NASA Hubble Space Telescope Daily Report # 3413
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3413
PERIOD COVERED: DOYs 206-208
OBSERVATIONS SCHEDULED
ACS 9482
ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES}
Ly-alpha line emission is an efficient tool for identifying young galaxies
at
high redshift, because it is strong in galaxies with young stars and little
or
no dust — properties expected in galaxies undergoing their first burst of
star- formation. Slitless spectroscopy with the ACS Wide-Field Camera and
G800L
grism allows an unmatched search efficiency for such objects over the
uninterrupted range 4 <~ z <~ 7. We propose the ACS Pure Parallel Ly-alpha
Emission Survey {“APPLES”}, to exploit this unique HST capability and so
obtain the largest and most uniform sample of high redshift Ly-alpha
emitters
yet. Parallel observations will allow this survey to be conducted with
minimal
impact on HST resources, and we will place reduced images and extracted
spectra
in the public domain within three months of observation. We aim to find ~
1000
Ly-alpha emitters, 5 times the biggest current sample of Ly-alpha emitters.
This
unprecedented sample will provide robust statistics on the populations and
evolution of Ly-alpha emitters between redshifts 4–7; a robust measurement
of
the reionization redshift completely independent of the Gunn-Peterson
trough;
spatial clustering information for Ly-alpha emitters which would let us
probe
their bias function and hence halo mass as a function of redshift; many
galaxies
at redshift exceeding 6; and lower redshift serendipitous discoveries.
ACS 9674
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 9984
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 9427
Globular Cluster Systems in Supergiant E Galaxies
The 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 9831
Multiplicity among brown dwarfs in the Pleiades cluster
We have compiled a sample of 32 confirmed brown dwarfs in the Pleiades
cluster.
We propose to observe this sample with HST/ACS in SNAPSHOT mode in order to
search for very low mass multiple systems. Our goals are: 1} to determine
the
occurrence and frequency of binary systems among substellar objects, which
hold
important clues to the formation and evolution mechanism{s} of ultracool and
brown dwarfs, 2} to get an estimate of the Initial Mass Function {IMF} at
very
low masses, which is still unknown and very much needed to be corrected for
binarity, 3} to compare the distribution of multiple systems in young open
clusters and in the field.
ACS/HRC 9747
An Imaging Survey of the Statistical Frequency of Binaries Among
Exceptionally-Young Dynamical Families in the Main Asteroid Belt
We propose an ambitious SNAPSHOT program to determine the frequency of
binaries
among two very young asteroid families in the Main Belt, with potentially
profound implications. These families {of C- and S-type} have recently been
discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical
modeling,
to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events.
This
is the first time such precise and young ages have been assigned to a
family.
Main-belt binaries are almost certainly produced by collisions, and we would
expect a young family to have a significantly higher frequency of binaries
than
the background, because they may not yet have been destroyed by impact or
longer-term gravitational instabilities. In fact, one of the prime
observables
from such an event should be the propensity for satellites. This is the
best way
that new numerical models for binary production by collisions {motivated
largely
by our ground-based discoveries of satellites among larger asteroids}, can
be
validated and calibrated. HST is the only facility that can be used to
search
for binaries among such faint objects {V>17.5}. We will also measure two
control
clusters, one being an "old" family, and the other a collection of
background
asteroids that do not have a family association, and further compare with
our
determined value for the frequency of large main-belt binaries {2%}. We
request
visits to 180 targets, using ACS/HRC.
ACS/HRC 9746
Binary systems in the Kuiper Belt
The properties of the orbits of Kuiper belt object {KBO} satellites hold
keys to
fundamental insight into masses and densities of KBOs, the interaction
history
of the early solar system, the internal structure of distant ice-rock
bodies,
and even the genesis of the Pluto-Charon binary. Within the past 18 months,
9
KBO satellite systems have been discovered, allowing for the first time the
possibility of characterizing a sample of KBO satellite orbital properties.
We
propose HRC observations to determine satellite orbits in the 6 best cases.
