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HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5203

PERIOD COVERED: 8:00pm October 11 - 7:59pm October 12, 2010 (DOY 285/00:00z-285/23:59z)

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS:

12464 - GSAcq(1,2,1) scheduled at 285/06:52:14z resulted in fine lock

           backup (2,0,2) using FGS-2 due to scan step limit exceeded.

           Observations possibly affected: ACS 39 Proposal ID#12210, WFC3 35 Proposal ID#11905

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                       SCHEDULED       SUCCESSFUL

FGS GSAcq                 10                 10

FGS REAcq                 05                05

OBAD with Maneuver   08                08

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 12210

SLACS for the Masses: Extending Strong Lensing to Lower Masses and

Smaller Radii

Strong gravitational lensing provides the most accurate possible

measurement of mass in the central regions of early-type galaxies

(ETGs). We propose to continue the highly productive Sloan Lens ACS

(SLACS) Survey for strong gravitational lens galaxies by observing a

substantial fraction of 135 new ETG gravitational-lens candidates with

HST-ACS WFC F814W Snapshot imaging. The proposed target sample has been

selected from the seventh and final data release of the Sloan Digital

Sky Survey, and is designed to complement the distribution of previously

confirmed SLACS lenses in lens-galaxy mass and in the ratio of Einstein

radius to optical half-light radius. The observations we propose will

lead to a combined SLACS sample covering nearly two decades in mass,

with dense mapping of enclosed mass as a function of radius out to the

half-light radius and beyond. With this longer mass baseline, we will

extend our lensing and dynamical analysis of the mass structure and

scaling relations of ETGs to galaxies of significantly lower mass, and

directly test for a transition in structural and dark-matter content

trends at intermediate galaxy mass. The broader mass coverage will also

enable us to make a direct connection to the structure of well-studied

nearby ETGs as deduced from dynamical modeling of their line-of-sight

velocity distribution fields. Finally, the combined sample will allow a

more conclusive test of the current SLACS result that the intrinsic

scatter in ETG mass-density structure is not significantly correlated

with any other galaxy observables. The final SLACS sample at the

conclusion of this program will comprise approximately 130 lenses with

known foreground and background redshifts, and is likely to be the

largest confirmed sample of strong-lens galaxies for many years to come.

COS/FUV 12212

What are the Locations and Kinematics of Mass Outflows in AGN?

Mass outflows of ionized gas in AGN, first revealed through blueshifted

UV and X-ray absorption lines, are likely important feedback mechanisms

for the enrichment of the IGM, self-regulation of black-hole growth, and

formation of structure in the early Universe. To understand the origin,

dynamics, and impact of the outflowing absorbers on their surroundings,

we need to know their locations (radial positions and polar angles with

respect to the AGN rotation axes) and kinematics (radial and transverse

velocities). We will use COS high-resolution spectra of 11 Seyfert 1

galaxies to derive velocity-dependent covering factors, ionic column

densities, number densities (via metastable lines or variability), and

ionization parameters (via photoionization models) of the UV absorbers,

and thereby determine their radial locations as we have done for NGC

4151. We will use absorption variability over time scales of up to ~20

years, to determine transverse velocities and detect changes in radial

velocities. We will use STIS G430M long-slit spectra and WFC3 [OIII]

images to resolve the kinematics of the narrow-line region (NLR) and

determine the inclinations of the AGN, to investigate the connection

between nuclear absorption and NLR emission outflows and their

dependence on polar angle.

COS/NUV/FUV 11742

Probing HeII Reionization with GALEX-selected Quasar Sightlines and

HST/COS

We propose spectroscopic observations with COS of eight z~3 QSOs that we

found to be bright in the far ultraviolet. Our aim is to study

intergalactic absorption caused by the onset of the He II Lyman forest.

Several lines of evidence suggest that helium reionization occurred at

z~3. Understanding this process is critical for a complete picture of

the intergalactic medium and its evolution; it also gives clues to

hydrogen reionization at z>6. The only direct means of assessing He II

reionization is through far-UV observations of the He II Lyman alpha

forest. Only 6 sightlines are known to date where this is feasible,

despite extensive surveys. Our program is designed to double the number

of available sightlines. To this effect, we cross- correlated all known

z>2.73 quasars with UV source lists from the GALEX satellite. The

selected quasars were all significantly detected in the far UV by GALEX,

and their UV colors are similar to those of already known quasars with

transparent sightlines. Spectra obtained with COS will allow us to

compile the first comprehensive sample of He II absorption spectra

probing similar redshifts, enabling a systematic investigation of the He

II reionization epoch and the spectral shape of the UV background.

