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NATIONAL
OPTICAL
ASTRONOMY
OBSERVATORIES
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
Cerro Tololo Inter-American Observatory
Kitt Peak National Observatory
National Solar Observatory
La Serena, Chile
Tucson, Arizona 85726
Sunspot, New Mexico 88349
ANNUAL REPORT
October 1995 - September 1996
October 31,1996
TABLE OF CONTENTS
I.
INTRODUCTION
II.
AURA BOARD
III.
SCIENTIFIC PROGRAM
A.
IV.
Cerro Tololo Inter-American Observatory (CTIO)
1. The Binary-Star Content of Globular Clusters
2. White Dwarfs and the Age of the Milky-Way Disk
3. A Census of the Outer Solar System
2
3
B.
Kitt Peak National Observatory (KPNO)
1. Dynamical Processes in Giant H II Regions
2. Large-Scale Streaming in the Galactic Halo
3. Structure and Dynamics of the Coma Cluster of Galaxies
3
3
4
5
C.
National Solar Observatory (NSO)
6
1. First Results from GONG
6
2. Acoustical Events as Source of the Global P-mode Energy
3. Chromospheric He I Observations: Looking for Solar Wind and Coronal Rain
8
8
DIVISION OPERATIONS
9
A.
Cerro Tololo Inter-American Observatory
1. CTIO Telescope Upgrades and Instrumentation
2. Facilities Operations
9
9
15
B.
Kitt Peak National Observatory
1. New KPNO Programs in FY 1996
2. KPNO Observing Improvements
3. KPNO Instrumentation Improvements
17
17
18
19
C.
National Solar Observatory
20
1. Kitt Peak
20
2. Sac Peak
23
D.
US Gemini Program
25
E.
NOAO Instrumentation Program
27
V.
VI.
MAJOR PROJECTS
30
A.
B.
Global Oscillation Network Group
Precision Solar Photometric Telescope
30
32
C.
SOLIS
32
D.
CLEAR Feasibility Study
33
CENTRAL COMPUTER SERVICES
Vn. SCIENTIFIC STAFF
A.
B.
C.
CTIO Scientific Staff Changes
KPNO Scientific Staff Changes
NSO Scientific Staff Changes
34
38
38
38
39
VIII. DIRECTOR'S OFFICE
39
EX.
NOAO STATISTICS
40
40
A.
CTIO Statistics
B.
KPNO Statistics
41
C.
NSO Statistics
42
D.
NOAO Tucson Headquarters Building Statistics
42
APPENDICES
Appendix A
Appendix B
Appendix C
Appendix D
NOAO Technical Reports List
CTIO Publications List
KPNO Publications List
NSO Publications List
I.
INTRODUCTION
This report covers the period 1 October 1995 - 30 September 1996.
The National Optical Astronomy Observatories (NOAO) are operated by the Association of
Universities for Research in Astronomy, Inc. (AURA), for the National Science Foundation (NSF).
The four divisions of the NOAO are: the Cerro Tololo Inter-American Observatory (CTIO) in
northern Chile; the Kitt Peak National Observatory (KPNO) near Tucson; the National Solar
Observatory (NSO) with facilities on Kitt Peak and at Sacramento Peak, New Mexico; and the US
Gemini Program (USGP) based in Tucson. NOAO observing and data reduction facilities are
available to the entire astronomical community. The NOAO Home Page contains on-line
information about NOAO services, including telescope schedules and instrument availability, and
information about how to apply for telescope time. The NOAO Home Page can be accessed through
the World Wide Web at http://www.noao.edu/.
II.
AURA BOARD
The NOAO is an operating center managed by AURA, a private, non-profit corporation. There are
twenty-eight AURA member institutions, including three international affiliates. The member
institutional representatives elect a governing Board of Directors, consisting of thirteen directors
(including the President, ex-officio). In addition to NOAO, AURA operates and manages the Space
Telescope Science Institute under contract with NASA, and the international Gemini Project under
cooperative agreement with the NSF.
III. SCIENTIFIC PROGRAM
The following paragraphs describe only a few of the many ongoing programs of research carried out at
the National Optical Astronomy Observatories. The programs described here are representative of the
important contributions to scientific research made by NOAO astronomers and NOAO facilities.
A. Cerro Tololo Inter-American Observatory (CTIO)
1. The Binary-Star Content of Globular Clusters
The fraction of binary stars is a basic parameter of any stellar population. The number and
types of binary stars are potentially important indicators of the mechanisms by which the
stars formed. For dense stellar systems such as globular clusters, the dynamical evolution
of the system is intimately tied to the number and type of binary stars present. Perhaps the
most dramatic consequence of a population of primordial binaries is their tendency to delay
the onset of core collapse.
While initial studies suggested that globular clusters were deficient in the fraction of
binaries compared to field stars, a number of more recent results all conclude that the
fraction of binaries in globular clusters is roughly comparable to that in the field
population. While the current fraction of binaries in globular clusters seems now to be well
established, the exact distribution of periods for globular-cluster binaries is still not well
known; as we shall see, this could have a bearing on our conclusions concerning the
primordial population of binaries.
In two studies, Patrick Cote (DAO) and his collaborators address the question of binaries in
globular clusters in very different regimes of orbital period. Using the Argus multi-object
spectrograph on the Blanco 4-m telescope, Cote and Philippe Fischer (Michigan U.) have
searched for main-sequence binaries with very short periods, between 2 days and 3 years,
in the cluster M4. In a sample of 33 main-sequence stars, two show velocity differences of
greater than 10 km/s in observations separated by 11 months. Including the efficiency for
discovering binaries with different periods and orbital parameters, Cote and Fischer's result
yields a binary fraction of 15% in M4.
