HST Daily Report #3499

HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3499

PERIOD COVERED: DOYs 332-334

OBSERVATIONS SCHEDULED

ACS/HRC/WFC 9992

Essential Observations of SN 1987A

We request Director's discretionary time to avoid a gap in understanding the
development of SN 1987A just at the time when it is changing most rapidly 
from a
supernova into a supernova remnant. There will be no way to go back in time 
if we
fail to do this now. We would like 3 orbits to image SN 1987A in Cycle 12.

ACS/WFC 9991

The Orbit of a Newly Discovered Transneptunian Binary

We have recently discovered a binary companion to the transneptunian object
{TNO} 1999 RZ253. We are requesting rapid follow up observations during 
cycle 12
to make observations sufficient for a preliminary characterization of the
orbital period, semimajor axis, eccentricity, and inclination. In 
particular, it
is urgent to determine if this object is a candidate for observable mutual
events in the near future, a possibility that would greatly add to its
scientific interest. The study of TNBs is in a stage of explosive growth, 
fueled
in large part by the capabilities of HST that we seek to exploit.

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.

NIC/NIC3 9865

The NICMOS Parallel Observing Program

We propose to continue managing the NICMOS pure parallel program. Based on our
experience, we are well prepared to make optimal use of the parallel
opportunities. The improved sensitivity and efficiency of our observations will
substantially increase the number of line-emitting galaxies detected. As our
previous work has demonstrated, the most frequently detected line is Halpha at
0.7<z<1.9, which provides an excellent measure of current star formation rate.
We will also detect star-forming and active galaxies in other redshift ranges
using other emission lines. The grism observations will produce by far the best
available Halpha luminosity functions over the crucial--but poorly
observed--redshift range where galaxies appear to have assembled most of their
stellar mass. This key process of galaxy evolution needs to be studied with IR
data; we found that observations at shorter wavelengths appear to have missed a
large fraction of the star-formation in galaxies, due to dust reddening. We 
will
also obtain deep F110W and F160W images, to examine the space densities and
morphologies of faint red galaxies. In addition to carrying out the public
parallels, we will make the fully reduced and calibrated images and spectra
available on-line, with some ground-based data for the deepest parallel fields
included.

ACS/WFC 9860

ESSENCE: Measuring the Dark Energy Equation of State

The accelerating universe appears to be dominated by a dark energy with a
significant negative pressure. The ratio of the pressure to density of this
mysterious energy {its equation of state} is an observable which can
differentiate between the proliferating candidate theories. We propose to
estimate the dark energy equation of state by observing Type Ia supernovae at
redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey
program that is discovering and studying supernovae between 0.3<z<0.8. We show
that an interesting constraint on the equation of state can be made with
supernovae observed at modest redshifts given the current knowledge of the
matter density. We will follow 10 Type Ia supernovae discovered from the ground
and passed to HST without disrupting its schedule. The full data set will
constrain the equation of state to 10% and strictly limit the range of possible
dark energy models. In keeping with the ESSENCE policy, these observations will
available to the community immediately.

NIC2 9856

A near-IR imaging survey of submm galaxies with spectroscopic redshifts

Submillimeter {submm} surveys with SCUBA have identified a population of
obscured star-forming and active galaxies at high redshift. Our recent
spectroscopic campaigns with the Keck-10m telescope have uncovered 
redshifts for
37 SCUBA galaxies. The wide redshift range of the radio identified submm
population {z=1-4} implies that many varieties of sources driven by different
physical processes may be selected in a submm survey. Only HST observations
have the resolution to detect any changes in the morphologies of SCUBA galaxies
with increasing cosmic time. We propose to use HST-NICMOS, ACS to obtain
2-filter images of a sample of 15 SCUBA galaxies with redshifts spanning
z=0.8-3.5. Our goal is to understand what physical process {major mergers?}
drive their strong evolution and great luminosities, and what the implications
are for galaxy evolution models.

STIS/CCD 9838

The Upper End of the Supermassive Black Hole Mass Function: Pushing the 10
Billion Solar Mass Limit.

