Daily 3500

HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3500

PERIOD COVERED: DOY 335

OBSERVATIONS SCHEDULED

10033

MAMA Sensitivity and Focus Monitor Cycle 12

Monitor sensitivity of each MAMA grating mode to detect any change due
to contamination or other causes. Also monitor the STIS focus in a
spectroscopic and an imaging mode.

ACS 9984

Cosmic Shear With ACS Pure Parallels

Small distortions in the shapes of background galaxies by foreground
mass provide a powerful method of directly measuring the amount and
distribution of dark matter. Several groups have recently detected
this weak lensing by large-scale structure, also called cosmic shear.
The high resolution and sensitivity of HST/ACS provide a unique
opportunity to measure cosmic shear accurately on small scales. Using
260 parallel orbits in Sloan textiti {F775W} we will measure for the
first time: beginlistosetlength sep0cm setlengthemsep0cm setlength
opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the
skewness of the shear distribution, and em the magnification effect.  
endlist Our measurements will determine the amplitude of the mass
power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20,
and the mass density Omega_m with s/n=4. They will be done at small
angular scales where non-linear effects dominate the power spectrum,
providing a test of the gravitational instability paradigm for
structure formation. Measurements on these scales are not possible
from the ground, because of the systematic effects induced by PSF
smearing from seeing. Having many independent lines of sight reduces
the uncertainty due to cosmic variance, making parallel observations
ideal.

ACS/HRC/WFC 10042

CCD Daily Monitor

This program consists of basic tests to monitor, the read noise, the
development of hot pixels and test for any source of noise in ACS CCD
detectors. This programme will be executed once a day for the entire
lifetime of ACS.

ACS/WFC 10046

CCD Hot Pixel Annealing

Hot pixel annealing will 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 this procedure, a bias and two dark images will be
taken after the annealing procedure for both WFC and HRC. The HRC
darks are taken in parallel with the WFC darks.

ACS/WFC 9744

HST Imaging of Gravitational Lenses

Gravitational lenses offer unique opportunities to study cosmology,
dark matter, galactic structure, galaxy evolution and quasar host
galaxies. They are also the only sample of galaxies selected based on
their mass rather than their luminosity or surface brightness. While
gravitational lenses can be discovered with ground-based optical and
radio observations, converting them into astrophysical tools requires
HST. HST has demonstrated that it is the only telescope that can in
each case precisely locate the lens galaxy, measure its luminosity,
color and structure, and search for lensed images of the source host
galaxy given the typical image separations of ~1''. We will obtain
ACS/WFC V and I images and NICMOS H images of 21 new lenses never
observed by HST and NICMOS H images of 16 lenses never observed by HST
in the IR. As in previous cycles, we request that the data be made
public immediately.

NIC/NIC3 9865

The NICMOS Parallel Observing Program

We propose to continue managing the NICMOS pure parallel program.
Based on our experience, we are well prepared to make optimal use of
the parallel opportunities. The improved sensitivity and efficiency of
our observations will substantially increase the number of
line-emitting galaxies detected. As our previous work has
demonstrated, the most frequently detected line is Halpha at
0.7<z<1.9, which provides an excellent measure of current star
formation rate. We will also detect star-forming and active galaxies
in other redshift ranges using other emission lines. The grism
observations will produce by far the best available Halpha luminosity
functions over the crucial--but poorly observed--redshift range where
galaxies appear to have assembled most of their stellar mass. This key
process of galaxy evolution needs to be studied with IR data; we found
that observations at shorter wavelengths appear to have missed a large
fraction of the star-formation in galaxies, due to dust reddening. We
will also obtain deep F110W and F160W images, to examine the space
densities and morphologies of faint red galaxies. In addition to
carrying out the public parallels, we will make the fully reduced and
calibrated images and spectra available on-line, with some
ground-based data for the deepest parallel fields included.

NIC1/NIC2/NIC3 9995

Photometric Stability

This NICMOS calibration proposal carries out photometric monitoring
observations during Cycle 12. The format of the program is identical
to that of the Cycle 11 program 9639, except that the frequency has
been reduced to bimonthly.

NIC2 9726

A NICMOS search for obscured supernovae in starburst galaxies

Recent near-IR monitoring campaigns were successful in detecting
obscured supernovae {SNe} in starburst galaxies. The inferred SN rate
is much higher than that obtained in previous optical campaigns, but
it is still significantly lower than expected by the high level star
formation of these systems. One possible explanation for the shortage
of SNe is that most of them occur in the nuclear region, where the
limited angular resolution of groundbased observations prevents their
detection. We propose NICMOS SNAP observations of a sample of
starburst galaxies already observed once by NICMOS, with the goal of
exploiting its sensitivity and angular resolution to detect nuclear
obscured SNe which might have been missed by groundbased surveys.
These observation will allow to assess the real SN rate in starbust
galaxies and deliver a sample of SN occurring in the extreme
environment of galactic nuclei. We expect to detect more than 55 SNe
{if the whole sample is observed}. If the number of SNe detected in
the program is much lower than expected it would prompt for a revision
of our understanding of the relation between the star formation rate
and the SN rate.

