Daily Rpt #4409

Notice: Due to the conversion of some ACS WFC or HRC observations into
WFPC2, or NICMOS observations after the loss of ACS CCD science capability
in January, there may be an occasional discrepancy between a proposal's
listed (and correct) instrument usage and the abstract that follows it.

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4409

PERIOD COVERED: UT July 20, 21 and 22, 2007 (DOY 201, 202 and 203)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8794

NICMOS Post-SAA calibration - CR Persistance 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.

WFPC2 11289

SL2S: The Strong Lensing Legacy Survey

Recent systematic surveys of strong galaxy-galaxy lenses {CLASS, SLACS,
GOODS, etc.} are producing spectacular results for galaxy masses roughly
below a transition mass M~10^13 Mo. The observed lens properties and their
evolution up to z~0.2, consistent with numerical simulations, can be
described by isothermal elliptical potentials. In contrast, modeling of
giant arcs in X-ray luminous clusters {halo masses M ~10^13 Mo} favors NFW
mass profiles, suggesting that dark matter halos are not significantly
affected by baryon cooling. Until recently, lensing surveys were neither
deep nor extended enough to probe the intermediate mass density regime,
which is fundamental for understanding the assembly of structures. The CFHT
Legacy Survey now covers 125 square degrees, and thus offers a large
reservoir of strong lenses probing a large range of mass densities up to
z~1. We have extracted a list of 150 strong lenses using the most recent
CFHTLS data release via automated procedures. Following our first SNAPSHOT
proposal in cycle 15, we propose to continue the Hubble follow-up targeting
a larger list of 130 lensing candidates. These are intermediate mass range
candidates {between galaxies and clusters} that are selected in the redshift
range of 0.2-1 with no a priori X-ray selection. The HST resolution is
necessary for confirming the lensing candidates, accurate modeling of the
lenses, and probing the total mass concentration in galaxy groups up to z~1
with the largest unbiased sample available to date.

FGS 11210

The Architecture of Exoplanetary Systems

Are all planetary systems coplanar? Concordance cosmogony makes that
prediction. It is, however, a prediction of extrasolar planetary system
architecture as yet untested by direct observation for main sequence stars
other than the Sun. To provide such a test, we propose to carry out FGS
astrometric studies on four stars hosting seven companions. Our
understanding of the planet formation process will grow as we match not only
system architecture, but formed planet mass and true distance from the
primary with host star characteristics for a wide variety of host stars and
exoplanet masses. We propose that a series of FGS astrometric observations
with demonstrated 1 millisecond of arc per-observation precision can
establish the degree of coplanarity and component true masses for four
extrasolar systems: HD 202206 {brown dwarf+planet}; HD 128311
{planet+planet}, HD 160691 = mu Arae {planet+planet}, and HD 222404AB =
gamma Cephei {planet+star}. In each case the companion is identified as such
by assuming that the minimum mass is the actual mass. For the last target, a
known stellar binary system, the companion orbit is stable only if coplanar
with the AB binary orbit.

WFPC2 11178

Probing Solar System History with Orbits, Masses, and Colors of
Transneptunian Binaries

The recent discovery of numerous transneptunian binaries {TNBs} opens a
window into dynamical conditions in the protoplanetary disk where they
formed as well as the history of subsequent events which sculpted the outer
Solar System and emplaced them onto their present day heliocentric orbits.
To date, at least 47 TNBs have been discovered, but only about a dozen have
had their mutual orbits and separate colors determined, frustrating their
use to investigate numerous important scientific questions. The current
shortage of data especially cripples scientific investigations requiring
statistical comparisons among the ensemble characteristics. We propose to
obtain sufficient astrometry and photometry of 23 TNBs to compute their
mutual orbits and system masses and to determine separate primary and
secondary colors, roughly tripling the sample for which this information is
known, as well as extending it to include systems of two near-equal size
bodies. To make the most efficient possible use of HST, we will use a Monte
Carlo technique to optimally schedule our observations.

