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- Daily Report #5100 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/7bdb7b152b1e5dba?hl=en
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============================================================================== TOPIC: Daily Report #5100
http://groups google com/group/sci astro hubble/t/7bdb7b152b1e5dba?hl=en
== 1 of 1 == Date: Thurs, May 20 2010 12:20 pm From: "Bassford, Lynn"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5100
PERIOD COVERED: 5am May 19 - 5am May 20, 2010 (DOY 139/09:00z-140/09:00z)
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )
HSTARS:
For DOY (136)
12284 - GSAcq(1,2,1) at 136/17:23:21z required 10 attempts to achieve CT-DV on FGS2 The acquisition was successful
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 8 8 FGS REAcq 9 9 OBAD with Maneuver 4 4
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
ACS/WFC 11564
Optical and Ultraviolet Photometry of Isolated Neutron Stars
We propose ultraviolet and B-band observations of 5 nearby, thermally emitting neutron stars These data will measure the Rayleigh-Jeans tails of their spectra, providing a vital complement to X-ray spectroscopy and helping to constrain atmospheric models, working toward the ultimate goal of unraveling the physics of neutron stars With these data we will have good-quality optical and UV data for the full sample of these objects, allowing detailed comparisons between them Finally, the data should allow us to measure proper motions for one or two objects, and will serve as the reference data for the remaining objects; such proper motions allow ages to be determined for these objects by tracing them back to likely birth locations
ACS/WFC 12012
Binary Formation in the Sparse Galactic Globular Cluster NGC 3201
Bright X-ray sources in globular clusters, X-ray binaries, cataclysmic variables, active binaries, and millisecond pulsars, are all binary systems or thought to be the products of such systems Studies of X-ray sources in GCs thus probe binary formation Most past observations have concentrated on dense GCs; these systems show clear evidence for strong dynamical formation of binaries; however, sparse clusters seem to fall off this pattern Potential explanantions include, among others, primordial binary formation and a misunderstanding of the dynamical state of some GCs We propose an 85 ks ACIS-S observation of NGC~3201, the nearest sparse GC unobserved by Chandra to test these explanations We request 1 orbit of HST to discriminate CVs from ABs, and 1 hour of GBT time to search for MSPs
ACS/WFC/WFC3/UVI 11233
Multiple Generations of Stars in Massive Galactic Globular Clusters
This is a follow-up to recent HST imaging of NGC 2808, which discovered that its main sequence is triple, with three well-separated parallel branches (Fig ~1) Along with the double MS of Omega Centauri, this challenges the long-held paradigm that globular clusters are simple, single stellar populations The cause of this main sequence multiplicity in both clusters is likely to be differences in helium abundance, which could play a fundamental role in the understanding of stellar populations We propose to image seven more of the most massive globular clusters, to examine their main sequences for indications of splitting
STIS/CCD 11845
CCD Dark Monitor Part 2
Monitor the darks for the STIS CCD
STIS/CCD 11847
CCD Bias Monitor-Part 2
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/MA1 11861
MAMA FUV Flats
This program will obtain FUV-MAMA observations of the STIS internal Krypton lamp to construct an FUV flat applicable to all FUV modes
STIS/MA2 11857
STIS Cycle 17 MAMA Dark Monitor
This proposal monitors the behavior of the dark current in each of the MAMA detectors
The basic monitor takes two 1380s ACCUM darks each week with each detector However, starting Oct 5, pairs are only included for weeks that the LRP has external MAMA observations planned The weekly pairs of exposures for each detector are linked so that they are taken at opposite ends of the same SAA free interval This pairing of exposures will make it easier to separate long and short term temporal variability from temperature dependent changes
For both detectors, additional blocks of exposures are taken once every six months These are groups of five 1314 s FUV-MAMA TIME-TAG darks or five 3x315 s NUV ACCUM darks distributed over a single SAA free interval This will give more information on the brightness of the FUV MAMA dark current as a function of the amount of time that the HV has been on, and for the NUV MAMA will give a better measure of the short term temperature dependence
WFC3/IR 11664
The WFC3 Galactic Bulge Treasury Program: Populations, Formation History, and Planets
Exploiting the full power of the Wide Field Camera 3 (WFC3), we propose deep panchromatic imaging of four fields in the Galactic bulge These data will enable a sensitive dissection of its stellar populations, using a new set of reddening-free photometric indices we have constructed from broad-band filters across UV, optical, and near-IR wavelengths These indices will provide accurate temperatures and metallicities for hundreds of thousands of individual bulge stars Proper motions of these stars derived from multi-epoch observations will allow separation of pure bulge samples from foreground disk contamination Our catalogs of proper motions and panchromatic photometry will support a wide range of bulge studies
