HST Daily Report # 3315
DAILY REPORT # 3315
PERIOD COVERED: DOYs 66-68
OBSERVATIONS SCHEDULED
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 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 9673
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
development
of hot pixels and test for any source of noise in ACS CCD detectors. This
programme will be executed once a day for the entire lifetime of ACS
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.
ACS 9293
Massive Black Holes in Early Type Galaxies
Recently, a nearly perfect relation has been recognized between the masses
of
the black holes {for 3×10^6 Msun < M_BH < 3×10^9 Msun} at the centers of
galaxies and the velocity dispersions of their bulges. However,
uncertainties
over the exact slope of the correlation still remain, and it is not known if
such a relation extends to black holes of lower and higher masses. The
discovery
of small {r ~ a few hundred pc}, well defined, dust and gas disks in the
nuclei
of some active elliptical galaxies opened a new avenue for measuring central
mass distributions. When ionized gas is present, a small number of high
spatial
resolution {e.g. STIS} spectra are sufficient to characterize the disk
dynamics
and the galaxy’s central mass {e.g., M87, M81, NGC 4374}. We propose to use
STIS
spectroscopy to measure black hole masses, using gas dynamics, in the
centers of
several brightest cluster galaxies {BCGs}, 2 nearby galaxies with low
velocity
dispersions, and a number of elliptical galaxies known to harbor small
nuclear
dust disks. The proposed targets encompass a wide range of black hole
masses,
allowing us to fully examine the M_BH — sigma relationship. We will also
obtain
H-alpha and continuum images to fully characterize the gaseous and dust
morphology as well as stellar surface profile in the central regions.
ACS 9409
The Evolution of Globular Cluster Systems in Merger Remnants
Mergers seem to have played a major role in determining the shapes and
dynamics
of elliptical galaxies. A few galactic mergers still occur and offer
valuable
clues to past evolutionary processes. Globular clusters formed during
mergers
are crucial probes for age-dating such events, and help shed light on the
process of cluster formation and evolution. With young globulars in ongoing
mergers now well studied, we propose to make deep ACS observations of
intermediate-age globular clusters in two bona fide ellipticals: NGC 1316
and
3610. These ellipticals have line-strength indices, UBV colors, and fine
structure indicative of their being 2 — 4 Gyr old merger remnants. Past
HST+WFPC2 observations have shown that they also possess significant numbers
of
intermediate-age globulars as part of their bimodal cluster populations. We
plan
to use the new HST+ACS observations to {1} measure high-accuracy BVI colors
for
clusters up to ~ 2 — 3 mag fainter than ever before, {2} use these colors
to
separate first- and second-generation clusters, and {3} determine the
luminosity
functions of the two kinds of clusters to 3 — 4 mag past the peak for old
globulars. Deep dithered BVI images form a crucial part of our observing
strategy. This program should permit—for the first time—to directly
detect
the predicted evolution of the cluster luminosity function from a power law
for
young clusters to the Gaussian distribution typical of old globulars.
ACS/CAL 9707
Elevated ACS CCD temperature study
To gain an understanding of the effects of detector temperature on hot pixel
dark rates and CTE behaviour, measurements will be taken with the TEC set
points
at -71.5C and -66.7C. Bias and dark frames plus CTE images will be recorded
at
the normal operating temperature, -77C, and at the two higher settings
ACS/WFC 9575
Default {Archival} Pure Parallel Program.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.
ACS/WFPC2 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
Survey
Fields
In anticipation of the allocation of ACS high-latitude imaging survey{s}, we
request a modification of the default pure parallel program for those WFPC2
parallels that fall within the ACS survey field. Rather than duplicate the
red
bands which will be done much better with ACS, we propose to observe in the
near-ultraviolet F300W filter. These data will enable study of the
rest-frame
ultraviolet morphology of galaxies at 0<z<1. We will determine the
morphological
k-correction, and the location of star formation within galaxies, using a
sample
that is likely to be nearly complete with multi-wavelength photometry and
spectroscopic redshifts. The results can be used to interpret observations
of
higher redshift galaxies by ACS.
NICMOS 9485
Completing A Near-Infrared Search for Very Low Mass Companions to Stars
within
10 pc of the Sun
Most stars are fainter and less massive than the Sun. Nevertheless, our
knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is
quite limited. Unknown are the true luminosity function {LF}, multiplicity
fraction, mass function, and mass-luminosity relation for red and brown
dwarfs,
though they dominate the Galaxy in both numbers and total mass. The best way
to
constrain these relations is a search for faint companions to nearby stars.
