NASA Hubble Space Telescope Daily Report #3444
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3444
PERIOD COVERED: DOY 252
OBSERVATIONS SCHEDULED
ACS 9650
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 WFC
detector temperature to about +10C. The HRC temperature will reach
about 30C.This state will be held for approximately 24 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 before and
after the annealing procedure for both WFC and HRC.
ACS 9675
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 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.
ACS/WFC/HRC 9696
Hubble Heritage observations of NGC 3370
Hubble Heritage proposes to observe NGC 3370 in conjunction with GO
program 9351 {PI Adam Riess} to use the combined data to produce a
three color image.
NIC1 9833
T Dwarf Companions: Searching for the Coldest Brown Dwarfs
Faint companions to known stars have historically led to the discovery
of new classes of stellar and substellar objects. Because these
discoveries are typically limited by the flux ratio of the components
in the system, the intrinsically faintest companions are most
effectively identified around the intrinsically faintest primaries. We
propose to use NICMOS to image a sample of 22 of the coolest known
{T-type} brown dwarfs in the Solar Neighborhood in order to search for
fainter and cooler brown dwarf companions. The high spatial resolution
of the NIC 1 detector enables us to distinguish binary systems with
apparent separations greater than 0″08, or physical separations
greater than 1.2 AU at the nominal distances of the objects in our
sample. Furthermore, the substantial sensitivity of NICMOS imaging
allows us to probe companion masses of 5-50 Jupiter masses and
companion effective temperatures of 250-1300 K in a maximally
efficient manner. Based on work to date, we expect that roughly 20% of
the objects in our sample will be binary, and that one or two of these
will likely harbor a significantly fainter secondary. Hence, we expect
to find a companion cooler than any currently known brown dwarf, a
potential prototype for the next spectral class. In addition, our
investigation will add substantially to the sample of known binary
brown dwarfs, allowing improved statistical analyses of the binary
fraction, separation distribution, and mass ratio distribution of
these systems, key quantities for probing brown dwarf formation. We
will also identify optimal substellar systems for astrometric mass
measurements, a critical check for theoretical models of brown dwarfs
and extrasolar planets.
NIC2 9875
The Fundamental Plane of Massive Gas-Rich Mergers
We propose deep NICMOS H-band imaging of a carefully selected sample
of 33 luminous, late-stage galactic mergers. This program is part of a
comprehensive investigation of the most luminous mergers in the nearby
universe, the ultraluminous infrared galaxies {ULIGs}. The
high-resolution HST images will complement an extensive set of
ground-based data that include long-slit NIR spectra from a recently
approved Large VLT Programme. This unique dataset will allow us to
derive with unprecedented precision structural -and- kinematic
parameters for a large unbiased sample of objects spanning the entire
ULIG luminosity function. These data will refine the fundamental plane
of massive gas-rich mergers and enable us to answer the following
questions: {1} Do ultraluminous mergers form elliptical galaxies, and
in particular, giant ellipticals? {2} Do ULIGs evolve into optically
bright QSOs? The results from this detailed study of massive mergers
in the local universe will be relevant to understanding galaxy
formation and evolution at earlier epochs, and in particular, the
dusty sub-mm population that accounts for more than half of the star
formation at z > 1.
NIC3/ACS/HRC/WFC 9803
Deep NICMOS Images of the UDF
The ACS Ultra Deep Field {UDF} images will greatly enhance the rich
suite of deep multi-wavelength images in the Chandra Deep Field South
{CDF–S}. We propose to complete the image set with deep near-IR
NICMOS images at 1.1 and 1.6 microns over a significant fraction of
the UDF, providing a critical link between the HST ACS and SIRTF
observations. The timely addition of the near-IR images ensures that
investigators will have images that span the spectrum from X-ray to
far IR. In recognition of the value of the near IR images this
proposal is submitted as a Treasury proposal with no proprietary
period. The proposal team will deliver science quality images,
mosaiced images covering 4.9 sq arc min, and a photometric catalog
complete to an AB mag of 28.2 in both the F110W and F160W filters. The
program also delivers a parallel extremely deep ACS field, 8′ away,
that reaches to within 0.6 mag of the UDF in the same filters as the
UDF. The scientific program of the proposal team focuses on the star
formation history of the universe, evolved galaxies at high redshift,
galaxies at the epoch of reionization, and the redshift evolution of
AGNs and ULIRGs. The HDF-N is currently the only field with
spatially-coincident deep HST imaging in both the optical and near-IR.
The small size of the HDF-N means that large scale structure is the
dominant error in the results from the HDF-N. Providing observations
in a field that is spatially uncorrelated is critically important. The
UDF/CDF-S fulfills that goal. The depth of the UDF ACS imaging, and
the wealth of Great Observatory and ground based observations in the
CDF-S, make these NICMOS observations uniquely valuable. An
extraordinarily rich array of science opportunities await the
community from the NICMOS UDF data.
NICMOS 8791
NICMOS Post-SAA calibration – CR Persistence Part 2
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.
NICMOS 9640
Flats Stability
This calibration proposal is the Cycle 11 NICMOS monthly monitor A
series of camera 1, 2, & 3 flat fields will be obtained to monitor the
health of the cameras.
