Notice: For the foreseeable future, the daily reports may
contain
apparent discrepancies between some proposal descriptions
and the listed
instrument usage. This is due to the conversion of
previously approved
ACS WFC or HRC observations into WFPC2, or NICMOS
observations
subsequent to the loss of ACS CCD science capability in
late January.
HUBBLE SPACE TELESCOPE - Continuing to collect World Class
Science
DAILY REPORT # 4380
PERIOD COVERED: UT June 08,09,10, 2007 (DOY 159,160,161)
OBSERVATIONS SCHEDULED
NIC1/NIC2/NIC3 8794
NICMOS Post-SAA calibration - CR Persistence Part 5
A new procedure proposed to alleviate the CR-persistence
problem of
NICMOS. Dark frames will be obtained immediately upon
exiting the SAA
contour 23, and every time a NICMOS exposure is scheduled
within 50
minutes of coming out of the SAA. The darks will be
obtained in parallel
in all three NICMOS Cameras. The POST-SAA darks will be
non- standard
reference files available to users with a USEAFTER
date/time mark. The
keyword 'USEAFTER=date/time' will also be added to the
header of each
POST-SAA DARK frame. The keyword must be populated with
the time, in
addition to the date, because HST crosses the SAA ~8 times
per day so
each POST-SAA DARK will need to have the appropriate time
specified, for
users to identify the ones they need. Both the raw and
processed images
will be archived as POST-SAA DARKSs. Generally we expect
that all NICMOS
science/calibration observations started within 50 minutes
of leaving an
SAA will need such maps to remove the CR persistence from
the science
images. Each observation will need its own CRMAP, as
different SAA
passages leave different imprints on the NICMOS detectors.
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
indvidual
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.
NIC1 11057
Cycle 15 NICMOS dark current, shading profile, and read
noise monitoring
program
The purpose of this proposal is to monitor the dark
current, read noise,
and shading profile for all three NICMOS detectors
throughout the
duration of Cycle 15. This proposal is a slightly modified
version of
proposal 10380 of cycle 13 and 9993 of cycle12 and is the
same as Cycle
14. that we cut down some exposure time to make the
observation fit
within 24 orbits.
FGS 10927
The Weight-Watcher Program for Subdwarfs
We propose to use HST/FGS1r to measure five subdwarf
spectroscopic
binaries to determine masses for the components. Their
metallicities,
[Fe/H], range from -0.5 to -2.5, and their projected
minimum separations
range from 9 to 24 mas. These binaries are resolvable with
HST/FGS1r but
not any ground-based technique. Currently, there are only
two subdwarf
systems having any mass measurements. The proposed work
will boost the
total number of subdwarf systems with masses from two to
seven, and
allow us to construct the first mass-luminosity relation
for
low-metallicity stars.
NIC2 10893
Sweeping Away the Dust: Reliable Dark Energy with an
Infrared Hubble
Diagram
We propose building a high-z Hubble Diagram using type Ia
supernovae
observed in the infrared rest-frame J-band. The infrared
has a number of
exceptional properties. The effect of dust extinction is
minimal,
reducing a major systematic tha may be biasing dark energy
measurements.
Also, recent work indicates that type Ia supernovae are
true standard
candles in the infrared meaning that our Hubble diagram
will be
resistant to possible evolution in the Phillips relation
over cosmic
time. High signal-to-noise measurements of 9 type Ia
events at z~0.4
will be compared with an independent optical Hubble
diagram from the
ESSENCE project to test for a shift in the derived dark
energy equation
of state due to a systematic bias. Because of the bright
sky background,
H-band photometry of z~0.4 supernovae is not feasible from
the ground.
