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Daily Report #4957



 
 
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Old October 23rd 09, 08:59 PM posted to sci.astro.hubble
Cooper, Joe
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Default Daily Report #4957

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #4957

PERIOD COVERED: 5am October 22 - 5am October 23, 2009 (DOY295/09:00z-296/09:00z)

OBSERVATIONS SCHEDULED

FGS 11788

The Architecture of Exoplanetary Systems

Are all planetary systems coplanar? Concordance cosmogony makes that
prediction. It is, however, a prediction of extrasolar planetary
system architecture as yet untested by direct observation for main
sequence stars other than the Sun. To provide such a test, we propose
to carry out FGS astrometric studies on four stars hosting seven
companions. Our understanding of the planet formation process will
grow as we match not only system architecture, but formed planet mass
and true distance from the primary with host star characteristics for
a wide variety of host stars and exoplanet masses.

We propose that a series of FGS astrometric observations with
demonstrated 1 millisecond of arc per-observation precision can
establish the degree of coplanarity and component true masses for four
extrasolar systems: HD 202206 (brown dwarf+planet); HD 128311
(planet+planet), HD 160691 = mu Arae (planet+planet), and HD 222404AB
= gamma Cephei (planet+star). In each case the companion is identified
as such by assuming that the minimum mass is the actual mass. For the
last target, a known stellar binary system, the companion orbit is
stable only if coplanar with the AB binary orbit.

NIC 11416

NICMOS Parallel Thermal Background

Characterize the stability of the HST+NCS+Instrument thermal emission
as seen by NICMOS on secular scales. The data will be obtained using
NIC3 and the F222M filter and will run throughout the SMOV4 activities
as a pure parallel program.

NIC 11417

NICMOS Detector Read noise and Dark Current

The NICMOS detector characteristics will be monitored during the
entire extent of the SMOV4 through a set of dark exposures. This will
also allow a determination of the detector temperature from bias
measurements. The data should be obtained in SAA-free orbits,
approximately every 24 hours. In addition, the detector read noise and
the detector shading profiles will be measured once a week.

NIC1/NIC2/NIC3 11820

NICMOS Post-SAA Calibration - CR Persistence Part 7

Internals for CR persistence


STIS/CCD 11844

CCD Dark Monitor Part 1

The purpose of this proposal is to monitor the darks for the STIS CCD.

STIS/CCD 11846

CCD Bias Monitor-Part 1

The purpose of this proposal is to 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.

WFC/ACS 11888

ACS Internal Flat Fields

The stability of the CCD flat fields will be monitored using the
calibration lamps and a sub-sample of the filter set. High signal
observations will be used to assess the stability of the
pixel-to-pixel flat field structure and to monitor the position of the
dust motes.

WFC3/ACS/UVIS 11360

Star Formation in Nearby Galaxies

Star formation is a fundamental astrophysical process; it controls
phenomena ranging from the evolution of galaxies and nucleosynthesis
to the origins of planetary systems and abodes for life. The WFC3,
optimized at both UV and IR wavelengths and equipped with an extensive
array of narrow-band filters, brings unique capabilities to this area
of study. The WFC3 Scientific Oversight Committee (SOC) proposes an
integrated program on star formation in the nearby universe which will
fully exploit these new abilities. Our targets range from the
well-resolved R136 in 30 Dor in the LMC (the nearest super star
cluster) and M82 (the nearest starbursting galaxy) to about half a
dozen other nearby galaxies that sample a wide range of star-formation
rates and environments. Our program consists of broad band
multiwavelength imaging over the entire range from the UV to the
near-IR, aimed at studying the ages and metallicities of stellar
populations, revealing young stars that are still hidden by dust at
optical wavelengths, and showing the integrated properties of star
clusters. Narrow-band imaging of the same environments will allow us
to measure star-formation rates, gas pressure, chemical abundances,
extinction, and shock morphologies. The primary scientific issues to
be addressed a (1) What triggers star formation? (2) How do the
properties of star-forming regions vary among different types of
galaxies and environments of different gas densities and compositions?
(3) How do these different environments affect the history of star
formation? (4) Is the stellar initial mass function universal or
determined by local conditions?

