HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #4951
PERIOD
COVERED: 5am October 14 - 5am October 15, 2009 (DOY 287/09:00z-288/09:00z)
OBSERVATIONS
SCHEDULED
ACS/WFC3
11879
CCD
Daily Monitor (Part 1)
This
program comprises basic tests for measuring the read noise and dark
current
of the ACS WFC and for tracking the growth of hot pixels. The
recorded
frames are used to create bias and dark reference images for
science
data reduction and calibration. This program will be executed
four
days per week (Mon, Wed, Fri, Sun) for the duration of Cycle 17. To
facilitate
scheduling, this program is split into three proposals. This
proposal
covers 352 orbits (22 weeks) from 31 August 2009 to 31 January
2010.
NIC1/NIC2/NIC3
11947
Extended
Dark Monitoring
This
program takes a series of darks to obtain darks (including
amplifier
glow, dark current, and shading profiles) for all three
cameras
in the read-out sequences used in Cycle 17. A set of 12 orbits
will
be observed every two months for a total of 72 orbits for a 12
month
Cycle 17. This is a continuation of Cycle 16 program 11330 scaled
down
by ~80%.
The
first orbit (Visit A0) should be scheduled in the NICMOS SMOV after
the
DC Transfer Test (11406) and at least 36h before the Filter Wheel
Test
(11407). Data download using fast track.
The
following 28 orbits (visit A1-N2) should be scheduled AFTER the SMOV
Proposal
11407 (Filter Wheel Test). This is done in order to monitor the
dark
current following an adjustment of the NCS set-point. These visits
should
be executed until the final temperature is reached during SMOV.
NIC1/NIC2/NIC3
8795
NICMOS
Post-SAA Calibration - CR Persistence Part 6
This
is 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 'Use After' 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 darks. 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.
NIC2/WFC3/IR
11548
Infrared
Imaging of Protostars in the Orion A Cloud: The Role of
Environment
in Star Formation
We
propose NICMOS and WFC3/IR observations of a sample of 252 protostars
identified
in the Orion A cloud with the Spitzer Space Telescope. These
observations
will image the scattered light escaping the protostellar
envelopes,
providing information on the shapes of outflow cavities, the
inclinations
of the protostars, and the overall morphologies of the
envelopes.
In addition, we ask for Spitzer time to obtain 55-95 micron
spectra
of 75 of the protostars. Combining these new data with existing
3.6
to 70 micron photometry and forthcoming 5-40 micron spectra measured
with
the Spitzer Space Telescope, we will determine the physical
properties
of the protostars such as envelope density, luminosity,
infall
rate, and outflow cavity opening angle. By examining how these
properties
vary with stellar density (i.e. clusters vs. groups vs.
isolation)
and the properties of the surrounding molecular cloud; we can
directly
measure how the surrounding environment influences protostellar
evolution,
and consequently, the formation of stars and planetary
systems.
Ultimately, this data will guide the development of a theory of
protostellar
evolution.
STIS/CCD
11844
CCD
Dark Monitor Part 1
The
purpose of this proposal is to monitor the darks for the STIS CCD.
STIS/CCD
11846
CCD
Bias Monitor-Part 1
The
purpose of this proposal is to monitor the bias in the 1x1, 1x2,
2x1,
and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up
high-S/N
superbiases and track the evolution of hot columns.
WFC3/IR
11719
A
Calibration Database for Stellar Models of Asymptotic Giant Branch
Stars
Studies
of galaxy formation and evolution rely increasingly on the
interpretation
and modeling of near-infrared observations. At these
wavelengths,
the brightest stars are intermediate mass asymptotic giant
branch
(AGB) stars. These stars can contribute nearly 50% of the
integrated
luminosity at near infrared and even optical wavelengths,
particularly
for the younger stellar populations characteristic of
high-redshift
galaxies (z>1). AGB stars are also significant sources of
dust
and heavy elements. Accurate modeling of AGB stars is therefore of
the
utmost importance.
The
primary limitation facing current models is the lack of useful
calibration
data. Current models are tuned to match the properties of
the
AGB population in the Magellanic Clouds, and thus have only been
calibrated
in a very narrow range of sub-solar metallicities.
Preliminary
observations already suggest that the models are
overestimating
AGB lifetimes by factors of 2-3 at lower metallicities.
At
higher (solar) metallicities, there are no appropriate observations
for
calibrating the models.
We
propose a WFC3/IR SNAP survey of nearby galaxies to create a large
database
of AGB populations spanning the full range of metallicities and
star
formation histories. Because of their intrinsically red colors and
dusty
circumstellar envelopes, tracking the numbers and bolometric
fluxes
of AGB stars requires the NIR observations we propose here. The
resulting
observations of nearby galaxies with deep ACS imaging offer
the
opportunity to obtain large (100-1000's) complete samples of AGB
stars
at a single distance, in systems with well-constrained star
formation
histories and metallicities.
WFC3/IR/UV
11835
The
Multi-faceted X-ray Activity of Low-redshift Active Galaxies
We
propose ACIS-I observations of Chandra-unobserved low-redshift 3CRR
active
galaxies and their environments. The data will complete Chandra
observations
of 3CRR at z < 0.1, making the sample useful for
statistical
studies. Only Chandra can resolve the multiple components of
these
sources, as is needed for an improved understanding of source
physics
and gas heating. The imaging and spectroscopy of cores, jets,
hot
spots, and atmospheres will be of permanent legacy value. We will
use
the data to investigate particle acceleration, interactions between
radio
plasma and the ISM and IGM, the emission mechanisms of hot spots,
and
AGN fueling. Comparison with our complete Spitzer coverage and HST
images
will aid interpretation. The dataset will be made public
immediately.
