HUBBLE
SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY
REPORT #4934
PERIOD
COVERED: 5am September 18 - 5am September 21, 2009 (DOY 261/09:00z-264/09:00z)
OBSERVATIONS
SCHEDULED
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.
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.
WFC3/IR/S/C
11929
IR
Dark Current Monitor
Analyses
of ground test data showed that dark current signals are more
reliably
removed from science data using darks taken with the same
exposure
sequences as the science data, than with a single dark current
image
scaled by desired exposure time. Therefore, dark current images
must
be collected using all sample sequences that will be used in
science
observations. These observations will be used to monitor changes
in
the dark current of the WFC3-IR channel on a day-to-day basis, and to
build
calibration dark current ramps for each of the sample sequences to
be
used by GOs in Cycle 17. For each sample sequence/array size
combination,
a median ramp will be created and delivered to the
calibration
database system (CDBS).
WFC3/UVIS
11925
UVIS
Detector Linearity
This
proposal will measure the in-orbit linear response of the UVIS
detectors
by sampling over the response curve through saturation. This
program
uses exposures of a standard star field (NGC 1850) to measure
the
absolute values, and exposures of a tungsten lamp to measure
positional
variations in response, following a similar procedure as the
ground
tests.
WFC3/IR
11915
IR
Internal Flat Fields
This
program is the same as 11433 (SMOV) and depends on the completion
of
the IR initial alignment (Program 11425). This version contains three
instances
of 37 internal orbits: to be scheduled early, middle, and near
the
end of Cycle 17, in order to use the entire 110-orbit allocation.
In
this test, we will study the stability and structure of the IR
channel
flat field images through all filter elements in the WFC3-IR
channel.
Flats will be monitored, i.e. to capture any temporal trends in
the
flat fields and delta flats produced. High signal observations will
provide
a map of the pixel-to-pixel flat field structure, as well as
identify
the positions of any dust particles.
WFC3/UVIS
11912
UVIS
Internal Flats
This
proposal will be used to assess the stability of the flat field
structure
for the UVIS detector throughout the 15 months of Cycle 17.
The
data will be used to generate on- orbit updates for the delta-flat
field
reference files used in the WFC3 calibration pipeline, if
significant
changes in the flat structure are seen.
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.
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).
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.
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.
STIS/CCD
11844
CCD
Dark Monitor Part 1
The
purpose of this proposal is to monitor the darks for the STIS CCD.
FGS
11789
An
Astrometric Calibration of Population II Distance Indicators
In
2002, HST produced a highly precise parallax for RR Lyrae. That
measurement
resulted in an absolute magnitude, M(V)= 0.61+/-0.11, a
useful
result, judged by the over ten refereed citations each year
since.
It is, however, unsatisfactory to have the direct,
parallax-based,
distance scale of Population II variables based on a
single
star. We propose, therefore, to obtain the parallaxes of four
additional
RR Lyrae stars and two Population II Cepheids, or W Vir
stars.
The Population II Cepheids lie with the RR Lyrae stars on a
common
K-band Period-Luminosity relation. Using these parallaxes to
inform
that relationship, we anticipate a zero-point error of 0.04
magnitude.
This result should greatly strengthen confidence in the
Population
II distance scale and increase our understanding of RR Lyrae
star
and Pop. II Cepheid astrophysics.
FGS
11788
The
Architecture of Exoplanetary Systems
Are
all planetary systems coplanar? Concordance cosmogony makes that
prediction.
It is, however, a prediction of extrasolar planetary system
architecture
as yet untested by direct observation for main sequence
stars
other than the Sun. To provide such a test, we propose to carry
out
FGS astrometric studies on four stars hosting seven companions. Our
understanding
of the planet formation process will grow as we match not
only
system architecture, but formed planet mass and true distance from
the
primary with host star characteristics for a wide variety of host
stars
and exoplanet masses.
We
propose that a series of FGS astrometric observations with
demonstrated
1 millisecond of arc per-observation precision can
establish
the degree of coplanarity and component true masses for four
extrasolar
systems: HD 202206 (brown dwarf+planet); HD 128311
(planet+planet),
HD 160691 = mu Arae (planet+planet), and HD 222404AB =
gamma
Cephei (planet+star). In each case the companion is identified as
such
by assuming that the minimum mass is the actual mass. For the last
target,
a known stellar binary system, the companion orbit is stable
only
if coplanar with the AB binary orbit.