In a companion study, Cote, Carlton Pryor (Rutgers U.), Robert McClure, J.M. Fletcher and
James Hesser (DAO) search for long-period binaries by combining observations of the
velocities of red giants in the globular cluster M22 taken over a period of 22 years at
Palomar, CFHT, MMT and CTIO. The complete data set, which consists of 333 repeat
velocity measurements for 109 stars, does not contain a single star that shows a velocity
difference greater than 7 km/s. These observations lead to a binary fraction of < 1%
assuming circular orbits; a binary fraction of < 3% results if the assumption of circular
orbits is relaxed. A possible explanation for the difference in the binary fraction between
the short-period, close binaries in M4 and the long-period, wide binaries in M22 is that
loosely bound, wide binaries are more easily disrupted by encounters with other stars than
are tightly bound, short-period binaries. Thus, a primordial population of long-period
binaries could be destroyed over the life of the cluster.
2. White Dwarfs and the Age of the Milky-Way Disk
White dwarfs are the remnants of low-to-moderate-mass stars after they have completely
exhausted their nuclear fuels; our Sun will eventually become a white dwarf in another five
billion years. An important result which has come from surveys for faint white dwarfs in
the vicinity of the Sun is the absence of low-luminosity, cool white dwarfs. With no
internal energy sources, white dwarfs simply cool and grow fainter as they age. Thus the
temperatures and luminosities of a white dwarf serve as a cosmic clock, recording the time
which has passed since the white dwarf formed. The lack of white dwarfs below a certain
critical luminosity indicates that insufficient time has elapsed for these oldest white dwarfs
to cool beyond this limiting luminosity. Thus, the ages of the least luminous white dwarfs
that can be found provide a lower limit for the age of the disk of the Galaxy.
A necessary step in establishing the age of a white dwarf is to derive quantities such as the
temperature, composition and surface gravity of the star from the available observations.
Pierre Bergeron (U. of Montreal), Maria Teresa Ruiz (U. de Chile), and S.K. Leggett (U. of
Hawaii) have recently completed an extensive study which used the colors and spectra from
a large sample of cool white dwarfs to calibrate a state-of-the-art sequence of model
atmospheres. The model atmospheres provide the transformation from observed quantities
into physical quantities such as the temperature and surface gravity.
Observations were made of 110 white dwarfs, primarily using the telescopes at CTIO.
These observations included optical spectroscopy with the CTIO 4-m, infrared photometry
with the CTIO 4-m and 1.5-m, and optical photometry with the CTIO 1.5-m and 0.9-m. The
principal result of this work is a calibrated and verified set of model atmospheres that
describe the observable properties of the coolest white dwarfs.
These model atmospheres can be used to derive the temperatures, masses and luminosities
for faint white dwarfs found in present and future surveys. When combined with models for
how the temperature and luminosity of white dwarfs change with time as these stars cool,
refinements to the model atmospheres should improve the accuracy with which the white
dwarf luminosity function may be used to reconstruct the star formation history in the disk
of the Galaxy. The oldest white dwarfs in the sample used to calibrate the model
atmospheres have ages in the range of 6.5 to 10 billion years. Since this sample is not a
complete sample of stars, these ages are strictly a lower limit to the age of the Galactic
disk.
3. A Census of the Outer Solar System
Much closer to home, the number and sizes of small, icy bodies in the outer solar system is
still poorly known. It is only within the last twenty years that the first of the Centaurs,
100 km-sized objects with orbits between Saturn and Neptune, was found. And it has only
been within the past few years that similar objects orbiting beyond Neptune, the Kuiper belt
objects, have been discovered. In an effort to improve our knowledge of the contents of the
solar system beyond the orbit of Saturn, David Jewitt (U. of Hawaii), Jane Luu (Harvard
U.), and Jun Chen (U. of Hawaii) have recently completed the Mauna Kea-Cerro Tololo
survey for Centaurs and Kuiper-belt objects. Jewett, Luu, and Chen employed the CTIO
1.5-m telescope to extend coverage into the Southern ecliptic plane for a survey that was
begun using the UH 2.2-m telescope on Mauna Kea. The survey revealed 15 new Kuiper
Belt objects and 2 Centaurs, bringing the total number of Kuiper Belt objects to 32 and
Centaurs to 6. The inferred number of objects in the Kuiper belt at 30 AU to 50 AU
heliocentric distance with diameters greater than 100 km is approximately 70,000. The total
population of Centaurs with diameters greater than 75 km is about 2600.
B. Kitt Peak National Observatory (KPNO)
1. Dynamical Processes in Giant H II Regions
A giant H II region is a complex of newly formed stars and ionized, neutral and molecular
gas, which can contain over a million solar masses of material. The nearest example is the
30 Doradus region in the Large Magellanic Cloud. These are sites of active star formation
and deposition of mechanical energy into the host galaxy's interstellar medium. From
studies of many such regions, correlations have been found between the luminosity radiated
in the H beta line of hydrogen, the physical diameter of the giant H U region, and the
integrated velocity width of the emission line. Such correlations suggest unifying
underlying physical mechanisms, and several models have been proposed. These models
include energy injection from stellar winds, bulk motions induced by supernovae and their
remnants, and the overall motions expected of material bound in a gravitational potential.
To explore the physical mechanisms in detail, adequate spatial and velocity resolution are
required. Yang (U. of Minnesota), Chu (U. of Illinois), Skillman (U. of Minnesota), and
Terlevich (Royal Greenwich Obs.) reported in the July 1996, Astronomical Journal on their
study of the giant H II region NGC 604 in the very nearby galaxy M 33. Key components of
their database were longslit echelle spectrograms taken with the Mayall 4-m telescope, and
narrowband images obtained on the KPNO 2.1-m telescope. The echellograms were taken
in a single spectral order to provide an emission-line map ~ 2 arcmin long with velocity
resolution of ~ 27 km/s. Nine E-W slices and 2 N-S slices were taken in Ha to produce a
2-dimensional velocity map.
