Hubble Space Telescope Daily Report #2981 – 22 Oct 2001

HUBBLE SPACE TELESCOPE

DAILY REPORT #2981

PERIOD COVERED: 0000Z (UTC) 10/19/01 – 0000Z (UTC) 10/22/01

Daily Status Report as of 295/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

1.1 Completed Seven 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.

1.2 Completed Five Sets of WF/PC-2 9080 (Transition from Non-radiative
to Radiative Shocks in the Cygnus Loop)

The WF/PC-2 was used to obtain narrow band HAlpha and O III imaging
of faint filaments in the northeastern Cygnus Loop that represent the
location of the primary shock front as it first encounters the ISM. There
were no reported problems.

1.3 Completed Twelve Sets of 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 UV filter set. The proposal had no problems.

1.4 Completed Two Sets of STIS/CCD 8906 (Hot Pixel Annealing)

The Space Telescope Imaging Spectrograph (CCD) was used to measure
the effectiveness of the CCD hot pixel annealing process by measuring the
dark current behavior before and after annealing and by searching for any
window contamination effects. In addition, CTE performance is examined by
looking for traps in a low signal level flat. There were no reported problems.

1.5 Completed WF/PC-2 9085 (Measuring The Masses Of High-Z Quasar Host
Galaxies)

The WF/PC-2 was used to investigate the close link between
black-hole mass and spheroid mass in both quiescent and active galaxies in
the local universe. Consequently black-hole and spheroid formation/growth
are now viewed as intimately related processes, and establishing the mass
of quasar host galaxies as a function of redshift is now seen as a key
measurement in observational cosmology. From the Cycle 7 NICMOS program,
the best estimate to date of the mass evolution of the hosts of both
radio-quiet and radio-loud quasars out to z ~eq 2 has been derived. Under
the assumption of passive stellar-population evolution our results are
consistent with the black-hole/spheroid population being unchanged out to z
~eq 2. However, the crucial assumption of passive evolution needs to be
tested. All observations competed nominally.

1.6 Completed Twelve 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.

1.7 Completed Six Sets of STIS/CCD 8901 (Dark Monitor-Part 1)

The Space Telescope Imaging Spectrograph (CCD) was used to monitor
the darks. There was no anomalous activity.

1.8 Completed 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.

1.9 Completed Eight 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. The observations were completed as planned, and no
anomalies were reported.

1.10 Completed Two Sets of WF/PC-2 9058 (Trigonometric Parallax of the
Globular Cluster 47 Tucanae)

The WF/PC-2 was used measure the trigonometric parallax of 47 Tuc,
which is about 1/4 milliarcsec, to an accuracy of 10%. By repeating a
field that was observed in 1995, we will measure the secular motion of the
cluster stars with respect to the SMC background with sufficient accuracy
that the parallax can be measured directly from the displacements within
Cycle 10. Constraints of orientation, and the shape of the WFPC2
footprint, require that we take images at 3-month intervals, rotating 90
degrees each time. The proposal completed with no reported problems.

1.11 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.

1.12 Completed Two Sets of STIS/CCD 9284 (POMS Test Proposal: STIS
Non-Scripted Parallel Proposal Continuation IV)

The Space Telescope Imaging Spectrograph (CCD) was used in the
parallel mode to make some low galactic latitude archive observations. The
observations were executed as scheduled, and no anomalies were noted.

1.13 Completed STIS/MA2 8710 (Timing And Proper Motion Measurement Of
The Proposed Optical Counterpart Of The Nearby Pulsar PSR1929+10)

The Space Telescope Imaging Spectrograph (MA2) was used to observe
PSR1929+10, an old, nearby isolated neutron star detected as an X-ray
pulsar. Optical observations of neutron stars include both young and
middle-aged objects for which different emission models {e.g.
magnetospheric and thermal} have been proposed. However, the general
picture is far from being clear. A firm optical identification of
PSR1929+10 would thus be crucial to understand the long term evolution of
the optical luminosity of pulsars and to investigate possible turnovers in
the emission physics. No anomalous activity occurred.

1.14 Completed STIS/CCD/MA1 9064 (HI Detection of an Extra-Solar
Planetary Atmosphere)

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe the extra-solar planet discovered around HD 209458 that is the
unique one also detected through occultation. During its transit, we will
obtain spectra of the HI and DI Lyman-Alpha line at 1215 Angstrom. No
problems occurred.

1.15 Completed STIS/MA1 8920 (Cycle 10 MAMA Dark Measurements)

The Space Telescope Imaging Spectrograph (MA1) 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. The proposal completed with no
reported anomalous activity.

1.16 Completed Two Sets of STIS/CCD/MA1 8590 (UV Imaging and
Spectroscopy of Luminous Blue Compact Galaxies from z=0 to z=1)

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe two well-defined samples of low-mass starburst galaxies, one in the
local universe {z<0.1} and another at intermediate redshifts {0.2 < z < 0.7}. Both samples show optical sizes, morphologies, emission line widths, and luminosities comparable to those of LBGs at z=3, and are therefore probably the best local analogs and testbeds for further study of LBGs. Our main goals are to: {1} explore the morphologies, surface brightness distributions, and half-light radii of nearby starforming galaxies in the FUV, near Ly-alpha; {2} search for systematic differences among UV, optical, and near-IR morphologies and structural parameters; {3} investigate the intrinsic emission and absorption spectra near Ly-alpha of starbursting dwarf galaxies, with special attention to Ly- alpha profiles and interstellar and stellar photospheric absorption from Si II, O I, C II, Si IV, and C IV; {4} measure their FUV-optical colors and dust extinction properties; and {5} test the hypothesis that low-mass starbursts are the local counterparts of LBGs. The observation completed normally.

