Daily #3992

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3992

PERIOD COVERED: UT November 18, 19, 20, 2005 (DOY 322, 323, 324)

OBSERVATIONS SCHEDULED

NICMOS 8790

NICMOS Post-SAA calibration - CR Persistence Part 1.

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.

ACS/WFC 10740

Absolute Photometric & Spectrophometric Calibration

This program has several goals: 1.}Verify repeatability of the ACS
instrumentation on a single bright star to +/-0.2%. 2.}Determine any
shift in the filter bandpasses since the preflight lab measurements.
3.}Determine the relative magnitude of the 3 primary WD calibrators to
0.1%. 4.}Refine the sensitivity calibration of the CCD prism and
grisms at field center and determine the repeatability accuracy of
this calibration. 5.}Determine the level of variability of the three
HST red standard stars: VB-8 {M7}, 2M0038+18 {L3.5} and 2M0559-14
{T5}, and also measure their short wavelength {7000A} fluxes.
6.}Cross calibrate with a faint STIS and NICMOS standard WD and solar
analog star.

ACS/HRC/WFC 10729

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 Oct, 2 2005- May, 29-2006. The
second half of the program has a different proposal number: 10758.

ACS/WFC 10635

Galaxy Transformation as probed by Morphology and Velocity Fields of
Distant Cluster Galaxies

We seek to obtain ACS imaging of four distant {0.3z0.6} clusters of
galaxies within a 6'x6' field covered by a 2x2 mosaic to determine
morphological and structural parameters of late-type galaxies. We
specifically concentrate on peculiarities indicative of past or
ongoing interaction processes. The ~90 target galaxies have been
{Period74} or will be {P75} observed with 3D- spectroscopy at ESO-VLT
yielding 2D-velocity fields with unprecedented spatial coverage and
sampling. The good spatial resolution of the ground-based data will be
further enhanced by a deconvolution method based on the proposed ACS
images. The velocity field and the morphology in restframe-UV light
will reveal possible transformation mechanisms affecting not only the
stellar populations but also the mass distribution of the galaxies.
Additionally, it will be possible to pin down the nature of the
interaction {e.g. tidally or ram-pressure induced}. This assessment
gets supported by our N-body/SPH simulations {including star
formation} of different interaction processes that allow the direct
comparison of structural and kinematical characteristics at each time
step with the observations on an individual basis taking into account
all observational constraints for a given galaxy. All together, we
will be able to explore the relative efficiency of the various
proposed transformation phenomena. In the case of non-disturbed
spirals, a rotation curve can be extracted from the full 2D velocity
field with unprecedented quality, from which the maximum rotation
speed can be derived with high confidence. In combination with
accurate size and luminosity determinations from the ACS images, we
will be able to establish the Tully-Fisher and Fundamental Plane
relations of cluster spiral members at cosmological epochs. At these
distances cluster assembly is predicted to peak and we can probe the
galaxies' luminosity, size and mass evolution with robust methods.
Together with our already existing sample of ~200 distant {z=1}
spiral galaxies in the field, we will put strong constraints on
current theories of galaxy formation and evolution in different
environments.

ACS/WFC 10634

White Dwarf Cooling Physics: Calibrating the Clock

We know approximate ages for the Galactic disk from white dwarf
cooling theory applied to local white dwarfs and for the Galactic halo
from main sequence stellar evolutionary theory applied to star
clusters. However, the two chronometers are not cross-calibrated to
the same absolute scale; our observations will perform this
cross-calibration and improve the precision of both chronometers. We
propose to use HST/ACS photometry of white dwarfs in five moderately
old open cluster {0.6-2.2 Gyr}, along with all available up-to-date
white dwarf interior and atmosphere models and a powerful new
statistical approach, to compare main sequence evolutionary theory and
white dwarf cooling theory. This comparison will be done in such a
manner as to test white dwarf crystallization and carbon/oxygen phase
separation, as well as main sequence models in the range where they
are sensitive to the degree of core overshooting and where PP burning
transitions to CNO burning. This confrontation is essential before we
can accurately and precisely apply white dwarf cosmochronometry to the
disk and halo field populations and to globular clusters. Past support
by HST for white dwarf ages in globular clusters {123 orbits for M4
and a similarly large scheduled campaign for NGC 6397} will only be
fully levereged by ensuring that both stellar chronometers are
calibrated to the same age scale. Only then can white dwarf
chronometers live up to their potential as fundamental, independent,
and new age estimators for the Galaxy.