In 1994, HST provided the first secure detection of a supermassive black hole
{SBH} in a galactic nucleus. The galaxy was M87, the black hole almost 4 
billion
solar masses. Since then, two dozen additional SBH detections have been the
outcome of the several hundred orbits of HST time devoted to this cause. Yet,
M87's black hole is still the most massive known, and in only two other 
galaxies
have SBHs in excess of a billion solar masses been detected. The aim of this
proposal is to characterize the high mass end of the local SBH mass function.
Four brightest cluster galaxies have been carefully selected. Their large
masses, luminosites and stellar velocity dispersions, as well as their having a
merging history which is unmatched by galaxies in less crowded environments,
make these galaxies the most promising hosts of the most massive SBHs in the
local Universe. It is in the high mass regime that the unavoidable link between
the evolution of supermassive black holes and the hierarchical build-up of
galaxies leaves its clearest signature. It is these galaxies that are expected
to be the relicts of the most luminous high redshift quasars, those so
spectacularly targeted by the Sloan Digital Sky Survey. Expanding {and
extending} the high mass end of the local SBH mass function is the next
obligatory step we need to take to improve our understanding of how SBHs, and
their hosts, formed and evolved.

ACS/STIS/MA2 9829

HST / Chandra Monitoring of a Dramatic Flare in the M87 Jet

As the nearest galaxy with an optical jet, M87 affords an unparalleled
opportunity to study extragalactic jet phenomena at the highest resolution.
During 2002, HST and Chandra monitoring of the M87 jet have detected a dramatic
flare in knot HST-1 located ~1" from the nucleus. Its brightness has increased
ten-fold in the optical band, and continues to increase, and the X-rays show a
similarly dramatic outburst. In both bands this HST-1 now rivals the nucleus in
brightness. To our knowledge this is the first incidence of an optical or X-ray
outburst from a jet region which is spatially distinct from the core source;
this presents an unprecedented opportunity to study the processes responsible
for non-thermal variability and the X-ray emission. We propose four epochs of
HST/ACS monitoring during Cycle 12, as well as seven epochs of Chandra/ACIS
observation {5ksec each}. We also include a brief STIS observation that will be
used with prior STIS data to measure proper motions, and ACS polarimetry to map
the magnetic field structure. The results of this investigation are of key
importance not only for understanding the nature of the X-ray emission of the
M87 jet, but also for understanding flares in blazar jets, which are highly
variable, but where we have never before been able to resolve the flaring 
region
in the optical or X-rays. These observations will allow us to test synchrotron
emission models for the X-ray outburst, constrain particle acceleration and 
loss
timescales, and study the jet dynamics associated with this flaring component.

NIC3 9824

NIC3 SNAPs of nearby galaxies imaged in the mid-UV: the remarkable cool stellar
population in late-type galaxies.

We propose a NIC3 H-band {F160W} SNAPshot survey of 48 nearby mid- to late-type
galaxies covering all inclinations. In Cycle 9 and 10, we imaged ~100 galaxies
in the mid-UV {F300W/F255W} and I-band {F814W} with WFPC2, and obtained 
UBVR CCD
surface photometry from the ground. Early-mid-type galaxies show the usual 
small
radial color-gradients, where disks become somewhat bluer at larger radii. But,
remarkably, the majority of {lower luminosity, smaller and rounder} late-type
galaxies shows the opposite trend and becomes redder outwards in all filters.
While young UV/blue-bright stellar populations dominate their inner morphology,
most late-type galaxies must have a significant halo or thick disk of older
stars. Combining our proposed NIC3 H-band with existing WFPC2 images will span
the wavelength range 0.29-1.6 micron at resolutions of 0.04-0.16" {FWHM}. This
Panchromatic Nearby Galaxy Atlas will be applicable to a wide range of 
problems,
and will be made public immediately. Our NIC3/F160W science goals are to: {1}
Establish the nature of the old outer stellar population. All target galaxies
have z<0.005, allowing us to resolve any luminous, cool supergiant population.
NIC3 is essential to make a pixel-to-pixel color-magnitude study of the nature,
distribution and uniformity of the outer stellar populations, which will
constrain dwarf galaxy formation theories. {2} Determine galaxy structure at
5-20 pc resolution, tracing the old stellar population and mass distribution
compared to the star-forming regions seen in the mid-UV. A range of 
inclinations
is needed to distinguish between old thick disks or halos in late-type 
galaxies.
{3} Make a multi-wavelength pixel-to-pixel decomposition to help delineate the
effects of dust, age, and metallicity. Since we must cover a range of
inclinations, NIC3 H-band is essential to map the effects from dust, and 
see how
these may affect the studies of {1} and {2}.

