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============================================================================== TOPIC: Daily Report #5104
http://groups google com/group/sci astro hubble/t/6bd4a91181f09ac3?hl=en
== 1 of 1 == Date: Wed, May 26 2010 5:24 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5104
PERIOD COVERED: 5am May 25 - 5am May 26, 2010 (DOY 145/09:00z-146/09:00z)
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)
SCHEDULED SUCCESSFUL
FGS GSAcq 06 06 FGS REAcq 09 09 OBAD with Maneuver 05 05
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
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
COS/FUV 11895
FUV Detector Dark Monitor
Monitor the FUV detector dark rate by taking long science exposures without illuminating the detector The detector dark rate and spatial distribution of counts will be compared to pre-launch and SMOV data in order to verify the nominal operation of the detector Variations of count rate as a function of orbital position will be analyzed to find dependence of dark rate on proximity to the SAA Dependence of dark rate as function of time will also be tracked
COS/FUV/COS/NUV 11579
The Difference Between Neutral- and Ionized-Gas Metal Abundances in Local Star-Forming Galaxies with COS
The metallicity of galaxies and its evolution with redshift is of paramount importance for understanding galaxy formation Abundances in the interstellar medium (ISM) are typically determined using emission-line spectroscopy of HII regions However, since HII regions are associated with recent SF they may not have abundances typical for the galaxy as a whole This is true in particular for star-forming galaxies (SFGs), in which the bulk of the metals may be contained in the neutral gas It is therefore important to directly probe the metal abundances in the neutral gas This can be done using absorption lines in the Far UV We have developed techniques to do this in SFGs, where the absorption is measured for sightlines toward bright SF regions within the galaxy itself We have successfully applied this technique to a sample of galaxies observed with FUSE The results have been very promising, suggesting in I Zw 18 that abundances in the neutral gas may be up to 0 5 dex lower than in the ionized gas However, the interpretation of the FUSE data is complicated by the very large FUSE aperture (30 arcsec), the modest S/N, and the limited selection of species available in the FUSE bandpass The advent of COS on HST now allows a significant advance in all of these areas We will therefore obtain absorption line spectroscopy with G130M in the same sample for which we already have crude constraints from FUSE We will obtain ACS/SBC images to select the few optimal sightlines to target in each galaxy The results will be interpreted through line-profile fitting to determine the metal abundances constrained by the available lines The results will provide important new insights into the metallicities of galaxies, and into outstanding problems at high redshift such as the observed offset between the metallicities of Lyman Break Galaxies and Damped Lyman Alpha systems
COS/FUV/COS/NUV 11601
UV spectroscopy of the hot bare stellar core H1504+65
H1504+65 is the hottest known white dwarf (Teff=200, 000 K) It has an extraordinary surface composition The surface is devoid of hydrogen and helium It is mainly composed of carbon and oxygen (by equal amounts) and neon (2%) We obviously see the exposed core of a former red giant The evolutionary history of this unique object is unknown We have identified magnesium absorption lines in the soft X-ray photospheric Chandra spectrum, which suggests that H1504+65 may be an O-Ne-Mg white dwarf We will test this hypothesis by abundance determinations of Mg and Na If confirmed, then H1504+65 would be the most compelling case for the existence of single O-Ne-Mg white dwarfs
COS/FUV/COS/NUV 11741
Probing Warm-Hot Intergalactic Gas at 0 5 < z < 1 3 with a Blind Survey for O VI, Ne VIII, Mg X, and Si XII Absorption Systems
Currently we can only account for half of the baryons (or less) expected to be found in the nearby universe based on D/H and CMB observations This "missing baryons problem" is one of the highest-priority challenges in observational extragalatic astronomy Cosmological simulations suggest that the baryons are hidden in low-density, shock-heated intergalactic gas in the log T = 5 - 7 range, but intensive UV and X-ray surveys using O VI, O VII, and O VIII absorption lines have not yet confirmed this prediction We propose to use COS to carry out a sensitive survey for Ne VIII and Mg X absorption in the spectra of nine QSOs at z(QSO) > 0 89 For the three highest-redshift QSOs, we will also search for Si XII This survey will provide more robust constraints on the quantity of baryons in warm-hot intergalactic gas at 0 5 < z < 1 3, and the data will provide rich constraints on the metal enrichment, physical conditions, and nature of a wide variety of QSO absorbers in addition to the warm-hot systems By comparing the results to other surveys at lower redshifts (with STIS, FUSE, and from the COS GTO programs), the project will also enable the first study of how these absorbers evolve with redshift at z < 1 By combining the program with follow-up galaxy redshift surveys, we will also push the study of galaxy-absorber relationships to higher redshifts, with an emphasis on the distribution of the WHIM with respect to the large-scale matter distribution of the universe