ACS/WFC 10626

A Snapshot Survey of Brightest Cluster Galaxies and Strong Lensing to
z = 0.9

We propose an ACS/WFC snapshot survey of the cores of 150 rich galaxy
clusters at 0.3 z 0.9 from the Red Sequence Cluster Survey {RCS}.
An examination of the galaxian light in the brightest cluster
galaxies, coupled with a statistical analysis of the strong-lensing
properties of the sample, will allow us to contrain the evolution of
both the baryonic and dark mass in cluster cores, over an
unprecedented redshift range and sample size. In detail, we will use
the high- resolution ACS images to measure the metric {10 kpc/h}
luminosity and morphological disturbances around the brightest
clusters galaxies, in order to calibrate their accretion history in
comparison to recent detailed simulations of structure formation in
cluster cores. These images will also yield a well-defined sample of
arcs formed by strong lensing by these clusters; the frequency and
detailed distribution {size, multiplicity, redshifts} of these strong
lens systems sets strong constraints on the total mass content {and
its structure} in the centers of the clusters. These data will also be
invaluable in the study of the morphological evolution and properties
of cluster galaxies over a significant redshift range. These analyses
will be supported by extensive ongoing optical and near-infrared
imaging, and optical spectroscopy at Magellan, VLT and Gemini
telescopes, as well as host of smaller facilities.

FGS 10610

Astrometric Masses of Extrasolar Planets and Brown Dwarfs

We propose observations with HST/FGS to estimate the astrometric
elements {perturbation orbit semi-major axis and inclination} of
extra-solar planets orbiting six stars. These companions were
originally detected by radial velocity techniques. We have
demonstrated that FGS astrometry of even a short segment of reflex
motion, when combined with extensive radial velocity information, can
yield useful inclination information {McArthur et al. 2004}, allowing
us to determine companion masses. Extrasolar planet masses assist in
two ongoing research frontiers. First, they provide useful boundary
conditions for models of planetary formation and evolution of
planetary systems. Second, knowing that a star in fact has a plantary
mass companion, increases the value of that system to future
extrasolar planet observation missions such as SIM PlanetQuest, TPF,
and GAIA.

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 10579

ULX counterparts: the key to finding intermediate-mass black holes

The origin and formation mechanism for supermassive black holes
{SMBHs} found in the centres of most, if not all, galaxies remains one
of the outstanding questions in astrophysics. Most scenarios involve
the presence of massive black holes in the early universe, formed by
the collapse of primordial Population III stars. It is predicted that
a relic of this population could still be present in galactic halos in
the current epoch, possessing masses from a few hundred times solar
mass upwards. However, to date no CONCLUSIVE evidence for such a class
of "intermediate-mass" black holes has been found. The most likely
current candidates are the ultraluminous X-ray sources {ULXs}, which
show tantalising evidence for IMBHs {e.g. the extreme X-ray
luminosities and low disk temperatures expected from accreting IMBHs}.
We propose to address this issue by identifying optical counterparts
for six of the nearest ULXs. We will use this programme as a
pathfinder for future radial velocity measurements, which will allow
the orbital parameters and hence the first undisputed mass constraints
for these systems to be determined.

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 z1.65.
However, HST has now permitted us to discover 41 DLAs at z1.65 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/HRC 10549

SAINTS - Supernova 1987A INTensive Survey

SAINTS is a program to observe SN 1987A, the brightest supernova in
384 years, as it morphs into the youngest supernova remnant at age 18.
HST is the unique and perfect tool for spatially- resolved
observations of the many physical components of SN 1987A. A violent
encounter is underway between the fastest-moving debris and the
circumstellar ring, exciting hotspots seen with HST that are suddenly
lighting up. The optical and X-ray flux from the ring are both rising
rapidly: HST and Chandra observations taken together are needed to
understand the physics of these shocked regions. In Cycle14, the
hotspots may fuse as the shock fully enters the ring. Photons from
these shocks may excite previously hidden gas outside the ring,
revealing the true extent of the mass loss that preceded the
explosion. The inner debris of the explosion itself, still excited by
radioactive isotopes produced in the explosion, is now well resolved
by ACS and seen to be aspherical, providing direct clues to the
mechanism of the explosion. Our search for a compact remnant is
beginning to eliminate some theoretical possibilities and we have the
opportunity in Cycle 14 to place much more stringent limits with
NICMOS. Many questions about SN 1987A remain unanswered. How did the
enigmatic three rings form in the late stages of Sanduleak -69 202?
Precisely what took place in the center during the core collapse and
bounce? Is a black hole or a neutron star left behind in the debris?
SAINTS has been a continuous program since HST was launched-- we
propose to extend this rich and deep data set for present use and
future reference to answer these central questions in the science of
supernovae.

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 10525

Characterizing the Near-UV Environment of M Dwarfs: Implications for
Extrasolar Planetary Searches and Astrobiology

We propose SNAP observations with the ACS HRC PR200L prism, designed
to measure the near ultraviolet emission in a sample of 107 nearby M
dwarfs. The sample spans the mass range from 0.1 - 0.6 solar masses
{temperature range 2200K - 4000K} where the UV energy distributions
vary widely between active and inactive stars. The strength and
distribution of this UV emission can have critical consequences for
the atmospheres of attendant planets. Our proposed observations will
provide desperately needed constraints on models of the habitability
zone and the atmospheres of possible terrestrial planets orbiting M
dwarf hosts, and will be used to sharpen TPF target selection. In
addition, the NUV data will be used in conjunction with existing
optical, FUV and X-ray data to constrain a new generation of M dwarf
atmospheric models, and to explore unanswered questions regarding the
dynamo generation and magnetic heating in these low-mass stars.

