Daily Report #4578

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4578

PERIOD COVERED: UT March 28,29,30, 2008 (DOY 088,089,090)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8795

NICMOS Post-SAA calibration - CR Persistence Part 6

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.

NIC 11495

The first direct detection of an extrasolar planetary stratosphere?

We request NICMOS grism spectroscopy to observe the transit of WASP-3b. This
newly discovered planet is the hottest nearby planet discovered so far. The
atmosphere is predicted to be so hot that TiO and VO remain in the gas
phase, creating a hot, strongly absorbing stratosphere. This molecular
absorption will cause a 6% enhancement in the transit depth at 0.8 microns,
compared to that at 1.3 microns. NICMOS/G096 and NICMOS/G141 observations
will therefore provide a straightforward test of the hot stratosphere
hypothesis. The HST observations will provide a precisely determined radius
measurement. This is required to drive advances in theories of planetary
formation, evolution, and atmospheric physics and chemistry. The atmospheric
TiO and VO absorption is predicted to cause an anomalously high IR
brightness temperature for the planet. We need HST's direct test of the hot
stratosphere hypothesis promptly to enable appropriate cold-Spitzer
observations to be planned and interpreted. Spitzer is likely to exhaust its
cryogens before these observations could be scheduled via the cycle 17 GO
process.

NIC1/NIC2/NIC3 11330

NICMOS Cycle 16 Extended Dark

This takes a series of Darks in parallel to other instruments.

WFPC2 11326

Polarizers Closeout (Internal Observations)

Verify stability of polarization calibration.

FGS 11300

Mass and Radius of a Near-Chandrasekhar-limit magnetic white dwarf

REJ0317-853 is a unique object. According to our analyses it is the most
massive white dwarf ever found, with a mass of 1.35 solar masses,
approaching the Chandrasekhar limit. With a period of just 725 seconds it is
the most rapidly rotating isolated white dwarf ever found. Moreover, RE
J0317-853 is the hottest magnetic white dwarf discovered so far and has a
strong magnetic field varying from about 180 to more than 700 MG over the
stellar surface. Due to its strong polarization and high mass it has been
used to test gravitational theories predicting gravitational birefringence.
However, the existing mass and radius determination is indirect and still
uncertain and would greatly profit from a high- precision parallax
determination with the HST FGS.

FGS 11212

Filling the Period Gap for Massive Binaries

The current census of binaries among the massive O-type stars is seriously
incomplete for systems in the period range from years to millennia because
the radial velocity variations are too small and the angular separations too
close for easy detection. Here we propose to discover binaries in this
observational gap through a Faint Guidance Sensor SNAP survey of relatively
bright targets listed in the Galactic O Star Catalog. Our primary goal is to
determine the binary frequency among those in the cluster/association,
field, and runaway groups. The results will help us assess the role of
binaries in massive star formation and in the processes that lead to the
ejection of massive stars from their natal clusters. The program will also
lead to the identification of new, close binaries that will be targets of
long term spectroscopic and high angular resolution observations to
determine their masses and distances. The results will also be important for
the interpretation of the spectra of suspected and newly identified binary
and multiple systems.

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 11198

Pure Parallel Imaging in the NDWFS Bootes Field

The NOAO Deep-Wide Field Survey {NDWFS} Bootes field is the target of one of
the most extensive multiwavelength campaigns in astronomy. In addition to
ground-based optical and near-infrared imaging, deep radio mapping, and
extensive spectroscopy, this entire region has been imaged by the Chandra,
Spitzer {IRAC and MIPS}, and GALEX missions. Robust photometric redshifts
{calibrated using over 20,000 spectroscopic redshifts} exist for all sources
brighter than R=24.5 or than 13 uJy at 4.5 microns. To enhance the value of
this data set, we propose pure parallel observations for all approved Cycle
16 programs in this region that lack coordinated parallel observations. The
primary aim of this program will be to provide a database useful for the
broad range of science programs underway in this region.

