HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4161
PERIOD COVERED: UT July 21,22,23, 2006 (DOY 202,203,204)
OBSERVATIONS SCHEDULED
NIC1/NIC2/NIC3 8794
NICMOS Post-SAA calibration - CR Persistence Part 5
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.
ACS/WFC 10775
An ACS Survey of Galactic Globular Clusters
We propose to conduct an ACS/WFC imaging survey of Galactic globular
clusters. We will construct the most extensive and deepest set of
photometry and astrometry to-date for these systems reaching a main
sequence mass of ~0.2 solar mass with S/N >= 10. We will combine
these
data with archival WFPC2 and STIS images to determine proper motions
for
the stars in our fields. The resultant cleaned cluster CMDs will
allow
us to study a variety of scientific questions. These include [but
are
not limited to] 1} the determination of cluster ages and distances
2}
the construction of main sequence mass functions and the issue of
mass
segregation 3} the internal motions and dynamical evolution of
globular
clusters, and 4} absolute cluster motions, orbits, and the Milky Way
gravitational potential. We anticipate that the unique resource
provided
by the proposed treasury archive will play a central role in the
field
of globular cluster studies for decades, with a stature comparable
to
that of the Hubble Deep Field for high redshift studies.
ACS/HRC/WFC 10758
ACS CCDs daily monitor
This program consists of a set of basic tests to monitor, the read
noise, the development of hot pixels and test for any source of noise
in
ACS CCD detectors. The files, biases and dark will be used to create
reference files for science calibration. This programme will be for
the
entire lifetime of ACS. Changes from cycle 13:- The default gain for
WFC
is 2 e- /DN. As before bias frames will be collected for both gain 1
and
gain 2. Dark frames are acquired using the default gain {2}. This
program cover the period May, 31 2006- Oct, 1- 2006. The first half
of
the program has a different proposal number: 10729.
WFPC2 10746
WFPC2 Cycle 14 CTE Monitor
Monitor CTE changes during Cycle 14. Test for chip-to-chip
differences
in CTE
CAL/ACS 10735
SBC MAMA Recovery
This proposal is designed for the initial turn-on of the ACS MAMA
detector and to permit recovery after an anomalous shutdown.
Anomalous
shutdowns can occur as a result of bright object violations which
trigger the Bright Scene Detection or Software Global Monitors.
Anomalous shutdowns can also occur as a result of MAMA hardware
problems. The Initial MAMA turn-on/recovery from anomalous shutdown
consists of three tests: a signal processing electronics check, high
voltage ramp-up to an intermediate voltage, and high voltage ramp-up
to
the full operating voltage. During each of the two high voltage
ramp-ups, diagnostics are performed during a dark ACCUM. The turn-on
is
followed by a MAMA Fold Analysis.
NIC3 10616
Gotcha! Using Swift GRBs to Pinpoint the Highest Redshift Galaxies
While there is convincing evidence that the Universe was re-ionized
between redshifts of 6.5 and 15, the role of galaxies in this process
is
still not understood. Several star-forming galaxies at z~6 have been
identified in recent deep, narrow-field surveys, but the expensive
observations along with cosmic variance and contamination make it
difficult to assess their contribution to re-ionization. Moreover,
the
detection of galaxies at z>7 is exceedingly difficult even with
the
Hubble UDF or cluster lensing. Significant progress can be made
using
gamma-ray bursts {GRBs} localized with the now-operational Swift
satellite, which is capable of detecting bursts out to z>10. GRBs
have
the advantage of being an uncontaminated signpost for
star-formation,
and their afterglows are sufficiently bright even at z>6 to allow
photometric selection {via the Ly-alpha drop out technique} with 2-5
meter telescopes. Using our approved TOO programs at an extensive
range
of facilities {from 1-m robotic telescopes to Keck/Magellan}, we can
rapidly find afterglows at z>6 and easily distinguish them from
dusty
low redshift bursts. This approach is highly efficient compared to
current techniques, especially at z>7. Here we request imaging
with
NICMOS {z>6}, ACS {z~6}, and Spitzer/IRAC to characterize the
properties
{SFR, age, morphology} of up to five galaxies located in this
manner,
and begin to address their role in re-ionization. These observations
are
requested as >2 month TOOs, allowing flexibility of scheduling and
at
the same time taking a unique and timely advantage of the exquisite
performance of three of NASA's premier missions.
