NASA Hubble Space Telescope Daily Report # 3395
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3395
PERIOD COVERED: DOY 181
OBSERVATIONS SCHEDULED
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 are: {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.
NICMOS/STIS CCD 9405
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
galaxies.
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
ACS 9482
ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES}
Ly-alpha line emission is an efficient tool for identifying young galaxies
ACS 9565
ACS Post-SMOV UV Contamination Monitor
This programme continues the UV sensitivity monitoring campaign {ACS SMOV
WFPC2 9592
WFPC2 CYCLE 11 Standard Darks
This dark calibration program obtains dark frames every week in order to
WFPC2 9596
WFPC2 CYCLE 11 INTERNAL MONITOR
This calibration proposal is the Cycle 11 routine internal monitor for
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 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and
STIS/CAL 9609
CCD Read Noise Monitor
This proposal measures the read noise of all the amplifiers {A, B, C, D} on
STIS 9615
Cycle 11 MAMA Dark Monitor
This test performs the routine monitoring of the MAMA detector dark noise.
ACS/STIS 9664
SDSS Primary Standards
The ACS HRC and WFC cameras have Sloan Digital Sky Survey standard filters,
ACS 9674
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
STIS 9708
STIS Pure Parallel Imaging Program: Cycle 11
This is the default archival pure parallel program for STIS during cycle 11.
WFPC2 9709
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel
ACS/HRC/WFC 9728
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
ACS/HRC 9746
Binary systems in the Kuiper Belt
The properties of the orbits of Kuiper belt object {KBO} satellites hold
ACS 9984
Cosmic Shear With ACS Pure Parallels
Small distortions in the shapes of background galaxies by foreground mass
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
HSTAR 9065: GS Acquisition (2,3,3) @ 181/18:36:14Z resulted in FL backup
HSTAR 9066: GS Acquisition (1,2,2) @ 182/02:18:27Z, which began in ZOE
COMPLETED OPS REQs: NONE
OPS NOTES EXECUTED:
1115-0 CCC IP CONFIG Connections @ 181/10:10z
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 0
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.
proposal 9010} of the HRC and SBC after the end of the SMOV period.
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, 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.
1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.
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 1×1, 1×2, 2×1 and 2×2.
All
exposures are internals. Pairs of visits are scheduled for monthly
execution.
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.
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
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.
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.
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.
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.
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 ideal.
potential non-nominal performance that will be investigated.)
on FGS 2.
HST was in LOS at time of event, upon AOS, there
were no FGS flags indicating
SRLEX or SSLEX. Under investigation.
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.
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 13 13
FGS REacq 07 07
FHST Update 26 26
LOSS of LOCK
SIGNIFICANT EVENTS:
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.
