HST Daily Report #3321
DAILY REPORT # 3321
PERIOD COVERED: DOY 76
OBSERVATIONS SCHEDULED
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.
FGS 9348
The Distances to AM CVn stars
We propose to determine the parallaxes and proper motions of the five
brightest
of the seven known AM CVn systems using the HST Fine Guidance Sensors. AM
CVn
systems are binaries where mass is transferred from a completely
hydrogen-deficient, degenerate mass donor to a white dwarf primary through a
helium accretion disk. A better understanding of these systems is crucial
for a
number of reasons:, to study the late stages of binary evolution, to study
the
effect of chemical composition on the physics of accretion discs; , o to
estimate their contribution to the Supernovae Ia rate and , to estimate
their
contribution to the gravitational radiation background. All these studies
rely
critically on a determination of the distances to the currently known
systems.
With brightnesses in the range 13<V<17 and estimated distances <400pc they
are
ideal targets for the HST-FGS.
ACS/HRC 9379
Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the
Starburst-AGN
Connection
We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC
and
the filter F330W, a configuration which is optimal to detect faint star
forming
regions around their nuclei. These images will complement optical and
near-IR
images available in the HST archive, thus providing a panchromatic atlas of
the
inner regions of active galaxies, which we will use to study the
starburst-AGN
connection. The main goals of this proposal are: {1} Determine the frequency
of
circumnuclear starbursts in Seyferts, down to levels which cannot be
observed
from the ground; {2} characterize the observational {fluxes, colors,
structure,
sizes} and intrinsic {luminosities, masses, ages, global star-formation
rate}
properties of these clusters; {3} derive the luminosity functions of young
star
clusters around the nucleus of Seyferts and compare these results with those
from normal and starburst galaxies to determine their survival rate close
to the
AGN; {4} address questions about the relation between AGNs and starbursts,
like
the possible connection between the masses and luminosities of black holes
and
starbursts, and the implications for the evolution of the black holes and
their
host galaxy bulges. By adding UV images to the existing optical and near-IR
ones, this project will create an extremely valuable database for
astronomers
with a broad range of scientific interests, from the properties of the AGN
to
the properties of their host galaxies.
ACS 9401
The ACS Virgo Cluster Survey
We propose the most comprehensive imaging survey to date of low-redshift,
early-type galaxies. Our goal is to exploit the exceptional imaging
capabilities
of the ACS by acquiring deep images — in the SDSS g^ and z^ bandpasses
— for
163 E, S0, dE, dE, N and dS0 galaxies in Virgo, the nearest rich cluster.
This
extraordinary dataset would likely constitute one of the principal legacies
of
HST, and would have widespread applications for many diverse areas of
astrophysics. Our immediate scientific objectives are threefold: {1} measure
metallicities, ages and radii for the many thousands of globular clusters
{GCs}
in these galaxies, and use this information to derive the protogalactic mass
spectrum of each galaxy; {2} measure the central luminosity and color
profile of
each galaxy, and use this information to carry out a completely independent
test
of the merging hierarchy inferred from the GCs, with the aid of N-body codes
that simulate the merger of galaxies containing massive black holes; and {3}
calibrate the z^ -band SBF method, measure Virgo’s 3-D structure, and carry
out
the definitive study of the GC luminosity function’s precision as a standard
candle. Our proposed Virgo Cluster Survey will yield a database of
unprecedented
depth, precision and uniformity, and will enable us to study the record of
galaxy and cluster formation in a level of detail which will never be
possible
with more distant systems.
STIS 9421
UV Observations of Hubble Flow Type Ia Supernovae
Two independent research groups have presented compelling evidence for an
accelerating universe from the observation of high-redshift Type Ia
supernovae
{SNe Ia}. These findings have such important ramifications for cosmology
that
every effort must be made to thoroughly test the calibrated standard candles
on
which they are based, improve upon our understanding of the underlying
physics
of the SN Ia explosion mechanism and attempt to constrain or determine their
progenitors. Here we propose to obtain STIS UV spectra of five Hubble Flow
SNe
Ia. The spectra will be taken at weekly intervals over a range in time
starting
slightly before maximum light and extending to +30 days. These observations
will
accomplish the following three goals: {1} Calibration of the rest frame UV
light
curves of SNe Ia and an assessment of their potential use as distance
indicators
through UV light curve shape analyses. {2} Improvement in our understanding
of
the physics of SNe Ia, metallicity/evolutionary effects and correlations
between
peak brightness and UV spectral features. {3} Calibration of the SNe Ia
previously observed by HST at high-redshift. For z > 0.8 SNe Ia discovered
by
the Supernova Cosmology Project, the High-Z Supernovae Search Team and
future
HST discovered SNe Ia {like SN 1997ff found in the HDF} this data is
crucial for
proper cross-filter K-corrections and calibration of the supernova
photometry.
