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Daily 3445

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Old September 11th 03, 05:27 PM
Dave Lychenheim
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Default Daily 3445


DAILY REPORT******* # 3445



ACS 9675

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 9760

ACS Imaging of the Gemini Deep Deep Survey Fields: Galaxy Assembly at
z = 1.5

We are presently carrying out the deepest redshift survey ever
undertaken {the Gemini Deep Deep Survey}. Spectra of extraordinary
quality have been taken in order to obtain redshifts in the so-called
"redshift desert" at 1z2. This redshift range corresponds to the
epoch of peak galaxy formation. In this proposal we request 40 orbits
of ACS imaging to determine the morphologies of 100-120 candidate
early-type galaxies with known redshifts in our survey fields. We seek
to determine if these systems are indeed elliptical galaxies and to
link their morphological states to their spectroscopically determined
ages, recent star-formation histories, and to the evolving global
stellar mass function at the peak epoch of galaxy assembly.

ACS/HRC 9719

Metallicity Spreads in M31 Globular Clusters

Our recent deep HST photometry of the M31 halo globular cluster {GC}
Mayall~II, also called G1, has revealed a red-giant branch with a
clear spread that we attribute to an intrinsic metallicity dispersion
of at least 0.4 dex in [Fe/H]. The only other GC exhibiting such a
metallicity dispersion is Omega Centauri, the brightest and most
massive Galactic GC, whose range in [Fe/H] is about 0.5 dex. These
observations are obviously linked to the fact that both G1 and Omega
Cen are bright and massive GC, with potential wells deep enough to
keep part of their gas, which might have been recycled, producing a
metallicity scatter among cluster stars. These observations
dramatically challenge the notion of chemical homogeneity as a
defining characteristic of GCs. It is critically important to find out
how common this phenomenon is and how it can constrain
scenarios/models of GC formation. The obvious targets are other bright
and massive GCs, which exist in M31 but not in our Galaxy where Omega
Cen is an isolated giant. We propose to acquire, with ACS/HRC, deep
imaging of 3 of the brightest M31 GCs for which we have observed
velocity dispersion values similar to those observed in G1 and Omega
Cen. A sample of GCs with chemical abundance dispersions will provide
essential information about their formation mechanism. This would
represent a major step for the studies of the origin and evolution of
stellar populations.

ACS/WFC 9744

HST Imaging of Gravitational Lenses

Gravitational lenses offer unique opportunities to study cosmology,
dark matter, galactic structure, galaxy evolution and quasar host
galaxies. They are also the only sample of galaxies selected based on
their mass rather than their luminosity or surface brightness. While
gravitational lenses can be discovered with ground-based optical and
radio observations, converting them into astrophysical tools requires
HST. HST has demonstrated that it is the only telescope that can in
each case precisely locate the lens galaxy, measure its luminosity,
color and structure, and search for lensed images of the source host
galaxy given the typical image separations of ~1''. We will obtain
ACS/WFC V and I images and NICMOS H images of 21 new lenses never
observed by HST and NICMOS H images of 16 lenses never observed by HST
in the IR. As in previous cycles, we request that the data be made
public immediately.


Deep NICMOS Images of the UDF

The ACS Ultra Deep Field {UDF} images will greatly enhance the rich
suite of deep multi-wavelength images in the Chandra Deep Field South
{CDF--S}. We propose to complete the image set with deep near-IR
NICMOS images at 1.1 and 1.6 microns over a significant fraction of
the UDF, providing a critical link between the HST ACS and SIRTF
observations. The timely addition of the near-IR images ensures that
investigators will have images that span the spectrum from X-ray to
far IR. In recognition of the value of the near IR images this
proposal is submitted as a Treasury proposal with no proprietary
period. The proposal team will deliver science quality images,
mosaiced images covering 4.9 sq arc min, and a photometric catalog
complete to an AB mag of 28.2 in both the F110W and F160W filters. The
program also delivers a parallel extremely deep ACS field, 8' away,
that reaches to within 0.6 mag of the UDF in the same filters as the
UDF. The scientific program of the proposal team focuses on the star
formation history of the universe, evolved galaxies at high redshift,
galaxies at the epoch of reionization, and the redshift evolution of
AGNs and ULIRGs. The HDF-N is currently the only field with
spatially-coincident deep HST imaging in both the optical and near-IR.
The small size of the HDF-N means that large scale structure is the
dominant error in the results from the HDF-N. Providing observations
in a field that is spatially uncorrelated is critically important. The
UDF/CDF-S fulfills that goal. The depth of the UDF ACS imaging, and
the wealth of Great Observatory and ground based observations in the
CDF-S, make these NICMOS observations uniquely valuable. An
extraordinarily rich array of science opportunities await the
community from the NICMOS UDF data.


NICMOS Post-SAA calibration - CR Persistence Part 2

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.

STIS 9606

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS 9608

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 9633

STIS parallel archive proposal - Nearby Galaxies - Imaging and

Using parallel opportunities with STIS which were not allocated by the
TAC, we propose to obtain deep STIS imagery with both the Clear
{50CCD} and Long-Pass {F28X50LP} filters in order to make
color-magnitude diagrams and luminosity functions for nearby galaxies.
For local group galaxies, we also include G750L slitless spectroscopy
to search for e.g., Carbon stars, late M giants and S-type stars. This
survey will be useful to study the star formation histories, chemical
evolution, and distances to these galaxies. These data will be placed
immediately into the Hubble Data Archive.

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 10000

STIS Pure Parallel Imaging Program: Cycle 12

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

WFPC2 9595


This dark calibration program obtains 3 dark frames every day to
provide data for monitoring and characterizing the evolution of hot

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.

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 0z1. 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


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

Executed Ops Note 1156:* Change Limits MAMA 1 Threshold Voltage @

****************************** Scheduled********** Successful
FGS Aquisitions************ 5************************* 5
FGS ReAcqs**************** 9************************* 9
FHST Updates************* 13*********************** 13


Completed FSW 2.4a RAM Installation/Backout and EEPROM Installation
OAT 252/10:11Z 253/01:55Z.* Both FSW 2.4a RAM Installation and
Backout (IP-42) and EEPROM Installation (IP-43) were completed
successfully.* In addition, IP-45 Enable/Disable/Preview Onboard
Magnetic Field Model Procedure was exercised in Preview Mode for 1
plus orbit.* At the end of the test, updated DMS,. TCLs: XSUBCWPF,
XSUBCWPN, QTABCHEK, and QTABCRD were run against the VEST using an
argument of 340, the new table value addition to the procedures.* This
completes Level 3 validation of these procedures.

Completed SUN Transition B Side Command testing 253/11:00Z 18:00Z.*
The SUN F String and SGI B String platforms compared nominally
through a series of command functions.* The test was run completely on
the B-side with Q, I, and S channel data being ingested.* No errors
were seen in telemetry.

Completed SDH/HSTPS Account Verification testing 252/11:02Z 19:55Z.
Testing was partially successful.* Compared D and F String results
against the B String.* Although, eventually got a Non-PN (RS)
encoded science SSR dump to work, it took 5 attempts to see success on
all strings.* Saw missing and incomplete packets first on D String,
then on F String, then Dand F and finally all three strings.*
All strings were on INTA, all objectives were eventually met.


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