COS/NUV 11520
COS-GTO: QSO Absorbers, Galaxies and Large-scale Structures in the Local Universe
This is a program to probe the large scale structure of baryons in the universe, including addressing questions of baryon fraction, physical conditions and relationships between absorbers and large-scale structures of galaxies Besides these specific goals, this proposed GTO program also probes a large enough total path length in Ly alpha and OVI to add significantly to what STIS/FUSE has already observed Several Galactic High Velocity Cloud Complexes also are probed by these sightlines, particularly the M Complex The total path length of this proposed program for Ly alpha large-scale structure surveys is delta_z~5 5
We have selected a variety of targets to address these questions, under the following subcategories:
Target 8 bright BL Lac objects to search for low contrast Ly alpha absorbers from the warm-hot interstellar medium (WHIM) Science drivers: What are physical conditions and extent of warm-hot IGM in the current epoch? Can we discover metal-poor WHIM using very broad Ly alpha lines? What is the number density of such lines (dN/dz) and what is their relationship if any with tentative Chandra detections of even hotter gas?
Ly alpha cloud sizes: The targets are a bright AGN pair which yield tangential distance separations of 100--500 kpc at z=0 01--0 05, where galaxy surveys are excellent This pair has two filaments and two voids in this distance range Science drivers: What are the characteristic sizes of Ly alpha absorbers, weak metal-line absorbers and absorbers in voids? Better size determinations will tighten current estimates of the baryon content of the photoionzed IGM
Probes of starburst outflows: The targets are bright AGN, <= 100 kpc in projection out of the minor axis of nearby starburst galaxies Science drivers: Outflowing, unbound winds have been implicated as a primary mechanism to enrich the IGM in mass, metals and energy But do starburst winds from massive galaxies escape the galaxy's gravitational potential? If so, what is the metallicity and what are mass outflow rates of these winds?
A large galaxy's gaseous halo: Three probes of the kinematics and metallicity of a single L* galaxy halo These observations includes G130M, G160M exposures at SNR~20 and G285M at 2850A and SNR~10 for MgII The 2L* galaxy, ESO 157-G049 (cz=1678 km/s), being probed by these sightlines has an available H I 21cm map from ATCA, H alpha imaging from CTIO and long-slit spectra from MSSSO Science drivers: What are the extent, metallicity, ionization conditions and kinematics of gaseous halos of normal luminous (L*) galaxies? Is there evidence for outflow, inflow or galactic fountain circulation of gas in massive galaxy halos? What is the source of halo gas (outflowing winds, infalling metal-poor gas from stripping of nearby dwarf galaxies, nuclear outflows, large numbers of bound dark matter halos??) and what is the relationship between this gas and Galactic high-velocity clouds (HVCs)?
Dwarf galaxy
COS/NUV 11894
NUV Detector Dark Monitor
Measure the NUV detector dark rate by taking long science exposures with no light on the detector The detector dark rate and spatial distribution of counts will be compared to pre-launch and SMOV data in order to verify the nominal operation of the detector Variations of count rate as a function of orbital position will be analyzed to find dependence of dark rate on proximity to the SAA Dependence of dark rate as function of time will also be tracked
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/CCD 11855
STIS/CCD Spectroscopic Sensitivity Monitor for Cycle 17
Monitor sensitivity of each CCD grating mode to detect any change due to contamination or other causes
WFC3/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
WFC3/IR 11712
Calibration of Surface Brightness Fluctuations for WFC3/IR
We aim to characterize galaxy surface brightness fluctuations (SBF), and calibrate the SBF distance method, in the F110W and F160W filters of the Wide Field Camera 3 IR channel Because of the very high throughput of F110W and the good match of F160W to the standard H band, we anticipate that both of these filters will be popular choices for galaxy observations with WFC3/IR The SBF signal is typically an order of magnitude brighter in the near-IR than in the optical, and the characterisitics (sensitivity, FOV, cosmetics) of the WFC3/IR channel will be enormously more efficient for SBF measurements than previously available near-IR cameras As a result, our proposed SBF calibration will allow accurate distance derivation whenever an early-type or bulge-dominated galaxy is observed out to a distance of 150 Mpc or more (i e , out to the Hubble flow) in the calibrated passbands For individual galaxy observations, an accurate distance is useful for establishing absolute luminosities, black hole masses, linear sizes, etc Eventually, once a large number of galaxies have been observed across the sky with WFC3/IR, this SBF calibration will enable accurate mapping of the total mass density distribution in the local universe using the data available in the HST archive The proposed observations will have additional important scientific value; in particular, we highlight their usefulness for understanding the nature of multimodal globular cluster color distributions in giant elliptical galaxies