Using these photometric and astrometric tools, we will reconstruct the detailed star-formation history as a function of position within the bulge, and thus differentiate between rapid- and extended-formation scenarios We will also measure the dependence of the stellar mass function on metallicity, revealing how the characteristic mass of star formation varies with chemistry Our sample of bulge stars with accurate metallicities will include 12 candidate hosts of extrasolar planets Planet frequency is correlated with metallicity in the solar neighborhood; our measurements will extend this knowledge to a remote environment with a very distinct chemistry
Our proposal also includes observations of six well-studied globular and open star clusters; these observations will serve to calibrate our photometric indices, provide empirical population templates, and transform the theoretical isochrone libraries into the WFC3 filter system Besides enabling our own program, these products will provide powerful new tools for a host of other stellar-population investigations with HST/WFC3 We will deliver all of the products from this Treasury Program to the community in a timely fashion
WFC3/IR 11696
Infrared Survey of Star Formation Across Cosmic Time
We propose to use the unique power of WFC3 slitless spectroscopy to measure the evolution of cosmic star formation from the end of the reionization epoch at z>6 to the close of the galaxy-building era at z~0 3 Pure parallel observations with the grisms have proven to be efficient for identifying line emission from galaxies across a broad range of redshifts The G102 grism on WFC3 was designed to extend this capability to search for Ly-alpha emission from the first galaxies Using up to 250 orbits of pure parallel WFC3 spectroscopy, we will observe about 40 deep (4-5 orbit) fields with the combination of G102 and G141, and about 20 shallow (2-3 orbit) fields with G141 alone
Our primary science goals at the highest redshifts are: (1) Detect
Lya in ~100 galaxies with z>5
6 and measure the evolution of the Lya
luminosity function, independent of of cosmic variance; 2) Determine
the connection between emission-line selected and continuum-break
selected galaxies at these high redshifts, and 3) Search for the
proposed signature of neutral hydrogen absorption at re-ionization
At
intermediate redshifts we will (4) Detect more than 1000 galaxies in
Halpha at 0
5 To identify single-line Lya emitters, we will exploit the wide
0
8--1
9um wavelength coverage of the combined G102+G141 spectra
All
[OII] and [OIII] interlopers detected in G102 will be reliably
separated from true LAEs by the detection of at least one strong line
in the G141 spectrum, without the need for any ancillary data
We
waive all proprietary rights to our data and will make high-level data
products available through the ST/ECF
WFC3/IR/WFC3/UVI 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 are: (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/UVI 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 ==============================================================================
TOPIC: Daily Report #5101 == 1 of 1 ==
Date: Fri, May 21 2010 7:06 am
From: "Cooper, Joe" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5101 PERIOD COVERED: 5am May 20 - 5am May 21, 2010 (DOY 140/09:00z-141/09:00z) FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: 12285 - OBD Failed Quaternion @ 140/15:38:34z
GSAcq(1,0,1) at
140/15:52:06z was successful
COMPLETED OPS REQUEST: 17543-3 - Dump OBAD tables after failed OBAD COMPLETED OPS NOTES: (None) FGS GSAcq 10 10
FGS REAcq 6 6
OBAD with Maneuver 6 5 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED: ACS/WFC 11591 Are Low-Luminosity Galaxies Responsible for Cosmic Reionization? Our group has demonstrated that massive clusters, acting as powerful
cosmic lenses, can constrain the abundance and properties of
low-luminosity star-forming sources beyond z~6; such sources are
thought to be responsible for ending cosmic reionization
The large
magnification possible in the critical regions of well-constrained
clusters brings sources into view that lie at or beyond the limits of
conventional exposures such as the UDF
We have shown that the
combination of HST and Spitzer is particularly effective in delivering
the physical properties of these distant sources, constraining their
mass, age and past star formation history
Indirectly, we therefore
gain a valuable glimpse to yet earlier epochs
Recognizing the result
(and limitations) of blank field surveys, we propose a systematic
search through 10 lensing clusters with ACS/F814W and
WFC3/[F110W+F160W] (in conjunction with existing deep IRAC data)
Our
goal is to measure with great accuracy the luminosity function at z~7
over a range of at least 3 magnitude, based on the identification of
about 50 lensed galaxies at 6
5 ACS/WFC 11995 CCD Daily Monitor (Part 2) 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 320 orbits (20 weeks) from 1 February
2010 to 20 June 2010
ACS/WFC/WFC3/IR 11597 Spectroscopy of IR-Selected Galaxy Clusters at 1 < z < 1
5 We propose to obtain WFC3 G141 and G102 slitless spectroscopy of
galaxy clusters at 1 < z < 1
5 that were selected from the IRAC survey
of the Bootes NDWFS field
Our IRAC survey contains the largest sample
of spectroscopically confirmed clusters at z > 1
The WFC3 grism data
will measure H-alpha to determine SFR, and fit models to the low
resolution continua to determine stellar population histories for the
brighter cluster members, and redshifts for the red galaxies too faint
for ground-based optical spectroscopy
ACS/WFC/WFC3/IR 11663 Formation and Evolution of Massive Galaxies in the Richest
