HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #5118
PERIOD
COVERED: 5am June 15 - 5am June 16, 2010 (DOY 166/09:00z-167/09:00z)
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
(None)
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSAcq
6
6
FGS
REAcq
9
9
OBAD
with Maneuver 4
4
SIGNIFICANT
EVENTS: (None)
OBSERVATIONS
SCHEDULED:
COS/NUV
11538
COS-GTO:
Imaging of Mid-UV Emissions from Io in Eclipse
The
atmosphere and corona of Jupiter's volcanic moon Io emit light at a
wide
variety of wavelengths, from FUV neutral O and S lines to SO
emission
at 1.7 microns. These emissions provide important constraints
on
the distribution and chemistry of Io's atmosphere, and Io's
interaction
with the Jovian magnetosphere. The neutral O and S FUV
emissions,
shortward of 2000, have been imaged extensively by HST/STIS
and
visible emissions (from neutral Na, K and O line emission, and SO2
continuum
emission) have been imaged by the Galileo, Cassini, and New
Horizons
spacecraft, but the spatial distribution of emissions in the
2000-3000
region, thought to be dominated by SO2 electron impact
continuum
emission, has not yet been determined. Earlier long-slit
observations
with STIS indicated strong concentration of 2800? emission
over
the active volcano Prometheus (Jessup et al. 2004), suggesting
local
volcanic control, but Cassini images suggest that the SO2
continuum
seen at longer wavelengths is instead concentrated over the
sub-Jovian
and anti-Jovian points where there are magnetic connections
between
Io and the Jovian magnetosphere- the anti-Jovian point is close
to
Prometheus. A series of 200-second integrations taken in Jupiter
eclipse
should determine whether emission is concentrated over volcanos
or
over the sub-Jovian point, and should be able to observe motion of
the
emission due to changing magnetic field orientation if it is
magnetically
controlled. This observation will also provide experience
in
the use of COS in imaging mode.
COS/NUV/FUV
11598
How
Galaxies Acquire their Gas: A Map of Multiphase Accretion and
Feedback
in Gaseous Galaxy Halos
We
propose to address two of the biggest open questions in galaxy
formation
- how galaxies acquire their gas and how they return it to the
IGM
- with a concentrated COS survey of diffuse multiphase gas in the
halos
of SDSS galaxies at z = 0.15 - 0.35. Our chief science goal is to
establish
a basic set of observational facts about the physical state,
metallicity,
and kinematics of halo gas, including the sky covering
fraction
of hot and cold material, the metallicity of infall and
outflow,
and correlations with galaxy stellar mass, type, and color -
all
as a function of impact parameter from 10 - 150 kpc. Theory suggests
that
the bimodality of galaxy colors, the shape of the luminosity
function,
and the mass-metallicity relation are all influenced at a
fundamental
level by accretion and feedback, yet these gas processes are
poorly
understood and cannot be predicted robustly from first
principles.
We lack even a basic observational assessment of the
multiphase
gaseous content of galaxy halos on 100 kpc scales, and we do
not
know how these processes vary with galaxy properties. This ignorance
is
presently one of the key impediments to understanding galaxy
formation
in general. We propose to use the high-resolution gratings
G130M
and G160M on the Cosmic Origins Spectrograph to obtain sensitive
column
density measurements of a comprehensive suite of multiphase ions
in
the spectra of 43 z < 1 QSOs lying behind 43 galaxies selected from
the
Sloan Digital Sky Survey. In aggregate, these sightlines will
constitute
a statistically sound map of the physical state and
metallicity
of gaseous halos, and subsets of the data with cuts on
galaxy
mass, color, and SFR will seek out predicted variations of gas
properties
with galaxy properties. Our interpretation of these data will
be
aided by state-of-the-art hydrodynamic simulations of accretion and
feedback,
in turn providing information to refine and test such models.
We
will also use Keck, MMT, and Magellan (as needed) to obtain optical
spectra
of the QSOs to measure cold gas with Mg II, and optical spectra
of
the galaxies to measure SFRs and to look for
outflows.
In addition to our other science goals, these observations
will
help place the Milky Way's population of multiphase, accreting High
Velocity
Clouds (HVCs) into a global context by identifying analogous
structures
around other galaxies. Our program is designed to make
optimal
use of the unique capabilities of COS to address our science
goals
and also generate a rich dataset of other absorption-line systems
STIS/CC
11845
CCD
Dark Monitor Part 2
Monitor
the darks for the STIS CCD.
STIS/CC
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.
STIS/CCD
11849
STIS
CCD Hot Pixel Annealing
This
purpose of this activity is to repair radiation induced hot pixel
damage
to the STIS CCD by warming the CCD to the ambient instrument
temperature
and annealing radiation-damaged pixels.
Radiation
damage creates hot pixels in the STIS CCD Detector. Many of
these
hot pixels can be repaired by warming the CCD from its normal
operating
temperature near -83 deg. C to the ambient instrument
temperature
(~ +5 deg. C) for several hours. The number of hot pixels
repaired
is a function of annealing temperature. The effectiveness of
the
CCD hot pixel annealing process is assessed by measuring the dark
current
behavior before and after annealing and by searching for any
window
contamination effects.