WFC3/UVI 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
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
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)
WFC3/UVI 11909
UVIS Hot Pixel Anneal
The on-orbit radiation environment of WFC3 will continually generate new hot pixels This proposal performs the procedure required for repairing those hot pixels in the UVIS CCDs During an anneal, the two-stage thermo-electric cooler (TEC) is turned off and the four-stage TEC is used as a heater to bring the UVIS CCDs up to ~20C As a result of the CCD warmup, a majority of the hot pixels will be fixed; previous instruments such as WFPC2 and ACS have seen repair rates of about 80% Internal UVIS exposures are taken before and after each anneal, to allow an assessment of the procedure's effectiveness in WFC3, provide a check of bias, global dark current, and hot pixel levels, as well as support hysteresis (bowtie) monitoring and CDBS reference file generation One IR dark is taken after each anneal, to provide a check of the IR detector
============================================================================== TOPIC: Daily Report #5105
http://groups google com/group/sci astro hubble/t/57d5d62643e7602d?hl=en
== 1 of 1 == Date: Thurs, May 27 2010 8:20 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5105
PERIOD COVERED: 5am May 26 - 5am May 27, 2010 (DOY 146/09:00z-147/09:00z)
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)
SCHEDULED SUCCESSFUL
FGS GSAcq 07 07 FGS REAcq 08 08 OBAD with Maneuver 04 04
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
COS/FUV 11592
Testing the Origin(s) of the Highly Ionized High-Velocity Clouds: A Survey of Galactic Halo Stars at z>3 kpc
Cosmological simulation predicts that highly ionized gas plays an
important role in the formation and evolution of galaxies and their
interplay with the intergalactic medium
The NASA HST and FUSE
missions have revealed high-velocity CIV and OVI absorption along
extragalactic sightlines through the Galactic halo
These highly
ionized high-velocity clouds (HVCs) could cover 85% of the sky and
have a detection rate higher than the HI HVCs
Two competing, equally
exciting, theories may explain the origin of these highly ionized
HVCs: 1) the "Galactic" theory, where the HVCs are the result of
feedback processes and trace the disk-halo mass exchange, perhaps
including the accretion of matter condensing from an extended corona;
2) the "Local Group" theory, where they are part of the local warm-hot
intergalactic medium, representing some of the missing baryonic matter
of the Universe
Only direct distance determinations can discriminate
between these models
Our group has found that some of these highly
ionized HVCs have a Galactic origin, based on STIS observations of one
star at z<5
3 kpc
We propose an HST FUV spectral survey to search for
and characterize the high velocity NV, CIV, and SiIV interstellar
absorption toward 24 stars at much larger distances than any previous
searches (4 COS/FUV 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
COS/FUV 11895 FUV Detector Dark Monitor Monitor the FUV detector dark rate by taking long science exposures
without illuminating the detector
The detector dark rate and spatial
distribution of counts will be compared to pre-launch and SMOV data in
order to verify the nominal operation of the detector
Variations of
count rate as a function of orbital position will be analyzed to find
dependence of dark rate on proximity to the SAA
Dependence of dark
rate as function of time will also be tracked
COS/FUV/COS/NUV 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 along a significant
total pathlength through the IGM (Delta z ~ 20)
COS/FUV/COS/NUV 11829 Coronal and Transition Region Heating Due to Magnetic Activity on
Metal-Poor Dwarf Stars How does low metallicity affect the heating and resultant temperature
structure of the chromospheres, transition regions, and coronae of old
solar-like dwarf stars? Our ACIS-S observations of 7 Gyr old Arcturus
Moving Group (AMG) dwarfs show very little conventional coronal (> 1
MK) plasma and suggest that these stars have insufficient magnetic
energy input to power a solar-like corona
However, they do have
chomospheres and transition regions similar to the minimum activity
Quiet Sun
It this typical or an aberration of the AMG? We propose a
