NASA Hubble Space Telescope Daily Report # 3370 (part 2)

ACS 9583

The Great Observatories Origins Deep Survey: Imaging with ACS

We propose a Treasury program of ACS imaging as part of the Great
Observatories
Origins Deep Survey {GOODS}, covering 320{square}’, or 32* the area of
the two
original WFPC2 HDFs, to within 0.5–0.8 mag of their depth in four ACS
bands,
BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep
Field
South, are the premier deep survey areas from X– ray to radio
wavelengths. ACS
data will provide unique angular resolution, sensitivity, and wavelength
coverage to close the gap between the deepest Chandra and SIRTF
observations.
Supported by extensive imaging and spectroscopy from the VLT, Keck,
Subaru,
NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data
set will
make it possible to map the evolution of the Hubble sequence with
redshift,
reconstruct the history of galaxy mass assembly, star formation and
nuclear
activity from the epoch of reionization to the present, trace the growth
of
density perturbations via cosmic shear, and, with properly phased z–band
observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the
cosmic
acceleration and the presence of dark energy. All HST, SIRTF, Chandra,
and
supporting GOODS data are non– proprietary, with science–quality images
and
catalogs released on a timescale of months. This will constitute the
deepest,
largest, and most uniform panchromatic data set ever assembled to study
the
distant universe.

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 9379

Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the
Starburst-AGN
Connection

We propose a near-UV snapshot survey of 101 Seyfert galaxies using
ACS/HRC and
the filter F330W, a configuration which is optimal to detect faint star
forming
regions around their nuclei. These images will complement optical and
near-IR
images available in the HST archive, thus providing a panchromatic atlas
of the
inner regions of active galaxies, which we will use to study the
starburst-AGN
connection. The main goals of this proposal are: {1} Determine the
frequency of
circumnuclear starbursts in Seyferts, down to levels which cannot be
observed
from the ground; {2} characterize the observational {fluxes, colors,
structure,
sizes} and intrinsic {luminosities, masses, ages, global star-formation
rate}
properties of these clusters; {3} derive the luminosity functions of
young star
clusters around the nucleus of Seyferts and compare these results with
those
from normal and starburst galaxies to determine their survival rate close
to the
AGN; {4} address questions about the relation between AGNs and
starbursts, like
the possible connection between the masses and luminosities of black
holes and
starbursts, and the implications for the evolution of the black holes and
their
host galaxy bulges. By adding UV images to the existing optical and
near-IR
ones, this project will create an extremely valuable database for
astronomers
with a broad range of scientific interests, from the properties of the
AGN to
the properties of their host galaxies.

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/

ACS/WFPC2 9481

Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
Survey
Fields

In anticipation of the allocation of ACS high-latitude imaging survey{s},
we
request a modification of the default pure parallel program for those
WFPC2
parallels that fall within the ACS survey field. Rather than duplicate
the red
bands which will be done much better with ACS, we propose to observe in
the
near-ultraviolet F300W filter. These data will enable study of the
rest-frame
ultraviolet morphology of galaxies at 0<z<1. We will determine the
morphological
k-correction, and the location of star formation within galaxies, using a
sample
that is likely to be nearly complete with multi-wavelength photometry and
spectroscopic redshifts. The results can be used to interpret
observations of
higher redshift galaxies by ACS.

NICMOS 9402

A NICMOS Study of Merging Nuclei in the Toomre Sequence: Finding Order
Amid
Chaos

