HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4229
PERIOD COVERED: UT October 27,28,29, 2006 (DOY 300.301,302)
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.
NIC1/NIC2/NIC3 8793
NICMOS Post-SAA calibration - CR Persistence Part 4
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.
ACS/WFC 11015
The Proper Motion of Supernova Remnant E0509-67.5
We propose to measure independently the proper motion expansions of
the
ejecta and forward shock in E0509-67.5. The metal-enriched
reverse-shock-heated ejecta emits only in X-rays, while the forward
shock is traced to high precision by H alpha emission. The proposed
measurements require the unique high resolution imaging capabilities
of
Chandra and Hubble. The optical {forward shock} and X-ray {ejecta}
results will yield important constraints on the remnant's
evolutionary
state; we will search in particular for evidence of cosmic-ray
modified
dynamics. An important component of this project is an integrated
theoretical investigation using realistic models of SN Ia explosions
evolved to the remnant stage.
ACS/WFC 10911
Calibration of ACS F814W Surface Brightness Fluctuations
The surface brightness fluctuations {SBF} method has emerged as the
primary distance indicator for mapping local large-scale structures
{Virgo, Fornax}, as well as the velocity field out to nearly 15,000
km/s
{z < 0.05}. This is because other precision distance indicators
either
lack the requisite depth {Cepheids, TRGB} or are too rare for
adequate
sampling {supernovae}, while more traditional methods {Tully-Fisher,
fundamental plane} lack the necessary precision. The SBF method is
now
being used with great success in several major ACS Wide Field Camera
programs. However, whereas the band of choice for the nearby
structure
studies has been F850LP, for the distant large-scale flow studies it
is
F814W because of its much greater throughput. As a result, the
current
calibration for the more distant studies is inadequate. We propose
to
establish the first systematic calibration of the SBF method in the
important F814W ACS WFC bandpass. We will do this by measuring SBF in
an
optimized sample of galaxies in the nearby compact Fornax cluster.
Given
the large amount of effort and HST time being dedicated to F814W SBF
measurements, it is imperative that we correct this outstanding
calibration problem while time remains. For an extremely modest
expenditure of orbits, we will remove a significant systematic error
and
vastly improve the overall accuracy of the ongoing ACS F814W SBF
work.
These data will also greatly enhance the legacy value of the HST
archive
for future SBF studies.
ACS/WFC 10905
The Dynamic State of the Dwarf Galaxy Rich Canes Venatici I Region
With accurate distances, the nearest groups of galaxies can be
resolved
in 3 dimensions and the radial component of the motions of galaxies
due
to local density perturbations can be distinguished from
cosmological
expansion components. Currently, with the ACS, galaxy distances within
8
Mpc can be measured effectively and efficiently by detecting the tip
of
the red giant branch {TRGB}. Of four principal groups at high
galactic
latitude in this domain, the Canes Venatici I Group {a} is the least
studied, {b} is the most populated, though overwhelmingly by dwarf
galaxies, and {c} is likely the least dynamically evolved. It is
speculated that galaxies in low mass groups may fail to retain
baryons
as effectively as those in high mass groups, resulting in
significantly
higher mass-to-light ratios. The CVn I Group is suspected to lie in
the
mass regime where the speculated astrophysical processes that affect
baryon retention are becoming important.
ACS/HRC/WFC 10896
An Efficient ACS Coronagraphic Survey for Debris Disks around Nearby
Stars
We propose to finish our Cycle 11 optical survey for nearby debris
disks
using the ACS/HRC coronagraph. Out of 43 orbits originally proposed
for
the survey, 23 orbits were allocated, leading to a survey of 22
stars,
from which two new debris disks were imaged for the first time. Our
analysis of the initial survey gives an empirical estimate for the
detection rate of debris disks relative to heliocentric distance and
dust optical depth. Our target list for Cycle 15 is now optimized to
yield more frequent disk detections. Likewise our observing strategy
is
improved to maximize sensitivity per telescope orbit allocated.