ACS/WFC 10522

Calibrating Star Formation: The Link between Feedback and Galaxy
Evolution

Stellar feedback - the return of mass and energy from star formation
to the interstellar medium - is one of the primary engines of galaxy
evolution. Yet, the theoretical foundation of mechanical feedback is,
to date, unconstrained by observations. We propose to investigate this
fundamental aspect of star formation on a sample of two local actively
star-forming galaxies, NGC4449, and Holmberg II. The two galaxies have
been selected to occupy an unexplored, yet crucial for quantifying
mechanical feedback, niche in the two-parameter space of star
formation intensity and galaxy mass. ACS/WFC and WFPC2 narrow-band
observations in the light of H-beta, [OIII], H-alpha, and [NII] will
be obtained for both galaxies, in order to: {1} discriminate the
feedback- induced shock fronts from the photoionization regions; {2}
map the shocks inside and around the starburst regions; and {3}
measure the energy budget of the star-formation-produced shocks. These
observations, complemented by existing data, will yield: {1} the
efficiency of the feedback, i.e. the fraction of the star formation's
mechanical energy that is transported out of the starburst volume
rather than confined or radiated away; {2} the dependence of this
efficiency on the two fundamental parameters of star formation
intensity and stellar mass. The high angular resolution of HST is
crucial for separating the spatially narrow shock fronts {~5 pc,
~0.25" at 4 Mpc} from the more extended photoionization fronts. The
legacy from this project will be the most complete quantitative
measurement of the energetics associated with feedback processes. We
will secure the first milestone for placing feedback mechanisms on a
solid physical ground, and for understanding quantitatively their role
on the energetics, structure, and star formation history of galaxies
at all redshifts.

ACS/HRC/WFC 10438

The Late Formation of Satellite Galaxies

Tiny isolated HII regions have been discovered up to 30 kpc from the
closest galaxy in the NOAO Survey for Ionization in Neutral Gas
Galaxies {SINGG}. These halo HII regions can be ionized by only a few
OB stars and seem to be most commonly found in interacting systems.
They may represent the beginning of the formation of satellite
galaxies at low redshift and/or are the source of the numerous
intracluster planetary nebula. The halo HII regions are a unique mode
of star formation in a low density and low metallicity environment and
high resolution HST images are required to identify their underlying
stellar populations. Determining the stellar populations of these HII
regions will establish whether in-situ star formation is a significant
contributor to the stellar content and enrichment of galactic halos
and intergalactic space. In particular, ACS/HRC observations are
required for their resolution, UV sensitivity, and wide wavelength
coverage, allowing young and intermediate age populations to be
identified. Parallel ACS/WFC observations will explore the possibility
of a further stellar population in the interactive debris. The results
of this project have implications on the formation of satellite
galaxies, the origin of Galactic halo B stars, IGM ionization and
enrichment, and star formation principles.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

10020 - OBAD Failed ID / REAcq (1,2,1) not attempted @ 322/12:20:47z
OBAD1 scheduled @ 322/12:06:18 failed. At 12:08:02 recveived 486 ESB
1805(X2)(T2G Moving Target Detected) & 1902 (OBAD Failed ID). OBAD2
was successful and showed errors of: V1 -50.42, V2 2412.56, V3 -30.46,
RSS 2413.28. REAcq (1,2,1) scheduled @ 12:20:47 was not attempted.
There were no indications of transitioning to M2G. MAP @ 12:28:07
showed errors of: V1=6.77, V2=9.76, V3=11.58, RSS=16.59.

COMPLETED OPS REQUEST:
17590-0 - Update Benchmark SOC, SOC1, SOC2, and Pressure Limits @ 322/1412z
17537-1 - Restore TMDIAG Slot 0 for VehConLaw.Integral Path Data @ 322/1415z
17591-0 - Full Memory Dump @ 322/1701z

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 23 23
FGS
REacq 16 15 322/12:20:47
(HSTAR #10020)
OBAD with Maneuver 78 77 322/12:06:18
(HSTAR #10020)

SIGNIFICANT EVENTS:

FLASH REPORT

"Battery SOC Modifications"): On DOY 2005/322, Ops Request 17590-0 was
successfully executed to update the benchmark SOC, SOC1, SOC2, and
Pressure Limits. These updates were made because the six-battery
benchmark SOC, SOC 1 and SOC 2 should be adjusted periodically to
reflect changes in battery capacity. The Electrical Power Subsystem
continues to perform as expected.