Such
a search has several advantages over field surveys, including greater
sensitivity to VLM objects and the availability of precise parallaxes from
which
luminosities and masses can be derived. We propose to complete our
four-filter
NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma
detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10
and
100 AU that are at least 9 mag fainter than the empirical end of the main
sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When
completed, our search will be the largest, most sensitive, volume-limited
search
for VLM companions ever undertaken. Our four-filter search will permit
unambiguous identification of VLM-companion candidates for follow-up
observation. Together with IR speckle and deep imaging surveys, our program
will
firmly establish the LF for VLM companions at separations of 1-1000 AU and
the
multiplicity fraction of all stars within 10 pc.
NICMOS 9640
Flats Stability
This calibration proposal is the Cycle 11 NICMOS monthly monitor A series of
camera 1, 2, & 3 flat fields will be obtained to monitor the health of the
cameras.
NICMOS 9702
NICMOS Parallel Thermal Background
NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to
establish the stability of the HST+NCS+Instrument thermal emission. This
data
will be compared against the already available Camera 3 measurements in
F222M
which show an increased thermal background.
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.
NICMOS 9360
Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample
We propose to carry out a NICMOS snapshot survey in the Paschen-alpha
{PAlpha}
emission line and H-band of the sample of galaxies being observed at 3.5 —
160
microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related
guaranteed
time survey of starburst galaxies. The PAlpha images, accessible only from
HST,
will be combined with groundbased HAlpha imaging to measure the extinction
in
the star-forming centers of these galaxies, and obtain robust, extinction-
corrected maps of the massive star formation rate {SFR}. The PAlpha data by
themselves will provide reliable `extinction- free’ SFRs, and a
cross-calibration of the {dust–affected} HAlpha– and UV–based SFRs. The
PAlpha–based SFR measurements will extend the SFR-vs.-gas density law
{Schmidt–law} to surface densities at least 30 times higher than what is
accessible using HAlpha–based SFR measurements alone, bridging the gap
between
normal galaxies and IR–luminous starbursts. Furthermore, the combination
of the
HST PAlpha images with the SIRTF images and spectra, as well as ancillary
ground–based UBVRIJHK images and GALEX UV images being obtained as part of
the
SINGS project, will provide a definitive study of the radiative transfer of
starlight and dust heating in star–forming galaxies. The processed NICMOS
images will be incorporated into the public SINGS Legacy Data Archive, to
enable
scores of follow-up studies by the astronomical community at large.
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.
STIS 9607
CCD Bias Monitor – Part 1
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 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9380
Determination of Extragalactic Extinction Laws at UV wavelengths with
gravitationally-lensed QSOs
The study of extragalactic extinction laws is of paramount importance as it
plays a key role in galaxy evolution, as well as for the determination of
the
cosmological parameters, for example using SNe. We propose to utilize a new
technique based on flux measurements of gravitationally lensed,
multiply-imaged
QSOs to estimate the extinction law of the lensing galaxy. Here we propose a
pilot project of STIS observations of the doubly-imaged QSO SBS 0909+532
with a
separation between images of 1.1 arcsec. Our goal would be to determine the
extinction law at UV wavelengths in the lens galaxy {z=0.83}. In a study
that is
the first of this type, we have obtained ground-based Integral Field
Spectroscopy {IFS} data in the region of the 2175Angstrom PAH bump for SBS
0909+532. Our proposed observations will allow us to complete and extend the
extinction law farther in the UV. Such observations would be impossible
from the
ground because they extend too far into the UV, and HST is the only
instrument
available with the necessary spatial resolution and sensitivity.
STIS 9631
Faint Standard Extension {FASTEX}
Fainter standard stars are needed for the flux calibration of COS, for the
prism
modes on ACS, and for astronomical community, in general. The bright object
safety limit for COS is 1.25 ct/s per pixel, while the total countrate
limit per
FUV detector segment is 20000/s. In addition, the GALEX project {see
Appendix}
requires more secondary standards in the flux range of the two fainter
original
FASTEX stars. Customarily, one NASA project provides observing time in
support
of other NASA projects. The existing observations of the two fainter FASTEX
standards, WD0947+857 and WD1657+343, have the most CTE losses in the G430L
data
and are still a bit marginal on S/N. Since the stellar models are normalized
to
V, good spectrophotometry to 5500A is important. All five targets will be
observed at the new G430L aperture to minimize CTE loss and at the original
aperture to constrain CTE models. Combined with additional planned cal data
for
stars of intermediate flux, the CTE model for spectra can be tuned to cover
the
full range of signal levels.
