NASA Hubble Space Telescope Daily Report # 3543
HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science
DAILY REPORT # 3543
PERIOD COVERED: DOY 33
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/HRC/WFC 9919
The Morphological, Photometric, and Spectroscopic Properties of
Intermediate
Redshift Cluster Galaxies:
New and fundamental constraints on the evolutionary state of high
redshift
clusters will be made by obtaining deep, multiband images {SDSS r, i, z}
over
the central 1.5 Mpc regions of seven distant clusters in the range 0.76
< z <
1.27. The ACS data will allow us to {1} definitively establish the
morphological
composition and star formation rates as functions of clustercentric
radius,
local density, x-ray luminosity {obtained from accompanying Chandra, and
XMM
data}, {2} explore the relationship between substructure, kinematics,
and
morphology, {3} strongly constrain the galaxy merger frequency and the
origins
of elliptical and S0 galaxies, {4} measure the mass distribution
independently
from the light {via gravitational lensing} enabling comparisons with
kinematically derived masses, and {5} study the evolution of the
structure of
the brightest cluster members. The clusters selected for this program
already
have extensive spectroscopic observations and NIR imaging is either in
hand or
underway from approved ground based programs. To date, the lower part of
this
redshift range has only been marginally studied with HST. Our sample
includes
the two most distant, spectroscopically confirmed superclusters and will
significantly increase the baseline over which evolutionary effects can
be
studied. The data will also be used to identify very high-z galaxies via
their
unique spectral properties.
ACS/WFC/HRC 9771
The local Hubble flow and the density field within 6 Mpc
Great progress has been made recently in accurate distance measurements
of
nearby galaxies beyond the Local Group based on the luminosity of the
tip
of the
red giant branch {TRGB}. Over the last three years, snapshot surveys
with HST
have provided us with the TRGB distances for more than a hundred nearby
galaxies
obtained with an accuracy of about 10%. The local velocity field within
5 Mpc
exhibits a significant anisotropy which disagrees with a spherical
Virgo-centric
flow. The local Hubble flow is very cold, with 1-D rms deviations of ~30
km/s.
Cosmological simulations with Cold Dark Matter can only realize such low
dispersions with a combination of a low mean density of matter and a
substantial
component with negative pressure. There may be a constraint on the
equation of
state w=-p/rho. Our observations will concentrate on 116 galaxies
whose
expected
distances lie within 4 – 6 Mpc, allowing us to trace a Dark Matter
distribution
in the Local Volume with twice the information currently available. The
program
is a good one for SNAP mode because the order and rate that the
observations are
made are not very important, as long as there is good completion over
several
years.
ACS/WFC/HRC 9977
Gravitational Microlensing in the NGC 3314A-B Galaxy Pair
Determining the composition of the dark matter that dominates the masses
of
galaxies is an important unsolved problem, and the results of the MACHO
Collaboration suggest that some of Milky Way’s dark matter may be in the
form of
very old white dwarfs. However, some have argued that the excess of
microlensing
events seen by MACHO are due to a larger than expected microlensing rate
for
lens stars in the LMC itself or its tidal debris. We propose to address
this
question by detecting microlensing events in the line-of-sight galaxy
pair NGC
3314 A & B. The large line-of-sight distance between these galaxies
gives an
optical depth that is 3-4 orders of magnitude larger than if the source
stars
and lenses were in the same galaxy, and the fact that the background
galaxy
is a
spiral ensures that there will be a sufficient number of bright,
non-variable
source stars. Our proposed observations should have the sensitivity to
detect
microlensing by both ordinary stars and dark matter in NGC 3314A {the
foreground
galaxy}. If there are dark matter microlensing events to be found, they
can be
clearly distinguished from stellar microlensing events because they will
occur
outside the visible disk of NGC 3314A. If baryonic dark matter is
detected in
NGC 3314A, we will be able to map its radial density variation.