WFC3/UVI
11580
Watching
Young Planetary Nebulae Grow: The Movie
The
development of magneto-hydro gas dynamical models is the key to the
understanding
of both the physics (processes) and astronomy (initial
conditions)
of astrophysical nebulae of all sorts. The models are
reaching
their highest degree of accuracy when applied to and compared
against
pre Planetary Nebulae (pPNe) thanks to the simplicity, relative
lack
of extinction, and the detail of the imaging and kinematic data
that
have bcome available for these objects. The primary barrier to
progress
is inadequate kinematic data of pPNe against which the
predictions
models can be tested. Unlike PNe, pPNe do not emit emission
lines
for detailed Doppler measurements. Therefore it is essential to
find
another way to monitor the morphological evolution.
Only
HST can uncover the dynamics of the growth patterns by subtracting
multi-epoch
images spanning a decade or more. We have selected four pPNe
with
highly collimated outflows in different evolutionary stages for
which
high-quality first epoch images were obtained from 1996 to 2002.
All
of them display regularly shaped thin rims, sharp edges, and
symmetric
pairs of knots or bowshocks that are ideal for our purposes.
We
will closely mimic many of the earlier exposures using ACS and to
monitor
changes in structures. The morphology and its evolution will be
compared
to 3-D MHD models with adaptive grids in order to build a far
clearer
picture of the nuclear geometry which shaped the outflows and
constrained
their propagation to the present. We shall also obtain R, J,
and
H images for use with a 3-D dust radiative transfer code LELUYA to
model
the dust distribution deep into the nuclear zones.
WFC3/UVI
11615
Hunting
for Optical Companions to Binary MSPs in Globular Clusters
Here
we present a proposal which exploits the re-newed potential of HST
after
the Service Mission 4 for probing the population of binary
Millisecond
Pulsars (MSPs) in Globular Clusters. In particular we intend
to:
(1) extend the search for optical counterparts in Terzan 5, by
pushing
the performance of the WFC3 IR channel to sample the entire MS
extension
down to M=0.1 Mo; (2) perform a deep multi-band search of MSP
companions
with the WFC3, in 3 clusters (namely NGC6440, M28 and M5),
where
recent radio observations have found particularly interesting
objects;
(3) derive an accurate radial velocity (with STIS) of the
puzzling
optical companion COM6266B recently discovered by our group, to
firmly
assess its cluster membership. This program is the result of a
large
collaboration among the three major groups (lead by Freire, Ransom
and
Possenti) which are performing extensive MSP search in GCs in the
radio
bands, and our group which has a large experience in performing
accurate
stellar photometry in crowded environments. This collaboration
has
produced a number of outstanding discoveries. In fact, three of the
6
optical counterparts to binary MSP companions known to date in GCs
have
been discovered by our group. The observations here proposed would
easily
double/triple the existing sample of known MSP companions,
allowing
the first meaningful approach to the study of the formation,
evolution
and recycling process of pulsar in GCs. Moreover, since most
of
binary MSPs in GCs are thought to form via stellar interactions in
the
high density core regions, the determination of the nature of the
companion
and the incidence of this collisionally-induced population has
a
significant impact on our knowledge of the cluster dynamics. Even more
interesting,
the study of the optical companions to NSs in GCs allows
one
to derive tighter constraints (than those obtainable for NS binaries
in
the Galactic field) on the system properties. This has, in turn, an
intrisic
importance for fundamental physics, since it offers the
opportunity
of measuring the mass of the NS and hence constraining the
equation
of state of matter at the nuclear equilibrium density.
WFC3/UVIS
11905
WFC3
UVIS CCD Daily Monitor
The
behavior of the WFC3 UVIS CCD will be monitored daily with a set of
full-frame,
four-amp bias and dark frames. A smaller set of 2Kx4K
subarray
biases are acquired at less frequent intervals throughout the
cycle
to support subarray science observations. The internals from this
proposal,
along with those from the anneal procedure (Proposal 11909),
will
be used to generate the necessary superbias and superdark reference
files
for the calibration pipeline (CDBS).
WFC3/UVIS
11908
Cycle
17: UVIS Bowtie Monitor
Ground
testing revealed an intermittent hysteresis type effect in the
UVIS
detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially
found via an unexpected bowtie-shaped feature in flatfield
ratios,
subsequent lab tests on similar e2v devices have since shown
that
it is also present as simply an overall offset across the entire
CCD,
i.e., a QE offset without any discernable pattern. These lab tests
have
further revealed that overexposing the detector to count levels
several
times full well fills the traps and effectively neutralizes the
bowtie.
Each visit in this proposal acquires a set of three 3x3 binned
internal
flatfields: the first unsaturated image will be used to detect
any
bowtie, the second, highly exposed image will neutralize the bowtie
if
it is present, and the final image will allow for verification that
the
bowtie is gone.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
(None)
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSAcq
07
07
FGS
REAcq
10
10
OBAD
with Maneuver
05
05
SIGNIFICANT
EVENTS: (None)