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    # 4367

PERIOD COVERED: UT May 21, 2007 (DOY 141)

OBSERVATIONS SCHEDULED

WFPC2 10800

Kuiper Belt Binaries: Probes of Early Solar System Evolution

Binaries in the Kuiper Belt are a scientific windfall: in them we have

relatively fragile test particles which can be used as tracers of the

early dynamical evolution of the outer Solar System. We propose to

continue a Snapshot program using the ACS/HRC that has a demonstrated

discovery potential an order of magnitude higher than the HST

observations that have already discovered the majority of known

transneptunian binaries. With this continuation we seek to reach the

original goals of this project: to accumulate a sufficiently large

sample in each of the distinct populations collected in the Kuiper Belt

to be able to measure, with statistical significance, how the fraction

of binaries varies as a function of their particular dynamical paths

into the Kuiper Belt. Today's Kuiper Belt bears the imprints of the

final stages of giant-planet building and migration; binaries may offer

some of the best preserved evidence of that long-ago era.

WFPC2 10832

Solving the microlensing puzzle: An HST high-resolution imaging approach

We propose to use the HST Advanced Camera for Surveys High Resolution

Channel to obtain high resolution imaging data for 10 bona-fide LMC

microlensing events seen in the original MACHO survey. The purpose of

this survey will be to assess whether or not the lens and source stars

have separated enough to be resolved since the original microlensing

event took place - about a decade has passed since the original MACHO

survey and the HST WFPC2 follow-up observations of the microlensing

events. If the components of the lensing event are resolved, we will

determine the apparent magnitude and color of both the lens and the

source stars. These data, in combination with Spitzer/IRAC data and

Magellan near-IR JHK data, will be used to ascertain the basic

properties of the lens stars. With the majority of the microlensing

events in the original MACHO survey observed at the highest spatial

resolution currently possible, we will be able to draw important

conclusions as to what fraction of these events have lenses which belong

to some population of dwarf stars in the disk and what fraction must be

due to lenses in the halo or beyond. These data will greatly increase

our understanding of the structure of the Galaxy by characterizing the

stellar population responsible for the gravitational microlensing.

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}.

NIC2 10858

NICMOS Imaging of the z ~ 2 Spitzer Spectroscopic Sample of

Ultraluminous Infrared Galaxies

We propose to obtain NICMOS images of the first large sample of high-z

ultra-luminous infrared galaxies {ULIRGs} whose redshifts and physical

states have been determined with Spitzer mid-IR spectra. The detection

of strong silicate absorption and/or PAH emission lines suggest that the

these sources are a mixture of highly obscured starbursts, AGNs and

composite systems at z=2. Although some of the spectra show PAH emission

similar to local starburst ULIRGs, their bolometric luminosities are

roughly an order of magnitude higher. One important question is if major

mergers, which are the trigger for 95% of local ULIRGs, also drive this

enormous energy output observed in our z=2 sample. The NICMOS images

will allow us to {1} measure surface brightness profiles of z~2 ULIRGs

and establish if major mergers could be common among our luminous

sources at these early epochs, {2} determine if starbursts and AGNs

classified based on their mid-IR spetra would have different

morphological signatures, thus different dynamic state; {3} make

comparisons with the similar studies of ULIRGs at z ~ 0 - 1, thus infer

any evolutionary connections between high-z ULIRGs and the formation of

normal, massive galaxies and quasars observed today.

WFPC2 10880

The host galaxies of QSO2s: AGN feeding and evolution at high

luminosities

Now that the presence of supermassive black holes in the nuclei of

galaxies is a well established fact, other questions related to the AGN

phenomena still have to be answered. Problems of particular interest are

how the AGN gets fed, how the black hole evolves and how the evolution

of the black hole is related to the evolution of the galaxy bulge. Here

we propose to address some of these issues using ACS/WFC + F775W

snapshot images of 73 QSO2s with redshifts in the range 0.3<z<0.4. These

observations will be combined with similar archival data of QSO1s and

ground based data of Seyfert and normal galaxies. First, we will

intestigate whether interactions are the most important feeding

mechanism in high luminosity AGNs. This will be done in a quantitative

way, comparing the asymmetry indices of QSO2 hosts with those of lower

luminosity AGNs and normal galaxies. Second, we will do a detailed study

of the morphology of the host galaxies of both QSO types, to determine

if they are similar, or if there is an evolutionary trend from QSO2s to

QSO1s. The results from this project will represent an important step in

the understanding of AGN evolution, and may also introduce a substantial

modification to the Unified Model.

