Hubble Space Telescope Daily Report #2949 – 4 Sep 2001
HUBBLE SPACE TELESCOPE
DAILY REPORT #2949
PERIOD COVERED: 0000Z (UTC) 08/31/01 – 0000Z (UTC) 09/04/01
Daily Status Report as of 247/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed STIS/CCD/MA2 9051 (Identifying Damped Lyman-alpha
Galaxies at z~1)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
look for samped 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 double the sample
size at this redshift. No problems were encountered.
1.2 Completed Sixteen Sets of WF/PC-2 9244 (POMS Test Proposal: WFII
Parallel Archive Proposal Continuation)
The WF/PC-2 was used to perform a generic target version of the
Archival Pure Parallel program. The program will be used to take parallel
images of random areas of the sky, following the recommendations of the
Parallels Working Group. The observations completed with no anomalous
activity.
1.3 Completed Two Sets of STIS/CCD 8864 (CCD Dark Monitor-Part 2)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor
the darks for the CCD. The proposal completed nominally.
1.4 Completed STIS/CCD/MA2 8569 (A New Survey for Low-Redshift Damped
Lyman-Alpha Lines in QSO MgII Systems)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
support studies which have shown that most of the observable neutral gas
mass in the Universe resides in QSO damped LyAlpha {DLA} systems. However,
at low redshift, DLA can only be found by searching in the UV with HST. By
boot-strapping from the MgII statistics, we will be able to further improve
the determination of the low- redshift statistical properties of DLA {their
incidence and cosmological mass density} and open up new opportunities for
studies at low redshift. The observations completed nominally.
1.5 Completed STIS/CCD/MA1/MA2 9113 (Solar UV Radiation and the Origin
of Life on Earth)
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to observe chromospheric models that will enable the proposers to
predict the extreme-UV emission of the early Sun and its consequences for
the erosion of the early Earth’s atmosphere and the altered oxidation state
of the planet, and investigate the effect of metallicity on the UV emission
and its consequences for the photochemistry of Earth-like planets. There
was no anomalous activity.
1.6 Completed Thirteen Sets of STIS/CCD 9285 (POMS Test Proposal: STIS
Non-scripted Parallel Proposal Continuation III)
The Space Telescope Imaging Spectrograph (CCD) was used to make low
galactic latitude, non-scripted parallel observations as part of a POMS
test proposal. As described in 2.1 and HSTAR 8321, the acquisition for the
first iteration of this proposal defaulted to fine lock backup on one FGS
only, possibly affecting eleven observations. Then, during the second
iteration the loss of lock mentioned in 2.1 and HSTAR 8324 occurred,
possibly affecting an observation. Otherwise, the observations were
completed as planned, and no other anomalies were reported.
1.7 Completed WF/PC-2 8656 (The Hydrogen-Burning Limit in the Globular
Cluster NGC 6397)
The WF/PC-2 was used to perform a major enhancement of an earlier
study of the bottom of the main sequence (MS) of NGC 6397, the globular
cluster with the smallest distance modulus. In the earlier work the lowest
part of the MS had been lost among the numerically dominant field stars;
but accurate astrometry, over a baseline of a few years, now allows an
excellent proper-motion separation of faint cluster stars from the
field. As described in 2.1 and HSTAR 8321, the acquisition for this
proposal defaulted to fine lock backup on one FGS only, possibly affecting
eleven observations. Then, during the proposal the loss of lock mentioned
in 2.1 and HSTAR 8324 occurred, possibly affecting an
observation. Otherwise, the proposal completed with no other reported
problems.
1.8 Completed STIS/CCD 8865 (Bias Monitor-Part 2)
The Space Telescope Imaging Spectrograph (CCD) was used to 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. The proposal completed with no anomalous activity.
1.9 Completed Two Sets of 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 enrichment history of the LMC. There were no reported problems.
1.10 Completed Three Sets of WF/PC-2 9249 (POMS Test Proposal: WFII
Backup Parallel Archive Proposal II)
The WF/PC-2 was used to execute a POMS test proposal designed to
simulate scientific plans. The proposal completed with no reported problems.
