Status Report

NASA Hubble Space Telescope Daily Report #3519

By SpaceRef Editor

December 29, 2003

Filed under Hubble Space Telescope, Space Telescope Science Institute, US

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3519

PERIOD COVERED: DOYs 360-362

OBSERVATIONS SCHEDULED

NIC3 9999

The COSMOS 2-Degree ACS Survey NICMOS Parallels

The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to
program 9822.

STIS/CCD 9981

The Ultra Deep Field – STIS parallels

We propose to obtain slitless spectroscopy of objects in the GEMS and GOODS
area
around the UDF.

WFPC2 9980

The Ultra Deep Field – WFPC2 Parallels

The ACS Ultra Deep Field {UDF} is a survey carried out by using Director’s
Discretionary time. The main science drivers are galaxy evolution and
cosmology.
The primary instrument is the Advanced Camera for Surveys but WFPC2,
NICMOS, and
STIS will also be used in pure parallel mode. The data will be made public. The
UDF consists of a single ultra-deep field {410 orbits in total} within the
CDF-S
GOODS area. We request a modification of the default pure parallel programs.
Rather than duplicate the redder 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,
allowing determination of 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.

NIC3 9979

The Ultra Deep Field – NICMOS Parallels

This is a plan to manage the NICMOS pure parallels of the ACS Ultra Deep
Survey.
We will obtain a mix of F110W and F160W images along sight-lines within the
mosaiced ACS fields of the CDF-S GOODS and GEMS surveys, with these sight-lines
enabling an examination of the space density and morphologies of the reddest
galaxies.

ACS/CCD/WFC 9978

The Ultra Deep Field with ACS

The ACS Ultra Deep Field {UDF} is a survey carried out by using Director’s
Discretionary time. The main science driver are galaxy evolution and cosmology.
The primary instrument is the Advanced Camera for Surveys but WFPC2 and NICMOS
will also be used in parallel. The data will be made public. The UDF
consists of
a single ultra-deep field {410 orbits in total} within the CDF-S GOODS
area. The
survey will use four filters: F435W {55 orbits}, F606W {55 orbits}, F775W {150
orbits}, and F850LP {150 orbits}. The F435W {B} and F606W {V} exposures will be
one magnitude deeper than the equivalent HDF filters. The F775W {I} exposure
will be 1.5 magnitude deeper than the equivalent HDF exposure. The depth in
F775W and F850LP is optimized for searching very red objects – like z=6
galaxies
– at the detection limit of the F850LP image. The pointing will be RA{J2000}=3
32 40.0 and Decl.{J2000}=-27 48 00. These coordinates may change slightly
due to
guide star availability and implementation issues. We will attempt to
include in
the field both a spectroscopically confirmed z=5.8 galaxy and a
spectroscopically confirmed type Ia SN at z=1.3. The pointing avoids the gaps
with the lowest effective exposure on the Chandra ACIS image of CDFS. This
basic
structure of the survey represents a consensus recommendation of a Scientific
Advisory Committee to the STScI Director Steven Beckwith. A local Working Group
is looking in detail at the implementation of the survey.

STIS/CCD 9866

First Spectroscopic Study of a Unique Set of Young Stars in the Orion Nebula

We propose to obtain the first spectra of the central stars of Orion proplyds
for which the stars are visible in WFPC images. While it is known that the
central stars are broadly late-type, they have never been spectrally classified
or studied in detail as pre-MS objects. The Orion proplyds are generally
thought
to be protoplanetary disks similar to the primordial disk of the Solar System.
They offer a unique opportunity to understand the physical conditions of
protoplanetary disks in a nebular environment generally believed to be typical
of that in which most stars formed. Models of the proplyds are available which
predict the observable IR spectral energy distribution using the spectral type
of the central star as part of the numerical input. Further progress in
understanding proplyds will require knowledge of the spectral types of these
stars. We will use already-proven diagnostics for spectrally classifying
late-type PMS stars. In addition, many emission lines are expected in
objects of
this age which can be used to look for infall and outflow. Different accretion
models of young stars predict different line widths, so our observations can
help test models of late-type pre-MS stars and can be used to compare as pre-MS
objects the proplyd stars with other pre-MS stars.

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.

ACS/WFC 9860

ESSENCE: Measuring the Dark Energy Equation of State

The accelerating universe appears to be dominated by a dark energy with a
significant negative pressure. The ratio of the pressure to density of this
mysterious energy {its equation of state} is an observable which can
differentiate between the proliferating candidate theories. We propose to
estimate the dark energy equation of state by observing Type Ia supernovae at
redshifts near z=0.7 with HST in concert with the on-going ESSENCE NOAO Survey
program that is discovering and studying supernovae between 0.3<z<0.8. We show
that an interesting constraint on the equation of state can be made with
supernovae observed at modest redshifts given the current knowledge of the
matter density. We will follow 10 Type Ia supernovae discovered from the ground
and passed to HST without disrupting its schedule. The full data set will
constrain the equation of state to 10% and strictly limit the range of possible
dark energy models. In keeping with the ESSENCE policy, these observations will
available to the community immediately.

