HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT #4651
PERIOD
COVERED: 5am July 11 - 5am July 14, 2008 (DOY193/0900z-196/0900z)
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 i
mages.
Each observation will need its own CRMAP, as different SAA
passages
leave different imprints on the NICMOS detectors.
NIC3
11545
A
NICMOS Survey of Newly-Discovered Young Massive Clusters
We
are on the cusp of a revolution in massive star research triggered by
2MASS
and Spitzer/GLIMPSE, and now is the ideal time to capitalize on
these
projects by performing the first survey of massive stars in young
stellar
clusters throughout the Galactic plane. A search of the 2MASS
and
GLIMPSE surveys has produced over 450 newly-identified massive
stellar
cluster candidates in the Galactic plane which are hidden from
our
view at optical wavelengths due to extinction. Here we propose a
program
of 29 orbits to image the most promising candidate clusters in
broad
and narrow band filters using HST/NICMOS. We will be complementing
these
observations with approved Spitzer and Chandra programs,
numerous
approved and planned ground-based spectroscopic observations,
and
state-of-the-art modeling. We expect to substantially increase the
numbers
of massive stars known in the Galaxy, including main sequence
stars
and post-main sequence stars in the Red Supergiant, Luminous Blue
Variable
and Wolf-Rayet stages. Ultimately, this program will address
many
of the fundamental topics in astrophysics: the slope to the initial
mass
function (IMF), an upper-limit to the masses of stars, the
formation
and evolution of the most massive stars, gamma-ray burst (GRB)
progenitors,
the chemical enrichment of the interstellar medium, and
nature
of the first stars in the Universe.
NIC1/NIC2/NIC3
11330
NICMOS
Cycle 16 Extended Dark
This
takes a series of Darks in parallel to other instruments.
S/C
11320
NICMOS
Focus Monitoring Cycle 16
This
program is a version of the standard focus sweep used since cycle
7.
It has been modified to go deeper and uses more narrow filters for
improved
focus determination. A new source was added in Cycle 14 in
order
to accommodate 2-gyro mode: the open cluster NGC1850. This source
is
part of the current proposal. The old target, the open cluster
NGC3603,
will be used whenever available and the new target used to fill
the
periods when NGC3603 is not visible. Steps: a) Use refined target
field
positions as determined from cycle 7 calibrations b) Use
MULTIACCUM
sequences of sufficient dynamic range to account for defocus
c)
Do a 17-point focus sweep, +/- 8mm about the PAM mechanical zeropoint
for
each cameras 1 and 2, in 1.0mm steps. For NIC3 we step from -0.5mm
to
-9.5mm relative to mechanical zero, in steps of 1.0mm. d) Use PAM X/Y
tilt
and OTA offset slew compensations refined from previous focus
monitoring/optical
alignment activities
NIC2
11237
The
Origin of the Break in the AGN Luminosity Function
We
propose to use NICMOS imaging to measure rest-frame optical
luminosities
and morphological properties of a complete sample of faint
AGN
host galaxies at redshifts z ~ 1.4. The targets are drawn from the
VLT-VIMOS
Deep Survey, and they constitute a sample of the lowest
luminosity
type 1 AGN known at z > 1. The spectroscopically estimated
black
hole masses are up to an order of magnitude higher than expected
given
their nuclear luminosities, implying highly sub-Eddington
accretion
rates. This exactly matches the prediction made by recent
theoretical
models of AGN evolution, according to which the faint end of
the
AGN luminosity function is populated mainly by big black holes that
have
already exhausted a good part of their fuel. In this proposal we
want
to test further predictions of that hypothesis, by focusing on the
host
galaxy properties of our low-luminosity, low- accretion AGN. If the
local
ratio between black hole and bulge masses holds at least
approximately
at these redshifts, one expects most of these
low-luminosity
AGN to reside in fairly big ellipticals with stellar
masses
around and above 10^11 solar masses (in contrast to the Seyfert
phenomenon
in the local universe). With NICMOS imaging we will find out
whether
that is true, implying also a sensitive test for the validity of
the
M_BH/M_bulge relation at z ~ 1.4.
WFPC2
11235
HST
NICMOS Survey of the Nuclear Regions 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
NICMOS
NIC2 imaging of the nuclear regions 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
and resolution of NICMOS NIC2 on HST enables a unique
opportunity
to study the detailed structure of the nuclear regions,
where
dust obscuration may mask star clusters, AGN and additional nuclei
from
optical view, with a resolution significantly higher than possible
with
Spitzer IRAC. This survey thus provides a crucial component to our
study
of the dynamics and evolution of IR galaxies presently underway
with
Wide-Field, HST ACS/WFC and Spitzer IRAC observations of these 88
galaxies.
