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[email protected] July 1st 03 07:23 PM

Daily 3395


DAILY REPORT******* # 3395



ACS/HRC 9379

Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the
Starburst-AGN Connection

We propose a near-UV snapshot survey of 101 Seyfert galaxies using
ACS/HRC and the filter F330W, a configuration which is optimal to
detect faint star forming regions around their nuclei. These images
will complement optical and near-IR images available in the HST
archive, thus providing a panchromatic atlas of the inner regions of
active galaxies, which we will use to study the starburst-AGN
connection. The main goals of this proposal a {1} Determine the
frequency of circumnuclear starbursts in Seyferts, down to levels
which cannot be observed from the ground; {2} characterize the
observational {fluxes, colors, structure, sizes} and intrinsic
{luminosities, masses, ages, global star-formation rate} properties of
these clusters; {3} derive the luminosity functions of young star
clusters around the nucleus of Seyferts and compare these results with
those from normal and starburst galaxies to determine their survival
rate close to the AGN; {4} address questions about the relation
between AGNs and starbursts, like the possible connection between the
masses and luminosities of black holes and starbursts, and the
implications for the evolution of the black holes and their host
galaxy bulges. By adding UV images to the existing optical and near-IR
ones, this project will create an extremely valuable database for
astronomers with a broad range of scientific interests, from the
properties of the AGN to the properties of their host galaxies.


The Origin of Gamma-Ray Bursts

The rapid and accurate localization of gamma-ray bursts {GRBs}
promised by a working HETE-2 during the coming year may well
revolutionize our ability to study these enigmatic, highly luminous
transients. We propose a program of HST and Chandra observations to
capitalize on this extraordinary opportunity. We will perform some of
the most stringent tests yet of the standard model, in which GRBs
represent collimated relativistic outflows from collapsing massive
stars. NICMOS imaging and STIS CCD spectroscopy will detect broad
atomic features of supernovae underlying GRB optical transients, at
luminosities more than three times fainter than SN 1998bw. UV,
optical, and X-ray spectroscopy will be used to study the local ISM
around the GRB. Chandra spectroscopy will investigate whether the GRB
X-ray lines are from metals freshly ripped from the stellar core by
the GRB. HST and CTIO infra-red imaging of the GRBs and their hosts
will be used to determine whether `dark' bursts are the product of
unusually strong local extinction; imaging studies may for the first
time locate the hosts of `short' GRBs. Our early polarimetry and
late-time broadband imaging will further test physical models of the
relativistic blast wave that produces the bright GRB afterglow, and
will provide unique insight into the influence of the GRB environment
on the afterglow.

STIS 9415

Is the Compact HVC Toward Ton S210 Remnant Debris from the Formation
of the Local Group?

There is a fortuitous coincidence in the positions of the quasar Ton
S210 and a compact ionH1 high velocity cloud on the sky that makes it
possible to test the hypothesis that such clouds are extragalactic
entities located in the Local Group. The HVC toward Ton S210 has H I
21 cm emission properties similar to those of isolated compact HVCs
suspected of being Local Group clouds. It has recently been detected
in O VI absorption by FUSE, which suggests that either there is hot
gas associated with the collapse of the cloud or that the HVC is
interacting with a hot, tenuous Galactic halo or Local Group medium.
We propose to observe the HVC in absorption against the smooth
ultraviolet continuum of Ton S210 with HST/STIS. To answer the
question posed in the proposal title, we will combine the STIS
observation with extant FUSE and H I 21 cm data to determine the
metallicity, elemental abundances, and ionization properties of the
HVC. To date, such information has been difficult to obtain for all
but a few HVCs, and this is the first time such an opportunity has
been available for a compact HVC. The results of this study will bear
directly upon the issues of the locations of compact HVCs, the
ionization conditions of HVCs detected in O VI absorption, and the
possible influence HVCs might have on the chemical evolution of

ACS/WFPC2 9481

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

ACS 9482

ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES}

Ly-alpha line emission is an efficient tool for identifying young
galaxies at high redshift, because it is strong in galaxies with young
stars and little or no dust --- properties expected in galaxies
undergoing their first burst of star- formation. Slitless spectroscopy
with the ACS Wide-Field Camera and G800L grism allows an unmatched
search efficiency for such objects over the uninterrupted range 4 ~ z
~ 7. We propose the ACS Pure Parallel Ly-alpha Emission Survey
{``APPLES''}, to exploit this unique HST capability and so obtain the
largest and most uniform sample of high redshift Ly-alpha emitters
yet. Parallel observations will allow this survey to be conducted with
minimal impact on HST resources, and we will place reduced images and
extracted spectra in the public domain within three months of
observation. We aim to find ~ 1000 Ly-alpha emitters, 5 times the
biggest current sample of Ly-alpha emitters. This unprecedented sample
will provide robust statistics on the populations and evolution of
Ly-alpha emitters between redshifts 4--7; a robust measurement of the
reionization redshift completely independent of the Gunn-Peterson
trough; spatial clustering information for Ly-alpha emitters which
would let us probe their bias function and hence halo mass as a
function of redshift; many galaxies at redshift exceeding 6; and lower
redshift serendipitous discoveries.

ACS 9565

ACS Post-SMOV UV Contamination Monitor

This programme continues the UV sensitivity monitoring campaign {ACS SMOV
proposal 9010} of the HRC and SBC after the end of the SMOV period.

WFPC2 9592

WFPC2 CYCLE 11 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.

