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Daily Report #4944



 
 
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Old October 5th 09, 02:48 PM posted to sci.astro.hubble
Cooper, Joe
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Default Daily Report #4944

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #4944

PERIOD COVERED: 5am October 2 - 5am October 5, 2009 (DOY 275/09:00z-278/09:00z)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8795

NICMOS Post-SAA Calibration - CR Persistence Part 6

This is 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
'Use After' 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 darks. 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.

NIC1/NIC2/NIC3 11947

Extended Dark Monitoring

This program takes a series of darks to obtain darks (including
amplifier glow, dark current, and shading profiles) for all three
cameras in the read-out sequences used in Cycle 17. A set of 12 orbits
will be observed every two months for a total of 72 orbits for a 12
month Cycle 17. This is a continuation of Cycle 16 program 11330
scaled down by ~80%.

The first orbit (Visit A0) should be scheduled in the NICMOS SMOV
after the DC Transfer Test (11406) and at least 36h before the Filter
Wheel Test (11407). Data download using fast track.

The following 28 orbits (visit A1-N2) should be scheduled AFTER the
SMOV Proposal 11407 (Filter Wheel Test). This is done in order to
monitor the dark current following an adjustment of the NCS set-point.
These visits should be executed until the final temperature is reached
during SMOV.

WFC3/IR 11936

IR Grism Flux Calibration

This program will determine image displacement, spectral trace and
flux calibration for the IR G102 and G141 grisms as a function of
spatial position within the field of view. The HST flux standard GD71
will be observed in a 9-point pattern in the IR field of view, which
will provide the necessary image displacement, spectral trace, and
throughput measurements.

WFC3/IR/S/C 11929

IR Dark Current Monitor

Analyses of ground test data showed that dark current signals are more
reliably removed from science data using darks taken with the same
exposure sequences as the science data, than with a single dark
current image scaled by desired exposure time. Therefore, dark current
images must be collected using all sample sequences that will be used
in science observations. These observations will be used to monitor
changes in the dark current of the WFC3-IR channel on a day-to-day
basis, and to build calibration dark current ramps for each of the
sample sequences to be used by GOs in Cycle 17. For each sample
sequence/array size combination, a median ramp will be created and
delivered to the calibration database system (CDBS).

WFC3/IR 11926

IR Zero Points

We will measure and monitor the zeropoints through the IR filters
using observations of the white dwarf standard stars, GD153, GD71 and
GD191B2B and the solar analog standard star, P330E. Data will be taken
monthly during Cycle 17. Observations of the star cluster, NGC 104,
are made twice to check color transformations. We expect an accuracy
of 2% in the wide filter zeropoints relative to the HST photometric
system, and 5% in the medium- and narrow-band filters.

WFC3/UVIS 11924

WFC3/UVIS External and Internal CTE Monitor

CCD detector Charge Transfer Inefficiency (CTI)-induced losses in
photometry and astrometry will be measured using observations of the
rich open cluster NGC6791 and with the EPER (Extended Pixel Edge
Response) method using tungsten lamp flat field exposures. Although we
do not expect to see CTE effects at the outset of Cycle 17, this CTE
monitoring program is the first of a multi-cycle program to monitor
and establish CTE-induced losses with time. We expect to measure CTE
effects with a precision comparable to the ACS measurements.

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 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 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).

ACS/WFC3 11882

CCD Hot Pixel Annealing

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 the Wide
Field Channel (WFC). The High Resolution Channel (HRC) visits have
been removed since it could not be repaired during SM4.

ACS/WFC3 11879

CCD Daily Monitor (Part 1)

This program comprises basic tests for measuring the read noise and
dark current of the ACS WFC and for tracking the growth of hot pixels.
The recorded frames are used to create bias and dark reference images
for science data reduction and calibration. This program will be
executed four days per week (Mon, Wed, Fri, Sun) for the duration of
Cycle 17. To facilitate scheduling, this program is split into three
proposals. This proposal covers 352 orbits (22 weeks) from 31 August
2009 to 31 January 2010.

