Daily # 4310

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 # 4310

PERIOD COVERED: UT March 01, 2007 (DOY 060)

OBSERVATIONS SCHEDULED

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}.

ACS/SBC 11050

ACS UV contamination monitor

The observations consist of imaging and spectroscopy with SBC of the
cluster NGC 6681 in order to monitor the temporal evolution of the UV
sensitivity of the SBC.

ACS/SBC 11056

Improved Sensitivity SBC Prisms

The flux calibration of the SBC {PR110L and PR130L} will be improved
by observing for each prism white dwarf standards {WD1657+343 and
LTT9491}. The blue standard star WD1657+343 has previously been
observed with ACS/SBC and will serve as a reference point to track
time dependent variations. LTT9491 is much redder and thus will be
used to investigate the sensitivity curve of ?red? targets to check
for a potential red leak of the SBC. Additionally, LTT9491 shows
various strong absorption lines which can be used to confirm the
wavelength calibration of the PR110L and PR130L prisms. The standard
stars are observed at a variety of pointings across the SBC detector
in order to map spatial variations. LTT9491 will also be observed with
ACS/HRC PR200L to obtain an improved flux calibration from about 1800
A to 4000 A.

FGS 10931

Dynamical Masses and Radii of Four White Dwarf Stars

We will use FGS1R in its high angular resolution observing mode
(TRANS) to resolve the white dwarf binary systems. Each exposure will
be comprised of about 20 scans. The interferograms derived from each
scan will be cross- correlated and co-added to yield a high SNR. To
further surpress the noise (these targets are near the FGS's faint
limiting magnitude), the co-added inteferograms will be carefully
smoothed by being represented as a piece-wise We will use FGS1R in its
high angular resolution observing mode (TRANS) to resolve the white
dwarf binary systems. Each exposure will be comprised of about 20
scans. The interferograms derived from each scan will be
cross-correlated and co-added to yield a high SNR. To further surpress
the noise(these targets are near the FGS's faint limiting magnitude),
the co-added inteferograms will be carefully smoothed by being
represented as a piece-wise smooth segmanted polynomial. These
observations will yield the separation and position angle of the
binary components, as well as the brightness of each. In addition, the
binary and field stars simultaneously in the FGS FOV will be observed
in POS mode to accurately determine the relative positions of the
stars. This will facilitate the construction of an inertial reference
frame for the binary, thereby allowing the relative orbit that will be
ultimately determined from the TRANS data to be converted into a
physical orbit. This will allow us to determine the relative mass of
each white dwarf in the binarty system. In addition, the POS mode data
will give the proper motion and parallax of the binary, which will
allow us to compute the mass and radius of each white dwarf.

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.

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 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 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 11029

WFPC2 CYCLE 15 Intflat Linearity Check and Filter Rotation Anomaly
Monitor

Intflat observations will be taken to provide a linearity check: the
linearity test consists of a series of intflats in F555W, in each gain
and each shutter. A combination of intflats, visflats, and earthflats
will be used to check the repeatability of filter wheel motions.
{Intflat sequences tied to decons, visits 1-18 in prop 10363, have
been moved to the cycle 15 decon proposal xxxx for easier scheduling.}
Note: long-exposure WFPC2 intflats must be scheduled during ACS
anneals to prevent stray light from the WFPC2 lamps from contaminating
long ACS external exposures.

WFPC2 11096

Hubble Heritage imaging of Jupiter during the New Horizons encounter
HST Proposal 11096

WFPC2 images of Jupiter in Feb 2007 in support of New Horizons flyby
of Jupiter. This Hubble Heritage DD program is working in concert with
the existing GO programs by John Clarke {10862} and John Spencer
{10871}.

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

10723 - GSACQ(2,1,2) failed, Search Radius Limit Exceeded on FGS 2

GSACQ(2,1,2) at 060/11:52:07 failed due to Search Radius Limit
Exceeded on FGS 2 at 11:57:44.

10724 - GSAcq (2,1,1) results in Fine Lock Back-up (2,0,2)

At 061/02:29:23 GSAcq (2,1,1) scheduled from 061/02:26:00-02:33:12
resulted in Fine Lock Back-up (2,0,2) using FGS 2, due to (QF1STOPF)
stop flag indication on the secondary FGS.
OBAD #1 RSS: 755.71
OBAD #2 RSS: 12.44

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL

FGS GSacq 12 12
FGS REacq 02 02
OBAD with Maneuver 28 28

SIGNIFICANT EVENTS: (None)