FGS
11704
The
Ages of Globular Clusters and the Population II Distance Scale
Globular
clusters are the oldest objects in the universe whose age can
be
accurately determined. The dominant error in globular cluster age
determinations
is the uncertain Population II distance scale. We propose
to
use FGS 1R to obtain parallaxes with an accuracy of 0.2
milliarcsecond
for 9 main sequence stars with [Fe/H] < -1.5. This will
determine
the absolute magnitude of these stars with accuracies of 0.04
to
0.06mag. This data will be used to determine the distance to 24
metal-poor
globular clusters using main sequence fitting. These
distances
(with errors of 0.05 mag) will be used to determine the ages
of
globular clusters using the luminosity of the subgiant branch as an
age
indicator. This will yield absolute ages with an accuracy of 5%,
about
a factor of two improvement over current estimates. Coupled with
existing
parallaxes for more metal-rich stars, we will be able to
accurately
determine the age for globular clusters over a wide range of
metallicities
in order to study the early formation history of the Milky
Way
and provide an independent estimate of the age of the universe.
The
Hipparcos database contains only 1 star with [Fe/H] < -1.4 and an
absolute
magnitude error less than 0.18 mag which is suitable for use in
main
sequence fitting. Previous attempts at main sequence fitting to
metal-poor
globular clusters have had to rely on theoretical
calibrations
of the color of the main sequence. Our HST parallax program
will
remove this source of possible systematic error and yield distances
to
metal- poor globular clusters which are significantly more accurate
than
possible with the current parallax data. The HST parallax data will
have
errors which are 10 times smaller than the current parallax data.
Using
the HST parallaxes, we will obtain main sequence fitting distances
to
11 globular clusters which contain over 500 RR Lyrae stars. This will
allow
us to calibrate the absolute magnitude of RR Lyrae stars, a
commonly
used Population II distance indicator.
ACS/WFC3
11670
The
Host Environments of Type Ia Supernovae in the SDSS Survey
The
Sloan Digital Sky Survey Supernova Survey has discovered nearly 500
type
Ia supernovae and created a large, unique, and uniform sample of
these
cosmological tools. As part of a comprehensive study of the
supernova
hosts, we propose to obtain Hubble ACS images of a large
fraction
of these galaxies. Integrated colors and spectra will be
measured
from the ground, but we require high-resolution HST imaging to
provide
accurate morphologies and color information at the site of the
explosion.
This information is essential in determining the systematic
effects
of population age on type Ia supernova luminosities and
improving
their reliability in measuring dark energy. Recent studies
suggest
two populations of type Ia supernovae: a class that explodes
promptly
after star-formation and one that is delayed by billions of
years.
Measuring the star-formation rate at the site of the supernova
from
colors in the HST images may be the best way to differentiate
between
these classes.
WFC3/UVIS
11594
A
WFC3 Grism Survey for Lyman Limit Absorption at z=2
We
propose to conduct a spectroscopic survey of Lyman limit absorbers at
redshifts
1.8 < z < 2.5, using WFC3 and the G280 grism. This proposal
intends
to complete an approved Cycle 15 SNAP program (10878), which was
cut
short due to the ACS failure. We have selected 64 quasars at 2.3 < z
<
2.6 from the Sloan Digital Sky Survey Spectroscopic Quasar Sample, for
which
no BAL signature is found at the QSO redshift and no strong metal
absorption
lines are present at z > 2.3 along the lines of sight. The
survey
has three main observational goals. First, we will determine the
redshift
frequency dn/dz of the LLS over the column density range 16.0 <
log(NHI)
< 20.3 cm^-2. Second, we will measure the column density
frequency
distribution f(N) for the partial Lyman limit systems (PLLS)
over
the column density range 16.0 < log(NHI) < 17.5 cm^-2. Third, we
will
identify those sightlines which could provide a measurement of the
primordial
D/H ratio. By carrying out this survey, we can also help
place
meaningful constraints on two key quantities of cosmological
relevance.
