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============================================================================== TOPIC: Daily Report #5020
http://groups google com/group/sci astro hubble/t/33ffef504a45330d?hl=en
== 1 of 1 == Date: Wed, Jan 27 2010 6:48Â am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5020
PERIOD COVERED: 5am January 26 - 5am January 27, 2010 (DOY 026/10:00z-027/10:00z)
OBSERVATIONS SCHEDULED
NIC2/WFC3/IR 11548
Infrared Imaging of Protostars in the Orion A Cloud: The Role of Environment in Star Formation
We propose NICMOS and WFC3/IR observations of a sample of 252 protostars identified in the Orion A cloud with the Spitzer Space Telescope These observations will image the scattered light escaping the protostellar envelopes, providing information on the shapes of outflow cavities, the inclinations of the protostars, and the overall morphologies of the envelopes In addition, we ask for Spitzer time to obtain 55-95 micron spectra of 75 of the protostars Combining these new data with existing 3 6 to 70 micron photometry and forthcoming 5-40 micron spectra measured with the Spitzer Space Telescope, we will determine the physical properties of the protostars such as envelope density, luminosity, infall rate, and outflow cavity opening angle By examining how these properties vary with stellar density (i e clusters vs groups vs isolation) and the properties of the surrounding molecular cloud; we can directly measure how the surrounding environment influences protostellar evolution, and consequently, the formation of stars and planetary systems Ultimately, this data will guide the development of a theory of protostellar evolution
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/CC/MA 11516
COS-GTO: Cold ISM
With the COS, we will be able to observe interstellar spectra in a new regime, translucent clouds, for atomic, ionic, and molecular lines and bands, and extinction curves The COS will allow us to observe stars with total visual extinctions up to 10 magnitudes, and the grain size indicator Rv up to 4 5 In translucent clouds we expect to see the transition from neutral and ionized carbon to mostly C I, and then from there, we should expect to see carbon increasingly locked up in molecular form, as CO Other species are expected to make similar transitions, so we should find detectable abundances of molecules such as H2O, OH, CS, CH2, SiO, and others; also, lower ionization fractions of the metallic elements - and higher depletions of those elements as well Given that we expect to find higher depletions, we should see an altered grain size distribution, which may show up in the extinction curves, probably as lower far-UV extinction than in diffuse clouds Finally, we will search for neutral PAHs in absorption, as diffuse bands in the UV, paralleling the optical DIBs (which are thought by some scientists to be formed by singly-ionized PAHs) In translucent clouds, models show that the PAHs will be neutral, not in cationic form
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
STIS/CCD 11844
CCD Dark Monitor Part 1
The purpose of this proposal is to monitor the darks for the STIS CCD
STIS/CCD 11846
CCD Bias Monitor-Part 1
The purpose of this proposal is to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns
STIS/CCD 11849
STIS CCD Hot Pixel Annealing
This purpose of this activity is to repair radiation induced hot pixel damage to the STIS CCD by warming the CCD to the ambient instrument temperature and annealing radiation-damaged pixels
Radiation damage creates hot pixels in the STIS CCD Detector Many of these hot pixels can be repaired by warming the CCD from its normal operating temperature near -83 deg C to the ambient instrument temperature (~ +5 deg C) for several hours The number of hot pixels repaired is a function of annealing temperature The effectiveness of the CCD hot pixel annealing process is assessed by measuring the dark current behavior before and after annealing and by searching for any window contamination effects
STIS/CCD/MA1 11737
The Distance Dependence of the Interstellar N/O Abundance Ratio: A Gould Belt Influence?