The emission region is very complex, with four expanding shells identified. One is
probably asymmetric because of its encounter with an associated molecular cloud; the
largest expansion velocity is over 100 km/s. With densities derived from emission line
diagnostics and accurate velocity maps, the kinetic energy requirements for driving the
shells were derived. They were found to exceed by a factor of at least 3 the energy in stellar
winds associated with the hot young stars observed in Hubble Space Telescope images of
the region. The extra energy is likely to be attributable to supernova remnants because of
the high expansion velocities and the bright, diffuse X-ray emission associated with the
shells.
The integrated velocity profile of the H U region has a core with velocity width of 42 km/s
and broad wings produced by the fast expanding shells from stellar winds and supernova
remnants. Individual emitting sub-regions show line widths of -36 km/s. The gas
temperature of 8550 K would produce emission lines of only -20 km/s from thermal
motions. Additional broadening is consistent with the motion of gas in the gravitational
potential of the 4.7 million solar masses of material in the region. The remaining
discrepancy between 36 km/s and 42 km/s is again attributable to the higher velocity
regions with stellar winds and supernova remnants, which produce about 1/3 of the total
emission line flux.
The conclusion is that the observed velocity profiles in this giant H II region are produced
from about equal contributions of internal thermal motion, stellar winds and supernova
remnants, and motion in the gravitational potential. Observations in similar detail are
required in a number of other regions to verify the global correlations between power, size,
and velocity, and to assess the universality of the physical mechanisms at work.
2. Large-Scale Streaming in the Galactic Halo
The spherical halo of the Galaxy was long thought to represent the earliest phase of the
Galaxy's formation. Halo stars are very metal-poor, and early samples showed them to have
little rotation, in comparison with the rapidly rotating disk. Those facts suggested to Eggen,
Lynden-Bell, and Sandage in 1962 that the halo consisted of stars formed during a phase of
spherical collapse, with little angular momentum and weak metal enrichment. Newer data
collected by S. Majewski (U. of Virginia) and colleagues indicate that the formation history
of the halo may be much more complex.
Majewski's original dataset consisted of stars with accurately measured proper motions
near the North Galactic Pole. He developed that sample from photographic plates taken at
the prime focus of the Mayall 4-m Telescope on Kitt Peak over a baseline of some 15 years.
The random error of proper motions of stars as faint as B = 22 mag is 0.1 arcsecond/
century, and the proper motions are tied to the stationary frame of quasars and galaxies in
the field to better than 0.01 arcsecond/century accuracy. From that sample, he found that
the true halo population does not begin to dominate until distances above the Galactic plane
of greater than 5.5 kpc, below which there is an extended or thick disk. A surprising result
was that the true halo objects appear to be rotating in retrograde motion of some 55 km/s,
instead of being at rest with respect to a disk rotation of 220 km/s. That result contradicts
the spherical collapse picture in which angular momentum is conserved in the rapidly
rotating disk; a retrograde halo has angular momentum in the opposite direction to that of
the disk!
The first conclusions were based on proper (angular) motions only. Radial velocities
complete the full 3-dimensional distribution. In the direction of the North Galactic Pole, the
radial velocities are directed almost exactly toward or away from the Galactic plane. In the
Astrophysical Journal Letters of 10 March 1996, Majewski, J. Munn (U. of Chicago), and
S. Hawley (Michigan State U.) report on Hydra multi-fiber spectroscopy of the NGP field.
They obtained over 200 new radial velocities for stars with previously measured proper
motions with distances out to 8 kiloparsecs from the plane. They found that the stars tend to
be concentrated in groups with common space velocities and metallicities. One of the most
distinct groups is metal-poor, and is moving toward the Galactic plane with a mean velocity
of 56 km/s. That result is consistent with two previous surveys in the same direction, with
negative net radial velocities of blue horizontal branch stars, RR Lyrae variables, and A
stars. In the initial sample, there are very few stars that are not associated with one of the
major common motion groups. The consequence is that the halo is dynamically young, with
comingling but identifiable streams of stars of different ages, metallicities and trajectories,
presumably from capture of satellite systems by the Milky Way. This "can of worms"
model for the halo may explain seemingly discrepant results of surveys of the halo in
different directions. Each line of sight may intersect different streams with unique local
trajectories dominating the population sample. If that is the case, the entire halo may not be
in retrograde rotation, but the halo from 5 to 10 kpc in the direction of the North Galactic
Pole is dominated by a stream heading retrograde and down. Ultimately, such studies
should allow us to trace the formation history by accretion and tidal shredding of a
population of satellites to form the extended, tenuous stellar halo of the Galaxy.
3. Structure and Dynamics of the Coma Cluster of Galaxies
Ongoing observations of the rich Coma Cluster have revealed a cluster in an active
dynamical state. It contains at least three giant D and cD galaxies, shows a two-component
X-ray morphology, and displays different velocity dispersions for the early and late type
galaxies. The signature of the dynamical history of the cluster should be found in the
relative motions of the galaxies within it. Although substantial redshift surveys have been
undertaken in the past, the Hydra multi-fiber spectrograph has created the opportunity to
nearly double the available sample. Finding a significant signal of substructure and mergers
is now possible with the new redshift database.
M. Colless (Mt. Stromlo & Siding Spring Obs.), and A. Dunn (Inst, of Astronomy,
Cambridge) report in the Astrophysical Journal of 20 February 1996, on their reanalysis of
the dynamics of the Coma Cluster based on 243 new redshifts obtained with Hydra plus the
bench spectrograph on the KPNO 4-m telescope. Their total sample of cluster members was
552 galaxies. The velocity distribution of the entire sample is inconsistent with that of a
single, relaxed population. With a new test for localized departures from a Gaussian
velocity distribution, they found a highly significant substructure of galaxies around the cD
galaxy NGC 4389, 40 arcminutes SW of the cluster core. That location is essentially
identical to the secondary peak of X-ray emission. They applied a mixture-modeling
algorithm to assign galaxies to the main cluster and to the NGC 4389 subcluster; the main
Coma Cluster is centered on the giant NGC 4874 with a mean recession velocity of 6853
km/s and a dispersion of 1082 km/s. The NGC 4389 cluster has a mean recession velocity
of 7339 km/s and a dispersion of 329 km/s.
