Notice: For the foreseeable future, the daily reports may contain

apparent discrepancies between some proposal descriptions and the listed

instrument usage. This is due to the conversion of previously approved

ACS WFC or HRC observations into WFPC2, or NICMOS observations

subsequent to the loss of ACS CCD science capability in late January.

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4311

PERIOD COVERED: UT March 02,03,04, 2007 (DOY 061,062,063)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8794

NICMOS Post-SAA calibration - CR Persistence Part 5

A new procedure proposed to alleviate the CR-persistence problem of

NICMOS. Dark frames will be obtained immediately upon exiting the SAA

contour 23, and every time a NICMOS exposure is scheduled within 50

minutes of coming out of the SAA. The darks will be obtained in parallel

in all three NICMOS Cameras. The POST-SAA darks will be non- standard

reference files available to users with a USEAFTER date/time mark. The

keyword 'USEAFTER=date/time' will also be added to the header of each

POST-SAA DARK frame. The keyword must be populated with the time, in

addition to the date, because HST crosses the SAA ~8 times per day so

each POST-SAA DARK will need to have the appropriate time specified, for

users to identify the ones they need. Both the raw and processed images

will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS

science/calibration observations started within 50 minutes of leaving an

SAA will need such maps to remove the CR persistence from the science

images. Each observation will need its own CRMAP, as different SAA

passages leave different imprints on the NICMOS detectors.

WFPC2 11096

Hubble Heritage imaging of Jupiter during the New Horizons encounter HST

Proposal 11096

WFPC2 images of Jupiter in Feb 2007 in support of New Horizons flyby of

Jupiter. This Hubble Heritage DD program is working in concert with the

existing GO programs by John Clarke {10862} and John Spencer {10871}.

WFPC2 11083

The Structure, Formation and Evolution of Galactic Cores and Nuclei

A surprising result has emerged from the ACS Virgo Cluster Survey

{ACSVCS}, a program to obtain ACS/WFC gz imaging for a large, unbiased

sample of 100 early-type galaxies in the Virgo Cluster. On subarcsecond

scales {i.e., <0.1"-1"}, the HST brightness profiles vary systematically

from the brightest giants {which have nearly constant surface brightness

cores} to the faintest dwarfs {which have compact stellar nuclei}.

Remarkably, the fraction of galaxy mass contributed by the nuclei in the

faint galaxies is identical to that contributed by supermassive black

holes in the bright galaxies {0.2%}. These findings strongly suggest

that a single mechanism is responsible for both types of Central Massive

Object: most likely internally or externally modulated gas inflows that

feed central black holes or lead to the formation of "nuclear star

clusters". Understanding the history of gas accretion, star formation

and chemical enrichment on subarcsecond scales has thus emerged as the

single most pressing question in the study of nearby galactic nuclei,

either active or quiescent. We propose an ambitious HST program {199

orbits} that constitutes the next, obvious step forward:

high-resolution, ultraviolet {WFPC2/F255W} and infrared {NIC1/F160W}

imaging for the complete ACSVCS sample. By capitalizing on HST's unique

ability to provide high-resolution images with a sharp and stable PSF at

UV and IR wavelengths, we will leverage the existing optical HST data to

obtain the most complete picture currently possible for the history of

star formation and chemical enrichment on these small scales. Equally

important, this program will lead to a significant improvement in the

measured structural parameters and density distributions for the stellar

nuclei and the underlying galaxies, and provide a sensitive measure of

"frosting" by young stars in the galaxy cores. By virtue of its superb

image quality and stable PSF, NICMOS is the sole instrument capable of

the IR observations proposed here. In the case of the WFPC2

observations, high-resolution UV imaging {< 0.1"} is a capability unique

to HST, yet one that could be lost at any any time.

NIC3 11082

NICMOS Imaging of GOODS: Probing the Evolution of the Earliest Massive

Galaxies, Galaxies Beyond

Deep near-infrared imaging provides the only avenue towards

understanding a host of astrophysical problems, including: finding

galaxies and AGN at z > 7, the evolution of the most massive galaxies,

the triggering of star formation in dusty galaxies, and revealing

properties of obscured AGN. As such, we propose to observe 60 selected

areas of the GOODS North and South fields with NICMOS Camera 3 in the

F160W band pointed at known massive M > 10^11 M_0 galaxies at z > 2

discovered through deep Spitzer imaging. The depth we will reach {26.5

AB at 5 sigma} in H_160 allows us to study the internal properties of

these galaxies, including their sizes and morphologies, and to

understand how scaling relations such as the Kormendy relationship

evolved. Although NIC3 is out of focus and undersampled, it is currently

our best opportunity to study these galaxies, while also sampling enough

area to perform a general NIR survey 1/3 the size of an ACS GOODS field.

