Daily # 4316

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*** # 4316

PERIOD COVERED: UT March 09,10,11, 2007 (DOY 068,069,070)

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 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 11083

The Structure, Formation and Evolution of Galactic Cores and Nuclei

A surprising result has emerged from the ACS Virgo Cluster Survey
{ACSVCS}, a program to obtain ACS/WFC gz imaging for a large, unbiased
sample of 100 early-type galaxies in the Virgo Cluster. On
subarcsecond scales {i.e., 0.1"-1"}, the HST brightness profiles vary
systematically from the brightest giants {which have nearly constant
surface brightness cores} to the faintest dwarfs {which have compact
stellar nuclei}. Remarkably, the fraction of galaxy mass contributed
by the nuclei in the faint galaxies is identical to that contributed
by supermassive black holes in the bright galaxies {0.2%}. These
findings strongly suggest that a single mechanism is responsible for
both types of Central Massive Object: most likely internally or
externally modulated gas inflows that feed central black holes or lead
to the formation of "nuclear star clusters". Understanding the history
of gas accretion, star formation and chemical enrichment on
subarcsecond scales has thus emerged as the single most pressing
question in the study of nearby galactic nuclei, either active or
quiescent. We propose an ambitious HST program {199 orbits} that
constitutes the next, obvious step forward: high-resolution,
ultraviolet {WFPC2/F255W} and infrared {NIC1/F160W} imaging for the
complete ACSVCS sample. By capitalizing on HST's unique ability to
provide high-resolution images with a sharp and stable PSF at UV and
IR wavelengths, we will leverage the existing optical HST data to
obtain the most complete picture currently possible for the history of
star formation and chemical enrichment on these small scales. Equally
important, this program will lead to a significant improvement in the
measured structural parameters and density distributions for the
stellar nuclei and the underlying galaxies, and provide a sensitive
measure of "frosting" by young stars in the galaxy cores. By virtue of
its superb image quality and stable PSF, NICMOS is the sole instrument
capable of the IR observations proposed here. In the case of the WFPC2
observations, high-resolution UV imaging { 0.1"} is a capability
unique to HST, yet one that could be lost at any any time.

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.

NIC3 11064

CYCLE 15 NICMOS SPECTROPHOTOMETRY CALIBRATION PROGRAM

Now that the spectrophotometric capabilities of the NICMOS grism have
been established, cycle 15 observations are needed to refine the
sensitivity estimates, to check for sensitivity loss with time, to
improve the accuracy of the linearity correction, to improve the
secondary flux standards by re-observation, and to expand the G206
data set now that the sky subtraction technique has been shown to
produce useful fluxes for some of the fainter secondary standards.
These faint secondary IR standards will be a significant step towards
establishing flux standards for JWST, as well as for SNAP, Spitzer,
and SOFIA. 1.Re- observe the 3 primary WDs GD71, G191B2b, & GD153
twice each, once at the beginning and once near the end of the 18
month cycle. To date, we have only 2 observation of each star, while
the corresponding STIS data set for these primary standards ranges
from 6 to 23 obs. No observations exist for GD71 or GD153 with G206,
so that the current G206 sensitivity is defined solely by G191B2B.
Purposes: Refine sensitivities, measure sens losses. Orbits: 2 for
each of 6 visits = 12 2. Re-observe WD1057 & WD1657 plus another P041C
lamp-on visit to improve the scatter in the non-lin measurements per
Fig. 8 of NIC ISR 2006-02. The WD stars require 2 orbits each, while
the lamp-on test is done in one. The very faintest and most crucial
standard WD1657 has 2 good visits already, so to substantially improve
the S/N, two visits of two orbits are needed. Include G206 for P041C
in the lamp-off baseline part of that orbit. Orbits: WD1057-2,
WD1657-4, P041C-1 -- 7 3. Re-observe 9 secondary standards to improve
S/N of the faint ones and to include G206 for all 9. BD+17 {3 obs} is
not repeated in this cycle. Four are bright enough to do in one orbit:
VB8, 2M0036+18, P330E, and P177D. Orbits:2*5+4=14 Grand Total orbits
over 18 month cycle 15 is 12+6+14=32 {Roelof will submit the P041C
lamp-on visit in a separate program.}

NIC1 11057

Cycle 15 NICMOS dark current, shading profile, and read noise
monitoring program

The purpose of this proposal is to monitor the dark current, read
noise, and shading profile for all three NICMOS detectors throughout
the duration of Cycle 15. This proposal is a slightly modified version
of proposal 10380 of cycle 13 and 9993 of cycle12 and is the same as
Cycle 14. that we cut down some exposure time to make the observation
fit within 24 orbits.