1.11 Completed WF/PC-2 9145 (A Snapshot Survey of the Optically
Selected Type-2 Quasars)
The WF/PC-2 was used to observe an identified population of
emission-line objects in DPOSS, which can be plausibly interpreted as the
long-sought type-2 quasars. They have high-ionization Seyfert-2 like
spectra, but with narrow-line luminosities comparable to those of the
luminous type-1 quasars in the same redshift range. This population may be
a major contributor to the cosmic hard x-ray background. It is proposed to
obtain multi-color images of a representative sample of these objects, in
order to examine their morphology. We may be able to detect point-like
nuclei which are not detectable in ground-based images, the dust lanes
hiding them from our view, possible evidence for tidal interactions and the
overall morphology of their hosts, etc. The proposal completed with no
reported problems.
1.12 Completed STIS/CCD 9128 (A Snapshot Survey of Absorption Lines
from High Velocity Clouds in the Milky Way)
The Space Telescope Imaging Spectrograph (CCD) was used to search
for Mg II and Mg I absorption from Galactic High Velocity Clouds {HVCs}
along the sightlines of 51 of the brightest QSOs, BL Lacs and Seyfert 2
galaxies in the sky. The observations completed with no reported problems.
1.13 Completed Six Sets of WF/PC-2 8815 (Cycle 9 Earth Flats)
The WF/PC-2 was used to monitor flatfield stability. This proposal
obtains sequences of Earth streak flats to construct high quality flat
fields for the WF/PC-2 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. The
proposal completed nominally.
1.14 Completed STIS/CCD/MA2 8770 (The Nucleosynthesis of Boron –
Benchmarks for the Galactic Disk)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
determine boron (B) abundance. In spite of several HST cycles of B
abundance determinations, we do not know the true, ambient, present-day
abundance of B. Only two stars {with undepleted Li and Be} have been
observed to derive the Population I true B abundance. Past cycles have
focused on {1} halo stars with low metallicity and {2} solar-type stars
with Li and/or Be deficiencies. In this proposal, the stellar abundances
of B will be determined, measured from the B I 2497 Angstrom line from STIS
echelle spectra, of main sequence F-G stars that have retained their full
initial abundances of boron. Our target stars are those for which
ground-based observations show that beryllium is undepleted. These new
abundances will map evolution of the B abundance in the Galactic disk in
the metallicity range from one-third solar up to solar. Then the B, and
previously determined Li and Be abundances, will be used to improve
understanding of the nucleosynthesis of B. There were no reported anomalies.
1.15 Completed Nine Sets of WF/PC-2 8936 (Cycle 10 Supplemental Darks
Pt1/3)
The WF/PC-2 was used to perform a dark calibration program that
obtains three dark frames every day to provide data for monitoring and
characterizing the evolution of hot pixels. The proposal completed with no
reported problems.
1.16 Completed STIS/CCD 8912 (Full-Field Sensitivity Monitor C10)
The Space Telescope Imaging Spectrograph (CCD) was used to measure
a photometric standard star field in Omega Cen in 50CCD mode every few
months to monitor CCD sensitivity over the whole field of view. No
problems were encountered.
1.17 Completed Six Sets of STIS/CCD 8901 (Dark Monitor-Part 1)
The Space Telescope Imaging Spectrograph (CCD) was used to
monitor. There was no anomalous activity.
1.18 Completed Two Sets of FGS/1 9034 (The Masses and Luminosities of
Population II Stars)
Fine Guidance Sensor #1 was used to observe the mass-luminosity
relation {MLR} of Population II stars of which very little is currently
known. With the advent of the Hipparcos Catalogue, improved distances to
many spectroscopic binaries known to be Pop II systems are now
available. After surveying the literature and making reasonable estimates
of the secondary masses, we find 13 systems whose minimum separation should
be larger than the resolution limit of FGS #1. The observations completed
nominally.
1.19 Completed Five Sets of STIS/CCD 8900 (Performance Monitor)
The Space Telescope Imaging Spectrograph (CCD) was used to measure
the baseline performance and commandability of the CCD subsystem. All
exposures are internals. The observations completed normally.
1.20 Completed WF/PC-2 9160 (Disks and Envelopes of Nearby Nebulous
Young Stellar Objects: A Snapshot Survey)
The WF/PC-2 was used to perform a snapshot survey of nearby
nebulous young stellar objects to study the detailed morphology of the
their disks and envelopes and probe the effect of inclination on the
infrared spectral energy distribution of disk/envelope systems. The
proposal completed as planned.
