HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science



DAILY REPORT #5135



PERIOD COVERED: 5am July 9 - 5am July 12, 2010 (DOY 190/09:00z-193/09:00z)



FLIGHT OPERATIONS SUMMARY:



Significant Spacecraft Anomalies: (The following are preliminary reports

of potential non-nominal performance that will be investigated.)



HSTARS:

12325 - GSAcq(2,1,1) at 190/17:54:12z resulted in Fine lock Backup on FGS2.

The subsequent REAcqs at 190/19:29:27z and 190/21:05:20z also resulted in

fine lock backup on FGS2.



Observations possibly affected COS 98-109 Proposal ID# 11598;

WFC3 135 Proposal ID# 11908





12326 - GSAcq(1,2,1) at 191/01:33:56z resulted in fine lock backup on

FGS2 after scan step limit exceeded on FGS2. The subsequent REAcq at

191/02:52:29z also resulted in fine lock backup on FGS2.



Observations possibly affected: STIS 36, 37 Proposal ID# 11845;

STIS 38-40 Proposal ID# 11847; WFC3 140-142 Proposal ID# 11661





COMPLETED OPS REQUEST:

18871-0 - Execute ROP NS-12 to Reset STIS FSW Error Count @ 190/1450z

17543-3 - Dump OBAD Tables After Failed OBAD @ 191/2048z, 191/2049z

18870-1 - Eclipse Management for 192/18:26 Eclipse (July 11) @ 192/2141z





COMPLETED OPS NOTES: (None)



SCHEDULED SUCCESSFUL

FGS GSAcq 20 20

FGS REAcq 23 23

OBAD with Maneuver 16 16



SIGNIFICANT EVENTS:



Lunar Solar Eclipse 2010/192



OPS Request 18870 was successfully executed to configure the FSW

processing of CSS data and temporarily disable Rate of Charge (ROC)

safemode test during the moon shadow that occurred from 192/18:16z to

18:54z.



During the eclipse period, the minimum FSW SOC was approximately 438

A-hr, the maximum 482 A-hr and the FSW Benchmark was not reset. However,

the batteries were charged nominally on the following orbit and

benchmark reset was achieved.





OBSERVATIONS SCHEDULED:



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.



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.



WFC3/IR 11931



IR Signal Non-Linearity Calibration



These observations will be used to quantify the non-linear signal

behavior of the IR channel, as well as to create the IR channel

non-linearity calibration reference file. The non-linearity behavior of

each pixel in the detector will be investigated through the use of flat

fields, while the photometric behavior of point sources will be studied

using observations of 47 Tuc.



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/UV 11923



UVIS Filter Wedge Check



The position of each UVIS filter will be checked to verify that the

filters meet the CEI (Contract End Item) specification for image

displacement. We will observe NGC 1850 with all full-frame UVIS filters

using a subarray (UVIS1-C512A) without moving the telescope, as well as

the quad filters with a 512x512 specifically designed subarray. We will

also acquire one grism exposure. The relative displacement of the stars

in each image will be measured from one filter to the next.



WFC3/UV 11918



WFC3 UVIS Image Quality



The UVIS imaging performance over the detector will be assessed

periodically (every 4 months) in two passbands (F275W and F621M) to

check for image stability. The field around star 58 in the open cluster

NGC188 is the chosen target because it is sufficiently dense to provide

good sampling over the FOV while providing enough isolated stars to

permit accurate PSF (point spread function) measurement. It is available

year-round and used previously for ACS image quality assessment. The

field is astrometric, and astrometric guide stars will be used, so that

the plate scale and image orientation may also be determined if

necessary (as in SMOV proposals 11436 and 11442). Full frame images will

be obtained at each of 4 POSTARG offset positions designed to improve

sampling over the detector.



