Notice: Due to the conversion of some ACS WFC or HRC observations into

WFPC2, or NICMOS observations after the loss of ACS CCD science

capability in January, there may be an occasional discrepancy between a

proposal's listed (and correct) instrument usage and the abstract that

follows it.

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT       # 4485

PERIOD COVERED: UT November 07, 2007 (DOY 311)

OBSERVATIONS SCHEDULED

ACS/SBC 10864

Mapping the Gaseous Content of Protoplanetary and Young Planetary

Systems with ACS

One of the key problems in planetary system formation is understanding

how rapidly, and over what time interval Jovian planets can form. Dust

in the protoplanetary disk is critical in planetesimal formation, but it

is the gas which produces giant planets, and which is essential for

their migration. However, compared to data on the circumstellar dust,

information on the gas component is sparse, especially in the

planet-formation zone. This severely limits our ability to put

observational constraints on giant planet formation, except to note that

the process must be largely complete by 12 Myr, given the paucity of

Herbig Ae or classical T Tauri stars older than 10-12 Myr. In the FUV,

photo-excited molecular hydrogen transitions have the requisite contrast

to the stellar photosphere, accretion shock, and reflection nebulosity,

and can be traced 50-100 AU from the exciting stars in both envelopes

and outflow cavities and protoplanetary disks. Central disk cavities, an

expected consequence of planet formation, larger than 0.1" are directly

detectable in HST FUV spectra, while smaller cavities may be detected by

comparison with protoplanetary disks which are still accreting onto

their stars. We propose augmenting existing HST coronagraphic imagery of

6 Herbig Fe and T Tauri disks with ACS Solar-Blind Channel Lyman alpha

imagery and slitless spectroscopy simultaneously sampling the disk in

molecular hydrogen and small-grain reflection nebulosity. These data

will be used to quantify the amount of vertical stratification in these

disks, to map the mass-loss geometry from the star, and to determine

whether removal of molecular material precedes, lags, or is contemporary

with clearing of the dust.

WFPC2 11015

The Proper Motion of Supernova Remnant E0509-67.5

We propose to measure independently the proper motion expansions of the

ejecta and forward shock in E0509-67.5. The metal-enriched

reverse-shock-heated ejecta emits only in X-rays, while the forward

shock is traced to high precision by H alpha emission. The proposed

measurements require the unique high resolution imaging capabilities of

Chandra and Hubble. The optical {forward shock} and X-ray {ejecta}

results will yield important constraints on the remnant's evolutionary

state; we will search in particular for evidence of cosmic-ray modified

dynamics. An important component of this project is an integrated

theoretical investigation using realistic models of SN Ia explosions

evolved to the remnant stage.

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 DARKs. 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.

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.

S/C 4974

TRTTEST

The Transient Response Trending Testis for the periodic performance monitoring

of the FGS 2R servo A mechanism.

WEPC2 11196

An Ultraviolet Survey of Luminous Infrared Galaxies in the Local

Universe

At luminosities above 10^11.4 L_sun, the space density of far-infrared

selected galaxies exceeds that of optically selected galaxies. These

Luminous Infrared Galaxies {LIRGs} are primarily interacting or merging

disk galaxies undergoing starbursts and creating/fueling central AGN. We

propose far {ACS/SBC/F140LP} and near {WFPC2/PC/F218W} UV imaging of a

sample of 27 galaxies drawn from the complete IRAS Revised Bright Galaxy

Sample {RBGS} LIRGs sample and known, from our Cycle 14 B and I-band ACS

imaging observations, to have significant numbers of bright {23 < B < 21

mag} star clusters in the central 30 arcsec. The HST UV data will be

combined with previously obtained HST, Spitzer, and GALEX images to {i}

calculate the ages of the clusters as function of merger stage, {ii}

measure the amount of UV light in massive star clusters relative to

diffuse regions of star formation, {iii} assess the feasibility of using

the UV slope to predict the far- IR luminosity {and thus the star

formation rate} both among and within IR-luminous galaxies, and {iv}

provide a much needed catalog of rest-frame UV morphologies for

comparison with rest-frame UV images of high-z LIRGs and Lyman Break

Galaxies. These observations will achieve the resolution required to

perform both detailed photometry of compact structures and spatial

correlations between UV and redder wavelengths for a physical

interpretation our IRX-Beta results. The HST UV data, combined with the

HST ACS, Spitzer, Chandra, and GALEX observations of this sample, will

result in the most comprehensive study of luminous starburst galaxies to

date.

