Notice:
Due to the conversion of some ACS WFC or HRC observations into
WFPC2,
or NICMOS observations after the loss of ACS CCD science
capability
in January, there may be an occasional discrepancy between a
proposal's
listed (and correct) instrument usage and the abstract that
follows
it.
HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4453
PERIOD
COVERED: UT September 21,22,23, 2007 (DOY 264,265,266)
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 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.
NIC3
11335
NICMOS
Defocus parameter test
This
proposal tests the new NICMOS non-nominal focus positions, which
are
implemented in the front-end systems and are specified in the Phase
II
using the CAMERA-FOCUS=DEFOCUS Optional Parameter. The targets from
Proposals
9832 and 11063 are used in this Proposal. The GO Proposal 9832
is
an example of how GOs may use the new non-nominal focus
implementation
for detector 3. Proposal 11063 is the NICMOS focus
monitor,
which will be used to verify the non-nominal focus for all 3
detectors.
WFPC2
11224
Unraveling
Wind
accretion is one of the most common yet poorly understood phenomena
in
astrophysics. A key step toward advancing our understanding of
physical
processes and accretion geometries in wind accreting systems is
direct
imaging of the individual components and mass flows. The nearby
symbiotic
binary
compact
companion, is a unique target since it can be easily spatially
resolved
with the HST, and thus serves as a perfect test laboratory for
accretion
studies in wind interacting systems. We propose to carry out
WFPC2
observations of
of
an unprecedented outburst from the cool giant, and the discovery of
an
accretion stream showing for the first time evidence for a direct
mass
transfer between the components in a wind accreting system.
High-angular-
resolution multiwavelength imaging at UV /optical
wavelengths
will allow us to determine the properties of the ejected
material
as it flows throughout the binary and interacts with the Mira A
circumstellar
material and wind; the physical characteristics of mass
transfer
in this system and especially the role of the accretion stream
between
Mira A and Mira B; and the response of the system to the
increased
accretion rate onto Mira B following the outburst. These
results
will provide crucial inputs and quantitative constraints to
models
of wind interacting systems and will also anchor our
understanding
of accretion processes in a wide range of interacting
binaries
that cannot be currently resolved, including in other
symbiotics
and more exotic systems such as accreting black holes and
neutron
stars in high-mass X-ray binaries.
WFPC2
11178
Probing
Solar System History with Orbits, Masses, and Colors of
Transneptunian
Binaries
The
recent discovery of numerous transneptunian binaries {TNBs} opens a
window
into dynamical conditions in the protoplanetary disk where they
formed
as well as the history of subsequent events which sculpted the
outer
Solar System and emplaced them onto their present day heliocentric
orbits.
To date, at least 47 TNBs have been discovered, but only about a
dozen
have had their mutual orbits and separate colors determined,
frustrating
their use to investigate numerous important scientific
questions.
The current shortage of data especially cripples scientific
investigations
requiring statistical comparisons among the ensemble
characteristics.
We propose to obtain sufficient astrometry and
photometry
of 23 TNBs to compute their mutual orbits and system masses
and
to determine separate primary and secondary colors, roughly tripling
the
sample for which this information is known, as well as extending it
to
include systems of two near-equal size bodies. To make the most
efficient
possible use of HST, we will use a
optimally
schedule our observations.
WFPC2
11134
WFPC2
Tidal Tail Survey: Probing Star Cluster Formation on the Edge
The
spectacular HST images of the interiors of merging galaxies such as
the
Antennae and NGC 7252 have revealed rich and diverse populations of
star
clusters created over the course of the interaction. Intriguingly,
our
WFPC2 study of tidal tails in these and other interacting pairs has
shown
that star cluster birth in the tails does not follow a similarly
straightforward
evolution. In fact, cluster formation in these
relatively
sparse environments is not guaranteed -- only one of six
tails
in our initial study showed evidence for a significant population
of
young star clusters. The tail environment thus offers the opportunity
to
probe star cluster formation on the edge of the physical parameter
space
{e.g., of stellar and gas mass, density, and pressure} that
permits
it to occur. We propose to signficantly extend our pilot sample
of
optically bright, gas-rich tidal tails by a factor of 4 in number to
include
a more diverse population of tails, encompassing major and minor
mergers,
gas-rich and gas-poor tails, as well as early, late, and merged
interaction
stages. With 21 orbits of HST WFPC2 imaging in the F606W and
F814W
filters, we can identify, roughly age-date, and measure sizes of
star
clusters to determine what physical parameters affect star cluster
formation.