1.17 Completed STIS/CCD 8678 (Galaxy Mass and the Fate of the ISM in
Candidate Proto-Spheroidals at z~0.2-0.4)

The Space telescope Imaging Spectrograph (CCD) was used to obtain
long-slit spectra for a sample of 5 faint blue compact galaxies {BCGs} at z
~ 0.2 to 0.4. The observations completed nominally.

1.18 Completed Two Sets of 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.

1.19 Completed WF/PC-2 9149 (The Nature Of The Most Luminous Star-
Forming Galaxies In The Redshift Range 0.4 To 1.5)

The WF/PC-2 was used to perform additional ISO deep surveys that have
previously uncovered a population of galaxies which are making stars at the
fantastic rate of > 100 M_odotyr^-1 in the redshift range from 0.4 to
1.5. However this population evolves rapidly and luminous star-forming
galaxies are 5 to 10 times more numerous at z=1 than today. Combination of
ISO data with radio {VLA}, sub-mm {SCUBA} and optical data shows that they
contribute a major fraction {30-50$ representing only a few percent of the
field galaxy population. HST imaging of a small subsample of these
galaxies indicates that most of them are disks showing disrupted
morphologies or possessing companions, emphasizing the role of merging in
their star formation history. The proposal completed without incident.

1.20 Completed Two Sets of STIS/CCD/MA1/MA2 9116 (Understanding
High-Redshift and Starburst Galaxies: A UV Spectroscopic Survey of B- Stars
in the SMC)

The Space Telescope Imaging Spectrograph (CCD, MA1 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. No problems were reported.

1.21 Completed WF/PC-2 8059 (POMS Test Proposal: Targeted Parallel
Archive Proposal)

The WF/PC-2 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 in
star-forming regions. The observations completed nominally.

1.22 Completed Two Sets of STIS/CCD 7912 (STIS Parallel Archive
Proposal – Nearby Galaxies – Imaging and Spectroscopy)

The Space Telescope Imaging Spectrograph (CCD) was used to make
parallel observations of nearby galaxies. This survey will be useful to
study the star formation histories, chemical evolution, and distances to
these galaxies. These data will be placed immediately into the Hubble Data
Archive. The observations were completed as scheduled, and no problems
were reported.

1.23 Completed 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.

1.24 Completed STIS/CCD 8930 (Investigating The Effect Of The Optical
Baffles On STIS CCD Imaging)

The Space Telescope Imaging Spectrograph (CCD) was used to
characterize the optical baffles around the edge of the STIS detector that
may affect some images. This proposal will investigate the effect of the
stars outside the STIS CCD detector on the STIS images. The idea would be
to image a bright star at various positions outside the field and check the
contamination effects on the detector. The proposal completed nominally.

1.25 Completed STIS/CCD 9088 (Next Generation Spectral Library of Stars)

The Space Telescope Imaging Spectrograph (CCD) was used to produce
a “Next Generation” Spectral Library of 600 stars for use in modeling the
integrated light of galaxies and clusters by using the low dispersion UV
and optical gratings of STIS. The library will be roughly equally divided
among four metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar {-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling
the entire HR-diagram in each bin. Such a library will surpass all extant
compilations and have lasting archival value, well into the Next Generation
Space Telescope era. No problems occurred.

1.26 Completed FGS/1 8898 (Calibrating FGS1r’s Interferometric Response
as a Function of Spectral Color)

Fine Guidance Sensor #1 was used to obtain reference point source
Transfer Functions {S-Curves} through the F583W filter and the F5ND
attenuator at the center position of the FGS1r FOV for a variety of stellar
spectral colors. The data will be added to the library of point source
interferograms that was assembled from the Cycles 8 and 9 calibration
program. These Transfer Functions are needed to support the analysis of GO
science data for the study of close and wide binary star systems and for
determining the angular diameter of extended sources. The proposal
completed with no reported problems.

2.0 FLIGHT OPERATIONS SUMMARY:

2.1 Guide Star Acquisitions:

Scheduled Acquisitions: 21

Successful: 21

Scheduled Re-acquisitions: 23

Successful: 23

2.2 FHST Updates:

Scheduled: 50

Successful: 50

2.3 Operations Notes:

Using ROP SR-1A, the SSR EDAC error counter was cleared eight times.

The engineering status buffer limits were adjusted twice per ROP
DF-18A.

An SSR-3 pointer was set at 292/1131Z per ROP SR-6.

Using ROP SR-6, SSR-3 memory dump locations were set at 292/1200Z,
at 292/1223Z, and at 292/1240Z.

TTRs were written for required re-transmits during NSSC-1 loads at
292/123413Z and at 294/030843Z. In each case, ROP NS-5 was utilized to
reset SI C&DH errors.

ROP SR-9A was used to reset SSR EDAC errors on SSR-3 at 292/1404Z
and at 293/0114Z.

The SSR-3 performance verification test was completed at 292/1856Z.

The NSSC-1 status buffer was dumped and reset at 294/2012Z, using
ROP NS-3.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

A new SMS for this week’s commanding was received on Friday with
two target-of-opportunity proposals.

GSFC Internal Simulation #14 (Planning/Contingency EVA) will be
conducted today and tomorrow, beginning at 8:00 a.m. today.

Continuation of normal science observations and calibrations.