HST Daily Report #3345
HUBBLE SPACE TELESCOPE
DAILY REPORT #3345
PERIOD COVERED: DOY 108-110
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 9468
ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7
We propose an ACS grism parallel survey to search for emission-line
galaxies toward 50 random lines of
sight over the redshift interval 0 < zpl 7. We request ACS parallel
observations of duration more than
one orbit at high galactic latitude to identify ~ 300 HAlpha
emission-line galaxies at 0.2pl zpl
0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3pl zpl 1.68, and
pg 1000 Ly-alpha
emission-line galaxies at 3pl zpl 7 with total emission line flux fpg 2*
10^-17 ergs s^-1 cm^-2 over
578 arcmin^2. We will obtain direct images with the F814W and F606W
filters and dispersed images with
the WFC/G800L grism at each position. The direct images will serve to
provide a zeroth order model both
for wavelength calibration of the extracted 1D spectra and for
determining extraction apertures of the
corresponding dispersed images. The primary scientific objectives are
as follows: {1} We will
establish a uniform sample of HAlpha and O II emission-line galaxies at
z<1.7 in order to obtain
accurate measurements of co-moving star formation rate density versus
redshift over this redshift
range. {2} We will study the spatial and statistical distribution of
star formation rate intensity in
individual galaxies using the spatially resolved emission-line
morphology in the grism images. And {3}
we will study high-redshift universe using Ly-alpha emitting galaxies
identified at z pl 7 in the
survey. The data will be available to the community immediately as they
are obtained.
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 9476
Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster
Sample
The study of distant cluster galaxies requires two key ingredients: {1}
deep high-resolution imaging,
to constrain galaxy structure; and {2} 8m-class spectroscopy, to measure
stellar content,
star-formation rates, dynamics, and cluster membership. We will reach
both conditions with the addition
of HST/ACS imaging to our suite of VLT {36 nights} and NTT {20 nights}
observations of 10 confirmed
clusters at z~0.8, drawn from the ESO Distant Cluster Survey {EDisCS}.
The proposed HST/ACS data will
complement our existing optical/IR imaging and spectroscopy with
quantitative measures of cluster
galaxy morphologies {i.e. sizes and shapes, bulge-disk decompositions,
asymmetry parameters}, and with
measurements of cluster masses via weak lensing. Major advantages unique
to the EDisCS project
include: {i} uniform selection of clusters; {ii} large enough sample
sizes to characterize the
substantial cluster-to-cluster variation in galaxy populations; {iii}
large quantities of high quality
data from 8m telescopes; {iv} uniform measurements of morphologies,
spectroscopic and photometric
redshifts, SEDs, star-formation/AGN activities, and internal kinematics;
{v} optical selection of
clusters to complement the X-ray selection of almost all high-z clusters
in the ACS GTO programs; {vi}
forefront numerical simulations designed specifically to allow physical
interpretation of observed
differences between the high-z and local clusters.
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/HRC 9391
High-Resolution Imaging of Pluto’s Surface
We will collect a series of observations with the ACS/HRC from which we
will derive a two-color global
map of Pluto’s surface. We will image Pluto at F435W and F555W,
wavelengths that have been extensively
studied from the ground over the past 50 years. The maps will provide
albedos with accurate error
determinations down to 52 degrees South latitude. These observations
will provide a second epoch of HST
mapping of the active surface of Pluto as it continues to recede from
the
Sun and will provide an important context for other detailed studies of
Pluto.
ACS/WFC/HRC 9445
Gravitational Microlensing in the NGC 3314A-B Galaxy Pair.
The Advanced Camera for Surveys (WFC and HRC) was used to determine the
composition of the dark matter
that dominates the masses of galaxies which is an important unsolved
problem.