WEPC2 11196

An Ultraviolet Survey 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 starbursts and creating/fueling central AGN. We propose
far {ACS/SBC/F140LP} and near {WFPC2/PC/F218W} UV imaging of a sample of 27
galaxies drawn from the complete IRAS Revised Bright Galaxy Sample {RBGS}
LIRGs sample and known, from our Cycle 14 B and I-band ACS imaging
observations, to have significant numbers of bright {23 B 21 mag} star
clusters in the central 30 arcsec. The HST UV data will be combined with
previously obtained HST, Spitzer, and GALEX images to {i} calculate the ages
of the clusters as function of merger stage, {ii} measure the amount of UV
light in massive star clusters relative to diffuse regions of star
formation, {iii} assess the feasibility of using the UV slope to predict the
far-IR luminosity {and thus the star formation rate} both among and within
IR-luminous galaxies, and {iv} provide a much needed catalog of rest- frame
UV morphologies for comparison with rest-frame UV images of high-z LIRGs and
Lyman Break Galaxies. These observations will achieve the resolution
required to perform both detailed photometry of compact structures and
spatial correlations between UV and redder wavelengths for a physical
interpretation our IRX-Beta results. The HST UV data, combined with the HST
ACS, Spitzer, Chandra, and GALEX observations of this sample, will result in
the most comprehensive study of luminous starburst galaxies to date.

NIC3 11195

Morphologies of the Most Extreme High-Redshift Mid-IR-luminous Galaxies II:
The `Bump' Sources

The formative phase of some of the most massive galaxies may be extremely
luminous, characterized by intense star- and AGN-formation. Till now, few
such galaxies have been unambiguously identified at high redshift, and thus
far we have been restricted to studying the low-redshift ultraluminous
infrared galaxies as possible analogs. We have recently discovered a sample
of objects which may indeed represent this early phase in galaxy formation,
and are undertaking an extensive multiwavelength study of this population.
These objects are optically extremely faint {R26} but nevertheless bright
at mid-infrared wavelengths {F[24um] 0.5 mJy}. Mid-infrared spectroscopy
with Spitzer/IRS reveals that they have redshifts z~2, implying luminosities
~1E13 Lsun. Their mid-IR SEDs fall into two broad, perhaps overlapping,
categories. Sources with brighter F[24um] exhibit power-law SEDs and SiO
absorption features in their mid-IR spectra characteristic of AGN, whereas
those with fainter F[24um] show a "bump" characteristic of the redshifted
1.6um peak from a stellar population, and PAH emission characteristic of
starformation. We have begun obtaining HST images of the brighter sources in
Cycle 15 to obtain identifications and determine kpc-scale morphologies for
these galaxies. Here, we aim to target the second class {the "bump" sources}
with the goal of determining if these constitute morphologically different
objects, or simply a "low-AGN" state of the brighter class. The proposed
observations will help us determine whether these objects are merging
systems, massive obscured starbursts {with obscuration on kpc scales!} or
very reddened {locally obscured} AGN hosted by intrinsically low-luminosity
galaxies.

WFPC2 11169

Collisions in the Kuiper belt

For most of the 15 year history of observations of Kuiper belt objects, it
has been speculated that impacts must have played a major role in shaping
the physical and chemical characteristics of these objects, yet little
direct evidence of the effects of such impacts has been seen. The past 18
months, however, have seen an explosion of major new discoveries giving some
of the first insights into the influence of this critical process. From a
diversity of observations we have been led to the hypotheses that: {1}
satellite-forming impacts must have been common in the Kuiper belt; {2} such
impacts led to significant chemical modification; and {3} the outcomes of
these impacts are sufficiently predictable that we can now find and study
these impact-derived systems by the chemical and physical attributes of both
the satellites and the primaries. If our picture is correct, we now have in
hand for the first time a set of incredibly powerful tools to study the
frequency and outcome of collisions in the outer solar system. Here we
propose three linked projects that would answer questions critical to the
multiple prongs of our hypothesis. In these projects we will study the
chemical effects of collisions through spectrophotometric observations of
collisionally formed satellites and through the search for additional
satellites around primaries with potential impact signatures, and we will
study the physical effects of impacts through the examination of tidal
evolution in proposed impact systems. The intensive HST program that we
propose here will allow us to fully test our new hypotheses and will provide
the ability to obtain the first extensive insights into outer solar system
impact processes.