FGS 9888
Trigonometric Calibration of the Period- Luminosity Relations for
Fundamental
and First-Overtone Galactic Cepheids
Cepheids are the primary distance indicators for the extragalactic
distance
scale and the Hubble constant. The Hubble Constant Key Project set the
zero-point for their Cepheid distance scale by adopting a distance to
the LMC,
averaged over a variety of techniques. However, different methods give
an LMC
distance modulus ranging from 18.1 to 18.8, and the uncertainty in the
Cepheid
zero-point is now the largest contributor to the error budget for H 0.
Moreover,
the low metallicity of the LMC raises additional concerns, since the PL
relation
probably depends on metallicity. The zero-point can be determined from
Hipparcos
parallaxes of Galactic Cepheids out to several hundred parsecs, but with
a
typical parallax error of 0.5-1 mas, the Hipparcos error bars are
uncomfortably
large for this demanding application. By contrast, HST’s FGS1R
interferometer
can achieve astrometric accuracy of 0.2 mas. We propose to use FGS1R to
determine trigonometric parallaxes for a sample of 9 nearby Cepheids,
including
both fundamental {F} and first-overtone {FO} pulsators. We show that the
improvement in the PL relations for F and FO Cepheids will be dramatic.
We will
determine the PL slopes from our nearby solar- metallicity sample alone,
without
recourse to nearby galaxies and the issue of [Fe/H] dependence. The
zero-point
will be determined robustly to about 0.05 mag, based on accurate, purely
geometrical measurements. All of this can be achieved in the next few
years
with
HST, without having to wait for the technically demanding and risky SIM
and
GAIA
missions well into the next decade.
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.
NIC2 9768
Enabling Coronagraphic Polarimetry with NICMOS
We propose to enable a new mode on NICMOS that combines the powerful
diffracted
light rejection of the coronagraph with the diagnostic power of
polarimetry.
This new capability will open a new regime in high contrast imaging that
has not
been possible before. We will enable this capability by observing
calibration
targets with the coronagraph and the NIC2 polarizers in place. The
enabled
science includes, but is not limited to, detection and imaging of
circumstellar
debris in polarized light, the polarized emission surrounding bright
planetary
nebulae, and the extended structure around bright active galaxies. A
similar
capability is possible with the ACS, and therefore HST would provide the
only
platform for this extremely high contrast imaging covering the entire
near-UV,
optical and near-infrared wavelength regime. Only the combined HST
NICMOS
system
has the combined resolution and stability {especially with the NCS} to
provide
high spatial resolution, coronagraphic, near-infrared polarimetry in the
foreseeable future. The technique is absolutely unique to HST and will
enable a
new regime in high contrast imaging.
NIC3 10014
Spectrophotometry of FAINT IR STANDARDS
Faint spectrophotometric standard stars required for COS and the SBC
channel on
ACS have been established via the STIS FASTEX program that has executed
over the
last three cycles. Cycle 12 is an especially opportune time to establish
companion faint IR standards for WFC3, because the NICMOS proposal 9998
includes
observations in cycle 12 of all 6 of the primary standard stars in order
to
establish the absolute flux calibration of the three grism modes to 1%.
In
addition to WFC3, these new faint secondary IR standards will be a
significant
step towards establishing flux standards for JWST, as well as for SNAP,
SIRTF,
and SOFIA. The 6 primary standards included in Propid=9998 are in the
range of
V=11-13 and include three hot pure hydrogen WDs and 3 solar analogs.
We propose
to establish new IR faint standards in the 15-17 mag range. Appropriate
spectral
types for faint IR standards are solar analogs and hotter WDs. Many M
type and
cooler stars are variable, so that long term monitoring is required
before
committing HST time to such cool stars. A few G type and WD faint stars
will
provide a set of faint IR standards with minimal sky and color coverage.