STIS 9625
STIS NUV-MAMA Cycle 11 Flats
This program will obtain NUV-MAMA observations of the STIS internal
Deuterium
lamp to construct an NUV flat applicable to all NUV modes
STIS 9362
STIS Observations of the Intrinsic UV Absorption in the Dwarf Seyfert
Nucleus of
NGC 4395
The Sd IV dwarf galaxy NGC 4395 is one of the nearest {d ~ 4.2 Mpc} and
least
luminous {L_bol ~ 10^41 ergs s^-1} examples of Seyfert 1 galaxies.
Furthermore,
it is the only known example of an active nucleus within a bulgeless,
extreme
late-type galaxy. This unique object possesses all of the classic Seyfert 1
properties in miniature, including broad and narrow emission lines and
highly
variable X-ray emission, presumably powered by a small {few x 10^4 M_odot}
black
hole. Furthermore, we have discovered evidence for blueshifted, intrinsic
absorption lines in the UV {C IV LambdaLambda1548.2, 1550.8}, while X-ray
spectra show the presence of bound-free edges from O VII and O VIII. We
propose
HST/STIS echelle observations to determine the properties {ionization
states,
column densities, velocity coverages, covering factors} of the intrinsic UV
absorbers in NGC 4395. Due to the high covering factor of its narrow-line
emission, NGC 4395 offers the best case for testing the connection between
the
absorbers and the narrow-line region {NLR}. Furthermore, an empirical
comparison
of its absorption properties with those in higher luminosity active galactic
nuclei {AGN} will provide valuable constraints on dynamical models of the
absorbers, which make predictions that are strongly dependent on luminosity
and/or central black hole mass.
STIS 9633
STIS parallel archive proposal – Nearby Galaxies – Imaging and Spectroscopy
Using parallel opportunities with STIS which were not allocated by the TAC,
we
propose to obtain deep STIS imagery with both the Clear {50CCD} and
Long-Pass
{F28X50LP} filters in order to make color-magnitude diagrams and luminosity
functions for nearby galaxies. For local group galaxies, we also include
G750L
slitless spectroscopy to search for e.g., Carbon stars, late M giants and
S-type
stars. This survey will be useful to study the star formation histories,
chemical evolution, and distances to these galaxies. These data will be
placed
immediately into the Hubble Data Archive.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle 10.
STIS/ACS 9384
Ozone, Condensates, and Dust in the Martian Atmosphere
We propose to utilize the unique UV capabilities of STIS and ACS/HRC in
order to
study the spatial and seasonal variations in ozone, condensates, and dust
in the
Martian atmosphere. The data obtained will be critical in addressing recent
breakthroughs in understanding the basic radiative, transport, and
microphysical
processes that provide for both long-term and short-term balance within the
global Mars climate system. The proposal includes both Cycle 11 & 12
observations in order to span the classic dust storm season on Mars and
provide
the first good opportunity for HST to synoptically observe a dusty
atmosphere on
the planet. The UV observations will complement broad-band visible and IR
observations that will be made during the Mars Global Surveyor Extended
Mission
and will provide support for the future UV observations of MARCI on the 2005
Mars Reconnaissance Orbiter.
STIS/CCD 9239
Absolute Proper Motions of Nearby Dwarf Spheroidal Galaxies-Cycle 10.
The Space Telescope Imaging Spectrograph (CCD) was used to measure precise
absolute proper motions for four dwarf spheroidal satellites of the Milky
Way
using spectroscopically-confirmed background QSOs to define a zero- velocity
reference frame.
STIS/CCD 9068
Accurate Determination of the BH Mass in Early-Type Disk Galaxies.
The Space Telescope Imaging Spectrograph (CCD) was used to map the ionized
gas
velocity field of three early-type disk galaxies, for which we will be able
to
derive high precision BH mass measurements. The sample galaxies have been
selected by means of ground-based high resolution spectroscopy among 37
observed
objects, since it is recognized in their central regions the clear presence
of a
circumnuclear Keplerian disk of ionized disk suitable for dynamical
modeling.