Environments at 1
5 < z < 2
0 We propose to image seven 1
5 ACS/WFC/WFC3/IR/WFC3/UVI 11570 Narrowing in on the Hubble Constant and Dark Energy A measurement of the Hubble constant to a precision of a few percent
would be a powerful aid to the investigation of the nature of dark
energy and a potent "end-to-end" test of the present cosmological
model
In Cycle 15 we constructed a new, streamlined distance ladder
utilizing high-quality type Ia supernova data and observations of
Cepheids with HST in the near-IR to minimize the dominant sources of
systematic uncertainty in past measurements of the Hubble constant and
reduce its total uncertainty to a little under 5%
Here we propose to
exploit this new route to reduce the remaining uncertainty by more
than 30%, translating into an equal reduction in the uncertainty of
the equation of state of dark energy
We propose three sets of
observations to reach this goal: a mosaic of NGC 4258 with WFC3 in
F160W to triple its sample of long period Cepheids, WFC3/F160W
observations of the 6 ideal SN Ia hosts to triple their samples of
Cepheids, and observations of NGC 5584 the host of a new SN Ia, SN
2007af, to discover and measure its Cepheids and begin expanding the
small set of SN Ia luminosity calibrations
These observations would
provide the bulk of a coordinated program aimed at making the
measurement of the Hubble constant one of the leading constraints on
dark energy
COS/FUV/COS/NUV 11742 Probing HeII Reionization with GALEX-selected Quasar Sightlines and
HST/COS We propose spectroscopic observations with COS of eight z~3 QSOs that
we found to be bright in the far ultraviolet
Our aim is to study
intergalactic absorption caused by the onset of the He II Lyman
forest
Several lines of evidence suggest that helium reionization
occurred at z~3
Understanding this process is critical for a complete
picture of the intergalactic medium and its evolution; it also gives
clues to hydrogen reionization at z>6
The only direct means of
assessing He II reionization is through far-UV observations of the He
II Lyman alpha forest
Only 6 sightlines are known to date where this
is feasible, despite extensive surveys
Our programme is designed to
double the number of available sightlines
To this effect, we
cross-correlated all known z>2
73 quasars with UV source lists from
the GALEX satellite
The selected quasars were all significantly
detected in the far UV by GALEX, and their UV colors are similar to
those of already known quasars with transparent sightlines
Spectra
obtained with COS will allow us to compile the first comprehensive
sample of He II absorption spectra probing similar redshifts, enabling
a systematic investigation of the He II reionization epoch and the
spectral shape of the UV background
S/C/WFC3/IR 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)
STIS/CCD 11845 CCD Dark Monitor Part 2 Monitor the darks for the STIS CCD
STIS/CCD 11847 CCD Bias Monitor-Part 2 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/MA2 11857 STIS Cycle 17 MAMA Dark Monitor This proposal monitors the behavior of the dark current in each of the
MAMA detectors
The basic monitor takes two 1380s ACCUM darks each week with each
detector
However, starting Oct 5, pairs are only included for weeks
that the LRP has external MAMA observations planned
The weekly pairs
of exposures for each detector are linked so that they are taken at
opposite ends of the same SAA free interval
This pairing of exposures
will make it easier to separate long and short term temporal
variability from temperature dependent changes
For both detectors, additional blocks of exposures are taken once
every six months
These are groups of five 1314 s FUV-MAMA TIME-TAG
darks or five 3x315 s NUV ACCUM darks distributed over a single SAA
free interval
This will give more information on the brightness of
the FUV MAMA dark current as a function of the amount of time that the
HV has been on, and for the NUV MAMA will give a better measure of the
short term temperature dependence
WFC3/IR 11696 Infrared Survey of Star Formation Across Cosmic Time We propose to use the unique power of WFC3 slitless spectroscopy to
measure the evolution of cosmic star formation from the end of the
reionization epoch at z>6 to the close of the galaxy-building era at
z~0
3
Pure parallel observations with the grisms have proven to be
efficient for identifying line emission from galaxies across a broad
range of redshifts
The G102 grism on WFC3 was designed to extend this
capability to search for Ly-alpha emission from the first galaxies
Using up to 250 orbits of pure parallel WFC3 spectroscopy, we will
observe about 40 deep (4-5 orbit) fields with the combination of G102
and G141, and about 20 shallow (2-3 orbit) fields with G141 alone
Our primary science goals at the highest redshifts are: (1) Detect Lya
in ~100 galaxies with z>5
6 and measure the evolution of the Lya
luminosity function, independent of of cosmic variance; 2) Determine
the connection between emission-line selected and continuum-break
selected galaxies at these high redshifts, and 3) Search for the
proposed signature of neutral hydrogen absorption at re-ionization
At
intermediate redshifts we will (4) Detect more than 1000 galaxies in
Halpha at 0
5 To identify single-line Lya emitters, we will exploit the wide
0
8--1
9um wavelength coverage of the combined G102+G141 spectra
All
[OII] and [OIII] interlopers detected in G102 will be reliably
separated from true LAEs by the detection of at least one strong line
in the G141 spectrum, without the need for any ancillary data