WFPC2 11084

Probing the Least Luminous Galaxies in the Local Universe

We propose to obtain deep color-magnitude data of eight new Local Group
galaxies which we recently discovered: Andromeda XI, Andromeda XII, and
Andromeda XIII {satellites of M31}; Canes Venatici I, Canes Venatici II,
Hercules, and Leo IV {satellites of the Milky Way}; and Leo T, a new
"free-floating" Local Group dwarf spheroidal with evidence for recent star
formation and associated H I gas. These represent the least luminous
galaxies known at *any* redshift, and are the only accessible laboratories
for studying this extreme regime of galaxy formation. With deep WFPC-2 F606W
and F814W pointings at their centers, we will determine whether these
objects contain single or multiple age stellar populations, as well as
whether these objects display a range of metallicities.

NIC3 11082

NICMOS Imaging of GOODS: Probing the Evolution of the Earliest Massive
Galaxies, Galaxies Beyond Reionization, and the High Redshift Obscured
Universe

Deep near-infrared imaging provides the only avenue towards understanding a
host of astrophysical problems, including: finding galaxies and AGN at z
7, the evolution of the most massive galaxies, the triggering of star
formation in dusty galaxies, and revealing properties of obscured AGN. As
such, we propose to observe 60 selected areas of the GOODS North and South
fields with NICMOS Camera 3 in the F160W band pointed at known massive M
10^11 M_0 galaxies at z 2 discovered through deep Spitzer imaging. The
depth we will reach {26.5 AB at 5 sigma} in H_160 allows us to study the
internal properties of these galaxies, including their sizes and
morphologies, and to understand how scaling relations such as the Kormendy
relationship evolved. Although NIC3 is out of focus and undersampled, it is
currently our best opportunity to study these galaxies, while also sampling
enough area to perform a general NIR survey 1/3 the size of an ACS GOODS
field. These data will be a significant resource, invaluable for many other
science goals, including discovering high redshift galaxies at z 7, the
evolution of galaxies onto the Hubble sequence, as well as examining
obscured AGN and dusty star formation at z 1.5. The GOODS fields are the
natural location for HST to perform a deep NICMOS imaging program, as
extensive data from space and ground based observatories such as Chandra,
GALEX, Spitzer, NOAO, Keck, Subaru, VLT, JCMT, and the VLA are currently
available for these regions. Deep high-resolution near-infrared observations
are the one missing ingredient to this survey, filling in an important gap
to create the deepest, largest, and most uniform data set for studying the
faint and distant universe. The importance of these images will increase
with time as new facilities come on line, most notably WFC3 and ALMA, and
for the planning of future JWST observations.

NIC3 11080

Exploring the Scaling Laws of Star Formation

As a variety of surveys of the local and distant Universe are approaching a
full census of galaxy populations, our attention needs to turn towards
understanding and quantifying the physical mechanisms that trigger and
regulate the large-scale star formation rates {SFRs} in galaxies.

WFPC2 11079

Treasury Imaging of Star Forming Regions in the Local Group:
Complementing the GALEX and NOAO Surveys

We propose to use WFPC2 to image the most interesting star-forming regions
in the Local Group galaxies, to resolve their young stellar populations. We
will use a set of filters including F170W, which is critical to detect and
characterize the most massive stars, to whose hot temperatures colors at
longer wavelengths are not sensitive. WFPC2's field of view ideally matches
the typical size of the star-forming regions, and its spatial resolution
allows us to measure individual stars, given the proximity of these
galaxies. The resulting H-R diagrams will enable studies of star- formation
properties in these regions, which cover largely differing metallicities {a
factor of 17, compared to the factor of 4 explored so far} and
characteristics. The results will further our understanding of the
star-formation process, of the interplay between massive stars and
environment, the properties of dust, and will provide the key to interpret
integrated measurements of star-formation indicators {UV, IR, Halpha}
available for several hundreds more distant galaxies. Our recent deep
surveys of these galaxies with GALEX {FUV, NUV} and ground-based imaging
{UBVRI, Halpha, [OIII] and [SII]} provided the identification of the most
relevant SF sites. In addition to our scientific analysis, we will provide
catalogs of HST photometry in 6 bands, matched corollary ground-based data,
and UV, Halpha and IR integrated measurements of the associations, for
comparison of integrated star-formation indices to the resolved populations.
We envisage an EPO component.