1.21 Completed STIS/CCD 9107 (The Fundamental Plane for Nuclear Black
Holes)
The Space Telescope Imaging Spectrograph (CCD) was used to conduct
more in-depth searches for supermassive black holes in galaxy
centers. Previous work has led to the discoveries that {1} most or all hot
galaxies contain massive dark objects at their centers, presumably black
holes; {2} there is a remarkably tight correlation between the black-hole
mass and the luminosity-weighted velocity dispersion of the hot component
of the galaxy. This mbh-Sigma relation has a scatter which is <0.3 dex in
mbh and consistent with zero. This relationship suggests a strong link
between black-hole formation, AGN activity, and galaxy formation, and once
it is understood this link should advance our understanding of all three
processes. The goal of this proposal is to investigate the scatter in the
mbh-Sigma relation and the role of possible second parameters, by examining
a sample of galaxies at fixed velocity dispersion Sigma=200+/- 20
kms. This approach decouples the effects of a second parameter from
uncertainties in the shape of the mbh-Sigma relation, and minimizes
spurious correlations because all of the galaxies will be studied using the
same well-tested observational and modeling techniques. No anomalous
activity occurred.
1.22 Completed Three Sets of STIS/CCD 8903 (Bias Monitor – Part 1)
The Space Telescope Imaging Spectrograph (CCD) was used to 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. There were no problems.
1.23 Completed WF/PC-2 9133 (Imaging of Gravitational Lenses)
The WF/PC-2 was used to observe gravitational lenses that offer
unique opportunities to study cosmology, galactic structure, galaxy
evolution, quasar hosts and extinction. They are also the only sample of
galaxies selected on the basis of their mass rather than their luminosity
or surface brightness. While gravitational lenses can be discovered with
ground-based optical and radio observatories, converting them from
curiosities into scientific tools requires HST. There were no reported
anomalies.
1.24 Completed Two Sets of WF/PC-2 9124 (Mid-UV SNAPSHOT Survey of
Nearby Irregulars: Galaxy Structure and Evolution Benchmark)
The WF/PC-2 was used to investigate the relation between star
formation and the global physical characteristics of galaxies to interpret
the morphologies of distant galaxies in terms of their evolutionary
status. Distant galaxies are primarily observed in their rest frame
mid-ultraviolet. They resemble nearby late-type galaxies, but are they
really physically similar classes of objects? It is proposed to address
this question through a SNAPSHOT survey in the 2 mid-UV filter F300W of 98
nearby late-type, irregular and peculiar galaxies. No problems were reported.
1.25 Completed STIS/CCD/MA2 9156 (Spectrum And Pulse Profile Of PSR
0656+14 In The Near-UV)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
perform prism observations of the middle-aged pulsar PSR B0656+14. This
would allow the proposers to make for the first time phase- resolved
spectroscopy of a middle-aged pulsar as a function of wavelength in the UV,
and to study how the pulse profile of such a pulsar at these wavelengths
differs from the only similar data available so far, namely those of the
much younger Crab pulsar. This is important for the understanding of how
the spectral evolution evolves with pulsar age. There were no reported
problems.
1.26 Completed 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. The proposal completed uneventfully.
1.27 Completed WF/PC-2 9155 (The Cepheid Distance to NGC 1637: A Direct
Comparison with the EPM Distance to SN 1999em)
The WF/PC-2 was used to directly compare distances estimated by two
primary extragalactic distance indicators. T he appearance of supernova
1999em, a bright, extremely well- observed type II plateau event in the
nearby SBc galaxy NGC 1637 offers the best chance to test the consistency
of the Expanding Photosphere Method {EPM} of supernova distance
determination with that derived from Cepheid variable stars. Although EPM
distances have been measured to 18 type II supernovae out to 180 Mpc and
used to determine Hubble’s constant independent of the Cepheid distance,
there have never been any measurements of Cepheids in a galaxy that has
hosted a normal type II-P supernova, the classic variety of core-collapse
event to which EPM-derived distances are most robust. The proposal
completed nominally.
1.28 Completed STIS/CCD 8669 (Merger-Driven Evolution Of Galactic
Nuclei: Observations Of The Toomre Sequence)
The Space Telescope Imaging Spectrograph (CCD) was used to observe
galaxy mergers that are believed responsible for triggering starburst and
AGN activity in galaxies, and even perhaps transforming spiral galaxies
into ellipticals. The proposal completed nominally.