ACS/WFPC2 9488
Cosmic Shear – with ACS Pure Parallel Observations
The ACS, with greater sensitivity and sky coverage, will extend our
ability to measure the weak
gravitational lensing of galaxy images caused by the large scale
distribution of dark matter. We
propose to use the ACS in pure parallel {non- proprietary} mode,
following the guidelines of the ACS
Default Pure Parallel Program. Using the HST Medium Deep Survey WFPC2
database we have measured cosmic
shear at arc-min angular scales. The MDS image parameters, in particular
the galaxy orientations and
axis ratios, are such that any residual corrections due to errors in the
PSF or jitter are much smaller
than the measured signal. This situation is in stark contrast with
ground-based observations. We have
also developed a statistical analysis procedure to derive unbiased
estimates of cosmic shear from a
large
number of fields, each of which has a very small number of galaxies. We
have therefore set the stage
for measurements with the ACS at fainter apparent magnitudes and
smaller, 10 arc-second scales
corresponding to larger cosmological distances. We will adapt existing
MDS WFPC2 maximum likelihood
galaxy image analysis algorithms to work with the ACS. The analysis
would also yield an online database
similar to that in archive.stsci.edu/mds/
FGS/CAL 9602
Long Term Monitoring of FGS1r in Position Mode
It is known from our experience with FGS3, and later with FGS1r, that an
FGS on orbit experiences long
term evolution, presumably due to disorption of water from the
instrument’s graphite epoxy composites.
This manifests principally as a change in the plate scale and
secondarily as a change in the geometric
distortions. These effects are well modeled by adjustments to the rhoA
and kA parameters which are used
to transform the star selector servo angles into FGS {x, y} detector
space coordinates. By
observing the relative positions of selected stars in a standard cluster
at a fixed telescope pointing
and orientation, the evolution of rhoA and kA can be monitored and
calibrated to preserve the
astrometric performance of FGS1r.
FGS1R 9408
Calibrating the Mass-Luminosity Relation at the End of the Main Sequence
We propose to use HST-FGS1R to calibrate the mass-luminosity relation
{MLR} for stars less massive than
0.2 Msun, with special emphasis on objects near the stellar/brown dwarf
border. Our goals are to
determine M_V values to 0.05 magnitude, masses to 5 than double the
number of objects with masses
determined to be less than 0.20 Msun. This program uses the combination
of HST-FGS3/FGS1R at optical
wavelengths and ground-based infrared interferometry to examine nearby,
subarcsecond binary systems.
The high precision measurements with HST-FGS3/FGS1R {to 1 mas in the
separations} for these faint
targets {V = 10–15} simply cannot be equaled by any ground based
technique. As a result of these
measurements, we are deriving high quality luminosities and masses for
the components in the observed
systems, and characterizing their spectral energy distributions from 0.5
to 2.2 Mum. Several of the
objects included have M < 0.1 Msun, placing them at the very end of the
stellar main sequence. Three of
the targets are brown dwarf candidates, including the current low mass
record holder, GJ
1245C, with a mass of 0.062 +/- 0.004 Msun. The payoff of this proposal
is high because all 10 of the
systems selected have already been resolved with HST- FGS3/FGS1R during
Cycles 5–10 and contain most
of the reddest objects for which masses can be determined.
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 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<z<1.60. Only QSOs brighter than g’=19
were selected. The QSO
emission and DLA absorption redshifts were constrained to virtually
eliminate data loss due to
intervening Lyman limit absorption. Consequently, we expect to discover
~40 new DLAs, which is a
three-fold increase in this redshift interval. This will significantly
improve our earlier low-z DLA
statistical results on their incidence, cosmological mass density, and
N_HI distribution. The results
will also allow us to better quantify the empirical DLA — metal-line
correlation. With this improved
understanding, the need for follow-up UV spectroscopy will lessen and,
with the release of the final
database of SDSS QSO spectra {an ~25-fold increase}, the number of low-z
DLAs could be increased
arbitrarily. Thus, the power of the large and statistically-sound SDSS
database in combination with a
proven technique for finding low-z DLAs will, over the next few years,
essentially solve the problem of
making an accurate determination of the cosmic evolution of the neutral
gas component down to z~0.4.
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 9639
Photometric Stability
This NICMOS calibration proposal carries out photometric monitoring
observations during cycle 11.
