legacy value
which
will greatly complement further studies with next generation
facilities
such as ALMA and JWST.
WFC3/IR/S/C
11929
IR
Dark Current Monitor
Analyses
of ground test data showed that dark current signals are more
reliably
removed from science data using darks taken with the same
exposure
sequences as the science data, than with a single dark current
image
scaled by desired exposure time. Therefore, dark current images
must
be collected using all sample sequences that will be used in
science
observations. These observations will be used to monitor changes
in
the dark current of the WFC3-IR channel on a day-to-day basis, and to
build
calibration dark current ramps for each of the sample sequences to
be
used by Gos in Cycle 17. For each sample sequence/array size
combination,
a median ramp will be created and delivered to the
calibration
database system (CDBS).
WFC3/IR/UV
12163
Structure
and Stellar Content of the Nearest Nuclear Clusters in
Late-Type
Spiral Galaxies
HST
surveys have shown that nuclear star clusters are nearly ubiquitous
in
late-type, bulgeless disk galaxies. In early-type galaxies, the
central
black hole mass correlates with the bulge mass and velocity
dispersion,
but the relationship between black hole mass and host galaxy
properties
in bulgeless galaxies is not yet understood. Some nuclear
clusters
(such as the one in M33) do not contain a central massive black
hole
at all, while other late-type galaxies (such as NGC 4395) are known
to
contain accretion-powered active nuclei within their nuclear
clusters,
indicating that a central black hole is present. But, the
overall
"occupation fraction" of black holes within nuclear clusters is
largely
unconstrained. Measurement of the structure, dynamics, and
stellar
content of nuclear star clusters is an important pathway toward
understanding
the demographics of low-mass black holes in late-type
galaxies.
We
propose to obtain multi-filter WFC3 UV, optical, and near-IR images
of
10 of the nearest and brightest nuclear clusters in late-type spiral
galaxies.
We will use the new WFC3 data to measure the cluster radial
profiles,
to search for color gradients, and in combination with
ground-based
spectroscopy and stellar population modeling, to determine
the
stellar masses of the clusters. Since nuclear clusters are known to
contain
stellar populations with a wide range of ages, the broad
wavelength
coverage of our data will provide new leverage to constrain
the
star formation history of the clusters. We will carry out dynamical
modeling
for the clusters, using the cluster structural parameters and
stellar
M/L ratios measured from the WFC3 data and kinematics measured
from
ground-based, adaptive-optics assisted integral-field spectroscopy
(already
obtained or approved for 8 of the 10 targets). This will yield
tight
new constraints on the masses of intermediate-mass black holes
(IMBH)
within the clusters, and may result in the first dynamical
detections
of IMBHs in the nuclei of late-type spirals.
WFC3/IR/WFC/ACS/UV
12061
Cosmic
Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-South
Field,
Early Visits of SNe Search
This
survey will document the first third of galactic evolution from z=8
to
1.5 and test for evolution in the properties of Type Ia supernovae to
z~2
by imaging more than 250, 000 galaxies with WFC3/IR and ACS. Five
premier
multi-wavelength regions are selected from within the Spitzer
SEDS
survey, providing complementary IRAC data down to 26.5 AB mag, a
unique
resource for stellar masses at high redshifts. The use of five
widely
separated fields mitigates cosmic variance and yields
statistically
robust samples of galaxies down to 10^9 M_Sun out to z~8.
We
adopt a two-tiered strategy with a "Wide" component (roughly 2 orbits
deep
over ~0.2 sq. degrees) and a "Deep" component (roughly 12 orbits
deep
over ~0.04 sq. degrees). Combining these with ultra-deep imaging
from
the Cycle 17 HUDF09 program yields a three-tiered strategy for
efficient
sampling of both rare/bright and faint/common objects.
Three
of the Wide-survey fields are located in COSMOS, EGS, and
UKIDSS/UDS.
Each of these consists of roughly 3x15 WFC3/IR tiles. Each
WFC3
tile will be observed for 2 orbits, with single orbits separated in
time
to allow a search for high-redshift Type Ia SNe. The co-added
exposure
times will be approximately 2/3 orbit in J (F125W) and 4/3
orbit
in H (F160W). ACS parallels overlap most of the WFC3 area and will
consist
of roughly 2/3 orbits in V (F606W) and 4/3 orbit in I (F814W).
Because
of the larger area of ACS, this results in effective exposures
that
are twice as long (4/3 in V, 8/3 in I), making a very significant
improvement
to existing ACS mosaics in COSMOS and EGS and creating a new
ACS
mosaic in UDS/UKIDSS where none now exists. Other Wide-survey
components
are located in the GOODS fields (North and South) surrounding
the
Deep-survey areas.
The
Deep-survey fields cover roughly half of each GOODS field, with
exact
areas and placements to be determined as part of the Phase-2
process.
Each WFC3/IR tile within the Deep regions will receive
approximately
12 orbits of exposure time split between Y (F105W), J
(F125W),
and H (F160W). Multi-epoch imaging will provide an efficient
search
for high-redshift Type Ia SNe here also. ACS parallels are also
taken
in the Deep regions, with the goal of assembling enough total
exposure
time in F850LP and other filters to identify high redshift z>6
galaxies
in concert with WFC3/IR data using the Lyman break technique.
A
portion of the GOODS-N campaign will take place while the field is in
the
HST Continuous Viewing Zone (CVZ). The bright time in those orbits
will
be used to obtain UV imaging with WFC3 in the F275W and F336W
filters.
