HST Daily Report # 3312
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3312
PERIOD COVERED: DOY 63
OBSERVATIONS SCHEDULED
NICMOS 8791
NICMOS Post-SAA calibration – CR Persistence Part 2
A new procedure proposed to alleviate the CR-persistence problem of
NICMOS.
Dark
frames will be obtained immediately upon exiting the SAA contour 23, and
every
time a NICMOS exposure is scheduled within 50 minutes of coming out of
the SAA.
The darks will be obtained in parallel in all three NICMOS Cameras. The
POST-SAA
darks will be non-standard reference files available to users with a
USEAFTER
date/time mark. The keyword ‘USEAFTER=date/time’ will also be added to
the
header of each POST-SAA DARK frame. The keyword must be populated with
the
time,
in addition to the date, because HST crosses the SAA ~8 times per day so
each
POST-SAA DARK will need to have the appropriate time specified, for users
to
identify the ones they need. Both the raw and processed images will be
archived
as POST-SAA DARKSs. Generally we expect that all NICMOS
science/calibration
observations started within 50 minutes of leaving an SAA will need such
maps to
remove the CR persistence from the science images. Each observation will
need
its own CRMAP, as different SAA passages leave different imprints on the
NICMOS
detectors.
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.
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 9409
The Evolution of Globular Cluster Systems in Merger Remnants
Mergers seem to have played a major role in determining the shapes and
dynamics
of elliptical galaxies. A few galactic mergers still occur and offer
valuable
clues to past evolutionary processes. Globular clusters formed during
mergers
are crucial probes for age-dating such events, and help shed light on the
process of cluster formation and evolution. With young globulars in
ongoing
mergers now well studied, we propose to make deep ACS observations of
intermediate-age globular clusters in two bona fide ellipticals: NGC 1316
and
3610. These ellipticals have line-strength indices, UBV colors, and fine
structure indicative of their being 2 — 4 Gyr old merger remnants. Past
HST+WFPC2 observations have shown that they also possess significant
numbers of
intermediate-age globulars as part of their bimodal cluster populations.
We
plan
to use the new HST+ACS observations to {1} measure high-accuracy BVI
colors for
clusters up to ~ 2 — 3 mag fainter than ever before, {2} use these
colors to
separate first- and second-generation clusters, and {3} determine the
luminosity
functions of the two kinds of clusters to 3 — 4 mag past the peak for
old
globulars. Deep dithered BVI images form a crucial part of our observing
strategy. This program should permit—for the first time—to directly
detect
the predicted evolution of the cluster luminosity function from a power
law for
young clusters to the Gaussian distribution typical of old globulars.
ACS 9463
Are OH/IR stars the youngest post-AGB stars? An ACS SNAPshot imaging
survey
Essentially all well-characterized preplanetary nebulae {PPNs}– 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
propose an ACS/SNAPshot imaging survey of a large, morphologically
unbiased
sample of these objects, selected using their IRAS 12-to-25micron colors.
Our
ground-based imaging study of OH/IR stars has revealed a few compact
bipolar
objects, supporting our hypothesis. However since most objects remain
unresolved, HST observations are needed to determine how and when the
bipolar
geometry asserts itself. 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 PPNs, are common or rare phenomena.
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 < z pl 7. We
request ACS parallel observations of duration more than one orbit at high
galactic latitude to identify ~ 300 HAlpha emission-line galaxies at
0.2 pl
z pl
0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3 pl z pl 1.68, and
pg
1000 Ly-alpha emission-line galaxies at 3 pl z pl 7 with total emission
line
flux f pg 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.
STIS 9469
NGC 4303: A Seyfert 2 nucleus powered by stars?
NGC 4303 is to date the best example of the claimed starburst- AGN
connection.
HST images have unveiled the existence of an unresolved {size <= 4 pc}
UV-optical-NIR bright core connected with a star-forming spiral {radius ~
250
pc}. The STIS UV spectrum of the core shows prominently the
characteristic
broad
absorption lines produced by the winds of massive young stars, and it is
best
fitted with the synthesised spectrum of a massive, young {<= 5 Myr}
stellar
cluster. Ground-based optical spectra of the nucleus containing the
bright
core,
place it at the borderline of low-excitation Seyfert 2 and LINER nuclei.
STIS
0.1^” slit spectroscopy of the unresolved core is requested to obtain an
unambiguous AGN classification of it, and to measure its enclosed mass,
i.e.
determine the presence and mass of the black-hole. In addition, the
spectra
will
be combined with evolutionary spectral synthesis and photoionization
models to
quantify the relative AGN and stellar energy contributions. If the
Seyfert
classification is confirmed, NGC 4303 will be the first ever detected
galaxy
with a Seyfert nucleus where the ionizing and bolometric energy output of
its
core {size <= 4 pc} could be dominated by a massive stellar cluster of
young
stars, as implied by the STIS UV spectrum. NGC 4303 will also be one of
the few
Seyferts for which the mass enclosed within the inner few pc would have
been
determined independently from stellar and gas kinematics.