We
waive all proprietary rights to our data and will make high-level data
products available through the ST/ECF
WFC3/IR 11915 IR Internal Flat Fields This program is the same as 11433 (SMOV) and depends on the completion
of the IR initial alignment (program 11425)
This version contains
three instances of 37 internal orbits; to be scheduled early, middle,
and near the end of Cycle 17, in order to use the entire 110-orbit
allocation
In this test, we will study the stability and structure of the IR
channel flat field images through all filter elements in the WFC3-IR
channel
Flats will be monitored, i
e
to capture any temporal trends
in the flat fields, and delta flats produced
High signal observations
will provide a map of the pixel-to-pixel flat field structure, as well
as identify the positions of any dust particles
WFC3/IR/WFC3/UVI 11557 The Nature of low-ionization BAL QSOs The rare subclass of optically-selected QSOs known as low-ionization
broad absorption line (LoBAL) QSOs show signs of high-velocity gas
outflows and reddened continua indicative of dust obscuration
Recent
studies show that galaxies hosting LoBAL QSOs tend to be ultraluminous
infrared systems that are undergoing mergers, and that have dominant
young (< 100 Myr) stellar populations
Such studies support the idea
that LoBAL QSOs represent a short-lived phase early in the life of
QSOs, when powerful AGN-driven winds are blowing away the dust and gas
surrounding the QSO
If so, understanding LoBALs would be critical in
the study of phenomena regulating black hole and galaxy evolution,
such as AGN feedback and the early stages of nuclear accretion
These
results, however, come from very small samples that may have serious
selection biases
We are therefore taking a more aggressive approach
by conducting a systematic multiwavelength study of a volume limited
sample of LoBAL QSOs at 0
5 < z < 0
6 drawn from SDSS
We propose to
image their host galaxies in two bands using WFC3/UVIS and WFC3/IR to
study the morphologies for signs of recent tidal interactions and to
map their interaction and star forming histories
We will thus
determine whether LoBAL QSOs are truly exclusively found in young
merging systems that are likely to be in the early stages of nuclear
accretion
WFC3/UVI 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 are: (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/UVI 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 WFC3/UVI 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
==============================================================================
TOPIC: Daily Report #5102 == 1 of 1 ==
Date: Mon, May 24 2010 6:24 am
From: "Cooper, Joe" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5102 PERIOD COVERED: 5am May 21 - 5am May 24, 2010 (DOY 141/09:00z-144/09:00z) FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: 12286 - GSAcq(1,2,1) at 141/18:30:00z fails to fine lock backup on FGS
2
Observation possibly affected: proposal ID# 11704
COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 24 24
FGS REAcq 23 23
OBAD with Maneuver 17 17 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED WFC3/IR/S/C 12089 Persistence - Part 2 The IR detectors on WFC3, like other IR detectors, trap charge when
exposed to sources near or above the full well of the detector diodes
This charge leaks out, producing detectable afterglow images for
periods which can last for several hours, depending on the amount of
over exposure
These visits, which consist of tungsten lamp exposures
of varying durations followed by darks, are intended to provide a
better calibration of persistence over the full area of the IR
detector of WFC3
COS/NUV/FUV 12086 Generation of 1-D Fixed Pattern Templates Tests have shown that application of a 1-D fixed pattern template to a
COS spectrum can reduce the fixed pattern noise in G130M or G160M
spectra to an equivalent S/N of about 30/1
For this to be occur, the
template must be derived from data for the same grating and nearly the
same central wavelength as the observation
This is because each
grating has a different cross dispersion profile, and different
central wavelengths fall at different cross dispersion detector
locations
As a result, spectra obtained at each grating and central
wavelength setting are derived from different regions of the detectors
-- each with their own, unique detector features and grid wire
shadows
ACS/WFC 11995 CCD Daily Monitor (Part 2) 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 320 orbits (20 weeks) from 1 February
2010 to 20 June 2010
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 11915 IR Internal Flat Fields This program is the same as 11433 (SMOV) and depends on the completion
of the IR initial alignment (Program 11425)
This version contains
three instances of 37 internal orbits: to be scheduled early, middle,
and near the end of Cycle 17, in order to use the entire 110-orbit
allocation
In this test, we will study the stability and structure of the IR
channel flat field images through all filter elements in the WFC3-IR
channel
Flats will be monitored, i
e
to capture any temporal trends
in the flat fields and delta flats produced
High signal observations
will provide a map of the pixel-to-pixel flat field structure, as well
as identify the positions of any dust particles
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)
COS/NUV 11900 NUV Internal/External Wavelength Scale Monitor This program monitors the offsets between the wavelength scale set by
the internal wavecal versus that defined by absorption lines in
external targets