First, we will estimate the amount of metals in the LLS using
the
f(N), and ground based observations of metal line transitions.
Second,
by determining f(N) of the PLLS, we can constrain the amplitude
of
the ionizing UV background at z~2 to a greater precision. This survey
is
ideal for a snapshot observing program, because the on-object
integration
times are all well below 30 minutes, and follow-up
observations
from the ground require minimal telescope time due to the
QSO
sample being bright.
WFC3/UVIS
11559
Jovian
Upheaval and Its Impact on Vortices
We
propose observations of Jupiter with global coverage at high
resolution
to quantify changes in its atmosphere during and following
the
global upheaval. Only HST has the capability to obtain images with
enough
spatial resolution and contrast to extract velocity fields (we
will
use our newly developed technique to accomplish this), and with
WFC3
we can image Jupiter in its entirety in a single exposure. We are
in
particular interested in the Red Oval BA: Will the Oval be long
lived,
remain red, or turn white again, disappear? Both the merger of
its
precursors, and change in color has never before been witnessed. The
Great
Red Spot: This storm system appears to decrease in size and has
become
rounder, both as derived from its associated cloud deck, but also
from
its potential vorticity, a more dynamically-relevant quantity. How
will
the GRS evolve? Will it swallow the new vortices detected in
amateur
images at this same latitude band? How will this effect the
potential
vorticity? In addition, we hope to understand disturbances and
stagnation
points, both of which were detected during the present global
upheaval:
are these cyclonic regions, can they spawn anticyclones (as
suggested
by amateur images)?
COS/NUV/FUV/WFC3/UVIS/IR
11534
COS-GTO:
Atmosphere of a Transiting Planet
COS
observations of a transiting planet at different orbital locations
will
be useful in identifying the chemical content, size, temperature,
and
flows in the atmosphere of a transiting planet.
COS/NUV/FUV
11487
COS
FUV Internal/External Wavelength Scales
Observe
external radial velocity standard targets in Time-Tag
(Flash=Yes)
mode with all grating and central wavelength combinations.
The
purpose is to obtain zero point offsets for the wavelength scale
(internal
wavecal lamp scale to external standard wavelength scale) and
PSA
dispersion relations for all central wavelengths.
Following
this determination, adjustments of the nominal science target
spectral
range for each grating and central wavelength combination will
be
made via SMS-patchable constant for nominal OSM1 positions
corresponding
to each central wavelength. Subsequent to this
modification
of the wavelength scale (and its verification via analysis
of
COS30 - Program 11488), FUV science-related operations and
wavelength-
dependent EROs can commence.
COS/NUV
11471
COS
NUV Imaging Acquisition Algorithm Verification
The
purpose of this proposal is to verify the ability of the COS FSW to
place
an isolated point source at the center of the aperture, both for
the
BOA and PSA, and for Mirror A and Mirror B. The various options for
target
centering should be exercised and shown to work properly. This
test
is for acquisitions in imaging mode only. Acquisitions using
dispersed
light are tested in separate SMOV activities.
NIC1/NIC2/NIC3/S/C
11407
NICMOS
Filter Wheel Test
This
is an engineering test (described in SMOV4 Activity Description
NICMOS-04)
to verify the aliveness, functionality, operability, and
electro-mechanical
calibration of the NICMOS filter wheel motors and
assembly
after NCS restart in SMOV4. This test has been designed to
obviate
concerns over possible deformation or breakage of the filter
wheel
"soda-straw" shafts due to excess rotational drag torque and/or
bending
moments which may be imparted due to changes in the dewar
metrology
from warm-up/cool- down. This test should be executed after
the
NCS (and filter wheel housing) has reached and approximately
equilibrated
to its nominal operating temperature.
WFC3/ACS/IR
11359
Panchromatic
WFC3 Survey of Galaxies at Intermediate z: Early Release
Science
Program for Wide Field Camera 3.
The
unique panchromatic capabilities of WFC3 will be used to survey the
structure
and evolution of galaxies at the peak of the galaxy assembly
epoch.
Deep ultraviolet and near-IR imaging and slitless spectroscopy of
existing
deep multi-color ACS fields will be used to gauge
star-formation
and the growth of stellar mass as a function of
morphology,
structure and surrounding density in the critical epoch 1 <
z
< 4. Images in the F225W, F275W, and F336W filters will identify
galaxies
at z < 1.5 from their UV continuum breaks, and provide
star-formation
indicators tied directly to both local and z > 3
populations.
