Status Report

NASA Hubble Space Telescope Daily Report # 3540

By SpaceRef Editor
January 29, 2004
Filed under , ,

HUBBLE SPACE TELESCOPE – Continuing to collect World Class Science




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
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.

ACS/HRC 9746

Binary systems in the Kuiper Belt

The properties of the orbits of Kuiper belt object {KBO} satellites hold
keys to
fundamental insight into masses and densities of KBOs, the interaction history
of the early solar system, the internal structure of distant ice-rock bodies,
and even the genesis of the Pluto-Charon binary. Within the past 18 months, 9
KBO satellite systems have been discovered, allowing for the first time the
possibility of characterizing a sample of KBO satellite orbital properties. We
propose HRC observations to determine satellite orbits in the 6 best cases. We
have carefully devised a strategy for each of these 6 systems to make maximum
use of ground-based observations, previous HST observations, and the smallest
possible number of new HST observations. Our proposed observations will
efficiently provide highly reliable orbital solutions which are critical to
achieving the scientific promise available from the study of these systems. Our
strategy relies heavily on extensive Monte Carlo simulations to define optimal
times of observing such that each new point obtained gives maximum leverage for
refining the orbital solution. We find that with this strategy we can provide
mass solutions for all 6 systems to an accuracy of better than 10% using
only 25
new HST observations. This highly efficient program provides extreme scientific
output with optimal use of scarce resources.


CCD Daily Monitor

This program consists of basic tests to monitor, the read noise, the
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.


The role of dark matter and intracluster gas in galaxy formation and cluster

We propose a fully-sampled mosaic of 41 ACS images to survey galaxy
and measure weak lensing signals to the turn-around radius in the X-ray
cluster, MS0451-03 {z=0.54}. The aim is to isolate the physical processes which
affect the evolution of cluster galaxy morphologies in the context of
well-defined dynamical system. The study will be used in contrast to a
successful campaign undertaken in Cycle 9 on a optically-selected target. By
comparing morphologies with spectroscopic and Chandra X-ray data, we will
quantify the role of the intracluster medium and associated substructures and
establish the timescales and physical regions within which the various
environmental processes occur.


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
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
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.


An ACS/WFC H-alpha Survey of the Orion Nebula

We propose to survey nearly 500 square arcminutes of the Orion Nebula in
using the ACS/WFC, increasing the sky coverage by an order of magnitude
over the
sum of all previous HST observations. This survey will, for the first time,
sample the majority of young stars and circumstellar environments in the
extended Trapezium cluster of 2, 000 low-mass stars. Our primary goal is to
determine the survival rate and statistical properties of protoplanetary disks
in the type of radiation field and dynamical environment in which most
stars are
born. The survey will be used to search for new silhouette disks, bright
proplyds, microjets, large-scale outflows, and to characterize the
properties of
these objects as a function of location in the nebula. We will determine
accurate proper motions in regions where previous HST data exist. However, 90%
of our fields will be observed with HST for the first time. This survey will
provide the first complete census of pre-main sequence objects and outflows in
an HII region and will constrain the extent of hazards to planet formation in
such environments. The images will also provide a legacy for future stellar and
nebular variability studies and proper motion measurements by providing a first
epoch data base.

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
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


NICMOS Post-SAA calibration – CR Persistence Part 2

A new procedure proposed to alleviate the CR-persistence problem of NICMOS.
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
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
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

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

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.


Black Holes in Big Galaxies with Small Bulges

In early-type galaxies the black hole {BH} mass is tightly correlated with the
bulge velocity dispersion. This correlation suggests that the BH mass is
determined by local processes in the central part of the galaxy. However, the
bulge dispersion in these galaxies is correlated with the disk circular speed
which in turn correlates with the inferred halo circular speed {the "disk-halo
conspiracy"}. For this reason, existing data cannot decide whether the BH mass
is set by the bulge dispersion or the disk or halo circular speed. We
propose to
break this degeneracy by weighing the BH in 3 Sc galaxies in which the ratio of
bulge circular speed to bulge velocity dispersion is large, leading to large
differences between BH masses predicted from these quantities. These
measurements will increase the number of carefully studied Sc bulges from
one to
four and will determine whether the masses of nuclear BHs are set by
baryonic} processes in galaxy bulges or by {presumably non-baryonic} processes
in their dark halos.

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

STIS/MA1 10083

HST UV Images of Saturn’s Aurora Coordinated with Cassini Solar Wind

A key measurement goal of the Cassini mission to Saturn is to obtain
simultaneous solar wind and auroral imaging measurements in a campaign
for Jan. 2004. Cassini will measure the solar wind approaching Saturn
continuously from 9 Jan. – 6 Feb., but not closer to Saturn due to competing
spacecraft orientation constraints. The only system capable of imaging Saturn’s
aurora in early 2004 will be HST. In this community DD proposal we request the
minimum HST time needed to support the Cassini mission during the solar wind
campaign with UV images of Saturn’s aurora. Saturn’s magnetosphere is
intermediate between the "closed" Jovian case with large internal sources of
plasma and the Earth’s magnetosphere which is open to solar wind interactions.
Saturn’s aurora has been shown to exhibit large temporal variations in
brightness and morphology from Voyager and HST observations. Changes of auroral
emitted power exceeding one order of magnitude, dawn brightenings, and
latitudinal motions of the main oval have all been observed. Lacking knowledge
of solar wind conditions near Saturn, it has not been possible to determine its
role in Saturn’s auroral processes, nor the mechanisms controlling the auroral
precipitation. During Cassini’s upcoming approach to Saturn there will be a
unique opportunity to answer these questions. We propose to image one complete
rotation of Saturn to determine the corotational and longitudinal
dependences of
the auroral activity. We will then image the active sector of Saturn once every
two days for a total coverage of 26 days during the Cassini campaign to measure
the upstream solar wind parameters. This is the minimum coverage needed to
ensure observations of the aurora under solar wind pressure variations of more
than a factor of two, based on the solar wind pressure variations measured by
Voyager 2 near Saturn on the declining phase of solar activity. The team of
proposers has carried out a similar coordinated observing campaign of Jupiter
during the Cassini flyby, resulting in a set of papers and HST images on the
cover of Nature on 28 February 2002.

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 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.


Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.) None

17083-0 Off-line +BB and -D SPA Trim Relays @028/2102z

1191-0 Bay 5 ES WEB Temperature @029/0032z

FGS GSacq 9 9
FGS REacq 7 7
FHST Update 16 16


Successfully returned -E SPA back online and off-lined +BB and -D SPA Trim
in the PCU-R and SSM486 FSW (TRSWCC and macros) on second opportunity @
(OR 17083 with attached, updated IP-051 procedure). Following the uplink,
monitored power system operations for two orbits to verify nominal
operations of
TRSWCC (+BB and -D SPA Trim Relays remained disconnected, commanded relay
upon Trickle Charge initiation, etc.). During the first and second orbits
the uplink, the batteries experienced Trickle Charge durations of 15 and 17
respectively. EPS SEs will continue close monitoring of power system
especially battery temperatures and pressures to assess the effects of this

FGS 3 ITS Test (SU 0497413) scheduled 029/23:34:23Z – 23:43:26Z.

SpaceRef staff editor.