Only the superb image quality and dark infrared sky seen
by HST makes
this test possible. This experiment may also lead to a
better, more
reliable way of mapping the expansion history of the
universe with the
Joint Dark Energy
NIC2/WFPC2/NIC1 10887
Stellar Populations in a z=4 Lensed Galaxy with NICMOS
We propose to use NICMOS on HST to undertake deep
high-resolution H-band
imaging of a z=4 galaxy, lensed by a rich foreground
cluster into
highly-magnified arcs 3-5arcsec in length. By combining
this with
existing deep K-band imaging from Keck and high-quality
archival WFPC2
and ACS data, we can spatially resolve stellar populations
along the
arcs. The WFPC2 images clearly reveal several bright
knots, which may
correspond to sites of active star formation. Indeed, our
Keck/LRIS
spectra {Bunker, Moustakas & Davis 2000} are
consistent with OB-star
spectral energy distributions in the rest-ultraviolet.
However, there
are considerable portions of the arcs which appear redder
with no
Ly-alpha emission, consistent with being post-starburst
regions. The
sensitivity and resolution afforded by NIC2 is crucial to
study the
inter-knot flux in H-band {F160W}, a goal unachievable
from the ground.
In conjunction with our deep Keck K' data, NIC2 imaging
will straddle
the 4000Ang+Balmer break and thus allow us to `age-date'
the stellar
populations by the inferred amplitude of the break along
the transverse
extent of the arcs. We can achieve this in 8 orbits, and
address whether
this star-forming galaxy at z=4 has had extended formation
histories -
vital for the interpretation of the Lyman Break Galaxies,
and their
relation to the evolved Extremely Red Objects.
WFPC2 10870
The Ring Plane Crossings of Uranus in 2007
The rings of Uranus turn edge-on to Earth in May and
August 2007. In
between, we will have a rare opportunity to see the unlit
face of the
rings. With the nine optically thick rings essentialy
invisible, we will
observe features and phenomena that are normally lost in
their glare. We
will use this opportunity to search thoroughly for the
embedded
"shepherd" moons long believed to confine the
edges of the rings,
setting a mass limit roughly 10 times smaller than that of
the smallest
shepherd currently known, Cordelia. We will measure the
vertical
thicknesses of the rings and study the faint dust belts
only known to
exist from a single Voyager image. We will also study the
colors of the
newly-discovered faint, outer rings; recent evidence
suggests that one
ring is red and the other blue, implying that each ring is
dominated by
a different set of physical processes. We will employ
near- edge-on
photometry from 2006 and 2007 to derive the particle filling
factor
within the rings, to observe how ring epsilon responds to
the "traffic
jam" as particles pass through its narrowest point,
and to test the
latest models for preserving eccentricities and apse
alignment within
the rings. Moreover, this data set will allow us to
continue monitoring
the motions of the inner moons, which have been found to
show possibly
chaotic orbital variations; by nearly doubling the time
span of the
existing ACS astrometry, the details of the variations
will become much
clearer.
WFPC2 10869
The upper atmosphere and the escape state of the
transiting
very-hot-Jupiter HD189733b
The observation of the HD209458b transits in Lyman-alpha
revealed that
the atmosphere of this planet is escaping. These
observations raised the
question of the evaporation state of hot-Jupiters. Is the
evaporation
specific to HD209458b or general to hot-Jupiters? What is
the
evaporation mechanism, and how does the escape rate depend
on the
planetary system characteristics? The recent discovery of
HD189733b, a
planet transiting a bright and nearby K0 star {V=7.7},
offers the
unprecedented opportunity to answer these questions.
Indeed, among the
stars harboring transiting planets, HD189733 presents the
largest
apparent brightness in Lyman-alpha, providing capabilities
to constrain
the escape rate to high accuracy. With ACS/PR110L we will
observe
stellar emission lines to search for atmospheric
absorptions during the
transits. HD189733b being a very short period planet
orbiting a nearby
late type star with bright chromospheric emission lines,
it is by far
the best target to make significant progress in that
field.
