HST Daily Report # 3305
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3305
PERIOD COVERED: DOYs 52-54
OBSERVATIONS SCHEDULED
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
ACS 9462
Systemic and Internal Proper Motions of the Magellanic Clouds from
Astrometry
with ACS
We request first epoch observations with ACS of Magellanic Cloud fields
centered
on background quasars. Second epoch observations will be requested ~ 5
years
later to allow the measurement of the systemic and internal proper
motions of
the Clouds with error <~0.05 mas/year. These motions are of fundamental
importance. The systemic motions of the LMC and SMC probe the
gravitational
potential of the dark halo. The internal proper motion due to rotation
can be
exploited to yield a rotational parallax distance to the LMC; the first
time
that this will be done for any galaxy. This is particularly important for
the
LMC because of its crucial role in the extragalctic distance ladder.
Previous
measurements of the proper motion of the LMC yield a systemic component
ranging
from 1.4 mas/year to 3.4 mas/year {differing by several times the quoted
errors}, with no useful determination of the internal motions. The main
problem
with measurements of the proper motion of the LMC has been the lack of a
sample
of background quasars to use as reference frame. We have recently been
able to
identify a sample of 54 quasars behind the Magellanic Clouds from their
variability characteristics in the MACHO database. With this sample and
the
advent of ACS an accurate proper motion measurement has become possible
for the
very first time.
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.
ACS 9583
The Great Observatories Origins Deep Survey: Imaging with ACS
We propose a Treasury program of ACS imaging as part of the Great
ACS/WFC 9584
ACS Default {Archival} Pure Parallel Program II.
The Advanced Camera for Surveys (WFC) was used to test ACS pure
ACS/WFC 9575
Default {Archival} Pure Parallel Program.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels
ACS/WFPC2 9488
Cosmic Shear – with ACS Pure Parallel Observations
The ACS, with greater sensitivity and sky coverage, will extend our
ACS/WFPC2 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
In anticipation of the allocation of ACS high-latitude imaging survey{s},
FGS 9348
The Distances to AM CVn stars
We propose to determine the parallaxes and proper motions of the five
HST 9382
A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO
MgII-FeII Systems.
We have searched the first public release of SDSS QSO spectra for low-z
NICMOS 9485
Completing A Near-Infrared Search for Very Low Mass Companions to Stars
Most stars are fainter and less massive than the Sun. Nevertheless, our
NICMOS 9324
Gain Test
Test of the viability and advantaged of multiple NICMOS gain settings
NICMOS 8791
NICMOS Post-SAA calibration – CR Persistence Part 2
A new procedure proposed to alleviate the CR-persistence problem of
NICMOS 9360
Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample
We propose to carry out a NICMOS snapshot survey in the Paschen-alpha
STIS 9607
CCD Bias Monitor – Part 1
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1,
STIS 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9615
Cycle 11 MAMA Dark Monitor
This test performs the routine monitoring of the MAMA detector dark
STIS 9612
STIS CCD Hot Pixel Annealing Cycle 11
The effectiveness of the CCD hot pixel annealing process is assessed by
STIS 9625
STIS NUV-MAMA Cycle 11 Flats
This program will obtain NUV-MAMA observations of the STIS internal
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle
STIS/CCD/MA1 9357
Towards a global understanding of accretion physics –, Clues from an UV
Accretion inflows and outflows are fundamental phenomena in a wide
STIS/MA1 9343
The UV Light Echo of Shock Breakout During SN 1987A
Light echoes {transient reflection nebulae} from SN1987A were discovered
WFPC2 9676
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
HSTAR 8938: GS Re-acquisition (3,2,2) @ 053/13:03:13Z failed to RGA
HSTAR 8939: GS Acquisition (3,2,3) @ 053/17:19:07Z resulted in FL back
COMPLETED OPS REQs:
OPS NOTES EXECUTED:
SIGNIFICANT EVENTS:
Observatories
Origins Deep Survey {GOODS}, covering 320{square}’, or 32* the area of
the two
original WFPC2 HDFs, to within 0.5–0.8 mag of their depth in four ACS
bands,
BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep
Field
South, are the premier deep survey areas from X– ray to radio
wavelengths. ACS
data will provide unique angular resolution, sensitivity, and wavelength
coverage to close the gap between the deepest Chandra and SIRTF
observations.
Supported by extensive imaging and spectroscopy from the VLT, Keck,
Subaru,
NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data
set will
make it possible to map the evolution of the Hubble sequence with
redshift,
reconstruct the history of galaxy mass assembly, star formation and
nuclear
activity from the epoch of reionization to the present, trace the growth
of
density perturbations via cosmic shear, and, with properly phased z–band
observations, detect ~ 12 Type Ia supernovae at 1.2
parallels.
in
POMS.
ability to
measure the weak gravitational lensing of galaxy images caused by the
large
scale distribution of dark matter. We propose to use the ACS in pure
parallel
{non- proprietary} mode, following the guidelines of the ACS Default Pure
Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have
measured cosmic shear at arc-min angular scales. The MDS image
parameters, in
particular the galaxy orientations and axis ratios, are such that any
residual
corrections due to errors in the PSF or jitter are much smaller than the
measured signal. This situation is in stark contrast with ground-based
observations. We have also developed a statistical analysis procedure to
derive
unbiased estimates of cosmic shear from a large number of fields, each of
which
has a very small number of galaxies. We have therefore set the stage for
measurements with the ACS at fainter apparent magnitudes and smaller, 10
arc-second scales corresponding to larger cosmological distances. We will
adapt
existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to
work
with the ACS. The analysis would also yield an online database similar to
that
in archive.stsci.edu/mds/
Survey
Fields
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 0
brightest
of the seven known AM CVn systems using the HST Fine Guidance Sensors. AM
CVn
systems are binaries where mass is transferred from a completely
hydrogen-deficient, degenerate mass donor to a white dwarf primary
through a
helium accretion disk. A better understanding of these systems is crucial
for a
number of reasons:, to study the late stages of binary evolution, to
study the
effect of chemical composition on the physics of accretion discs; , o to
estimate their contribution to the Supernovae Ia rate and , to estimate
their
contribution to the gravitational radiation background. All these studies
rely
critically on a determination of the distances to the currently known
systems.