FGS 10928

Calibrating Cosmological Chronometers: White Dwarf Masses

We propose to use HST/FGS1R to determine White Dwarf {WD} masses. The
unmatched resolving power of HST/FGS1R will be utilized to follow up four
selected WD binary pairs. This high precision obtained with HST/FGS1R simply
cannot be equaled by any ground based technique. This proposed effort
complements that done by CoI Nelan in which a sample of WDs is being
observed with HST/FGS1R. This proposal will dramatically increase the number
of WDs for which dynamical mass measurements are possible, enabling a better
calibration of the WD mass-radius relation, cooling curves, initial to final
mass relations, and ultimately giving important clues to the star formation
history of our Galaxy and the age of its disk as well as in other galaxies.

ACS/WFC/WFPC2 10904

Star formation in extended UV disk {XUV-disk} galaxies

The Galaxy Evolution Explorer {GALEX} has discovered the existence of
extended UV-disk {XUV-disk} galaxies. This class of intriguing spiral
galaxies is distinguished by UV-bright regions of star formation located at
extreme galactocentric radii, commonly reaching many times the optical
extent of each target. XUV-disks represent a population of late-type
galaxies still actively building, or significantly augmenting, their stellar
disk in the outer, low-density environment. Prior to GALEX, such regions
were considered to be far more stable against star formation than now
realized. Our work on these targets has led to the recognition of the XUV
phenomenon as probing a diverse population of galaxies which, although
having certain commonality in terms of their present XUV star formation,
have apparently experienced different star formation histories {as judged by
their outer disk UV-optical colors and morphology}. In ordinary spirals,
disk formation occurred at a much earlier epoch, making today's XUV-disks
useful templates for commonplace, high z galaxies. The diverse XUV-disks in
our sample may represent snapshots of different phases in the disk building
process. We seek to characterize the demographics of star forming regions
occupying this environmental range, especially in contrast to their inner
disk counterparts. HST imaging is needed to accurately characterize the
massive stars and clusters which have, in fact, managed to form. The GALEX
observations are limited by 5" resolution. Deep ACS FUV, B, V, I, and
H-alpha imaging {along with parallel WFPC2 data} will allow: {1} photometric
classification of the OB star population, {2} constraint on the cluster mass
function and age distribution, {3} critical accounting for possible leakage
of Lyman continuum photons in a porous ISM or an IMF change, and {4}
population synthesis modeling of the field SFH on Gyr timescales. We benefit
from extensive archival HST observations of our target galaxies, although
the outer disk has yet to be probed.

NIC3 10874

Search for Extremely Faint z7 Galaxy Population with Cosmic Lenses

Deep UDF/NICMOS observations find a significant decrease in the number of
galaxy candidates between redshift z=6 and 7, but the sample at z7 is too
small to draw conclusions. From our observations of 15 clusters we have
found a number of bright z-dropouts, aided by the lensing amplification. We
propose deep NICMOS observations of the best cases of cluster centers where
a rare combination of a significant lensing effect and the richness in
z-band dropouts in background may dramatically increase the discovery rate.
The NICMOS images will reach an unprecedented depth of AB~27.8, or AB~30 in
nonlensed intrinsic magnitude, and may find many faint {~0.05L*} galaxies at
z=7-10, at a level that the UDF reaches for z~6 objects. We produce
precision mass distribution maps from weak-lensing models, which enable us
to derive the candidates' intrinsic magnitudes and their luminosity
function. The knowledge of such faint galaxy population at z7 will
facilitate the models of the IGM reionization and future JWST planning.

WFPC2 10841

A Proper Motion Search for Intermediate Mass Black Holes in Globular
Clusters {2nd Epoch Observations}

Establishing the presence or absence of intermediate-mass black holes {IMBH}
in globular clusters is crucial for understanding the evolution of dense
stellar systems. Observationally, this search has been hampered by the low
number of stars with known velocities in the central few arcseconds. This
limits our knowledge of the velocity dispersion in the region where the
gravitational influence of any IMBH would be felt. In Cycle 13, we
successfully obtained ACS/HRC images of the centers of five carefully chosen
Galactic globular clusters {GO-10401} for a new proper motion study.
Although the science case was approved and the first epoch images obtained,
the requested future cycle observations were not granted {due to a general
policy decision based on the strong uncertainties at the time concerning the
immediate future of HST}. We have now assessed the quality of the first
epoch observations. The HRC resolution reveals many isolated stars in to the
very center of each cluster that remained blended or unresolved in previous
WFPC2 data. Given a two year baseline, we are confident that we can achieve
the proper motion precision required to place strict limits on the presence
of an IMBH. Therefore, we request the second-epoch, follow-up observations
to GO-10401 in order to measure the proper motions of stars in our target
clusters. These velocity measurements will allow us to: {i} place
constraints on the mass of a central black hole in each cluster; {ii} derive
the internal velocity dispersion as a function of cluster radius; {iii}
verify or reject previous reports of cluster rotation; and {iv} directly
measure velocity anisotropy as a function of radius. If no second epoch data
are obtained then the observing time already invested in the first epoch
will have been wasted.

