HST Daily Report #3270
DAILY REPORT # 3270
PERIOD COVERED: DOY 364
OBSERVATIONS SCHEDULED
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.
STIS/CCD/MA2 9116
Understanding High-Redshift and Starburst Galaxies: A UV Spectroscopic
Survey of
B- Stars in the SMC.
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to construct
a
high quality spectral library at low metallicity in order to synthesize the
UV
spectra of high redshift star-forming galaxies and nearby starbursts.
WF/PC-2 9345
Fundamental Properties of L-type Dwarfs in Binaries.
The WF/PC-2 was used to characterize the physical properties of eight
L-dwarfs
in four binary systems. The goal is to obtain astrometric, photometric and
spectroscopic measurements of each component that will yield basic
information
on their atmospheric and dynamical properties.
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.
NICMOS 9484
The NICMOS Parallel Observing Program
We propose to manage the default set of pure parallels with NICMOS. Our
experience with both our GO NICMOS parallel program and the public parallel
NICMOS programs in cycle 7 prepared us to make optimal use of the parallel
opportunities. The NICMOS G141 grism remains the most powerful survey tool
for
HAlpha emission-line galaxies at cosmologically interesting redshifts. It is
particularly well suited to addressing two key uncertainties regarding the
global history of star formation: the peak rate of star formation in the
relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star
formation missing from UV continuum-based estimates due to high extinction.
Our
proposed deep G141 exposures will increase the sample of known HAlpha
emission-
line objects at z ~ 1.3 by roughly an order of magnitude. We will also
obtain a
mix of F110W and F160W images along random sight-lines to examine the space
density and morphologies of the reddest galaxies. The nature of the
extremely
red galaxies remains unclear and our program of imaging and grism
spectroscopy
provides unique information regarding both the incidence of obscured star
bursts and the build up of stellar
mass at intermediate redshifts. In addition to carrying out the parallel
program
we will populate a public database with calibrated spectra and images, and
provide limited ground- based optical and near-IR data for the deepest
parallel
fields.
STIS/ACS 9498
The Nature of the Close Binary Quasar LBQS 0103-2753
We propose STIS spectroscopic and ACS imaging observations of the
small–separation quasar pair LBQS 0103-2753 A/B {= CT 344}. This quasar
pair
with z = 0.85, has a projected separation of only 0.3 arcsec or 2.3 kpc. The
brighter member of the pair {V = 18.2} is a BAL quasar while the fainter {V
=
19.4} is a quasar at a similar redshift without BALs. It is very likely
that the
two quasars are a binary quasar, and not a chance superposition along the
line
of sight or a gravitational lens {Junkkarinen et al. 2001}. The goals of the
STIS spectroscopic observations are to accurately measure the systemic
redshifts
and redshift difference, to search for variability, and to quantify the
emission
line differences between the two quasars. Deep ACS WFC images, in the F606W
and
F814W filters, will be used to provide information on the host galaxy
morphologies, to look for the signatures of a merger/interaction — in
particular disturbed isophotes and tidal tails, and to study any cluster of
galaxies around this quasar pair. These observations will test the lensing
versus binary hypothesis and help differentiate between merging and a high
relative velocity galaxy–galaxy interaction. Studies of binary quasars with
such close separations will put constraints on merger timescales and duty
cycles
for AGN fueling at these separations.
WFPC2 9592
WFPC2 CYCLE 11 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 9593
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt1/3
This dark calibration program obtains 3 dark frames every day to provide
data
for monitoring and characterizing the evolution of hot pixels.
WFPC2 9596
WFPC2 CYCLE 11 INTERNAL MONITOR
This calibration proposal is the Cycle 11 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.
STIS 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9607
CCD Bias Monitor – Part 1
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and
1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.
STIS 9615
Cycle 11 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 9634
POMS Test Proposal: WFII targeted parallel archive proposal
The parallel opportunities available with WFPC2 in the neighborhood of
bright
galaxies are treated in a slightly different way from the normal pure
parallels.
Local Group galaxies offer the opportunity for a closer look at young
stellar
populations. Narrow-band images in F656N can be used both to identify young
stars via their emission lines, and to map the gas distribution in
star-forming
regions. Thus, the filter F656N is added to the four standard filters. Near
more
distant galaxies, up to about 10 Mpc, we can map the population of globular
clusters; for this purpose, F300W is less useful, and only F450W, F606W, and
F814W will be used.
ACS 9647
CCD Daily Monitor Part I
for any source of noise in ACS CCD detectors. This programme will be
executed
once a day for the entire lifetime of ACS.
ACS 9660
Earth Bright Limb Calibration
The proposal will determine whether there are any scattered light problems
for
ACS as the bright limb of the Earth is approached, and measure the
background
light level as a function of limb angle. Potential impact is primarily the
definition of the CVZ and hence duration of CVZ availability.
WFPC2 9676
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.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle 10.
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 06 06 FGS REacq 08 08 FHST Update 10 10 LOSS of LOCK
SIGNIFICANT EVENTS: None