WFC3/ACS/UVIS 11877

HST Cycle 17 and Post-SM4 Optical Monitor

This program is the Cycle 17 implementation of the HST Optical
Monitoring Program.

The 36 orbits comprising this proposal will utilize ACS (Wide Field
Channel) and WFC3 (UVIS Channel) to observe stellar cluster members in
parallel with multiple exposures over an orbit. Phase retrieval
performed on the PSF in each image will be used to measure primarily
focus, with the ability to explore apparent coma, and astigmatism
changes in WFC3.

The goals of this program are to: 1) monitor the overall OTA focal
length for the purposes of maintaining focus within science tolerances
2) gain experience with the relative effectiveness of phase retrieval
on WFC3/UVIS PSFs 3) determine focus offset between the imagers and
identify any SI-specific focus behavior and dependencies

If need is determined, future visits will be modified to interleave
WFC3/IR channel and STIS/CCD focii measurements.

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.

STIS/CCD 11844

CCD Dark Monitor Part 1

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

WFC3/IR 11838

Completing a Flux-limited Survey for X-ray Emission from Radio Jets

We will measure the changing flow speeds, magnetic fields, and energy
fluxes in well- resolved quasar jets found in our short-exposure
Chandra survey by combining new, deep Chandra data with radio and
optical imaging. We will image each jet with sufficient sensitivity to
estimate beaming factors and magnetic fields in several distinct
regions, and so map the variations in these parameters down the jets.
HST observations will help diagnose the role of synchrotron emission
in the overall SED, and may reveal condensations on scales less than
0.1 arcsec.

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.

STIS/CCD/MA1 11737

The Distance Dependence of the Interstellar N/O Abundance Ratio: A
Gould Belt

The degree of elemental abundance homogeneity in the interstellar
medium is a function of the enrichment and mixing processes that
govern galactic chemical evolution. Observations of young stars and
the interstellar gas within ~500 pc of the Sun have revealed a local
ISM that is so well-mixed it is having an impact on ideas regarding
the formation of extrasolar planets. However, the situation just
beyond the local ISM is not so clear. Sensitive UV absorption line
measurements have recently revealed a pattern of inhomogeneities in
the interstellar O, N, and Kr gas-phase abundances at distances of
~500 pc and beyond that appear nucleosynthetic in origin rather than
due to dust depletion. In particular, based on a sample of 13
sightlines, Knauth et al. (2006) have found that the nearby stars (d
500 pc) exhibit a mean interstellar N/O abundance ratio that is
significantly higher (0.18 dex) than that toward the more distant
stars. Interestingly, all of their sightlines lie in the sky vicinity
of the Gould Belt of OB associations, molecular clouds, and diffuse
gas encircling the Sun at a distance of ~400 pc. Is it possible that
mixing processes have not yet smoothed out the recent ISM enrichment
by massive stars in the young Belt region? By measuring the
interstellar N/O ratios in a strategic new sample of sightlines with
STIS, we propose to test the apparent N/O homogeneity inside the Gould
Belt and determine if the apparent decline in the N/O ratio with
distance is robust and associated with the Belt region.

WFC3/UVIS 11729

Photometric Metallicity Calibration with WFC3 Specialty Filters

The community has chosen to include several filters in the WFC3 filter
complement that have been designed to allow fairly precise estimates
of stellar metallicities, and many science programs are enabled by
this capability. Since these filters do not exactly match those used
for this purpose on the ground, however, the mapping of stellar colors
to stellar metallicities needs to be calibrated. We propose to achieve
this calibration through observations of five stellar clusters with
well known metallicities. We will calibrate several different filter
calibrations which will allow future users to determine what filter
combination best meets their science needs.

WFC3/UVIS 11714

Snapshot Survey for Planetary Nebulae in Local Group Globular Clusters

Planetary nebulae (PNe) in globular clusters (GCs) raise a number of
interesting issues related to stellar and galactic evolution. The
number of PNe known in Milky Way GCs, four, is surprisingly low if one
assumes that all stars pass through a PN stage. However, it is likely
that the remnants of stars now evolving in galactic GCs leave the AGB
so slowly that any ejected nebula dissipates long before the star
becomes hot enough to ionize it. Thus there should not be ANY PNe in
Milky Way GCs--but there are four! It has been suggested that these
PNe are the result of mergers of binary stars within GCs, i.e., that
they are descendants of blue stragglers. The frequency of occurrence
of PNe in external galaxies poses more questions, because it shows a
range of almost an order of magnitude.