WFPC2 imaging has been used effectively in our initial study
of
four mergers, and it will be possible in this program to reach
similar
limits of Mv=-8.5 for each of 16 more tails. With the much
larger
sample we expect to isolate which factors, such as merger stage,
HI
content, and merger mass ratio, drive the formation of star clusters.
WFPC2
11122
Expanding
PNe: Distances and Hydro Models
We
propose to obtain repeat narrowband images of a sample of eighteen
planetary
nebulae {PNe} which have HST/WFPC2 archival data spanning time
baselines
of a decade. All of these targets have previous high
signal-to-noise
WFPC2/PC observations and are sufficiently nearby to
have
readily detectable expansion signatures after a few years. Our main
scientific
objectives are {a} to determine precise distances to these
PNe
based on their angular expansions, {b} to test detailed and highly
successful
hydrodynamic models that predict nebular morphologies and
expansions
for subsamples of round/elliptical and axisymmetric PNe, and
{c}
to monitor the proper motions of nebular microstructures in an
effort
to learn more about their physical nature and formation
mechanisms.
The proposed observations will result in high-precision
distances
to a healthy subsample of PNe, and from this their expansion
ages,
luminosities, CSPN properties, and masses of their ionized cores.
With
good distances and our hydro models, we will be able to determine
fundamental
parameters {such as nebular and central star masses,
luminosity,
age}. The same images allow us to monitor the changing
overall
ionization state and to search for the surprisingly
non-homologous
growth patterns to bright elliptical PNe of the same sort
seen
by Balick & Hajian {2004} in NGC 6543. Non-uniform growth is a sure
sign
of active pressure imbalances within the nebula that require
careful
hydro models to understand.
NIC3
11107
Imaging
of Local Lyman Break Galaxy Analogs: New Clues to Galaxy
Formation
in the Early Universe
We
have used the ultraviolet all-sky imaging survey currently being
conducted
by the Galaxy Evolution Explorer {GALEX} to identify for the
first
time a rare population of low- redshift starbursts with properties
remarkably
similar to high-redshift Lyman Break Galaxies {LBGs}. These
"compact
UV luminous galaxies" {UVLGs} resemble LBGs in terms of size,
SFR,
surface brightness, mass, metallicity, kinematics, dust, and color.
The
UVLG sample offers the unique opportunity of investigating some very
important
properties of LBGs that have remained virtually inaccessible
at
high redshift: their morphology and the mechanism that drives their
star
formation. Therefore, in Cycle 15 we have imaged 7 UVLGs using ACS
in
order to 1} characterize their morphology and look for signs of
interactions
and mergers, and 2} probe their star formation histories
over
a variety of timescales. The images show a striking trend of
small-scale
mergers turning large amounts of gas into vigorous
starbursts
{a process referred to as dissipational or "wet" merging}.
Here,
we propose to complete our sample of 31 LBG analogs using the
ACS/SBC
F150LP {FUV} and WFPC2 F606W {R} filters in order to create a
statistical
sample to study the mechanism that triggers star formation
in
UVLGs and its implications for the nature of LBGs. Specifically, we
will
1} study the trend between galaxy merging and SFR in UVLGs, 2}
artificially
redshift the FUV images to z=1-4 and compare morphologies
with
those in similarly sized samples of LBGs at the same rest-frame
wavelenghts
in e.g. GOODS, UDF, and COSMOS, 3} determine the presence
and
morphology of significant stellar mass in "pre-burst" stars, and 4}
study
their immediate environment. Together with our Spitzer
{IRAC+MIPS},
GALEX, SDSS and radio data, the HST observations will form
a
unique union of data that may for the first time shed light on how the
earliest
major episodes of star formation in high redshift galaxies came
about.
This proposal was adapted from an ACS HRC+WFC proposal to meet
the
new Cycle 16 observing constraints, and can be carried out using the
ACS/SBC
and WFPC2 without compromising our original science goals.
