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Daily 3631

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Old June 11th 04, 05:22 PM
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Default Daily 3631

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science





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.


Galaxy Evolution in Action : The Detailed Morphology of Post-Starburst

If galaxies evolve morphologically, then some should be in transition
between late and early types. One proposed evolutionary mechanism is a
galaxy-galaxy merger, but evolved merger products are difficult to
find. Fortunately, spectroscopic surveys have now uncovered large
numbers of E+A galaxies, a class of objects whose post-starburst
spectra, current lack of HI gas, and pressure-supported kinematics
suggest that they are the missing panel that connects the "Toomre
sequence" of merging spirals with normal ellipticals and S0s. Our
first HST observations of five of these galaxies are intriguing. We
find a considerable range of tidally disturbed morphologies, an "E+A"
fundamental plane, significant differences among the color gradients
within 1 kpc {~0.8''}, and populations of bright, blue globular
clusters. These initial results are difficult to interpret, however,
because they are drawn from a small sample of galaxies whose very blue
overall colors may have selected a particular evolutionary path of
E+As. Here we propose for ACS imaging of the remaining 15 E+As from
the Las Campanas Redshift Survey to probe the full range of E+A
properties. The proposed observations will allow us to 1} determine
what fraction of the interactions that lead to E+As destroy all
disk-like structures {and therefore necessarily lead to elliptical
formation}, 2} measure the inner color gradients and constrain the
spatial distribution of stars produced as gas sinks to the center
during a merger, and 3} determine whether these interactions produce
globular clusters in the required numbers to account for the increased
specific frequency of clusters in early-type galaxies.

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. 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.

ACS/WFC 9777

The environment of QSOs at the reionization epoch

Our goal is to elucidate the role of QSOs and galaxies at the tail end
of reionization by identifying z~6 galaxies near SDSS z6 QSOs through
their red i-z colors. A similar technique was used by the SDSS to
identify the QSOs themselves. Based on our understanding of the growth
of structure in the Universe and on observations at z ~= 4, we expect
z~6 QSOs to be associated to the high peaks in the matter density
distribution. Therefore, they should be surrounded by an excess of
objects - as compared to random fields - unless the ionizing radiation
from the QSOs themselves is inhibiting star formation. We will
concentrate on 5 QSOs discovered by the SDSS at z~6 and spend 7
orbits with ACS on each of the QSO fields {2.5 in F775W - i - and 4.5
in F850LP - z}, for a total of 35 orbits. The exposures are optimized
for the detection of objects with i-z 2. The reference properties of
the field population will be provided by GOODS which is reaching the
same depth. The proposed observations will be capable of revealing the
dominant effect between galaxy suppression by the QSO ionizing flux
and number density excess due to clustering. We will test whether the
balance between suppression and enhancement evolves with redshift. We
will also be able to estimate for these fields the ionizing continuum
contribution by galaxies and compare it with that of the QSOs. If
galaxies are found to be comparably important to QSOs in these
selected fields, the idea that hydrogen reionization is primarily due
to stellar radiation would be significantly strengthened.

ACS/WFC 9902

The Evolution of the Host Galaxies of Radio-Quiet Quasars

Study of the host galaxies and environments of high redshift AGN is
proving a valuable probe of current theories of how galaxies form and
evolve. Results from our NICMOS imaging program have indicated that
the hosts of z ~ 2 -- 3 faint radio-quiet quasars {RQQ} have
luminosities only around local L*, making them similar to Lyman-break
field galaxies at the same redshifts, and to the low-z hosts RQQ
hosts. This is roughly consistent with theoretical predictions of
Kauffmann & Haehnelt {2000} for the hierarchical buildup of galaxy
hosts and their relation to their resident supermassive black holes.
The luminosity of the AGN in these RQQ is key to understanding this
relationship, however, and we are making a comprehensive archival HST
imaging study of the hosts of RQQs from low to high z at a range of
nuclear luminosities. At intermediate z, however, there are no studies
of the hosts of RQQs in the faint luminosity range that represents the
bulk of the quasar population. In the present proposal, we request
imaging at the same rest-wavelengths as our high-z sample of the hosts
of 10 similarly luminous RQQs at z ~ 0.9. These data will fill in an
important part of the parameter space defined by quasar luminosity and
redshift. Combined with existing HST data they will allow us to trace
the evolution of the hosts of RQQ and that of the relationship between
quasar luminosity and host galaxy luminosity.

