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- Daily Report #5186 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/a7027af2be9ada03?hl=en
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============================================================================== TOPIC: Daily Report #5186
http://groups google com/group/sci astro hubble/t/a7027af2be9ada03?hl=en
== 1 of 1 == Date: Wed, Sep 22 2010 10:43 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5186
PERIOD COVERED: 5am September 21 - 5am September 22, 2010 (DOY 264/09:00z-265/09:00z)
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )
HSTARS FOR DOY 251 & 252:
12422 - GSAcq(2,1,1) at 252/07:46:00z required two attempts for CT-DV on FGS2 12423 - GSAcq(1,2,1) at 251/06:57:37z required multiple attempts to achieve CT-DV
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 6 6 FGS REAcq 7 7 OBAD with Maneuver 8 8
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
COS/FUV 11619
Definitive ISM Abundances through Low-mass X-ray Binaries as Lighthouses
We propose observations of the UV spectra of two low-mass X-ray binaries (Sco X-1 and Cyg X-2) with existing Chandra X-Ray Observatory (CXO) data From the X-ray data we will measure total (phase-independent) column densities of O, Ne, and Fe From the UV data we will determine gas-phase column densities of H and O The data in conjunction will allow us to make unique measurements of the total interstellar abundances of oxygen, neon, and iron, and direct measurements of the dust-phase abundances of O and Fe
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
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
S/C 12046
COS FUV DCE Memory Dump
Whenever the FUV detector high voltage is on, count rate and current draw information is collected, monitored, and saved to DCE memory Every 10 msec the detector samples the currents from the HV power supplies (HVIA, HVIB) and the AUX power supply (AUXI) The last 1000 samples are saved in memory, along with a histogram of the number of occurrences of each current value
In the case of a HV transient (known as a "crackle" on FUSE), where one of these currents exceeds a preset threshold for a persistence time, the HV will shut down, and the DCE memory will be dumped and examined as part of the recovery procedure However, if the current exceeds the threshold for less than the persistence time (a "mini-crackle" in FUSE parlance), there is no way to know without dumping DCE memory By dumping and examining the histograms regularly, we will be able to monitor any changes in the rate of "mini-crackles" and thus learn something about the state of the detector
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
WFC3/ACS/IR 11600
Star Formation, Extinction, and Metallicity at 0
7 The global star formation rate (SFR) is ~10x higher at z=1 than today
This could be due to drastically elevated SFR in some fraction of
galaxies, such as mergers with central bursts, or a higher SFR across
the board
Either means that the conditions in z=1 star forming
galaxies could be quite different from local objects
The next step
beyond measuring the global SFR is to determine the dependence of SFR,
obscuration, metallicity, and size of the star-forming region on
galaxy mass and redshift
However, SFR indicators at z=1 typically
apply local calibrations for UV, [O II] and far-IR, and do not agree
with each other on a galaxy-by-galaxy basis
Extinction, metallicity,
and dust properties cause uncontrolled offsets in SFR calibrations
The great missing link is Balmer H-alpha, the most sensitive probe of
SFR
We propose a slitless WFC3/G141 IR grism survey of GOODS-N, at 2
orbits/pointing
It will detect Ha+[N II] emission from 0
7 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/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/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)
==============================================================================
TOPIC: Daily Report #5187 == 1 of 1 ==
Date: Thurs, Sep 23 2010 9:30 am
From: "Bassford, Lynn" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5187 PERIOD COVERED: 5am September 22 - 5am September 23, 2010 (DOY 265/09:00z-266/09:00z) FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: (None) COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 5 5
FGS REAcq 8 8
OBAD with Maneuver 7 7 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED: ACS/WFC 11996 CCD Daily Monitor (Part 3) 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 308 orbits (19
25 weeks) from 21 June
2010 to 1 November 2010
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
COS/NUV/FUV/STIS/CCD/MA1 11692 The LMC as a QSO Absorption Line System We propose to obtain high resolution, high signal-to-noise
observations of QSOs behind the Large Magellanic Clouds
These QSOs
are situated beyond the star forming disk of the galaxy, giving us the
opportunity to study the distribution of metals and energy in regions
lacking significant star formation
In particular, we will derive the
metallicities and study the ionization characteristics of LMC gas at
impact parameters 3-17 kpc