NIC3
11082
NICMOS
Imaging of GOODS: Probing the Evolution of the Earliest Massive
Galaxies,
Galaxies Beyond Reionization, and the High Redshift Obscured
Universe
(uses
ACS/SBC and WFPC2)
Deep
near-infrared imaging provides the only avenue towards
understanding
a host of astrophysical problems, including: finding
galaxies
and AGN at z > 7, the evolution of the most massive galaxies,
the
triggering of star formation in dusty galaxies, and revealing
properties
of obscured AGN. As such, we propose to observe 60 selected
areas
of the GOODS North and South fields with NICMOS Camera 3 in the
F160W
band pointed at known massive M > 10^11 M_0 galaxies at z > 2
discovered
through deep Spitzer imaging. The depth we will reach {26.5
AB
at 5 sigma} in H_160 allows us to study the internal properties of
these
galaxies, including their sizes and morphologies, and to
understand
how scaling relations such as the Kormendy relationship
evolved.
Although NIC3 is out of focus and undersampled, it is currently
our
best opportunity to study these galaxies, while also sampling enough
area
to perform a general NIR survey 1/3 the size of an ACS GOODS field.
These
data will be a significant resource, invaluable for many other
science
goals, including discovering high redshift galaxies at z > 7,
the
evolution of galaxies onto the Hubble sequence, as well as examining
obscured
AGN and dusty star formation at z > 1.5. The GOODS fields are
the
natural location for HST to perform a deep NICMOS imaging program,
as
extensive data from space and ground based observatories such as
Chandra,
GALEX, Spitzer, NOAO, Keck, Subaru, VLT, JCMT, and the VLA are
currently
available for these regions. Deep high-resolution
near-infrared
observations are the one missing ingredient to this
survey,
filling in an important gap to create the deepest, largest, and
most
uniform data set for studying the faint and distant universe. The
importance
of these images will increase with time as new facilities
come
on line, most notably WFC3 and ALMA, and for the planning of future
JWST
observations.
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 individual
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.
NIC3
11064
CYCLE
15 NICMOS SPECTROPHOTOMETRY CALIBRATION PROGRAM
Now
that the spectrophotometric capabilities of the NICMOS grism have
been
established, cycle 15 observations are needed to refine the
sensitivity
estimates, to check for sensitivity loss with time, to
improve
the accuracy of the linearity correction, to improve the
secondary
flux standards by re-observation, and to expand the G206 data
set
now that the sky subtraction technique has been shown to produce
useful
fluxes for some of the fainter secondary standards. These faint
secondary
IR standards will be a significant step towards establishing
flux
standards for JWST, as well as for SNAP, Spitzer, and
observe
the 3 primary WDs GD71, G191B2b, & GD153 twice each, once at the
beginning
and once near the end of the 18 month cycle. To date, we have
only
2 observation of each star, while the corresponding STIS data set
for
these primary standards ranges from 6 to 23 obs. No observations
exist
for GD71 or GD153 with G206, so that the current G206 sensitivity
is
defined solely by G191B2B. Purposes: Refine sensitivities, measure
sens
losses. Orbits: 2 for each of 6 visits = 12 2. Re-observe WD1057 &
WD1657
plus another P041C lamp-on visit to improve the scatter in the
non-lin
measurements per Fig. 8 of NIC ISR 2006-02. The WD stars require
2
orbits each, while the lamp-on test is done in one. The very faintest
and
most crucial standard WD1657 has 2 good visits already, so to
substantially
improve the S/N, two visits of two orbits are needed.
Include
G206 for P041C in the lamp-off baseline part of that orbit.
Orbits:
WD1057-2, WD1657-4, P041C-1 --> 7 3. Re-observe 9 secondary
standards
to improve S/N of the faint ones and to include G206 for all
9.
BD+17 {3 obs} is not repeated in this cycle. Four are bright enough
to
do in one orbit: VB8, 2M0036+18, P330E, and P177D. Orbits:2*5+4=14
Grand
Total orbits over 18 month cycle 15 is 12+6+14=32 {Roelof will
submit
the P041C lamp-on visit in a separate program.}
NIC2
11016
NICMOS
Flats: narrow and broad filters for NIC1 {+ NIC2, NIC3 in
parallel}
This
proposal obtains sequences of NICMOS narrow band filter flat fields
for
camera 1. In cameras 2 and 3, parallel observations will allow us to
obtain
high S/N flats for all spectral elements.