Imaging will be done with the F160W filter {H-band} to examine
as
a function of both luminosity and merger stage {i} the luminosity and
distribution
of embedded star clusters, {ii} the presence of optically
obscured
AGN and nuclei, {iii} the correlation between the distribution
of
1.6 micron emission and the mid-IR emission as detected by Spitzer
IRAC,
{iv} the evidence of bars or bridges that may funnel fuel into the
nuclear
region, and {v} the ages of star clusters for which photometry
is
available via ACS/WFC observations. The NICMOS data, combined with
the
HST ACS, Spitzer, and GALEX observations of this sample, will result
in
the most comprehensive study of merging and interacting galaxies to
date.
WFPC2
11222
Direct
Detection and Mapping of Star Forming Regions in Nearby, Luminous
Quasars
We
propose to carry out narrow-band emission line imaging observations
of
8 quasars at z=0.05-0.15 with the WFPC2 ramp filters and with the
NICMOS
narrow-band filters. We will obtain images in the [O II], [O
III],
H-beta, and Pa-alpha emission line bands to carry out a series of
diagnostic
tests aimed at detecting and mapping out star-forming regions
in
the quasar host galaxies. This direct detection of star-forming
regions
will confirm indirect indications for star formation in quasar
host
galaxies. It will provide a crucial test for models of quasar and
galaxy
evolution, that predict the co-existence of starbursts and
"monsters"
and will solve the puzzle of why different indicators of star
formation
give contradictory results. A secondary science goal is to
assess
suggested correlations between quasar luminosity and the size of
the
narrow-line region.
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
11211
An
Astrometric Calibration of Population II Distance Indicators
In
2002 HST produced a highly precise parallax for RR Lyrae. That
measurement
resulted in an absolute magnitude, M{V}= 0.61+/-0.11, a
useful
result, judged by the over ten refereed citations each year
since.
It is, however, unsatisfactory to have the direct,
parallax-based,
distance scale of Population II variables based on a
single
star. We propose, therefore, to obtain the parallaxes of four
additional
RR Lyrae stars and two Population II Cepheids, or
stars.
The Population II Cepheids lie with the RR Lyrae stars on a
common
K-band Period- Luminosity relation. Using these parallaxes to
inform
that relationship, we anticipate a zero- point error of 0.04
magnitude.
This result should greatly strengthen confidence in the
Population
II distance scale and increase our understanding of RR Lyrae
star
and Pop II Cepheid astrophysics.
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.
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.
WFPC2
11167
A
Unique High Resolution Window to Two Strongly Lensed Lyman Break
Galaxies
On
rare occasions, the otherwise very faint Lyman Break Galaxies {LBGs}
are
magnified by gravitational lensing to provide exceptional targets
for
detailed spectroscopic and imaging studies. We propose HST WFPC2 and
NICMOS
imaging of two strongly lensed Lyman Break Galaxies {LBGs} that
were
recently discovered by members of our team. These two LBGs -- the
"8
O'Clock Arc" and the "SDSS J1206+5142 Arc" -- are currently the
brightest
known LBGs, roughly 3 times brighter than the former
record-holder,
MS1512-cB58 {a.k.a. "cB58"}. The z=2.73 "8 O'Clock Arc"
extends
~10 arcsec in length and is magnified by a factor of 12. The
z=2.00
"SDSS J1206+5142 Arc" also extends ~10 arcsec in length and is
magnified
by a factor of 30. Due to their brightness and magnification,
these
two strongly lensed LBGs offer an unprecedented opportunity for
the
very detailed investigation of two individual galaxies at high
redshift.
We are currently pursuing a vigorous ground-based campaign to
obtain
multi- wavelength {UV, optical, NIR, radio} observations of these
two
LBGs, but our campaign currently lacks a means of obtaining
high-resolution
optical/NIR imaging -- a lack that currently only HST
can
address. Our prime objective for this proposal is to obtain high
resolution
HST images of these two systems with two-orbit WFPC2 images
in
the BVI bands and two-orbit NICMOS/NIC2 images in the J and H bands.
These
data will allow us to construct detailed lensing models, probe the
mass
and light profiles of the lenses and their environments, and
constrain
the star formation histories and rest-frame UV/optical
spectral
energy distributions of the LBGs.