WFC3/UV/ACS/WFC 11688

Exploring the Bottom End of the White Dwarf Cooling Sequence in the
Open Cluster NGC6819

The recent discovery by our group of an unexpectedly bright end of the
white-dwarf (WD) luminosity function (LF) of the metal-rich, old open
cluster NGC 6791 casts serious doubts on our understanding of the
physical process which rules the formation and the cooling of WDs. It
is clear at this point that the theory badly needs more observations.
Here we propose WFC3/UVIS and ACS/WFC HST observations reaching the
bottom end of the WD LF, for the first time in a solar-metallicity,
2.5-Gyr-old, populous open cluster: NGC 6819.

WFC3/UVIS 11630

Monitoring Active Atmospheres on Uranus and Neptune

We propose Snapshot observations of Uranus and Neptune to monitor
changes in their atmospheres on time scales of weeks and months, as we
have been doing for the past seven years. Previous Hubble Space
Telescope observations (including previous Snapshot programs 8634,
10170, 10534, and 11156), together with near-IR images obtained using
adaptive optics on the Keck Telescope, reveal both planets to be
dynamic worlds which change on time scales ranging from hours to
(terrestrial) years. Uranus equinox occurred in December 2007, and the
northern hemisphere is becoming fully visible for the first time since
the early 1960s. HST observations during the past several years
(Hammel et al. 2005, Icarus 175, 284 and references therein) have
revealed strongly wavelength-dependent latitudinal structure, the
presence of numerous visible-wavelength cloud features in the northern
hemisphere, at least one very long- lived discrete cloud in the
southern hemisphere, and in 2006 the first clearly defined dark spot
seen on Uranus. Long term ground-based observations (Lockwood and
Jerzekiewicz, 2006, Icarus 180, 442; Hammel and Lockwood 2007, Icarus
186, 291) reveal seasonal brightness changes that seem to demand the
appearance of a bright northern polar cap within the next few years.
Recent HST and Keck observations of Neptune (Sromovsky et al. 2003,
Icarus 163, 256 and references therein) show a general increase in
activity at south temperate latitudes until 2004, when Neptune
returned to a rather Voyager-like appearance with discrete bright
spots rather than active latitude bands. Further Snapshot observations
of these two dynamic planets will elucidate the nature of long-term
changes in their zonal atmospheric bands and clarify the processes of
formation, evolution, and dissipation of discrete albedo features.

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

The behavior of the WFC3 UVIS CCD will be monitored daily with a set
of full-frame, four-amp bias and dark frames. A smaller set of 2Kx4K
subarray biases are acquired at less frequent intervals throughout the
cycle to support subarray science observations. The internals from
this proposal, along with those from the anneal procedure (Proposal
11909), will be used to generate the necessary superbias and superdark
reference files for the calibration pipeline (CDBS).

WFC3/UVIS 11907

UVIS Cycle 17 Contamination Monitor

The UV throughput of WFC3 during Cycle 17 is monitored via weekly
standard star observations in a subset of key filters covering
200-600nm and F606W, F814W as controls on the red end. The data will
provide a measure of throughput levels as a function of time and
wavelength, allowing for detection of the presence of possible
contaminants.

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

Ground testing revealed an intermittent hysteresis type effect in the
UVIS detector (both CCDs) at the level of ~1%, lasting hours to days.
Initially found via an unexpected bowtie-shaped feature in flatfield
ratios, subsequent lab tests on similar e2v devices have since shown
that it is also present as simply an overall offset across the entire
CCD, i.e., a QE offset without any discernable pattern. These lab
tests have further revealed that overexposing the detector to count
levels several times full well fills the traps and effectively
neutralizes the bowtie. Each visit in this proposal acquires a set of
three 3x3 binned internal flatfields: the first unsaturated image will
be used to detect any bowtie, the second, highly exposed image will
neutralize the bowtie if it is present, and the final image will allow
for verification that the bowtie is gone.