SNAP 9356
SNAPSHOT survey of the Planetary Nebulae population of the Galactic
Bulge
The spectacular structures seen in HST images of planetary nebulae {PNe}
are generally accepted as
originating from hydrodynamical interactions between stellar winds: the
interacting-stellar wind model
{ISW}. Traditionally, the shaping is thought to occur after the star
becomes hot enough to ionize the
PN. But recent HST images indicate that the shaping may occur earlier,
and the newer GISW model puts
the shaping during the pre-planetary nebula evolution. The relative
importance of both models is not
known: GISW shaping will account for some fraction of PNe, but estimates
range from 15–100 during the
PN phase, especially for the youngest PNe. We here propose an HST
Snapshot survey of compact PNe in the
Galactic Bulge, to test these predictions. The Bulge provides the only
PNe population for which
progenitor masses are known and nebular ages can be measured. In support
of these HST measurements we
have already measured velocity fields and emission line fluxes. The
survey will give an unbiased
sampling of morphologies, and allow evolutionary sequences to be
determined to test the ISW versus the
GISW model. By-products of the survey will be the determination of
nebular masses, diameters and
filling factors. We will also obtain the White Dwarf mass distribution
in the Bulge, and the
initial-final mass function for low-mass stars.
STIS 9506
A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS
We propose a STIS G140L spectroscopic Snapshot program of bright
{V<=16.5} AGN not previously observed
in the UV to discover new high-column density {N_H >= 10^15 cm^-2}
LyAlpha absorbers in the local
Universe {z <= 0.45}. Many more of these high column density systems are
needed because: {1} They
contribute most of the baryons to the local IGM; {2} They include
systems for which valuable
metallicity and D/H measurements can be made with the Cosmic Origins
Spectrograph {COS}; {3} They
include many of the “warm-hot” absorbers, thought to be a large baryon
reservoir in the local
Universe; and {4} They are most likely to be “associated” with galaxy
halos. Because of their low-z,
many of these absorbers can be located relative to galaxies of known
redshifts, allowing an immediate
scientific return from these snapshots. Perhaps the most important,
lasting results of this survey
require higher resolution reobservations with COS by our GTO team. Using
these snapshots to select the
best targets, we will obtain COS R~22, 000 spectra to determine the D/H
and metallicity of absorbers in
galaxy halos, groups, and voids. We will use pairs and
“constellations” of AGN to determine absorber
sizes, shapes, and covering factors. Candidate “warm-hot” absorbers
will be reobserved with COS to
determine their numbers accurately and to assess their metallicity,
sizes, and relationships to
galaxies and galaxy groups.
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 9606
CCD Dark Monitor-Part 2
Monitor the darks for the STIS CCD.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle
10.
STIS 9507
STIS/UV snapshot survey of bright AGN
We propose a UV spectroscopic snapshot survey of bright AGN, quadrupling
the number of Seyferts UV
spectra and adding dozens of new quasars, aimed at the following goals:
beginenumerate em Finding the
relationship between the intrinsic luminosity of the AGN and the maximum
velocity {and width} of the
outflow emanating from it, and determining the frequency of outflows in
low-z AGN as a function of
luminosity. em Surveying IGM absorption line systems in numerous new
sight-lines. em Identifying
promising targets for observations with the future highly sensitive
Cosmic Origin Spectrograph.
endenumerate A 35-minute snapshot with exposures in either the G140L or
G230L will yield spectra with a
minimum S/N > 15 per resolution element at all wavelengths for all our
potential targets. This will
allow
us to be sensitive to absorption lines to a limiting equivalent width of
0.3 Angstrom at the 3 Sigma
level. In order to facilitate rapid observational followup, we waive the
data proprietary period
entirely.
STIS/CCD 9126
Galaxy Mass and the Fate of Luminous, Blue Compact Galaxies at z~0.6.
The Space Telescope Imaging Spectrograph (CCD) was used to obtain
long-slit spectra for a sample of 6
luminous, blue, compact galaxies {LBCGs} at z ~ 0.6. Despite being very
luminous, LBCGs have velocity
widths Sigma ~ 60 kms and half-light radii r_e ~ 0.5” {or R_e ~ 3Kpc}.
Small sizes and velocity
widths suggest LBCGs are low- mass stellar systems , while their blue
colors, strong emission lines and
low M/L-ratios indicate they are undergoing a major starburst. I f the
star-forming process halts
after the current burst, models predict that LBCGs will fade by ~2-4
magnitudes after a few Gyrs to
reach the low luminosities and surface brightnesses characteristic of
spheroidal galaxies.
STIS/CCD 9074
The Origin and Physics of Gamma-Ray Bursts.
The Space Telescope Imaging Spectrograph (CCD) was used to make
observations that will provide the most
stringent tests yet performed of the hypothesis that GRBs are powered
by the collapse of massive
stars. STIS CCD spectroscopy will be used to detect broad atomic
features of supernovae underlying GRB
optical transients, at flux levels more than a factor of three fainter
than SN 1998bw.