We will compare our results with high-z
QSO absorption line systems
FGS 12320 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 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
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
WFC3/UV 11605 Obtaining the Missing Links in the Test of Very Low Mass Evolutionary
Models with HST We are proposing for spatially resolved ACS+HRC observations of 11
very low mass binaries spanning late-M, L and T spectral types in
order to obtain precise effective temperature measurements for each
component
All of our targets are part of a program in which we are
measuring dynamical masses of very low-mass binaries to an
unprecedented precision of 10% (or better)
However, without precise
temperature measurements, the full scientific value of these mass
measurements cannot be realized
Together, mass and temperature
measurements will allow us to distinguish between brown dwarf
evolutionary models that make different assumptions about the interior
and atmospheric structure of these ultra-cool objects
While dynamical
masses can be obtained from the ground in the near-IR, obtaining
precise temperatures require access to optical data which, for these
sub-arcsecond binaries, can only be obtained from space with Hubble
WFC3/UV 12245 Orbital Evolution and Stability of the Inner Uranian Moons Nine densely-packed inner moons of Uranus show signs of chaos and
orbital instability over a variety of time scales
Many moons show
measureable orbital changes within a decade or less
Long-term
integrations predict that some moons could collide in less than one
million years
One faint ring embedded in the system may, in fact, be
the debris left behind from an earlier such collision
Meanwhile, the
nearby moon Mab falls well outside the influence of the others but
nevertheless shows rapid, as yet unexplained, changes in its orbit
It
is embedded within a dust ring that also shows surprising variability
A highly optimized series of observations with WFC3 over the next
three cycles will address some of the fundamental open questions about
this dynamically active system: Do the orbits truly show evidence of
chaos? If so, over what time scales? What can we say about the masses
of the moons involved? What is the nature of the variations in Mab's
orbit? Is Mab's motion predictable or random? Astrometry will enable
us to derive the orbital elements of these moons with 10-km precision
This will be sufficient to study the year-by-year changes and,
combined with other data from 2003-2007, the decadal evolution of the
orbits
The pairing of precise astrometry with numerical integrations
will enable us to derive new dynamical constraints on the masses of
these moons
Mass is the fundamental unknown quantity currently
limiting our ability to reproduce the interactions within this system
This program will also capitalize upon our best opportunity for nearly
40 years to study the unexplained variations in Uranus's faint outer
rings
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 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 11914 UVIS Earth Flats This program is an experimental path finder for Cycle 18 calibration
Visible-wavelength flat fields will be obtained by observing the dark
side of the Earth during periods of full moon illumination
The
observations will consist of full-frame streaked WFC3 UVIS imagery:
per 22- min total exposure time in a single "dark-sky" orbit, we
anticipate collecting 7000 e/pix in F606W or 4500 e/pix in F814W
To
achieve Poisson S/N > 100 per pixel, we require at least 2 orbits of
F606W and 3 orbits of F814W
For UVIS narrowband filters, exposures of 1 sec typically do not
saturate on the sunlit Earth, so we will take sunlit Earth flats for
three of the more-commonly used narrowband filters in Cycle 17 plus
the also-popular long-wavelength quad filters, for which we get four
filters at once
Why not use the Sunlit Earth for the wideband visible-light filters?
It is too bright in the visible for WFC3 UVIS minimum exposure time of
0
5 sec
Similarly, for NICMOS the sunlit-Earth is too bright which
saturates the detector too quickly and/or induces abnormal behaviors
such as super-shading (Gilmore 1998, NIC 098-011)
In the narrowband
visible and broadband near- UV its not too bright (predictions in Cox
et al
1987 "Standard Astronomical Sources for HST: 6
Spatially Flat
Fields
" and observations in ACS Program 10050)
Other possibilities? Cox et al
's Section II
D addresses many other
possible sources for flat fields, rejecting them for a variety of
reasons
A remaining possibility would be the totally eclipsed moon
Such eclipses provide approximately 2 hours (1 HST orbit) of
opportunity per year, so they are too rare to be generically useful
An advantage of the moon over the Earth is that the moon subtends less
than 0
25 square degree, whereas the Earth subtends a steradian or
more, so scattered light and light potentially leaking around the
shutter presents additional problems for the Earth
Also, we're unsure
if HST can point 180 deg from the Sun
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