Hubble Space Telescope Daily Report #2851 – 16 Apr 2001
HUBBLE SPACE TELESCOPE
DAILY REPORT #2851
PERIOD COVERED: 0000Z (UTC) 04/13/01 – 0000Z (UTC) 04/16/01
Daily Status Report as of 106/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed Six 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.
1.2 Completed Five Sets of WF/PC-2 8699 (The Origin of Short-Period Comets)
The WF/PC-2 was used to detect and characterize cometary nuclei in
order to determine the basic physical properties of a large fraction of the
population of short-period comets. By acquiring statistically significant
data, we can study the origin of this family of comets and test the
hypothesis that they are collisional fragments from the Kuiper Belt
Objects. As described in the previous report and in HSTAR 8162, the
acquisition for the third iteration of this proposal failed, affecting one
observation. Then, as described in the previous report and in HSTAR 8163,
the acquisition for the third iteration of this proposal failed, affecting
two observations. Otherwise, the observations completed with no further
reported problems.
1.3 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.
1.4 Completed Eight Sets of WF/PC-2 8827 (Cycle 9 Supplemental Darks pt2/3)
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. The proposal completed nominally.
1.5 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.
1.6 Completed STIS/MA2 8863 (NUV-MAMA Cycle 9 Flats)
The Space Telescope Imaging Spectrograph (MA2) was to be used to
obtain NUV-MAMA observations of the internal Deuterium lamp to construct an
NUV flat applicable to all NUV modes. As described in the previous report
and in HSTAR 8162, the acquisition this proposal failed, affecting two
observations.
1.7 Completed STIS/MA1 8862 (FUV-MAMA Cycle 9 Flats)
The Space Telescope Imaging Spectrograph (MA1) was to be used to
obtain FUV-MAMA observations of the internal Krypton lamp to construct an
FUV flat applicable to all FUV modes. As described in the previous report
and in HSTAR 8163, the acquisition for this proposal failed, affecting one
observation.
1.8 Completed Six 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.
1.9 Completed Two Sets of WF/PC-2 8583 (Imaging Snapshots of Asteroids)
The WF/PC-2 was used to obtain images of the fifty largest main
belt asteroids that have favorable apparitions during cycle 9. The images
will be searched for companion bodies, as well as mineralogical variegation
on the resolved main bodies. There were no reported problems.
1.10 Completed Fourteen Sets of STIS/CCD 9248 (Probing the Large Scale
Structure: Cosmic Shear Observations)
The Space Telescope Imaging Spectrograph (CCD) was used to measure
the distortion of light bundles from distant galaxies that probe the
statistical properties of the intervening inhomogeneous {dark} matter
distribution. Its tidal gravitational field distorts the observable image
shapes thereby causing a coherent ellipticity pattern {Cosmic
Shear}. During the eleventh iteration of this proposal, the re-acquisition
failure described in 2.1 and HSTAR 8168 occurred, affecting one
observation. Otherwise, the observations completed nominally with no other
reported problems.
1.11 Completed WF/PC-2 8703 (A Spectacular Post-Starburst Quasar and
the AGN–Starburst Connection)
The WF/PC-2 was used to perform broad-band imaging of the
spectacular post- starburst quasar UN J1025-0040 {V=19, z=0.634}. The
optical spectrum is a chimera, dominated in the blue by light from a
quasar, and dominated in the red by light from a 400-Myr-old starburst with
a mass possibly as much as 10^11 M_SUN. The total energy budget of both
sources appears similar, 10^11.6 L_SUN. The extended fuzz of the host
galaxy is asymmetric toward a nearby companion {dominated by an 800-Myr-old
starburst}, signifiying some kind of interaction. There were no reported
problems.
1.12 Completed Two Sets of WF/PC-2 8677 (Extragalactic Novae: the
Maximum Magnitude – Rate of Decline Relation in NGC 4472)
The WF/PC-2 was used to accomplish two goals: {1} to provide the
first homogeneous observational constraints on theoretical models for novae
outbursts; and {2} to assess the reliability of novae as standard candles
by using WFPC2 to collect well sampled light curves for 20-50 novae in the
supergiant elliptical galaxy NGC 4472, the brightest galaxy within 30
Mpc. Both the length of the observing window and the temporal sampling of
the observations are specifically designed to ensure that the novae peak
magnitudes and decline rates are measured accurately. These data will be
used to construct the first `Maximum Magnitude versus Rate of Decline’
{MMRD} relation for a galaxy beyond the Local Group. This relation is not
only a potentially powerful standard candle, but its shape and dispersion
are directly linked to physical parameters which govern the physics of
novae outbursts such as the white dwarf mass, temperature and mass
accretion rate. The proposal completed with no reported problems.
