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Daily 3605



 
 
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Old May 5th 04, 05:21 PM
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Default Daily 3605

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3605

PERIOD COVERED: DOY 125

OBSERVATIONS SCHEDULED

ACS 9476

Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster
Sample

The study of distant cluster galaxies requires two key ingredients:
{1} deep high-resolution imaging, to constrain galaxy structure; and
{2} 8m-class spectroscopy, to measure stellar content, star-formation
rates, dynamics, and cluster membership. We will reach both conditions
with the addition of HST/ACS imaging to our suite of VLT {36 nights}
and NTT {20 nights} observations of 10 confirmed clusters at z~0.8,
drawn from the ESO Distant Cluster Survey {EDisCS}. The proposed
HST/ACS data will complement our existing optical/IR imaging and
spectroscopy with quantitative measures of cluster galaxy morphologies
{i.e. sizes and shapes, bulge-disk decompositions, asymmetry
parameters}, and with measurements of cluster masses via weak lensing.
Major advantages unique to the EDisCS project include: {i} uniform
selection of clusters; {ii} large enough sample sizes to characterize
the substantial cluster-to-cluster variation in galaxy populations;
{iii} large quantities of high quality data from 8m telescopes; {iv}
uniform measurements of morphologies, spectroscopic and photometric
redshifts, SEDs, star-formation/AGN activities, and internal
kinematics; {v} optical selection of clusters to complement the X-ray
selection of almost all high-z clusters in the ACS GTO programs; {vi}
forefront numerical simulations designed specifically to allow
physical interpretation of observed differences between the high-z and
local clusters.

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.

ACS/HRC/WFC 10060

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 9766

The Globular Cluster Systems of Spiral Galaxies along the Hubble Sequence

While the globular cluster {GC} systems of ellipticals and ongoing
mergers have been relatively well-studied with HST, very little is
known about the GC systems of spirals besides the Milky Way and M31.
To constrain GC/galaxy formation models, especially where spirals are
the merger progenitors of ellipticals, it is crucial to understand
their GC properties. We propose to obtain ACS images of three edge-on
spirals, spanning the Hubble sequence, with Keck spectroscopic
follow-up. This will effectively double the number of well-studied
spiral systems. We will detect 100-200 GCs per galaxy, sufficient to
reveal GC subpopulations, their relative numbers, radial trends, and
dependences on Hubble type {e.g., a bulge vs. disk origin for red
GCs}. For half of our GCs we will be able to measure individual sizes.
By providing a much-needed comparative benchmark, these data will
allow researchers to better exploit the large existing HST database of
GCs in E/S0 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.

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
0.7z1.9, 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.

NIC1/NIC2/NIC3 8792

NICMOS Post-SAA calibration - CR Persistence Part 3

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.

NIC1/NIC2/NIC3 9723

Deep NICMOS imaging

We have obtained ultra-deep Js, H, Ks imaging of the Hubble Deep Field
South WFPC2 field with the VLT, in order to study high redshift
galaxies. The Ks-band data are the deepest obtained to date in any
field. We find that the population of Ks selected galaxies at z=2-4 in
HDF-South differs in two important aspects from previous studies in
HDF-North. First, we find several galaxies which are large and
apparently regular in the rest-frame optical, with more complex rest-
frame UV morphologies. These objects resemble large disk galaxies in
the local Universe. Second, we have identified a population of
galaxies with red J-K colors that are extremely faint in the
rest-frame UV. The galaxies have ages of 0.5-2 Gyr and are highly
clustered, and may be progenitors of nearby bulges and early-type
galaxies. We propose to obtain a deep mosaic with the NICMOS/NIC3
camera in the H band, covering the WFPC2 field. The increased depth
and spatial resolution of the NICMOS mosaic would allow us to
determine the restframe optical morphologies of a large sample of high
redshift galaxies, in order to study the relative distributions of
young and old stars, to decompose the galaxies in bulges and disks, to
measure scale lengths, and to model the stellar populations of the
sub-components. The lack of large U- dropouts and red galaxies in
HDF-North, and the need for larger samples call for the proposed
imaging of HDF-South. We waive all prioprietary rights.

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 9786

The Next Generation Spectral Library

We propose to continue the Cycle 10 snapshot program to produce a Next
Generation Spectral Library of 600 stars for use in modeling the
integrated light of galaxies and clusters. This program is using the
low dispersion UV and optical gratings of STIS. The library will be
roughly equally divided among four metallicities, very low {[Fe/H] lt
-1.5}, low {[Fe/H] -1.5 to -0.5}, near-solar {[Fe/H] -0.3 to 0.1}, and
super-solar {[Fe/H] gt 0.2}, well-sampling the entire HR-diagram in
each bin. Such a library will surpass all extant compilations and have
lasting archival value, well into the Next Generation Space Telescope
era. Because of the universal utility and community-broad nature of
this venture, we waive the entire proprietary period.

STIS/CCD 10018

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS/CCD 10020

CCD Bias Monitor - Part 2

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,
and 1x1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.

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.

FLIGHT OPERATIONS SUMMARY:

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

COMPLETED OPS REQs: NONE


OPS NOTES EXECUTED:
1234-0 TDW Cross-support tracking (T77 CODE) @ 125/18:00z
1234-0 TDW Cross-support tracking (T77 CODE) @ 126/04:21z

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 07 07
FGS REacq 08 08
FHST Update 14 14
LOSS of LOCK


SIGNIFICANT EVENTS: None


 




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