WFPC2 10608
Probing the star formation law in the extreme outer limits of M83, a
prototypical XUV-disk galaxy
The Galaxy Evolution Explorer {GALEX} has discovered a new sub-class
of
spiral galaxy, which we refer to as extended UV-disk {XUV-disk}
galaxies. They are distinguished by conspicuous UV-bright star
clusters
located at galactocentric radii extending to many times the optical
{R25} extent, and appear to represent a population of spiral
galaxies
still actively building, or augmenting, their stellar disk. However,
XUV-disks pose a mystery in the form of a relative lack of HII
regions
{traced by H-alpha emission} associated with outer disk, UV-bright
stellar clusters. M83 is an XUV-disk prototype and the focus of this
proposal. It has an H-alpha surface brightness profile characterized
by
a steep decline at the radius beyond which the gaseous disk is
thought
to become dynamically stable {against collapse and ensuing star
formation}, but GALEX UV profiles show no "edge" at this
location. Our
HST study of M83 aims to resolve this puzzling discrepancy, confirmed
in
several XUV-disks, by searching for Lyman-continuum producing O
stars
that are either absent or present without nebulosity. HST provides
the
only means of resolving individual massive stars in the FUV band at
M83's distance. Without HST, we lose the critical ability to
photometrically classify O and B stars. Our multiwavelength
observations
will also constrain the history of star formation in the outer disk
over
Gyr timescales by characterizing the evolved stellar population,
both
using resolved giants and color analysis of the diffuse background.
ACS/WFC 10597
Resolving the Connection Between Globular Clusters and Low-Mass
X-ray
Binaries
Because of their high central densities, globular clusters {GCs} are
efficient producers of low-mass X-ray binaries {LMXBs}. To shed light
on
the detailed formation mechanism of LXMBs in GCs, we propose to
measure
accurate structural parameters for hundreds of GCs in NGC 5128: the
only
giant elliptical galaxy within 5 Mpc of the Milky Way. We will carry
out
the first complete survey of GCs in the inner region of NGC 5128,
measure GC structural parameters of unprecedented acccuracy, and
derive
GC luminosity profiles in the cluster cores. These measurement will
allow us to determine precisely which GC structural properties
control
the presence of an X-ray source and thus probe the details of the
LXMB
formation process in GCs. We will additionally use the measured
structural parameters to perform the most comprehensive study of the
fundamental plane of GCs in early-type galaxies, a fundamental set
of
correlations which holds key information on GC formation and evolution.
ACS/WFC 10592
An ACS Survey of a Complete Sample of Luminous Infrared Galaxies in
the
Local Universe
At luminosities above 10^11.4 L_sun, the space density of
far-infrared
selected galaxies exceeds that of optically selected galaxies. These
`luminous infrared galaxies' {LIRGs} are primarily interacting or
merging disk galaxies undergoing enhanced star formation and Active
Galactic Nuclei {AGN} activity, possibly triggered as the objects
transform into massive S0 and elliptical merger remnants. We propose
ACS/WFC imaging of a complete sample of 88 L_IR > 10^11.4 L_sun
luminous
infrared galaxies in the IRAS Revised Bright Galaxy Sample {RBGS:
i.e.,
60 micron flux density > 5.24 Jy}. This sample is ideal not only in
its
completeness and sample size, but also in the proximity and
brightness
of the galaxies. The superb sensitivity, resolution, and field of
view
of ACS/WFC on HST enables a unique opportunity to study the detailed
structure of galaxies that sample all stages of the merger process.
Imaging will be done with the F439W and F814W filters {B and I-band}
to
examine as a function of both luminosity and merger state {i} the
evidence at optical wavelengths of star formation and AGN activity
and
the manner in which instabilities {bars and bridges} in the galaxies
may
funnel material to these active regions, {ii} the relationship
between
star formation and AGN activity, and {iii} the structural properties
{AGN, bulge, and disk components} and fundamental parameters
{effective
radius and surface brightness} of LIRGs and their similarity with
putative evolutionary byproducts {elliptical, S0 and classical AGN
host
galaxies}. This HST survey will also bridge the wavelength gap between
a
Spitzer imaging survey {covering seven bands in the 3.6-160 micron
range} and a GALEX UV imaging survey of these galaxies, but will
resolve
complexes of star clusters and multiple nuclei at resolutions well
beyond the capabilities of either Spitzer or GALEX. The combined
datasets will result in the most comprehensive multiwavelength study
of
interacting and merging galaxies to date.