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/IR 12224

Measuring the Stellar Populations of Individual Lyman Alpha Emitters

During the Epoch of Peak Star Formation

Selecting galaxies by their strong Lyman-alpha emission provides a

powerful means of probing the reionization epoch and the faint/low-mass

galaxies that dominate star formation at high redshift. Yet, our

understanding of high-redshift Lyman-alpha emitters (LAEs) has lagged

behind that of other well-studied populations (e.g., Lyman break

galaxies) due to their continuum faintness and the shifting of

age/mass-sensitive features into the near-IR where the high terrestrial

background inhibits deep observations. All existing studies of LAEs at

z>2 have used stacked optical and/or Spitzer infrared data to discern

their median properties, but the actual distributions of ages,

reddenings, and stellar masses for these populations are poorly

characterized. To fill this glaring gap in the observations and advance

our understanding of this important population, we propose WFC3/IR+F160W

imaging of fields where we have conducted a survey of low redshift

(z~1.9) Lyman-alpha emitters (LAEs), in order to measure their ages and

stellar masses at an epoch where such observations directly probe the

age-sensitive Balmer/4000 AA breaks. The targeted sample will include

45-50 spectroscopically confirmed LAEs at z=1.7-2.1 and roughly twice as

many candidates, making it the largest sample of homogeneously selected

LAEs with individual measurements of the ages, masses, and dust

extinction. With these data we will (1) carefully take into account the

age-dependence of the extinction curve to make robust comparisons

between LAEs and continuum-selected galaxies at the same redshifts; (2)

combine clustering and stellar mass measurements to infer the duty

cycles of LAEs and determine if they are triggered in the presence of

large-scale structures; and (3) quantify the importance of the LAE phase

at different galaxy luminosity and mass scales, over a large dynamic

range in these properties. An economical investment of just 12 orbits

will allow us to accomplish these goals, and remains the only hope of

efficiently studying such low luminosity high-redshift galaxies in the

near-IR prior to the JWST-era.

WFC3/IR 12286

Hubble Infrared Pure Parallel Imaging Extragalactic Survey (HIPPIES)

WFC3 has demonstrated its unprecedented power in probing the early

universe. Here we propose to continue our pure parallel program with

this instrument to search for LBGs at z~6--8. Our program, dubbed as the

Hubble Infrared Pure Parallel Imaging Extragalactic Survey ("HIPPIES"),

will carry on the HST pure parallel legacy in the new decade. We request

205 orbits in Cycle-18, which will spread over ~ 50 high Galactic

latitude visits (|b|>20deg) that last for 3 orbits and longer, resulting

a total survey area of ~230 square arcmin. Combining the WFC3 pure

parallel observations in Cycle-17, HIPPIES will complement other

existing and forthcoming WFC3 surveys, and will make unique

contributions to the study in the new redshift frontier because of the

randomness of the survey fields. To make full use of the parallel

opportunities, HIPPIES will also take ACS parallels to study LBGs at

z~5--6. Being a pure parallel program, HIPPIES will only make very

limited demand on the scarce HST resources, but will have potentially

large scientific returns. As in previous cycle, we waive all proprietary

data rights, and will make the enhanced data products public in a timely

manner.

(1) The WFC3 part of HIPPIES aims at the most luminous LBG population at

z~8 and z~7. As its survey fields are random and completely

uncorrelated, the number counts of the bright LBGs from HIPPIES will be

least affected by the "cosmic variance", and hence we will be able to

obtain the best constraint on the bright-end of the LBG luminosity

function at z~8 and 7. Comparing the result from HIPPIES to the

hydrodynamic simulations will test the input physics and provide insight

into the nature of the early galaxies. (2) The z~7--8 candidates from

HIPPIES, most of which will be the brightest ones that any surveys would

be able to find, will have the best chance to be spectroscopically

confirmed at the current 8--10m telescopes. (3) The ACS part of HIPPIES

will produce a significant number of candidate LBGs at z~5 and z~6 per

ACS field. Combining with the existing, suitable ACS fields in the HST

archive, we will be able to utilize the random nature of the survey to

quantify

the cosmic variance and to measure the galaxy bias at z~5--6, and

therefore the galaxy halo masses at these redshifts. (4) We will also

find a large number of extremely red, old galaxies at intermediate

redshifts, and the fine spatial resolution offered by the WFC3 will

enable us constrain their formation history based on the study of their

morphology, and hence shed light on their connection to the very early

galaxies in the universe.