We
have carefully devised a strategy for each of these 6 systems to make
maximum
use of ground-based observations, previous HST observations, and the
smallest
possible number of new HST observations. Our proposed observations will
efficiently provide highly reliable orbital solutions which are critical to
achieving the scientific promise available from the study of these systems.
Our
strategy relies heavily on extensive Monte Carlo simulations to define
optimal
times of observing such that each new point obtained gives maximum leverage
for
refining the orbital solution. We find that with this strategy we can
provide
mass solutions for all 6 systems to an accuracy of better than 10% using
only 25
new HST observations. This highly efficient program provides extreme
scientific
output with optimal use of scarce resources.
ACS/HRC 9361
Searching for Primeval Galaxies: the promising case of SBS 1415+437
Do primeval galaxies exist in the local Universe? The best candidates are
extremely metal-poor {Z < 1/20 Zo} blue compact dwarf {BCD} galaxies whose
photometric and chemical properties are consistent with a stellar population
younger than 100 Myr. SBS 1415+437 {Z = 1/21 Zo} is the closest candidate:
its
proximity {d = 11.4 Mpc}, detailed spectroscopic knowledge of its HII
regions
and low metal content, used to infer the primordial He^4 abundance, make it
the
best target for this investigation. We propose to take deep exposures of SBS
1415+437 with the ACS in the F814W and F606W filters. This instrument has
resolution and magnitude limits allowing us to reach and resolve with the
required accuracy individual stars 1 mag below the tip of the red giant
branch
{RGBT}. If present, these stars will provide a clear sign of an old stellar
population {with ages > 1 Gyr} and an independent distance indicator. If
absent,
this will unambiguously show that the system has started to form stars only
recently and can be considered the first robust case of local primeval
galaxy.
We propose to take exposures in the F658N {HAlpha Lambda6563} and FR505N
{HBeta
Lambda4861} filters to study the morphology of the ionized gas through
HAlpha
emission and map the dust content with the HAlpha/HBeta ratio in order to
solve
the age-dust degeneracy of the photometry by constraining reddening effects.
ACS/WFC 9891
A snapshot survey of rich stellar clusters in the Large and Small Magellanic
Clouds
Rich stellar clusters are vital to a wide variety of astrophysical 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.
ACS/WFC 9902
The Evolution of the Host Galaxies of Radio-Quiet Quasars
Study of the host galaxies and environments of high redshift AGN is proving
a
valuable probe of current theories of how galaxies form and evolve. Results
from
our NICMOS imaging program have indicated that the hosts of z ~ 2 — 3 faint
radio-quiet quasars {RQQ} have luminosities only around local L*, making
them
similar to Lyman-break field galaxies at the same redshifts, and to the
low-z
hosts RQQ hosts. This is roughly consistent with theoretical predictions of
Kauffmann & Haehnelt {2000} for the hierarchical buildup of galaxy hosts and
their relation to their resident supermassive black holes. The luminosity
of the
AGN in these RQQ is key to understanding this relationship, however, and we
are
making a comprehensive archival HST imaging study of the hosts of RQQs from
low
to high z at a range of nuclear luminosities. At intermediate z, however,
there
are no studies of the hosts of RQQs in the faint luminosity range that
represents the bulk of the quasar population. In the present proposal, we
request imaging at the same rest-wavelengths as our high-z sample of the
hosts
of 10 similarly luminous RQQs at z ~ 0.9. These data will fill in an
important
part of the parameter space defined by quasar luminosity and redshift.
Combined
with existing HST data they will allow us to trace the evolution of the
hosts of
RQQ and that of the relationship between quasar luminosity and host galaxy
luminosity.
ACS/WFC/HRC 9905
The Host Galaxies of Type II Quasars
Type II quasars are the luminous analogues of Type II Seyferts; the central
engines are presumably heavily obscured by dust. We have defined a sample of
9
highly luminous Type II quasar candidates with 0.24 < z < 0.40 from the
spectroscopic data of the Sloan Digital Sky Survey, which have high
equivalent
width, narrow emission-line spectra characteristic of a nonthermal
continuum. We
estimate that the obscured AGN in these objects have optical luminosities of
order 10^{12} solar luminosities. We propose to image this sample in
rest-frame
U, B and V, to determine the morphology and color of the host galaxies, and
look
for recent star formation. We will also probe the extended environments of
these
objects, to determine whether they are undergoing interactions with close
companions, and whether they live in appreciably clustered environments.