ACS/WFC 10588
The Host Galaxies of Post-Starburst Quasars
We propose to use ACS to conduct a snapshot imaging survey of
post-starburst quasars now being discovered in signficant numbers by
the
Sloan Digital Sky Survey. Post- starburst quasars are broad-lined
AGN
that also possess Balmer jumps and high-n Balmer absorption lines
indicative of luminous stellar populations on order of 100 Myr old.
These objects, representing a few percent of the z < 0.5 quasar
population, may be an evolutionary stage in the transition of
ultraluminous infrared galaxies into normal quasars, or a type of
galaxy
interaction that triggers both star formation and nuclear activity.
These sources may also illustrate how black hole mass/bulge mass
correlations arise. Ground- based imaging of individual
poststarburst
quasars has revealed merger remnants, binary systems, and single
point
sources. Our ACS snapshots will enable us to determine morphologies
and
binary structure on sub-arcsecond scales {surely present in the
sample},
as well as basic host galaxy properties. We will be looking for
relationships among morphology, particularly separation of double
nuclei, the starburst age, the quasar black hole mass and accretion
rate, that will lead to an understanding of the triggering activity
and
mutual evolution. This project will bring quantitative data and
statistics to the previously fuzzy and anecdotal topic of the
"AGN-starburst connection" and help test the idea that
post-starburst
quasars are an early evolutionary stage of normal quasars.
ACS/HRC 10556
Neutral Gas at Redshift z=0.5
Damped Lyman-alpha systems {DLAs} are used to track the bulk of the
neutral hydrogen gas in the Universe. Prior to HST UV spectroscopy,
they
could only be studied from the ground at redshifts z>1.65. However,
HST
has now permitted us to discover 41 DLAs at z<1.65 in our
previous
surveys. Followup studies of these systems are providing a wealth of
information about the evolution of the neutral gas phase component
of
the Universe. But one problem is that these 41 low-redshift systems
are
spread over a wide range of redshifts spanning nearly 70% of the age
of
the Universe. Consequently, past surveys for low-redshift DLAs have
not
been able to offer very good precision in any small redshift regime.
Here we propose an ACS-HRC-PR200L spectroscopic survey in the
redshift
interval z=[0.37, 0.7] which we estimate will permit us to discover
another 41 DLAs. This will not only allow us to double the number of
low-redshift DLAs, but it will also provide a relatively
high-precision
regime in the low-redshift Universe that can be used to anchor
evolutionary studies. Fortunately DLAs have high absorption
equivalent
width, so ACS- HRC-PR200L has high-enough resoultion to perform this
proposed MgII-selected DLA survey.
ACS/WFC/HRC 10536
What Are Stalled Preplanetary Nebulae? An ACS SNAPshot Survey
Essentially all planetary nebulae {PNs} are aspherical, whereas the
mass-loss envelopes of AGB stars are strikingly spherical. Our
previous
SNAPshot surveys of a morphologically unbiased sample of
pre-planetary
nebulae {PPNs} -- objects in transition between the AGB and PN
evolutionary phases -- show that roughly half our observed targets
are
resolved, with bipolar or multipolar morphologies. Spectroscopic
observations of our sample confirm that these objects have not yet
evolved into planetary nebulae. Thus, the transformation from
spherical
to aspherical geometries has already fully developed by the time
these
dying stars have become PPNs. Although our current studies have
yielded
exciting results, they are limited in two important ways -- {1} the
number of well-resolved objects is still small {18}, and the variety
of
morphologies observed relatively multitudinous, hence no clear
trends
can yet be established between morphology and other source
properties
{e.g., near-IR, far-IR colors, stellar spectral type, envelope
mass},
and {2} the current samples are strongly biased towards small PPNs,
as
inferred from their low 60-to- 25 micron flux ratios
[R{60/25}<1].
However, the prototype of objects with R{60/25}>1, the Frosty Leo
Nebula, has a puzzlingly large post-AGB age {almost 10^4 yr} and a
fairly cool central star, very different from the expectations of
single-star stellar evolutionary models. A proposed, but still
speculative, hypothesis for such objects is that the slow evolution
of
the central star is due to backflow of material onto the mass-losing
star, retarding its evolution towards the PN phase. This hypothesis
has
significant consequences for both stellar and nebular evolution. We
therefore propose a survey of PPNs with R{60/25}>1 which is
heavily
weighted towards the discovery of such "stalled PPNs".
Supporting
kinematic observations using long-slit optical spectroscopy {with
the
Keck}, millimeter and radio interferometric observations {with OVRO,
VLA
& VLBA} are being undertaken. The results from this survey
{together
with our previous work} will allow us to draw general conclusions
about
the complex mass-outflow processes affecting late stellar evolution,
and
will provide crucial input for theories of post-AGB stellar
evolution.