Using only the galaxies assigned to the main cluster, Colless and Dunn found that the
apparent velocity dispersion of the late-type galaxies is V2 x the dispersion of the earlytype galaxies, confirming earlier suggestions that the spirals are freely falling into a
virialized cluster dominated by early-type systems. They calculated the virial mass for the
main cluster to be 0.9 x 1015 solar masses, in excellent agreement with the X-ray results.
The smaller cluster around NGC 4389 is bound and contains 5-10% of the mass of the main
cluster, again in good agreement with the X-ray observations.
A linear two-body model suggests a most probable orbital configuration for the two
clusters. That solution has the NGC 4389 cluster bound to the Coma Cluster, with the two
clusters projected at 74° to the line of sight with a true separation of 0.8 Mpc and
approaching each other at 1700 km/s. The existence of NGC 4389 as a cD central galaxy,
the low velocity dispersion, and distinct X-ray emission all suggest that the NGC 4389
cluster is about to make its first encounter with the Coma Cluster, and has not yet been
disrupted by a passage through the main cluster. The NGC 4389 cluster is approaching the
main cluster from the direction of the Great Wall.
There appears to be some substructure within the main body of the Coma Cluster itself,
consisting of two subclusters: a true central peak close to the projected position of NGC
4874 with mean recession velocity of 6800 km/s, and a secondary peak near NGC 4889
with mean velocity of 7600 km/s. Neither of the giant galaxies lies near the velocity center
of its associated spatial sub-condensation. A possible scenario is that the NGC 4889 group
is in the process of completing a merger with the larger Coma Cluster group. NGC 4889
itself was ejected from the cluster central potential and lost its cD halo in the process. NGC
4874 was also ejected from the center of the main gravitational potential, and its apparent
cD halo could be a projection effect against the stellar population still trapped there.
This study represents another example of the qualitative gains of multi-fiber
spectroscopy—in this case, revealing the active dynamical processes at work in the Coma
Cluster. Models of mergers and ongoing dynamical relaxation have been previously
proposed, but significant results depend on significant quantities of imaging and
spectroscopic information.
C. National Solar Observatory (NSO)
1.
First Results from GONG
The GONG network became operational in early October 1995. It has lived up to our hopes
in terms of operational reliability, observing duty cycle, instrument performance, and data
processing capabilities. In addition, the GONG scientific teams—which have been working
together since the conception of GONG to define the scientific program and to prepare the
analysis techniques—were able to get to work rapidly and effectively. The first fruits of
their efforts appeared in a special issue of the journal Science on 31 May. Within the
colorful GONG cover, this issue contains seven articles, resulting from the contributions of
71 different authors and a supporting cast of hundreds. These first results just scratch the
surface, in terms of the accuracy and precision that will progressively improve as the data
collection, and our understanding of its interpretation, proceeds. Nevertheless, they are
extremely heartening in terms of what they already show and what they promise for the
future. It is clear that we are entering a whole new realm of analysis in terms of the care
and subtlety required to pursue inference from data with such high frequency resolution
and low noise.
The GONG Project was undertaken to test models of stellar structure. It appears that the
adiabatic stratification in the Sun penetrates more deeply than in the Standard Solar Model.
Part of the difference in u (= p/p) between Sun and model could be associated simply with
the fact that the model convection zone may be too shallow. However, the excess u caused
by that effect is of lesser magnitude than that found, and extends more deeply. A small
increase in u between 0.3 Rsun and 0.6 Rsun might be accounted for in this manner, but a
relatively substantial, localized bump between 0.6 Rsun and 0.7 Rsun cannot. The decrease in
u immediately beneath the convection zone may arise from the accumulation of helium
(which augments the mean molecular mass) which has been overestimated in the reference
model. The bump could in principle have been produced by an opacity error that drops
abruptly to zero immediately beneath the base of the convection zone; such a fortuitous
occurrence is unlikely. The discrepancy in the core is the third prominent feature. Most
secure is the lower value of u between about 0.1 Rsun and 0.2 Rsun, which implies that the
variation of u itself is flatter than in the model. Once again this would be a symptom of too
steep a composition gradient in the model, which here has been produced by nuclear
reactions. The density variation is consistent with this interpretation: the regions of
relatively steep positive slope in 5p/p in the core and immediately beneath the convection
zone imply that the magnitude of the (negative) gradient of density is too high in the model.
In addition to helioseismic inferences of the solar interior structure, GONG's measurements
of the velocity of the solar surface are of interest for the measurement of its nearly steady
motions—large scale flows and convection, as well as rotation—all of which are thought to
play important roles in generating the Sun's magnetic field. The differential rotation
stretches meridional magnetic field lines to form strong toroidal fields (field in longitudinal
rings about the Sun's rotation axis). The meridional circulation transports magnetic flux
and angular momentum across parallels of latitude and from one radius to another. The
nonaxisymmetric convective motions also redistribute magnetic flux and angular
momentum in more complex and subtle ways. The Sun's differential rotation is accurately
determined from single GONG observations. The rotation profile with latitude agrees well
with previous measures, but also shows a slight north-south asymmetry. Rotation profiles
averaged over 27-day rotations of the Sun reveal the torsional oscillation signal: weak,
5 m/s, jet-like features, which are fairly broad (15° wide), associated with the sunspot
latitude activity belts. The latitudes of these features (18° north and 22° south) are slightly
poleward of the latitudes where sunspots were found during this period. The jets appear
consistently in three different temporal averages.