NIC2 9834

Finding Planets in the Stellar Graveyard: A Faint Companion Search of
White Dwarfs with NICMOS

We propose to do a deep search for substellar objects in orbit around
white dwarfs with the newly refurbished NICMOS camera as part of the
PI's doctoral thesis work. Direct imaging of planets around main
sequence stars is difficult due to the large contrast ratio, a problem
which is much less severe for companions to white dwarfs. White dwarfs
are not usually considered in planet searches but recent theoretical
work and observations are motivating new searches for planetary
systems and dust disks around DAZ white dwarfs. We propose to conduct
the search with the NIC2 coronagraph to find resolved companions and
do photometry to search for unresolved companions through Near-IR
excesses. We estimate that the survey will be sensitive to brown
dwarfs, high mass jovian planets, and dust disks. By probing a wide
range of orbital separations and companion masses, this survey will
help to answer questions about the brown dwarf desert, common envelope
evolution, and planet formation. HST and NICMOS provide a unique
capability to do this search, as no ground based observatory with AO
can adequately search for faint companions as close and with such high
contrast.

NIC2 9856

A near-IR imaging survey of submm galaxies with spectroscopic redshifts

Submillimeter {submm} surveys with SCUBA have identified a population
of obscured star-forming and active galaxies at high redshift. Our
recent spectroscopic campaigns with the Keck-10m telescope have
uncovered redshifts for 37 SCUBA galaxies. The wide redshift range of
the radio identified submm population {z=1-4} implies that many
varieties of sources driven by different physical processes may be
selected in a submm survey. Only HST observations have the resolution
to detect any changes in the morphologies of SCUBA galaxies with
increasing cosmic time. We propose to use HST-NICMOS, ACS to obtain
2-filter images of a sample of 15 SCUBA galaxies with redshifts
spanning z=0.8-3.5. Our goal is to understand what physical process
{major mergers?} drive their strong evolution and great luminosities,
and what the implications are for galaxy evolution models.

NICMOS 8790

NICMOS Post-SAA calibration - CR Persistence Part 1.

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.

NICMOS 9424

Externally Illuminated Circumstellar Material in the Young Nebulous
Cluster NGC 2024

HST imaging of the Orion M42 H II region has revealed circumstellar
emission and absorption regions {``proplyds''} with sizes comparable
to those expected for protoplanetary disks. Disk morphology is
directly observed in a dozen cases; disk photoevaporation is now the
working model to explain the ionized rims seen at more than 100
Trapezium cluster stars. Are the Trapezium circumstances unique?
Different cluster ages, densities, and UV radiation fields may
strongly affect proplyd characteristics. To address these questions,
we have searched for proplyds in several other young nebulous
clusters, and found that the embedded infrared cluster associated with
the NGC 2024 H II region has a large group of strong proplyd
candidates. Our WFPC2 images of the optically visible edge of the
cluster have identified an HAlpha proplyd aligned toward a B0 star.
Our VLA 3.6 cm maps show compact ionization regions coincident with 20
members of the infrared cluster - a result similar to the original VLA
proplyd discovery in M42 by Churchwell {1987}. These results strongly
indicate that infrared emission line imaging of selected cluster
members should reveal many objects similar to the those in M42. We
propose NIC2 Paschen Alpha and continuum imaging of fourteen of the
NGC 2024 compact VLA sources. Our goal is to resolve and characterize
their circumstellar structures, and compare them with those seen in
M42.

STIS 9435

Systematic Search for Rotation at the Base of Outflows from T Tauri
Stars

We wish to search for rotation signatures in the initial portion
{first 100 AU} of a sample of outflows emanating from T Tauri stars
{TTSs}. This project originates from our detection of systematic
transverse radial velocity shifts in STIS spectra of the DG Tau jet
{Bacciotti et al., 2002}. The shifts, observed in a region where the
flow is already collimated, but has not yet manifestly interacted with
its environment, are consistent with the predictions of magneto-
centrifugal launching models, and may constitute the first observed
indication for rotation in the initial portion of a jet flow. Rotation
is a fundamental ingredient in star formation theories, thus we
propose to confirm the above result by carrying out a systematic
survey in similar flows. We plan to take for each jet a STIS spectrum
in the 6300 -- 6800 Angstrom range, with the slit perpendicular to the
flow direction and at a distance of about 0.''3 from the source {i.e.,
in our targets, 40 -- 70 AU along the jet depending on inclination
angle}. Since the flows are resolved transversely with HST, the
proposed slit orientation allows for the direct detection of
systematic velocity shifts.  Where found, we will check for
consistency between the sense of rotation observed and that of the
underlying disk through CO interferometric measurements. As a
by-product, estimates of the excitation conditions across the flow
{including ionization fraction} and of the mass outflow rates will be
derived.

STIS/CCD 10000

STIS Pure Parallel Imaging Program: Cycle 12

This is the default archival pure parallel program for STIS during
cycle 12.