ACS/SBC 10862
Comprehensive Auroral Imaging of Jupiter and Saturn during
the
International Heliophysical Year
A comprehensive set of observations of the auroral
emissions from
Jupiter and Saturn is proposed for the International
Heliophysical Year
in 2007, a unique period of especially concentrated
measurements of
space physics phenomena throughout the solar system. We propose
to
determine the physical relationship of the various auroral
processes at
Jupiter and Saturn with conditions in the solar wind at
each planet.
This can be accomplished with campaigns of observations,
with a sampling
interval not to exceed one day, covering at least one
solar rotation.
The solar wind plasma density approaching Jupiter will be
measured by
the New Horizons spacecraft, and a separate campaign near
opposition in
May 2007 will determine the effect of large-scale
variations in the
interplanetary magnetic field {IMF} on the Jovian aurora
by
extrapolation from near-Earth solar wind measurements. A
similar Saturn
campaign near opposition in Jan. 2007 will combine
extrapolated solar
wind data with measurements from a wide range of locations
within the
Saturn magnetosphere by Cassini. In the course of making
these
observations, it will be possible to fully map the auroral
footprints of
Io and the other satellites to determine both the local
magnetic field
geometry and the controlling factors in the
electromagnetic interaction
of each satellite with the corotating magnetic field and
plasma density.
Also in the course of making these observations, the
auroral emission
properties will be compared with the properties of the near-IR
ionospheric emissions {from ground-based observations} and
non thermal
radio emissions, from ground-based observations for
Jupiter?s decametric
radiation and Cassini plasma wave measurements of the
Saturn Kilometric
Radiation {SKR}.
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.
NIC2 10802
SHOES-Supernovae, HO, for the Equation of State of Dark
energy
The present uncertainty in the value of the Hubble constant
{resulting
in an uncertainty in Omega_M} and the paucity of
redshifts exceeding 1 are now the leading obstacles to
determining the
nature of dark energy. We propose a single, integrated set
of
observations for Cycle 15 that will provide a 40%
improvement in
constraints on dark energy. This program will observe
known Cepheids in
six reliable hosts of
uncertainty in H_0 by a factor of two because of the
smaller dispersion
along the instability strip, the diminished extinction,
and the weaker
metallicity dependence in the infrared. In parallel with
ACS, at the
same time the NICMOS observations are underway, we will
discover and
follow a sample of
measurements, along with prior constraints from WMAP, will
provide a
great improvement in HST's ability to distinguish between
a static,
cosmological constant and dynamical dark energy. The
Hubble Space
Telescope is the only instrument in the world that can
make these IR
measurements of Cepheids beyond the Local Group, and it is
the only
telescope in the world that can be used to find and follow
supernovae at
z > 1. Our program exploits both of these unique
capabilities of HST to
learn more about one of the greatest mysteries in science.
WFPC2 10800
Kuiper Belt Binaries: Probes of Early Solar System
Evolution
Binaries in the Kuiper Belt are a scientific windfall: in
them we have
relatively fragile test particles which can be used as
tracers of the
early dynamical evolution of the outer Solar System. We
propose to
continue a Snapshot program using the ACS/HRC that has a
demonstrated
discovery potential an order of magnitude higher than the
HST
observations that have already discovered the majority of
known
transneptunian binaries. With this continuation we seek to
reach the
original goals of this project: to accumulate a
sufficiently large
sample in each of the distinct populations collected in
the Kuiper Belt
to be able to measure, with statistical significance, how
the fraction
of binaries varies as a function of their particular
dynamical paths
into the Kuiper Belt. Today's Kuiper Belt bears the
imprints of the
final stages of giant-planet building and migration;
binaries may offer
some of the best preserved evidence of that long-ago era.