Our survey will produce an archival legacy of long-standing value
for
future studies of dying stars.
WFPC2 10534
Active Atmospheres on Uranus and Neptune
We propose Snapshot observations of Uranus and Neptune to monitor
changes in their atmospheres on time scales of weeks, months, and
years.
Uranus is rapidly approaching equinox in 2007, with another 4 degrees
of
latitude becoming visible every year. Recent HST observations during
this epoch {including 6818: Hammel, Lockwood, and Rages; 8680:
Hammel,
Rages, Lockwood, and Marley; 8634: Rages, Hammel, Lockwood, Marley,
and
McKay; and 10170: Rages, Hammel, Lockwood, and Marley} have revealed
strongly wavelength-dependent latitudinal structure and the presence
of
numerous visible- wavelength cloud features in the northern
hemisphere.
Long-term ground-based observations {Lockwood and Thompson 1999}
show
seasonal brightness changes whose origins are not well understood.
Recent near-IR images of Neptune obtained using adaptive optics on
the
Keck Telesccope together with images from our Cycle 9 Snapshot
program
{8634} show a general increase in activity at south temperate
latitudes
as well as the possible development of another Great Dark Spot.
Further
Snapshot observations of these two dynamic planets will elucidate
the
nature of long-term changes in their zonal atmospheric bands and
clarify
the processes of formation, evolution, and dissipation of discrete
albedo features.
NIC2 10527
Imaging Scattered Light from Debris Disks Discovered by the Spitzer
Space Telescope Around 20 Sun-like Stars
We propose to use the high contrast capability of the NICMOS
coronagraph
to image a sample of newly discovered circumstellar disks associated
with sun-like stars. These systems were identified by their strong
thermal infrared emission with the Spitzer Space Telescope as part
of
the Spitzer Legacy Science program titled, "The Formation and
Evolution
of Planetary Systems {FEPS}." Modelling of the thermal excess
emission
in the form of spectral energy distributions alone cannot
distinguish
between narrowly confined high opacity disks and broadly
distributed,
low opacity disks. However, our proposed NICMOS observations can, by
imaging the light scattered from this material. Even non- detections
will place severe constraints on the disk geometry, ruling out
models
with high optical depth. Unlike previous disk imaging programs, our
program contains a well defined sample of solar mass stars covering
a
range of ages from ~10Myrs to a few Gyrs, allowing us to study the
evolution of disks from primordial to debris for the first time.
These
results will greatly improve our understanding of debris disks
around
Sun-like stars at stellar ages nearly 10x older than any previous
investigation. Thus we will have fit a crucial piece into the puzzle
concerning the formation and evolution of our own solar system.
ACS/HRC/WFC 10514
Kuiper Belt Binaries: Probes of Early Solar System Evolution
Binaries in the Kuiper Belt are a scientific windfall: in them we
have
relatively fragile test particles which can be used as tracers of
the
early dynamical evolution of the outer Solar System. We propose a
Snapshot program using the ACS/HRC that has a potential discovery
efficiency an order of magnitude higher than the HST observations
that
have already discovered the majority of known transneptunian
binaries.
By more than doubling the number of observed objects in dynamically
hot
and cold subpopulations we will be able to answer, with statistical
significance, the question of whether these groups differ in the
abundance of binaries as a result of their particular dynamical
paths
into the Kuiper Belt. Today's Kuiper Belt bears the imprints of the
final stages of giant-planet building and migration; binaries may
offer
some of the best preserved evidence of that long-ago era.
ACS/HRC 10512
Search for Binaries Among Faint Jupiter Trojan Asteroids
We propose an ambitious SNAPSHOT program to survey faint Jupiter
Trojan
asteroids for binary companions. We target 150 objects, with the
expectation of acquiring data on about 50%. These objects span Vmag
=
17.5-19.5, a range inaccessible with ground-based adaptive optics.
We
now have a significant sample from our survey of brighter Trojans to
suggest that the binary fraction is similar to that which we find
among
brighter main-belt asteroids, roughly 2%. However, our observations
suggest a higher binary fraction for smaller main-belt asteroids,
probably the result of a different formation mechanism {evident also
from the physical characteristics of the binaries}. Because the
collision environment among the Trojans is similar to that of the
Main
Belt, while the composition is likely to be very different, sampling
the
binary fraction among the fainter Trojans should help us understand
the
collisional and binary formation mechanisms at work in various
populations, including the Kuiper Belt, and help us evaluate
theories
for the origin of the Trojans. Calibration of and constraints on
models
of binary production and collisional evolution can only be done
using
these large-scale, real-life physical systems that we are beginning
now
to find and utilize.