WFPC2 11161

Revealing the Explosion Geometry of Nearby GRB-SNe

The connection between gamma-ray bursts and Type Ibc supernovae is
well-established in broad terms. However, our recent identification of an
intermediate class of sub-energetic GRBs, and the overall overlap in Nickel
production between GRB-SNe and ordinary SNe Ibc suggest that the properties
leading to the production of a relativistic engine are yet to be uncovered.
A fundamental difference between the two classes of explosions may be
imprinted in the overall geometry of the explosion. The relativistic
component of GRBs is known to be highly collimated, but it is unclear if the
SN blast is spherical or mildly collimated as well. Here we propose HST
observations of the late (30 days) decay tails of two GRB-SNe as an
independent measure of the Nickel mass synthesized in the explosion. A
comparison to the Nickel mass inferred from the peak brightness of the SNe
will provide a direct measure of the explosion asymmetry, since at late time
the explosion is essentially spherical. These observations will form the
core of a multi-wavelength (optical, X-ray, radio) effort to fully
characterize all aspects of the explosions, from the energy and geometry of
the relativistic material (VLA, Chandra) to the early SN evolution (Keck,
Magellan). The proposed observations require two slow-response (30 days)
TOOs, ideally suited to the 2-gyro operations of HST.

NIC3 11153

The Physical Nature and Age of Lyman Alpha Galaxies

In the simplest scenario, strong Lyman alpha emission from high redshift
galaxies would indicate that stellar populations younger than 10 Myrs
dominate the UV. This does not, however, constrain the stellar populations
older than 100 Myrs, which do not contribute to UV light. Also, the Lyman
alpha line can be boosted if the interstellar medium is both clumpy and
dusty. Different studies with small samples have reached different
conclusions about the presence of dust and old stellar populations in Lyman
alpha emitters. We propose HST- NICMOS and Spitzer-IRAC photometry of 35
Lyman-alpha galaxies at redshift 4.5z6.5, in order to determine their
spectral energy distribution {SED} extending through rest-frame optical.
This will allow us to measure accurately {1} The total stellar mass in these
objects, including old stars which may have formed at redshifts {z 8} not
easily probed by any other means. {2} The dust extinction in the rest-frame
UV, and therefore a correction to their present star-formation rates. Taken
together, these two quantities will yield the star-formation histories of
Lyman alpha galaxies, which form fully half of the known galaxies at z=4-6.
They will tell us whether these are young or old galaxies by straddling the
4000A break. Data from NICMOS is essential for these compact and faint
{i=25-26th magnitude AB} high redshift galaxies, which are too faint for
good near-IR photometry from the ground.

WFPC2 11130

AGNs with Intermediate-mass Black Holes: Testing the Black Hole-Bulge
Paradigm, Part II

The recent progress in the study of central black holes in galactic nuclei
has led to a general consensus that supermassive {10^6-10^9 solar mass}
black holes are closely connected with the formation and evolutionary
history of large galaxies, especially their bulge component. Two outstanding
issues, however, remain unresolved. Can central black holes form in the
absence of a bulge? And does the mass function of central black holes extend
below 10^6 solar masses? Intermediate-mass black holes {10^6 solar masses},
if they exist, may offer important clues to the nature of the seeds of
supermassive black holes. Using the SDSS, our group has successfully
uncovered a new population of AGNs with intermediate-mass black holes that
reside in low-luminosity galaxies. However, very little is known about the
detailed morphologies or structural parameters of the host galaxies
themselves, including the crucial question of whether they have bulges or
not. Surprisingly, the majority of the targets of our Cycle 14 pilot program
have structural properties similar to dwarf elliptical galaxies. The
statistics from this initial study, however, are really too sparse to reach
definitive conclusions on this important new class of black holes. We wish
to extend this study to a larger sample, by using the Snapshot mode to
obtain WFPC2 F814W images from a parent sample of 175 AGNs with
intermediate- mass black holes selected from our final SDSS search. We are
particularly keen to determine whether the hosts contain bulges, and if so,
how the fundamental plane properties of the host depend on the mass of their
central black holes. We will also investigate the environment of this unique
class of AGNs.