35 ksec ACIS-S observation and HST COS spectroscopy of the nearest
(9
2 pc), truely metal-poor ([Fe/H] = -1
4) dwarf star that is known
to have definite magnetic dynamo activity (activity cycles, active
region modulation) -- HD103095 -- to investigate this question
further
COS/NUV 11667 Detailed Probing of a 3000 km/s Ly-alpha + Metal Line Absorption
Complex Near Two Galaxies at z=0
67 At intermediate redshifts, Ly-alpha absorbers cluster around rich
metal-line systems [those with numerous low and high ionization
species (Bahcall et al
)], and at z=3, higher ionization clouds reside
at the velocity extremes of clustered Ly-alpha lines, a signature of
the physics of collapse and layered gas structures (Songaila & Cowie)
These extraordinary HI environments provide unique astrophysical
laboratories for probing relatively high overdensity IGM structures
and for placing powerful constraints on our understanding of the
intergalactic medium and extended galaxy halos in the context of
structure evolution, galactic stellar feedback chemical enrichment to
large galactocentric distances, and the cosmic baryon budget
We have undertaken a comprehensive study of the remarkable 1400 km/s
velocity width, optically thin Ly-alpha only complex (five components)
at z=0
67 within 1600 km/s of the Lyman limit z=0
66 metal-line system
toward TON 153 (Churchill et al
)
We have collected FOS, STIS, and
HIRES quasar spectra covering the Lyman series, OVI, CIV, and MgII
absorption, an F702W/WFPC-2 image, and set of ground based narrow-band
SDSS filter images of the quasar field
Two galaxies aligned in
velocity with the z=0
67 Ly-alpha complex and z=0
66 metal-line system
lie within 100 kpc of the quasar sightline; the absorption is not
consistent with our standard model of extended "halo" gas for either
galaxy, which suggests that a large scale structure (i
e
, filament)
may extend between these galaxies
We propose to obtain G160M/1600 and G185M/1921+1941 (S/N>10) COS
spectra of the z=1
01 quasar TON 153 to obtain detailed kinematic,
chemical, and ionization conditions of this extraordinary
absorber/galaxy system (total velocity spread 3000 km/s)
The propose
observations will provide an unprecedented first high resolution
examination of the full Lyman series and MgII, CIV, and OVI metal
lines arising in galaxy halos or a possible large scale structure
(i
e
, filament) asscociated with thoroughly studied galaxies
We aim
to discern if the HI extends between the galaxies and test for
multiphase absorption signatures suggestive of a galactic feedback or
large scale collapsing structure
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 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
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 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 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/UVI 11909 UVIS Hot Pixel Anneal The on-orbit radiation environment of WFC3 will continually generate
new hot pixels
This proposal performs the procedure required for
repairing those hot pixels in the UVIS CCDs
During an anneal, the
two-stage thermo-electric cooler (TEC) is turned off and the
four-stage TEC is used as a heater to bring the UVIS CCDs up to ~20C
As a result of the CCD warmup, a majority of the hot pixels will be
fixed; previous instruments such as WFPC2 and ACS have seen repair
rates of about 80%
Internal UVIS exposures are taken before and after
each anneal, to allow an assessment of the procedure's effectiveness
in WFC3, provide a check of bias, global dark current, and hot pixel
levels, as well as support hysteresis (bowtie) monitoring and CDBS
reference file generation
One IR dark is taken after each anneal, to
provide a check of the IR detector
==============================================================================
TOPIC: Daily Report #5106 == 1 of 1 ==
Date: Fri, May 28 2010 7:37 am
From: "Cooper, Joe" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5106 PERIOD COVERED: 5am May 27 - 5am May 28, 2010 (DOY 147/09:00z-148/09:00z) FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: FOR DOY 137 12289 - GSAcq(2,1,2) at 137/17:14:52z failed to Fine Lock backup on
FGS2 with scan step limit exceed on FGS1
Observations possibly affected, WFC 34 Proposal ID# 11536 COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 08 08
FGS REAcq 10 10
OBAD with Maneuver 02 02 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED: 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
COS/FUV/COS/NUV 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 along a significant
total pathlength through the IGM (Delta z ~ 20)
COS/FUV/COS/NUV 11741 Probing Warm-Hot Intergalactic Gas at 0
5 < z < 1
3 with a Blind
Survey for O VI, Ne VIII, Mg X, and Si XII Absorption Systems Currently we can only account for half of the baryons (or less)
expected to be found in the nearby universe based on D/H and CMB
observations
This "missing baryons problem" is one of the
highest-priority challenges in observational extragalatic astronomy