This proposal is a periodic repeat (once every 4 months) of visits

similar to those in SMOV proposal 11436 (activity ID WFC3-23). The data

will be analyzed using the code and techniques described in ISR WFC3

2008-40 (Hartig). Profiles of encircled energy will be monitored and

presented in an ISR. If an update to the SIAF is needed, (V2, V3)

locations of stars will be obtained from the Flight Ops Sensors and

Calibrations group at GSFC, the (V2, V3) of the reference pixel and the

orientation of the detector will be determined by the WFC3 group, and

the Telescopes group will update and deliver the SIAF to the PRDB

branch.



The specific PSF metrics to be examined are encircled energy for

aperture diameter 0.15, 0.20, 0.25, and 0.35 arcsec, FWHM, and

sharpness. (See ISR WFC3 2008-40 tables 2 and 3 and preceding text.)

about 20 stars distributed over the detector will be measured in each

exposure for each filter. The mean, rms, and rms of the mean will be

determined for each metric. The values determined from each of the 4

exposures per filter within a visit will be compared to each other to

see to what extent they are affected by "breathing". Values will be

compared from visit to visit, starting with the values obtained during

SMOV after the fine alignment has been performed, to see if the measures

of the compactness of the PSF indicate degradation over time. The

analysis will be repeated for stars on the inner part of the detector

and stars on the outer part of the detector to check for differential

degradation of the PSF.



As an example of the analysis, one can examine the sharpness of the

F275W PSF exposures made during thermal vacuum testing (ISR WFC3

2008-40). To compare two samples, one can define the PSFs on each CCD

chip as a sample of 8. The mean, rms, and rms of the mean sharpness are

0.0676, 0.0093, and 0.0035 for one chip, and 0.0701, 0.0085, and 0.0032

for the other. The difference of the means is 0.0025 and the statistical

error in that difference is 0.0048, so the difference is not

significant.



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 11905



WFC3 UVIS CCD Daily Monitor



The behavior of the WFC3 UVIS CCD will be monitored daily with a set of

full-frame, four-amp bias and dark frames. A smaller set of 2Kx4K

subarray biases are acquired at less frequent intervals throughout the

cycle to support subarray science observations. The internals from this

proposal, along with those from the anneal procedure (Proposal 11909),

will be used to generate the necessary superbias and superdark reference

files for the calibration pipeline (CDBS).



ACS/WFC3 11882



CCD Hot Pixel Annealing



This program continues the monthly anneal that has taken place every

four weeks for the last three cycles. We now obtain WFC biases and darks

before and after the anneal in the same sequence as is done for the ACS

daily monitor (now done 4 times per week). So the anneal observation

supplements the monitor observation sets during the appropriate week.

Extended Pixel Edge Response (EPER) and First Pixel Response (FPR) data

will be obtained over a range of signal levels for the Wide Field

Channel (WFC). This program emulates the ACS pre-flight ground

calibration and post-launch SMOV testing (program 8948), so that results

from each epoch can be directly compared. The High Resolution Channel

(HRC) visits have been removed since it could not be repaired during

SM4.



This program also assesses the read noise, bias structure, and amplifier

cross-talk of ACS/WFC using the GAIN=1.4 A/D conversion setting. This

investigation serves as a precursor to a more comprehensive study of WFC

performance using GAIN=1.4.



STIS/CC 11847



CCD Bias Monitor-Part 2



Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,

and 1x1 at gain = 4, to build up high-S/N superbiases and track the

evolution of hot columns.



STIS/CC 11845



CCD Dark Monitor Part 2



Monitor the darks for the STIS CCD.



ACS/WFC 11831



Probing X-Ray Jet Emission Mechanisms in a Complete Blazar Sample



We propose deep (70 ksec) followup Chandra X-ray observations and new

HST ACS/WFC/F475W observations of two quasars, viz., 0106+013 and

1641+399, belonging to the complete flux-limited MOJAVE Chandra blazar

sample. These two quasars have HST WFPC2/F702W data available in the

archive. Combining the existing optical and radio data with the new

Chandra and HST data at an additional optical band we aim to construct a

significantly more accurate multi-waveband (four frequency) spectral

energy distributions for distinct knots in the jets. This will serve as

a first step towards resolving longstanding ambiguities surrounding the

primary X-ray emission mechanisms in a well-defined sample of powerful

FR-II class jets.