STIS 9608
CCD Bias Monitor – Part 2
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/CCD 10000
STIS Pure Parallel Imaging Program: Cycle 12
This is the default archival pure parallel program for STIS during
cycle 12.
STIS/CCD 9866
First Spectroscopic Study of a Unique Set of Young Stars in the Orion
Nebula
We propose to obtain the first spectra of the central stars of Orion
proplyds for which the stars are visible in WFPC images. While it is
known that the central stars are broadly late-type, they have never
been spectrally classified or studied in detail as pre-MS objects. The
Orion proplyds are generally thought to be protoplanetary disks
similar to the primordial disk of the Solar System. They offer a
unique opportunity to understand the physical conditions of
protoplanetary disks in a nebular environment generally believed to be
typical of that in which most stars formed. Models of the proplyds are
available which predict the observable IR spectral energy distribution
using the spectral type of the central star as part of the numerical
input. Further progress in understanding proplyds will require
knowledge of the spectral types of these stars. We will use
already-proven diagnostics for spectrally classifying late-type PMS
stars. In addition, many emission lines are expected in objects of
this age which can be used to look for infall and outflow. Different
accretion models of young stars predict different line widths, so our
observations can help test models of late-type pre-MS stars and can be
used to compare as pre-MS objects the proplyd stars with other pre-MS
stars.
WFPC2 9595
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt3/3
This dark calibration program obtains 3 dark frames every day to
provide data for monitoring and characterizing the evolution of hot
pixels.
WFPC2 9712
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS
Survey Fields
In anticipation of the allocation of ACS high-latitude imaging
WFPC2 9729
Probing the nature of Type Ia SNe through HST astrometry
Type Ia supernovae are of key importance in cosmology. Empirical
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
HSTAR 9143: GS Re-acquisition (2,3,2) requires two attempts to
COMPLETED OPS REQs:
OPS NOTES EXECUTED:
survey{s}, we request a modification of the default pure parallel
program for those WFPC2 parallels that fall within the ACS survey
field. Rather than duplicate the red bands which will be done much
better with ACS, we propose to observe in the near-ultraviolet F300W
filter. These data will enable study of the rest-frame ultraviolet
morphology of galaxies at 0
relations allow their use as cosmological standard candles. The
generally accepted picture is that the exploding star is a C+O white
dwarf which accretes matter from a companion in a binary system.
However, the nature of the companion is still unknown. It could either
be another WD, or be a giant, subgiant, or main-sequence star.
Calculations have shown that it is possible to distinguish among those
possibilities by the effect that the supernova explosion has on the
companion star. We propose to identify the companion star of the two
historical well-known SNeIa through ACS imaging of the targets
complemented by WFPC2 observations. A radial-velocity study of the
stars in those two Galactic SNeIa has been done from ground-based
facilities. To obtain the full motion vector of those stars, we plan
to use ACS for high-resolution astrometry in two different epochs.
That should allow to detect motion imparted during the explosion in
the d ir ection perpendicular to the line of sight, down to a level of
a few milliarcsecs/yr.
reports of potential non-nominal performance that will be
investigated.)
achieve FL on FGS 3 @ 246/12:31:53Z. OTA SE review of PTAS Error Log
showed the GS Re-acquisition (2,3,2) that began @ 246/12:29:16Z had
problems achieving FL. Playback of FGS Pickles Display confirmed FGS 3
experienced SSLEX on the 1st attempt, but succeeded on the 2nd
attempt. Under investigation.
17032-0 – OPS O6300 CCL Quick Update (GSCA 700-0) @ 253/0336z
1154-0 – Change Limits MAMA2 Threshold Voltage @ 252/2100z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 9 9
FGS REacq 8 8
FHST Update 19 19
LOSS of LOCK
SIGNIFICANT EVENTS:
Completed CCS “B” String quick look, post power down integrity
checks. Test was successful, found the link between HSTPS/SDH and CCS
had not been correctly established using the normal DOC procedures.
Re-cycled HSTPS/SDH, after which processed SI SSR PB “all packets”
correctly. Also preformed the following without problems: IP
configuration/PF connects and disconnects, processed HN telemetry, SSR
engineering playback, received and processed PNM 2003247150859, sent
single and block commands, sent NSSC-1 ATP load and associated RTCSs,
inspected File manager and Command Queue for completeness, accessed
Configuration report from the HSTnet and inspected, and exercised
CCSLite.
Set-up and execution of HSTFSW Release 2.4a Acceptance Test for RAM
Installation, Back-out and EEPROM Installation scheduled 253/11:00Z –
254/01:00Z with GDOC, HITT, SE, and VEST using CCS “B” String with CCS
Release 4.0.3 and PRD D06300. The purpose of this testing is to
verify installation and back-out procedures for RAM Version of FSW
2.4a in an operational scenario and to verify EEPROM installation
procedures in an operational scenario.
HST Command Timing test scheduled 253/11:00Z – 20:00Z with GDOC, SOC,
HITT, and CCS using CCS “C” String with CCS Release 4.0.3 and PRD
D06300 and CCS “D” String with Release 5.0.3 and PRD D06300S. The
purpose of this testing is to run comparison testing with CCS Release
5.0.3 on the “D” String and CCS Release 4.0.3 on the “C” String.