Stay tuned, GONG is just getting going.
2. Acoustical Events as Source of the Global P-mode Energy
Stebbins and Goode (1987) studied phase change with altitude in Doppler velocities in one
horizontal dimension in the p-mode band of frequencies and noted that these phase changes
in certain temporally and spatially isolated events were much too large to be explained as
(nearly evanescent, or phase-change-less) p-modes. Goode, Gough, and Kosovichev (1992)
modeled these occurrences as traveling waves which are excited in impulsive acoustical
events, and conclude that these events occur less than 200 km below the photosphere, and
that many of the 5-minute modes are excited by them.
Rimmele, et al. (1995) studied three-dimensional velocity data derived from high-resolution
observations and noted that the acoustical events occur preferentially in the intergranular
lanes, and are associated with an extra darkening of the lane just prior to the maximum of
the energy flux at the surface (the acoustical flux) in the traveling waves. They argued that
the excitation of solar p-modes is closely associated with the cooling and collapse of the
solar surface which follows convective overshooting—rather than arising from the
drumming by the convective overshooting itself. They also demonstrated that the acoustical
flux is comparable to the energy that is required to power the entire p-mode spectrum.
Rimmele, et al. (1995b) demonstrated an anticorrelation between the acoustical flux and
the line-center intensity in a magnetically non-sensitive (g = 0) spectral line. Since
moderate magnetic flux density enhances line-center intensity (Chapman and Sheeley,
1968; Solanki 1993), they conclude that acoustical flux is suppressed by magnetic field.
Strous (1996, work in progress) averages the characteristics of the largest 2,000 acoustical
flux events in his data set and shows that the average acoustical event occurs off to the side
of the intergranular lane, and that the lane apparently narrows at the height of the acoustical
event. He also notes a significant residual 5-minute oscillation in the average velocity,
which may point at a correlation between the occurrence of an acoustical event and the
phase of the dominant p-mode(s) at that time and place, thus leading to a feedback loop in
p-mode generation.
In summary, we now have strong indirect evidence that the acoustical events pump power
into the p-modes. We are currently looking for direct observational evidence of this.
Chapman and Sheeley, 1968, Solar Physics, 5, 442
Goode, Gough, and Kosovichev, 1992, AstrophysicalJournal, 387, 707
Rimmele, Goode, Harold, and Stebbins, 1995a, Astrophysical Journal, AAA, 119
Rimmele, Goode, Strous, and Stebbins, 1995b, Proceedings SOH04, 1,219
Solanki, 1993, Space Science Reviews, 63, 1
Stebbins and Goode, 1987, Solar Physics, 110, 237
3. Chromospheric He I Observations: Looking for Solar Wind and Coronal Rain
Imaging spectroscopy with the NASA/NSO Spectromagnetograph at the NSO Kitt Peak
Vacuum Telescope has been used to study dynamic events in the solar atmosphere. Recent
work (Penn and Jones, 1996; Dupree, Penn, and Jones, 1996; Penn and Allen, 1996) has
used line profile measurements of the He I 1083 nm absorption feature to study outflows,
downflows, spicules, and oscillations high in the solar chromosphere.
The He I absorption line is very weak (with a central depth of only a few percent of the
intensity of the continuum), but data from the KPVT have been used to measure the
asymmetry of the line profile (Dupree, Penn, and Jones, 1996). In the quiet Sun outside of
coronal holes no line asymmetry was observed. But the line profile showed a blue
asymmetry, consistent with an outflowing gas component, in large regions of coronal holes
near the solar poles. The asymmetry varied with the cosine of the viewing angle, suggesting
that the gas flow was radial on the Sun, with an outward velocity of 8 km s'1. Although
there have been no previous observations of the solar wind outflow in the chromosphere,
polar coronal holes have long been known to be a source of the high speed component of
the solar wind. Some recent modeling of coronagraph data (Habbal, Esser, Guhathakurta,
and Fisher, 1995) suggests that significant acceleration of this wind may occur at low
heights, and these initial KPVT data may be measuring part of that acceleration. More work
is in progress to follow up these early results.
In contrast to the broad outflow regions, redshifts in the He I line are observed in spatially
compact features scattered across the whole solar disk. Time series observations (Penn and
Allen, 1996) have shown that these downflow events undergo significant morphological
changes during their lifetime, and often show large transverse velocities. The events have
broad spectral line widths, indicating that turbulent or high temperature plasma is involved.
It is not clear where the downflow material originates; is it a return of the previously
discussed outflow? Is it associated with macrospicule eruptions? Or are these downflow
events true condensation of hotter coronal plasma, perhaps a cool coronal rain associated
with coronal loop interactions seen in higher temperature lines (Airapetian and Smartt,
1995)? These questions will be answered when data from the Solar and Heliospheric
Observatory (SOHO) are combined with simultaneous KPVT observations to measure the
dynamics of both hot and cold components of the coronal plasma.
Airapetian and Smartt, 1995, Astrophysical Journal, 445, 489
Dupree, Penn, and Jones, 1996, Astrophysical Journal, 467, L121
Habbal, Esser, Guhathakurta, and Fisher, 1995, Geophysical Research Let., 22, 1465
Penn and Jones, 1996, Solar Physics, in press
Penn and Allen, 1996, Solar Physics, submitted
IV. DIVISION OPERATIONS
A. Cerro Tololo Inter-American Observatory
1. CTIO Telescope Upgrades and Instrumentation
CTIO's program continues to focus on upgrading and instrumenting our telescopes so that
they remain at a high level of scientific productivity in an era of modern 4-m and 8-m
apertures. The Gemini 8-m project is well advanced on Cerro Pachon, and it should have a
modern 4-m companion in the SOAR telescope. Various NOAO/CTIO in-house projects
will be coming on-line in the next 3-5 years, and we anticipate that CTIO technical and
scientific resources will be used extensively in the SOAR (and possibly Gemini)
instrumentation and commissioning. The combination of SOAR and the Blanco 4-m, and
their instruments, will be configured as far as possible—through sharing arrangements
between the 4-m telescopes—as a complementary observing system in support of work
with Gemini.