COS/NUV/FUV 11727



UV Spectroscopy of Local Lyman Break Galaxy Analogs: New Clues to Galaxy

Formation in the Early Universe



Much of our information about galaxy evolution and the interaction

between galaxies and the IGM at high-z has been provided by the Lyman

Break Galaxies (LBGs). However, it is difficult to investigate these

faint and distant objects in detail. To address this, we have used the

GALEX All-Sky Imaging Survey and the SDSS to identify for the first time

a rare population of low- redshift galaxies with properties remarkably

similar to the high-redshift LBGs. These local "Lyman Break Analogs"

(LBAs) resemble LBGs in terms of morphology, size, UV luminosity, star

formation rate, UV surface brightness, stellar mass, velocity

dispersion, metallicity, and dust content. We are assembling a wide

range of data on these objects with the goal of using them as local

laboratories for better understanding the relevant astrophysical

processes in LBGs. These data include HST imaging (95 orbits in Cy15 and

16), Spitzer photometry and spectroscopy, Chandra and XMM X-ray imaging

and spectroscopy, and near-IR integral field spectroscopy (VLT, Keck,

and Gemini). In this proposal we are requesting the most important

missing puzzle piece: far-UV spectra with a signal-to-noise and spectral

resolution significantly better than available for typical LBGs. We will

use these spectra to study the LBA's galactic winds, probe the processes

that regulate the escape of Ly-a and Lyman continuum radiation,

determine chemical abundances for the stars and gas, and constrain the

form of the high-end of the Initial Mass Function. Adding these new COS

data will give us vital information about these extraordinary sites of

star formation in the local universe. In so-doing it will also shed new

light on the processes that led to the formation of stars, the building

of galaxies, and the enrichment and heating of the IGM in the early

universe.



WFC3/UVIS 11697



Proper Motion Survey of Classical and SDSS Local Group Dwarf Galaxies



Using the superior resolution of HST, we propose to continue our proper

motion survey of Galactic dwarf galaxies. The target galaxies include

one classical dwarf, Leo II, and six that were recently identified in

the Sloan Digital Sky Survey data: Bootes I, Canes Venatici I, Canes

Venatici II, Coma Berenices, Leo IV, and Ursa Major II. We will observe

a total of 16 fields, each centered on a spectroscopically-confirmed

QSO. Using QSOs as standards of rest in measuring absolute proper

motions has proven to be the most accurate and most efficient method.

HST is our only option to quickly determine the space motions of the

SDSS dwarfs because suitable ground-based imaging is only a few years

old and such data need several decades to produce a proper motion. The

two most distant galaxies in our sample will require time baselines of

four years to achieve our goal of a 30-50 km/s uncertainty in the

tangential velocity; given this and the finite lifetime of HST, it is

imperative that first-epoch observations be taken in this cycle. The

SDSS dwarfs have dramatically lower surface brightnesses and

luminosities than the classical dwarfs. Proper motions are crucial for

determining orbits of the galaxies and knowing the orbits will allow us

to test theories for the formation and evolution of these galaxies and,

more generally, for the formation of the Local Group.



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<z<1.8 to measure the evolution of the extinction-corrected

star formation density across the peak epoch of star formation. This is

over an order-of-magnitude improvement in the current statistics, from

the NICMOS Parallel grism survey. (5) Trace ``cosmic downsizing" from

0.5<z<2.2; and (6) Estimate the evolution in reddening and metallicty in

star- forming galaxies and measure the evolution of the Seyfert

population. For hundreds of spectra we will be able to measure one or

even two line pair ratios -- in particular, the Balmer decrement and

[OII]/[OIII] are sensitive to gas reddening and metallicity. As a bonus,

the G102 grism offers the possibility of detecting Lya emission at

z=7-8.8.