Cosmological simulations suggest that the baryons are hidden in
low-density, shock-heated intergalactic gas in the log T = 5 - 7
range, but intensive UV and X-ray surveys using O VI, O VII, and O
VIII absorption lines have not yet confirmed this prediction
We
propose to use COS to carry out a sensitive survey for Ne VIII and Mg
X absorption in the spectra of nine QSOs at z(QSO) > 0
89
For the
three highest-redshift QSOs, we will also search for Si XII
This
survey will provide more robust constraints on the quantity of baryons
in warm-hot intergalactic gas at 0
5 < z < 1
3, and the data will
provide rich constraints on the metal enrichment, physical conditions,
and nature of a wide variety of QSO absorbers in addition to the
warm-hot systems
By comparing the results to other surveys at lower
redshifts (with STIS, FUSE, and from the COS GTO programs), the
project will also enable the first study of how these absorbers evolve
with redshift at z < 1
By combining the program with follow-up galaxy
redshift surveys, we will also push the study of galaxy-absorber
relationships to higher redshifts, with an emphasis on the
distribution of the WHIM with respect to the large-scale matter
distribution of the universe
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 11202 The Structure of Early-type Galaxies: 0
1-100 Effective Radii The structure, formation and evolution of early-type galaxies is still
largely an open problem in cosmology: how does the Universe evolve
from large linear scales dominated by dark matter to the highly
non-linear scales of galaxies, where baryons and dark matter both play
important, interacting, roles? To understand the complex physical
processes involved in their formation scenario, and why they have the
tight scaling relations that we observe today (e
g
the Fundamental
Plane), it is critically important not only to undertstand their
stellar structure, but also their dark-matter distribution from the
smallest to the largest scales
Over the last three years the SLACS collaboration has developed a
toolbox to tackle these issues in a unique and encompassing way by
combining new non-parametric strong lensing techniques, stellar
dynamics, and most recently weak gravitational lensing, with
high-quality Hubble Space Telescope imaging and VLT/Keck spectroscopic
data of early-type lens systems
This allows us to break degeneracies
that are inherent to each of these techniques seperately and probe the
mass structure of early-type galaxies from 0
1 to 100 effective radii
The large dynamic range to which lensing is sentive allows us both to
probe the clumpy substructure of these galaxies, as well as their
low-density outer haloes
These methods have convincingly been
demonstrated, by our team, using smaller pilot-samples of SLACS lens
systems with HST data
In this proposal, we request observing time with WFPC2 and NICMOS to
observe 53 strong lens systems from SLACS, to obtain complete
multi-color imaging for each system
This would bring the total number
of SLACS lens systems to 87 with completed HST imaging and effectively
doubles the known number of galaxy-scale strong lenses
The deep HST
images enable us to fully exploit our new techniques, beat down
low-number statistics, and probe the structure and evolution of
early-type galaxies, not only with a uniform data-set an order of
magnitude larger than what is available now, but also with a fully
coherent and self-consistent methodological approach! WFC3/IR 11219 Active Galactic Nuclei in nearby galaxies: a new view of the origin of
the radio-loud radio-quiet dichotomy? Using archival HST and Chandra observations of 34 nearby early-type
galaxies (drawn from a complete radio selected sample) we have found
evidence that the radio-loud/radio-quiet dichotomy is directly
connected to the structure of the inner regions of their host galaxies
in the following sense: [1] Radio-loud AGN are associated with
galaxies with shallow cores in their light profiles [2] Radio-quiet
AGN are only hosted by galaxies with steep cusps
Since the brightness
profile is determined by the galaxy's evolution, through its merger
history, our results suggest that the same process sets the AGN
flavour
This provides us with a novel tool to explore the
co-evolution of galaxies and supermassive black holes, and it opens a
new path to understand the origin of the radio-loud/radio-quiet AGN
dichotomy
Currently our analysis is statistically incomplete as the
brightness profile is not available for 82 of the 116 targets
Most
galaxies were not observed with HST, while in some cases the study is
obstructed by the presence of dust features
We here propose to
perform an infrared NICMOS snapshot survey of these 82 galaxies
This
will enable us to i) test the reality of the dichotomic behaviour in a
substantially larger sample; ii) extend the comparison between
radio-loud and radio-quiet AGN to a larger range of luminosities
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 11700 Bright Galaxies at z>7
5 with a WFC3 Pure Parallel Survey The epoch of reionization represents a special moment in the history
