Daily 3841

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 3841

PERIOD COVERED: DOY 108

OBSERVATIONS SCHEDULED

ACS 10140

Identification of a magnetic anomaly at Jupiter from satellite
footprints

Repeated imaging of Jupiter's aurora has shown that the northern main
oval has a distorted 'kidney bean' shape in the general range of
90-140? System III longitude, which appears unchanged since 1994.
While it is more difficult to observe the conjugate regions in the
southern aurora, no corresponding distortion appears in the south.
Recent improved accuracy in locating the satellite footprint auroral
emissions has provided new information about the geometry of Jupiter's
magnetic field in this and other areas. The study of the magnetic
field provides us with insight into the state of matter and the
dynamics deep down Jupiter. There is currently no other way to do this
from orbit. The persistent pattern of the main oval implies a
disturbance of the local magnetic field, and the increased latitudinal
separation of the locus of satellite footprints from each other and
from the main oval implies a locally weaker field strength. It is
possible that these phenomena result from a magnetic anomaly in
Jupiter's intrinsic magnetic field, as was proposed by A. Dessler in
the 1970's. There is presently only limited evidence from the scarcity
of auroral footprints observed in this longitude range. We propose to
obtain HST UV images with specific observing geometries of Jupiter to
determine the locations of the auroral footprints of Io, Europa, and
Ganymede in cycle 13 to accurately determine the magnetic field
geometry in the suggested anomaly region, and to either confirm or
refute the suggestion of a local magnetic anomaly.

ACS/HRC 10391

Wavelength and Flux Calibration of the ACS prisms

The wavelength calibration of the SBC {PR110L and PR130L} and HRC
{PR200L} prisms will be established by observing a planetary nebula in
the LMC and QSOs at carefully selected redshifts. Flux calibrations
will be derived for each prism by observing white dwarf standards.

ACS/HRC/WFC 10370

CCD Hot Pixel Annealing

Hot pixel annealing will continue to be performed once every 4 weeks.
The CCD TECs will be turned off and heaters will be activated to bring
the detector temperatures to about +20C. This state will be held for
approximately 12 hours, after which the heaters are turned off, the
TECs turned on, and the CCDs returned to normal operating condition.
To assess the effectiveness of the annealing, a bias and four dark
images will be taken before and after the annealing procedure for both
WFC and HRC. The HRC darks are taken in parallel with the WFC darks.
The charge transfer efficiency {CTE} of the ACS CCD detectors declines
as damage due to on-orbit radiation exposure accumulates. This
degradation has been closely monitored at regular intervals, because
it is likely to determine the useful lifetime of the CCDs. We will now
combine the annealling activity with the charge transfer efficiency
monitoring and also merge into the routine dark image collection. To
this end, the CTE monitoring exposures have been moved into this
proposal . All the data for this program is acquired using internal
targets {lamps} only, so all of the exposures should be taken during
Earth occultation time {but not during SAA passages}. This program
emulates the ACS pre-flight ground calibration and post-launch SMOV
testing {program 8948}, so that results from each epoch can be
directly compared. Extended Pixel Edge Response {EPER} and First Pixel
Response {FPR} data will be obtained over a range of signal levels for
both the Wide Field Channel {WFC}, and the High Resolution Channel
{HRC}.

ACS/HRC/WFC 10389

ACS CCDs daily monitor - Cycle 13 - Part 2

This program consists of a set of basic tests to monitor, the read
noise, the development of hot pixels and test for any source of noise
in ACS CCD detectors. The files, biases and dark will be used to
create reference files for science calibration. This programme will be
for the entire lifetime of ACS.

ACS/HRC/WFC 10399

Accurate and Robust Calibration of the Extragalactic Distance Scale
with the Maser Galaxy NGC4258 II

The extragalactic distance scale {EDS} is defined by a comparison of
Cepheid Period- Luminosity {PL} relations for nearby galaxies and the
LMC, whose uncertain distance is thereby the SOLE anchor. Studies of
masers orbiting the central black hole in NGC4258 have provided the
most accurate extragalactic distance ever {7.2+/-0.5 Mpc}, and new
radio data and analysis techniques will reduce the uncertainty to
3.5% {0.07 mag} by 2005. Since this distance is well determined and
based on geometric arguments, NGC4258 can provide a much needed new
anchor for the EDS. Ultimately, the combination of an independent
measurement of H0 and measurements of CMB fluctuations {e.g., WMAP}
can be used to directly constrain cosmological parameters including
the equation of state of dark energy. In our Cycle 12 proposal, we
defined a program spanning two cycles. The Cycle 12 portion was
accepted. We have acquired WFC images and are constructing well
sampled PL relations in 3 colors {BVI}. The purpose of the Cycle 13
observations is to address systematic sources of error and is crucial
for the success of the entire program. To disentangle the effects of
reddening and metallicity, and to characterize the effects of
blending, we require 50 orbits to obtain H-band photometry
{NICMOS/NIC2} and high resolution images {ACS/HRC}.