1.29 Completed Two Sets of STIS/CCD 9187 (A Lyman Limit Snapshot
Survey: The Search for Candidate D/H Absorbers)
The Space Telescope Imaging Spectrograph (CCD) was used to measure
D/H in gas clouds seen against background QSOs. This provides a unique and
fundamental cosmological probe of the baryonic density parameter. To date,
most of the QSO absorption line D/H constraints have been derived at high
redshift. In this proposal the proposers investigate a lower redshift
range, because there are two potentially crucial advantages to be gained by
carrying out D/H measurements at intermediate redshift. First, the
background of HI forest lines is lower and contamination of the DI feature
is significantly reduced. Second, a far larger sample of very bright QSOs
exists. There were no reported problems.
1.30 Completed STIS/CCD 8846 (Imaging Flats C9)
The Space Telescope Imaging Spectrograph (CCD) was used to
investigate flat-field stability over a monthly period. The proposal
completed nominally.
1.31 Completed STIS/CCD 9121 (Evolution of the Host Galaxies in Low-
Power AGN)
The Space Telescope Imaging Spectrograph (CCD) was used to study
the evolution of low-power AGN host galaxies to z~1.3, allowing the direct
study of how the formation and life cycles of radio-loud AGN depend on
intrinsic power. There were no reported problems.
1.32 Completed Three Sets of WF/PC-2 9060 (Photometry of a
Statistically Significant Sample of Kuiper Belt Objects)
The WF/PC-2 was used to propel the physical study of KBOs forward
by performing accurate photometry at V, R, and I on a sample of up to 150
KBOs. The sample is made up of objects that will be observed at thermal
infrared wavelengths by SIRTF and will be used with those data to derive
the first accurate diameters and albedos for a large sample of KBOs. As
described in 2.1 and HSTAR 8326, the acquisition for the middle iteration
of this proposal failed, affecting six observations when the take data flag
remained down. Otherwise, the observations completed nominally.
1.33 Completed Two Sets of STIS/CCD 9110 (A Search for Kuiper Belt
Object Satellites)
The Space Telescope Imaging Spectrograph (CCD) was used to
investigate whether the large number of collisions thought to have taken
place in the primordial Kuiper belt suggest that many Kuiper belt objects
{KBOs} could have suffered binary-forming collisions similar to that which
formed the Pluto — Charon binary. Detection of such KBO satellites would
allow measurement of KBO masses, would help to understand the past
collisional environment of the Kuiper belt, and would give a context to the
otherwise unique-seeming formation of the Pluto — Charon binary. The loss
of lock documented in HSTAR 8325 and 2.1 occurred during the second
iteration of this proposal. Otherwise, the proposal completed with no
other problems.
1.34 Completed STIS/CCD/MA1 8638 (Temperature Scale And Metal
Abundances Of Hot Hydrogen-Rich Central Stars Of Planetary Nebulae)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
perform UV spectroscopy on a sample of hot hydrogen-rich central stars of
PNe, covering the hottest phase of post-AGB evolution. The spectra will
then be analyzed with fully metal line blanketed NLTE model atmospheres in
order to determine T_eff, surface gravity, and chemical composition. The
proposal completed with no reported problems.
1.35 Completed Two Sets of STIS/MA1/MA2 8843 (Cycle 9 MAMA Dark
Measurements)
The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to
perform the routine monitoring of the MAMA detector dark noise. The
proposal completed nominally.
1.36 Completed Two Sets of WF/PC-2 9057 (Host Galaxies of Obscured QSOs
Identified by 2MASS)
The WF/PC-2 was used to perform a snapshot survey of red QSOs
discovered in The Two Micron All Sky Survey {2MASS} to investigate the
detailed properties of their host galaxies. This large, possibly dominant,
population of QSOs in the local universe has been previously overlooked
because reddening by {intrinsic} obscuration along our line of sight causes
their colors to be too red for identification by traditional “UV- excess”
techniques. Their near-IR colors are similar to PG- type {UV-excess} QSOs,
but it is far from certain whether they are indeed from the same parent
population or represent a completely new class of QSO. There were no
reported problems.
1.37 Completed Two Sets of STIS/CCD/MA2 8614 (NUV Extension of the
Arcturus Project: Probing the Onset of Chromospheric Heating)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
observe two stars that have multi-wavelength atlases at resolutions high
enough to resolve dynamically interesting line structure: the Sun {G2 V}
and Arcturus {K2 III}. The observations completed with no reported problems.