ACS 9427
Globular Cluster Systems in Supergiant E Galaxies
he most populous globular cluster systems are found in the giant ellipticals
at
the centers of galaxy clusters {Brightest Cluster Galaxies}. It is among
this
BCG class that the characteristics of globular cluster systems display their
widest range in metallicity distribution and specific frequency and thus
confront galaxy formation models with their most varied challenges. Were
these
systems built primarily by early in situ conversion of gas clouds, by later
mergers, or by ongoing accretions of dwarfs? Their extensive halo cluster
systems contain many clues to these relic events. BCGs are the biggest and
rarest type of galaxy, and to date the globular clusters in only two BCGs
{M87,
NGC 1399} are well studied. The ACS camera now brings many more such systems
within reach. We propose to image the globular cluster systems in 13 BCGs
in the
distance regime cz ~eq 2000 – 5000 km s^-1. With deep {B, I} exposures we
will
measure the globular cluster metallicity distribution functions, specific
frequency, radial distributions, and luminosity distributions, as well as
correlations among these quantities. This work will be the first
comprehensive,
homogeneous deep survey of globular clusters in BCGs. The superior area and
sensitivity of ACS will yield a gain of a factor of eight over previous
WFPC2
studies for sample size and metallicity discrimination.
ACS 9454
The Nature of the UV Continuum in LINERs: A Variability Test
LINERs may be the most common AGNs, and the signposts of accretion onto the
massive black holes present in most galaxies. However, the LINER spectrum
is the
result of UV excitation, and, in at least some LINERs, a nuclear cluster of
hot
stars, rather than an AGN, dominates the energetics in the UV. Thus, it is
still
unknown if the UV continuum, or the optical emission lines it excites, have
anything to do with an AGN. The demographics and accretion physics of
low-luminosity AGNs hinge on this question. We propose to search for
variability
in a sample of 17 LINERs with compact UV nuclei. Variability can reveal an
AGN
component in the UV continuum, even when its light is not dominant. We will
test
systematically the handful of non-definitive reports of UV variability, and
potentially quantify the AGN contribution to the UV emission. Variability
in all
or most objects will be strong evidence that LINERs mark dormant AGNs in
most
galaxies. Alternatively, a general null detection of variability will
suggest
that, even in LINERs with additional AGN signatures, the UV continuum is
stellar
in origin. Contemporaneous monitoring with the VLA/VLBA of 11 objects which
have
radio cores {five of which we already know are radio-variable} will reveal
the
relations between UV and radio variations. The UV-variable objects will be
targeted for future, better-sampled, monitoring.
ACS 9463
Are OH/IR stars the youngest post-AGB stars? An ACS SNAPshot imaging survey
Essentially all well-characterized preplanetary nebulae {PPNs}– objects in
transition between the AGB and planetary nebula evolutionary phases – are
bipolar, whereas the mass-loss envelopes of AGB stars are strikingly
spherical.
In order to understand the processes leading to bipolar mass-ejection, we
need
to know at what stage of stellar evolution does bipolarity in the mass-loss
first manifest itself? We have recently hypothesized that most OH/IR stars
{evolved mass- losing stars with OH maser emission} are very young PPNe. We
propose an ACS/SNAPshot imaging survey of a large, morphologically unbiased
sample of these objects, selected using their IRAS 12-to-25micron colors.
Our
ground-based imaging study of OH/IR stars has revealed a few compact bipolar
objects, supporting our hypothesis. However since most objects remain
unresolved, HST observations are needed to determine how and when the
bipolar
geometry asserts itself. Our complementary program of interferometric
mapping of
the OH maser emission in our sources is yielding kinematic information with
spatial resolution comparable to that in the HST images. The HST/radio data
will
provide crucial input for theories of post-AGB stellar evolution. In
addition,
these data will also indicate whether the multiple concentric rings,
“searchlight beams”, and truncated equatorial disks recently discovered
with
HST in a few PPNs, are common or rare phenomena.
ACS 9480
Cosmic Shear With ACS Pure Parallels
Small distortions in the shapes of background galaxies by foreground mass
provide a powerful method of directly measuring the amount and distribution
of
dark matter. Several groups have recently detected this weak lensing by
large-scale structure, also called cosmic shear. The high resolution and
sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear
accurately on small scales. Using 260 parallel orbits in Sloan textiti
{F775W}
we will measure for the first time: beginlistosetlength sep0cm
setlengthemsep0cm
setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em
the
skewness of the shear distribution, and em the magnification effect.
endlist Our
measurements will determine the amplitude of the mass power spectrum
sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density
Omega_m with s/n=4. They will be done at small angular scales where
non-linear
effects dominate the power spectrum, providing a test of the gravitational
instability paradigm for structure formation. Measurements on these scales
are
not possible from the ground, because of the systematic effects induced by
PSF
smearing from seeing. Having many independent lines of sight reduces the
uncertainty due to cosmic variance, making parallel observations ideal.