WFC3/UVIS/IR 11644

A Dynamical-Compositional Survey of the Kuiper Belt: A New Window Into
the Formation of the Outer Solar System

The eight planets overwhelmingly dominate the solar system by mass,
but their small numbers, coupled with their stochastic pasts, make it
impossible to construct a unique formation history from the dynamical
or compositional characteristics of them alone. In contrast, the huge
numbers of small bodies scattered throughout and even beyond the
planets, while insignificant by mass, provide an almost unlimited
number of probes of the statistical conditions, history, and
interactions in the solar system. To date, attempts to understand the
formation and evolution of the Kuiper Belt have largely been dynamical
simulations where a hypothesized starting condition is evolved under
the gravitational influence of the early giant planets and an attempt
is made to reproduce the current observed populations. With little
compositional information known for the real Kuiper Belt, the test
particles in the simulation are free to have any formation location
and history as long as they end at the correct point. Allowing
compositional information to guide and constrain the formation,
thermal, and collisional histories of these objects would add an
entire new dimension to our understanding of the evolution of the
outer solar system. While ground based compositional studies have hit
their flux limits already with only a few objects sampled, we propose
to exploit the new capabilities of WFC3 to perform the first ever
large-scale dynamical-compositional study of Kuiper Belt Objects
(KBOs) and their progeny to study the chemical, dynamical, and
collisional history of the region of the giant planets. The
sensitivity of the WFC3 observations will allow us to go up to two
magnitudes deeper than our ground based studies, allowing us the
capability of optimally selecting a target list for a large survey
rather than simply taking the few objects that can be measured, as we
have had to do to date. We have carefully constructed a sample of 120
objects which provides both overall breadth, for a general
understanding of these objects, plus a large enough number of objects
in the individual dynamical subclass to allow detailed comparison
between and within these groups. These objects will likely define the
core Kuiper Belt compositional sample for years to come. While we have
many specific results anticipated to come from this survey, as with
any project where the field is rich, our current knowledge level is
low, and a new instrument suddenly appears which can exploit vastly
larger segments of the population, the potential for discovery -- both
anticipated and not -- is extraordinary.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12051 - At 295/12:30:47 the SIC&DH safed. Telemetry indicated that the
SIC&DH Pit toggle test failed.

COMPLETED OPS REQUEST:

18728-1 - Recycle SIC&DH after lock-up @ 295/1435z
18730-1 - Execute Safemode Recovery Macro @ 295/1755z
18729-2 - Recover NSSC1 back to Normal Mode 295/2001z
18731-1 - Re-enable ACR to Reset MEB of SIs @ 295/2005z
18732-0 - Re-enable NSSC-1 HV Protect Function @ 295/2115z
18733-0 - Recover the ESM, NCS CPL, and PCE @ 295/2141z

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL
FGS GSAcq 10 09
FGS REAcq 04 03
OBAD with Maneuver 08 08

SIGNIFICANT EVENTS:

Flash Report: SIC&DH lock-up

The PIT Toggle test failed at 295/12:30:47 The SIs were then
transitioned to their respective safe modes.

SIC&DH was recovered to NORMAL mode at 295/19:21z

Currently, the SIC&DH is in Fixed mode with all SIs in safe mode.

Flash Report: HV Protect Enable and ESM / NCS CPL / PCE Recovery

Ops Request 18732 to re-enable the NSSC-1 HV Protect sequence was
successfully completed at 295/21:14 UTC.

Ops Request 18733 followed and was successfully completed at 295/21:40
UTC, recovering the ESM up to its Operate mode, placing the NCS CPL in
its Standby state at a reservoir setpoint of -34 degC, and re-enabling
the PCE to restore visibility into various NCC telemetry.
 




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