I propose a SNAPshot survey aimed at discovering PNe in the GC systems
of Local Group galaxies outside the Milky Way. These clusters, some of
which may be much younger than their counterparts in our galaxy, might
contain many more PNe than those of our own galaxy. I will use the
standard technique of emission-line and continuum imaging, which
easily discloses PNe. This proposal continues a WFPC2 program started
in Cycle 16, but with the more powerful WFC3. As a by-product, the
survey will also produce color-magnitude diagrams for numerous
clusters for the first time, reaching down to the horizontal branch.

STIS/CCD/MA1/MA2 11690

EG And: Providing the Missing Link Required for Modeling Red Giant
Mass-Loss

For the majority of red giant stars, the basic mass-loss processes at
work are unknown. Indeed, for stars of spectral types between K0 III
and M5-M6 III, much remains unknown about the regions above the
visible photosphere and the transportation of the processed material
outwards to the ISM. Eclipsing symbiotic binary systems, consisting of
an evolved giant in orbit with a white dwarf, provide an opportunity
to take advantage of the finite size of the hot component to probe
different levels of the chromosphere and wind acceleration region in
absorption. This provides spatially resolved thermal, ionization and
dynamic information on the wind which can then be compared against
predictions of hydrodynamical stellar atmosphere codes. The symbiotic
binary EG And can be considered as a Rosetta Stone for understanding
the winds of these objects. The system is ideal on a number of counts
for utilizing the ultraviolet eclipse of the white dwarf (WD)
component to probe, layer-by-layer, the thermal and dynamic conditions
at the very base of the wind and chromosphere of the RG. This
information is vital for constraining, testing and calibrating the new
generation of cool giant wind+chromosphere models and is not possible
to obtain for isolated RGs. This team has studied the UV eclipses of
this system in depth and detail, however in order to definitively
constrain the wind acceleration profile and identify the location of
the temperature rise just above the photosphere, we require 4 STIS
E140M observations of EG And at specific orbital phases. We are also
requesting a E230M observation of an isolated spectral standard,
corresponding to the RG in the binary, which will help place the EG
And results into the context of the general RG population from
analysis of the MgII wind diagnostic lines.

WFC3/UVIS/IR 11685

Supermassive Neutron Stars or Odd Binaries: Searching for Companions
to Pulsars NGC 6440B and Terzan 5J

Recent sensitive pulsar searches of globular clusters uncovered four
pulsars with very high inferred masses, between 1.7 and 2.7 solar
masses. These strongly constrain the behavior of matter in the
ultra-dense interiors of neutron stars, since for most models such
massive neutron stars could not exist. All four masses are inferred
from the measured advance of periastron with time, under the
assumption that it is due to General Relativity only. Here, we propose
to test whether part of the observed periastron advance could be
induced by the quadrupole moment of a suitably large, rotationally
distorted companion. We infer the radii such companions need to have
and show that they would be relatively bright, easily detectable with
HST. For one pulsar, M 5B, we find a plausible candidate counterpart
in archival data. We propose to use 2 orbits with WFC3 to search for
suitably large counterparts to two of the other systems, including the
one with the highest inferred mass.

WFC3/UVIS 11657

The Population of Compact Planetary Nebulae in the Galactic Disk

We propose to secure narrow- and broad-band images of compact
planetary nebulae (PNe) in the Galactic Disk to study the missing link
of the early phases of post-AGB evolution. Ejected AGB envelopes
become PNe when the gas is ionized. PNe expand, and, when large
enough, can be studied in detail from the ground. In the interim, only
the HST capabilities can resolve their size, morphology, and central
stars. Our proposed observations will be the basis for a systematic
study of the onset of morphology. Dust properties of the proposed
targets will be available through approved Spitzer/IRS spectra, and so
will the abundances of the alpha-elements. We will be able thus to
explore the interconnection of morphology, dust grains, stellar
evolution, and populations. The target selection is suitable to
explore the nebular and stellar properties across the galactic disk,
and to set constraints on the galactic evolutionary models through the
analysis of metallicity and population gradients.