NIC3/ACS/WFC 10504
Characterizing the Sources Responsible for Cosmic Reionization
Our group has demonstrated the role that massive clusters, acting as
powerful cosmic lenses, can play in constraining the abundance and
properties of low-luminosity star- forming sources beyond z~6; such
sources are thought to be responsible for ending cosmic
reionization.
The large magnification possible in the critical regions of well-
constrained clusters brings sources into view that lie at or beyond
the
limits of conventional exposures such as the UDF, as well as those
in
imaging surveys being undertaken with IRAC onboard Spitzer. We have
shown that the combination of HST and Spitzer is particularly
effective
in delivering the physical properties of these distant sources,
constraining their mass, age and past star formation history.
Indirectly, we therefore gain a valuable glimpse to yet earlier
epochs.
Recognizing the result {and limitations} of the UDF exposure, we
propose
a systematic search through 6 lensing clusters with ACS and NICMOS
for
further z~6-7 sources in conjunction with existing deep IRAC data.
Our
survey will mitigate cosmic variance and extend the search both to
lower
luminosities and, by virtue of the NICMOS/IRAC combination, to
higher
redshift. The goal is to count and characterize representative
sources
at z~6-10 and to delineate the redshift range of activity for the
planning of future observations.
ACS/WFC/NIC2 10496
Decelerating and Dustfree: Efficient Dark Energy Studies with
Supernovae
and Clusters
We propose a novel HST approach to obtain a dramatically more useful
"dust free" Type Ia supernovae {SNe Ia} dataset than available
with the
previous GOODS searches. Moreover, this approach provides a
strikingly
more efficient search-and-follow-up that is primarily pre-scheduled.
The
resulting dark energy measurements do not share the major systematic
uncertainty at these redshifts, that of the extinction correction with
a
prior. By targeting massive galaxy clusters at z > 1 we obtain a
five-times higher efficiency in detection of Type Ia supernovae in
ellipticals, providing a well-understood host galaxy environment.
These
same deep cluster images then also yield fundamental calibrations
required for future weak lensing and Sunyaev-Zel'dovich measurements
of
dark energy, as well as an entire program of cluster studies. The
data
will make possible a factor of two improvement on supernova
constraints
on dark energy time variation, and much larger improvement in
systematic
uncertainty. They will provide both a cluster dataset and a SN Ia
dataset that will be a longstanding scientific resource.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies:
(The following are preliminary reports of potential non-nominal
performance that will be investigated.)
HSTARS:
#10368 REacq(2,3,3) failed to RGA control. @ 203/20:13:36z
The
REacq(2,3,3) scheduled at 203/20:10:18 failed due to scan step limit
exceeded
on FGS 2. The OBAD2 at 20:05:14 showed errors of V1= 8.38, V2=
-4.70, V3=
-1.22, and RSS= 9.68. The Map at 20:28:52 showed errors of
V1=5.75,V2=0.16,V3=1.95, and RSS=6.07. Observation affected: ACS 3
#10370 REacq(2,3,2) resulted in fine lock backup (2,0,2) @
204/15:23:04z
REacq(2,3,2) scheduled at 204/15:19:40 resulted in fine lock backup
(2,0,2)
due to receiving stop flag QF2STOPF on FGS 3 at 15:23:04. OBAD2
showed
errors of V1=15.52, V2=7.93, V3=10.74,and RSS=20.49. The map at
15:27:06
showed errors of V1=1.27, V2=-9.92, V3=-2.77, and RSS=10.38.
Observations affected: ACS 32-34
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES:
#1510-0 Adjust ACS Error Count @ 204/00:38z
SCHEDULED SUCCESSFUL FAILURE
TIMES
FGS
GSacq
24
24
FGS
REacq
19
18
203/20:10:18z (HSTAR #10368)
OBAD with Maneuver
80
80
SIGNIFICANT EVENTS: (None)
-Lynn
Lynn F. Bassford
CHAMP HST Missions Operations Manager
Lockheed Martin Technical Operations
GSFC PH#: 301-286-2876
"The Hubble Space Telescope is the Babe Ruth of astronomical
observatories, the Muhammad Ali of cosmic photography
"
- Robert Roy Britt, space.com 7-14-4
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