Hubble Space Telescope Daily Report #2934 – 13 Aug 2001

HUBBLE SPACE TELESCOPE

DAILY REPORT #2934

PERIOD COVERED: 0000Z (UTC) 08/10/01 – 0000Z (UTC) 08/13/01

Daily Status Report as of 225/0000Z

1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:

1.1 Completed Seventeen Sets of STIS/CCD 8808 (POMS Test Proposal: STIS
Non-Scripted Parallel Proposal Continuation III)

The Space Telescope Imaging Spectrograph (CCD) was used to make
non-scripted, parallel observations as part of a POMS test proposal. As
described in 2.1 and HSTAR 8298, the acquisition for the first iteration of
this proposal defaulted to fine lock backup on one FGS only, possibly
affecting all observations it that iteration. Otherwise, the observations
completed with no further anomalous activity.

1.2 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. As described in 2.1 and
HSTAR 8298, the acquisition for the first iteration of this proposal
defaulted to fine lock backup on one FGS only, possibly affecting all
observations it that iteration. Otherwise, no other problems were reported.

1.3 Completed Seven 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. As described in 2.1 and HSTAR 8298, the acquisition
for the first iteration of this proposal defaulted to fine lock backup on
one FGS only, possibly affecting all observations it that
iteration. Otherwise, the proposal completed nominally.

1.4 Completed Seven Sets of WF/PC-2 8828 (Cycle 9 Supplemental Darks pt3/3)

The WF/PC-2 was used to obtain three dark frames every day to
provide data for monitoring and characterizing the evolution of hot
pixels. As described in 2.1 and HSTAR 8298, the acquisition for the first
iteration of this proposal defaulted to fine lock backup on one FGS only,
possibly affecting all observations it that iteration. Otherwise, the
proposal completed with no further reported problems.

1.5 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.

1.6 Completed Three Sets of 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.

1.7 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.

1.8 Completed Two Sets of WF/PC-2/STIS/CCD 9052 (A Global Search for
Alteration Minerals on Mars)

The WF/PC-2 and the Space Telescope Imaging Spectrograph (CCD) were
used to perform high spatial resolution and moderate spectral resolution
long-slit imaging spectroscopy of Mars, to search for and globally map the
presence of iron-bearing minerals that are diagnostic of specific climatic
conditions. These hyperspectral image cubes will be complemented by
near-simultaneous WFPC2 UV-VIS imaging that will allow us to quantify the
effects of water ice clouds or other aerosols on our STIS spectra. These
STIS data will provide the ability to detect and map small abundances {~1
jarosite K, Na, H_3OFe_3{SO_4}_2{OH}_6, goethite {AlphaFeOOH}, hematite
{alphaFe_2O_3}, and other ferric and ferrous phases. These minerals are
formed under specific environmental conditions, and some are potential
sinks for Martian atmospheric volatiles. There were no reported problems.

1.9 Completed Three Sets of WF/PC-2 8825 (Decontaminations and
Associated Observations 4/4)

The WF/PC-2 was used to perform the monthly decontaminations
(decons). Also included are instrument monitors tied to decons:
photometric stability check, focus monitor, pre- and post-decon internals
{bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and
internal UV flat check. The proposal completed with no reported problems.

1.10 Completed STIS/CCD 9106 (The Biggest Black Holes)

The Space Telescope Imaging Spectrograph (CCD) was used to perform
searches for supermassive black holes in galaxy centers that have led to
the discoveries that {1} most or all hot galaxies contain massive dark
objects at their centers, presumably black holes; and {2} there is a tight
correlation between the black-hole mass and the luminosity-weighted
velocity dispersion of the hot component of the galaxy. This remarkable
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. There were no reported
problems.

1.11 Completed Five Sets of WF/PC-2 9042 (An Archive To Detect The
Progenitors Of Massive, Core-Collapse Supernovae)

The WF/PC-s was used to search for supernovae which have massive
star progenitors. The already extensive HST archive and high-resolution
ground-based images of galaxies within ~20 Mpc enables us to resolve and
quantify their individual bright stellar content. As massive, evolved
stars are the most luminous single objects in a galaxy, the progenitors of
core-collapse supernovae should be directly detectable on pre-explosion
images. One Type II progenitor has been observed this year, and the
investigators have proposed a short, companion WFPC2 proposal to confirm
this candidate and identify a second. The observations completed nominally.

1.12 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.

1.13 Completed Two 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.

1.14 Completed Four Sets of FGS/1 9169 (An Interferometric Harvest of
Double Degenerates)

Fine Guidance Sensor #1R was used to observe the white dwarf mass
and age distributions that hold clues to the star formation history of our
Galaxy and the age of the disk. No problems were reported.

1.15 Completed Two Sets of STIS/CCD 8909 (CCD Dispersion Solutions)

The Space Telescope Imaging Spectrograph (CCD) was used to perform
wavelength dispersion solutions that are determined on a yearly basis as
part of a long-term monitoring program and to obtain deep engineering
wavecals for all CCD gratings at several wavelength centers. The proposal
completed with no reported problems.

