Status Report

NASA Hubble Space Telescope Daily Report # 3519

By SpaceRef Editor

January 1, 2004

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

SpaceRef Editor

SpaceRef staff editor.

Follow on Twitter