HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT    #4899

PERIOD COVERED: 5am July 30 - 5am July 31, 2009 (DOY 211/09:00z-212/09:00z)

OBSERVATIONS SCHEDULED

ACS 11465

ACS CCD Monitoring and Calibration for WFC3

This program is a smaller version of our routine CCD monitoring program,

designed to run throughout SMOV, after which our regular Cycle 17 CAL

proposal will begin. This program obtains the bias and dark frames

needed to generate reference files for calibrating science data, and

allows us to monitor detector noise and the growth of hot pixels.

STIS07 11404

CCD Dark and Bias Monitor for SMOV4/Cycle 17 Activity STIS-07

Monitor the darks for the STIS CCD. 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 11426

UVIS SMOV Contamination Monitor

The UV throughput of WFC3 during SMOV is monitored via weekly standard

star observations in a subset of key filters (as many as will fit into a

single orbit but to include at a minimum F218W, F225W, F275W, and

F606W). The data will provide a measure of throughput levels as a

function of time and wavelength, allowing for detection of the presence

of possible contaminants. In addition, a small set of internal exposures

are included with the externals, to provide verification of detector

stability.

This proposal corresponds to Activity WFC3-13.

WFC3 11437

WFC3 IR Image Quality

The IR imaging performance over field will be assessed in two passbands

to verify PSF encircled energy CEI specifications and other performance

metrics at 1 and 1.6 um, after the instrument has been aligned to the

OTA.

This proposal is Activity ID WFC3-24.

WFC3 11438

WFC3 UVIS PSF Wings

The UVIS PSF wings will be evaluated at 5 field points, near field

center and corners in two passbands to verify CEI specifications at 250

and 633 nm. The F275W and F625W filters will be used. Subarray images of

a moderately bright, isolated star will be obtained at each field

position with a series of increasing exposure times designed to permit

construction of a very high SNR PSF with dynamic range sufficient to

evaluate the wing intensity to >5 arcsec radius. Deep, saturated full

field images will also be obtained at each field point to permit

evaluation of the wings at larger radii. The images will also permit

examination of potential straylight effects, image persistence and

electronic cross-talk.

This is SMOV Activity WFC3-25

WFC3 11446

WFC3 UVIS Dark Current, Readnoise, and CTE

This proposal obtains full-frame, four-amp readout bias and dark frames

at regularly- spaced intervals throughout SMOV in order to assess and

monitor dark current, bad (warm, hot, dead) pixels, and readnoise. In

addition, a set of internals using the WFC3 calsystem are taken to

provide a baseline CTE measurement. WFC3-33

WFC3 11808

WFC3 UVIS Bowtie Monitor

The UVIS detector was observed during ground testing to occasionally

exhibit flat field and dark variations with a bowtie pattern. These

variations are most significant as ~1% flat field (gain) variations

across the field of view. It is believed that this represents a state or

condition into which the detector can transition for reasons and under

circumstances which are not currently understood. It is also very

unlikely that most science observations will determine the state (bowtie

or no-bowtie) of the detector. Ground test data indicates that this

state is long lived (many hours to ~one day). Hysteresis or memory of

past light exposure is also associated with this state.

Recent evidence suggests that exposing the detector to ~200k to 500k

electrons may quench this state. This proposal obtains an internal flat

field sequence of three exposures: one at 10x full well with two at 0.5x

full well immediately before and after. Each exposure is 3x3 binned to

reduce the data volume required.

These visits should be scheduled 2x per day until further direction is

provided.

WFC3/UVI 11657

The Population of Compact Planetary Nebulae in the Galactic Disk

We propose to secure narrow- and broad-band images of compact planetary

nebulae (PNe) in the Galactic Disk to study the missing link of the

early phases of post-AGB evolution. Ejected AGB envelopes become PNe

when the gas is ionized. PNe expand, and, when large enough, can be

studied in detail from the ground. In the interim, only the HST

capabilities can resolve their size, morphology, and central stars. Our

proposed observations will be the basis for a systematic study of the

onset of morphology. Dust properties of the proposed targets will be

available through approved Spitzer/IRS spectra, and so will the

abundances of the alpha-elements. We will be able thus to explore the

interconnection of morphology, dust grains, stellar evolution, and

populations. The target selection is suitable to explore the nebular and

stellar properties across the Galactic Disk, and to set constraints on

the galactic evolutionary models through the analysis of metallicity and

population gradients.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS: (None)

COMPLETED OPS REQUEST:

18663-0 - Genslew for proposal 11487 (slot # 6) @ 211/1407z

18664-0 - Genslew for proposal 11487 (slot # 7) @ 211/1409z

COMPLETED OPS NOTES: (None)

                       SCHEDULED      SUCCESSFUL

FGS GSAcq               8                    8              

FGS REAcq               7                    7            

OBAD with Maneuver 5                    5           

SIGNIFICANT EVENTS: (None)