WFPC2 11103

A Snapshot Survey of The Most Massive Clusters of Galaxies

We propose the continuation of our highly successful SNAPshot survey of

a sample of 125 very X-ray luminous clusters in the redshift range

0.3-0.7. As demonstrated by the 25 snapshots obtained so far in Cycle14

and Cycle15 these systems frequently exhibit strong gravitational

lensing as well as spectacular examples of violent galaxy interactions.

The proposed observations will provide important constraints on the

cluster mass distributions, the physical nature of galaxy-galaxy and

galaxy-gas interactions in cluster cores, and a set of optically bright,

lensed galaxies for further 8-10m spectroscopy. All of our primary

science goals require only the detection and characterization of

high-surface-brightness features and are thus achievable even at the

reduced sensitivity of WFPC2. Because of their high redshift and thus

compact angular scale our target clusters are less adversely affected by

the smaller field of view of WFPC2 than more nearby systems.

Acknowledging the broad community interest in this sample we waive our

data rights for these observations. Due to a clerical error at STScI our

approved Cycle15 SNAP program was barred from execution for 3 months and

only 6 observations have been performed to date - reinstating this SNAP

at Cycle16 priority is of paramount importance to reach meaningful

statistics.

WFPC2 11128

Time Scales Of Bulge Formation In Nearby Galaxies

Traditionally, bulges are thought to fit well into galaxy formation

models of hierarchical merging. However, it is now becoming well

established that many bulges formed through internal, secular evolution

of the disk rather than through mergers. We call these objects

pseudobulges. Much is still unknown about pseudobulges, the most

pressing questions being: How, exactly, do they build up their mass? How

long does it take? And, how many exist? We are after an answer to these

questions. If pseudobulges form and evolve over longer periods than the

time between mergers, then a significant population of pseudobulges is

hard to explain within current galaxy formation theories. A pseudobulge

indicates that a galaxy has most likely not undergone a major merger

since the formation of the disk. The ages of pseudobulges give us an

estimate for the time scale of this quiescent evolution. We propose to

use 24 orbits of HST time to complete UBVIH imaging on a sample of 33

nearby galaxies that we have observed with Spitzer in the mid-IR. These

data will be used to measure spatially resolved stellar population

parameters {mean stellar age, metallicity, and star formation history};

comparing ages to star formation rates allows us to accurately constrain

the time scale of pseudobulge formation. Our sample of bulges includes

both pseudo- and classical bulges, and evenly samples barred and

unbarred galaxies. Most of our sample is imaged, 13 have complete UBVIH

coverage; we merely ask to complete missing observations so that we may

construct a uniform sample for studying bulge formation. We also wish to

compare the stellar population parameters to a variety of bulge and

global galaxy properties including star formation rates, dynamics,

internal bulge morphology, structure from bulge-disk decompositions, and

gas content. Much of this data set is already or is being assembled.

This will allow us to derive methods of pseudobulge identification that

can be used to accurately count pseudobulges in large surveys. Aside

from our own science goals, we will present this broad set of data to

the community. Thus, we waive proprietary periods for all observations.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS:

11047 - GSAcq (1,2,1) failed to RGA Hold (Gyro Control)

           At AOS 311/12:49:16, GSAcq (1,2,1) scheduled from 311/12:19:11

           12:26:36 had failed to RGA Hold (Gyro Control) due to QSTOP and QF1STOPF

           flags on FGS 1.

           OBAD #1 data unavailable due to LOS

           OBAD #2 data at AOS: V1 0.27, V2 -0.69, V3 0.72, RSS 1.03

           OBAD MAP not scheduled

11048 - REAcq (1,2,1) failed to RGA Hold (Gyro Control)

           At AOS (311/15:24:28) REAcq (1,2,1) scheduled from 311/15:19:05

           15:26:30 had failed to RGA Hold (Gyro Control) due to QSTOP & QF1STOPF

           flags on FGS 1. No 486 STB messages noted.

           OBAD #1 unavailable due to LOS

           OBAD #2: V1 1.26, V2 -1.82, V3 9.62, RSS 9.87

           OBAD MAP: V1 -0.72, V2 -6.13, V3 11.87, RSS 13.38

11049 - (Note, For Day 307) GSAcq(2,1,1) requires two attempts to achieve CT-DV

           OTA SE review of PTAS processing revealed that GSAcq(2,1,1) scheduled

           for 307/13:28:02 required two attempts to achieve CT-DV on FGS1. The

           acquisition was successful.

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                       SCHEDULED      SUCCESSFUL  

FGS GSacq               05                 04         

FGS REacq               10                 09           

OBAD with Maneuver 30                 30                    

SIGNIFICANT EVENTS: (None)