NIC3 10792
Quasars at Redshift z=6 and Early Star Formation History
We propose to observe four high-redshift quasars {z=6} in
the NIR in
order to estimate relative Fe/Mg abundances and the central
black hole
mass. The results of this study will critically constrain
models of
joint quasar and galaxy formation, early star formation,
and the growth
of supermassive black holes. Different time scales and
yields for
alpha-elements {like O or Mg} and for iron result into an
iron
enrichment delay of ~0.3 to 0.6 Gyr. Hence, despite the
well-known
complexity of the FeII emission line spectrum, the ratio
iron/alpha -
element is a potentially useful cosmological clock. The
central black
hole mass will be estimated based on a recently revised
back hole mass -
luminosity relationship. The time delay of the iron
enrichment and the
time required to form a supermassive black hole {logM>8
Msol, tau
~0.5Gyr} as evidenced by quasar activity will be used to
date the
beginning of the first intense star formation, marking the
formation of
the first massive galaxies that host luminous quasars, and
to constrain
the epoch when supermassive black holes start to grow by
accretion.
WFPC2 10561
A deep UV imaging survey of the Globular Cluster M 30
We propose to carry out a deep FUV and NUV survey of M30
{NGC 7099} in
order to find and study the hot and/or dynamically-formed
stellar
populations in the globular cluster. In particular, we
will {i} search
for the UV counterpart to a MSP binary, {ii} find and
study the full
population of cataclysmic variables in this cluster, {iii}
study the UV
properties of the cluster's extensive blue straggler
population, {iv}
detect the first set of white dwarfs in this cluster. Our
survey will be
sensitive to variability on time-scales from minutes to
weeks, allowing
us to search for variable stars in all of the FUV
populations.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are
preliminary reports
of potential non-nominal performance that will be
investigated.)
HSTARS:
10856 - GSAcq (2,0,2) failed due to Search Radius Limit
Exceeded on FGS 2
At
2007.160/14:35:16 GSAcq (2,0,2) scheduled at 160/14:31:09-14:36:47
had
failed due to Search Radius Limit Exceeded on FGS 2.
OBAD #1 V1 -238.71, V2 4023.22, V3 -1185.43, RSS 4201.01
OBAD #2 V1 -76.88, V2 31.13, V3 -64-97, RSS 105.36
OBAD MAP not available due to ongoing astrometry
OBAD MAP V1 69.99, V2 -35.93, V3 61.70, RSS 99.98
10857 - GSAcq (1,0,1) failed due to Search Radius Limit
Exceeded on FGS 1
GSAcq (1,0,1) scheduled from 161/13:12:29-13:18:13 failed due to search
radius limit exceeded on FGS 1. Historical extracts showed at 13:16:55
the FGS 1 PMT count reached a high value of 598.00018.
OBAD #1: V1 826.02, V2 3677.62, V3 194.74,
RSS 3774.27
OBAD #2: V1 2.77, V2 5.49, V3 4.65, RSS 7.71
OBAD
MAP: V1 -15.61, V2 -144.05, V3 -15.07,
RSS
145.67
10858 - REAcq (1,2,2) failed to RGA Hold (Gyro Control)
REAcq (1,2,2) scheduled from 19:44:23-19:52:00 failed to RGA Hold (Gyro
Control) due to QF1STOPF & QSTOP flags on FGS 1.
OBAD #1: V1 -23.85, V2 172.36, V3 -14.01, RSS 174.57
OBAD #2: V1 0.97, V2 -4.67, V3 -7.03, RSS 8.50
At
22:19:39 ReAcq (1,2,2) scheduled from 21:20:19-21:27:56 failed to RGA
Hold (Gyro Control) due to QSTOP flag on FGS 1.
OBAD #2 V1 3.04, V2 -7.03, V3 2.12, RSS 7.95
At
22:59:39 REacq(1,2,2) scheduled at 22:56:15 failed to RGA Control due
to
QSTOP flag on FGS 1. OBAD1 showed errors of V1=-28.18, V2=-616.76,
V3=-27.44 and RSS=618.01. OBAD2 showed errors of V1=-0.64, V2=-3.72,
V3=-8.15, and RSS = 8.98
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS GSacq
19
17
FGS REacq
21
18
OBAD with Maneuver
80
80
SIGNIFICANT EVENTS: (None)