Therefore we present the most efficient survey possible. The
scientific
motivation is to obtain scattered light images of previously
unresolved
debris disks to determine their viewing geometry and physical
architecture, both of which may characterize the underlying
planetary
system. We choose 25 debris disk targets for which we predict a
detection rate of 25% ? 5%. Four targets have extrasolar planets
from
which the viewing geometry revealed by a disk detection will resolve
the
v sin{i} ambiguity in the planet masses. These targets present the
remarkable opportunity of finally seeing a debris disk in system
with
known planets.
ACS/HRC/WFC 10758
ACS CCDs daily monitor
This program consists of a set of basic tests to monitor, the read
noise, the development of hot pixels and test for any source of noise
in
ACS CCD detectors. The files, biases and dark will be used to create
reference files for science calibration. This programme will be for
the
entire lifetime of ACS. Changes from cycle 13:- The default gain for
WFC
is 2 e-/DN. As before bias frames will be collected for both gain 1
and
gain 2. Dark frames are acquired using the default gain {2}. This
program cover the period May, 31 2006- Oct, 1-2006. The first half
of
the program has a different proposal number: 10729.
ACS/HRC 10738
Earth Flats
Sky flats will be obtained by observing the bright Earth with the
HRC
and WFC. These observations will be used to verify the accuracy of
the
flats currently in the pipeline and to monitor any changes. Weekly
coronagraphic monitoring is required to assess the changing position
of
the spots.
ACS/WFC/NIC3 10632
Searching for galaxies at z>6.5 in the Hubble Ultra Deep Field
We propose to obtain deep ACS {F606W, F775W, F850LP} imaging in the
area
of the original Hubble Ultra Deep Field NICMOS parallel fields and -
through simultaneous parallel observations - deep NICMOS {F110W,
F160W}
imaging of the ACS UDF area. Matching the extreme imaging depth in
the
optical and near-IR bands will result in seven fields with
sufficiently
sensitive multiband data to detect the expected typical galaxies at
z=7
and 8. Presently no such a field exist. Our combined optical and
near-IR
ultradeep fields will be in three areas separated by about 20
comoving
Mpc at z=7. This will allow us to give a first assessment of the
degree
of cosmic variance. If reionization is a process extending over a
large
redshift interval and the luminosity function doesn't evolve
strongly
beyond z=6, these data will allow us to identify of the order of a
dozen
galaxies at 6.5<z<8.5 - using the Lyman break technique - and to
place a
first constrain on the luminosity function at z>6.5. Conversely,
finding
fewer objects would be an indication that the bulk of reionization
is
done by galaxies at z=6. By spending 204 orbits of prime HST time we
will capitalize on the investment of 544 prime orbits already made
on
the Hubble Ultra Deep Field {UDF}. We have verified that the program
as
proposed is scheduable and that it will remain so even if forced to
execute in the 2-gyro mode. The data will be non-proprietary and the
reduced images will be made public within 2 months from the
completion
of the observations.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
reports
of potential non-nominal performance that will be investigated.)
HSTARS:
10489 - GSAcq(1,2,1) scheduled at 301/00:46:22 results in finelock backup
(1,0,1)
using FGS-1 due to a stop flag (QF2STOPF) on FGS-2. Pre-acquisition
OBADs had (RSS) attitude error corrections values of 4432.82 and
12.88
arcseconds. Post-acquisition OBAD/MAP had 3-axis (RSS) value of 4.93
arcseonds.
10490 - GSAcq (2,1,2) failed due to search radius limit exceeded on FGS
At
303/04:52:46 GSAcq (2,1,2) scheduled for 303/04:49:33-04:57:00
failed
to
RGA control due to search radius limit exceeded on FGS 1.
OBAD #1 RSS = 7082.47
OBAD #2 RSS = 8.71
At
303/06:28:51 REAcq (2,1,2) scheduled for 303/06:25:28-06:32:55
failed
to
RGA control due to search radius limit exceeded on FGS 1.
OBAD #1 RSS= 3289.39 a-s
OBAD #2 RSS = 17.54 a-s
OBAD MAP RSS = 2585.32 a-s
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS
GSacq
29
28
FGS
REacq
13
12
OBAD with Maneuver
84
84
SIGNIFICANT EVENTS: (None)
Joe L. Cooper
Office: 301 286-6970
Home: 301 490-2449
Mobile: 410 299-8123
Home E-mail: joecooper81@comcast.net
Work E-mail:
jcooper@hst.nasa.gov