NASA Hubble Space Telescope Daily Report # 3399
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3399
PERIOD COVERED: DOY 188
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 9229
Orbits of Pre-Main Sequence Binaries
Our goal is to dynamically measure the masses of low mass pre-main
sequence stars. This is important because there are still no such
objects with an accurately measured mass. In cycle 5 we began to map
the orbits of young multiple star systems in Taurus using FGS3. In
cycle 8 we switched to the more capable FGS1r. We propose to continue
to observe these binary and triple systems so that we can establish
their visual orbits. In addition to our Transfer mode observations, we
include Position mode observations of reference field stars so that
the position of the multiple systems’ barycenter can be located,
giving the relative masses of the components. In addition, the
Position mode data will allow us to determine accurate parallaxes for
these systems, and hence the physical, absolute masses of the young
pre-main sequence stars along with absolute magnitudes.
HST 9382
A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO MgII-FeII Systems.
We have searched the first public release of SDSS QSO spectra for ACS 9401 The ACS Virgo Cluster Survey We propose the most comprehensive imaging survey to date of STIS 9437 Quantitative Constraints for Massive Star Evolution Models with Rotation Rotation is now recognized as an important physical component in NICMOS 9484 The NICMOS Parallel Observing Program We propose to manage the default set of pure parallels with NICMOS. WFPC2 9592 WFPC2 CYCLE 11 Standard Darks This dark calibration program obtains dark frames every week in order WFPC2 9595 WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3 This dark calibration program obtains 3 dark frames every day to WFPC2 9596 WFPC2 CYCLE 11 INTERNAL MONITOR This calibration proposal is the Cycle 11 routine internal monitor for 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, STIS 9613 STIS CCD Spectroscopic Flats C11 Obtain CCD flats on the STIS CCD in spectroscopic mode. STIS 9614 STIS CCD Imaging Flats C11 Investigate flat-field stability over a monthly period. STIS 9633 STIS parallel archive proposal – Nearby Galaxies – Imaging and Using parallel opportunities with STIS which were not allocated by the NICMOS 9640 Flats Stability This calibration proposal is the Cycle 11 NICMOS monthly monitor A ACS 9658 ACS Earth Flats This program will obtain sequences of flat field images by observing WFPC2/PC1 9663 Focus Monitoring The HST focus is monitored using WFPC2/PC1. In principle ACS/HRC ACS 9674 CCD Daily Monitor This program consists of basic tests to monitor, the read noise, the STIS 9708 STIS Pure Parallel Imaging Program: Cycle 11 This is the default archival pure parallel program for STIS during cycle WFPC2 9709 POMS Test Proposal: WFII parallel archive proposal This is the generic target version of the WFPC2 Archival Pure Parallel STIS/CCD/MA1 9840 Wind Accretion and State Transitions in the Black Hole Binary Cyg X-1 The black hole binary, Cyg X-1, is generally observed in one of two ACS/WFC/WFC2 9857 A tailored survey of proplyds with the ACS While our specific understanding of the proto-planetary disks in Orion ACS/WFC 9891 A snapshot survey of rich stellar clusters in the Large and Small Rich stellar clusters are vital to a wide variety of astrophysical ACS/WFC 9892 H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star Previous studies of nearby galaxies show large discrepancies between ACS 9984 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary COMPLETED OPS REQs: None OPS NOTES EXECUTED: 0915-1 HSTAR Documentation for FHST Map/Update Failures @ 188/0953z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 10 10 LOSS of LOCK SIGNIFICANT EVENTS: None
low-z {z<1.65} metal absorption lines and found over 200 large rest
equivalent width MgII-FeII systems. Previously, we empirically showed
that such systems are good tracers of large neutral gas columns, with
~50% being classical damped Lyman alpha {DLA} systems {N_HI>=2*10^20
cm^-2}. Here we propose to follow up a well-defined subset of 79 of
them to search for DLAs with 0.47
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.
understanding massive stars. Theory suggests that rotation affects the
lifetimes, chemical yields, stellar evolution tracks, and the
supernova and compact remnant properties {Heger & Langer 2000, Maeder
& Meynet 2000}. In a Cycle 7 program, we proved that rotational mixing
occurs in massive main sequence stars {Venn et al. 2001}. In this
proposal, we want to quantitatively test model predictions and
constrain the theory for a better understanding of massive star
evolution. We are requesting HST STIS observations of the BIII 2066
Angstrom resonance line of seven massive stars in three young clusters
carefully selected from IUE analyses. These stars show traces of boron
depletion, but without nitrogen enrichment; rotation is the only
theory able to explain this abundance pattern. These new abundances
will allow us to test rotating model predictions: that mixing strength
increases with stellar age, mass, and rotation rate. They will also
help to quantitatively constrain the rotational mixing efficiencies in
massive stars. One very high S/N spectrum of a moderately
boron-depleted star is also requested. We wish to measure its 11B/10B
ratio, which is predicted to change as boron is depleted in the
rotating models. This ratio will further confirm rotational effects
and observationally constrain the 10B{p, Alpha} thermonuclear reaction
rate, which is presently highly uncertain.
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.
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.
provide data for monitoring and characterizing the evolution of hot
pixels.
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.
and 1×1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.