FGS 9971
FGS Astrometry of a Star Hosting an Extrasolar Planet: The Mass of Upsilon
Andromedae d
We propose observations with HST/FGS to determine the astrometric elements
{perturbation orbit semimajor axis and inclination} produced by the
outermost
extra-solar planet orbiting the F8V star Upsilon Andromedae. These
observations
will permit us to determine the actual mass of the planet by providing the
presently unknown sin i factor intrinsic to the radial velocity method which
discovered this object. An inclination, i = 30degrees, within the range of
one
very low precision determination using reanalyzed HIPPARCOS intermediate
data
products, would produce the observed radial velocity amplitude, K = 66 ms
with a
companion mass of ~8 M_Jupiter. Such a mass would induce in Upsilon
Andromedae a
perturbation semi-major axis, Alpha = 0arcs0012, easily within the reach of
HST/FGS fringe tracking astrometry. The proposed observations will yield a
planetary mass, rather than, as previous investigations have done, only
suggest
a planetary mass companion.
NIC2 9801
Are OH/IR Stars the Youngest post-AGB stars? A NICMOS Imaging Survey
Essentially all well-characterized preplanetary nebulae {PPNe}– 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
are
conducting a multiwavelength survey program of imaging and spectroscopic
observations of such objects, using a large, morphologically unbiased sample
selected using IRAS 12-to-25 micron colors. Our ongoing HST/SNAP imaging
survey
of the optically bright half of this sample with WFPC2 and ACS is highly
successful: 19/32 objects observed are extended with bipolar/multipolar
shapes
{remaining objects are unresolved}. Slightly more than 50% of our sample are
optically too faint or undetected but have strong near-IR counterparts — we
therefore propose a NICMOS SNAPshot imaging survey of these optically-faint
OH/IR stars. These observations are crucial for determining how and when the
bipolar geometry asserts itself. The results from our NICMOS survey
{together
with the WFPC2/ACS survey} will allow us to draw general conclusions about
the
onset of bipolar mass-ejection during late stellar evolution. 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 PPNe, are common or rare
phenomena.
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/STIS CCD 9405
The Origin of Gamma-Ray Bursts
The rapid and accurate localization of gamma-ray bursts {GRBs} promised by a
working HETE-2 during the coming year may well revolutionize our ability to
study these enigmatic, highly luminous transients. We propose a program of
HST
and Chandra observations to capitalize on this extraordinary opportunity. We
will perform some of the most stringent tests yet of the standard model, in
which GRBs represent collimated relativistic outflows from collapsing
massive
stars. NICMOS imaging and STIS CCD spectroscopy will detect broad atomic
features of supernovae underlying GRB optical transients, at luminosities
more
than three times fainter than SN 1998bw. UV, optical, and X-ray spectroscopy
will be used to study the local ISM around the GRB. Chandra spectroscopy
will
investigate whether the GRB X-ray lines are from metals freshly ripped from
the
stellar core by the GRB. HST and CTIO infra-red imaging of the GRBs and
their
hosts will be used to determine whether `dark’ bursts are the product of
unusually strong local extinction; imaging studies may for the first time
locate
the hosts of `short’ GRBs. Our early polarimetry and late-time broadband
imaging
will further test physical models of the relativistic blast wave that
produces
the bright GRB afterglow, and will provide unique insight into the influence
of
the GRB environment on the afterglow.
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 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 9708
STIS Pure Parallel Imaging Program: Cycle 11
This is the default archival pure parallel program for STIS during cycle 11.
STIS 9786
The Next Generation Spectral Library
We propose to continue the Cycle 10 snapshot program to produce a Next
Generation Spectral Library of 600 stars for use in modeling the integrated
light of galaxies and clusters. This program is using the low dispersion UV
and
optical gratings of STIS. The library will be roughly equally divided among
four
metallicities, very low {[Fe/H] lt -1.5}, low {[Fe/H] -1.5 to -0.5},
near-solar
{[Fe/H] -0.3 to 0.1}, and super-solar {[Fe/H] gt 0.2}, well-sampling the
entire
HR-diagram in each bin. Such a library will surpass all extant compilations
and
have lasting archival value, well into the Next Generation Space Telescope
era.