Deep near-IR (F125W and F160W) images will probe the
stellar
mass function well below 10^9 Msun for mass-complete samples.
Lastly,
the WFC3 slitless UV and near-IR grisms will be used to measure
redshifts
and star-formation rates from H- alpha and rest-frame UV
continuum
slope. This WFC3 ERS program will survey one 4 x 2 mosaic for
a
total area of 50 square arcminutes to 5-sigma depths of m_AB = 27 in
most
filters from the mid-UV through the near-IR.
This
multicolor high spatial resolution data set will allow the user to
gauge
the growth of galaxies through star-formation and merging. High
precision
photometric and low- resolution spectroscopic redshifts will
allow
accurate determinations of the faint-end of the luminosity and
mass
functions, and will shed light on merging and tidal disruption of
stellar
and gaseous disks. The WFC3 images will also allow detailed
studies
of the internal structure of galaxies, and the distribution of
young
and old stellar populations. This program will demonstrate the
unique
power of WFC3 by applying its many diverse modes and full
panchromatic
capability to a forefront problem in astrophysics.
FGS
11213
Distances
to Eclipsing M Dwarf Binaries
We
propose HST FGS observations to measure accurate distances of 5
nearby
M dwarf eclipsing binary systems, from which model-independent
luminosities
can be calculated. These objects have either poor or no
existing
parallax measurements. FGS parallax determinations for these
systems,
with their existing dynamic masses determined to better than
0.5%,
would serve as model-independent anchor points for the low-mass
end
of the mass-luminosity diagram.
WFC3/ACS/IR
11142
Revealing
the Physical Nature of Infrared Luminous Galaxies at 0.3<z<2.7
Using
HST and Spitzer
We
aim to determine physical properties of IR luminous galaxies at
0.3<z<2.7
by requesting coordinated HST/NIC2 and MIPS 70um observations
of
a unique, 24um flux- limited sample with complete Spitzer mid-IR
spectroscopy.
The 150 sources investigated in this program have S(24um)
>
0.8mJy and their mid-IR spectra have already provided the majority
targets
with spectroscopic redshifts (0.3<z<2.7). The proposed
150~orbits
of NIC2 and 66~hours of MIPS 70um will provide the physical
measurements
of the light distribution at the rest-frame ~8000A and
better
estimates of the bolometric luminosity. Combining these
parameters
together with the rich suite of spectral diagnostics from the
mid-IR
spectra, we will (1) measure how common mergers are among LIRGs
and
ULIRGs at 0.3<z<2.7, and establish if major mergers are the drivers
of
z>1 ULIRGs, as in the local Universe, (2) study the co-evolution of
star
formation and blackhole accretion by investigating the relations
between
the fraction of starburst/AGN measured from mid-IR spectra vs.
HST
morphologies, L(bol) and z, and (3) obtain the current best
estimates
of the far-IR emission, thus L(bol) for this sample, and
establish
if the relative contribution of mid-to-far IR dust emission is
correlated
with morphology (resolved vs. unresolved).
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
12014
- GSAcq(2,1,1) scheduled at 261/16:17:51z failed to RGA Hold (gyro
control) with Search Radius Limit Exceeded on FGS-2 at
261/16:23:06z.
Observations affected: WFC3 111 - 114, Proposal ID# 11559
12015
- GSAcq (1,2,1) scheduled from 263/04:26:41z - 04:33:41z resulted in
Fine Lock Back-up (2,0,2) at 263/04:31:43z using FGS 2
Observations possibly affected: WFC3 165 - 166, Proposal ID#
11594.
COMPLETED
OPS REQUEST:
18706-0
- Set up Tasking orders for NICMOS FW test @ 261/1551z
18707-0
- Configure Tasking Orders after FW test EDD dumps completed @ 261/2312z
18708-1
- Enable NICMOS Filter Wheel flag to continue test @ 262/1742z
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSAcq
24
23
FGS
REAcq
17
17
OBAD
with Maneuver
25
25
SIGNIFICANT
EVENTS: (None)