1.13 Completed WF/PC-2 8655 (Geometric Distances of Globular Clusters
{GO part})
The WF/PC-2 was used to establish a globular-cluster distance scale
of unprecedented accuracy and reliability, with far- reaching impact on the
distance and time scales of cosmology. Our method is to compare internal
dispersions of proper motion with ground-based determinations of the
dispersion of radial velocities. The prospect is a geometrically based
distance scale with an accuracy of better than 2 ability to make such
measurements, and we are progressing with the conversion of them to a
distance for the cluster. The observations completed with no reported
problems.
1.14 Completed 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. The
observations completed with no anomalous activity.
1.15 Completed STIS/CCD 8603 (Secular Changes In The Temperatures And
Radii Of Extreme Helium Stars)
The Space Telescope Imaging Spectrograph (CCD) was used to make
observations of 15 extreme helium stars (EHEs_ which, together with IUE
data, will give a 20-year baseline of ultraviolet spectrophotometry. EHEs
are luminous stellar remnants evolving rapidly to become white
dwarfs. They represent an important stage in the evolution of at least
some low-mass stars, and are closely related to the R Coronae Borealis
variables. Models do not agree about their origin, nor about what fraction
of normal stars pass through this phase, in which the stars have been
completely stripped of their outer layers. The models do predict that EHEs
are contracting and provide rate predictions and evolutionary
lifetimes. The observations completed with no reported problems.
1.16 Completed FGS/1 8774 (Calibrating the Mass-Luminosity Relation at
the End of the Main Sequence)
The Fine Guidance Sensor #1 was used to calibrate the
mass-luminosity relation {MLR} for stars less massive than 0.2 Msun, with
special emphasis on objects near the stellar/brown dwarf border. Our goals
are to determine Mv values to 0.10 magnitude, masses to 5%, and more than
double the number of objects with masses determined to be less than 0.20
Msun. The proposal completed with no reported problems.
1.17 Completed Seven 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/MA1/MA2 8877 (Simultaneous HST and Chandra
Observations of the X-Ray/UV absorbers in Seyfert 1 Galaxies)
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to make UV and X-ray observations of intrinsic absorption that reveal
that outflowing photoionized gas with a substantial covering factor is a
major nuclear component in at least 50% of Seyfert 1 galaxies. X-ray
observations suggest multiple zones with highly variable ionization states
and column densities. UV observations reveal multiple kinematic components,
with column densities that vary in time. This variability indicates that
simultaneous UV and X-ray observations at high spectral resolution are the
only way to decipher the complex kinematic and ionization structure and the
true connection between UV and X-ray absorbers, and hence form an accurate
picture of the environs of the inner nucleus. The observations completed
with no reported problems.
1.19 Completed STIS/CCD/MA1 8473 (Key Project: The Nuclear Region Of
NGC 4151 Observations)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe the Seyfert 1 galaxy NGC 4151. This galaxy will be studied in
several ways. 1} low-resolution spectra over the entire UV and visible
range will be obtained through a slit at several different orientations to
model the physical conditions in the emission-line regions; 2} slitless and
long-slit spectra of strong emission lines at moderate resolution and
narrow-band WFPC2 images will be used to map the dynamics of the regions;
3} echelle spectra over the entire UV bandpass will be used to study the
intrinsic absorption in the nucleus; and 4} parallel imaging will be
performed of the outer galaxy and other galaxies or QSOs. There were no
reported problems.
1.20 Completed Two Sets of STIS/CCD/MA1 8662 (A Snapshot Survey of the
Hot Interstellar Medium)
The Space Telescope Imaging Spectrograph (CCD And MA1) was used to
obtain snapshot STIS echelle observations of key tracers of hot
interstellar gas {C IV, N IV, and Si IV} for selected FUSE Team O VI survey
targets with known UV fluxes. By taking advantage of the snapshot
observing mode we will efficiently obtain a large number of spectra
suitable for the study of the highly ionized hot component of the
interstellar medium {ISM}. Our goals are to explore the physical
conditions in and distribution of such gas, as well as to explore the
nature of the interfaces between the hot ISM and the other interstellar gas
phases. The observations completed with no reported problems.
1.21 Completed Two Sets of STIS/CCD 8776 (Absolute Proper Motions of
Nearby Dwarf Spheroidal Galaxies)
The Space Telescope Imaging Spectrograph (CCD) was used to measure
precise absolute proper motions for four dwarf spheroidal satellites of the
Milky Way using spectroscopically-confirmed background QSOs to define a
zero- velocity reference frame. No anomalous activity was reported.