FGS 10989

Astrometric Masses of Extrasolar Planets and Brown Dwarfs

We propose observations with HST/FGS to estimate the astrometric
elements {perturbation orbit semi-major axis and inclination} of
extra-solar planets orbiting six stars. These companions were
originally detected by radial velocity techniques. We have
demonstrated that FGS astrometry of even a short segment of reflex
motion, when combined with extensive radial velocity information, can
yield useful inclination information {McArthur et al. 2004}, allowing
us to determine companion masses. Extrasolar planet masses assist in
two ongoing research frontiers. First, they provide useful boundary
conditions for models of planetary formation and evolution of
planetary systems. Second, knowing that a star in fact has a plantary
mass companion, increases the value of that system to future
extrasolar planet observation missions such as SIM PlanetQuest, TPF,
and GAIA.

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 10847

Coronagraphic Polarimetry of HST-Resolved Debris Disks

We propose to take full advantage of the recently commissioned
coronagraphic polarimetry modes of ACS and NICMOS to obtain imaging
polarimetry of circumstellar debris disks that were imaged previously
by the HST coronagraphs, but without the polarizers. It is well
established that stars form in gas-rich protostellar disks, and that
the planets of our solar system formed from a circum-solar disk.
However, the connection between the circumstellar disks that we
observe around other stars and the processes of planet formation is
still very uncertain. Mid-IR spectral studies have suggested that disk
grains are growing in the environments of young stellar objects during
the putative planet-formation epoch. Furthermore, structures revealed
in well resolved images of circumstellar disks suggest gravitational
influences on the disks from co-orbital bodies of planetary mass.
Unfortunately, existing imaging data provides only rudimentary
information abou the disk grains and their environments. Our proposed
observations, which can be obtained only with HST, will enable us to
quantitatively determine the sizes of the grains and optical depths as
functions of their location within the disks {i.e., detailed
tomography}. Armed with these well-determine physical and geometrical
systemic parameters, we will develop a set of self- consistent models
of disk structures to investigate possible interactions between unseen
planets and the disks from which they formed. Our results will also
calibrate models of the thermal emission from these disks, that will
in turn enable us to infer the properties of other debris disks that
cannot be spatially resolved with current or planned instruments and
telescopes.

NIC3 10836

The Red Sequence at 1.3 z 1.4 in Galaxy Clusters

We propose to obtain NIC3/F160W imaging of three new IRAC-selected
galaxy clusters at 1.3 z 1.5. In combination with deep ACS/F850LP
images being obtained in Cycle 14, the resulting precision photometry
in a rest ~U - R color will allow us to construct color- magnitude
diagrams which can be used to measure the slope and scatter in the red
sequence galaxies, thereby constraining the history of star formation
in the early-type galaxies. The number of morphologically-selected
early-type galaxies more luminous than L* will allow us to test the
predictions of the hierarchical merging scenario for galaxy formation
in clusters at the highest available redshifts in galaxy clusters.

WFPC2 10807

The knotty jet of He 2-90: An ideal laboratory for studying the
formation and propagation of jets in dying stars

Previous WFPC2 observations have led to the serendipitous discovery of
an extended, highly-collimated, ``pulsed" bipolar jet emanating from a
compact planetary nebula, He 2- 90. Subsequently, an average proper
motion of the knots in the jet was measured, which together with
radial velocities, enabled us to characterise the basic physical
properties of the jet. The knotty jet in He 2-90 resembles other
prominent examples of pulsed jets in young stellar objects or
symbiotic stars, but is probably by far the best example yet of a
non-relativistic, symmetric, jet in a ``clean" astrophysical
environment. The formation {acceleration and collimation} of jets is
not fully understood, specially in the case of jets in dying stars. We
now propose to re-image He 2-90 with WFPC2 and exploit the factor 3.5
longer time baseline now available from the first-epoch observations
in September 1999, in order to measure the proper motion of individual
knots in the jet with unprecedented accuracy. These data will enable
us to characterise the ejection history of the source, specially
deviations from a constant period {latter is related to the binary
period of the system}, e.g., due to instabilities in the accretion
mechanism. We will also be able to test if the ejection mechanism is
symmetric: any deviation in the ejection history of the knots in the
opposing jet beams, will indicate a magnetic field structure and/or
the accretion disk which is not symmetric across the equatorial plane.
We will also carry out deep imaging with the ACS/WFC camera in order
to determine the shapes/sizes of a large number of knots. The
shapes/sizes of the knots, and changes with distance from the source
probe the strength of the magnetic field inside the jet. HRC imaging
of the central source and jet on sub-arcsecond scales will be carried
out to probe the magnetic field close to the jet source, and
deviations from linearity in the jet-beam which may result from
instabilities in the magnetic field. These data will allow us to
significantly improve our existing 2- dimensional MHD model of the
He2-90 jet, and/or provide impetus for new 3-dimensional models.

