HST Daily Report #3343
HUBBLE SPACE TELESCOPE
DAILY REPORT #3343
PERIOD COVERED: DOY 106
OBSERVATIONS SCHEDULED
NICMOS 8791
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.
ACS/WFC 9351
Determining Hubble’s Constant from Observations of Cepheids in the Host
Galaxy of SN Ia 1994ae
the host spiral galaxy NGC 3370. Modern CCD photometry has yielded an
extremely tight Hubble diagram
for SNe Ia with a precisely determined intercept {i.e., Delta H_0/H_0} 1
measurement of the true Hubble
constant is still limited by the calibration. The HST calibration of
all but a few SNe Ia observed to
date is significantly compromised by the systematics of photographic
photometry and host galaxy
extinction, as well as by the photometric uncertainties associated with
WFPC2. In contrast, SN 1994ae
is one of the very best-observed SNe Ia with CCD photometry. The
exquisite B, V, R, and I light curves
are well-sampled beginning 10 days before maximum brightness, and they
indicate little reddening. From
our supernova photometry and the current provisional SN Ia calibration
we would find a distance of 30
+/- 2.1 Mpc, well within the range where ACS can accurately observe
Cepheid light curves and
distinguish Cepheids from nonvariable stars.
ACS 9352
The Deceleration Test from Treasury Type Ia Supernovae at Redshifts 1.2
to 1.6
Type Ia supernovae {SNe Ia} provide the only direct evidence for an
accelerating universe, an
extraordinary result that needs a rigorous test. The case for cosmic
acceleration rests on the
observation that SNe Ia at z ~ 0.5 are ~ 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 SN
Ia result attributed to grey dust or cosmic evolution of the SN Ia peak
luminosity would not show this
change of sign. We have demonstrated proof of this concept with a
single SN Ia, SN 1997ff at z = 1.7,
found and followed by HST. The results suggest an early epoch of
deceleration, but this is too
important a conclusion to rest on just one object. Here we propose to
use HST for observations of six
SNe Ia in the range 1.2 <= z <= 1.6, that will be discovered as a
byproduct from proposed Treasury
programs for high-latitude ACS surveys. Six objects will provide a much
firmer foundation for a
conclusion that touches on important questions of fundamental physics.
STIS/CCD/MA1 9357
Towards a global understanding of accretion physics –, Clues from an UV
spectroscopic survey
of cataclysmic variables
Accretion inflows and outflows are fundamental phenomena in a wide
variety of astrophysical
environments, such as Young Stellar Objects, galactic binaries, and AGN.
Observationally, cataclysmic
variables {CVs} are particularly well suited for the study of accretion
processes. We propose to carry
out a STIS UV spectroscopic snapshot survey of CVs that fully exploits
the diagnostic potential of
these objects for our understanding of accretion physics. This survey
will provide an homogenous
database of accretion disc and wind outflow spectra covering a wide
range of mass transfer rates and
binary inclinations. We will analyse these spectra with state-of-the-art
accretion disc model spectra
{SYNDISK}, testing our current knowledge of the accretion disc
structure, and, thereby, providing new
insight into the so far not well understood process of viscous
dissipation. We will use our
parameterised wind model PYTHON for the analysis of the radiation driven
accretion disc wind spectra,
assessing the fundamental question whether the mass loss rate correlates
with the disc luminosity. In
addition, our survey data will identify a number of systems in which the
white dwarf significantly
contributes to the UV flux, permitting an analysis of the impact of mass
accretion on the evolution of
these compact stars. This survey will at least double, if not triple,
the number of high-quality
accretion disc / wind outflow / accreting white dwarf spectra, and we
waive our proprietary rights to
permit a timely use of this database.
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.
ACS/WFC/HRC 9445
Gravitational Microlensing in the NGC 3314A-B Galaxy Pair.
The Advanced Camera for Surveys (WFC and HRC) was used to determine the
composition of the dark matter
that dominates the masses of galaxies which is an important unsolved
problem.
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
data for monitoring and
characterizing the evolution of hot pixels
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 1×1 at gain = 4, to build up
high-S/N superbiases and track the evolution of hot columns.
STIS 9614
STIS CCD Imaging Flats C11
Investigate flat-field stability over a monthly period.
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.
STIS/CAL 9628
MAMA Sensitivity and Focus Monitor Cycle 11
Monitor sensitivity of each MAMA grating mode to detect any change due
to contamination or other
causes. Also monitor the STIS focus in a spectroscopic and imaging mode.
ACS 9649
ACS internal CTE monitor
The charge transfer efficiency {CTE} of the ACS CCD detectors will
decline as damage due to on-orbit
radiation exposure accumulates. This degradation will be closely
monitored at regular intervals,
because it is likely to determine the useful lifetime of the CCDs. All
the data for this program is
acquired using internal targets {lamps} only, so all of the exposures
should be taken during Earth
occultation time {but not during SAA passages}. This program emulates
the ACS pre-flight ground
calibration and post-launch SMOV testing {program 8948}, so that results
from each epoch can be
directly compared. Extended Pixel Edge Response {EPER} and First Pixel
Response {FPR} data will be
obtained over a range of signal levels for both the Wide Field Channel
{WFC}, and the High Resolution
Channel {HRC}.
ACS 9658
ACS Earth Flats
This program will obtain sequences of flat field images by observing the
bright Earth. Several UV
filters from the interim calibration program {9564} require additional
exposures to obtain the required
illumination. A few UV filters from this program will be repeated to
monitor for changes in the flat
fields and to verify the interim results. Since no streaks are observed
in the UV, the wavelength
coverage is extended to longer wavelengths in order to explore the
severity of streaks in the flats
from clouds in the FOV. We have added exposures for the HRC in the
visible filters to verify the
results derived from the L-flat campaign and to explore the severity of
streaks. We have also added
exposures on WFC using the minimum exposure time and using filters which
will not saturate the
brightest WFC pixel by more than 10 times the full well.
ACS 9673
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 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle
10.
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 paralell images of random areas of the sky, following the
recommendations of the 2002
Parallels Working Group.
WFPC2 9710
POMS Test Proposal: WFII backup parallel archive proposal
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies:
(The following are preliminary reports of potential non-nominal
performance that will be investigated.)
HSTARs:
8991 – Failure of Track to schedule for TDRS-J Test @ 099/1306z
COMPLETED OPS REQs:
None
OPS NOTES EXECUTED:
1098-0 – Document limits for FSW Main Bus C Voltage Monitor @ 106/1852z
SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 4 4 FGS REacq 12 12 FHST Update 7 7 LOSS of LOCK