ACS 11603

A Comprehensive Study of Dust Formation in Type II Supernovae with
HST, Spitzer, and Gemini

The recent discovery of three extremely bright Type II SNe, (2007it,
2007oc, 2007od) gives us a unique opportunity to combine observations
with HST, Spitzer, and Gemini to study the little understood dust
formation process in Type II SNe. Priority 1 Spitzer Cycle 5 and band
1 Gemini 2008A time has already been approved for this project. Since
late-time Type II SNe are faint and tend to be in crowded fields, we
need the high sensitivity and high spatial resolution of ACS and
NICMOS/NIC2 for these observations. This project is motivated by the
recent detection of large amounts of dust in high redshift galaxies.
The dust in these high-z galaxies must come from young, massive stars
so Type II SNe could be potential sources. The mechanism and the
efficiency of dust condensation in Type II SN ejecta are not well
understood, largely due to the lack of observational data. We plan to
produce a unique dataset, combining spectroscopy and imaging in the
visible, near- and mid-IR covering the key phase, 400- 700 days after
maximum when dust is known to form in the SN ejecta. Therefore, we are
proposing for coordinated HST/NOAO observations (HST ACS, NICMOS/NIC2
& Gemini/GMOS and TReCS) which will be combined with our Spitzer Cycle
5 data to study these new bright SNe. The results of this program will
place strong constraints on the formation of dust seen in young high
redshift (z5) galaxies.

WFC3/UVIS 11594

A WFC3 Grism Survey for Lyman Limit Absorption at z=2

We propose to conduct a spectroscopic survey of Lyman limit absorbers
at redshifts 1.8 z 2.5, using WFC3 and the G280 grism. This
proposal intends to complete an approved Cycle 15 SNAP program
(10878), which was cut short due to the ACS failure. We have selected
64 quasars at 2.3 z 2.6 from the Sloan Digital Sky Survey
Spectroscopic Quasar Sample, for which no BAL signature is found at
the QSO redshift and no strong metal absorption lines are present at z
2.3 along the lines of sight. The survey has three main

observational goals. First, we will determine the redshift frequency
dn/dz of the LLS over the column density range 16.0 log(NHI) 20.3
cm^-2. Second, we will measure the column density frequency
distribution f(N) for the partial Lyman limit systems (PLLS) over the
column density range 16.0 log(NHI) 17.5 cm^-2. Third, we will
identify those sightlines which could provide a measurement of the
primordial D/H ratio. By carrying out this survey, we can also help
place meaningful constraints on two key quantities of cosmological
relevance. First, we will estimate the amount of metals in the LLS
using the f(N), and ground based observations of metal line
transitions. Second, by determining f(N) of the PLLS, we can constrain
the amplitude of the ionizing UV background at z~2 to a greater
precision. This survey is ideal for a snapshot observing program,
because the on-object integration times are all well below 30 minutes,
and follow-up observations from the ground require minimal telescope
time due to the QSO sample being bright.

COS/NUV/FUV/WFC3/UVIS/IR 11534

COS-GTO: Atmosphere of a Transiting Planet

COS observations of a transiting planet at different orbital locations
will be useful in identifying the chemical content, size, temperature,
and flows in the atmosphere of a transiting planet.

STIS/CCD/MA1 11525

COS-GTO: STIS High Resolution Observations of the Local ISM

We shall use bright early-type B stars located within 150pc of the Sun
to probe the absorption properties of the interstellar gas associated
with the local cavity. By utilizing the high sensitivity and high
spectral resolution of the HST-STIS spectrograph we shall be able to
place new detection limits on absorption occurring in any highly
ionized gas associated with the lines of NV, SiIV and CIV that may be
present along these sight-lines within the local cavity. These data
will be used to test current theoretical models that generally predict
far higher absorption column densities than have been previously
found. Also, the high spectral resolution will enable far stricter
limits to be placed on the thermal widths of such highly ionized
absorption lines, which previous observations towards the Loop I
region have suggested anomalously narrow profiles consistent with
their formation by either photo ionization or highly non-equilibrium
processes.

