HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT       # 4610

PERIOD COVERED: 5am May 13 - 5am May 14, 2008 (DOY 134/0900z-135/0900z)

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 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.

NIC2/WFPC2 11142

Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3<z<2.7

Using HST and Spitzer

We aim to determine physical properties of IR luminous galaxies at

0.3<z<2.7 by requesting coordinated HST/NIC2 and MIPS 70um observations

of a unique, 24um flux-limited sample with complete Spitzer mid-IR

spectroscopy. The 150 sources investigated in this program have S{24um}

> 0.8mJy and their mid-IR spectra have already provided the majority

targets with spectroscopic redshifts {0.3<z<2.7}. The proposed

150~orbits of NIC2 and 66~hours of MIPS 70um will provide the physical

measurements of the light distribution at the rest-frame ~8000A and

better estimates of the bolometric luminosity. Combining these

parameters together with the rich suite of spectral diagnostics from the

mid-IR spectra, we will {1} measure how common mergers are among LIRGs

and ULIRGs at 0.3<z<2.7, and establish if major mergers are the drivers

of z>1 ULIRGs, as in the local Universe. {2} study the co-evolution of

star formation and blackhole accretion by investigating the relations

between the fraction of starburst/AGN measured from mid-IR spectra vs.

HST morphologies, L{bol} and z. {3} obtain the current best estimates of

the far-IR emission, thus L{bol} for this sample, and establish if the

relative contribution of mid-to-far IR dust emission is correlated with

morphology {resolved vs. unresolved}.

S/C 11163

Accreting Pulsating White Dwarfs in Cataclysmic Variables

Recent ground-based observations have increased the number of known

pulsating white dwarfs in close binaries with active mass transfer

{cataclysmic variables} from 5 to 11 systems. Our past Cycles 8 and 11

STIS observations of the first 2 known, followed by our Cycle 13 SBC

observations of the next 3 discovered, revealed the clear presence of

the white dwarf and increased amplitude of the pulsations in the UV

compared to the optical. The temperatures derived from the UV spectra

show 4 systems are much hotter than non-interacting pulsating white

dwarfs. A larger sample is needed to sort out the nature of the

instability strip in accreting pulsators i.e. whether effects of

composition and rotation due to accretion result in a well- defined

instability strip as a function of Teff.

WFPC2 10890

Morphologies of the Most Extreme High-Redshift Mid-IR-Luminous Galaxies

The formative phase of the most massive galaxies may be extremely

luminous, characterized by intense star- and AGN-formation. Till now,

few such galaxies have been unambiguously identified at high redshift,

restricting us to the study of low-redshift ultraluminous infrared

galaxies as possible analogs. We have recently discovered a sample of

objects which may indeed represent this early phase in galaxy formation,

and are undertaking an extensive multiwavelength study of this

population. These objects are bright at mid-IR wavelengths

{F[24um]>0.8mJy}, but deep ground based imaging suggests extremely faint

{and in some cases extended} optical counterparts {R~24-27}. Deep K-band

images show barely resolved galaxies. Mid-infrared spectroscopy with

Spitzer/IRS reveals that they have redshifts z ~ 2-2.5, suggesting

bolometric luminosities ~10^{13-14}Lsun! We propose to obtain deep ACS

F814W and NIC2 F160W images of these sources and their environs in order

to determine kpc-scale morphologies and surface photometry for these

galaxies. The proposed observations will help us determine whether these

extreme objects are merging systems, massive obscured starbursts {with

obscuration on kpc scales!} or very reddened {locally obscured} AGN

hosted by intrinsically low-luminosity galaxies.

WFPC2 11113

Binaries in the Kuiper Belt: Probes of Solar System Formation and

Evolution

The discovery of binaries in the Kuiper Belt and related small body

populations is powering a revolutionary step forward in the study of

this remote region. Three quarters of the known binaries in the Kuiper

Belt have been discovered with HST, most by our snapshot surveys. The

statistics derived from this work are beginning to yield surprising and

unexpected results. We have found a strong concentration of binaries

among low-inclination Classicals, a possible size cutoff to binaries

among the Centaurs, an apparent preference for nearly equal mass

binaries, and a strong increase in the number of binaries at small

separations. We propose to continue this successful program in Cycle 16;

we expect to discover at least 13 new binary systems, targeted to

subgroups where these discoveries can have the greatest impact.

WFPC2 11222

Direct Detection and Mapping of Star Forming Regions in Nearby, Luminous

Quasars

We propose to carry out narrow-band emission line imaging observations

of 8 quasars at z=0.05-0.15 with the WFPC2 ramp filters and with the

NICMOS narrow-band filters. We will obtain images in the [O II], [O

III], H-beta, and Pa-alpha emission line bands to carry out a series of

diagnostic tests aimed at detecting and mapping out star-forming regions

in the quasar host galaxies. This direct detection of star-forming

regions will confirm indirect indications for star formation in quasar

host galaxies. It will provide a crucial test for models of quasar and

galaxy evolution, that predict the co-existence of starbursts and

"monsters" and will solve the puzzle of why different indicators of star

formation give contradictory results. A secondary science goal is to

assess suggested correlations between quasar luminosity and the size of

the narrow-line region.

WFPC2 11518

Mutual eclipses of a Kuiper belt-satellite system

Ground-based observations two weeks ago strongly suggest that the orbit

of the small inner satellite of 2003 EL61, the 5th largest known dwarf

planet, is possibly precisely edge-on and thus somewhere in the middle

of a ~3 year long cycle of mutual eclipses, occultations, and transits.

We anticipate that with another year of ground-based observation we may

have sufficient data to accurately predict the times and durations of

these events, but by then the events may well be over. If events are

indeed occuring, measurement of the timing and depths of such events

provides a wealth of precise geometric information for constraining

sizes, shapes, orbits, and dynamics of the system.

We propose to obtain 5 quick WFPC2 visits to 2003 EL61 over the ~19 day

orbital period of the inner satellite to determine a precise orbit and

predict mutual event times. We will instantly (within ~1 day of the end

of the observations) make these predictions public to allow the maximum

number of attempts to collect the data as possible.

WFPC2/NIC3 11209

Determining the Structural Parameters of the First Globular Cluster

Found to Host an Black-Hole X-ray Binary

We recently published the discovery of the first black hole X-ray binary

in a globular cluster. This object is located in a bright globular

cluster around the Virgo elliptical NGC 4472. Here we propose to obtain

HST PC images of this black- hole hosting globular cluster and a sample

of other NGC 4472 globulars. We will use these data to determine the

structural parameters of both the globular cluster known to have a black

hole and a control sample of other NGC 4472 clusters. This will test

recent theoretical predictions how black holes affect the structural

parameters of globular clusters, and more generally will allow for the

first time constraints on any relationship between the presence of a

black hole and the surface brightness profiles of globular clusters. The

deep WFPC2 images outside of the galaxy's central regions will also be

invaluable for studying how the sizes and luminosity function of

globular clusters depend on distance from the center of the galaxy, and

thus address questions about the origin of the size differences between

metal-rich and metal-poor clusters and the shape of the globular cluster

luminosity function. In addition, parallel NIC3 images will allow the

optical to near-infrared colors of NGC 4472 globular cluster to be

determined over a wide range of galactocentric radii.

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:

18233-0 - Clear ACS Event Flag # 2 for OBS # 11163 @ 134/1534z

COMPLETED OPS NOTES: (None)

                        SCHEDULED      SUCCESSFUL

FGS GSacq               05                   05                  

FGS REacq               10                   10                  

OBAD with Maneuver 30                   30                        

SIGNIFICANT EVENTS: (None)