ACS/HRC/WFC 10436

Black Hole Growth and the Black Hole Mass -- Bulge Relations for AGNs

Recent work has shown that the mass of a black hole is tightly
correlated with the bulge mass of its host galaxy. This relation needs
to be understood in the context of black hole growth in its active
phase. Highly accreting AGNs, like narrow line Seyfert 1 galaxies
{NLS1s}, are found to lie below the black hole mass -- bulge velocity
dispersion correlation of normal galaxies and broad line AGNs. This
result was obtained using FWHM{[OIII]} as a surrogate for the bulge
velocity dispersion. To test this result we propose to obtain high
resolution images of 10 NLS1s that do not lie on the black hole
mass--sigma relation and measure accurate bulge parameters {luminosity
and effective radius}. We will obtain an alternate handle on the bulge
velocity dispersion through the fundamental plane relations and also
find the locus of these NLS1s on the black hole mass--bulge luminosity
plane. Testing this result is crucial to understanding the role of
accretion on black hole growth, the observed correlations of the black
hole mass with the bulge, and the formation and evolution of galaxies.

ACS/WFC 10369

ACS internal CTE monitor

The charge transfer efficiency {CTE} of the ACS CCD detectors will
decline as damage due to on-orbit radiation exposure accumulates. This
degradation will be closely monitored at regular intervals, because it
is likely to determine the useful lifetime of the CCDs. All the data
for this program is acquired using internal targets {lamps} only, so
all of the exposures should be taken during Earth occultation time
{but not during SAA passages}. This program emulates the ACS
pre-flight ground calibration and post-launch SMOV testing {program
8948}, so that results from each epoch can be directly compared.
Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
data will be obtained over a range of signal levels for both the Wide
Field Channel {WFC}, and the High Resolution Channel {HRC}.

ACS/WFC 10412

The host galaxies of dust-reddened quasars

We have used the 2MASS near-infrared and FIRST radio surveys, together
with the Palomar Observatory Sky Survey plates to select a sample of
dust-reddened, radio- intermediate quasars. We wish to use ACS to
study the host galaxies of these quasars. The dust reddening of the
quasars makes it possible to study the hosts at rest-frame optical-UV
wavelengths much more easily than the hosts of normal quasars of
similar bolometric luminosity. Our study will compare the hosts of our
dust-reddened quasars to those of normal quasars from the HST archive
to test the hypothesis that dust-reddened quasars are young objects,
whose hosts still show morphological evidence of recent merger events
which triggered the quasar.

FGS 10104

Calibrating the Mass-Luminosity Relation at the End of the Main
Sequence

We propose to use HST-FGS1R to calibrate the mass-luminosity relation
{MLR} for stars less massive than 0.2 Msun, with special emphasis on
objects near the stellar/brown dwarf border. Our goals are to
determine M_V values to 0.05 magnitude, masses to 5 than double the
number of objects with masses determined to be less than 0.20 Msun.
This program uses the combination of HST-FGS3/FGS1R at optical
wavelengths and ground-based infrared interferometry to examine
nearby, subarcsecond binary systems. The high precision measurements
with HST-FGS3/FGS1R {to 1 mas in the separations} for these faint
targets {V = 10--15} simply cannot be equaled by any ground based
technique. As a result of these measurements, we are deriving high
quality luminosities and masses for the components in the observed
systems, and characterizing their spectral energy distributions from
0.5 to 2.2 Mum. Several of the objects included have M 0.1 Msun,
placing them at the very end of the stellar main sequence. Three of
the targets are brown dwarf candidates, including the current low mass
record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The
payoff of this proposal is high because all 10 of the systems selected
have already been resolved with HST- FGS3/FGS1R during Cycles 5--10
and contain most of the reddest objects for which masses can be
determined.

NIC2 10418

Morphologies and Color Gradients of Galaxies with the Oldest Stellar
Populations at High Redshifts We have isolated a sample of 9 luminous
{~2L*} galaxies with the very oldest stellar populations at their
respective redshifts. The galaxies have been found in radio-source
fields chosen to be at the key redshifts z~1.5 and z~2.5, which allow
the cleanest separation of old stellar populations from highly
reddened starbursts with colors derived from standard filter
combinations. Ground-based observations in excellent seeing and with
adaptive optics of 3 of these galaxies indicate that all 3 are
dominated by well relaxed disks of old stars, suggesting that the
first large stellar systems to form in the universe were disks in
which star formation proceeded extremely rapidly and efficiently. In
order to test this conjecture, we are requesting NICMOS2 exposures of
our sample to obtain high S/N imaging in the F160W filter to determine
detailed morphologies of the old stellar population, coupled with
either NICMOS2 F110W or ACS F814W exposures {depending on redshift} to
determine color gradients and/or other systematic color variations
that might provide clues to formation processes.

WFPC2 10359

WFPC2 CYCLE 13 Standard Darks

This dark calibration program obtains dark frames every week in order
to provide data for the ongoing calibration of the CCD dark current
rate, and to monitor and characterize the evolution of hot pixels.
Over an extended period these data will also provide a monitor of
radiation damage to the CCDs.

WFPC2 10363

WFPC2 CYCLE 13 Intflat and Visflat Sweeps and Filter Rotation Anomaly
Monitor

Using intflat observations, this WFPC2 proposal is designed to monitor
the pixel-to-pixel flatfield response and provide a linearity check.
The intflat sequences, to be done once during the year, are similar to
those from the Cycle 12 program 10075. The images will provide a
backup database as well as allow monitoring of the gain ratios. The
sweep is a complete set of internal flats, cycling through both
shutter blades and both gains. The linearity test consists of a series
of intflats in F555W, in each gain and each shutter. As in Cycle 12,
we plan to continue to take extra visflat, intflat, and earthflat
exposures to test the repeatability of filter wheel motions.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.) None

COMPLETED OPS REQs: None

OPS NOTES EXECUTED: None

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS Gsacq 12 12
FGS Reacq 6 6
FHST Update 20 20
LOSS of LOCK



SIGNIFICANT EVENTS: None