Because of the universal utility and community-broad nature of this venture,
we
waive the entire proprietary period.
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/MA1/CCD 9464
Exploring the Role of Acoustic Heating in Cool Dwarfs and Subgiants
Recent observations cast doubt on the importance of acoustic waves for
chromospheric heating in stars. These include low upper limits to their
contribution to upper layers of the solar chromosphere, and evidence for
significant magnetic heating contribution even in “basal" activity stars.
These
findings contradict the widely accepted picture that acoustic heating
accounts
for a significant fraction, the “basal component”, of chromospheric
heating in
inactive stars. To help resolve this issue, we propose to observe two very
inactive stars with significantly different properties to search for
specific
signatures of upward propagating acoustic waves: blue-shifts and enhanced
blue
wings in chromospheric lines. Solar data show that the degree of blue-shift
can
be used to estimate the acoustic contribution to chromospheric heating. We
will
compare the data to HST spectra of similar stars, and solar spectra from the
SUMER instrument on SOHO. Lack of a significant acoustic signature in our
targets would indicate that magnetic heating generated by a local
{turbulent,
non-cycling} dynamo is responsible for the basal component of chromospheric
heating in inactive stars. Our targets may be in a phase analogous to the
solar
Maunder minimum, and the HST spectra might serve as a proxy for the solar
spectrum in this state. The spectra will also be used for emission measure
analysis differentially between the Sun and solar-like stars.
STIS/MA2 9474
Intriguing Transient Sources in M87
We have found a remarkable number of transient point sources in M87. Within
the
jet itself we have observed dramatic changes in less than a year. The point
sources are seen well in the bluest regions of the spectrum, where we obtain
high spatial resolution, are free from cosmic ray artifacts and obtain
excellent
discrimination against the underlying old, red galaxy. They display a
variety of
unusual properties: one is brighter than any in the catalogue of novae in
M31;
several are very close to the jet; another hints at rapid variability. We
propose to investigate the population of transient sources in M87 and to
probe
the intrinsic jet variability on short timescales by taking images in the
near
UV. Do the sources show nova-type light curves? Is there a
decline-rate/luminosity relation? If yes, may we use it for distance
estimation,
as in Galactic novae, and hence constrain the still very important Virgo
distance. Are there very rapidly varying sources, flare stars or
gravitational
lenses? Is the variable stellar population related to the excess globular
cluster frequency in M87? Is there a population of flickering objects in and
around the jet, which may be responsive emission arising from their close
proximity to a BL Lac nucleus {viewed down the jet axis}? Can we find
variability in the jet itself indicative of light week length scales?
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 parallel images of random areas of the sky,
following the recommendations of the 2002 Parallels Working Group.
WFPC2 9595
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3
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.)
HSTAR 9097: GS Acquisition (2,3,3) @ 208/10:21:14Z required two attempts
to achieve FL
on FGS 2 due to SSLE. GS Re-acquisition was
successful on 2nd attempt.
Under investigation.
COMPLETED OPS REQs: NONE
OPS NOTES EXECUTED: NONE
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 24 24
FGS REacq 20 20
FHST Update 62 62
LOSS of LOCK
SIGNIFICANT EVENTS:
Completed Load, Uplink, Dump and Compare testing 206/11:04Z – 14:05Z using
CCS "B" String
with Release 4.0.3 and PRD O06100R1T. Successfully verified ground system
processing of
loads and dumps. The SOC is investigating a configuration issue concerning
missing bits
during the compare process of the hardware and software loads.
HST Command Timing test, Day 1 of 2, scheduled 209/11:00Z – 20:00Z with
GDOC, SOC, HITT,
and CCS using CCS "C" String with CCS Release 4.0.2 and PRD S07200. The
purpose of this
testing is to verify platform releases for SIMSS replacement of OS2 PTP.