NIC1/NIC2
11155
Dust
Grain Evolution in Herbig Ae Stars: NICMOS Coronagraphic Imaging
and
Polarimetry
We
propose to take advantage of the sensitive coronagraphic capabilities
of
NICMOS to obtain multiwavelength coronagraphic imaging and
polarimetry
of primordial dust disks around young intermediate-mass
stars
{Herbig Ae stars}, in order to advance our understanding of how
dust
grains are assembled into larger bodies. Because the polarization
of
scattered light is strongly dependent on scattering particle size and
composition,
coronagraphic imaging polarimetry with NICMOS provides a
uniquely
powerful tool for measuring grain properties in spatially
resolved
circumstellar disks. It is widely believed that planets form
via
the gradual accretion of planetesimals in gas-rich, dusty
circumstellar
disks, but the connection between this suspected process
and
the circumstellar disks that we can now observe around other stars
remains
very uncertain. Our proposed observations, together with
powerful
3-D radiative transfer codes, will enable us to quantitatively
determine
dust grain properties as a function of location within disks,
and
thus to test whether dust grains around young stars are in fact
growing
in size during the putative planet-formation epoch. HST imaging
polarimetry
of Herbig Ae stars will complement and extend existing
polarimetric
studies of disks around lower-mass T Tauri stars and debris
disks
around older main-sequence stars. When combined with these
previous
studies, the proposed research will help us establish the
influence
of stellar mass on the growth of dust grains into larger
planetesimals,
and ultimately to planets. Our results will also let us
calibrate
models of the thermal emission from these disks, a critical
need
for validating the properties of more distant disks inferred on the
basis
of spectral information alone.
ACS/SBC
11151
Evaluating
the Role of Photoevaporation of Protoplanetary Disk Dispersal
Emission
produced by accretion onto the central star leads to
photoevaporation,
which may play a fundamental role in disk dispersal.
Models
of disk photoevaporation by the central star are challenged by
two
potential problems: the emission produced by accretion will be
substantially
weaker for low-mass stars, and photoevaporation must
continue
as accretion slows. Existing FUV spectra of CTTSs are biased to
solar-mass
stars with high accretion rates, and are therefore
insufficient
to address these problems. We propose use HST/ACS SBC
PR130L
to obtain FUV spectra of WTTSs and of CTTSs at low masses and
mass
accretion rates to provide crucial data to evaluate
photoevaporation
models. We will estimate the FUV and EUV luminosities
of
low-mass CTTSs with small mass accretion rates, CTTSs with transition
disks
and slowed accretion, and of magnetically-active WTTSs.
WFPC2/NIC3/ACS/SBC
11144
Building
on the Significant NICMOS Investment in GOODS: A Bright,
Wide-Area
Search for z>=7 Galaxies
One
of the most exciting frontiers in observational cosmology has been
to
trace the buildup and evolution of galaxies from very early times.
While
hierarchical theory teaches us that the star formation rate in
galaxies
likely starts out small and builds up gradually, only recently
has
it been possible to see evidence for this observationally through
the
evolution of the LF from z~6 to z~3. Establishing that this build up
occurs
from even earlier times {z~7-8} has been difficult, however, due
to
the small size of current high-redshift z~7-8 samples -- now
numbering
in the range of ~4-10 sources. Expanding the size of these
samples
is absolutely essential, if we are to push current studies of
galaxy
buildup back to even earlier times. Fortunately, we should soon
be
able to do so, thanks to ~50 arcmin**2 of deep {26.9 AB mag at 5
sigma}
NICMOS 1.6 micron data that will be available over the two ACS
GOODS
fields as a result of one recent 180-orbit ACS backup program and
a
smaller program. These data will nearly triple the deep near-IR
imaging
currently available and represent a significant resource for
finding
and characterizing the brightest high-redshift sources -- since
high-redshift
candidates can be easily identified in these data from
their
red z-H colours. Unfortunately, the red z-H colours of these
candidates
are not sufficient to determine that these sources are at
z>=7,
and it is important also to have deep photometry at 1.1 microns.
To
obtain this crucial information, we propose to follow up each of
these
z-H dropouts with NICMOS at 1.1 microns to determine which are at
high
redshift and thus significantly expand our sample of luminous, z>=7
galaxies.
Since preliminary studies indicate that these candidates occur
in
only 30% of the NIC3 fields, our follow-up strategy is ~3 times as
efficient
as without this preselection and 9 times as efficient as a
search
in a field with no pre-existing data. In total, we expect to
identify
~8 luminous z-dropouts and possibly ~2 z~10 J-dropouts as a
result
of this program, more than tripling the number currently known.
The
increased sample sizes are important if we are to solidify current
conclusions
about galaxy buildup and the evolution of the LF from z~8.
In
addition to the high redshift science, these deep 1.1 micron data
would
have significant value for many diverse endeavors, including {1}
improving
our constraints on the stellar mass density at z~7-10 and {2}
doubling
the number of galaxies at z~6 for which we can estimate dust
obscuration.
