NASA Hubble Space Telescope Daily Report # 3553
HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science
DAILY REPORT # 3553
PERIOD COVERED: DOY 48
OBSERVATIONS SCHEDULED
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/HRC/WFC 10059
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/WFC 10055
ACS Polarization Calibration
This proposal aims to address several specific issues for the polarization
calibration: {1} variations in calibration with position on the detector
{field
dependence}, {2} dependence on telescope roll-angle relative to the target,
{3}
orientation of the polarizer axes, and {4} geometric distortion contributed
by
the polarizers.
ACS/WFC 9892
H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star
Formation in a Dusty Universe
Previous studies of nearby galaxies show large discrepancies between
different
star formation {SF} indicators on large {>100 pc, or even global} scales:
the
strikingly complex interplay of young stars, dust and ionized gas are the
primary cause of this variance. The few galaxies in the HST Archive with
both
WFPC2 H-alpha and mid-UV {F255W or F300W} imaging show this complex geometry
extending down to <10 pc scales. We propose a SNAPshot survey in the ACS/WFC
H-alpha filter of 48 galaxies of all Hubble types, that are nearby but
beyond
the Local Group, and that were previously imaged with WFPC2 in the mid-UV
and in
F814W. We aim to provide a benchmark for understanding the SF processes in
both
normal and star-bursting galaxies, at spatial resolutions unattainable from
the
ground for a large and varied galaxy sample. These data can be applied to a
wide
range of astrophysical problems and will, therefore, be made public
immediately.
Our science goals are to: {1} spatially resolve the dust clouds and
filaments
which strongly affect mid-UV and H-alpha derived SF rates, {2} test how the
large-scale correlation between H-alpha and mid-UV flux breaks down on pc
scales, and {3} model the propagation of star formation by comparing the SF
over
time scales of ~100 Myr {via mid-UV} and ~5 Myr {via H-alpha}. This will {4}
significantly improve our insight into, and calibration of SF in UV-bright
galaxies at high z, and into the cosmic SF history.
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 9879
An Astrometric Calibration of the Cepheid Period-Luminosity Relation
We propose to measure the parallaxes of 10 Galactic Cepheid variables. There
is
no other instrument on or off the earth that can consistently deliver HST
FGS
level of precision for critical parallaxes. When these parallaxes {with
1-sigma
precisions of 10% or better} are added to our recent HST FGS parallax
determination of delta Cep {Benedict et al 2002}, we anticipate determining
the
Period-Luminosity relation zero point with a 0.03 mag precision. In addition
to
permitting the test of assumptions that enter into other Cepheid distance
determination techniques, this calibration will reintroduce Galactic
Cepheids as
a fundamental step in the extragalactic distance scale ladder. A
Period-Luminosity relation derived from solar metallicity Cepheids can be
applied directly to extragalactic solar metallicity Cepheids, removing the
need
to bridge with the Large Magellanic Cloud and its associated metallicity
complications.
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.
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 9414
Resolved halo stellar populations in the Milky Way analogue edge-on galaxy
NGC
891
The stellar halo is one of the fundamental building blocks of galaxies.
Although
ground-based surface photometry has shown that stellar halos exist in some
spiral galaxies, with colours similar to those of the main disk, little else
is
known about their stellar populations. We propose to carry out a systematic
study of the halo regions of the edge-on galaxy NGC 891. The resulting deep
colour-magnitude diagrams will be used to infer the mean metallicity of the
bright halo giants at the tip of the RGB and below, and its metallicity
spread.
Recently, Zepf et al. {2000} inferred that the halo metallicity of NGC 5907
has
to be low {Fe/H <= -1.7}, with a large stellar M/L ratio. We will be able to
test this hypothesis with much better and deeper data. If we can confirm a
similar halo composition in NGC 891, this would imply that the Milky Way
halo
might be very different from external halos. Since galactic halos trace the
history of galaxy formation, this will have important implications for our
understanding of galactic evolution on cosmological time scales. Using these
survey data, we will be able to conclusively distinguish between genuine
halo
objects and merger remnants, without having to assume a scenario in which
the
halo field population is fully mixed. Surprisingly, such studies have not
yet
been undertaken for NGC 891, although the galaxy is a prime Milky Way
analogue.
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/CCD 10017
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD.
STIS/CCD 10019
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/CCD 10023
STIS CCD Spectroscopic Flats C12
Obtain CCD flats on the STIS CCD in spectroscopic mode
STIS/CCD 10024
STIS CCD Imaging Flats C12
Investigate flat-field stability over a bimonthly period.
STIS/CCD 10085
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during cycle 12.
WFPC2 10067
WFPC2 Cycle 12 Decontaminations and Associated Observations
This proposal is for the monthly WFPC2 decons. Also included are instrument
monitors tied to decons: photometric stability check, focus monitor, pre-
and
post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,
VISFLAT sweep, and internal UV flat check.
WFPC2 10070
WFPC2 CYCLE 12 Supplemental Darks Part 2/3
This dark calibration program obtains 3 dark frames every day to provide
data
for monitoring and characterizing the evolution of hot pixels.
WFPC2 10084
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.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)
HSTAR 9328: OTA SE review of PTAS Processing Log revealed GS Reacquisition
(2,1,2), starting @ 041/08:41:41Z, required two
attempts to achieve
FL-DV on FGS 2. During the first FL walkdown, FGS 2
suffered SSLEX.
As the second attempt was successful, no science
impact should have
been seen.
COMPLETED OPS REQs: None
OPS NOTES EXECUTED:
0911-0 Limit Management During WFPC2 Decontamination (M001) @ 048/2005z
1115-0 CCC IPCONFIG Connections @ 049/0238z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 08 08
FGS REacq 06 06
FHST Update 22 22
LOSS of LOCK
SIGNIFICANT EVENTS:
PSS Serial testing scheduled 049/12:00Z – 21:00Z with GDOC, SOC, and HITT
using CCS "C"
String with CCS Release 4.0.3.1 and PRD S07300. The purpose of this
testing is to
verify CCS PSS Release 3.3 can simulate HST for telemetry transmission and
command
response via serial link from Building x (intentionally removed).