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 9993

Cycle 12 NICMOS dark current, shading profile, and read noise
monitoring program

The purpose of this proposal is to monitor the dark current, read
noise, and shading profile for all three NICMOS detectors throughout
the duration of Cycle 12. This proposal is an essentially unchanged
continuation of PID 9636 which cover the duration of Cycle 11.

NIC2 9875

The Fundamental Plane of Massive Gas-Rich Mergers

We propose deep NICMOS H-band imaging of a carefully selected sample
of 33 luminous, late-stage galactic mergers. This program is part of a
comprehensive investigation of the most luminous mergers in the nearby
universe, the ultraluminous infrared galaxies {ULIGs}. The
high-resolution HST images will complement an extensive set of
ground-based data that include long-slit NIR spectra from a recently
approved Large VLT Programme. This unique dataset will allow us to
derive with unprecedented precision structural -and- kinematic
parameters for a large unbiased sample of objects spanning the entire
ULIG luminosity function. These data will refine the fundamental plane
of massive gas-rich mergers and enable us to answer the following
questions: {1} Do ultraluminous mergers form elliptical galaxies, and
in particular, giant ellipticals? {2} Do ULIGs evolve into optically
bright QSOs? The results from this detailed study of massive mergers
in the local universe will be relevant to understanding galaxy
formation and evolution at earlier epochs, and in particular, the
dusty sub-mm population that accounts for more than half of the star
formation at z 1.

STIS/CCD 10018

CCD Dark Monitor-Part 2

Monitor the darks for the STIS CCD.

STIS/CCD 10022

STIS CCD Hot Pixel Annealing Cycle 12

The effectiveness of the CCD hot pixel annealing process is assessed
by measuring the dark current behavior before and after annealing and
by searching for any window contamination effects. In addition CTE
performance is examined by looking for traps in a low signal level
flat. Follows on from proposal 9612.


Iron deficiency in hot hydrogen-deficient post-AGB stars

The first attempt to measure the iron abundance in hot
hydrogen-deficient post-AGB stars arrived at a surprising result. From
the non-detection of iron lines in FUSE spectra of three extremely hot
{Teff100, 000K} PG1159-type central stars of the planetary nebulae,
we found that iron is deficient by at least one order of magnitude. We
propose HST/STIS observations of three hydrogen-deficient post-AGB
stars, each representing the UV-brightest member of a spectroscopic
subclass. High-resolution UV spectroscopy will reveal the origin of
the iron deficiency. The determination of the Fe/Ni abundance ratio
can decide if dust fractionation in the former AGB star atmosphere or
s-process neutron-capture in the interior helium-buffer layer is
responsible for the iron depletion. In the latter case we can verify
our understanding of the "born-again'' star phenomenon and of the
s-process synthesis of trans-iron elements in low-mass AGB stars.

WFPC2 10071

WFPC2 CYCLE 12 Supplemental Darks Part 3/3

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

WFPC2 9817

The mass of the Milky Way: orbits for Leo I and Leo II

Constraining the mass of the galaxy at large radii remains a difficult
problem. Available data are still rather scarce, and orbits of even a
few objects at large radii can have a large impact. We propose to
obtain proper motions for the two satellites Leo I and Leo II, which
orbit the Galaxy at about 200kpc. Together with the radial velocities
of these galaxies, which are well-known, the proper motions allow
space velocities to be constructed: these can remove significant
uncertainty in the Galactic mass models, and in particular settle the
vexed question whether Leo I is gravitationally bound to the Galaxy or


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


1243 - Adjust Recharge Ratio Limits for High Sun DOY 2004/155-169 @ 162/1222z

GSacq 7 7
FGS REacq 9 9
FHST Update 8 8


Set-up and execution of CCS Release CT Verification Test
scheduled 163/11:00Z - 19:00Z with GDOC, HITT, and SOC using CCS "H"
String with CCS Release and PRD xxx (intentionally removed).
The purpose of this testing is to verify GSCA 793 Packet Filter 13


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