NIC2/WFPC2
11142
Revealing
the Physical Nature of Infrared Luminous Galaxies at 0.3<z<2.7
Using
HST and Spitzer
We
aim to determine physical properties of IR luminous galaxies at
0.3<z<2.7
by requesting coordinated HST/NIC2 and MIPS 70um observations
of
a unique, 24um flux-limited sample with complete Spitzer mid-IR
spectroscopy.
The 150 sources investigated in this program have S{24um}
>
0.8mJy and their mid-IR spectra have already provided the majority
targets
with spectroscopic redshifts {0.3<z<2.7}. The proposed
150~orbits
of NIC2 and 66~hours of MIPS 70um will provide the physical
measurements
of the light distribution at the rest-frame ~8000A and
better
estimates of the bolometric luminosity. Combining these
parameters
together with the rich suite of spectral diagnostics from the
mid-IR
spectra, we will {1} measure how common mergers are among LIRGs
and
ULIRGs at 0.3<z<2.7, and establish if major mergers are the drivers
of
z>1 ULIRGs, as in the local Universe. {2} study the co-evolution of
star
formation and blackhole accretion by investigating the relations
between
the fraction of starburst/AGN measured from mid-IR spectra vs.
HST
morphologies, L{bol} and z. {3} obtain the current best estimates of
the
far-IR emission, thus L{bol} for this sample, and establish if the
relative
contribution of mid-to-far IR dust emission is correlated with
morphology
{resolved vs. unresolved}.
WFPC2
11129
The
Star Formation History of the Fornax Dwarf Spheroidal Galaxy
The
Fornax dwarf spheroidal galaxy is one of the most luminous dwarf
satellites
of the Milky Way. It is unusual in many ways: it hosts 5
globular
clusters, shows some relatively young stars, and has faint
sub-structures
which have been interpreted as signs of recent
interactions.
It is thus of great interest to learn the complete star
formation
history {SFH} of Fornax to establish a link between its
evolutionary
path and the predictions from numerical simulations, as a
test
of our understanding of dwarf galaxy evolution. Yet many questions
remain
open. Is the old stellar population made up of stars formed in a
very
early burst, perhaps before the epoch of re- ionization, or the
result
of a more continuous star formation between 13 and 9 Gyr ago ?
How
quickly did Fornax increase its metallicity during its initial
assembly
and during subsequent episodes of star formation ? Are
accretion
episodes required to explain the age-metallicity history of
Fornax
? However, there has never been a comprehensive study of the
global
SFH of the Fornax field based on data of sufficient depth to
unambiguously
measure the age mixture of the stellar populations and
their
spatial variation. We propose to use the WFPC2 to obtain very deep
images
in several fields across the central region of Fornax in order to
reach
the oldest main-sequence turnoffs. The number of fields is
determined
by the need to measure the SFH over different regions with
distinct
kinematics and metallicity. The resolution achievable with HST
is
crucial to answer these questions because, to derive the age
distribution
of the oldest stars, we are interested in I magnitude
differences
of the order 0.2 mag in crowded fields at V=24.5. We will
directly
measure the time variation in star-formation rate over the
entire
galaxy history, from first stars coeval with the Milky Way halo
to
the youngest populations 200 Myr ago. The combination of detailed CMD
analysis
with WFPC2 with our existing metallicity and kinematic
information
will allow us to trace out the early phases of its
evolution.
WFPC2
11039
Polarizers
Closeout
Observations
of standard stars and a highly polarized reflection nebula
are
made as a final calibration for the WFPC2 polarizers. VISFLATS are
also
obtained.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
11386
- GSACQ(2,0,2) failed
GSACQ(2,0,2) at 194/13:34:20 failed to RGA control with QF2STOPF and
QSTOP flags set at 13:39:26. No other flags were seen. Three 486 ESB
"1805" messages (T2G_MOVING_TARGET_DETECTED) were received at that
time,
with two more received at 13:41:06 and 13:41:18.
Observations affected: Astrometry, Proposal 11210.
COMPLETED
OPS REQUEST:
18250-0
- Off-Line +BB SPA Trim Relay @ 193/1406z
COMPLETED
OPS NOTES: None
SCHEDULED SUCCESSFUL
FGS
GSacq 23 22
FGS
REacq 16 16
OBAD
with Maneuver 78 78
SIGNIFICANT
EVENTS:
Battery
3 SPA Off-lined Flash Report:
The
+BB SPA Trim relay (
post-beta-peak
warming of the Bay 2 battery module. Commanding to
off-line
the SPA was performed at 193/1405 GMT via Ops Request 18250. In
the
orbit immediately following the uplink
was
below 5.0 degrees C. The same action was taken following the beta
peak
in May.