This is accomplished by observing two external
radial velocity standard targets: HD187691 with G225M and G285M and
HD6655 with G285M and G230L
The two standard targets have little flux
in the wavelength range covered by G185M and so Feige 48 (sdO) is
observed with this grating
Both Feige 48 and HD6655 are also observed
in SMOV
The cenwaves observed in this program are a subset of the
ones used during Cycle 17
Observing all cenwaves would require a
considerably larger number of orbits
Constraints on scheduling of
each target are placed so that each target is observed once every ~2-3
months
Observing the three targets every month would also require a
considerably larger number of orbits
STIS/CC 11847 CCD Bias Monitor-Part 2 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/CC 11845 CCD Dark Monitor Part 2 Monitor the darks for the STIS CCD
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
COS/NUV/FUV 11742 Probing HeII Reionization with GALEX-selected Quasar Sightlines and
HST/COS We propose spectroscopic observations with COS of eight z~3 QSOs that
we found to be bright in the far ultraviolet
Our aim is to study
intergalactic absorption caused by the onset of the He II Lyman
forest
Several lines of evidence suggest that helium reionization
occurred at z~3
Understanding this process is critical for a complete
picture of the intergalactic medium and its evolution; it also gives
clues to hydrogen reionization at z>6
The only direct means of
assessing He II reionization is through far-UV observations of the He
II Lyman alpha forest
Only 6 sightlines are known to date where this
is feasible, despite extensive surveys
Our program is designed to
double the number of available sightlines
To this effect, we
cross-correlated all known z>2
73 quasars with UV source lists from
the GALEX satellite
The selected quasars were all significantly
detected in the far UV by GALEX, and their UV colors are similar to
those of already known quasars with transparent sightlines
Spectra
obtained with COS will allow us to compile the first comprehensive
sample of He II absorption spectra probing similar redshifts, enabling
a systematic investigation of the He II reionization epoch and the
spectral shape of the UV background
WFC3/UVIS 11732 The Temperature Profiles of Quasar Accretion Disks We can now routinely measure the size of quasar accretion disks using
gravitational microlensing of lensed quasars
At optical wavelengths
we observe a size and scaling with black hole mass roughly consistent
with thin disk theory but the sizes are larger than expected from the
observed optical fluxes
One solution would be to use a flatter
temperature profile, which we can study by measuring the wavelength
dependence of the disk size over the largest possible wavelength
baseline
Thus, to understand the size discrepancy and to probe closer
to the inner edge of the disk we need to extend our measurements to UV
wavelengths, and this can only be done with HST
For example, in the
UV we should see significant changes in the optical/UV size ratio with
black hole mass
We propose monitoring 5 lenses spanning a broad range
of black hole masses with well-sampled ground based light curves,
optical disk size measurements and known GALEX UV fluxes during Cycles
17 and 18 to expand from our current sample of two lenses
We would
obtain 5 observations of each target in each Cycle, similar to our
successful strategy for the first two targets
COS/NUV/FUV 11720 Detailed Analysis of Carbon Atmosphere White Dwarfs We propose to obtain UV spectra for the newly discovered white dwarf
stars with a carbon- dominated atmosphere
Model calculations show
that these stars emit most of their light in the UV part of the
electromagnetic spectrum and that an accurate determination of the
flux in this region is crucial for an accurate determination of the
atmospheric parameters
It will also provide a unique opportunity to
test the atomic data and broadening theory in stellar conditions never
met before
This will play a primordial role in our path to understand
the origin of these objects as well to obtain a better understanding
of the evolution of stars in general
The principal objective we hope
to achieve with these observations are 1) obtain accurate surface
gravity/mass for these stars, 2) constrain/determine the abundance of
other elements (O, He, Mg, Ne etc
), especially oxygen, 3) verify the
accuracy of the various theoretical atomic data used in the model
calculations, 4) understand the origin and evolution of carbon
atmosphere white dwarfs, in particular whether progenitor stars as
massive as 10
5 solar masses can produce white dwarfs, rather than
supernovae
We propose to observe 5 objects chosen carefully to cover
the range of observed properties among carbon atmosphere white dwarfs
(effective temperature, surface gravity, abundance of hydrogen/helium
and magnetic field)
FGS 11704 The Ages of Globular Clusters and the Population II Distance Scale Globular clusters are the oldest objects in the universe whose age can
be accurately determined
The dominant error in globular cluster age
determinations is the uncertain Population II distance scale
We
propose to use FGS 1R to obtain parallaxes with an accuracy of 0
2
milliarcsecond for 9 main sequence stars with [Fe/H] < -1
5
This will
determine the absolute magnitude of these stars with accuracies of
0
04 to 0
06mag
This data will be used to determine the distance to
24 metal-poor globular clusters using main sequence fitting
These
distances (with errors of 0
05 mag) will be used to determine the ages