4-m Upgrades
A main focus in FY 1996 continued to be upgrading the performance and general
maintainability of the Blanco 4-m Telescope. The addition of active optics, image analyzer,
and careful thermal monitoring and controls over the past several years have been very
successful, and delivered image performance has improved significantly.
The image analyzer has been in routine use at the Cassegrain focus during the year, which
has allowed the active primary support system and careful collimation of the prime focus
and secondaries to deliver optical images as good as 0.56 arcsec FWHM. During FY 1996
monitoring of the thermal environment of the telescope and dome has been extensive.
Analysis of the data produced by the many temperature probes installed on the telescope
and on the dome interior has indicated that heat sources in the dome and building interior
are still significant; control and removal of these heat sources are being addressed. The
primary-mirror cooling system is run for up to several hours each day to try to bring the
mirror to within 0.5 degree of the estimated mean nighttime air temperature. The system is
under computer control, and we are experimenting with the algorithm so as to improve the
accuracy of the nighttime temperature prediction. The capacity of the cooling system has
proven to be marginal during wintertime, and we are investigating ways to improve this. An
air extraction system was installed to flush the primary mirror cell and chimney area during
observing, which has also helped to maintain proper mirror temperature.
During this year, a 10-week shutdown of the 4-m was undertaken for several purposes:
1) to renovate the old control wiring and logic; 2) to test the servo performance to
investigate guiding and tracking issues; and 3) to upgrade aspects of the TCS and computer
control system. Most of the control wiring and logic for the 4-m was more than 20 years
old. Not only was the performance well below today's standards, but it is no longer
possible to get spare parts for basic elements such as encoders and drive servos. During the
shutdown, the antiquated 4-m telescope control logic has been replaced with a modem
programmable- logic-controller-based system, following the upgrades made to the KPNO
4-m several years ago. With the improvement of the optical quality of the telescope,
tracking and guiding performance have become limiting factors on delivered image quality.
During FY 1996 (and continuing into FY 1997) effort has therefore been devoted to
studying and improving the servo systems performance. Initially this involved careful
tuning of the existing servo system and the addition of filters and ramps in the servo loop,
which has been accomplished in the shutdown. We have also begun a pilot project to
replace the actual servo system itself, to provide a modem and maintainable level of
performance.
Previously the telescope has tracked at a fixed rate in RA and not at all in Dec. A number
of effects including misalignment of the polar axis, flexure, and refraction, result in
position-dependent tracking rates. These terms are included in the pointing model. In order
to improve the open loop tracking, tracking corrections are now being derived from the first
derivative of the pointing model.
The Cassegrain instrument rotator is now being controlled via a Smart Motor Controller
rather than manually. This will allow for example, the spectrograph slit to be set to the
parallactic angle while the telescope is slewing to the target coordinates and the guide
10
probe is being moved to the position of a suitable guide star. The scope of the project was
extended to include the handling of signals passed through the old MUX system such as the
readout of the guide probe position, and control lines for the rotator mirror and the image
analyzer. This has the laudable goal of eliminating the old CAMAC system, which has been
a source of heat as well as an increasing maintenance problem.
Major Instrumentation Efforts
A major feature of the program in the past year has been preparations for new instruments
which are due to arrive in 1997-98. In collaboration with the Tucson IPG effort, we will be
equipping the Blanco 4-m with: a) the Cryogenic Optical Bench (COB) with at least a
512 x 512 InSb array; b) the NOAO 8K Mosaic imager at prime focus; c) the Phoenix highresolution IR spectrometer; and d) the Hydra/CTIO multi-fiber spectrograph. Thus within
two years we should have a 4-m telescope with excellent image quality over a small field at
f/14, mainly for near IR imaging and spectroscopy. In the optical, the wide-field aspects are
emphasized with the Mosaic imager and Hydra spectrograph; the telescope will be able to
deliver good image quality over a 45 arcmin field.
During the past year, work has started on a new 400 mm camera for the 4-m bench
spectrograph. Most of the optical figuring has been finished, and the camera will be
installed next year, for initial implementation with the Argus multifiber spectrograph.
Remaining aspects of the spectrograph will be modified next year in preparation for the
Hydra system, involving a change in collimator and detector, to accommodate the slower
f/ratio in the change from the prime focus to Cass and the larger number of fibers (from 48
to 138). A SITe 2K CCD has been purchased and will be the detector for this system.
One of our top-priority projects has been the implementation of the new f/14 secondary
mirror on the 4-m telescope. The goal is to make our IR instrumentation compatible with
the KPNO 4-m (f/15) and Gemini (f/16). The new secondary is also being installed with
piezo-electric actuators in place to make it "tip-tilt ready." This will give CTIO the only
major ER tip-tilt capability in the southern hemisphere. This is the logical extension of the
program to improve the imaging capability of the Blanco Telescope. The emphasis needs to
be on the near IR (JHK) because this is where tip-tilt achieves the greatest proportional
gains in image diameter for a 4-m telescope with good seeing. This will produce an
important improvement in the performance of our near-IR instrumentation.