With brightnesses in the range 13
{z<1.65}
metal absorption lines and found over 200 large rest equivalent width
MgII-FeII
systems. Previously, we empirically showed that such systems are good
tracers of
large neutral gas columns, with ~50% being classical damped Lyman alpha
{DLA}
systems {N_HI>=2*10^20 cm^-2}. Here we propose to follow up a
well-defined
subset of 79 of them to search for DLAs with 0.47
within
10 pc of the Sun
knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins
is
quite limited. Unknown are the true luminosity function {LF},
multiplicity
fraction, mass function, and mass-luminosity relation for red and brown
dwarfs,
though they dominate the Galaxy in both numbers and total mass. The best
way to
constrain these relations is a search for faint companions to nearby
stars.
Such
a search has several advantages over field surveys, including greater
sensitivity to VLM objects and the availability of precise parallaxes
from
which
luminosities and masses can be derived. We propose to complete our
four-filter
NICMOS snapshot search for companions to stars within 10 pc. With a 10
sigma
detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10
and
100 AU that are at least 9 mag fainter than the empirical end of the main
sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When
completed, our search will be the largest, most sensitive, volume-limited
search
for VLM companions ever undertaken. Our four-filter search will permit
unambiguous identification of VLM-companion candidates for follow-up
observation. Together with IR speckle and deep imaging surveys, our
program
will
firmly establish the LF for VLM companions at separations of 1-1000 AU
and the
multiplicity fraction of all stars within 10 pc.
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.
{PAlpha}
emission line and H-band of the sample of galaxies being observed at 3.5
— 160
microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related
guaranteed
time survey of starburst galaxies. The PAlpha images, accessible only
from HST,
will be combined with groundbased HAlpha imaging to measure the
extinction in
the star-forming centers of these galaxies, and obtain robust,
extinction-
corrected maps of the massive star formation rate {SFR}. The PAlpha data
by
themselves will provide reliable `extinction- free’ SFRs, and a
cross-calibration of the {dust–affected} HAlpha– and UV–based SFRs.
The
PAlpha–based SFR measurements will extend the SFR-vs.-gas density law
{Schmidt–law} to surface densities at least 30 times higher than what is
accessible using HAlpha–based SFR measurements alone, bridging the gap
between
normal galaxies and IR–luminous starbursts. Furthermore, the combination
of the
HST PAlpha images with the SIRTF images and spectra, as well as ancillary
ground–based UBVRIJHK images and GALEX UV images being obtained as part
of the
SINGS project, will provide a definitive study of the radiative transfer
of
starlight and dust heating in star–forming galaxies. The processed
NICMOS
images will be incorporated into the public SINGS Legacy Data Archive, to
enable
scores of follow-up studies by the astronomical community at large.
and 1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of
hot
columns.
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.
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
8906.
Deuterium
lamp to construct an NUV flat applicable to all NUV modes
10.
spectroscopic survey of cataclysmic variables
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.
in the
optical in 1988 and have been detected in the vacuum ultraviolet by IUE.
The UV
data would be the first “direct” observation of the hot spectrum
emitted by a
supernova shock destroying its progenitor star; unfortunately the large
aperture
and pointing instabilities of IUE make these data difficult to calibrate
and
interpret in great detail. The breakout signal has also been modified by
the
spectral reflectance of the echoing dust. We propose to confirm the UV
detection
and to disentangle the incident SN spectrum from the dust reflectance by
observing the UV echo at two scattering phase angles and combining them
with HST
and ground-based data. Sampling two echoes at widely-spaced spectral
points and
two scattering angles will provide us with enough independent information
to
factor these separately. The resulting early UV spectrum of SN 1987A will
allow
a direct test of theoretical models of supernova shock propagation and
breakout
from a star, as well as provide an accurate input ionization spectrum for
understanding the excitation and recombination of gas in the observed
circumstellar nebulosity around SN1987A. This study will also strongly
constrain
the physical properties of interstellar dust in the Large Magellanic
Cloud.
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.
data
for monitoring and characterizing the evolution of hot pixels
of
potential non-nominal performance that will be investigated.)
control @ 13:06:18Z.
Four 486 ESB messages A0Ehex were observed when telemetry
was
re-acquired
@ 053/13:13:30Z, indicating “FGS sequential attitude update
failed because error
too large to correct”. Vehicle was in LOS at time of
occurrence. Primary GS
Acquisition (3,2,2) @ 053/11:48:48Z was successful with no
errors. GS Re-acquisition
@ 053/14:39:33Z also acquired FL, but lost it due to four
more 486 ESB messages
starting @ 053/14:42:36Z. Under investigation.
up
on FGS 3 with SSLE on
FGS 2. One subsequent GS Re-acquisition also failed to FL
back up.
Under investigation.
None
1051-0 – NICMOS MEB Temperature Limit Increase @ 053/02:21:49z
1078-0 – Near Term Guidance on Redumps @ 053/18:52:00z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 24 24
FGS
REacq 29 27
053/14:39:33z, 053/13:06:18z
FHST Update 32 32
LOSS of LOCK
