HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4149
PERIOD COVERED: UT July 5, 2006 (DOY 186)
OBSERVATIONS SCHEDULED
ACS/HRC 10738
Earth Flats
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 in the pipeline and to monitor any changes. Weekly
coronagraphic monitoring is required to assess the changing position
of
the spots.
ACS/HRC 10752
Cycle 14 Focus Monitor
The focus of HST is measured primarily with ACS/HRC over full CVZ
orbits
to obtain accurate mean focus values via a well sampled breathing
curve.
Coma and astigmatism are also determined from the same data in order
to
further understand orbital effects on image quality and optical
alignments. To monitor the stability of ACS to WFPC2 relative focii,
we've carried over from previous focus monitor programs parallel
observations taken with the two cameras at suitable orientations of
previously observed targets, and interspersed them with the HRC CVZ
visits.
ACS/HRC 9746
Binary systems in the Kuiper Belt
The properties of the orbits of Kuiper belt object {KBO} satellites
hold
keys to fundamental insight into masses and densities of KBOs, the
interaction history of the early solar system, the internal structure
of
distant ice-rock bodies, and even the genesis of the Pluto- Charon
binary. Within the past 18 months, 9 KBO satellite systems have been
discovered, allowing for the first time the possibility of
characterizing a sample of KBO satellite orbital properties. We
propose
HRC observations to determine satellite orbits in the 6 best cases.
We
have carefully devised a strategy for each of these 6 systems to
make
maximum use of ground-based observations, previous HST observations,
and
the smallest possible number of new HST observations. Our proposed
observations will efficiently provide highly reliable orbital
solutions
which are critical to achieving the scientific promise available
from
the study of these systems. Our strategy relies heavily on extensive
Monte Carlo simulations to define optimal times of observing such
that
each new point obtained gives maximum leverage for refining the
orbital
solution. We find that with this strategy we can provide mass
solutions
for all 6 systems to an accuracy of better than 10% using only 25
new
HST observations. This highly efficient program provides extreme
scientific output with optimal use of scarce resources.
ACS/WFC 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.
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 10630
The Fine Structure of Elliptical Galaxies in Voids
Elliptical galaxies constitute a remarkably homogeneous class of
objects
with a tight color- magnitude relation and a well-defined
Fundamental
Plane. In spite of their bland and symmetrical morphology, they are
characterized by a wealth of structural features {such as nuclear
disks,
dust lanes, shells, blue cores, etc.} which contain important clues
to
their formation history. Little is known about how and if these
sub-structures vary as a function of environment; in fact, due to
the
morphology density relation, our knowledge of ellipticals is
strongly
biased towards overdense regions such as clusters. But what of the
fine
structure of ellipticals in voids? According to theoretical
predictions,
void galaxies should have different merger histories than those in
clusters, which may imply that their fine structure also differs. We
address these issues using the exquisite angular resolution of
HST/ACS
to resolve sub-structures in the most accurately classified sample,
to
date, of truly isolated ellipticals, identified using the 2dFGRS.
ACS/WFC/HRC 11005
Funcional test - MEB2 switch
This is a functional test to be executed after the switch to MEB2.
NIC1 10879
A search for planetary-mass companions to the nearest L dwarfs -
completing the survey
We propose to extend the most sensitive survey yet undertaken for
very
low-mass companions to ultracool dwarfs. We will use NICMOS to
complete
imaging of an all-sky sample of 87 L dwarfs in 80 systems within 20
parsecs of the Sun. The combination of infrared imaging and
proximity
allows us to search for companions with mass ratios q>0.25 at
separations exceeding ~3 AU, while probing companions with q>0.5 at
~1.5
AU separation. This resolution is crucial, since no ultracool
binaries
are known in the field with separations exceeding 15 AU. Fifty L
dwarfs
from the 20-parsec sample have high- resolution imaging, primarily
through our Cycle 13 HST proposal which identified six new binaries,
including an L/T system. Here, we propose to target the remaining 30
dwarfs
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.
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.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
reports
of potential non-nominal performance that will be investigated.)
HSTARS:
10341 - GSacq(2,1,2) results in fine lock backup @ 186/1404z
GSacq(2,1,2) scheduled at 186/14:01:29 resulted in fine lock backup
(2,0,2).
The GSacq resulted in fine lock backup at 14:04:36 due to stop
flag
QF1STOPF on FGS 1. Possible observations affected: WFPC 19-22.
10342 - GSacq(2,1,1) failed due to search radius limit exceeded @
186/1713z
During LOS
GSacq(2,1,1) failed due to search radius limit exceeded. At
AOS
(17:19:45) flags were set indicating the GSacq failed due to search
radius
limit exceeded on FGS 2. OBAD2 showed errors of V1=-5.85,
V2=-8.44,
V3=-2.80, RSS=10.65. The Map at 17:20:24 showed erros of
V1=1.60,
V2=4.29, V3=-2.79, RSS=5.36. Possible obs affected: ACS 89-93.
10343 - GSAcq (2,1,1) failed due to search radius limit exceeded @
187/0737z
GSAcq
(2,1,1) scheduled at 187/08:05:06 failed during LOS due to search
raduis
limit exceeded of FGS 1. Performed 486 ESB dump that showed one
ESB
message a05 (FGS Coarse Track failed - Search Radius Limit exceeded
)and 2 ESB
message 1805 (FHST moving target detected) were received
during
LOS. OBAD 1: V1 -606.16, V2 1595.22, V3 -394.30, RSS
1751.47
OBAD 2: V1 -4.90, V2 -3.92, V3 -5.78, RSS 8.53 OBAD MAP: V1
-2.55, V2
12.74, V3 -6.28, RSS 14.43 Possible observations affected:
ACS
150-154. GSAcq Scheduled time should read 187/07:37:10 - 07:44:38
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS
GSacq
8
6
186/1713z (HSTAR 10342)
&187/0737z (HSTAR 10343)
FGS
REacq
5
5
OBAD with Maneuver
26
26
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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