COS/NUV 11466

NUV Detector Dark

The purpose of this proposal is to measure the NUV detector dark rate
by taking long science exposures with no light on the detector. The
detector dark rate and spatial distribution of counts will be compared
to pre-launch data in order to verify the nominal operation of the
detector, and for use in the CalCOS calibration pipeline. Variations
of count rate as a function of orbital position will be analyzed to
find dependence of dark rate on proximity to the SAA.

WFC3/ACS/IR 11359

Panchromatic WFC3 Survey of Galaxies at Intermediate z: Early Release
Science Program for Wide Field Camera 3

The unique panchromatic capabilities of WFC3 will be used to survey
the structure and evolution of galaxies at the peak of the galaxy
assembly epoch. Deep ultraviolet and near-IR imaging and slitless
spectroscopy of existing deep multi-color ACS fields will be used to
gauge star-formation and the growth of stellar mass as a function of
morphology, structure and surrounding density in the critical epoch 1
z 4. Images in the F225W, F275W, and F336W filters will identify
galaxies at z 1.5 from their UV continuum breaks, and provide
star-formation indicators tied directly to both local and z 3
populations. Deep near-IR (F125W and F160W) images will probe the
stellar mass function well below 10^9 Msun for mass-complete samples.
Lastly, the WFC3 slitless UV and near-IR grisms will be used to
measure redshifts and star-formation rates from H- alpha and
rest-frame UV continuum slope. This WFC3 ERS program will survey one 4
x 2 mosaic for a total area of 50 square arcminutes to 5-sigma depths
of m_AB = 27 in most filters from the mid-UV through the near-IR.

This multicolor high spatial resolution data set will allow the user
to gauge the growth of galaxies through star-formation and merging.
High precision photometric and low- resolution spectroscopic redshifts
will allow accurate determinations of the faint-end of the luminosity
and mass functions, and will shed light on merging and tidal
disruption of stellar and gaseous disks. The WFC3 images will also
allow detailed studies of the internal structure of galaxies, and the
distribution of young and old stellar populations. This program will
demonstrate the unique power of WFC3 by applying its many diverse
modes and full panchromatic capability to a forefront problem in
astrophysics.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12034 - GSAcq(2,3,3) scheduled at 276/09:26:46z failed due to scan
step limit exceeded on FGS 3.

Observation affected, NIC 46 Proposal ID# 08795

HSTAR FOR DAY 269

12031 - REAcq(1,2,1) scheduled to start at 269/09:26:53z ran longer
than allotted (266 sec). Further review shows FGS2 suffer scan step
limit exceed on its initial FL-WD attempt but succeeded in the 2nd
(ie, failure path). The take data flag (P4TAKDAT) didn't come up until
269/09:32:33z.

HSTAR FOR DAY 246

12032 - REAcq(2,1,1) schedule to start @ 2009.246/05:12:35z lost data
valid on FGS2 during a Profile slew (and the FGS Mailbox
(Q4DMRFGS)went to PauseExp (246/05:45:21z). LoL was successfully
recovered with take data flag (P4TAKDAT) back up (246/05:47:57z). No
further LoL events occurred prior to PCPTERM (246/06:27:16z).

HSTAR FOR DAY 262

12033 - GSAcq(1,2,1) schedule to start @ 262/01:52:41z lost star
presence and data valid on FGS1 (262/01:56:32z) during a Profile slew
with both FGSes going to SSM control (262/02:07:47z). LoL was
successfully recovered with take data flag (P4TAKDAT) back up
(262/02:35:39z).

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL
FGS GSAcq 28 27
FGS REAcq 23 23
OBAD with Maneuver 24 24
LOSS of LOCK

SIGNIFICANT EVENTS: (None)


 




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