The final death throes of merging spiral galaxy nuclei are hidden behind
dusty
maelstroms of colliding gas clouds and glaring star formation activity.
The
dynamically important centers of mass can only be uncovered by imaging at
NIR
wavelengths and with the high spatial resolution of HST. We propose a
near-infrared imaging program to inspect the physical processes of
merging at
spatial scales of ~100 pc. The Toomre Sequence provides the best sample
of
merging galaxies for such a study, because it has been studied
extensively from
the ground, and the global properties are well understood. Our previous
Cycle 9
WFPC2 images of the nuclei have revealed a wealth of information on star
forming
activity and dust, but based on those data alone it is impossible to
determine
the locations of the current centers

of mass. Determining the mass centers and stellar density profiles is
important
for understanding both the kinematics and the dynamical evolution of the
nuclei,
and the formation of nuclear density cusps in galaxies. We propose J, H
and K
band imaging of the nuclei in early and intermediate stage mergers in the
Toomre
Sequence. Because of the much reduced effect of dust extinction, the
near-infrared images are also optimally suited to searches for nuclear
rings and
bars around the nuclei. Combined with our ongoing Cycle 9 program, these
data
will provide a detailed view of the structure and evolution of a sequence
of
merger nuclei.

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.

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 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 9431

Composition and history of Beta Pictoris- like circumstellar gaseous
disks

The gaseous parts of dust disks surrounding main sequence stars have been
the
subject of intense investigations since 1985. The origin of the gas
content was
a puzzle around such evolved stars. But the spectral signatures of Beta
Pictoris
led to the explanation that the gas is probably produced by the
evaporation of
many small bodies {see Lecavelier et al., 2001, Nature 412, 706}. It is
thus
believed that BetaPic-like disks are young planetary systems in the
clearing-out
phase. Our previous HST observations confirmed the presence of gas disks
similar
to the Beta Pic one. Here we propose new STIS observations of four stars
with
known circumstellar gas. Four main objectives can be achieved with STIS
observations: the determination of the composition of the gas, the
investigation
of the puzzling high ionization species, the determination of the CO and
CI
history and monitoring of spectral variability. The analysis of these
issues
will provide valuable clues to the origin of these gas disks and the
subsequent
evolution of young planetary systems. In particular, from abundance
studies it
will be possible to show if the gas is produced by evaporation of bodies
like
extra-solar comets.

STIS 9615

Cycle 11 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
noise. This
proposal will provide the primary means of checking on health of the MAMA
detectors systems through frequent monitoring of the background count
rate. The
purpose is to look for evidence of change in dark indicative of detector
problem
developing.

STIS 9604

STIS CCD Performance Monitor

This activity measures the baseline performance and commandability of the
CCD
subsystem. Only primary amplifier D is used. Bias and Flat Field
exposures are
taken in order to measure bias level, read noise, CTE, and gain. Numerous
bias
frames are taken to permit construction of "superbias" frames in which
the
effects of read noise have been rendered negligible. Full frame and
binned
observations are made, with binning factors of 2 x 1, 1 x 2, 2 x 2, 4 x
1,
and 4
x 2. Dark images are taken in 2×2 binning mode; 1×1 binning darks are
being
taken in the nominal CCD Dark Monitor. Bias frames are taken in subarray
readouts to check the bias level for ACQ and ACQ/PEAK observations. All
exposures are internals.

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/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 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 9596

WFPC2 CYCLE 11 INTERNAL MONITOR

This calibration proposal is the Cycle 11 routine internal monitor for
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.

WFPC2 9592

WFPC2 CYCLE 11 Standard Darks

This dark calibration program obtains dark frames every week in order 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.

WFPC2 9594

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3

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

WFPC2 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 9043: GS Acquisition (2,3,2) @ 145/22:25:46Z failed to RGA control
due to SRLE
on primary FGS 2; during a period of no data. The
guide star acquisition for
this observation was non-nominal, further analysis
will determine if a repeat
observation is required.

HSTAR 9044: GS Acquisition (2,1,1) @ 146/23:57:20Z resulted in FL backup
(2,0,2)
using FGS 2. FGS 1 started its walk down and got
as
far as CRTRK, then
just stopped. No flags were set and after playing
back the pickles display,
FGS 1 scanned out and did nothing. Under
investigation.

                         SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq             34                        33             (see HSTAR
9043)
FGS REacq             33                        33
FHST Update           54                        54
LOSS of LOCK

SIGNIFICANT EVENTS: None