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/ACS/IR 11142
Revealing the Physical Nature of Infrared Luminous Galaxies at
0
3 Using HST and Spitzer We aim to determine physical properties of IR
luminous galaxies at 0
3 WFC3/ACS/IR 11677 Is 47 Tuc Young? Measuring its White Dwarf Cooling Age and Completing
a Hubble Legacy With this proposal we will firmly establish the age of 47 Tuc from its
cooling white dwarfs
47 Tuc is the nearest and least reddened of the
metal-rich disk globular clusters
It is also the template used for
studying the giant branches of nearby resolved galaxies
In addition,
the age sensitive magnitude spread between the main sequence turnoff
and horizontal branch is identical for 47 Tuc, two bulge globular
clusters and the bulge field population
A precise relative age
constraint for 47 Tuc, compared to the halo clusters M4 and NGC 6397,
both of which we recently dated via white dwarf cooling, would
therefore constrain when the bulge formed relative to the old halo
globular clusters
Of particular interest is that with the higher
quality ACS data on NGC 6397, we are now capable with the technique of
white dwarf cooling of determining ages to an accuracy of +/-0
4 Gyrs
at the 95% confidence level
Ages derived from the cluster turnoff are
not currently capable of reaching this precision
The important role
that 47 Tuc plays in galaxy formation studies, and as the metal-rich
template for the globular clusters, makes the case for a white dwarf
cooling age for this metal-rich cluster compelling
Several recent analyses have suggested that 47 Tuc is more than 2 Gyrs
younger than the Galactic halo
Others have suggested an age similar
to that of the most metal poor globular clusters
The current
situation is clearly uncertain and obviously a new approach to age
dating this important cluster is required
With the observations of 47 Tuc, this project will complete a legacy
for HST
It will be the third globular cluster observed for white
dwarf cooling; the three covering almost the full metallicity range of
the cluster system
Unless JWST has its proposed bluer filters (700
and 900 nm) this science will not be possible perhaps for decades
until a large optical telescope is again in space
Ages for globular
clusters from the main sequence turnoff are less precise than those
from white dwarf cooling making the science with the current proposal
truly urgent
WFC3/IR 11189 Probing the Early Universe with GRBs Cosmology is beginning to constrain the nature of the earliest stars
and galaxies to form in the Universe, but direct observation of
galaxies at z>6 remains highly challenging due to their scarcity,
intrinsically small size, and high luminosity distance
GRB
afterglows, thanks to their extreme luminosities, offer the
possibility of circumventing these normal constraints by providing
redshifts and spectral information which couldn't be obtained through
direct observation of the host galaxies themselves
In addition, the
association of GRBs with massive stars means that they are an
indicator of star formation, and that their hosts are likely
responsible for a large proportion of the ionizing radiation during
that era
Our collaboration is conducting a campaign to rapidly
identify and study candidate very high redshift bursts, bringing to
bear a network of 2, 4 and 8m telescopes with near-IR instrumentation
Swift has proven capable of detecting faint, distant GRBs, and
reporting accurate positions for many bursts in near real-time
Here
we propose to continue our HST program of targeting GRBs at z~6 and
above
HST is crucial to this endeavor, allowing us (a) to
characterize the basic properties, such as luminosity and color, and
in some cases morphologies, of the hosts, which is essential to
understanding these primordial galaxies and their relationship to
other galaxy populations; and (b) to monitor the late time afterglows
and hence compare them to lower-z bursts and test the use of GRBs as
standard candles
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)
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
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 6 6
FGS REAcq 8 8
OBAD with Maneuver 6 6 SIGNIFICANT EVENTS: (None) ==============================================================================
TOPIC: Daily Report #5021 == 1 of 1 ==
Date: Thurs, Jan 28 2010 7:14Â am
From: "Cooper, Joe" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5021 PERIOD COVERED: 5am January 27 - 5am January 28, 2010 (DOY 027/10:00z-028/10:00z) OBSERVATIONS SCHEDULED 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
STIS/CCD 11634 Probing the Collimation of Pristine Post-AGB Jets with STIS The shaping of planetary and protoplanetary nebulae (PNe and PPNe) is
probably the most exciting yet least understood problem in the late
evolution of ~1-8 solar mass stars
An increasing number of
astronomers believe that fast jet-like winds ejected in the PPN phase
are responsible for carving out the diverse shapes in the dense
envelopes of the Asymptotic Giant Branch (AGB) stars
To date, the
properties of these post-AGB jets have not been characterized and,
indeed, their launching/collimation mechanism is still subject to
controversial debate
This is due to the lack of the direct
observations probing the spatio-kinematic structure of post-AGB winds
in the stellar vicinity (~10e16cm), which is only possible with
