HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT       # 4560

PERIOD COVERED: UT March 04, 2008 (DOY 064)

OBSERVATIONS SCHEDULED

FGS 11295

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.

NIC1/NIC2/NIC3 11330

NICMOS Cycle 16 Extended Dark

This takes a series of Darks in parallel to other instruments.

NIC1/NIC2/NIC3 8795

NICMOS Post-SAA calibration - CR Persistence Part 6

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 i

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

passages leave different imprints on the NICMOS detectors.

NIC2 11142

Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3

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}.

NIC3 11153

The Physical Nature and Age of Lyman Alpha Galaxies

In the simplest scenario, strong Lyman alpha emission from high redshift

galaxies would indicate that stellar populations younger than 10 Myrs

dominate the UV. This does not, however, constrain the stellar

populations older than 100 Myrs, which do not contribute to UV light.

Also, the Lyman alpha line can be boosted if the interstellar medium is

both clumpy and dusty. Different studies with small samples have reached

different conclusions about the presence of dust and old stellar

populations in Lyman alpha emitters. We propose HST- NICMOS and

Spitzer-IRAC photometry of 35 Lyman-alpha galaxies at redshift

4.5<z<6.5, in order to determine their spectral energy distribution

{SED} extending through rest-frame optical. This will allow us to

measure accurately {1} The total stellar mass in these objects,

including old stars which may have formed at redshifts {z > 8} not

easily probed by any other means. {2} The dust extinction in the

rest-frame UV, and therefore a correction to their present

star-formation rates. Taken together, these two quantities will yield

the star-formation histories of Lyman alpha galaxies, which form fully

half of the known galaxies at z=4-6. They will tell us whether these are

young or old galaxies by straddling the 4000A break. Data from NICMOS is

essential for these compact and faint {i=25-26th magnitude AB} high

redshift galaxies, which are too faint for good near-IR photometry from

the ground.

WFPC2 10827

Imaging Polarimetry of the Seyfert 1 MCG-6-30-15: Clues to the Structure

of Warm Absorbers

Imaging polarimetry at high spatial resolution, which is only possible

with HST, offers a potentially powerful new tool for determining the

orientation and geometry of AGN containing warm absorbers. These

absorbed AGN tend to be more highly polarized than unabsorbed Type 1s,

but less polarized than Type 2s. If the polarized flux is due to a polar

scattering region as seen in polarized flux images of Seyfert 2s,

imaging polarimetry of nearby absorbed Type 1 objects using HST can

detect and resolve these scattering regions. We propose to make the

first HST imaging polarimetry study of an absorbed Seyfert 1 by

obtaining broad-band polarization images with WFPC2 of the prototypical

"dusty warm absorber" in MCG-6-30-15 {z=0.0077, D~33 Mpc}. We will

measure the wavelength dependence of the polarized light free from

dilution by the host galaxy starlight in order to assess whether the

polarization is due to a nuclear scattering region or dichroic

transmission through the absorbing dust. These observations will enable

us to {1} use the wavelength dependence of unresolved polarized flux to

understand the properties of the absorbing dust suggested by X-ray

spectral features attributed to Fe~I absorption, and {2} test whether

polarization in warm absorbers is due to resolved polar scattering

regions. Resolving the scattering region in a moderately polarized

Seyfert 1 such as MCG-6-30-15 will let us answer the question of whether

line-of-sight inclination can be directly linked to observed outflow

characteristics, as suggested by the most recent unified models of AGN

outflows.

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 11138

The Physics of the Jets of Powerful Radio Galaxies and Quasars

We propose to obtain HST polarimetry of the jets of the quasars 1150+497

and PKS 1136-135. Our goal is to solve the riddle of their high-energy

emission mechanism, and tackle issues such as particle acceleration and

jet dynamics. Our targets are the optically brightest quasar jets, and

they span the range of luminosities and beaming parameters seen in these

objects. Recent observations with Spitzer, HST and Chandra have shed new

light on the spectral morphology of quasar jets, throwing wide open the

question of the nature of their optical and X-ray emission. Three

mechanisms are possible, including synchrotron emission as well as two

Comptonization processes. Polarimetry can uniquely determine which of

these mechanisms operates in the optical. We will compare the optical

polarimetry to in- hand radio polarimetry as well as in-hand and new

Spitzer, HST and Chandra imaging to gain new insights on the structure

of these jets, as well as particle acceleration mechanisms and jet

dynamics.

WFPC2 11198

Pure Parallel Imaging in the NDWFS Bootes Field

The NOAO Deep-Wide Field Survey {NDWFS} Bootes field is the target of

one of the most extensive multiwavelength campaigns in astronomy. In

addition to ground-based optical and near-infrared imaging, deep radio

mapping, and extensive spectroscopy, this entire region has been imaged

by the Chandra, Spitzer {IRAC and MIPS}, and GALEX missions. Robust

photometric redshifts {calibrated using over 20,000 spectroscopic

redshifts} exist for all sources brighter than R=24.5 or than 13 uJy at

4.5 microns. To enhance the value of this data set, we propose pure

parallel observations for all approved Cycle 16 programs in this region

that lack coordinated parallel observations. The primary aim of this

program will be to provide a database useful for the broad range of

science programs underway in this region.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS:

11207 - OBAD Failed Quaternion (ESB 1903)

           At 065/08:48:39, OBAD using FHST trackers 1 & 3 failed. OBAD Flag

           mnemonic GOBSTAT=AttDtErr. One 486 ESB 1903 "OBAD Failed Quaternion" was

           received. OBAD1 had (RSS) value of 5261.56 arcseconds. OBAD2 had (RSS)

           value of 70.45 arcseconds. Dumped OBAD Tables 369 & 370 at 065/08:52:45

           per (OPS REQUEST 17543-2). Subsequent GSAcq at 065/08:53:49 was

           successful.

COMPLETED OPS REQUEST:

17543-2 - Dump OBAD tables after failed OBAD (Generic) @ 065/0852z

COMPLETED OPS NOTES: (None)

                        SCHEDULED      SUCCESSFUL  

FGS GSacq                08                  08                  

FGS REacq                06                  06                 

OBAD with Maneuver  28                  27      

SIGNIFICANT EVENTS: (None)