This project to implement the tip-tilt capability for IR imaging and spectroscopy and also
for optical imaging began in FY 1995 and is now more than half complete. Some delays
have occurred due to difficulties with the final figuring of the secondary; it will be installed
in early September 1996. The guider box at the Cassegrain focus uses a dichroic or
beam-splitter to feed light from a guide star through re-imaging optics to a fast CCD
camera. The guider box will have a remotely controlled x-y stage for the guide camera, and
eventually will offer remotely controlled selection between different dichroics and beam
splitters. The fast CCD camera is an upgraded version of our existing CCD-TV acquisition
cameras, and has been shown in lab tests to work at 700 Hz for small readouts, with
acceptable noise performance. The project includes a significant software effort to make
the system efficient to use for visiting astronomers. The guider box and fast CCD are
scheduled for engineering tests on the telescope in October-November 1996. The principal
remaining work (which will carry over into FY 1997) will thus be software, user interface,
and integration of the tip-tilt system.
11
This tip-tilt focus will feed the Cryogenic Optical Bench (COB), which is being upgraded
by the Tucson IPG with a InSb array with at least 512x512 usable pixels. COB is
scheduled for engineering tests on the Blanco Telescope in early FY 1997. In preparation
for COB, cryocoolers and associated plumbing are being installed in both the 4-m and in
the La Serena laboratories.
CCD Implementation and Arcon Controller Development
Implementation of CCDs on our telescopes and the development of the Arcon controller
continued to be a central part of our optical instrumentation program this year. All of our
detector systems are now under Arcon control and continue to work reliably; our ancient
VEB CCD controllers were finally retired this year. Two new CCDs were implemented:
•
A thinned Loral 1200 x 800 CCD was successfully commissioned on the spectrograph
of the 1.5-m telescope. This chip replaced a small-format, thick, GEC CCD, and the
resultant throughput gains are more than a factor of two. It has been in routine use
throughout the year.
•
A SITe 2048 x 2048 CCD (with two good amplifiers) was purchased, eventually to be
used for the Hydra spectrograph. It will be used initially as an imaging system (thus we
will have four 2K chips running, including the STIS on the Schmidt), and then will be
dedicated for use with the Argus/Hydra spectrograph. First science use is scheduled in
September 1996.
During FY 1996 a major effort has gone into production of the five Arcons needed for the
NOAO 8K Mosaic Imager system; this integrated hardware and software effort is finishing
now, and the system should be delivered to Tucson in September 1996. Several engineers
and scientists from CTIO have participated in engineering runs at KPNO in May, June, and
September 1996 as part of this project.
During the Arcon development work over the past year, hardware and software upgrades
have allowed a speed improvement of more than a factor of two, and current systems on
Tololo are capable of reading out a conventional CCD at 100K pix/sec/channel. For the
Mosaic work, planned upgrades should allow a readout approximately twice this fast, or
200K pix/s/ch. We intend to begin retrofitting the existing ARCONS on CTIO with the
final versions of three new controller electronics cards (Video, VTT and ADC), which have
been developed over the past year.
Small Telescopes
Our second largest telescope, the 1.5-m suffers from a poor thermal environment and
several optical problems with the secondary mirrors. Ventilation doors have been designed
and constructed for the 1.5-m dome, and are scheduled to be installed starting in October
1996. An array of 32 doors with a total area of over 500 square feet will be installed in the
segments around the lower rim of the dome. A new project has been started to provide
more stable secondary mirror mounts, with encoders to permit reliable collimation runs.
At the Schmidt, the long-awaited NFCCD mounting box, shutter/filterbolt and smart motor
controller were integrated and installed. The Schmidt now joins the 4-m in having a fully
automated focus from the Arcon user-interface, thus increasing observing efficiency. The
0.9-m now has the focus readout also via computer, with the focus motor control loop
12
scheduled to be closed near the end of September. The 1.5-m telescope is scheduled early
next year for a focus readout upgrade.
The Save-the-Bits (STB) software and dedicated exabyte drives have been installed on the
0.9-m and Schmidt telescopes. STB, a completely automatic data archiver, was transferred
to CTIO from the successful KPNO system. STB will be installed on other telescopes and
for use with IR data systems during engineering runs occurring in 1996-1997.
Other
Although Cerro Tololo and Cerro Pachon are still very dark sites, CTIO has become
increasingly concerned with the growing threat of light pollution from neighboring cities
and towns. Thus we have begun to collaborate with local officials as well as private
industry to ensure that future lighting installations are as "astronomer-friendly" as possible.
This program has concentrated on several fronts, including public information,
consultations on street lighting installation in local towns, and a regional light pollution
ordinance as part of a newly-created national environmental commission.
Following a meeting of the international SOAR consortium in Chapel Hill, North Carolina
in August, the following press release was issued in Tucson in mid-October along with
locally-tailored versions in Brazil, Chile, North Carolina and Michigan:
National Observatories to Get New Telescope through International Partnership
The Tucson-based National Optical Astronomy Observatories (NOAO) announced today
that they have entered into an international partnership to construct a new state-of-the-art
telescope. The telescope will have a primary mirror 4 meters (160 inches) in diameter,
comparable to that of the Mayall Telescope on Kitt Peak. The observatory will be located
in the western foothills of the Chilean Andes. The facility will be operated by the staff of
the National Observatories' Cerro Tololo Inter-American Observatory, with headquarters in
La Serena, Chile, on the coast about 300 miles north of Santiago.
The new telescope will be designed with actively controlled optics to produce images
sharper than those made by older generation 4-meter telescopes. The new WIYN Telescope
on Kitt Peak is of similar design, with the primary mirror resting on a bed of dozens of
computer-controlled supports. WIYN routinely produces the sharpest images of any
ground-based telescope of its size. A small, rapidly deformable mirror can be added to
compensate for the blurring of turbulence in the Earth's atmosphere. With that addition, the
new telescope will be capable of producing images in deep red light from the ground that
are as sharp as those of Hubble Space Telescope.
Astronomers will design the light-analyzing instruments to be operated remotely. Scientists
and students in their labs at their home universities or at the NOAO Tucson Headquarters
will then be able to carry out their observations on the telescope in Chile. The plan calls for
several instruments to be mounted on the telescope simultaneously. A quick change
capability will allow a wide variety of programs to be carried out during any observing
session.