WFPC2 11024

WFPC2 CYCLE 15 INTERNAL MONITOR

This calibration proposal is the Cycle 15 routine internal monitor for

WFPC2, to be run weekly to monitor the health of the cameras. A variety

of internal exposures are obtained in order to provide a monitor of the

integrity of the CCD camera electronics in both bays {both gain 7 and

gain 15 -- to test stability of gains and bias levels}, a test for

quantum efficiency in the CCDs, and a monitor for possible buildup of

contaminants on the CCD windows. These also provide raw data for

generating annual super-bias reference files for the calibration

pipeline.

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 11023

WFPC2 CYCLE 15 Standard Darks - part 1

This dark calibration program obtains dark frames every week in order to

provide data for the ongoing calibration of the CCD dark current rate,

and to monitor and characterize the evolution of hot pixels. Over an

extended period these data will also provide a monitor of radiation

damage to the CCDs.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS:

10820 - GSAcq (1,2,2) failed to RGA Hold (Gyro Control)

           AT AOS (141/13:29:30) GSAcq (1,2,2) had failed to RGA Hold (Gyro

           Control) due to QSTOP flag on FGS 1.

           OBAD #1 unavailable due to LOS

           OBAD #2 RSS: 15.84

10821 - ACS 779 Fold Mechanism Move was Blocked

           At 141/13:31:24 "Fold Mechanism Move Was Blocked P=0, T=1001. This was

           the result of the failed GSAcq at 13:22:49 so the TDF was down when the

           fold mechanism move to the SBC position was commanded. The move is

           blocked and SBC MAMA HV will remain on. The MAMA HV staying on is a new

           feature for ACS FSW CS4.01.

10824 - FHST OBAD1 Failure

           During LOS OBAD1 scheduled at 142/04:18:07 using trackers 1 and 2

           failed. Subsequent OBAD2 and guide star acquisition was successful.

10825 - REacq(1,2,1) failed due to search radius limit exceeded

           During LOS REacq(1,2,1) scheduled at 142/06:06:34 failed due to search

           radius limit exceeded on FGS 1.

COMPLETED OPS REQUEST:

18083-1 - MSS/Gyro2 Initialization Test#35 @141/1301z

18084-0 - MSS/Gyro1 Initialization Test#11 @141/2126z

18085-0 - PCS KF OOT Support,141/1302z

18086-0 - PCS KF OOT Support,141/2134z

COMPLETED OPS NOTES: (None)

                       SCHEDULED      SUCCESSFUL   

FGS GSacq                09                 07               

FGS REacq                03                 03       

OBAD with Maneuver  24                 23               

SIGNIFICANT EVENTS:

Evaluation of Universal Kalman Filter performance continued. Multiple

text segments were executed, all of them successfully. Details follow.

The KF was halted at 141/12:48. It was restarted at 141/12:50 with the

MSS and Gyro2 sensor inputs enabled. The initialization occurred during

orbit day with the CSS input disabled. The initialization was executed

during a vehicle slew and during a slow changing B-field. All UKF

parameters showed nominal operation. The test was an MSS/Gyro2

Initialization test case during a slow changing B-field (M_G2_IVS, Test

#35). The filter was reconfigured back to MSS only input at 141/13:00.

The KF was halted at 141/21:24. It was restarted at 141/21:26 with the

MSS and Gyro1 sensor inputs enabled. The initialization occurred during

orbit day with the CSS input disabled. The initialization was executed

during a vehicle slew and during a fast changing B-field. All UKF

parameters showed nominal operation. The test was an MSS/Gyro1

Initialization test case during a fast changing B-field (M_G1_IVF, Test

#11). The filter was reconfigured back to MSS only input at 141/22:06.