The exact number of orbits will not be known until Phase-2
planning
is complete, but we anticipate that it will be possible to
schedule
at least 100 orbits, resulting in 5-sigma point-source depths
of
26.6, 26.4 in F275W and F336W, respectively. The science goals
include
measuring the Lyman-continuum escape fractions for galaxies at
z~2.5
and identifying Lyman-break galaxies at z~2-3.
The
Type Ia supernova search program in this proposal is integrated with
that
in the Postman cluster MCT proposal, with this one stressing the
more
distant supernovae. A combined follow-up program will provide light
curves
and grism spectra of 15-20 of the best candidates at
redshifts
1<z<2. The observing configuration for the follow up will
depend
on the redshift of the supernova, and will likely include a grism
observation
with either ACS G800L, WFC3-IR G102, or G141, and light
curves
observed with F850LP, WFC3-IR F125W, and F160W.
The
new data will be used to answer many urgent questions in galaxy
evolution
and cosmology. In the reionization era, we will identify
hundreds
of high-confidence z>7 galaxies in the Deep regions, in
addition
to hundreds of highly-luminous candidates in the Wide regions
for
detailed follow-up. These samples will be used to construct a
unified
picture of star-formation and stellar mass buildup in early
galaxies.
Extremely deep X-ray data will reveal distant AGNs to z>6,
shedding
light on the earliest stages of BH growth. In the peak star
formation/QSO
era, z~2, we will document the properties of early disks,
the
build-up of bulges, the evolution of mergers, and the nature of AGN
hosts
to construct an integrated model for structural evolution, star
formation
quenching, and AGN triggering. Finally, the ~8 Type Ia SNe
found
beyond z>1.5 in the supernova programs will establish the
constancy
of these standard candles independent of dark energy and yield
the
first measurement of the Type Ia rate at z~2 to distinguish among
different
progenitor models. Lower-redshift SNe Ia at 1<z<1.5 will be
used
to measure the evolution of dark energy.
This
program takes full advantage of MCTP mode to fulfill Hubble's
legacy
for deep extragalactic science and prepare the way for JWST.
WFC3/UV
12344
Cycle
18: UVIS Bowtie Monitor
Ground
testing revealed an intermittent hysteresis type effect in the
UVIS
detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially
found via an unexpected bowtie-shaped feature in flatfield
ratios,
subsequent lab tests on similar e2v devices have since shown
that
it is also present as simply an overall offset across the entire
CCD,
i.e., a QE offset without any discernable pattern. These lab tests
have
further revealed that overexposing the detector to count levels
several
times full well fills the traps and effectively neutralizes the
bowtie.
Each visit in this proposal acquires a set of three 3x3 binned
internal
flatfields: the first unsaturated image will be used to detect
any
bowtie, the second, highly-exposed image will neutralize the bowtie
if
it is present, and the final image will allow for verification that
the
bowtie is gone.
WFC3/UVIS
11905
WFC3
UVIS CCD Daily Monitor
The
behavior of the WFC3 UVIS CCD will be monitored daily with a set of
full-frame,
four-amp bias and dark frames. A smaller set of 2Kx4K
subarray
biases are acquired at less frequent intervals throughout the
cycle
to support subarray science observations. The internals from this
proposal,
along with those from the anneal procedure (Proposal 11909),
will
be used to generate the necessary superbias and superdark reference
files
for the calibration pipeline (CDBS).
WFC3/UVIS/IR
11700
Bright
Galaxies at z>7.5 with a WFC3 Pure Parallel Survey
The
epoch of reionization represents a special moment in the history of
the
Universe as it is during this era that the first galaxies and star
clusters
are formed. Reionization also profoundly affects the
environment
where subsequent generations of galaxies evolve. Our
overarching
goal is to test the hypothesis that galaxies are responsible
for
reionizing neutral hydrogen. To do so we propose to carry out a pure
parallel
WFC3 survey to constrain the bright end of the redshift z>7.5
galaxy
luminosity function on a total area of 176 arcmin^2 of sky.
Extrapolating
the evolution of the luminosity function from z~6, we
expect
to detect about 20 Lyman Break Galaxies brighter than M_* at z~8
significantly
improving the current sample of only a few galaxies known
at
these redshifts. Finding significantly fewer objects than predicted
on
the basis of extrapolation from z=6 would set strong limits to the
brightness
of M_*, highlighting a fast evolution of the luminosity
function
with the possible implication that galaxies alone cannot
reionize
the Universe. Our observations will find the best candidates
for
spectroscopic confirmation, that is bright z>7.5 objects, which
would
be missed by small area deeper surveys. The random pointing nature
of
the program is ideal to beat cosmic variance, especially severe for
luminous
massive galaxies, which are strongly clustered. In fact our
survey
geometry of 38 independent fields will constrain the luminosity
function
like a contiguous single field survey with two times more area
at
the same depth. Lyman Break Galaxies at z>7.5 down to m_AB=26.85 (5
sigma)
in F125W will be selected as F098M dropouts, using three to five
orbits
visits that include a total of four filters (F606W, F098M, F125W,
F160W)
optimized to remove low-redshift interlopers and cool stars. Our
data
will be highly complementary to a deep field search for high-z
galaxies
aimed at probing the faint end of the luminosity function,
allowing
us to disentangle the degeneracy between faint end slope and
M_*
in a Schechter function fit of the luminosity function. We waive
proprietary
rights for the data. In addition, we commit to release the
coordinates
and properties of our z>7.5 candidates within one month from
the
acquisition of each field.