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.

ACS/HRC/WFC/STIS/CCD 9767

Search for Black Holes in M31 Globular Clusters

Whether globular clusters contain a central massive black hole remains a very
controversial subject today, and yet is extremely important for theoretical
models for black hole and cluster formation. Furthermore, the existence of
intermediate-mass black holes has important implications for supermassive black
hole and galactic bulge formation, as well as providing signatures in
gravitational wave detectors. We propose to obtain high spatial resolution,
long-slit spectroscopy of two globular clusters in M31, G78 and G280. These two
clusters represent the best ones in which to constrain a central black hole.
Most importantly, both of these clusters have long central relaxation 
times, and
thus confusion between a central black hole and a collection of heavy stellar
remnants is alleviated. We have considered all globular clusters in our Galaxy
and in M31; STIS observations of these two will provide the strongest 
limits for
a black hole in any cluster, and better than the two claims made previously in
the literature. Combined with the data for G1, these three clusters have the
three highest central velocity dispersions for any cluster in the Local Group
and will shed light on possible connections between galaxy and globular cluster
formation.

STIS/MA1/MA2 9757

Abundances, Dust, and Physical Conditions in the LMC ISM

STIS echelle spectra of the SMC star Sk 155 have revealed patterns of gas-phase
interstellar abundances {and corresponding depletions into dust} that have not
been seen in the Galactic ISM. In particular, Mg and Si {generally thought 
to be
major dust constituents} are essentially undepleted in the SMC gas --- even for
components with severe depletions of Fe and Ni. We propose to obtain similar
spectra of 3 LMC stars --- sampling different regions of the LMC characterized
by different UV extinction curves --- first to see whether such "anomalous"
abundances might also be present in the LMC {as suggested by some FUSE spectra}
and then to explore the relationships between interstellar abundances,
depletions, physical conditions, and dust properties in environments
characterized by low metallicity and moderately strong radiation fields. These
would be the first extensive UV spectra of any LMC targets at resolutions 
better
than 6 km/s. The analysis of these spectra will have significant implications
for {1} making models of interstellar dust grains {which currently rely heavily
on silicates}; {2} understanding the relationships between depletions, 
dust, and
H_2 {which may be somewhat different in the Milky Way, LMC, and SMC}; {3}
understanding the processes affecting the ionization balance in diffuse
interstellar clouds {e.g., charge exchange with large molecules, cosmic-ray
ionization}; {4} testing theoretical cloud models {which predict higher
pressures in such environments}; and {5} interpreting the gas-phase abundances
observed for QSO absorption-line systems {which exhibit some similar
properties}.

ACS/WFC 9744

HST Imaging of Gravitational Lenses

Gravitational lenses offer unique opportunities to study cosmology, dark 
matter,
galactic structure, galaxy evolution and quasar host galaxies. They are 
also the
only sample of galaxies selected based on their mass rather than their
luminosity or surface brightness. While gravitational lenses can be discovered
with ground-based optical and radio observations, converting them into
astrophysical tools requires HST. HST has demonstrated that it is the only
telescope that can in each case precisely locate the lens galaxy, measure its
luminosity, color and structure, and search for lensed images of the source 
host
galaxy given the typical image separations of ~1''. We will obtain ACS/WFC 
V and
I images and NICMOS H images of 21 new lenses never observed by HST and 
NICMOS H
images of 16 lenses never observed by HST in the IR. As in previous cycles, we
request that the data be made public immediately.

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.

