Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.stsci.edu/ftp/observing/status_reports/hst_status_05_27_02 Дата изменения: Tue May 28 15:51:42 2002 Дата индексирования: Sat Dec 22 19:31:28 2007 Кодировка: Поисковые слова: reflection nebula

HUBBLE SPACE TELESCOPE

DAILY REPORT # 3124

PERIOD COVERED: 0000Z (UTC) 05/24/02 - 0000Z (UTC) 05/27/02

OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

ACS 9586

ACS Polarization Calibration

This proposal aims to calibrate the polarization modes most heavily used in
Cycle 11. We need L-flat observations, observations of a polarized star and an
unpolarized star, and an observation of an extended polarized source.

ACS 9476

Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster Sample

The study of distant cluster galaxies requires two key ingredients: {1} deep
high-resolution imaging, to constrain galaxy structure; and {2} 8m-class
spectroscopy, to measure stellar content, star-formation rates, dynamics, and
cluster membership. We will reach both conditions with the addition of HST/ACS
imaging to our suite of VLT {36 nights} and NTT {20 nights} observations of 10
confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey
{EDisCS}.
The proposed HST/ACS data will complement our existing optical/IR imaging and
spectroscopy with quantitative measures of cluster galaxy morphologies {i.e.
sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and with
measurements of cluster masses via weak lensing. Major advantages unique to the
EDisCS project include: {i} uniform selection of clusters; {ii} large enough
sample sizes to characterize the substantial cluster-to-cluster variation in
galaxy populations; {iii} large quantities of high quality data from 8m
telescopes; {iv} uniform measurements of morphologies, spectroscopic and
photometric redshifts, SEDs, star-formation/AGN activities, and internal
kinematics; {v} optical selection of clusters to complement the X-ray selection
of almost all high-z clusters in the ACS GTO programs; {vi} forefront numerical
simulations designed specifically to allow physical interpretation of observed
differences between the high-z and

ACS 9010

SMOV Contamination Plan.

This program has two main goals: {1} manage ACS operations to minimize the risk
of contamination of its optics by materials outgassed during servicing
activity,
and {2} initiate a program to monitor the UV sensitivity of HRC and SBC as
early
as possible after the service mission.

ACS/WFC 9575

Default {Archival} Pure Parallel Program.

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in

ACS/WFC/HRC 9075

Cosmological Parameters from Type Ia Supernovae at High Redshift.

The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble
diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a
record of the expansion history of the universe.

ACS/WFC/HRC 8947

Weekly Test. The Advanced Camera for Surveys (WFC and HRC) was used to perform
basic tests to monitor, the read noise, the development of hot pixels and test
for any source of noise in ACS CCD detectors. This program will be executed at
least once a day for the entire lifetime of ACS.

NICMOS 9321

Dark current, shading profile, and read noise monitoring program

The purpose of this proposal is to monitor the detector dark current, read
noise, and shading profile for all three NICMOS cameras from the onset of
normal
NCS operations throughout the start of Cycle 11.

NICMOS 8991

Grism Calibration

Grism Calibration

NICMOS 9322

NICMOS ACCUM Darks The goal is to obtain ACCUM darks with exposure time=256
seconds with NREADS=25, taken away from the SAA. These are needed to calibrate
the post-SAA darks that will be used to remove CR persistence from NICMOS
science images. In the early Cycle 11 calibration plan they should be obtained
every 4 weeks. We will evaluate need for repeats later

NICMOS 8988

NICMOS Astronomical Persistence Test

This proposal tests the persistence of the NICMOS cameras at the temperature
established by the NCS. A series of saturated exposures followed by dark
integrations are performed for each camera. The exposures have a duration to
saturate the detectors by more than a factor of 100. To facilitate comparison
with the previous SMOV results the same target, HD106965, is utilized.

NICMOS 9269

NICMOS Parallel Thermal Background

NICMOS Camera 3 pure parallel exposures in the F222M filter will be
obtained for
the entire duration of SMOV to establish the stability of the
HST+NCS+Instrument
thermal emission.

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

NICMOS 8987

NICMOS SAA CR Persistence Test

The data from this proposal will be used to design and test algorithms for
using
the "post-SAA darks" as a means of mitigating the effects of cosmic-ray induced
persistence in NICMOS exposures immediately following passages of the
spacecraft
through the South Atlantic Anomaly {SAA}. It mwill also serve as a
reconfirmation of the characteristics of the CR persistence in the cryo-cooler
era {i.e. for comparison with data from prop 7960 "NICMOS Persistence Test",
which was executed in late April of 1998.