1.22 Completed STIS/CCD 8687 (Elliptical Galaxies With Nuclear Disks of
Stars: Black Hole Search and Stellar Populations)
The Space telescope Imaging Spectrograph (CCD) was used to observe
galaxies NGC 3706 {E3} and NGC 4486A {E2} to search for supermassive black
holes {BHs}. NGC 3706 contains a bright, edge-on nuclear disk of
stars. Therefore we can measure the BH mass mbh as easily as in a galaxy
with a gas disk but without uncertainty about whether the motions are
affected by non-gravitational forces. NGC 4486A, like NGC 4486B, is a
dwarf elliptical companion of NGC 4486 {M s87} with signs of an unusually
massive BH. The observations completed and no anomalous activity occurred.
1.23 Completed Two Sets of WF/PC-2/STIS/CCD/MA2 8568 (A Seminal
Spectroscopic and Imagery Investigation of the Brightest Wolf-Rayet Shell
Nebula: NGC 6888)
The WF/PC-2 (for imagery) and the Space Telescope Imaging
Spectrograph (CCD for UV-optical-NIR spectroscopy of several regions in the
brightest Wolf-Rayet Shell) were used to observe Nebula {WRSN}, NGC
6888. The physical conditions in the wind-driven and/or stellar ejected
plasma {temperature, density, ionization, and composition} of WRSN, which
are dominated by strong stellar winds from hot massive stars in an advanced
state of evolution, often involve emission from both shock-ionized and
photoionized gas in close proximity. These new observations will comprise
the first combined spectroscopy and imagery of a WRSN at a resolution
sufficient to separate and individually analyze these two emission
regions. The proposal completed nominally with no reported problems.
1.24 Completed STIS/CCD 8845 (Spectroscopic Flats C9)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain
CCD flats in the spectroscopic mode. The observations completed with no
reported problems.
1.25 Completed WF/PC-2 8698 (Identification of the Galaxy’s Missing Mass)
The WF/PC-2 was used to observe the nature of dark matter that is
one of the key astrophysical questions of the day. The existence of dark
matter and its dynamical dominance in the outer parts of our Galaxy and
spiral galaxies with flat rotation curves is well established. The MACHO
project has identified ~half of the Milky Way’s dark matter with stellar
objects of ~0.5 M_sun, probably white dwarfs. But the location of the
microlensing in the halo is disputed. Several have detected two candidate
halo white dwarfs of L/L_sun ~ 10^-5 in the Hubble Deep Field with 25 +/- 5
mas/year proper motions. The observations completed with no reported problems.
1.26 Completed WF/PC-2 8780 (Secular Changes in the Jet of M87)
The WF/PC-2 was used to continue the ongoing investigation of the
M87 jet that had previously used the FOC. The investigators will compare
FOC and WFPC2 images to track secular changes and motions in the jet and
nucleus. During this proposal, the re-acquisition failure described in 2.1
and HSTAR 8168 occurred, affecting five observations. Otherwise, the
observations completed nominally.
1.27 Completed WF/PC-2 8173 (Alignment and Evolution of Redshift One
Radio Galaxies)
The WF/PC-2 was used to observe galaxies associated with powerful
distant radio sources which are the most massive ellipticals known at early
cosmic epochs, and are also uniquely important for understanding the
physics of AGN and the interactions between the radio source and its
environment. The observations completed with no reported problems.
1.28 Completed STIS/CCD 8667 (Nuclear Stellar Disks in Early Galaxies:
Black Hole Masses and Disk/Bar/Bulge Evolution)
The Space Telescope Imaging Spectrograph (CCD) was used to image of
an additional four E/SO galaxies to: {1} test whether the unusual
M_bh/M_bulge ratio is typical of these nuclear disk galaxies and {2} search
for additional ring/bar structures will help determine the source of the
accreted material and the time sequence of the disk/bar/bulge/Black Hole
fueling connection. The observations completed with no reported anomalies.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 22
Successful: 22
Scheduled Re-acquisitions: 27
Successful: 26
Per HSTAR 8168, the re-acquisition at 105/095204Z failed when the
scan step limit was exceeded on FGS-2. The proposals detailed in 1.10 and
1.26 were affected.
2.2 FHST Updates:
Scheduled: 48
Successful: 48
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared nine times.
The SSR pointer was set at 104/1212Z as directed by ROP SR-3.
There was a STIS EMC re-try at 104/192530Z. The STIS flight
software error counter was cleared at 104/2024Z per ROP NS-12.
A TTR was written for a required re-transmit at 106/081845Z during
a command load uplink.
The CCS engineering status buffer limits were adjusted at
106/0826Z, using ROP DF-18A.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
Continuation of normal science observations and calibrations.