STIS/CCD/MA1 9184
A Survey for Missing Baryons in Highly Ionized Intergalactic Gas at Low
Redshift.
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe six additional low-z QSOs
with the STIS FUV E140M echelle mode {7 km s^-1 resolution}. Combined
with archival data, this will
increase the sample redshift path by a factor of ~7 compared to the
published data. With the echelle
data, we will {1} measure the number of O VI absorbers per unit redshift
{dN/dz} and their minimum
cosmological mass density with a limiting equivalent width of W_Lambda
~50 mAngstrom , {2} examine
whether the O VI absorption arises in photoionized, collisionally
ionized, or multiphase gas, and {3}
study the dependence of the O VI system properties on environment. In
addition to testing this
prediction regarding the location of the missing baryons, the data will
have applications to many other
topics such as low-z LyAlpha absorbers and the physical properties and
abundances of gas in the Milky
Way halo.
WFPC2 9334
Dynamical Masses of White Dwarfs from Resolved Sirius-Like Binaries
In Cycle 8 we initiated a WFPC2 snapshot survey for resolved,
“Sirius-like” systems containing hot
white-dwarf companions of cooler main-sequence stars. Out of 17 systems
observed to date, 8 have been
resolved with WFPC2 by using UV filters. Two of the resolved
systems—56 Persei and Zeta Cygni—have
predicted or known orbital periods short enough that dynamical masses
can be determined for the white
dwarfs within reasonable times. These would thus add to the extremely
small number of white dwarfs
presently having accurately and directly measured masses. We propose to
image them annually in the UV
with WFPC2. In addition, we will observe Zeta Cyg with FGS in order to
measure the absolute motion of
the optical component, needed for the mass solution. We also propose to
observe
Sirius itself with WFPC2 over the next 3 Cycles. The resulting
astrometric data will not only greatly
improve the precision of the binary orbit and the dynamical mass
measurements for both the
main-sequence and white-dwarf components, but will also test
definitively for the claimed presence of a
third body in this famous system.
WFPC2 9033
Measuring the mass distribution in the most distant, very X-ray luminous
galaxy
cluster known
We propose to obtain a mosaic of deep HST/WFPC2 images to conduct a weak
lensing analysis of the mass
distribution in the massive, distant galaxy cluster ClJ1226.9+3332,
recently discovered by us. At
z=0.888 this exceptional system is more X-ray luminous and more distant
than both MS1054.4-0321 and
ClJ0152.7-1357, the previous record holders, thus providing yet greater
leverage for cosmological
studies of cluster evolution. ClJ1226.9+3332 differs markedly from all
other currently known distant
clusters in that it exhibits little substructure and may even host a
cooling flow, suggesting that it
could be the first cluster to be discovered at high redshift that is
virialized. We propose joint HST
and Chandra observations to investigate the dynamical state of this
extreme object. This project will
1} take advantage of HST’s superb resolution at optical wavelengths to
accurately map the mass
distribution within 1.9 h^{-1} 50 Mpc via strong and weak gravitational
lensing, and 2} use Chandra’s
unprecedented resolution in the X-ray waveband to obtain independent
constraints on the gas and dark
matter distribution in the cluster core, including the suspected cooling
flow region. As a bonus, the
proposed WFPC2 observations will allow us to test the results by van
Dokkum et al. {1998, 1999} on the
properties of cluster galaxies {specifically merger rate and
morphologies} at z~0.8 from their HST
study of MS1054.4-0321.
WFPC2 9710
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
WFPC2 9709
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 paralell images of random areas of the sky, following the
recommendations of the 2002
Parallels Working Group.
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
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies:
(The following are preliminary reports of potential non-nominal
performance that will be investigated.)
HSTARs:
8995 – LOL during GSacq(2,3,3) @ 088/1733z
8996 – REacq(1,2,1) requires 2 attempts to achieve Finelock Data Valid @ 097/0419z
COMPLETED OPS REQs:
16940-0 – Clear NICMOS Error Log @ 108/1714z
OPS NOTES EXECUTED:
None
SCHEDULED SUCCESSFUL
FAILURE TIMES
FGS GSacq 22
22
FGS REacq 27
27
FHST Update 43
43
LOSS of
LOCK
SIGNIFICANT EVENTS: None