WFC 9689

The Impending Destruction of NGC 1427A

The Fornax cluster member NGC 1427A provides a spectacular example of a hot ICM
and cluster potential operating on a gas-rich irregular galaxy. On its first
passage through the cluster core, NGC 1427A is being disrupted by the influence
of the hot ICM, its own vigorous star formation, and the cluster tidal 
field. We
propose joint Chandra/HST imaging of this x-ray source to explore the 
details of
the impending galaxy destruction. Such events are common in the lives of
clusters, and help build the intracluster components. NGC 1427A provides a
snapshot of the progenitor ingredients about 1 Gyr prior to becoming true
intracluster material, and a chance to study the forces which shred 
galaxies and
build cluster gas and stellar components over a Hubble time

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.

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.

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/

STIS 9435

Systematic Search for Rotation at the Base of Outflows from T Tauri Stars

We wish to search for rotation signatures in the initial portion {first 100 AU}
of a sample of outflows emanating from T Tauri stars {TTSs}. This project
originates from our detection of systematic transverse radial velocity 
shifts in
STIS spectra of the DG Tau jet {Bacciotti et al., 2002}. The shifts, 
observed in
a region where the flow is already collimated, but has not yet manifestly
interacted with its environment, are consistent with the predictions of 
magneto-
centrifugal launching models, and may constitute the first observed indication
for rotation in the initial portion of a jet flow. Rotation is a fundamental
ingredient in star formation theories, thus we propose to confirm the above
result by carrying out a systematic survey in similar flows. We plan to 
take for
each jet a STIS spectrum in the 6300 -- 6800 Angstrom range, with the slit
perpendicular to the flow direction and at a distance of about 0.''3 from the
source {i.e., in our targets, 40 -- 70 AU along the jet depending on 
inclination
angle}. Since the flows are resolved transversely with HST, the proposed slit
orientation allows for the direct detection of systematic velocity shifts. 
Where
found, we will check for consistency between the sense of rotation observed and
that of the underlying disk through CO interferometric measurements. As a
by-product, estimates of the excitation conditions across the flow {including
ionization fraction} and of the mass outflow rates will be derived.

NICMOS 8790

NICMOS Post-SAA calibration - CR Persistence Part 1.

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.

WFPC2 10069

WFPC2 CYCLE 12 Supplemental Darks, Part 1/3

This dark calibration program obtains 3 dark frames every day to provide data
for monitoring and characterizing the evolution of hot pixels.

ACS/HRC/WFC 10048

Stability of the ACS CCD: Flat fielding, Photometry, Geometry

This program will verify that the low frequency flat fielding, the photometry,
and the geometric distortion are stable in time and across the field of view of
the CCD detectors. A moderately crowded stellar field, located ~6' West of the
center of the cluster 47 Tuc, is observed every three months with the WFC and
HRC using the full suite of broad and narrow band filters. The same field has
been observed during SMOV to derive low frequency corrections to the ground
flats and to create a master catalogue of positions and magnitudes from 
dithered
observations of the cluster. In Cycle 11, this field was observed again using
single pointings at various roll angles. The positions and magnitudes of 
objects
are used to monitor local and large scale variations in the plate scale and the
sensitivity of the detectors. The Cycle 12 program will continue to monitor
these effects and will derive an independent measure of the detector CTE.

ACS/HRC/WFC 10042

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.

STIS/CCD 10019

CCD Bias Monitor - Part 1

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.

STIS/CCD 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.

STIS/CCD 10000

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during cycle 12.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)

HSTAR 9221:  GS Acquisition (2,1,2) @ 332/17:36:35Z ended in FL backup (2,0,2)
                       on FGS 2 due to SSLE on FGS 2 @ 332/17:39:43Z. Under 
investigation.

COMPLETED OPS REQs: None

OPS NOTES EXECUTED:
1174-0 - Adjust ACS Error Count Limit (closed; ACS to BOOT) @ 335/0526z

                           SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq               23                        23
FGS REacq               15                        15
FHST Update             47                        47
LOSS of LOCK



SIGNIFICANT EVENTS: None


Jacques :-)

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