NIC1 10797

HE0450-2958: Lonesome black hole, scantly dressed quasar or massively dust
obscured host galaxy?

We propose to obtain a deep NICMOS image of the bright z=0.285 quasar
HE0450-2958 that has an exceptional, undetected host galaxy, at least 6
times fainter than expected for the quasar luminosity. Several mutually
exclusive explanations that were put forward in the last weeks, attempting
to explain the apparently undermassive host galaxy, have important
implication for their respective areas: The host could be a dust obscured
ultra-luminous infrared galaxy in transition to become a quasar, HE450-2958
could have a normal host galaxy but an undermassive central black hole, or
the quasar could recently have been ejected from a nearby companion galaxy
in a 3-body black hole interaction or by gravitational recoil. We want to
use NIC2 with the minimum-background F160W filter to obtain a =10 times
fainter limit on the host galaxy mass than is currently available with ACS,
in order to set strong constraints for these very important scenarios.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)

HSTARS:

#10904 REAcq (1,2,1) failed due to Search Radius Limit Exceeded on FGS-1.

REAcq (1,2,1) was scheduled from 12:46:34-12:54:02 had
failed to RGA hold (Gyro Control).
OBAD #1 & #2 data unavailable due to LOS.
OBAD MAP: V1 95.03, V2 -19.52, V3 95.87, RSS 136.39


#10905 GSAcq (2,3,2) failed due to Search Radius Limit Exceeded on
FGS-2.

GSAcq (2,3,2) was scheduled from 14:14:28-14:21:49z.
OBAD #1: V1 -666.23, V2 -2175.08, V3 369.54, RSS 2304.65
OBAD #2: V1 -4.67, V2 -0.30, V3 140.71, RSS 140.79
OBAD MAP: v1 -46.66, V2 28.02, V3 -191.16, RSS 198.76
REAcq (2,3,2) scheduled from 15:47:31-15:54:52 had also failed due
to search radius limit exceeded on FGS-2.
OBAD #1 & #2 unavailable due to LOS.
OBAD MAP: v1 -4.86, V2 3.12, V3 -147.87, RSS 147.98

#10907 GSAcq(2,0,2) failed.

GSAcq(2,0,2) at 201/19:01:21 failed to RGA control (gyro control) with
QF2STOPF and QSTOP flags set. Vehicle had OBAD RSS error of 42.31
arcseconds. Occurred during LOS, additional info available following the
next engineering recorder dump.

#10909 REAcq(1,2,1) failed to RGA control.

REAcq(1,2,1) failed at 202/1542z and received stop flag QF1STOPF on FGS 1.
OBAD1 showed errors of V1=-32.18, V2=-584.13, V3=-18.99, and RSS=585.32.
OBAD2 occurred during LOS.

# 10910 GSAcq(2,3,3) failed to RGA Hold (Gyro Control).

GSAcq(2,3,3) scheduled at 203/04:39:21z failed to RGA Hold due to both
(QF2STOPF) stop flag and (QF2SRLEX) search radius limit exceeded
indication on FGS-2.
Pre-acquisition OBAD1 attitude correction value not available due to LOS.
OBAD2 had (RSS) value of 13.38 arcseconds.
Post-acq OBAD/MAP at 203/04:46:40z not available in 32K F-FORMAT.

#10911 OBAD Failed Identification.

OBAD1 scheduled at 203/20:18:37z failed. "OBAD Failed Identification" was
received at 203/22:21:29z. OBAD2 and the GSAcq were successful.

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL
FGS GSacq 18 15
FGS REacq 26 23
OBAD with Maneuver 88 85

SIGNIFICANT EVENTS: (None)