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/ACS/UVIS 11684



The First Proper Motion Measurement for M31: Dynamics and Mass of the

Local Group



We will perform observations to determine the proper motion of the

Andromeda galaxy M31, which has been sought for almost a century without

success. While challenging, this measurement has now become possible due

to the availability of existing deep ACS/WFC images of several M31

fields. The requested second epoch images will yield the average shift

of the M31 stars with respect to compact galaxies in the background. Our

observing strategy uses six different fields (three primary and three

coordinated parallel) with two different instruments (ACS and WFC3) to

provide a maximum handle on possible systematic effects. The expected

result will be sufficiently accurate to: (a) discriminate between

different histories for the dynamics of the Local Group; (b) constrain

the mass distribution of the Local Group; (c) determine the details of

the expected future merger between M31 and the Milky Way; (d) infer the

past interaction history between M31 and M33; (e) constrain the internal

proper motion kinematics of the M31 spheroid, outer disk, and tidal

stream; and (f) obtain a pilot estimate of the M31 distance through the

method of rotational parallax.



WFC3/UVI 11680



The Main Sequence Luminosity Function of Low-Mass Globular Clusters



Theoretical work indicates that the dynamical evolution of globular

clusters of low mass and low central concentration is strongly

determined by mass-loss processes, such as stellar evaporation and tidal

stripping, that can eventually lead to cluster dissolution. In fact,

mass loss and cluster disruption is now considered to be a viable

explanation for the form of the faint end of the Milky Way globular

cluster luminosity function. A clear observational demonstration of the

prevalence of cluster mass-loss would have ramifications not only for

the dynamical evolution of individual globular clusters and their

internal stellar mass distributions, but also for the relationships

between halo field and cluster stars and the properties of globular

cluster systems in galaxies. Our previous WFPC2 imaging of the low-mass

diffuse halo cluster Palomar 5 revealed a main sequence deficient in

stars compared to other low-concentration globular clusters of much

higher mass, consistent with there having been a considerable loss of

stars from this system. But is Pal 5 typical of low-mass,

low-concentration halo clusters? We propose to place the mass-loss

scenario on a firm observational footing (or otherwise) by using WFC3

imaging to measure the main-sequence stellar mass functions of two of

the lowest-mass lowest-concentration globular clusters in the Milky Way,

AM-4 and Palomar 13, in order to search for analogous evidence of

stellar depletion.



WFC3/UVIS 11661



The Black Hole Mass - Bulge Luminosity Relationship for the Nearest

Reverberation-Mapped AGNs



We propose to obtain WFC3 host galaxy images of the eight nearest AGNs

with masses from reverberation mapping, and one star as a PSF model.

These images will allow us to determine with unprecedented accuracy the

bulge luminosities of the host galaxies, a goal which is not achievable

from the ground due to the blurring of the very bright PSF component

under typical, and even very good, seeing conditions. High-resolution

ACS images of the host galaxies of more luminous AGNs reveal that the

black hole mass-bulge luminosity and black hole mass-bulge mass

relationships for AGNs are not well constrained and arise from what

appear to be fundamentally flawed data sets. With the addition of the

images proposed here to our current sample of ACS images, we will be

able to extend our determinations of the black hole mass- bulge

luminosity and black hole mass-bulge mass relationships for AGNs by an

order of magnitude and test our preliminary results for these

fundamentally important relationships against those previously

determined for quiescent galaxies.



COS/NUV/ACS/WFC/FUV 11658



Probing the Outer Regions of M31 with QSO Absorption Lines



We propose HST-COS spectroscopy of 10 quasars behind M31. Absorption

lines due to MgII, FeII, CIV, and a variety of other lines will be

searched for and measured. Six quasars lie between 1 and 4.2 Holmberg

radii near the major axis on the southwest side, where confusion with

Milky Way gas is minimized. Two lie even farther out on the southwest

side of the major axis. One lies within 1 Holmberg radius. Two of the 10

pass through M31's high velocity clouds seen in a detailed 21 cm

emission map. Exposure time estimates were based on SDSS magnitudes and

available GALEX magnitudes. Thus, using the most well-studied external

spiral galaxy in the sky, our observations will permit us to check,

better than ever before, the standard picture that quasar metal-line

absorption systems such as MgII and CIV arise in an extended gaseous

halo/disk of a galaxy well beyond its observable optical radius. The

observations will yield insights into the nature of the gas and its

connection to the very extended stellar components of M31 that have

recently been studied. Notably the observations have the potential of

extending M31's rotation curve to very large galactocentric distances,

thereby placing new constrants on M31's dark matter halo.