WFPC2
10919
Eclipsing
Binaries in the Local Group: II - Calibration of the Zeropoint
of
the Cosmic Distance Scale and Fundamental Properties of Stars in M33
(uses
ACS/SBC and WFPC2)
The
Great Spiral Galaxy in Triangulum {M33} is potentially a crucial
calibrator
for the Cosmic Distance Scale, and thus for determining the
age
and evolution of the Universe. M33 is viewed face-on, has a simple
geometry,
large and diverse stellar populations, and morphologies
similar
to our Galaxy and other more distant galaxies used for distance
determinations.
Yet currently the M33 distance {d ~ 830 +/- 110 kpc}
still
has measurement dispersions of 10-15%. We have demonstrated, in
our
work on the LMC and M31 distances, that double-line eclipsing
binaries
can serve as excellent "standard candles." Distances derived
from
eclipsing binaries are basically geometric and essentially free
from
many assumptions and uncertainties that plague other less direct
methods,
such as metallicity differences and calibration zeropoints. The
absolute
radii of the component stars of eclipsing binaries can be
determined
to better than a few percent from the time- tested analyses
of
their light and radial velocity curves. With accurate determinations
of
radii, temperatures, and ISM absorption it is possible to determine
reliable
distances. We are extending our program of using eclipsing
binaries
as standard candles to determine an accurate distance to M33.
As
a first step, we are proposing to carry out HST/ACS spectrophotometry
of
a well suited ~19th mag ~O7 + ~O7 eclipsing binary system in M33 that
has
been previously observed from the ground. HST/ACS prism/grism
low-resolution
spectrophotometry {118-850 nm} is the only missing key
element
of this program and is used to determine more reliable values
for
T_eff, [Fe/H], and ISM extinction. These quantities, when combined
with
the results from existing light and radial velocity curves for the
target,
yield the stellar masses, radii, luminosities and, importantly,
the
distance. The proposed HST/ACS program can be carried out
effectively
with only 1 HST orbit. Based on our previous experience, we
expect
to reduce the uncertainty of the M33 distance to better than
5-7%,
thereby leading to a firmer calibration of the Cosmic Distance
Scale
and the zeropoint of the Hubble Constant {Ho}.
WFPC2
10787
Modes
of Star Formation and Nuclear Activity in an Early Universe
Laboratory
Nearby
compact galaxy groups are uniquely suited to exploring the
mechanisms
of star formation amid repeated and ongoing gravitational
encounters,
conditions similar to those of the high redshift universe.
These
dense groups host a variety of modes of star formation, and they
enable
fresh insights into the role of gas in galaxy evolution. With
Spitzer
mid-IR observations in hand, we have begun to obtain high
quality,
multi-wavelength data for a well- defined sample of 12 nearby
{<4500km/s}
compact groups covering the full range of evolutionary
stages.
Here we propose to obtain sensitive BVI images with the ACS/WFC,
deep
enough to reach the turnover of the globular cluster luminosity
function,
and WFPC2 U-band and ACS H-alpha images of Spitzer-identified
regions
hosting the most recent star formation. In total, we expect to
detect
over 1000 young star clusters forming inside and outside
galaxies,
more than 4000 old globular clusters in >40 giant galaxies
{including
16 early-type galaxies}, over 20 tidal features,
approximately
15 AGNs, and intragroup gas in most of the 12 groups.
Combining
the proposed ACS images with Chandra observations, UV GALEX
observations,
ground-based H-alpha imaging, and HI data, we will conduct
a
detailed study of stellar nurseries, dust, gas kinematics, and AGN.
WFPC2
10766
A
Deep X-ray Survey of the Small Magellanic Cloud
We
request deep observations of 2 representative fields in the Small
Magellanic
Cloud with Chandra and HST,with the primary goal of measuring
the
luminosity function and space density of X-ray binaries and other
sources
down to an unprecedented faint luminosity limit of 2x10E32
erg/s.
This will be the faintest XLF ever obtained for any galaxy,
including
our own. HST photometry to 24th magnitude in V and I filters
will
identify the sources and provide Fx/Fopt, which will be vital in
quantifying
the LMXB population and in measuring the properties of the
first
coronally active stars ever detected in an external galaxy.
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
18
18
FGS
REacq
20
20
OBAD
with Maneuver
72
72
SIGNIFICANT
EVENTS: (None)