ACS 9475
ACS coronagraphic survey for debris disks around nearby stars
We propose a comprehensive imaging survey of nearby stars that will
realize the
full potential of the ACS coronagraph to map debris disks, the extrasolar
analogs of our Kuiper Belt. Most debris disks are detected only by excess
thermal emission at far-infrared wavelengths. Because they have a factor
of 100
less dust cross section than the young debris disks around HR 4796A and
beta
Pic, they are undectable by present techniques. In simulations of disk
detectability, Kalas and Jewitt {1996} determined that detecting the
scattered
light from the disk requires at least two orders of magnitude of
supression of
the central PSF than is attainable from the ground. The ACS coronagraph
finally
provides this increase in sensitivity, surpassing the WFPC2 sensitivity
to
faint
nebulosity near bright stars by at least three orders of magnitude.
Mapping the
debris around stars is particularly important for the indirect detection
of
planet-mass objects. Dynamical models have shown that unseen perturbers
dynamically modify the radial, azimuthal and vertical structure of debris
disks.
These data will provide the critical high-resolution mapping of debris
disks.
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 9484
The NICMOS Parallel Observing Program
We propose to manage the default set of pure parallels with NICMOS. Our
experience with both our GO NICMOS parallel program and the public
parallel
NICMOS programs in cycle 7 prepared us to make optimal use of the
parallel
opportunities. The NICMOS G141 grism remains the most powerful survey
tool for
HAlpha emission-line galaxies at cosmologically interesting redshifts. It
is
particularly well suited to addressing two key uncertainties regarding
the
global history of star formation: the peak rate of star formation in the
relatively unexplored but critical 1<= z <= 2 epoch, and the amount of
star
formation missing from UV continuum-based estimates due to high
extinction. Our
proposed deep G141 exposures will increase the sample of known HAlpha
emission-
line objects at z ~ 1.3 by roughly an order of magnitude. We will also
obtain a
mix of F110W and F160W images along random sight-lines to examine the
space
density and morphologies of the reddest galaxies. The nature of the
extremely
red galaxies remains unclear and our program of imaging and grism
spectroscopy
provides unique information regarding both the incidence of obscured star
bursts
and the build up of stellar mass at intermediate redshifts. In addition
to
carrying out the parallel program we will populate a public database with
calibrated spectra and images, and provide limited ground- based optical
and
near-IR data for the deepest parallel fields.
STIS 9506
A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS
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.
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
CAL/WF2 9597
Intflat Sweep, Visflat Sweep, and Filter Anomaly Check
No abstract available.
WFPC2 9599
WFPC2 Cycle 11 UV Earth Flats
Monitor flat field stability. This proposal obtains sequences of earth
streak
flats to improve the quality of pipeline flat fields for the WFPC2 UV
filter
set. These Earth flats will complement the UV earth flat data obtained
during
cycles 8-10.
STIS 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9607
CCD Bias Monitor – Part 1
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 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 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 9657
ACS Internal Flat Field Stability
The flat field stability and characterization obtained during the ground
calibration and SMOV phases will be tested and verified through a
sub-sample of
the filter set. Only internal exposures with the calibration lamps will
be
required.
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 9673
CCD Daily Monitor
for any source of noise in ACS CCD detectors. This programme will be
executed
once a day for the entire lifetime of ACS
WFPC2 9676
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.
NICMOS 9702
NICMOS Parallel Thermal Background
NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to
establish the stability of the HST+NCS+Instrument thermal emission. This
data
will be compared against the already available Camera 3 measurements in
F222M
which show an increased thermal background.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.) None
COMPLETED OPS REQs: None
OPS NOTES EXECUTED:1081-0 Adjust Software Main Bus Current, Red Limit
@064/1643z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 13 13
FGS REacq 5 5
FHST Update 25 25
LOSS of LOCK
SIGNIFICANT EVENTS:
On-Line Data Archive test 3/4/2003. The Online Data Archive test was
completed
successfully. The test was executed in the OPS account to ensure required
data
was available. All objectives were met and all requests performed as
expected.
No TSARs or CRs were written.
CCS 4.0.2 Source/Destination Codes test performed 3/4/2003. The test was
successful. All destination codes were verified along with the source
ID in both GSTDN and JSC single stage modes.
Engineering Data Products Test for CCS 4.0.1. Historical requests were
submitted on G- string (CCS 4.0.2). Plots and reports were generated
for a 24-hour time span and compared against plots and reports generated
on A-string (CCS 4.0.1) for the same time period. The comparison
revealed
no significant differences for either the plots or the reports.