STIS/CCD/MA1 9357
Towards a global understanding of accretion physics –, Clues from an UV
spectroscopic survey of cataclysmic variables
Accretion inflows and outflows are fundamental phenomena in a wide variety
of
astrophysical environments, such as Young Stellar Objects, galactic
binaries,
and AGN. Observationally, cataclysmic variables {CVs} are particularly well
suited for the study of accretion processes. We propose to carry out a STIS
UV
spectroscopic snapshot survey of CVs that fully exploits the diagnostic
potential of these objects for our understanding of accretion physics. This
survey will provide an homogenous database of accretion disc and wind
outflow
spectra covering a wide range of mass transfer rates and binary
inclinations. We
will analyse these spectra with state-of-the-art accretion disc model
spectra
{SYNDISK}, testing our current knowledge of the accretion disc structure,
and,
thereby, providing new insight into the so far not well understood process
of
viscous dissipation. We will use our parameterised wind model PYTHON for the
analysis of the radiation driven accretion disc wind spectra, assessing the
fundamental question whether the mass loss rate correlates with the disc
luminosity. In addition, our survey data will identify a number of systems
in
which the white dwarf significantly contributes to the UV flux, permitting
an
analysis of the impact of mass accretion on the evolution of these compact
stars. This survey will at least double, if not triple, the number of
high-quality accretion disc / wind outflow / accreting white dwarf spectra,
and
we waive our proprietary rights to permit a timely use of this database.
STIS/CCD/MA1/MA2 9036
An Ultraviolet Spectroscopic Survey of Star-Forming Galaxies in the Local
Universe.
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was used to
perform
a comprehensive STIS ultraviolet spectroscopic survey of star-forming
galaxies
in the local universe. The sample covers a broad range of morphologies,
chemical
composition, and luminosity. The observations will provide spectral coverage
between 1200 and 3100 Angstrom, at a resolution of 100 to 200 kms and S/N of
about 30. The data set will allow the proposers to document and quantify the
effects of massive stars on the interstellar medium and to infer
implications
for the evolution of the host galaxies.
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.
WFPC2 9634
POMS Test Proposal: WFII targeted parallel archive proposal
The parallel opportunities available with WFPC2 in the neighborhood of
bright
galaxies are treated in a slightly different way from the normal pure
parallels.
Local Group galaxies offer the opportunity for a closer look at young
stellar
populations. Narrow-band images in F656N can be used both to identify young
stars via their emission lines, and to map the gas distribution in
star-forming
regions. Thus, the filter F656N is added to the four standard filters. Near
more
distant galaxies, up to about 10 Mpc, we can map the population of globular
clusters; for this purpose, F300W is less useful, and only F450W, F606W, and
F814W will be used.
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/NICMOS/ACS/HRC 9354
Saturn’s Atmospheric Structure at Solstice
We propose to image Saturn near its solstice with the same 22 WFPC2/NICMOS
filters which we imaged Saturn near its equinox about six years ago.
Additionally, we propose to use the ACS/HRC with its high ultraviolet
throughput
and its superior spatial resolution. All filters span a wavelength range of
a
factor of 10, they cover methane band strengths over several orders of
magnitude, and they include the center and wings of the hydrogen dipole
absorption near 2000 nm. Thus, they probe many atmospheric levels over five
scale heights. The 22 WFPC2/NICMOS filters have proven to provide an
excellent
probe of Saturn’s vertical aerosol structure. The spatial resolution yields
several hundred resolution elements in latitude which can be grouped into
10-15
distinct zones. The best viewing of Saturn high southern latitudes occurs
at its
winter solstice which happens during Cycle 11. The three spacecraft which
have
visited Saturn flew by near Saturn’s equinox, and Cassini will miss the
solstice
too. HST acquired comprehensive data of Saturn near its last equinox in
1995.
The proposed observations will expand this data set to Saturn’s solstice and
thus provide a unique record of its seasonal variation.
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:
1082-0 What to expect during ACS WFC CCD on orbit test @ 066/12:30z
1083-0 Modify Observer Limits @ 066/2048z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 22 22
FGS REacq 23 23
FHST Update 50 50
LOSS of LOCK
SIGNIFICANT EVENTS:
CCS "G" String CCS Release 4.0.2. is being used for real time operations.
Command Timing Test (3/7/03). All test objectives were satisfied.
Numerous
runs of data with various command timing parameters were executed. Results
will
be compared to data from CCS release 4.01 and the established
baseline. At this
time there are no command timing issues with respect to release 4.02 going
operational.