WFPC2 11124

The Origin of QSO Absorption Lines from QSOs

We propose using WFPC2 to image the fields of 10 redshift z ~ 0.7 foreground
{FG} QSOs which lie within ~29-151 kpc of the sightlines to high-z
background {BG} QSOs. A surprisingly high fraction of the BG QSO spectra
show strong MgII {2796,2803} absorption lines at precisely the same
redshifts as the FG QSOs. The high resolution capabilities of WFPC2 are
needed to understand the origin of these absorption systems, in two ways.
First, we wish to explore the FG QSO environment as close as possible to the
position of the BG QSO, to search for interloping group or cluster galaxies
which might be responsible for the absorption, or irregularly shaped
post-merger debris between the FG and BG QSO which may indicate the presence
of large amount of disrupted gas along a sightline. Similarly, high
resolution images are needed to search for signs of tidal interactions
between any galaxies which might be found close to the FG QSO. Such features
might provide evidence of young merging events causing the start of QSO duty
cycles and producing outflows from the central AGN. Such winds may be
responsible for the observed absorption lines. Second, we seek to measure
the intrinsic parameters of the FG QSO host galaxy, such as luminosity and
morphology, to correlate with the properties of the MgII absorption lines.
We wish to observe each field through the F814W filter, close to the rest-
frame B-band of the FG QSO. These blue data can reveal enhanced star
formation regions close to the nucleus of the host galaxy, which may be
indicative of galaxy mergers with the FG QSO host. The FG QSO environment
offers quite a different set of phenomena which might be responsible for
MgII absorption, providing an important comparison to studies of MgII
absorption from regular field galaxies.

NIC3 11120

A Paschen-Alpha Study of Massive Stars and the ISM in the Galactic Center

The Galactic center (GC) is a unique site for a detailed study of a
multitude of complex astrophysical phenomena, which may be common to nuclear
regions of many galaxies. Observable at resolutions unapproachable in other
galaxies, the GC provides an unparalleled opportunity to improve our
understanding of the interrelationships of massive stars, young stellar
clusters, warm and hot ionized gases, molecular clouds, large scale magnetic
fields, and black holes. We propose the first large-scale hydrogen Paschen
alpha line survey of the GC using NICMOS on the Hubble Space Telescope. This
survey will lead to a high resolution and high sensitivity map of the
Paschen alpha line emission in addition to a map of foreground extinction,
made by comparing Paschen alpha to radio emission. This survey of the inner
75 pc of the Galaxy will provide an unprecedented and complete search for
sites of massive star formation. In particular, we will be able to (1)
uncover the distribution of young massive stars in this region, (2) locate
the surfaces of adjacent molecular clouds, (3) determine important physical
parameters of the ionized gas, (4) identify compact and ultra-compact HII
regions throughout the GC. When combined with existing Chandra and Spitzer
surveys as well as a wealth of other multi-wavelength observations, the
results will allow us to address such questions as where and how massive
stars form, how stellar clusters are disrupted, how massive stars shape and
heat the surrounding medium, and how various phases of this medium are
interspersed.