NIC2 10802

SHOES-Supernovae, HO, for the Equation of State of Dark energy

The present uncertainty in the value of the Hubble constant {resulting
in an uncertainty in Omega_M} and the paucity of Type Ia supernovae at
redshifts exceeding 1 are now the leading obstacles to determining the
nature of dark energy. We propose a single, integrated set of
observations for Cycle 15 that will provide a 40% improvement in
constraints on dark energy. This program will observe known Cepheids
in six reliable hosts of Type Ia supernovae with NICMOS, reducing the
uncertainty in H_0 by a factor of two because of the smaller
dispersion along the instability strip, the diminished extinction, and
the weaker metallicity dependence in the infrared. In parallel with
ACS, at the same time the NICMOS observations are underway, we will
discover and follow a sample of Type Ia supernovae at z 1. Together,
these measurements, along with prior constraints from WMAP, will
provide a great improvement in HST's ability to distinguish between a
static, cosmological constant and dynamical dark energy. The Hubble
Space Telescope is the only instrument in the world that can make
these IR measurements of Cepheids beyond the Local Group, and it is
the only telescope in the world that can be used to find and follow
supernovae at z 1. Our program exploits both of these unique
capabilities of HST to learn more about one of the greatest mysteries
in science.

NIC3 10792

Quasars at Redshift z=6 and Early Star Formation History

We propose to observe four high-redshift quasars {z=6} in the NIR in
order to estimate relative Fe/Mg abundances and the central black hole
mass. The results of this study will critically constrain models of
joint quasar and galaxy formation, early star formation, and the
growth of supermassive black holes. Different time scales and yields
for alpha-elements {like O or Mg} and for iron result into an iron
enrichment delay of ~0.3 to 0.6 Gyr. Hence, despite the well-known
complexity of the FeII emission line spectrum, the ratio iron/alpha -
element is a potentially useful cosmological clock. The central black
hole mass will be estimated based on a recently revised back hole mass
- luminosity relationship. The time delay of the iron enrichment and
the time required to form a supermassive black hole {logM8 Msol, tau
~0.5Gyr} as evidenced by quasar activity will be used to date the
beginning of the first intense star formation, marking the formation
of the first massive galaxies that host luminous quasars, and to
constrain the epoch when supermassive black holes start to grow by
accretion.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.)

HSTARS:

10733 - GSAcq (1,3,1) failed with STOP flag for FGS 1

During LOS the GSAcq scheduled at 23:03:48 failed.* At AOS the OBAD
RSS was 3.16 a-s.

10734 - GSAcq(2,1,1) failed to RGA Hold (Gyro Control)
**********
GSAcq(2,1,1) scheduled at 069/21:17:24 - 21:25:29 failed to RGA Hold
due to (QF2STOPF) stop flag indication on FGS2. Pre-acq OBADs showed
(RSS) attitude correction values of 3247.82 and 10.97 arcseconds.

10736 - GSAcq(2,3,2) results in fine lock backup (2,0,2)
***********
Upon acquisition of signal at 070/12:00:34, the GSAcq(2,3,2) scheduled
at 070/11:26:49 - 11:34:54 had resulted in fine lock backup (2,0,2)
using FGS2 due to (QF3STOPF) stop flag indication on the secondary
FGS3. Post-acq OBAD/MAP showed (RSS) value of 8.75.

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

*********************** SCHEDULED***** SUCCESSFUL*
FGS GSacq*************** 31***************** 29*****************
FGS REacq*************** 11***************** 10**************
OBAD with Maneuver 84******************
84**********************************

SIGNIFICANT EVENTS: (None)