Daily Report #4149

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 q0.25
at separations exceeding ~3 AU, while probing companions with q0.5 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)