Finally, we also request that the coordinated parallel orbits be

allocated to this program so that we may image the resolved stellar

content of M31's halo and outer disk.



WFC3/IR 11648



WFC3 Spectroscopy of an X-ray Luminous Galaxy Cluster at z>2



We propose to obtain deep WFC3+G141 grism observations to

spectroscopically confirm a remarkable z>2 cluster of galaxy candidate.

Over a 1000 arcmin^2 field imaged with Spitzer's IRAC we have discovered

a compact (<30�� diameter) concentration of extremely red galaxies with

a factor of >40 overdensity over the adjacent field. Among these

galaxies for which we can derive meaningful photometric redshifts, 17

are consistent with zphot=2-2.5, making it very likely that the

concentration is a real cluster at such high redshift. This is further

supported by a 3.5 sigma detection of extended X-Ray emission on

XMM-Newton data, by a likely color magnitude sequence of red galaxies,

and by the presence of a giant galaxy consistent with a BCG at the

cluster redshift. The general faintness of the red galaxies in all

optical bands and their high redshifts prevent confirmation of this

cluster with ordinary optical spectroscopy. The WFC3 camera with G141

grism provides the only way to confirm this record high-z cluster and

measure its redshift from spectral breaks typical of old stellar

populations. Our deep integrations will reveal redshifts for at least 19

ultra-red galaxies in the area and of a similar number of bluer galaxies

at the cluster redshift. Knowledge of the cluster redshift based on the

HST spectra will allow us to reach important scientific aims: find the

most distant Xray emitting evolved galaxy cluster, determine membership

of the other galaxies from photometric SED analysis, study their stellar

population properties, characterize the color-magnitude relation with

constraints on the formation redshift. The proposed observations will

establish a first z>2 benchmark for cluster field comparisons of galaxy

formation at this highest redshift and will firmly establish the

progenitors of local rich Abell clusters.



STIS/CC 11626



Searching for the Upper Mass Limit in NGC 3603, the Nearest Giant H II

Region



What is the mass of the highest mass star? 100Mo? 150Mo? 200Mo? Or

higher? Theory gives us little guidance as to what physics sets the

upper mass limit, presuming one exists. Is it due to limitations in the

highest masses that can coalesce? Or is it due to stability issues in

such a behemoth? Observationally, the upper mass limit is poorly

constrained at present, with the strongest evidence coming from the

K-band luminosity function of the Arches cluster near the Galactic

Center. Here we propose to investigate this question by determining the

Initial Mass Function of NGC 3603, the nearest giant H II region. This

cluster is known to contain a wealth of O3 and hydrogen-rich

Wolf-Rayets, the most luminous and massive of stars. By constructing an

accurate H-R diagram for the cluster, we will construct a present day

mass function using newly computed high mass evolutionary tracks, and

convert this to an initial mass function using the inferred ages. This

will allow us to see whether or not there is a true deficit of high mass

stars, evidence of an upper mass cutoff. At the same time we are likely

to establish good masses for the highest mass stars ever determined. We

have laid the groundwork for this project using the Magellan 6.5-m

telescope and the excellent seeing found on Las Campanas, plus analysis

of archival ACS/HRS frames, but we now need to obtain spectra of the

stars unobservable from the ground. This can only be done with HST and a

reburbished STIS.