STIS/CCD/MA2
11568
A
SNAPSHOT Survey of the Local Interstellar Medium: New NUV Observations
of
Stars with Archived FUV Observations
We
propose to obtain high-resolution STIS E230H SNAP observations of
MgII
and FeII interstellar absorption lines toward stars within 100
parsecs
that already have moderate or high-resolution far-UV (FUV),
900-1700
A, observations available in the MAST Archive. Fundamental
properties,
such as temperature, turbulence, ionization, abundances, and
depletions
of gas in the local interstellar medium (LISM) can be
measured
by coupling such observations. Due to the wide spectral range
of
STIS, observations to study nearby stars also contain important data
about
the LISM embedded within their spectra. However, unlocking this
information
from the intrinsically broad and often saturated FUV
absorption
lines of low-mass ions, (DI, CII, NI, OI), requires first
understanding
the kinematic structure of the gas along the line of
sight.
This can be achieved with high resolution spectra of high-mass
ions,
(FeII, MgII), which have narrow absorption lines, and can resolve
each
individual velocity component (interstellar cloud). By obtaining
short
(~10 minute) E230H observations of FeII and MgII, for stars that
already
have moderate or high- resolution FUV spectra, we can increase
the
sample of LISM measurements, and thereby expand our knowledge of the
physical
properties of the gas in our galactic neighborhood. STIS is the
only
instrument capable of obtaining the required high resolution data
now
or in the foreseeable future.
WFC3/ACS/IR
11731
Studying
Cepheid Systematics in M81: H-Band Observations
The
local value of the Hubble Constant remains one of the most important
constraints
in cosmology, but improving on the 10% accuracy of the HST
Key
Project is challenging. No improvements will be convincing until the
metallicity
dependence is well constrained and blending effects are
fully
understood. M81 and its dwarf companion Holmberg IX are superb
laboratories
for studying Cepheid systematics because they contain large
numbers
of bright Cepheids with a good spread in metallicity lying at a
common,
relatively close distance. We have identified 180 12<P< 70 day
Cepheids
in these two galaxies using the Large Binocular Telescope
(compared
to 30 in total by the KP), and will expand the sample further
in
2008-2009. We will use 10 orbits with WFC3/IR to obtain H-band images
of
100 Cepheids in M81 to add to the ACS/BVI calibrations we will obtain
from
archival data and 1 orbit with WFC3/UVIS to add B-band data for
Holmberg
IX. Four band BVIH photometry will allow us to flux calibrate,
estimate
extinction, measure metallicity effects and then check the
results
in detail. We can also examine blending effects on WFC3/IR data
in
a relatively nearby galaxy before it is applied to more distant
galaxies.
Our M81 sample is three times larger than the next best
sample,
that of NGC4258, and suffers less from blending because M81 is
at
half the distance, so it is an excellent laboratory for studying
Cepheid
systematics even if it lacks as precise a geometric distance as
NGC4258.
WFC3/IR
11694
Mapping
the Lnteraction Between High-Redshift Galaxies and the
Lntergalactic
Environment
With
the commissioning of the high-throughput large-area camera WFC3/IR,
it
is possible for the first time to undertake an efficient survey of
the
rest-frame optical morphologies of galaxies at the peak epoch of
star
formation in the universe. We therefore propose deep WFC3/IR
imaging
of over 320 spectroscopically confirmed galaxies between
redshift
1.6 < z < 3.4 in well-studied fields which lie along the line
of
sight to bright background QSOs. The spectra of these bright QSOs
probe
the IGM in the vicinity of each of the foreground galaxies along
the
line of sight, providing detailed information on the physical state
of
the gas at large galactocentric radii. In combination with our
densely
sampled UV/IR spectroscopy, stellar population models, and
kinematic
data in these fields, WFC3/IR imaging data will permit us to
construct
a comprehensive picture of the structure, dynamics, and star
formation
properties of a large population of galaxies in the early
universe
and their effect upon their cosmological environment.
WFC3/IR
11921
WFC3
IR PSF Wings
The
IR PSF wings will be evaluated at 5 field points (near the field
center
and corners) in two filters (F098M and F160W) to check for image
stability.
Full frame images of a moderately bright, isolated star will
be
obtained at each field position with a series of increasing exposure
times
designed to permit construction of a very high SNR PSF with
dynamic
range sufficient to evaluate the wing intensity to >5 arcsec
radius.
The images will also permit examination of potential straylight
effects,
electronic cross-talk and image persistence.
This
is a repeat of SMOV activity WFC3-26 (program 11439.) The results
of
the two programs will be compared. The data will be analyzed using
the
code and techniques described in ISR WFC3 2008-41 (Hartig). Profiles
of
encircled energy will be compared to those obtained from program
11439.
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/UV
11906
WFC3
UVIS CCD Gain
The
absolute gain of each quadrant of the WFC3 UVIS detector will be
measured
for the nominal detector readout configuration and at the
on-orbit
operating temperature.
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
11908
Cycle
17: 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/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.