WFC3/IR 12307

A public SNAPSHOT Survey of Gamma-ray Burst Host Galaxies

We propose to conduct a public infrared survey of the host galaxies of

Swift selected gamma-ray bursts (GRBs) at z<3. By obtaining deep,

diffraction limited imaging in the IR we will complete detections for

the host galaxies, and in concert with our extensive ground based

afterglow and host programmes will compile a detailed catalog of the

properties of high-z galaxies selected by GRBs. In particular these

observations will enable us to study the colours, luminosities and

morphologies of the galaxies. This in turn informs studies of the nature

of the progenitors and the role of GRBs as probes of star formation

across cosmic history. Ultimately it provides a product of legacy value

which will greatly complement further studies with next generation

facilities such as ALMA and JWST.

WFC3/IR/S/C 11929

IR Dark Current Monitor

Analyses of ground test data showed that dark current signals are more

reliably removed from science data using darks taken with the same

exposure sequences as the science data, than with a single dark current

image scaled by desired exposure time. Therefore, dark current images

must be collected using all sample sequences that will be used in

science observations. These observations will be used to monitor changes

in the dark current of the WFC3-IR channel on a day-to-day basis, and to

build calibration dark current ramps for each of the sample sequences to

be used by Gos in Cycle 17. For each sample sequence/array size

combination, a median ramp will be created and delivered to the

calibration database system (CDBS).

WFC3/IR/UV 12163

Structure and Stellar Content of the Nearest Nuclear Clusters in

Late-Type Spiral Galaxies

HST surveys have shown that nuclear star clusters are nearly ubiquitous

in late-type, bulgeless disk galaxies. In early-type galaxies, the

central black hole mass correlates with the bulge mass and velocity

dispersion, but the relationship between black hole mass and host galaxy

properties in bulgeless galaxies is not yet understood. Some nuclear

clusters (such as the one in M33) do not contain a central massive black

hole at all, while other late-type galaxies (such as NGC 4395) are known

to contain accretion-powered active nuclei within their nuclear

clusters, indicating that a central black hole is present. But, the

overall "occupation fraction" of black holes within nuclear clusters is

largely unconstrained. Measurement of the structure, dynamics, and

stellar content of nuclear star clusters is an important pathway toward

understanding the demographics of low-mass black holes in late-type

galaxies.

We propose to obtain multi-filter WFC3 UV, optical, and near-IR images

of 10 of the nearest and brightest nuclear clusters in late-type spiral

galaxies. We will use the new WFC3 data to measure the cluster radial

profiles, to search for color gradients, and in combination with

ground-based spectroscopy and stellar population modeling, to determine

the stellar masses of the clusters. Since nuclear clusters are known to

contain stellar populations with a wide range of ages, the broad

wavelength coverage of our data will provide new leverage to constrain

the star formation history of the clusters. We will carry out dynamical

modeling for the clusters, using the cluster structural parameters and

stellar M/L ratios measured from the WFC3 data and kinematics measured

from ground-based, adaptive-optics assisted integral-field spectroscopy

(already obtained or approved for 8 of the 10 targets). This will yield

tight new constraints on the masses of intermediate-mass black holes

(IMBH) within the clusters, and may result in the first dynamical

detections of IMBHs in the nuclei of late-type spirals.

WFC3/IR/WFC/ACS/UV 12061

Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey -- GOODS-South

Field, Early Visits of SNe Search

This survey will document the first third of galactic evolution from z=8

to 1.5 and test for evolution in the properties of Type Ia supernovae to

z~2 by imaging more than 250, 000 galaxies with WFC3/IR and ACS. Five

premier multi-wavelength regions are selected from within the Spitzer

SEDS survey, providing complementary IRAC data down to 26.5 AB mag, a

unique resource for stellar masses at high redshifts. The use of five

widely separated fields mitigates cosmic variance and yields

statistically robust samples of galaxies down to 10^9 M_Sun out to z~8.