NICMOS 9484
The NICMOS Parallel Observing Program
We propose to manage the default set of pure parallels with NICMOS. Our
experience with both our GO NICMOS parallel program and the public parallel
NICMOS programs in cycle 7 prepared us to make optimal use of the parallel
opportunities. The NICMOS G141 grism remains the most powerful survey tool
for
HAlpha emission-line galaxies at cosmologically interesting redshifts. It is
particularly well suited to addressing two key uncertainties regarding the
global history of star formation: the peak rate of star formation in the
relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star
formation missing from UV continuum-based estimates due to high extinction.
Our
proposed deep G141 exposures will increase the sample of known HAlpha
emission-
line objects at z ~ 1.3 by roughly an order of magnitude. We will also
obtain a
mix of F110W and F160W images along random sight-lines to examine the space
density and morphologies of the reddest galaxies. The nature of the
extremely
red galaxies remains unclear and our program of imaging and grism
spectroscopy
provides unique information regarding both the incidence of obscured star
bursts
and the build up of stellar mass at intermediate redshifts. In addition to
carrying out the parallel program we will populate a public database with
calibrated spectra and images, and provide limited ground- based optical and
near-IR data for the deepest parallel fields.
WFPC2 9592
WFPC2 CYCLE 11 Standard Darks
This dark calibration program obtains dark frames every week in order to
provide
data for the ongoing calibration of the CCD dark current rate, and to
monitor
and characterize the evolution of hot pixels. Over an extended period these
data
will also provide a monitor of radiation damage to the CCDs.
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
data
for monitoring and characterizing the evolution of hot pixels
WFPC2 9596
WFPC2 CYCLE 11 INTERNAL MONITOR
This calibration proposal is the Cycle 11 routine internal monitor for
WFPC2, to
be run weekly to monitor the health of the cameras. A variety of internal
exposures are obtained in order to provide a monitor of the integrity of
the CCD
camera electronics in both bays {gain 7 and gain 15}, a test for quantum
efficiency in the CCDs, and a monitor for possible buildup of contaminants
on
the CCD windows.
CAL/WF2 9597
Intflat Sweep, Visflat Sweep, and Filter Anomaly Check
No abstract available.
STIS 9606
CCD Dark Monitor-Part 2
Monitor the darks for the STIS CCD.
STIS 9608
CCD Bias Monitor – Part 2
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and
1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.
STIS/CAL 9609
CCD Read Noise Monitor
This proposal measures the read noise of all the amplifiers {A, B, C, D} on
the
STIS CCD using pairs of bias frames. Full frame and binned observations are
made
in both Gain 1 and Gain 4, with binning factors of 1×1, 1×2, 2×1 and 2×2.
All
exposures are internals. Pairs of visits are scheduled for monthly
execution.
STIS 9612
STIS CCD Hot Pixel Annealing Cycle 11
The effectiveness of the CCD hot pixel annealing process is assessed by
measuring the dark current behavior before and after annealing and by
searching
for any window contamination effects. In addition CTE performance is
examined by
looking for traps in a low signal level flat. Follows on from proposal 8906.
STIS 9613
STIS CCD Spectroscopic Flats C11
STIS 9614
STIS CCD Imaging Flats C11
ACS 9658
ACS Earth Flats
This program will obtain sequences of flat field images by observing the
bright
Earth. Several UV filters from the interim calibration program {9564}
require
additional exposures to obtain the required illumination. A few UV filters
from
this program will be repeated to monitor for changes in the flat fields and
to
verify the interim results. Since no streaks are observed in the UV, the
wavelength coverage is extended to longer wavelengths in order to explore
the
severity of streaks in the flats from clouds in the FOV. We have added
exposures
for the HRC in the visible filters to verify the results derived from the
L-flat
campaign and to explore the severity of streaks. We have also added
exposures on
WFC using the minimum exposure time and using filters which will not
saturate
the brightest WFC pixel by more than 10 times the full well.
ACS 9673
CCD Daily Monitor
for any source of noise in ACS CCD detectors. This programme will be
executed
once a day for the entire lifetime of ACS
WFPC2 9676
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel
program.
The program will be used to take parallel images of random areas of the sky,
following the recommendations of the 2002 Parallels Working Group.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle 10.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.) None
COMPLETED OPS REQs:
None
OPS NOTES EXECUTED:
0910-2 SI Console response to MCE Resets after FSW 4.8 is activated @
076/11:04:24z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 08 08
FGS REacq 06 06
FHST Update 20 20
LOSS of LOCK
SIGNIFICANT EVENTS:
CCS-C was released to Development for CCS 4.0.2 installation @ 076/1415z.