STIS/CCD 9849

AGN Black Hole Masses from Stellar Dynamics

We propose to measure the black-hole masses in two reverberation-mapped Seyfert
1 galaxies, NGC 3227 and NGC 4151, by using STIS spectroscopic observations of
the Ca II triplet absorption features in the nuclear stellar spectra of these
sources. The observations will be carried out on a TOO basis when the active
nuclei are faint, thus mitigating the problem of contamination of the starlight
component by the scattered light from the active nucleus. These observations
will enable the first direct comparison of black-hole masses determined from
stellar dynamics {the most frequently used method for quiescent galaxies} with
those determined by reverberation mapping {the most frequently used method for
active galaxies}.

ACS/WFC/WFPC2 9822

The COSMOS 2-Degree ACS Survey

We will undertake a 2 square degree imaging survey {Cosmic Evolution Survey —
COSMOS} with ACS in the I {F814W} band of the VIMOS equatorial field. This wide
field survey is essential to understand the interplay between Large Scale
Structure {LSS} evolution and the formation of galaxies, dark matter and AGNs
and is the one region of parameter space completely unexplored at present by
HST. The equatorial field was selected for its accessibility to all
ground-based
telescopes and low IR background and because it will eventually contain ~100,
000 galaxy spectra from the VLT-VIMOS instrument. The imaging will detect
over 2
million objects with I> 27 mag {AB, 10 sigma}, over 35, 000 Lyman Break
Galaxies
{LBGs} and extremely red galaxies out to z ~ 5. COSMOS is the only HST project
specifically designed to probe the formation and evolution of structures
ranging
from galaxies up to Coma-size clusters in the epoch of peak galaxy, AGN, star
and cluster formation {z ~0.5 to 3}. The size of the largest structures
necessitate the 2 degree field. Our team is committed to the assembly of
several
public ancillary datasets including the optical spectra, deep XMM and VLA
imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data
from
SIRTF. Combining the full-spectrum multiwavelength imaging and spectroscopic
coverage with ACS sub-kpc resolution, COSMOS will be Hubble’s ultimate legacy
for understanding the evolution of both the visible and dark universe.

ACS/HRC 9812

Ultraviolet Emission from Protostellar Accretion Disks

We propose to obtain ACS/prism observations of the UV continuum emitted by
protostellar accretion disks. By combining the ACS data with simultaneous
ground-based optical spectra and near-IR photometry, we will be able to observe
the entire spectral energy distribution of the young stars and their disks from
1800A to 3.5um. The combined data set will solve the long-standing problem of
degeneracy between reddening, spectral type, and excess emission in the
analysis
of such spectra by allowing us to measure reddenings directly from the 2175A
bump, bolometric corrections from the UV continuum, and effective temperatures
from the optical spectra. With this information in hand it will be possible for
the first time to quantify the mass accretion rates, stellar radii, masses, and
ages without the systematic uncertainties that have plagued previous efforts.
The new data will probe the physical conditions that exist where material from
the disk falls onto the star, such as filling factors, temperatures, and
optical
depths. We will also be able to place heavily veiled stars unambiguously in HR
diagram for first time to see if these stars are on average younger than their
more slowly accreting counterparts, and test whether or not the Mg II 2800A
doublet traces jets close to their stars. The proposed observations will yield
the first simultaneous coverage over all the principal wavelengths that these
accretion disks emit; a true multiwavelength approach is the only way to
clarify
what goes on in accretion/outflow systems, a process common throughout
astrophysics.

STIS/CCD/MA1 9759

Confirmation of New Candidates for the Study of Intergalactic Helium

The reionization of intergalactic helium is believed to take place between
redshift 3 and 4. The study of HeII Lyman-alpha absorption in four quasars at
2.7<z<3.3 demonstrates the great potential of such an intergalactic-medium
{IGM}
probe and suggests that the reionization epoch is at higher redshifts. Clean
quasar sightlines may be found only from massive pre-selection processes in the
optical and UV, because of random, severe absorption by intervening Lyman-limit
systems. The SDSS has discovered approximately 36000 quasars, and we propose to
verify the UV detectability in 70 top candidates for helium studies
extending to
even higher redshift. Our proposed approach has already proven successful, and
additional positive confirmations will allow follow-up observations, with STIS
or COS, to pinpoint the epoch of reionization of the IGM, and the evolution of
its properties near that period.