We adopt a two-tiered strategy with a "Wide" component (roughly 2 orbits

deep over ~0.2 sq. degrees) and a "Deep" component (roughly 12 orbits

deep over ~0.04 sq. degrees). Combining these with ultra-deep imaging

from the Cycle 17 HUDF09 program yields a three-tiered strategy for

efficient sampling of both rare/bright and faint/common objects.

Three of the Wide-survey fields are located in COSMOS, EGS, and

UKIDSS/UDS. Each of these consists of roughly 3x15 WFC3/IR tiles. Each

WFC3 tile will be observed for 2 orbits, with single orbits separated in

time to allow a search for high-redshift Type Ia SNe. The co-added

exposure times will be approximately 2/3 orbit in J (F125W) and 4/3

orbit in H (F160W). ACS parallels overlap most of the WFC3 area and will

consist of roughly 2/3 orbits in V (F606W) and 4/3 orbit in I (F814W).

Because of the larger area of ACS, this results in effective exposures

that are twice as long (4/3 in V, 8/3 in I), making a very significant

improvement to existing ACS mosaics in COSMOS and EGS and creating a new

ACS mosaic in UDS/UKIDSS where none now exists. Other Wide-survey

components are located in the GOODS fields (North and South) surrounding

the Deep-survey areas.

The Deep-survey fields cover roughly half of each GOODS field, with

exact areas and placements to be determined as part of the Phase-2

process. Each WFC3/IR tile within the Deep regions will receive

approximately 12 orbits of exposure time split between Y (F105W), J

(F125W), and H (F160W). Multi-epoch imaging will provide an efficient

search for high-redshift Type Ia SNe here also. ACS parallels are also

taken in the Deep regions, with the goal of assembling enough total

exposure time in F850LP and other filters to identify high redshift z>6

galaxies in concert with WFC3/IR data using the Lyman break technique.

A portion of the GOODS-N campaign will take place while the field is in

the HST Continuous Viewing Zone (CVZ). The bright time in those orbits

will be used to obtain UV imaging with WFC3 in the F275W and F336W

filters. The exact number of orbits will not be known until Phase-2

planning is complete, but we anticipate that it will be possible to

schedule at least 100 orbits, resulting in 5-sigma point-source depths

of 26.6, 26.4 in F275W and F336W, respectively. The science goals

include measuring the Lyman-continuum escape fractions for galaxies at

z~2.5 and identifying Lyman-break galaxies at z~2-3.

The Type Ia supernova search program in this proposal is integrated with

that in the Postman cluster MCT proposal, with this one stressing the

more distant supernovae. A combined follow-up program will provide light

curves and grism spectra of 15-20 of the best candidates at

redshifts 1<z<2. The observing configuration for the follow up will

depend on the redshift of the supernova, and will likely include a grism

observation with either ACS G800L, WFC3-IR G102, or G141, and light

curves observed with F850LP, WFC3-IR F125W, and F160W.

The new data will be used to answer many urgent questions in galaxy

evolution and cosmology. In the reionization era, we will identify

hundreds of high-confidence z>7 galaxies in the Deep regions, in

addition to hundreds of highly-luminous candidates in the Wide regions

for detailed follow-up. These samples will be used to construct a

unified picture of star-formation and stellar mass buildup in early

galaxies. Extremely deep X-ray data will reveal distant AGNs to z>6,

shedding light on the earliest stages of BH growth. In the peak star

formation/QSO era, z~2, we will document the properties of early disks,

the build-up of bulges, the evolution of mergers, and the nature of AGN

hosts to construct an integrated model for structural evolution, star

formation quenching, and AGN triggering. Finally, the ~8 Type Ia SNe

found beyond z>1.5 in the supernova programs will establish the

constancy of these standard candles independent of dark energy and yield

the first measurement of the Type Ia rate at z~2 to distinguish among

different progenitor models. Lower-redshift SNe Ia at 1<z<1.5 will be

used to measure the evolution of dark energy.

This program takes full advantage of MCTP mode to fulfill Hubble's

legacy for deep extragalactic science and prepare the way for JWST.

WFC3/UV 12344

Cycle 18: 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).

WFC3/UVIS/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.