1.16 Completed STIS/CCD 9143 (Spectrophotometry of Nearby Seyfert 2
Nuclei: Can We Eliminate the Seyfert 2 Class?)

The Space Telescope Imaging Spectrograph (CCD) was used to
investigate Seyfert 2s that are distinguished by the absence of the broad
emission lines characteristic of Seyfert 1s and more luminous QSOs. Are
Seyfert 2s fundamentally different from Seyfert 1s and their brighter
cousins? Or is the broad emission line region in Seyfert 2s simply
suppressed by obscuring material as postulated by the unification
model? If the latter model is correct, the weak broad emission lines in
the Seyfert 2s may simply be overwhelmed by starlight from the
circumnuclear region, particularly in the case of recent star
formation. It is proposed to determine if all Seyfert 2s have {weak} broad
emission line regions by obtaining long-slit STIS spectroscopy for a
well-defined sample of 20 Seyfert 2s {3 archival, 17 new}. The
observations completed with no anomalous activity.

1.17 Completed Six 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.

1.18 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.

1.19 Completed 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.

1.20 Completed 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
calibration for SBF and PNLF. The observations completed nominally.

1.21 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.

1.22 Completed Three Sets of WF/PC-2 8816 (Cycle 9 UV Earthflats)

The WF/PC-2 was used to obtain sequences of Earth streak flats to
improve the quality of pipeline flat fields for the WFPC2 UV filter set and
in order to monitor flat field stability. There were no reported problems.

1.23 Completed WF/PC-2 8825 (Decontaminations and Associated
Observations 4/4)

The WF/PC-2 was used to perform the monthly decontaminations
(decons). Also included are instrument monitors tied to decons:
photometric stability check, focus monitor, pre- and post-decon internals
{bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and
internal UV flat check. The proposal completed with no reported problems.

1.24 Completed Three Sets of STIS/MA1/MA2 8917 (MAMA Dispersion
Solution Check)

The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to
determine wavelength dispersion solutions on a yearly basis as part of a
long-term monitoring program {implemented as Program 7651 in Cycle 7,
Program 8430 in Cycle 8 and 8859 in Cycle 9}. No anomalous activity was
reported.

1.25 Completed STIS/CCD 8881 (An Unbiased Survey of X-Ray and Optical
Emission From Extended Radio Jets in AGN)

The Space Telescope Imaging Spectrograph (CCD) was used to an X-ray
bright jet in the distant quasar PKS 0637-752 that shows that X-rays can be
energetically dominant in relativistic jets. The observations completed
nominally.

1.26 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.

1.27 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.

1.28 Completed WF/PC-2 9045 (The Relationship Between Radio Luminosity
and Radio-Loud AGN Host Galaxy Properties)

The WF/PC-2 was used to determine the relationship between the
properties of the host galaxies of radio-loud AGN and their radio
luminosities. Previous studies in this area with the HST have concentrated
on the 3C sample which shows a tight correlation between luminosity and
redshift, such that evolutionary effects cannot be distinguished from those
depending upon radio luminosity. Our sample of 46 radio galaxies at z ~
0.5 comes from four complete, low-frequency-selected samples of radio
sources with differing flux limits. Thus the total sample spans an
unprecedented three orders of magnitude in radio luminosity at a fixed
redshift interval. The proposal completed with no reported problems.

1.29 Completed STIS/CCD/MA1 9114 (SINS: The Supernova Intensive Study–
Cycle 10)

The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
perform closer observations of supernovae that will create the chemical
history of the Universe, energize the interstellar gas, stiffen the spine
of the extragalactic distance scale and provide the only evidence for an
accelerating universe. A
violent encounter is underway between the fast-moving debris and the
stationary inner ring. Monitoring this interaction will help solve the
riddles of stellar evolution posed by the enigmatic three-ring system of SN
1987A. Our UV observations of Ly- Alpha emission reveal the present
location and velocity of a remarkable reverse shock that provides a unique
laboratory for studying fast shocks and a powerful tool for dissecting the
structure of the vanished star. No problems were encountered.

1.30 Completed Two Sets of STIS/CCD/MA1/MA2 8857 (MAMA Sensitivity and
Focus Monitor C9)

The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to monitor the sensitivity of each MAMA grating mode to detect any
change due to contamination or other causes. There were no problems.

1.31 Completed Two Sets of STIS/CCD 9136 (T Tauri Star Coronagraphic
Survey: A PMS Protoplanetary Disk Census)

The Space Telescope Imaging Spectrograph (CCD) was used to observe
pre-main sequence solar-mass stars, the T Tauri stars that Millimeter and
IR studies suggest at least 50 percent have circumstellar disks similar to
the disk from which our planetary system formed. High spatial resolution,
high dynamic range imaging of such systems will map the spatial
distribution of material around the star, constraining the disk sizes and
inclinations, and provide a first assessment of when structure in the disk,
such as cleared central zones and annuli, which has been linked to planet
formation, develops. All observations completed without incident.

2.0 FLIGHT OPERATIONS SUMMARY:

2.1 Guide Star Acquisitions:

Scheduled Acquisitions: 33

Successful: 33

Scheduled Re-acquisitions: 14

Successful: 14

2.2 FHST Updates:

Scheduled: 80

Successful: 80

2.3 Operations Notes:

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

The 486 engineering status buffer limits were adjusted twice per
ROP DF-18A.

TTRs were written for required re-transmits during a NSSC-1 uplink
at 223/1245Z and during a 486 load at 225/0842Z. For the first occurrence,
it became necessary to reset the SI C&DH error counter (at 223/1250Z),
using ROP NS-05.

3.0 SIGNIFICANT FORTHCOMING EVENTS:

Continuation of normal science observations and calibrations.