WFPC2 9596


This calibration proposal is the Cycle 11 routine internal monitor for
WFPC2, to be run weekly to monitor the health of the cameras. A
variety of internal exposures are obtained in order to provide a
monitor of the integrity of the CCD camera electronics in both bays
{gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a
monitor for possible buildup of contaminants on the CCD windows.

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.


CCD Read Noise Monitor

This proposal measures the read noise of all the amplifiers {A, B, C,
D} on the STIS CCD using pairs of bias frames. Full frame and binned
observations are made in both Gain 1 and Gain 4, with binning factors
of 1x1, 1x2, 2x1 and 2x2. All exposures are internals. Pairs of visits
are scheduled for monthly execution.

STIS 9615

Cycle 11 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
noise. This proposal will provide the primary means of checking on
health of the MAMA detectors systems through frequent monitoring of
the background count rate. The purpose is to look for evidence of
change in dark indicative of detector problem developing.


SDSS Primary Standards

The ACS HRC and WFC cameras have Sloan Digital Sky Survey standard
filters, the first use of these on HST. Calibration of the u, g, r, i,
z filters in ACS will be obtained in order to assure that observers
can place HST and SDSS observations on a common system. The SDSS has
adopted the 10th magnitude star, BD+17D4708 as their fundamental
reference. STIS calibration spectra of this will be obtained over the
full 0.2-1.0+ micron range covered by G230LB, G430L and G750L in order
to generate a reference spectrum of this star in the HST system in
order for SYNPHOT to generate robust synthetic magnitudes {the STIS
observations are through the STIS program, 9631, Bohlin PI}. ACS
observations will be obtained through the SDSS filters in order to
reference u, g, r, i, z photometry to the same fundamental standard
used by SDSS. In addition, since this will become a useful additional
standard star, we will also obtain observations through the full suite
of ACS UV-optical filters in order to assist photometric
transformations between different systems

ACS 9674

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.

STIS 9708

STIS Pure Parallel Imaging Program: Cycle 11

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

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.


Tracing the History of Cosmic Expansion to z~2 with Type Ia Supernovae

Type Ia supernovae {SNe Ia} provide the only direct evidence for an
accelerating universe, an extraordinary result that needs the most
rigorous test. The case for cosmic acceleration rests on the
observation that SNe Ia at z = 0.5 are about 0.25 mag fainter than
they would be in a universe without acceleration. A powerful and
straightforward way to assess the reliability of the SN Ia measurement
and the conceptual framework of its interpretation is to look for
cosmic deceleration at z 1. This would be a clear signature of a
mixed dark-matter and dark-energy universe. Systematic errors in the
SNe Ia result attributed to grey dust or cosmic evolution of the SN Ia
peak luminosity would not show this change of sign. We have obtained a
toehold on this putative ``epoch of deceleration'' with SN 1997ff at z
= 1.7, and 3 more at z 1 from our Cycle 11 program, all found and
followed by HST. However, this is too important a test to rest on just
a few objects, anyone of which could be subject to a lensed
line-of-sight or misidentification. Here we propose to extend our
measurement with observations of twelve SNe Ia in the range 1.0 z
1.5 or 6 such SNe Ia and 1 ultradistant SN Ia at z = 2, that will be
discovered as a byproduct from proposed Treasury and DD programs.
These objects will provide a much firmer foundation for a conclusion
that touches on important questions of fundamental physics.

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 9984

Cosmic Shear With ACS Pure Parallels

Small distortions in the shapes of background galaxies by foreground
mass provide a powerful method of directly measuring the amount and
distribution of dark matter. Several groups have recently detected
this weak lensing by large-scale structure, also called cosmic shear.
The high resolution and sensitivity of HST/ACS provide a unique
opportunity to measure cosmic shear accurately on small scales. Using
260 parallel orbits in Sloan textiti {F775W} we will measure for the
first time: beginlistosetlength sep0cm setlengthemsep0cm setlength
opsep0cm em the cosmic shear variance on scales 0.7 arcmin, em the
skewness of the shear distribution, and em the magnification effect.
endlist Our measurements will determine the amplitude of the mass
power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20,
and the mass density Omega_m with s/n=4. They will be done at small
angular scales where non-linear effects dominate the power spectrum,
providing a test of the gravitational instability paradigm for
structure formation. Measurements on these scales are not possible
from the ground, because of the systematic effects induced by PSF
smearing from seeing. Having many independent lines of sight reduces
the uncertainty due to cosmic variance, making parallel observations


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

HSTAR 9065:* GS Acquisition (2,3,3) @ 181/18:36:14Z resulted in FL
backup on FGS 2. HST was in LOS at time of event, upon AOS, there were
no FGS flags indicating SRLEX or SSLEX. Under investigation.

HSTAR 9066:* GS Acquisition (1,2,2) @ 182/02:18:27Z, which began in
ZOE period, resulted in FL backup (1,0,1) using FGS 1 due to SSLE on
FGS 2.* See HSTAR 9064, used same double star. Under investigation.


1115-0* CCC IP CONFIG Connections @ 181/10:10z

************************* SCHEDULED**** SUCCESSFUL*** FAILURE TIMES
FGS GSacq************* 13********************** 13
FGS REacq************* 07*********************** 07
FHST Update*********** 26*********************** 26


Battery 4 Capacity Test started on schedule at 1st opportunity (OR
16996-1 with attached Battery 4 Capacity Test script).

SM-4 SMGT SR 3.1.1 System Readiness test was completed on schedule.*
Main objectives were verified.

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