Spectroscopy
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.
series of camera 1, 2, & 3 flat fields will be obtained to monitor the
health of the cameras.
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.
should provide superior capability for monitoring the HST focus. Since
most of the HST science will shift to ACS in Cycle 11 trending
observations are continued with this program to establish the focus of
WFPC2/PC1 {and hence HST} and ACS/HRC {and WFC to a lessor degree}
using exposures over full orbits that are taken in parallel. With
parallel exposures breathing cancels out for the relative camera
offset.
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.
11.
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.
long duration X-ray states: a low flux, hard spectrum state {most
common} and a high flux, soft spectrum state {rare}. Models predict
that the high/soft state corresponds to a high mass transfer phase in
the binary, and since the X-ray source is fueled by accretion from the
stellar wind of the supergiant companion, the simple expectation is
that the high/soft state results from an increased wind mass loss
rate. Alternatively, a decrease in the wind mass loss rate could
result in a more ionized and slower wind in the vicinity of the black
hole, which would then be more easily accreted by the black hole. The
best test of these hypotheses is to observe the UV P Cygni lines of
the supergiant that are formed in its wind outflow. We recently used
HST/STIS to obtain the first ever high resolution UV spectra of the
system while it resided in the unusual high/soft state. Cyg X-1 has
now returned to the low/hard state, and here we propose to revisit Cyg
X-1 and complete our investigation of the wind – X-ray state
connection. The study will determine {1} the mass loss rate and the
dynamical {density and velocity} structure of the wind of the
supergiant star in both X-ray states, and {2} how the X-ray source
ionizes the wind. These spectra will be useful for other
investigations and will form an important resource for the entire
research community.
is increasing, our general knowledge of what promotes and hinders
their birth and longevity is hampered by having good observations in
only this one region. Observations of proplyds in other regions with
different conditions of ultraviolet irradiation and age can provide
more stringent tests of our present models. We have therefore designed
an ACS/WFC and parallel WFC2 survey of open clusters embedded in H II
regions that, with a small number of orbits, maximizes the probability
of succesfully finding proplyds there. Our observing strategy will
additionally afford a quantitative study of the detected proplyds, as
well as the derivation of a correlation between those characteristics
and the clusters’ stellar population. ACS gives us an unprecedented
opportunity to kick start the mass discovery of proplyds in many
environments, an obvious way in which progress can be made in this
field. This small tailored survey, gives us an excellent chance to
obtain a huge return at low cost.
Magellanic Clouds
research, from stellar evolution studies to the formation and
evolution of galaxies. In this context, it is important to understand
how rich star clusters form and evolve. The cluster systems in the LMC
and SMC are particularly important in achieving this, because they are
the only systems which contain clusters at all stages of evolution
while being close enough to be studied as fully resolved stellar
populations – although in general this requires the capabilities of
HST. We have recently investigated the structural evolution of LMC and
SMC clusters using archival WFPC2 data, and demonstrated a dramatic
trend in the sizes of these clusters with age. We have shown that this
trend likely represents genuine structural evolution in these
clusters, although it is not clear whether we are observing a
dynamical process or the signature of changing formation conditions.
This result has implications for all astronomical research involving
massive stellar clusters. To develop this work further requires the
extension of our two samples, so that they are statistically
quantifiable. This will allow a number of key questions regarding the
structural evolution trend to be answered. We propose a two-colour
ACS/WFC SNAP survey of rich Magellanic Cloud clusters to achieve this
aim. The unique resolution and sensitivity of ACS/WFC is required for
success, because of the crowded nature of the targets. The SNAP data
will have a large number of additional applications, both to globular
cluster and Magellanic Cloud research.
Formation in a Dusty Universe
different star formation {SF} indicators on large {>100 pc, or even
global} scales: the strikingly complex interplay of young stars, dust
and ionized gas are the primary cause of this variance. The few
galaxies in the HST Archive with both WFPC2 H-alpha and mid-UV {F255W
or F300W} imaging show this complex geometry extending down to <10 pc
scales. We propose a SNAPshot survey in the ACS/WFC H-alpha filter of
48 galaxies of all Hubble types, that are nearby but beyond the Local
Group, and that were previously imaged with WFPC2 in the mid-UV and in
F814W. We aim to provide a benchmark for understanding the SF
processes in both normal and star-bursting galaxies, at spatial
resolutions unattainable from the ground for a large and varied galaxy
sample. These data can be applied to a wide range of astrophysical
problems and will, therefore, be made public immediately. Our science
goals are to: {1} spatially resolve the dust clouds and filaments
which strongly affect mid-UV and H-alpha derived SF rates, {2} test
how the large-scale correlation between H-alpha and mid-UV flux breaks
down on pc scales, and {3} model the propagation of star formation by
comparing the SF over time scales of ~100 Myr {via mid-UV} and ~5 Myr
{via H-alpha}. This will {4} significantly improve our insight into,
and calibration of SF in UV-bright galaxies at high z, and into the
cosmic SF history.
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.
reports of potential non-nominal performance that will be
investigated.) None
1124-0 Perform Observation Re-Dumps on the Partial Obs. Level @188/1042z, 188/1222z
0900-1 COMMAND PROBLEM @ 188/0928
FGS REacq 06 06
FHST
Update 24 23 188/09:49:00z