These data will be a significant resource, invaluable for many other

science goals, including discovering high redshift galaxies at z > 7,

the evolution of galaxies onto the Hubble sequence, as well as examining

obscured AGN and dusty star formation at z > 1.5. The GOODS fields are

the natural location for HST to perform a deep NICMOS imaging program,

as extensive data from space and ground based observatories such as

Chandra, GALEX, Spitzer, NOAO, Keck, Subaru, VLT, JCMT, and the VLA are

currently available for these regions. Deep high-resolution

near-infrared observations are the one missing ingredient to this

survey, filling in an important gap to create the deepest, largest, and

most uniform data set for studying the faint and distant universe. The

importance of these images will increase with time as new facilities

come on line, most notably WFC3 and ALMA, and for the planning of future

JWST observations.

NIC3 11080

Exploring the Scaling Laws of Star Formation

As a variety of surveys of the local and distant Universe are

approaching a full census of galaxy populations, our attention needs to

turn towards understanding and quantifying the physical mechanisms that

trigger and regulate the large-scale star formation rates {SFRs} in

galaxies.

WFPC2 11029

WFPC2 CYCLE 15 Intflat Linearity Check and Filter Rotation Anomaly

Monitor

Intflat observations will be taken to provide a linearity check: the

linearity test consists of a series of intflats in F555W, in each gain

and each shutter. A combination of intflats, visflats, and earthflats

will be used to check the repeatability of filter wheel motions.

{Intflat sequences tied to decons, visits 1-18 in prop 10363, have been

moved to the cycle 15 decon proposal xxxx for easier scheduling.} Note:

long-exposure WFPC2 intflats must be scheduled during ACS anneals to

prevent stray light from the WFPC2 lamps from contaminating long ACS

external exposures.

FGS 10989

Astrometric Masses of Extrasolar Planets and Brown Dwarfs

We propose observations with HST/FGS to estimate the astrometric

elements {perturbation orbit semi-major axis and inclination} of

extra-solar planets orbiting six stars. These companions were originally

detected by radial velocity techniques. We have demonstrated that FGS

astrometry of even a short segment of reflex motion, when combined with

extensive radial velocity information, can yield useful inclination

information {McArthur et al. 2004}, allowing us to determine companion

masses. Extrasolar planet masses assist in two ongoing research

frontiers. First, they provide useful boundary conditions for models of

planetary formation and evolution of planetary systems. Second, knowing

that a star in fact has a plantary mass companion, increases the value

of that system to future extrasolar planet observation missions such as

SIM PlanetQuest, TPF, and GAIA.

WFPC2 10918

Reducing Systematic Errors on the Hubble Constant: Metallicity

Calibration of the Cepheid PL Relation

Reducing the systematic errors on the Hubble constant is still of

significance and of immediate importance to modern cosmology. One of the

largest remaining uncertainties in the Cepheid-based distance scale

{which itself is at the foundation of the HST Key Project determination

of H_o} which can now be addressed directly by HST, is the effect of

metallicity on the Cepheid Period-Luminosity relation. Three chemically

distinct regions in M101 will be used to directly measure and thereby

calibrate the change in zero point of the Cepheid PL relation over a

range of metallicities that run from SMC-like, through Solar, to

metallicities as high as the most metal-enriched galaxies in the pure

Hubble flow. ACS for the first time offers the opportunity to make a

precise calibration of this effect which currently accounts for at least

a third of the total systematic uncertainty on Ho. The calibration will

be made in the V and I bandpasses so as to be immediately and directly

applicable to the entire HST Cepheid-based distance scale sample, and

most especially to the highest-metallicity galaxies that were hosts to

the Type Ia supernovae, which were then used to extend the the distance

scale calibration out to cosmologically significant distances.

