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 # 4401
PERIOD COVERED: UT July 10, 2007 (DOY 191)
OBSERVATIONS SCHEDULED
FGS 11214
HST/FGS Astrometric Search for Young Planets Around Beta
Pic and AU Mic
Beta Pic and AU Mic are two nearby Vega-type debris disk
stars. Both of
these disk systems have been spatially resolved in
exquisite detail,
predominantly via the ACS coronagraph and WFPC-2 cameras
onboard HST.
These images exhibit a wealth of morphological features
which provide
compelling indirect evidence that these systems likely
harbor
short-period planetary body{ies}. We propose to use the
superlative
astrometric capabilities of HST/FGS to directly detect these
planets,
hence provide the first direct planet detection in a
Vega-type system
whose disk has been imaged at high spatial resolution.
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.
NIC1/NIC3 10924
Constraints on the Assembly and Dynamical Masses of z~2
Galaxies
We propose deep NICMOS/NIC2 F160W imaging of seven star-forming
galaxies
at z~2. These galaxies comprise an entirely unique sample,
with not only
redshifts measured from optical and near-IR spectra, but
also
SINFONI/VLT near-IR integral field spectroscopic
measurements providing
kinematic maps of H-alpha emission out to radii of >=10
kpc. We aim to
determine the dynamical masses and evolutionary states of
these systems,
as part of the larger goal of understanding how mass is
assembled in
distant galaxies. In order to interpret our novel H-alpha
integral field
maps in terms of mass, we require detailed knowledge of
the structural
parameters of our target objects at rest-frame optical
wavelengths and
on ~1 kpc scales. We want to establish if the mass is
distributed in a
disk, bulge, or merging sub-units, and if we can detect
tidal features
associated with a merger. F160W imaging with NICMOS/NIC2
provides the
perfect combination of sensitivity and resolution to
address these
questions, and arrive at the fundamental quantity: the
dynamical mass.
NICMOS 8791
NICMOS Post-SAA calibration - CR Persistence Part 2
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 10818
Very Young Globular Clusters in M31 ?
We propose to use HST's unique high spatial resolution imaging
capabilities to conclusively confirm or refute the
presence of alleged
very young globular clusters in M31. Such young globular
clusters with
ages < 3 Gyr are not present in our galaxy, and, if
real, would lead to
a striking difference in the age distribution of the GCs
between M31 and
the
in M31 is confirmed through our proposed ACS imaging {now
WFPC2 imaging}
with HST, this would suggest major differences in the
history of
assembly of the two galaxies, with probable substantial
late accretion
into M31 which did not occur in our own galaxy.
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.
WFPC2 11218
Snapshot Survey for Planetary Nebulae in Globular Clusters
of the Local
Group
Planetary nebulae {PNe} in globular clusters {GCs} raise a
number of
interesting issues related to stellar and galactic evolution.
The number
of PNe known in Milky Way GCs, 4, is surprisingly low if
one assumes
that all stars pass through a PN stage. However, it is
likely that the
remnants of stars now evolving in Galactic GCs leave the
AGB so slowly
that any ejected nebula dissipates long before the star
becomes hot
enough to ionize it. Thus there should not be ANY PNe in
Milky Way
GCs--but there are four! It has been suggested that these
PNe are the
result of mergers of binary stars within GCs, i.e., that
they are
descendants of blue stragglers. The frequency of
occurrence of PNe in
external galaxies poses more questions, because it shows a
range of
almost an order of magnitude. I propose a Snapshot survey
aimed at
discovering PNe in the GC systems of Local Group galaxies
more distant
than the Magellanic Clouds. These clusters, some of which
may be much
younger than their counterparts in the Milky Way, might
contain many
more PNe than those of our own galaxy. I will use the
standard technique
of emission-line and continuum imaging, which easily
discloses PNe.
WFPC2 11229
SEEDS: The Search for Evolution of Emission from Dust in
Supernovae with
HST and Spitzer
The role that massive stars play in the dust content of
the Universe is
extremely uncertain. It has long been hypothesized that
dust can
condense within the ejecta of supernovae {SNe}, however
there is a
frustrating discrepancy between the amounts of dust found
in the early
Universe, or predicted by nucleation theory, and inferred
from SN
observations. Our SEEDS collaboration has been carefully
revisiting the
observational case for dust formation by core- collapse
SNe, in order to
quantify their role as dust contributors in the early
Universe. As dust
condenses in expanding SN ejecta, it will increase in
optical depth,
producing three simultaneously observable phenomena: {1}
increasing
optical extinction; {2} infrared {IR} excesses; and {3}
asymmetric
blue-shifted emission lines. Our SEEDS collaboration
recently reported
all three phenomena occurring in SN2003gd, demonstrating
the success of
our observing strategy, and permitting us to derive a dust
mass of up to
0.02 solar masses created in the SN. To advance our
understanding of the
origin and evolution of the interstellar dust in galaxies,
we propose to
use HST's WFPC2 and NICMOS instruments plus Spitzer's
photometric
instruments to monitor ten recent core-collapse SNe for
dust formation
and, as a bonus, detect light echoes that can affect the
dust mass
estimates. These space-borne observations will be
supplemented by
ground-based spectroscopic monitoring of their optical
emission line
profiles. These observations would continue our 2-year HST
and Spitzer
monitoring of this phenomena in order to address two key
questions: Do
all SNe produce dust? and How much dust do they produce?
As all the SN
are witin 15 Mpc, each SN stands an excellent chance of
detection with
HST and Spitzer and of resolving potential light echoes.
WFPC2 11289
SL2S: The Strong Lensing Legacy Survey
Recent systematic surveys of strong galaxy-galaxy lenses
{CLASS, SLACS,
GOODS, etc.} are producing spectacular results for galaxy
masses roughly
below a transition mass M~10^13 Mo. The observed lens
properties and
their evolution up to z~0.2, consistent with numerical
simulations, can
be described by isothermal elliptical potentials. In
contrast, modeling
of giant arcs in X-ray luminous clusters {halo masses M
>~10^13 Mo}
favors NFW mass profiles, suggesting that dark matter
halos are not
significantly affected by baryon cooling. Until recently,
lensing
surveys were neither deep nor extended enough to probe the
intermediate
mass density regime, which is fundamental for
understanding the assembly
of structures. The CFHT Legacy Survey now covers 125
square degrees, and
thus offers a large reservoir of strong lenses probing a
large range of
mass densities up to z~1. We have extracted a list of 150
strong lenses
using the most recent CFHTLS data release via automated
procedures.
Following our first SNAPSHOT proposal in cycle 15, we
propose to
continue the Hubble follow-up targeting a larger list of
130 lensing
candidates. These are intermediate mass range candidates
{between
galaxies and clusters} that are selected in the redshift
range of 0.2-1
with no a priori X-ray selection. The HST resolution is
necessary for
confirming the lensing candidates, accurate modeling of
the lenses, and
probing the total mass concentration in galaxy groups up
to z~1 with the
largest unbiased sample available to date.
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)
SCHEDULED
SUCCESSFUL
FGS GSacq
8
8
FGS
REacq
7
7
OBAD with Maneuver
30
30
COMPLETED OPS NOTES: (None)
SIGNIFICANT EVENTS: (None)