of globular clusters using the luminosity of the subgiant branch as an
age indicator
This will yield absolute ages with an accuracy of 5%,
about a factor of two improvement over current estimates
Coupled with
existing parallaxes for more metal-rich stars, we will be able to
accurately determine the age for globular clusters over a wide range
of metallicities in order to study the early formation history of the
Milky Way and provide an independent estimate of the age of the
universe
The Hipparcos database contains only 1 star with [Fe/H] < -1
4 and an
absolute magnitude error less than 0
18 mag which is suitable for use
in main sequence fitting
Previous attempts at main sequence fitting
to metal-poor globular clusters have had to rely on theoretical
calibrations of the color of the main sequence
Our HST parallax
program will remove this source of possible systematic error and yield
distances to metal-poor globular clusters which are significantly more
accurate than possible with the current parallax data
The HST
parallax data will have errors which are 10 times smaller than the
current parallax data
Using the HST parallaxes, we will obtain main
sequence fitting distances to 11 globular clusters which contain over
500 RR Lyrae stars
This will allow us to calibrate the absolute
magnitude of RR Lyrae stars, a commonly used Population II distance
indicator
WFC3/UVIS/IR 11702 Search for Very High-z Galaxies with WFC3 Pure Parallel WFC3 will provide an unprecedented probe to the early universe beyond
the current redshift frontier
Here we propose a pure parallel program
using this new instrument to search for Lyman-break galaxies at
6
5 (1) We will use both the UVIS and the IR channels, and do not need to
seek optical data from elsewhere
(2) Our program will likely triple the size of the probable candidate
samples at z~7 and z~8, and will complement other targeted programs
aiming at the similar redshift range
(3) Being a pure parallel program, our survey will only make very
limited demand on the scarce HST resources
More importantly, as the
pure parallel pointings will be at random sight-lines, our program
will be least affected by the bias due to the large scale structure
("cosmic variance")
(4) We aim at the most luminous LBG population, and will address the
bright-end of the luminosity function at z~8 and z~7
We will
constrain the value of L* in particular, which is critical for
understanding the star formation process and the stellar mass assembly
history in the first few hundred million years of the universe
(5) The candidates from our survey, most of which will be the
brightest ones that any surveys would be able to find, will have the
best chance to be spectroscopically confirmed at the current 8--10m
telescopes
(6) We will also find a large number of extremely red, old galaxies at
intermediate redshifts, and the fine spatial resolution offered by the
WFC3 will enable us constrain their formation history based on the
study of their morphology, and hence shed light on their connection to
the very early galaxies in the universe
COS/FUV 11699 On the Evolutionary Status of Extremely Hot Helium Stars - are the
O(He) Stars Successors of the R CrB Stars? We propose UV spectroscopy of the four unique post-AGB stars of
spectral type O(He) in order to understand the origin of their
peculiar surface abundances
These stars are the only known amongst
the hottest post-AGB stars (effective temperatures > 100, 000 K) whose
atmospheres are composed of almost pure helium
This chemistry
markedly differs from that of the hydrogen-deficient post-AGB
evolutionary sequence with objects which have carbon dominated
atmospheres (PG1159 stars and Wolf-Rayet central stars)
While PG1159 and Wolf-Rayet stars are the result of a late
helium-shell flash, this scenario cannot explain the O(He) stars
Instead, they are possibly double-degenerate mergers
We speculate
that the four O(He) stars represent evolved RCrB stars, which also
have helium-dominated atmospheres
We aim to determine the C, N, O,
and Si abundances precisely, in order to proof this evolutionary link
COS/NUV/FUV 11698 The Structure and Dynamics of Virgo's Multi-Phase Intracluster Medium The dynamical flows of the intracluster medium (ICM) are largely
unknown
We propose to map the spatial and kinematic distribution of
the warm ICM of the nearby Virgo cluster using the Cosmic Origins
Spectrograph
15 sightlines at a range of impact parameters within the
virial radius of the cluster (0
2 - 1
7 Mpc) will be probed for
Lyman-alpha absorption and the data compared to blind HI, dust and
x-ray surveys to create a multi-phase map of the cluster's ICM
Absorption line sightlines are commonly 40-100 kpc from a galaxy,
allowing the flow of baryons between galaxies and the ICM to be
assessed
The velocity distribution of the absorbers will be directly
compared to simulations and used to constrain the turbulent motions of
the ICM
This proposal will result in the first map of a cluster's
warm ICM and provide important tests for our theoretical understanding
of cluster formation and the treatment of gas cooling in cosmological
simulations
WFC3/IR 11696 Infrared Survey of Star Formation Across Cosmic Time We propose to use the unique power of WFC3 slitless spectroscopy to
measure the evolution of cosmic star formation from the end of the
reionization epoch at z>6 to the close of the galaxy- building era at
z~0
3
Pure parallel observations with the grisms have proven to be
efficient for identifying line emission from galaxies across a broad
range of redshifts
The G102 grism on WFC3 was designed to extend this