FGS 10912

Trigonometric Calibration of the Distance Scale for Classical Novae

The distance scale for classical novae is important for understanding

the stellar physics of their thermonuclear runaways, their contribution

to Galactic nucleosynthesis, and their use as extragalactic standard

candles. Although it is known that there is a relationship between their

absolute magnitudes at maximum light and their subsequent rates of

decline--the well-known maximum-magnitude rate-of-decline {MMRD}

relation--it is difficult to set the zero-point for the MMRD because of

the very uncertain distances of Galactic novae. We propose to measure

precise trigonometric parallaxes for the quiescent remnants of the four

nearest classical novae. We will use the Fine Guidance Sensors, which

are proven to be capable of measuring parallaxes with errors of ~0.2

mas, well below what is possible from the ground.

NIC2 10906

The Fundamental Plane of Massive Gas-Rich Mergers: II. The QUEST QSOs

We propose deep NICMOS H-band imaging of a carefully selected sample of

23 local QSOs. This program is the last critical element of a

comprehensive investigation of the most luminous mergers in the nearby

universe, the ultraluminous infrared galaxies {ULIRGs} and the quasars.

This effort is called QUEST: Quasar / ULIRG Evolutionary STudy. The

high-resolution HST images of the QUEST QSOs will complement an

identical set of images on the ULIRG sample obtained during Cycle 12, an

extensive set of ground- based data that include long-slit NIR spectra

from a Large VLT Program, and a large set of mid-infrared spectra from a

Cycle 1 medium-size program with Spitzer. This unique dataset will allow

us to derive with unprecedented precision structual, kinematic, and

activity parameters for a large unbiased sample of objects spanning the

entire ULIRG/QSO luminosity function. These data will refine the

fundamental plane of massive gas-rich mergers and enable us to answer

the following quesitons: {1} Do ultraluminous mergers form elliptical

galaxies, and in particular, giant ellipticals? {2} Do ULIRGs evolve

into optical bright QSOs? The results from this detailed study of

massive mergers in the local universe will be relevant to understanding

the basic physical processes involved in creating massive early-type

host on the one hand, and growing/feeding embedded massive black holes

on the other, in major galaxy mergers. This is an important question

since 50% of cosmic star formation at high-z and most of the big BHs

appear to be formed in this process.

ACS/SBC 10862

Comprehensive Auroral Imaging of Jupiter and Saturn during the

International Heliophysical Year

A comprehensive set of observations of the auroral emissions from

Jupiter and Saturn is proposed for the International Heliophysical Year

in 2007, a unique period of especially concentrated measurements of

space physics phenomena throughout the solar system. We propose to

determine the physical relationship of the various auroral processes at

Jupiter and Saturn with conditions in the solar wind at each planet.

This can be accomplished with campaigns of observations, with a sampling

interval not to exceed one day, covering at least one solar rotation.

The solar wind plasma density approaching Jupiter will be measured by

the New Horizons spacecraft, and a separate campaign near opposition in

May 2007 will determine the effect of large-scale variations in the

interplanetary magnetic field {IMF} on the Jovian aurora by

extrapolation from near-Earth solar wind measurements. A similar Saturn

campaign near opposition in Jan. 2007 will combine extrapolated solar

wind data with measurements from a wide range of locations within the

Saturn magnetosphere by Cassini. In the course of making these

observations, it will be possible to fully map the auroral footprints of

Io and the other satellites to determine both the local magnetic field

geometry and the controlling factors in the electromagnetic interaction

of each satellite with the corotating magnetic field and plasma density.

Also in the course of making these observations, the auroral emission

properties will be compared with the properties of the near-IR

ionospheric emissions {from ground-based observations} and non thermal

radio emissions, from ground-based observations for Jupiter?s decametric

radiation and Cassini plasma wave measurements of the Saturn Kilometric

Radiation {SKR}.

NIC3 10836

The Red Sequence at 1.3 < z < 1.4 in Galaxy Clusters

We propose to obtain NIC3/F160W imaging of three new IRAC-selected

galaxy clusters at 1.3 < z < 1.5. In combination with deep ACS/F850LP

images being obtained in Cycle 14, the resulting precision photometry in

a rest ~U - R color will allow us to construct color- magnitude diagrams

which can be used to measure the slope and scatter in the red sequence

galaxies, thereby constraining the history of star formation in the

early-type galaxies. The number of morphologically-selected early-type

galaxies more luminous than L* will allow us to test the predictions of

the hierarchical merging scenario for galaxy formation in clusters at

the highest available redshifts in galaxy clusters.

