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Daily 3634



 
 
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Old June 16th 04, 09:00 PM
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Default Daily 3634

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3634

PERIOD COVERED: DOY 167

OBSERVATIONS SCHEDULED

ACS/HRC 10050

ACS Earth Flats

High signal sky flats will be obtained by observing the bright Earth
with the HRC and WFC. These observations will be used to verify the
accuracy of the flats currently used by the pipeline and will provide
a comparison with flats derived via other techniques: L-flats from
stellar observations, sky flats from stacked GO observations, and
internal flats using the calibration lamps. Weekly coronagraphic
monitoring is required to assess the changing position of the spots.

ACS/HRC 9703

Coronagraphic Search for Planets around Nearby Stars

We will use the HRC coronagraph to search for planets, disks, and
exo-zodiacal dust around nearby stars. We have selected the following
stars: alpha Cen A and B, tau Ceti, and epsilon Eridani. The
observations of each star will be taken at two or more epochs. The
observations will be broken into a sequence of short exposures and
taken at different roll angles to compensate for "telescope breathing"
during the orbit. As a further precaution, the observations will be
scheduled after the closest possible nearby pointing in order to
minimize thermal changes in the OTA during the first orbit of
observations. After matching phases, the PSFs from one star will be
subtracted from the other star.

ACS/HRC 9896

A Survey of Extinction Curves to Redshift z=1

The effects of dust are crucial to the study of galaxies {through
models of galaxy evolution and star formation rates/histories},
cosmology {e.g., through its effects on SNe Ia fluxes}, and the
interpretation of gamma-ray burst afterglows. However, classical
methods for obtaining precise extinction curves cannot be applied
outside the Local Group. Recently, we demonstrated that gravitational
lenses can be used to measure extinction curves at intermediate
redshifts with high accuracy. We propose a survey of the extinction
curves in 6 lens galaxies known to contain dust, to study the
evolution of dust properties in galaxies out to z=1. We will obtain
multi-wavelength photometry {6 filters from 8140 A to 2550 A} of each
system to {1} construct non-parametric extinction curves which overlap
the 2175 A feature, {2} measure R{V} to a 2-sigma accuracy better than
0.5 for parametric models of Galactic dust, and {3} discriminate
between Galactic and SMC extinction curves to better than 2-sigma
accuracy. The compact angular size of the lens systems {1-2 arcsec}
and the need for near-UV images means that HST is required to make the
measurements.

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/HRC 9771

The local Hubble flow and the density field within 6 Mpc

Great progress has been made recently in accurate distance
measurements of nearby galaxies beyond the Local Group based on the
luminosity of the tip of the red giant branch {TRGB}. Over the last
three years, snapshot surveys with HST have provided us with the TRGB
distances for more than a hundred nearby galaxies obtained with an
accuracy of about 10%. The local velocity field within 5 Mpc exhibits
a significant anisotropy which disagrees with a spherical
Virgo-centric flow. The local Hubble flow is very cold, with 1-D rms
deviations of ~30 km/s. Cosmological simulations with Cold Dark Matter
can only realize such low dispersions with a combination of a low mean
density of matter and a substantial component with negative pressure.
There may be a constraint on the equation of state w=-p/rho. Our
observations will concentrate on 116 galaxies whose expected distances
lie within 4 - 6 Mpc, allowing us to trace a Dark Matter distribution
in the Local Volume with twice the information currently available.
The program is a good one for SNAP mode because the order and rate
that the observations are made are not very important, as long as
there is good completion over several years.

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.

NIC2 9856

A near-IR imaging survey of submm galaxies with spectroscopic
redshifts

Submillimeter {submm} surveys with SCUBA have identified a population
of obscured star-forming and active galaxies at high redshift. Our
recent spectroscopic campaigns with the Keck-10m telescope have
uncovered redshifts for 37 SCUBA galaxies. The wide redshift range of
the radio identified submm population {z=1-4} implies that many
varieties of sources driven by different physical processes may be
selected in a submm survey. We propose to use HST-NICMOS, ACS to
obtain 2-filter images of a sample of 15 SCUBA galaxies with redshifts
spanning z=0.8-3.5. Our goal is to understand what physical process
{major mergers?} drive their strong evolution and great luminosities,
and what the implications are for galaxy evolution models.

NIC3 9878

The Age and Mass Function of the Intermediate Age Globular Cluster
System of NGC 4365

We propose to obtain deep H-band photometry of the globular cluster
system of the elliptical galaxy NGC 4365, which has previously been
shown from shallow data to have a significant population of
intermediate-age globular clusters. These data will allow us to
constrain the luminosity and mass function of the intermediate-aged
globular cluster system. This is a critical step in understanding the
relationship between the young dense star cluster systems observed in
galaxy mergers and starbursts, which have a power-law mass functions,
and well known old, globular cluster systems, which have a lognormal
mass functions. Specifically, the large intermediate-age cluster
population in NGC 4365 provides the best case to test whether the
power-law mass function of young systems evolves into a lognormal with
the properties of old globular cluster systems. Dynamical models have
long suggested such an evolution of a power-law mass function to a
roughly log-normal one but there is no clear observational evidence
yet in elliptical galaxies for steps along this process. Our proposed
study of the intermediate-age cluster system of NGC 4365 will provide
us with the fundamental information needed to conclusively establish
the relationship between young and old globular cluster systems.

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.

STIS/CCD 10030

STIS/CCD Spectroscopic Sensitivity Monitor for Cycle 12

Monitor sensitivity of each CCD grating mode to detect any change due
to contamination or other causes.

STIS/CCD/MA1/MA2/WFPC2 9828

Young Massive Clusters in M33

Young Massive Clusters {YMC} appear to be abundantly forming in
merging galaxies, but are not found in the Milky Way. They provide the
opportunity to study the conditions necessary for the formation of
massive, compact stellar systems, giving insight into conditions of
the earliest epochs of galaxy formation, when ancient Globular
Clusters {GC} formed, thus helping to constrain scenarios of galaxy
formation and evolution. We propose STIS UV spectroscopy of three
extremely young, UV-luminous clusters in the Local Group spiral galaxy
M33, selected from our extensive survey with WFPC2 imaging. From
multi-band integrated photometry we inferred age upper limits of 10
Myrs: UV spectra will provide precise ages, thus masses, for these
objects from the earliest spectral types present, revealed by the
strong spectral signatures, and from synthetic spectral modeling. We
will be able to assess whether their mass overlap with GC masses, and
whether such systems can survive internal dynamical evolution. These
young, massive and compact objects provide a key link to the young
cluster systems in mergers, and may be the only such counterparts
accessible to detailed studies.

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
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: None

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 9 9
FGS REacq 4 4
FHST Update 16 16
LOSS of LOCK

SIGNIFICANT EVENTS:

An additional series of FHST Rate Control and Intensity data
collections (6 each) are scheduled during SMS SA166O01 on Days 168
through 170. These activities provide additional high-rate FHST data
in support of the development of the T2G mode of the Two Gyro Science
effort. Each of the 12 intervals involves a brief (10 - 15 minutes)
transition to PN format and utilizes 4 TMDIAG slots. The 6 Intensity
collections also involve the DIU Reader. Total time in PN format
during the three days should be 170 minutes. All commanding is
conducted on a non interference basis (NIB) with routine or
contingency spacecraft activities. Periods of scheduled astrometry and
other critical science with SMS SA166O01 is specifically avoided. See
Ops Request for details.

Intensity:
FHST2 168/21:09:30 - 168/21:40:19Z
FHST1 168/23:47:35 - 169/00:23:00Z
FHST3 168/23:47:35 - 169/00:23:00Z


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