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Daily 3603



 
 
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Old May 5th 04, 05:21 PM
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Default Daily 3603

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3603

PERIOD COVERED: DOYs 121-123

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 9906

Volatile Abundances and the D/H Ratio in Long-Period Comets

Comet NEAT {C/2001 Q4} is predicted to reach naked-eye visibility in
the spring of 2004, under excellent conditions for observations with
HST. Although predicting cometary magnitudes more than 1 year in
advance is notoriously risky, C/NEAT seems likely to be exceptionally
active, allowing us for the first time to perform sensitive
measurements of the D/H and OD/OH ratios. Accurate measurements of the
deuterium abundance in comets, which can vary in different species,
are crucial for determining if comets retain a signature of their
possible interstellar origin and if they supplied a significant
fraction of the water on Earth. HST observations of C/NEAT will
additionally provide accurate abundances for highly volatile ices in
the nucleus, such as CO, CO2 {via Cameron band emission}, and S2,
which also provide important insights on the comet's origin and
evolution. This opportunity in cycle 12 is unique in the history of
HST and is unlikely to be repeated during its remaining lifetime.

FGS 9879

An Astrometric Calibration of the Cepheid Period-Luminosity Relation

We propose to measure the parallaxes of 10 Galactic Cepheid variables.
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.

WFPC2 9870

Low Mass Star Formation at Low Metallicity: Accretion Rates of
Pre-Main Sequence Stars in the Large Magellanic Cloud

As part of an ongoing effort to characterize the process of star
formation at low metallicity, we propose to measure by means of U-band
excess the current accretion rate for a homogenous sample of
newly-born stars in NGC 1850, a young {5 Myr} stellar cluster in the
LMC. Clearly, at this age most of the accretion has already taken
place and its intensity is declining with respect to the earliest
stages of formation. However, a comparison with Galactic Pre-Main
Sequence stars of the same age immediately leads to assessing the
relative strength of accretion when the metallicity is decreased by a
factor of three. We have already analyzed the images available in the
archive for these fields and we have determined the basic parameters
{effective temperature and luminosity} for all of the stars down to a
mass of ~0.9 Mo. To take the next step and determine the current
accretion rate we only need WFPC2 imaging of NGC 1850 in the F336W
passband. With three orbit worth of observations, we will reach
m{F336W}~23 with an accuracy of 0.1 mag. In spite of their unique
scientific potential, the data we apply for are relatively inexpensive
to gather, as they are the last missing tile of a large dataset
already available in the HST archive.

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.

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.

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.

ACS/HRC 9782

Measuring Black Hole Masses in Double Peaked Broad Lined AGNs

To date there have been few black hole {BH} mass estimates for
luminous broad line AGN, including those derived from reverberation
mapping. In this context, objects with "double-peaked" broad lines are
particularly important because the line emission is believed to arise
in a relativistically rotating accretion disk. If this model is
correct, then the BH mass can be determined directly from periodic
variations in the line-profile shape. In two cases {Arp 102B and NGC
1097} such variations have been claimed. The goal of this proposal is
to confront the relativistic disk model for the double-peaked Balmer
lines with independent limits on the central masses for 5 of the
nearest and brightest "double-peaked emitters" {NGC 1097, Arp 102B,
Pictor A, 3C390.3, 3C332}, determined by using STIS long-slit
spectroscopy to map the velocity field of circum-nuclear ionized gas.
These observations will critically test the idea that the line
emission in these objects comes from an accretion disk and thus
provide unique insights into the physical processes operating in both
the BLR and the "central engine".

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.

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.

WFPC2 10073

Earth Flats

This proposal monitors flatfield stability. This proposal obtains
sequences of Earth streak flats to construct high quality flat fields
for the WFPC2 filter set. These flat fields will allow mapping of the
OTA illumination pattern and will be used in conjunction with previous
internal and external flats to generate new pipeline superflats. These
Earth flats will complement the Earth flat data obtained during cycles
4-11.

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.

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.

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 10049

ACS Internal Flat Field Stability

The stability of the CCD flat fields will be monitored using the
calibration lamps and a sub-sample of the filter set. High signal
observations will be used to assess the stability of the pixel-to-
pixel flat field structure and to monitor the position of the dust
motes. Shorter exposures will be used to identify charge traps and to
assess the stability of the DQ arrays. Only internal exposures with
the calibration lamps will be required.

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.

STIS/CCD 10018

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS/CCD 10016

STIS CCD Performance Monitor

This activity measures the baseline performance and commandability of
the CCD subsystem. Only primary amplifier D is used. Bias and Flat
Field exposures are taken in order to measure bias level, read noise,
CTE, and gain. Numerous bias frames are taken to permit construction
of "superbias" frames in which the effects of read noise have been
rendered negligible. Full frame and binned observations are made, with
binning factors of 2 x 1, 1 x 2, 2 x 2, 4 x 1, and 4 x 2. Bias frames
are taken in subarray readouts to check the bias level for ACQ and
ACQ/PEAK observations. All exposures are internals.

WFPC2/ACS/HRC/WFC 10013

Focus Monitor

The focus of HST is measured from WFPC2/PC and ACS/HRC images of
stars. Multiple exposures are taken in parallel over an orbit to
determine the influence of breathing on the derived mean focus.
Observations are taken of clusters with suitable orientations to
ensure stars appear in all fields.

FLIGHT OPERATIONS SUMMARY:

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

HSTAR 9405: FHST Roll Delay Update (U1,3RD) @ 122/14:33:49Z failed
with Error Box results reading "1 FAILED". Under investigation.

COMPLETED OPS REQs:
17160-0 MTS Compensated MSS Data Collection @ 123/23:48z


OPS NOTES EXECUTED:
1231-1 Packet Filter and CCC config for On-going Network changes @ 121/13:08z
1232-0 MSS Data Collection Ops Req # 17160-0, @ 123/23:48z
1233-0 Adjust ACS Error Count Limit (ACS 935) @ 122/14:44z.
1233-1 Adjust ACS Error Count Limit (ACS 935) @ 122/19:03z
1233-2 Adjust ACS Error Count Limit (ACS 935) @ 122/21:26z


SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 36 36
FGS REacq 13 13
FHST Update 43 42 See Hstar
# 9405
LOSS of LOCK

SIGNIFICANT EVENTS: None


 




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