NIC2 10808

Morphologies of spectroscopically-confirmed "red and dead" galaxies at

z~2.5

Using a combination of wide-field near-infrared imaging and very deep

follow-up near-infrared spectroscopy we have identified a population of

massive "red and dead" galaxies at z~2.5. The galaxies lack emission

lines and have strong Balmer/4000 Angstrom breaks, demonstrating

directly that they have evolved stellar populations. These objects are

very likely progenitors of massive ellipticals today and may be

descendants of the first generation of galaxies. We propose to image 10

of these objects with the NIC2 camera to determine their morphologies.

The goals are to 1} determine whether they have the sizes of present-day

early-types or are more compact, as predicted by models, 2} determine

the morphology, using visual classification and quantitative methods,

and 3} constrain the evolution of the Kormendy relation from z~2.5 to

the present. These observations will show whether the oldest and most

massive galaxies at z~2.5 were already fully formed or still in the

process of assembly.

WFPC2 10802

SHOES-Supernovae, HO, for the Equation of State of Dark energy

The present uncertainty in the value of the Hubble constant {resulting

in an uncertainty in Omega_M} and the paucity of Type Ia supernovae at

redshifts exceeding 1 are now the leading obstacles to determining the

nature of dark energy. We propose a single, integrated set of

observations for Cycle 15 that will provide a 40% improvement in

constraints on dark energy. This program will observe known Cepheids in

six reliable hosts of Type Ia supernovae with NICMOS, reducing the

uncertainty in H_0 by a factor of two because of the smaller dispersion

along the instability strip, the diminished extinction, and the weaker

metallicity dependence in the infrared. In parallel with ACS, at the

same time the NICMOS observations are underway, we will discover and

follow a sample of Type Ia supernovae at z > 1. Together, these

measurements, along with prior constraints from WMAP, will provide a

great improvement in HST's ability to distinguish between a static,

cosmological constant and dynamical dark energy. The Hubble Space

Telescope is the only instrument in the world that can make these IR

measurements of Cepheids beyond the Local Group, and it is the only

telescope in the world that can be used to find and follow supernovae at

z > 1. Our program exploits both of these unique capabilities of HST to

learn more about one of the greatest mysteries in science.

NIC2 10798

Dark Halos and Substructure from Arcs & Einstein Rings

The surface brightness distribution of extended gravitationally lensed

arcs and Einstein rings contains super-resolved information about the

lensed object, and, more excitingly, about the smooth and clumpy mass

distribution of the lens galaxies. The source and lens information can

non-parametrically be separated, resulting in a direct "gravitational

image" of the inner mass-distribution of cosmologically-distant galaxies

{Koopmans 2005; Koopmans et al. 2006 [astro-ph/0601628]}. With this goal

in mind, we propose deep HST ACS-F555W/F814W and NICMOS-F160W WFC

imaging of 20 new gravitational-lens systems with spatially resolved

lensed sources, of the 35 new lens systems discovered by the Sloan Lens

ACS Survey {Bolton et al. 2005} so far, 15 of which are being imaged in

Cycle-14. Each system has been selected from the SDSS and confirmed in

two time- efficient HST-ACS snapshot programs {cycle 13&14}.

High-fidelity multi-color HST images are required {not delivered by the

420s snapshots} to isolate these lensed images {properly cleaned,

dithered and extinction-corrected} from the lens galaxy surface

brightness distribution, and apply our "gravitational maging" technique.

Our sample of 35 early-type lens galaxies to date is by far the largest,

still growing, and most uniformly selected. This minimizes selection

biases and small-number statistics, compared to smaller, often

serendipitously discovered, samples. Moreover, using the WFC provides

information on the field around the lens, higher S/N and a better

understood PSF, compared with the HRC, and one retains high spatial

resolution through drizzling. The sample of galaxy mass distributions -

determined through this method from the arcs and Einstein ring HST

images - will be studied to: {i} measure the smooth mass distribution of

the lens galaxies {dark and luminous mass are separated using the HST

images and the stellar M/L values derived from a joint stellar-dynamical

analysis of each system}; {ii} quantify statistically and individually

the incidence of mass-substructure {with or without obvious luminous

counter- parts such as dwarf galaxies}. Since dark-matter substructure

could be more prevalent at higher redshift, both results provide a

direct test of this prediction of the CDM hierarchical

structure-formation model.

FGS 10610