COS/NUV/FUV 11598



How Galaxies Acquire their Gas: A Map of Multiphase Accretion and

Feedback in Gaseous Galaxy Halos



We propose to address two of the biggest open questions in galaxy

formation - how galaxies acquire their gas and how they return it to the

IGM - with a concentrated COS survey of diffuse multiphase gas in the

halos of SDSS galaxies at z = 0.15 - 0.35. Our chief science goal is to

establish a basic set of observational facts about the physical state,

metallicity, and kinematics of halo gas, including the sky covering

fraction of hot and cold material, the metallicity of infall and

outflow, and correlations with galaxy stellar mass, type, and color -

all as a function of impact parameter from 10 - 150 kpc. Theory suggests

that the bimodality of galaxy colors, the shape of the luminosity

function, and the mass-metallicity relation are all influenced at a

fundamental level by accretion and feedback, yet these gas processes are

poorly understood and cannot be predicted robustly from first

principles. We lack even a basic observational assessment of the

multiphase gaseous content of galaxy halos on 100 kpc scales, and we do

not know how these processes vary with galaxy properties. This ignorance

is presently one of the key impediments to understanding galaxy

formation in general. We propose to use the high-resolution gratings

G130M and G160M on the Cosmic Origins Spectrograph to obtain sensitive

column density measurements of a comprehensive suite of multiphase ions

in the spectra of 43 z < 1 QSOs lying behind 43 galaxies selected from

the Sloan Digital Sky Survey. In aggregate, these sightlines will

constitute a statistically sound map of the physical state and

metallicity of gaseous halos, and subsets of the data with cuts on

galaxy mass, color, and SFR will seek out predicted variations of gas

properties with galaxy properties. Our interpretation of these data will

be aided by state-of-the-art hydrodynamic simulations of accretion and

feedback, in turn providing information to refine and test such models.

We will also use Keck, MMT, and Magellan (as needed) to obtain optical

spectra of the QSOs to measure cold gas with Mg II, and optical spectra

of the galaxies to measure SFRs and to look for outflows. In addition to

our other science goals, these observations will help place the Milky

Way's population of multiphase, accreting High Velocity Clouds (HVCs)

into a global context by identifying analogous structures around other

galaxies. Our program is designed to make optimal use of the unique

capabilities of COS to address our science goals and also generate a

rich dataset of other absorption-line systems.



WFC3/UVIS 11594



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



We propose to conduct a spectroscopic survey of Lyman limit absorbers at

redshifts 1.8 < z < 2.5, using WFC3 and the G280 grism. This proposal

intends to complete an approved Cycle 15 SNAP program (10878), which was

cut short due to the ACS failure. We have selected 64 quasars at 2.3 < z

< 2.6 from the Sloan Digital Sky Survey Spectroscopic Quasar Sample, for

which no BAL signature is found at the QSO redshift and no strong metal

absorption lines are present at z > 2.3 along the lines of sight. The

survey has three main observational goals. First, we will determine the

redshift frequency dn/dz of the LLS over the column density range 16.0 <

log(NHI) < 20.3 cm^-2. Second, we will measure the column density

frequency distribution f(N) for the partial Lyman limit systems (PLLS)

over the column density range 16.0 < log(NHI) < 17.5 cm^-2. Third, we

will identify those sightlines which could provide a measurement of the

primordial D/H ratio. By carrying out this survey, we can also help

place meaningful constraints on two key quantities of cosmological

relevance. First, we will estimate the amount of metals in the LLS using

the f(N), and ground based observations of metal line transitions.

Second, by determining f(N) of the PLLS, we can constrain the amplitude

of the ionizing UV background at z~2 to a greater precision. This survey

is ideal for a snapshot observing program, because the on-object

integration times are all well below 30 minutes, and follow-up

observations from the ground require minimal telescope time due to the

QSO sample being bright.



COS/FUV/STIS/CCD/MA1 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<d<21 kpc, 3<|z|<13 kpc). COS

will provide atomic to highly ionized species (e.g.,OI, CII, CIV, SiIV)

that can be observed at sufficient resolution (R~22, 000) to not only

detect these highly ionized HVCs but also to model their properties and

understand their physics and origins. This survey is only possible

because of the high sensitivity of COS in the FUV spectral range.