Existing HST images of any candidates can provide verification that
there
are no
contaminating stars above the 1% level within 2-3arcsec. However, the
ACS
calibration field in 47 Tuc is too crowded for linking to ground based
observations. If the other candidates are selected from SDSS or other
ground
based data, then the NICMOS and STIS acquisition images can provide this
verification, as well as correction factors for arbitrary photometric
size
apertures. The SNAP team is providing the northern faint stars using
unreleased
SDSS data. In addition, the extreme coolest types such as L and T stars
have
proven essential to sorting out the long wavelength QE of ACS; both the
ACS and
eventually WFC3 calibrations could be improved with knowledge of L and T
SEDs in
the region beyond 0.95 microns. In addition to the primary purpose of
ACS
QE vs.
wavelength and broad band F814W and F850LP calibrations, these three
stars in
C.} below are at the flux level required for WFC3 grism calibration. The
brighter M, L, and T standard stars will each require a NICMOS orbit,
while
each
faint standard requires two Nicmos orbits and one STIS orbit for
complete
wavelength coverage. The STIS spectra of the M and L stars are done as
ACS
calibrations in cycles 12 and 11, respectively. An additional faint WD
has
already been proposed for 2 Nicmos and 4 STIS orbits in their cycle 12
programs
already. See Table 1 for a summary of the 18 orbit allocation for this
program
10014. Bright stars in the V=0-6 mag range would be useful for direct
comparisons to NIST calibrated lamps. This comparison would offer the
opportunity to compare two fundamentally different realms of physics:
pure
hydrogen stellar models and laboratory black body physics.
Unfortunately, the
Nicmos bright limit is V=~8 for a solar analog and a 1s exposure
without
defocussing the OTA. The primary Sloan standard BD+17d4708 at V=9.9 is
safely
fainter than this Nicmos limit.
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.
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 10085
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during cycle
12.
STIS/CCD 10091
Soft X-ray Transient in Mira AB
Chandra Observations of Mira AB symbiotic-like system obtained in Dec.
2003
detected an unexpected bright soft source {<0.7 keV} in addition to the
previously observed harder {1-4 keV} emission which has been attributed
to the
accretion disk around Mira B. The newly discovered soft X-ray source
could
indicate an instability in the accretion disk, an accretion related
outburst in
the system, or a flare-like activity in Mira A. We request DD time to
carry out
HST/STIS imaging and spectroscopy of Mira AB at UV wavelengths, where
signatures
of these processes are very likely to be found. Because of the likely
transient
nature of this phenomenon, timely HST observations are critical for
determining
the nature and the characteristics of the soft X-ray source and
therefore we
cannot wait for Cucle 13 observatios including TOO observations.
STIS/MA1 10034
Cycle 12 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.
WFPC2 10068
WFPC2 CYCLE 12 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 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.
WFPC2 10072
WFPC2 CYCLE 12 INTERNAL MONITOR
This calibration proposal is the Cycle 12 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 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 9307: GS Re-acquisition (3,2,2) @ 033/13:44:32Z suffered one
occurrence of
SSLE on FGS 3 @ 033/13:46:33Z. GS Re-acquisition
was successful on
second try. GS Re-acquisition (3,2,2) @
033/16:56:24Z also suffer a
SSLE on FGS 2 @ 033/16:58:27Z, also successful on
second try. Under
investigation.
COMPLETED OPS REQs: None
OPS NOTES EXECUTED: None
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 08 08
FGS REacq 07 07
FHST Update 18 18
LOSS of LOCK
SIGNIFICANT EVENTS:
FOT moved to accommodate Building xx Network Failure Simulation
scheduled
034/19:00Z – 23:30Z. This is a periodic test of our ability to handle
a total network failure by moving to the Backup Control Center.
At the scheduled time, we will start a Network Failure Simulation and
sometime after that, at a time free of critical commanding, we will take
down the entire Network, except for the minimal essential Backup Control
Center elements in Building xx (information intentionally removed).
This will
impact ALL HSTnet users, including Ops, LMB, Vision, Frame Relay, etc.
The OC-3 from the will be down, thus, the VDS extension to the xx will
also
be down during this time frame. This will not affect xx.edu net
internal
traffic,
but it will isolate them from HSTnet and all other external networks.
FOT will return to SIMOR on 2/4/04 Day Shift.
HST Command Timing Test scheduled 034/12:00Z – 22:00Z with GDOC, SOC,
HITT,
and CCS using CCS "F" String with CCS Release 5.0.3.1 and PRD O06300ST.
The purpose of this testing is to check the command timing for CCS
Release 5.0.3.1 with historical, baselined numbers.