of the Universe as it is during this era that the first galaxies and
star clusters are formed
Reionization also profoundly affects the
environment where subsequent generations of galaxies evolve
Our
overarching goal is to test the hypothesis that galaxies are
responsible for reionizing neutral hydrogen
To do so we propose to
carry out a pure parallel WFC3 survey to constrain the bright end of
the redshift z>7
5 galaxy luminosity function on a total area of 176
arcmin^2 of sky
Extrapolating the evolution of the luminosity
function from z~6, we expect to detect about 20 Lyman Break Galaxies
brighter than M_* at z~8 significantly improving the current sample of
only a few galaxies known at these redshifts
Finding significantly
fewer objects than predicted on the basis of extrapolation from z=6
would set strong limits to the brightness of M_*, highlighting a fast
evolution of the luminosity function with the possible implication
that galaxies alone cannot reionize the Universe
Our observations
will find the best candidates for spectroscopic confirmation, that is
bright z>7
5 objects, which would be missed by small area deeper
surveys
The random pointing nature of the program is ideal to beat
cosmic variance, especially severe for luminous massive galaxies,
which are strongly clustered
In fact our survey geometry of 38
independent fields will constrain the luminosity function like a
contiguous single field survey with two times more area at the same
depth
Lyman Break Galaxies at z>7
5 down to m_AB=26
85 (5 sigma) in
F125W will be selected as F098M dropouts, using three to five orbits
visits that include a total of four filters (F606W, F098M, F125W,
F160W) optimized to remove low-redshift interlopers and cool stars
Our data will be highly complementary to a deep field search for
high-z galaxies aimed at probing the faint end of the luminosity
function, allowing us to disentangle the degeneracy between faint end
slope and M_* in a Schechter function fit of the luminosity function
We waive proprietary rights for the data
In addition, we commit to
release the coordinates and properties of our z>7
5 candidates within
one month from the acquisition of each field
WFC3/IR 11909 UVIS Hot Pixel Anneal The on-orbit radiation environment of WFC3 will continually generate
new hot pixels
This proposal performs the procedure required for
repairing those hot pixels in the UVIS CCDs
During an anneal, the
two-stage thermo-electric cooler (TEC) is turned off and the
four-stage TEC is used as a heater to bring the UVIS CCDs up to ~20C
As a result of the CCD warmup, a majority of the hot pixels will be
fixed; previous instruments such as WFPC2 and ACS have seen repair
rates of about 80%
Internal UVIS exposures are taken before and after
each anneal, to allow an assessment of the procedure's effectiveness
in WFC3, provide a check of bias, global dark current, and hot pixel
levels, as well as support hysteresis (bowtie) monitoring and CDBS
reference file generation
One IR dark is taken after each anneal, to
provide a check of the IR detector
WFC3/UVI 11903 UVIS Photometric Zero Points This proposal obtains the photometric zero points in 53 of the 62
UVIS/WFC3 filters: the 18 broad-band filters, 8 medium-band filters,
16 narrow-band filters, and 11 of the 20 quad filters (those being
used in cycle 17)
The observations will be primary obtained by
observing the hot DA white dwarf standards GD153 and G191-B2B
A
redder secondary standard, P330E, will be observed in a subset of the
filters to provide color corrections
Repeat observations in 16 of the
most widely used cycle 17 filters will be obtained once per month for
the first three months, and then once every second month for the
duration of cycle 17, alternating and depending on target
availability
These observations will enable monitoring of the
stability of the photometric system
Photometric transformation
equations will be calculated by comparing the photometry of stars in
two globular clusters, 47 Tuc and NGC 2419, to previous measurements
with other telescopes/instruments
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 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/UV/COS/FUV/WFC 11536 COS-GTO: Sleuthing the Source of Distant Cometary Activity Distant comets and Centaurs often show cometary activity and outbursts
well beyond 3 AU, the boundary of the sublimation zone of water
Super-volatiles (most likely CO, but possibly CH4, N2, or S2) are
suspected to be responsible, but have never been detected in distant
comets in the UV
We will obtain FUV spectra of active bodies to cover
important CO emission bands
We plan two sets of observations: comet
29P/Schwassmann-Wachmann at 6 AU, whose outbursts are too short to
capture as a Target of Opportunity, but which also shows persistent
cometary activity in quiescence; and Target of Opportunity
observations of the Centaur 2060 Chiron (at ~15
5 AU) in outburst
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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)
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