HST+STIS
Recently, STIS observations have allowed us for the first time the
DIRECT study of the structure and kinematics of the elusive post-AGB
winds in one PPN, He3-1475 (Sanchez Contreras & Sahai 2001)
Those
winds have been discovered through H-alpha blue-shifted absorption
features in the inner 0
3"-0
7" of the nebula
These STIS observations
have revealed an ultra-fast collimated outflow relatively unaffected
by the interaction with the AGB wind that is totally hidden in
ground-based spectroscopic observations and HST images
The discovery
of the pristine ultra-fast (~2300km/s) jet in He3-1475 is the first
observational confirmation of the presence of collimated outflows as
close as ~10e16cm from the central star
Most importantly, the
spatio-kinematic structure of the ultra-fast jet clearly rules out
hydrodynamical collimation alone and favors magnetic wind collimation
Therefore, STIS observations provide a unique method of probing the
structure, kinematics, and collimation mechanism of the elusive
post-AGB winds
We now propose similar observations for a sample of
bipolar PPNe with ongoing post-AGB ejections in order to investigate
the frequency of jets like those in He3-1475 in other PPNe and
elucidate their nature and collimation mechanism
The observational
characterization of these winds is indispensable for understanding
this violent and important phase of post-AGB evolution
STIS/CCD 11844 CCD Dark Monitor Part 1 The purpose of this proposal is to monitor the darks for the STIS CCD
STIS/CCD 11846 CCD Bias Monitor-Part 1 The purpose of this proposal is to monitor the bias in the 1x1, 1x2,
2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up
high-S/N superbiases and track the evolution of hot columns
STIS/MA1/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 1314s FUV-MAMA Time-Tag
darks or five 3x315s 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/ACS/IR 11677 Is 47 Tuc Young? Measuring its White Dwarf Cooling Age and Completing
a Hubble Legacy With this proposal we will firmly establish the age of 47 Tuc from its
cooling white dwarfs
47 Tuc is the nearest and least reddened of the
metal-rich disk globular clusters
It is also the template used for
studying the giant branches of nearby resolved galaxies
In addition,
the age sensitive magnitude spread between the main sequence turnoff
and horizontal branch is identical for 47 Tuc, two bulge globular
clusters and the bulge field population
A precise relative age
constraint for 47 Tuc, compared to the halo clusters M4 and NGC 6397,
both of which we recently dated via white dwarf cooling, would
therefore constrain when the bulge formed relative to the old halo
globular clusters
Of particular interest is that with the higher
quality ACS data on NGC 6397, we are now capable with the technique of
white dwarf cooling of determining ages to an accuracy of +/-0
4 Gyrs
at the 95% confidence level
Ages derived from the cluster turnoff are
not currently capable of reaching this precision
The important role
that 47 Tuc plays in galaxy formation studies, and as the metal-rich
template for the globular clusters, makes the case for a white dwarf
cooling age for this metal-rich cluster compelling
Several recent analyses have suggested that 47 Tuc is more than 2 Gyrs
younger than the Galactic halo
Others have suggested an age similar
to that of the most metal poor globular clusters
The current
situation is clearly uncertain and obviously a new approach to age
dating this important cluster is required
With the observations of 47 Tuc, this project will complete a legacy
for HST
It will be the third globular cluster observed for white
dwarf cooling; the three covering almost the full metallicity range of
the cluster system
Unless JWST has its proposed bluer filters (700
and 900 nm) this science will not be possible perhaps for decades
until a large optical telescope is again in space
Ages for globular
clusters from the main sequence turnoff are less precise than those
from white dwarf cooling making the science with the current proposal
truly urgent
WFC3/IR 11189 Probing the Early Universe with GRBs Cosmology is beginning to constrain the nature of the earliest stars
and galaxies to form in the Universe, but direct observation of
galaxies at z>6 remains highly challenging due to their scarcity,
intrinsically small size, and high luminosity distance
GRB
afterglows, thanks to their extreme luminosities, offer the
possibility of circumventing these normal constraints by providing
redshifts and spectral information which couldn't be obtained through
direct observation of the host galaxies themselves
In addition, the
association of GRBs with massive stars means that they are an
indicator of star formation, and that their hosts are likely
responsible for a large proportion of the ionizing radiation during
that era
Our collaboration is conducting a campaign to rapidly
identify and study candidate very high redshift bursts, bringing to
bear a network of 2, 4 and 8m telescopes with near-IR instrumentation
Swift has proven capable of detecting faint, distant GRBs, and
reporting accurate positions for many bursts in near real-time
Here
we propose to continue our HST program of targeting GRBs at z~6 and
above
HST is crucial to this endeavor, allowing us (a) to
characterize the basic properties, such as luminosity and color, and