capability to search for Ly-alpha emission from the first galaxies
Using up to 250 orbits of pure parallel WFC3 spectroscopy, we will
observe about 40 deep (4-5 orbit) fields with the combination of G102
and G141, and about 20 shallow (2-3 orbit) fields with G141 alone
Our primary science goals at the highest redshifts are: (1) Detect Lya
in ~100 galaxies with z>5
6 and measure the evolution of the Lya
luminosity function, independent of of cosmic variance; 2) Determine
the connection between emission line selected and continuum-break
selected galaxies at these high redshifts, and 3) Search for the
proposed signature of neutral hydrogen absorption at re-ionization
At
intermediate redshifts we will (4) Detect more than 1000 galaxies in
Halpha at 0
5 To identify single-line Lya emitters, we will exploit the wide
0
8--1
9um wavelength coverage of the combined G102+G141 spectra
All
[OII] and [OIII] interlopers detected in G102 will be reliably
separated from true LAEs by the detection of at least one strong line
in the G141 spectrum, without the need for any ancillary data
We
waive all proprietary rights to our data and will make high-level data
products available through the ST/ECF
WFC3/UV/IR 11620 A Quasar Light Echo in the Local Universe? The time history and duty cycle of individual AGN is an important part
of their evolution and the growth history of massive black holes, but
almost unconstrained on scales between galaxy-interaction timescales
(hundreds of Myr) and the scales of years probed by variability
measurements
We propose a detailed study of an object which seems to
be a large-scale light echo from a QSO-level episode in a nearby
galaxy
The Galaxy Zoo morphological survey of SDSS objects has
uncovered a peculiar emission-line structure whose spectrum matches
the narrow-line region of AGN, despite lying at least 20 kpc from a
galaxy whose activity is currently very weak
This is best explained
if the nucleus has faded dramatically on time scales of several tens
of thousands of years
We propose a suite of imaging and spectroscopic
observations to probe its properties, and the time history of this
episode of nuclear activity, measuring time scales hitherto
unavailable
COS/NUV/FUV 11598 How Galaxies Acquire their Gas: A Map of Multiphase Accretion and
Feedback in Gaseous Galaxy Halos We propose to address two of the biggest open questions in galaxy
formation - how galaxies acquire their gas and how they return it to
the IGM - with a concentrated COS survey of diffuse multiphase gas in
the halos of SDSS galaxies at z = 0
15 - 0
35
Our chief science goal
is to establish a basic set of observational facts about the physical
state, metallicity, and kinematics of halo gas, including the sky
covering fraction of hot and cold material, the metallicity of infall
and outflow, and correlations with galaxy stellar mass, type, and
color - all as a function of impact parameter from 10 - 150 kpc
Theory suggests that the bimodality of galaxy colors, the shape of the
luminosity function, and the mass-metallicity relation are all
influenced at a fundamental level by accretion and feedback, yet these
gas processes are poorly understood and cannot be predicted robustly
from first principles
We lack even a basic observational assessment
of the multiphase gaseous content of galaxy halos on 100 kpc scales,
and we do not know how these processes vary with galaxy properties
This ignorance is presently one of the key impediments to
understanding galaxy formation in general
We propose to use the
high-resolution gratings G130M and G160M on the Cosmic Origins
Spectrograph to obtain sensitive column density measurements of a
comprehensive suite of multiphase ions in the spectra of 43 z < 1 QSOs
lying behind 43 galaxies selected from the Sloan Digital Sky Survey
In aggregate, these sightlines will constitute a statistically sound
map of the physical state and metallicity of gaseous halos, and
subsets of the data with cuts on galaxy mass, color, and SFR will seek
out predicted variations of gas properties with galaxy properties
Our
interpretation of these data will be aided by state-of-the-art
hydrodynamic simulations of accretion and feedback, in turn providing
information to refine and test such models
We will also use Keck,
MMT, and Magellan (as needed) to obtain optical spectra of the QSOs to
measure cold gas with Mg II, and optical spectra of the galaxies to
measure SFRs and to look for outflows
In addition to our other
science goals, these observations will help place the Milky Way's
population of multiphase, accreting High Velocity Clouds (HVCs) into a
global context by identifying analogous structures around other
galaxies
Our program is designed to make optimal use of the unique
capabilities of COS to address our science goals and also generate a
rich dataset of other absorption-line systems WFC3/ACS/IR 11597 Spectroscopy of IR-Selected Galaxy Clusters at 1 < z < 1
5 We propose to obtain WFC3 G141 and G102 slitless spectroscopy of
galaxy clusters at 1 < z < 1
5 that were selected from the IRAC survey
of the Bootes NDWFS field
Our IRAC survey contains the largest sample
of spectroscopically confirmed clusters at z > 1
The WFC3 grism data
will measure H-alpha to determine SFR, and fit models to the low
resolution continua to determine stellar population histories for the
brighter cluster members, and redshifts for the red galaxies too faint
for ground-based optical spectroscopy
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