1.38 Completed Two Sets of 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. No problems were encountered.
1.39 Completed Two Sets of STIS/CCD 9148 (Light Echos and the Nature of
Type Ia Supernovae)
The Space Telescope Imaging Spectrograph (CCD) was used to take
STIS snapshot images of a subset of 43 well observed Type Ia supernovae
{SNIa}, most of which have been discovered in late type galaxies over the
last 40 years to make a systematic search for light echos around SN
Ia. STIS will also observe a sample of 10 SN II and SN Ib/c, which are
believed to be the result of massive star core collapse and, therefore, to
be thin-disk population objects, in order to make an empirical calibration
of the accuracy of our method for determining scale heights. The SN Ia
sample will provide a direct as well as accurate estimate of the scale
height of SN Ia which is an important clue to the progenitors of these
events. The proposal completed nominally.
1.40 Completed STIS/CCD 8905 (Read Noise Monitor)
The Space Telescope Imaging Spectrograph (CCD) was to be used to
measure the read noise of all the amplifiers {A, B, C, D} on the STIS CCD
using pairs of bias frames. However, as described in 2.1 and HSTAR 8326,
the acquisition for this proposal failed, affecting four observations when
the take data flag remained down.
1.41 Completed S/C 5582 (FOC/48 Monthly Activation (Camera Section
Only): Cycle 4)
This proposal was executed as scheduled, and no anomalies were noted.
1.42 Completed FGS/1 8729 (Speedy Gonzales Mass Determinations: Fast
Orbiting Red Dwarf Systems)
The FGS #1 was used to observe five fast-orbiting red dwarf systems
to determine masses for objects near the end of the stellar main
sequence. All five systems have periods of two years or less, hence the
moniker “Speedy Gonzales” systems. In addition, all have parallaxes
placing them within 10 parsecs, so high quality masses with errors less
than 5% can be derived. The observation completed as planned.
1.43 Completed FOC/96 7923 (FOC F/96 Turn-on)
The Faint Object Camera (f/96) was used to take an internal flat
and a dark to ensure that the 30-day limit for the FOC is not
exceeded. The observations were executed as scheduled, and no anomalies
were noted.
1.44 Completed WF/PC-2/STIS/CCD 8573 (Newborn Planets and Brown Dwarf
Companions in IC 348)
The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were
used to search for young giant planets and brown dwarfs around ~100
low-mass stars and brown dwarfs in the nearby cluster IC 348. The
observations completed with no reported problems.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 40
Successful: 39
Per HSTAR 8321, the acquisition at 243/094541Z and the following
re-acquisition defaulted to fine lock backup on FGS-3 only when the scan
step limit was exceeded on FGS-2. The proposals detailed in 1.6 and 1.7
may have been affected.
There was a loss of lock on FGS-3 at 243/134136Z. HSTAR 8324 was
written. The proposals described in 1.6 and 1.7 may have been affected.
As detailed in HSTAR 8325, there was another loss of lock at
246/074101Z that lasted until 246/074207Z. The proposal described in 1.33
was affected.
Per HSTAR 8326, following two full maneuver update failures at
246/093715Z and at 246/094000Z, the acquisition scheduled for 246/095501Z
failed when the search radius limit was exceeded for FGS-3. The proposals
described in 1.32 and 1.40 were affected.
Scheduled Re-acquisitions: 25
Successful: 25
2.2 FHST Updates:
Scheduled: 92
Successful: 90
Per HSTAR 8326, the full maneuver updates at 246/093715Z and at
247/090400Z failed due to FHST #3.
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared ten times.
Per an operations request, there was an EPS adjustment for high
suntime at 243/1356Z.
A TTR was written for multiple minor frame gaps beginning at
245/001506Z.
The engineering status buffer (ESB) limits were adjusted four times
per ROP DF-18A. Using the same ROP, the ESB was dumped and cleared at
246/1437Z.
Three TTRs were written for required re-transmits during uplinks at
244/034754Z, at 246/084237Z, and at 247/041837Z.
The ephemeris table was uplinked at 247/0011Z per ROP DF-07A.
Using ROP NS-5, SI C&DH errors were reset at 247/0424Z.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
Continuation of normal science observations and calibrations.