NICMOS 8989

NICMOS Thermal Background

Observations in NICMOS Camera 3 in the filters F110W, F175W, F240M, F222M,
F160W
will be obtained at a variety of spacecraft attitudes to characterize the
thermal background light from HST+NCS+Instrument which reaches the NICMOS
focal

STIS/CCD 8904

Bias Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in
the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order
to build up high-S/N superbiases and track the evolution of hot columns.

STIS/CCD 9066

Closing in on the Hydrogen Reionization Edge of the Universe. The Space
Telescope Imaging Spectrograph (CCD) was used in parallel constrain the
Hydrogen
reionization edge in emission that marks the transition from a neutral to a
fully ionized IGM at a predicted redshifts.

STIS/CCD 8902

Dark Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.

STIS/CCD 9176

LMC Eclipsing Binaries with Cepheid Components: The Key to the Extragalactic
Distance Scale.

The Space Telescope Imaging Spectrograph (CCD) was used to determine the
distance to the LMC and to observe the Cepheid P-L that form the backbone
of the
Cosmic Distance Scale and the determination of H_degrees. Unfortunately, in
spite of concerted efforts of many investigators, the zero point of the Cepheid
P-L law and the LMC distance remain controversial and uncertain to ~10-15,
using
eclipsing binaries {EBs} as "standard candles'' to include two recently
discovered LMC eclipsing binaries {EBs} with Cepheid components. These
observations of these extraordinary systems hold the key to determining
simultaneously the Cepheid P-L zero point and the LMC distance, and to
provide a

STIS/CCD 9317

Pure Parallel Imaging Program: Cycle 10.

The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.

STIS/CCD 9077

Survey of the LMC Planetary Nebulae.

The Space Telescope Imaging Spectrograph (CCD) was used to perform a snapshot
survey of all known LMC planetary nebulae {PNe} in order to study the
co-evolution of the nebulae and their central stars, and to probe the chemical

STIS/CCD/MA1 9051

Identifying Damped Lyman-alpha Galaxies at z~1.

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to look for
damped Lyman-alpha absorption systems that contain the bulk of the neutral gas
in the Universe in the redshift range z = 0.5 - 5, yet the nature of the
galaxies responsible for the absorption is not well understood. Only recently
have observers found more than a handful of damped absorbers at redshifts z <
1.5. Using the FIRST Bright Quasar Survey {FBQS}, with over a 1000 quasars, the
proposers have undertaken a survey to build a complete picture of he nature of
the galaxies responsible for damped Lyman-alpha absorption systems at z~1
and to

STIS/CCD/MA1 8919

MAMA Sensitivity and Focus Monitor C10.

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to monitor the
sensitivity of each MAMA grating mode to detect any change due to contamination
or other causes, and also to monitor the STIS focus in a spectroscopic and an
imaging mode.

STIS/MA1/MA2 8920

Cycle 10 MAMA Dark Measurements.

The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the
routine monitoring of the MAMA detector dark noise, and is the primary means of
checking on health of the MAMA detectors systems through frequent monitoring of
the background count rate.

WF/PC-2 9043

Cepheid Distances to Early-type Galaxies. The WF/PC-2 was used to continue
observations in the HST Key Project on the Extragalactic Distance Scale and the
HST project on the "Calibration of Nearby Type Ia Supernovae'' that have
greatly
improved our knowledge of the Hubble Constant by providing a solid zero point
for the Tully- Fisher {TF} relation and Type Ia Supernovae {SNIa}. However,
severe inconsistencies remain for distance estimators to early-type galaxies
such as surface brightness fluctuations {SBF}, the planetary nebula luminosity
function {PNLF}, the fundamental plane {FP}, and the globular cluster
luminosity
function {GCLF}. As a result, the distance to the Virgo cluster core remains
uncertain by as much as 20 determination is directly affected by a
lingering 0.1
mag {5 uncertainty in the photometric calibration of the WFPC2. Resolving these
issues is essential not only to firm up the extragalactic distance scale, but
also to understand the mass and velocity structure of the local universe.
SBF in
particular is emerging as the method of choice for mapping local velocity
fields
to 10, 000 kms because it offers an order of magnitude less Malmquist bias than
TF, and SNIa are too rare to study large scale flows effectively. This project
will tighten the photometric calibration of the WFPC2, and provide a solid
Cepheid

WF/PC-2 9232

Confirmation of Black Hole, Planetary, and Binary Microlensing Events.