WFC3/IR 11591 Are Low-Luminosity Galaxies Responsible for Cosmic Reionization? Our group has demonstrated that massive clusters, acting as powerful
cosmic lenses, can constrain the abundance and properties of
low-luminosity star-forming sources beyond z~6; such sources are
thought to be responsible for ending cosmic reionization
The large
magnification possible in the critical regions of well-constrained
clusters brings sources into view that lie at or beyond the limits of
conventional exposures such as the UDF
We have shown that the
combination of HST and Spitzer is particularly effective in delivering
the physical properties of these distant sources, constraining their
mass, age and past star formation history
Indirectly, we therefore
gain a valuable glimpse to yet earlier epochs
Recognizing the result
(and limitations) of blank field surveys, we propose a systematic
search through 10 lensing clusters with ACS/F814W and
WFC3/[F110W+F160W] (in conjunction with existing deep IRAC data)
Our
goal is to measure with great accuracy the luminosity function at z~7
over a range of at least 3 magnitude, based on the identification of
about 50 lensed galaxies at 6
5 WFC3/ACS/UVIS/IR 11570 Narrowing in on the Hubble Constant and Dark Energy A measurement of the Hubble constant to a precision of a few percent
would be a powerful aid to the investigation of the nature of dark
energy and a potent "end-to end" test of the present cosmological
model
In Cycle 15 we constructed a new streamlined distance ladder
utilizing high- quality type Ia supernova data and observations of
Cepheids with HST in the near-IR to minimize the dominant sources of
systematic uncertainty in past measurements of the Hubble constant and
reduce its total uncertainty to a little under 5%
Here we propose to
exploit this new route to reduce the remaining uncertainty by more
than 30%, translating into an equal reduction in the uncertainty of
the equation of state of dark energy
We propose three sets of
observations to reach this goal: a mosaic of NGC 4258 with WFC3 in
F160W to triple its sample of long period Cepheids, WFC3/F160W
observations of the 6 ideal SN Ia hosts to triple their samples of
Cepheids, and observations of NGC 5584 the host of a new SN Ia, SN
2007af, to discover and measure its Cepheids and begin expanding the
small set of SN Ia luminosity calibrations
These observations would
provide the bulk of a coordinated program aimed at making the
measurement of the Hubble constant one of the leading constraints on
dark energy
STIS/CCD 11567 Boron Abundances in Rapidly Rotating Early-B Stars Models of rotation in early-B stars predict that rotationally driven
mixing should deplete surface boron abundances during the
main-sequence lifetime of many stars
However, recent work has shown
that many boron depleted stars are intrinsically slow rotators for
which models predict no depletion should have occurred, while
observations of nitrogen in some more rapidly rotating stars show less
mixing than the models predict
Boron can provide unique information
on the earliest stages of mixing in B stars, but previous surveys have
been biased towards narrow- lined stars because of the difficulty in
measuring boron abundances in rapidly rotating stars
The two targets
observed as part of our Cycle 13 SNAP program 10175, just before STIS
failed, demonstrate that it is possible to make useful boron abundance
measurements for early-B stars with Vsin(i) above 100 km/s
We propose
to extend that survey to a large enough sample of stars to allow
statistically significant tests of models of rotational mixing in
early-B stars
ACS/WFC3/SBC 11564 Optical and Ultraviolet Photometry of Isolated Neutron Stars We propose ultraviolet and B-band observations of 5 nearby, thermally
emitting neutron stars
These data will measure the Rayleigh-Jeans
tails of their spectra, providing a vital complement to X-ray
spectroscopy and helping to constrain atmospheric models, working
toward the ultimate goal of unraveling the physics of neutron stars
With these data we will have good-quality optical and UV data for the
full sample of these objects, allowing detailed comparisons between
them
Finally, the data should allow us to measure proper motions for
one or two objects, and will serve as the reference data for the
remaining objects; such proper motions allow ages to be determined for
these objects by tracing them back to likely birth locations
WFC3/UV 11556 Investigations of the Pluto System We propose a set of high SNR observations of the Pluto system that
will provide improved lightcurves, orbits, and photometric properties
of Nix and Hydra
The key photometric result for Nix and Hydra will be
a vastly improved lightcurve shape and rotation period to test if the
objects are in synchronous rotation or not
A second goal of this
program will be to retrieve a new epoch of albedo map for the surface
of Pluto
These observations will also improve masses and in some case
densities for the bodies in the Pluto system
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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 (11909), will be used to generate the
necessary superbias
and superdark reference files for the
calibration pipeline (CDBS)
http://groups
google
com/group/sci
astro
hubble/t/559ccc9388346bab?hl=en
SCHEDULED SUCCESSFUL
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 (11909), will be used to generate the
necessary superbias
and superdark reference files for the
calibration pipeline (CDBS)
http://groups
google
com/group/sci
astro
hubble/t/9ab850417b6caa51?hl=en
SCHEDULED SUCCESSFUL
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