WFPC2 11083

The Structure, Formation and Evolution of Galactic Cores and Nuclei

A surprising result has emerged from the ACS Virgo Cluster Survey {ACSVCS},
a program to obtain ACS/WFC gz imaging for a large, unbiased sample of 100
early-type galaxies in the Virgo Cluster. On subarcsecond scales {i.e.,
0.1"-1"}, the HST brightness profiles vary systematically from the
brightest giants {which have nearly constant surface brightness cores} to
the faintest dwarfs {which have compact stellar nuclei}. Remarkably, the
fraction of galaxy mass contributed by the nuclei in the faint galaxies is
identical to that contributed by supermassive black holes in the bright
galaxies {0.2%}. These findings strongly suggest that a single mechanism is
responsible for both types of Central Massive Object: most likely internally
or externally modulated gas inflows that feed central black holes or lead to
the formation of "nuclear star clusters". Understanding the history of gas
accretion, star formation and chemical enrichment on subarcsecond scales has
thus emerged as the single most pressing question in the study of nearby
galactic nuclei, either active or quiescent. We propose an ambitious HST
program {199 orbits} that constitutes the next, obvious step forward:
high-resolution, ultraviolet {WFPC2/F255W} and infrared {NIC1/F160W} imaging
for the complete ACSVCS sample. By capitalizing on HST's unique ability to
provide high-resolution images with a sharp and stable PSF at UV and IR
wavelengths, we will leverage the existing optical HST data to obtain the
most complete picture currently possible for the history of star formation
and chemical enrichment on these small scales. Equally important, this
program will lead to a significant improvement in the measured structural
parameters and density distributions for the stellar nuclei and the
underlying galaxies, and provide a sensitive measure of "frosting" by young
stars in the galaxy cores. By virtue of its superb image quality and stable
PSF, NICMOS is the sole instrument capable of the IR observations proposed
here. In the case of the WFPC2 observations, high-resolution UV imaging {
0.1"} is a capability unique to HST, yet one that could be lost at any time.

NIC2 10852

Coronagraphic Polarimetry with NICMOS: Dust grain evolution in T Tauri stars

The formation of planetary systems is intimately linked to the dust
population in circumstellar disks, thus understanding dust grain evolution
is essential to advancing our understanding of how planets form. By
combining {1} the coronagraphic polarimetry capabilities of NICMOS, {2}
powerful 3-D radiative transfer codes, and {3} observations of objects known
to span the Class II- III stellar evolutionary phases, we will gain crucial
insight into dust grain growth. By observing objects representative of a
known evolutionary sequence of YSOs, we will be able to investigate how the
dust population evolves in size and distribution during the crucial
transition from a star+disk system to a system containing planetesimals.
When combine with our previous study on dust grain evolution in the Class
I-II phase, the proposed study will help to establish the fundamental time
scales for the depletion of ISM-like grains: the first step in understanding
the transformation from small submicron sized dust grains, to large
millimeter sized grains, and untimely to planetary bodies.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

11236 - GSacq(2,1,2) failed to RGA control.

GSacq(2,1,2) scheduled at 090/17:10:06 failed to RGA control. The GSacq
failed due to receiving stop flags QF2STOPF and QSTOP on FGS 2. OBAD1 showed
errors of V1=1299.52, V2=100.45, V3=-60.96 and RSS=1304.82. OBAD2 showed
errors of V1=-8.74, V2=-2.04, V3=-7.01 and RSS=11.38.

11237 - REacq(2,1,2) failed to RGA control.

The REacq(2,1,2) scheduled at 090/18:45:33 failed during LOS due to
receiving stop flags on FGS 1 and FGS 2. OBAD2 had an RSS value of 5.20a-s.

COMPLETED OPS REQUEST:

18218-1 - TGS/KFSP Safemode Reconfiguration @088/1000z @ 088/13:43:31z
18054-0 - Preview KF Sun Vector Data via Telemetry Diags (Generic) @
088/13:47z

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL

FGS GSacq 26 25
FGS REacq 16 15
OBAD with Maneuver 84 84

SIGNIFICANT EVENTS:

FLASH REPORT KFSP SAFEMODE RECONFIGURATION:

Ops Request 18218 was successfully executed at 13:43:31 on day 088 (March
28) to uplink and reconfigure FSW with KFSP as a potential safemode
response. Initial configuration of KFSP parameters were performed first
using IP-151 to set the proper UKF/KFSP control gains and limits, followed
by resetting of UKF database parameters for maximum error counts for MSS and
gyro A using IP-127 and modifying the co-alignment angular limit to the
expected value of 30 degrees per IP-152. Per IP-153, new SMACs, HMACs,
safemode response table and safemode recovery macro were uplinked to
configure for usage of KFSP. Following the completion of IP-153, the new
KFSP Bypass test was enabled, and Ops Note 1681 was executed to restore the
limit for the test.

Telemetry was monitored for 1 orbit following the macro uplink and
everything was nominal.