The WF/PC-2 was used to collect images of five MACHO Project microlensing
events
in order to confirm our microlensing models which indicate that these events
were caused by black holes and stars with extra-solar planets.

WF/PC-2 8939

Cycle 10 Internal Monitor.

The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to
monitor the health of the cameras.

WF/PC-2 8935

Cycle 10 Standard Darks.

The WF/PC-2 was used to obtain 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.

WF/PC-2 8941

Cycle 10 UV Earthflats. The WF/PC-2 was used to monitor flat field stability by
obtaining sequences of earth streak flats to improve the quality of pipeline
flat fields for the WFPC2

WF/PC-2 9072

Dynamical Masses of White Dwarfs from Resolved Sirius-Like Binaries.

The WF/PC-2 was used to observe resolved "Sirius-like'' systems containing hot
white-dwarf companions of cooler main-sequence stars. It is proposed to image
them annually in the UV.

WF/PC-2 8059

POMS Test Proposal: Targeted Parallel Archive Proposal.

was used to observe the parallel opportunities available 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

WF/PC-2 9318

POMS Test Proposal: WFII Parallel Archive Proposal Continuation.

The WF/PC-2 was used to perform the generic target version of the WFPC2
Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working
Group.

WF/PC-2 9111

The UV Light Echo of Shock Breakout During SN 1987A).

The WF/PC-2 was used to observe light echoes {transient reflection nebulae}
from
SN1987A that were discovered in the optical in 1988 and have been detected in
the vacuum ultraviolet by IUE.

WF/PC-2/STIS/CCD 8675

The Massive Star Content of NGC 6822.

The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were used to
characterize the young, coeval stellar population discovered with WFPC2
multiband imaging in a NGC6822 star-forming region, with follow-up spectroscopy
of the massive star candidates.

WFPC2 8938

WFPC2 CYCLE 9 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/STIS 8690

The Central Region of NGC4696: Manifestation of the Physics of Mergers?
Massive,
dominant ellipticals with attendant emission-line gas, dust and hot, heavy
X--ray emitting coronae lie at the very centers of galaxy clusters. The physics
of these complex, high pressure regions remains controversial: Are cooling
flows
responsible? Do mergers dominate, with massive accretion events triggering an
array of phenomena? Is the AGN crucial? A major impetus to understanding the
physics of these regions will come with Chandra. NGC4696 in the Centaurus
galaxy
cluster is archetypal. WFPC2 images have shown a dramatic bifurcation between
gas and dust. The nucleus itself is seen to be a compact triple, with two blue
components straddling a third red one. We propose to obtain STIS long- slit
spectra { omannumeral1} along a line-emission filament and { omannumeral2}
along
a dust filament: are we witnessing physical separation of gas and dust, as in
comet ion/dust tails, due to late stage merger physics; or are very high
velocities, due to powerful AGN influences, shifting emission lines out of
filters? Is the HAlpha+NII filament a shock, responsible for the known
off-center X--ray peak? {omannumeral3} A third spectrum will be across the
compact 0.26'' triple nucleus: is it a multiple nucleus confirming the merger
scenario; or a disk around a black-hole, allowing mass determination; or the
first double optical synchrotron jet; or a gravitational lens? A wealth of
vital
physical and kinematical data will result from these carefully selected
spectra.

FLIGHT OPERATIONS SUMMARY:

HSTARs:
8659 - GSacq(1,3,1) results in Fine Lock Backup (3,0,3) @144/1059z
8660 - A string's AppServer lost connection @144/1430z
8661 - C-String SAC Jobs failed @144/1900z
8662 - Gsacq(1,2,1) Results in FL/BU using FGS#1(1,0,1) @148/0327z

COMPLETED OPS REQs: None

OPS NOTES EXECUTED:
1008-0 Raise Battery#3 Upper Temp Limit to 3Deg @144/2040z


SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 27 27
FGS REacq 34 34
FHST Update 69 69
LOSS of LOCK None


Operations Notes:

FOT operated on CCS Release D3.5.0.0.68 throughout this reporting
period.

SIGNIFICANT EVENTS:

Continuation of Servicing Mission Orbital Verification and the gradual
resumption of normal science observations and calibrations.