ACS/HRC 9748

Ceres: High-Resolution Mapping and Determination of Physical Properties

We propose a modest, 6-orbit HST ACS/HRC program to fully map the asteroid 1
Ceres for the first time. These high signal-to-noise, high resolution maps will
be obtained in three ACS filter bandpasses from the visible to the UV. The
goals
of our program are to advance knowledge about Ceres dramatically, to resolve
certain longstanding issues regarding Ceres, and to support planning for the
Dawn Discovery mission’s planned orbital tour of Ceres. The specific scientific
objectives of this proposed Cycle 12 effort are: {1} To achieve dense
rotational
phase coverage with multi-spectral imaging over the complete rotation period of
Ceres to map its surface; {2} To resolve surface features and investigate the
nature of the Piazzi feature detected by HST/FOC in 1995; {3} To track surface
features in order to unambigously determine Ceres’ pole position; {4} To
measure
the three-dimensional shape of Ceres better than any existing shape model in
order to significantly refine density measurements; and {5} To map Ceres’ color
variegation and photometric parameters in order to identify possible surface
units for the first time. These goals require high resolution visible and
ultraviolet imaging, which can only be obtained with HST. As we demonstrate in
this proposal, the January, 2004 opposition of Ceres is the best in the next 6
years for both data quality and planning of the Dawn mission.

WFPC2 9712

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.

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.

ACS 9401

The ACS Virgo Cluster Survey

We propose the most comprehensive imaging survey to date of low-redshift,
early-type galaxies. Our goal is to exploit the exceptional imaging
capabilities
of the ACS by acquiring deep images — in the SDSS g^ and z^ bandpasses
— for
163 E, S0, dE, dE, N and dS0 galaxies in Virgo, the nearest rich cluster. This
extraordinary dataset would likely constitute one of the principal legacies of
HST, and would have widespread applications for many diverse areas of
astrophysics. Our immediate scientific objectives are threefold: {1} measure
metallicities, ages and radii for the many thousands of globular clusters {GCs}
in these galaxies, and use this information to derive the protogalactic mass
spectrum of each galaxy; {2} measure the central luminosity and color
profile of
each galaxy, and use this information to carry out a completely independent
test
of the merging hierarchy inferred from the GCs, with the aid of N-body codes
that simulate the merger of galaxies containing massive black holes; and {3}
calibrate the z^ -band SBF method, measure Virgo’s 3-D structure, and carry out
the definitive study of the GC luminosity function’s precision as a standard
candle. Our proposed Virgo Cluster Survey will yield a database of
unprecedented
depth, precision and uniformity, and will enable us to study the record of
galaxy and cluster formation in a level of detail which will never be possible
with more distant systems.

NICMOS 8790

NICMOS Post-SAA calibration – CR Persistence Part 1.

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.

ACS/WFC 10086

The Ultra Deep Field with ACS

STIS/CCD 10085

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during cycle 12.

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.

ACS/HRC/WFC 10042

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.

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 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.

ACS/WFC/WFPC2 10003

Deep Chandra and Hubble Observations of NGC4697, the Nearest Optically
Luminous,
X-ray Faint Elliptical Galaxy

We propose 4 new Chandra observations of NGC4697, the nearest X-ray-faint,
optically-bright elliptical, which was resolved into low mass X-ray binaries
{LMXBs} in Cycle 1. We will detect LMXBs at least three times fainter {~1e37
ergs/s} than possible for any luminous E galaxy at present, allowing a direct
comparison with the LMXBs in our Galaxy and M31. We will measure the
variability
of sources on times up to 4.5 yr. Models predict variability for LMXBs in
early-type galaxies, which is particularly strong for the brightest black hole
sources. We also propose 1 orbit of HST to detect >1500 globular clusters
{GCs}.
If the results for luminous LMXBs continue to low LX, most of the LMXBs will be
identified with GCs. We will study the formation history of LMXBs, GCs, and
field stars in N4697.

STIS/CCD 10000

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during cycle 12.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)

HSTAR 9254: GS Acquisition (3,1,3) @ 362/04:00:28Z resulted in FL backup
using
FGS 1 due to SSLE on FGS 3. Prior RD Update @
362/03:35Z showed good
attitude error vector. FHST Map @ 362/05:11Z showed
3-axis errors
of-1.411, -2.492, and 4.567 arcsec. Under investigation.

COMPLETED OPS REQs: None

OPS NOTES EXECUTED:
1184-0 – Change Limits MAMA1 Threshold Voltage (Closed) @ 362/0948z

SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 29 29 FGS REacq 17 17 FHST Update 46 46 LOSS of LOCK

SIGNIFICANT EVENTS: None