STIS/CCD 10017

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD.

STIS/CCD 10019

CCD Bias Monitor - Part 1

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1,
and 1x1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.

STIS/CCD/MA2 9807

Rotation in Jets from Young Stars: investigating NUV lines with very
high Spectral Resolution

Optical STIS spectra of the jets from DG Tau, RW Aur, TH 28 and LkHa
231 obtained by us {prop IDs. 7311, 9435} show systematic transverse
radial velocity shifts in the region where the flow has just been
accelerated and collimated {Bacciotti et al, 2002}, i.e. within about
100 AU from the source. We interpret such shifts as evidence for jet
rotation. Whether YSO jets rotate is a fundamental question in star
formation because it has been suggested that jets might be the way
excess angular momentum is removed from the star/disk system, thereby
allowing the star to accrete. In particular it is important to know if
observed toroidal velocities are in agreement with predictions of
magneto-centrifugal jet launching models. The limited spatial and
spectral resolution of STIS in the optical however, only allows one to
say qualitatively that the observed rotational velocities are in rough
agreement with theory. Moreover only the resolved peripheral regions
of the flow can be studied.  We are proposing here to exploit the
higher spatial and spectral resolution of STIS in the NUV to measure
transverse jet velocity profiles.This is a task which can only be
undertaken by the HST and which is ideally suited to the STIS. To
measure the velocity profiles, we will observe the Mg II doublet at
2800 Angstrom {using the E230M echelle and the 6 X 0.2 slit transverse
to the flow}. In comparison to the optical, the NUV affords us double
the spatial resolution and we will be able to detect velocity
differences across the jet down to 2 km/s. Not only should we be able
to determine for the first time the detailed rotational velocity
profile across a jet but we also expect to spatially resolve the high
velocity axial core of the jet in the NUV. Finally we add that as very
few NUV observations of the initial jet beam of YSO jets are
available, our datasets should be a valuable contribution to the HST
archive.

STIS/MA1 10034

Cycle 12 MAMA Dark Monitor

This test performs the routine monitoring of the MAMA detector dark
noise. This proposal will provide the primary means of checking on
health of the MAMA detectors systems through frequent monitoring of
the background count rate. The purpose is to look for evidence of
change in dark indicative of detector problem developing.

WFPC2 10068

WFPC2 CYCLE 12 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 10069

WFPC2 CYCLE 12 Supplemental Darks, Part 1/3

This dark calibration program obtains 3 dark frames every day to
provide data for monitoring and characterizing the evolution of hot
pixels.

WFPC2 10072

WFPC2 CYCLE 12 INTERNAL MONITOR

This calibration proposal is the Cycle 12 routine internal monitor for
WFPC2, to be run weekly to monitor the health of the cameras. A
variety of internal exposures are obtained in order to provide a
monitor of the integrity of the CCD camera electronics in both bays
{gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a
monitor for possible buildup of contaminants on the CCD windows.

WFPC2 10073

Earth Flats

This proposal monitors flatfield stability. This proposal obtains
sequences of Earth streak flats to construct high quality flat fields
for the WFPC2 filter set. These flat fields will allow mapping of the
OTA illumination pattern and will be used in conjunction with previous
internal and external flats to generate new pipeline superflats. These
Earth flats will complement the Earth flat data obtained during cycles
4-11.

WFPC2 10082

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans

WFPC2 9709

POMS Test Proposal: WFII parallel archive proposal

This is the generic target version of the WFPC2 Archival Pure Parallel
program. The program will be used to take parallel images of random
areas of the sky, following the recommendations of the 2002 Parallels
Working Group.

WFPC2 9968

Fundamental properties of L-type dwarfs in binaries

We propose to characterize the physical properties of eight L-dwarfs
in four binary systems. Our goal is to obtain astrometric, photometric
and spectroscopic measurements of each component that will yield basic
information on their atmospheric and dynamical properties. The high
angular resolution of HST is essential because all these systems have
angular separations $le$0.5 arcsec. They do not have bright enough
stars nearby that can be used for natural guide adaptive optics in
ground-based telescopes. In Cycles~10 and 11 we propose to obtain
WFPC2 and STIS data, allowing the determination of parallax, proper
motion, position and spectral type for each component. In Cycle 12 we
plan to obtain additional WFPC2 images for follow-up of the orbital
motion and refinement of parallax and proper motion. We will also
monitor possible intrinsic photometric variability in two filters
{F675W and F814W}. The STIS observations will provide spectral types,
gravity sensitive indicators, and chromospheric activity {H$_lpha$
emission} for each component. These 4 systems will constitute
benchmarks for determining dynamical masses of L dwarfs, and inferring
the age-mass-spectral type relationship of this new spectral class.

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:
1176-0 - HST486 Software Memory Dump - RAM @ 335/2210z and 336/0608z

                         SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq             12                       12
FGS REacq             6                          6
FHST Update           23                        23
LOSS of LOCK


SIGNIFICANT EVENTS: None