WFC3/UVIS 11588



Galaxy-Scale Strong Lenses from the CFHTLS Survey



We aim to investigate the origin and evolution of early-type galaxies

using gravitational lensing, modeling the mass profiles of objects over

a wide range of redshifts. The low redshift (z = 0.2) sample is already

in place following the successful HST SLACS survey; we now propose to

build up and analyze a sample of comparable size (~50 systems) at high

redshift (0.4 < z < 0.9) using HST WFC3 Snapshot observations of lens

systems identified by the SL2S collaboration in the CFHT legacy survey.



WFC3/UVI/IR 11557



The Nature of Low-Ionization BAL QSOs



The rare subclass of optically-selected QSOs known as low-ionization

broad absorption line (LoBAL) QSOs show signs of high-velocity gas

outflows and reddened continua indicative of dust obscuration. Recent

studies show that galaxies hosting LoBAL QSOs tend to be ultraluminous

infrared systems that are undergoing mergers, and that have dominant

young (< 100 Myr) stellar populations. Such studies support the idea

that LoBAL QSOs represent a short- lived phase early in the life of

QSOs, when powerful AGN-driven winds are blowing away the dust and gas

surrounding the QSO. If so, understanding LoBALs would be critical in

the study of phenomena regulating black hole and galaxy evolution, such

as AGN feedback and the early stages of nuclear accretion. These

results, however, come from very small samples that may have serious

selection biases. We are therefore taking a more aggressive approach by

conducting a systematic multiwavelength study of a volume limited sample

of LoBAL QSOs at 0.5 < z < 0.6 drawn from SDSS. We propose to image

their host galaxies in two bands using WFC3/UVIS and WFC3/IR to study

the morphologies for signs of recent tidal interactions and to map their

interaction and star forming histories. We will thus determine whether

LoBAL QSOs are truly exclusively found in young merging systems that are

likely to be in the early stages of nuclear accretion.



NIC2/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 flavor. 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 behavior in a substantially larger sample; ii) extend

the comparison between radio-loud and radio-quiet AGN to a larger range

of luminosities.



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 understand 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 separately and probe the

mass structure of early-type galaxies from 0.1 to 100 effective radii.

The large dynamic range to which lensing is sensitive 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

WFC3 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!



NIC3/WFC3/IR 11149



Characterizing the Stellar Populations in Lyman-Alpha Emitters and Lyman

Break Galaxies at 5.7<z<7 in the Subaru Deep Field



The epoch of reionization marks a major phase transition of the

Universe, during which the intergalactic space became transparent to UV

photons. Determining when this occurred and the physical processes

involved represents the latest frontier in observational cosmology. Over

the last few years, searches have intensified to identify the population

of high-redshift (z>6) galaxies that might be responsible for this

process, but the progress is hampered partly by the difficulty of

obtaining physical information (stellar mass, age, star formation

rate/history) for individual sources. This is because the number of z>6

galaxies that have both secure spectroscopic redshifts and high-quality

infrared photometry (especially with Spitzer/IRAC) is still fairly

small. Considering that only several photometric points are available

per source, and that many model SEDs are highly degenerate, it is

crucial to obtain as many observational constraints as possible for each

source to ensure the validity of SED modeling. To better understand the

physical properties of high-redshift galaxies, we propose here to

conduct HST/NICMOS (72 orbits) and Spitzer/IRAC (102 hours) imaging of

spectroscopically confirmed, bright (z<26 mag (AB)) Ly-alpha emitters

(LAEs) and Lyman-break galaxies (LBGs) at 5.7<z<7 selected from the

Subaru Deep Field. Spectroscopic redshifts remove one critical free

parameter from SED modeling while bright source magnitudes ensure

high-quality photometric data. By making accurate determinations of

stellar masses, ages, and star-formation histories, we will specifically

address the following major questions: (1) Do LAEs and LBGs represent

physically different galaxy populations at z>6 as suggested recently?

(2) Is Ly-alpha emission systematically suppressed at z>6 with respect

to continuum emission? (i.e., are we reaching the epoch of incomplete

reionization?), and (3) Do we see any sign of abnormally young stellar

population in any of the z>6 galaxies?