in some cases morphologies, of the hosts, which is essential to
understanding these primordial galaxies and their relationship to
other galaxy populations; and (b) to monitor the late time afterglows
and hence compare them to lower-z bursts and test the use of GRBs as
standard candles
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 11577 Opening New Windows on the Antennae with WFC3 We propose to use WFC3 to provide key observations of young star
clusters in "The Antennae" (NGC4038/39)
Of prime importance is the
WFC3's ability to push the limiting UV magnitude FIVE mag deeper than
our previous WFPC2 observations
This corresponds to pushing the
limiting cluster mass from ~10*5 to ~103 solar masses for cluster
ages ~10*8 yrs
In addition, the much wider field of view of the WFC3
IR channel will allow us to map out both colliding disks rather than
just the Overlap Region between them
This will be especially
important for finding the youngest clusters that are still embedded in
their placental cocoons
The extensive set of narrow-band filters will
provide an effective means for determining the properties of shocks,
which are believed to be a primary triggering mechanism for star
formation
We will also use ACS in parallel with WFC3 to observe
portions of both the northern and southern tails at no additional
orbital cost
Finally, one additional primary WFC3 orbit will be used
to supplement existing HST observations of the star-forming "dwarf"
galaxy at the end of the southern tail
Hence, when completed we will
have full UBVI + H_alpha coverage (or more for the main galaxy) of
four different environments in the Antennae
In conjunction with the
extensive multi- wavelength database we have collected (both HST and
ground based) these observations will provide answers to fundamental
questions such as: How do these clusters form and evolve? How is star
formation triggered? How do star clusters affect the local and global
ISM, and the evolution of the galaxy as a whole? The Antennae galaxies
are the nearest example of a major disk--disk merger, and hence may
represent our best chance for understanding how mergers form
tremendous numbers of clusters and stars, both in the local universe
and during galaxy assembly at high redshift
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/IR 11644 A Dynamical-Compositional Survey of the Kuiper Belt: A New Window Into
the Formation of the Outer Solar System The eight planets overwhelmingly dominate the solar system by mass,
but their small numbers, coupled with their stochastic pasts, make it
impossible to construct a unique formation history from the dynamical
or compositional characteristics of them alone
In contrast, the huge
numbers of small bodies scattered throughout and even beyond the
planets, while insignificant by mass, provide an almost unlimited
number of probes of the statistical conditions, history, and
interactions in the solar system
To date, attempts to understand the
formation and evolution of the Kuiper Belt have largely been dynamical
simulations where a hypothesized starting condition is evolved under
the gravitational influence of the early giant planets and an attempt
is made to reproduce the current observed populations
With little
compositional information known for the real Kuiper Belt, the test
particles in the simulation are free to have any formation location
and history as long as they end at the correct point
Allowing
compositional information to guide and constrain the formation,
thermal, and collisional histories of these objects would add an
entire new dimension to our understanding of the evolution of the
outer solar system
While ground based compositional studies have hit
their flux limits already with only a few objects sampled, we propose
to exploit the new capabilities of WFC3 to perform the first ever
large-scale dynamical-compositional study of Kuiper Belt Objects
(KBOs) and their progeny to study the chemical, dynamical, and
collisional history of the region of the giant planets
The
sensitivity of the WFC3 observations will allow us to go up to two
magnitudes deeper than our ground based studies, allowing us the
capability of optimally selecting a target list for a large survey
rather than simply taking the few objects that can be measured, as we
have had to do to date
We have carefully constructed a sample of 120
objects which provides both overall breadth, for a general
understanding of these objects, plus a large enough number of objects
in the individual dynamical subclass to allow detailed comparison
between and within these groups
These objects will likely define the
core Kuiper Belt compositional sample for years to come
While we have
many specific results anticipated to come from this survey, as with
any project where the field is rich, our current knowledge level is
low, and a new instrument suddenly appears which can exploit vastly
larger segments of the population, the potential for discovery -- both
anticipated and not -- is extraordinary
FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: (None) COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 6 6
FGS REAcq 9 9
OBAD with Maneuver 6 6 SIGNIFICANT EVENTS: (None) ============================================================================== You received this message because you are subscribed to the Google Groups "sci
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