The astronomical consortium chose the Southern Hemisphere site for several reasons: The
site has dark skies and clear, dry air. The location is near the large, existing Cerro Tololo
observatory and the new Gemini 8-meter telescope, now under construction and managed
by another international consortium based in Tucson. The Southern skies offer astronomers
13
the additional viewing advantage of our nearest neighbor galaxies, the Magellanic Clouds,
the center of our Milky Way Galaxy, and the brightest nearby stars. Many of these regions
of the sky are not accessible to existing telescopes situated north of the equator.
The telescope facility will be named SOAR, the Southern Observatory for Astronomical
Research. The international partnership consists of the US National Optical Astronomy
Observatories (NOAO) supported by the US National Science Foundation, the country of
Brazil, the University of North Carolina, and Michigan State University. The total project
cost is 42 million for constraction and operations. Astronomers are planning for the SOAR
telescope to be up and running within five years. NOAO will get about 1/3 of the time on
the SOAR telescope. Astronomers throughout the US will compete for that time on the
basis of project proposals. Astronomers from Chile will also get time on SOAR because the
country provides access to the excellent site.
An English-language Web page is being set up in Tucson for SOAR. Look under the
NOAO home page: http://www.noao.edu/ and click on SOAR (in the list of NOAO
Observatories and Telescope Projects).
2MASS at Cerro Tololo
2MASS is a project to carry out an all-sky infrared survey with 2.0" pixels to 10-sigma
limiting magnitudes of J = 15.8, H = 15.1 and K = 14.3. The sole existing large-area survey
in the near infrared, the Two-Micron Sky Survey, reaches only to 3rd magnitude, covers
just half the sky, and contains 5600 objects. With the 25,000-fold sensitivity improvement,
2MASS is expected to catalog 100 million point sources and hundreds of thousands of
galaxies and other extended objects. Near-term scientific objectives include the study of
Galactic structure via IR luminous stars visible throughout the galaxy, galaxies in the local
universe (imaged at wavelengths that characterize their underlying mass distribution), and
searches for rare objects such as brown dwarfs. Since the most exciting applications of the
2MASS database will probably be unforeseen ones, the Project team has a strong
commitment to making the completed Survey data available to the community without a
lengthy proprietary period.
Two telescopes of 1.3-m aperture are being constructed to carry out the survey—one will
be installed on Mount Hopkins, the other on Cerro Tololo. The project is being managed by
a group at the University of Massachusetts, with the data product to be produced by the
Infrared Processing and Analysis Center at Cal Tech. CTIO is acting as a contractor for
construction on the Tololo site, and will play some contract role in operations as well.
On 14 May CTIO scientific, engineering and administrative staff members met with the
UMass Project Manager to decide the most desirable site location for the southern 2MASS
Telescope, explore practical construction solutions, and discuss the future operation of this
telescope on CTIO. These meetings were later complemented with a visit to the designated
telescope construction site just below the GONG site above the North-East face of Tololo.
A month later, on 14 June, CTIO presented two proposals for the construction of the
enclosure and the control room (designs prepared by CTIO and 3M Engineering). UMASS
opted for the CTIO version, which uses reinforced concrete for the enclosure and
brickwork for the control room. We are currently working on the civil engineering design
detail and statement of work concepts. Construction work began on the site in September.
14
An outline description of the project and more information (so far mainly about the
identical northern telescope on Mount Hopkins) can be found at:
http://pegasus.phast.umass.edu/2mass/telescope.html.
2. Facilities Operations
This year the CTIO budget was once again afflicted by financial constraints that seem to
have become a permanent feature of our operations. This condition was further aggravated
by the fact that the budgeting levels were unknown until we were well into the fiscal year.
Certainly the most distressing result of these budget cuts was the formal Reduction In Force
in March, when approximately 12% of the Observatory workforce was laid off, culminating
in a series of observatory-wide staff reductions totaling more than 20% over the last three
years.
Following is a summary of the main activities performed in the Administrative Services
and Operations Division during the FY 1996.
Logistics and Administration Reduction in Force (RIF)
The loss of 16 people from Operations and Administration in less than 12 months has
brought with it the need to make a number of radical changes in the management strategies
of CTIO. The most relevant change was the merging of the Administrative and Operations
Divisions, in order to provide for a more efficient use of CTIO's shrinking manpower
resources.
IVA (Value Added Tax) Refund Procedures
AURA has continued to exercise its prerogatives granted by Law Decree 560 of 18 June
1985, whereby it can request from the Chilean Treasury Department the reimbursement of
IVA Tax paid by CTIO. In the past these presentations were submitted at irregular periods;
a more efficient strategy has been implemented in which refund claims are presented to the
government comptrolling agencies on a monthly basis.
Information Service Upgrade - Phase I: Hardware
The quality of the Information Services in Administration has suffered for several years
now. These problems originated mostly in the choice of inadequate technologies, archaic
software, shortage of resources, and lack of a coherent plan to provide the observatory with
reliable business information services.
Upgrading of the Administrative LAN hardware is now underway. Completion of the first
stage of this project is expected to occur during the first quarter of FY 1997; in addition to
upgrading current access, the LAN will incorporate crucial additional stations located in
Santiago, Cerro Tololo, and La Serena.
The next step is to replace the old administrative computer software with modem and
efficient applications that will contribute to increase the quality, availability, and timely
reception of the information that Administration originates. The local market offers
software applications for the Chilean environment to improve the Accounting, Payroll,
Warehouse and Personnel modules' efficiency, with the added benefit of an array of
15
analysis and report tools to provide the means for increasing the soundness and quality of
financial controls.
Blanco 4-m Telescope - Fire Prevention
The first stage of the installation of a modem fire detection and alarm system for the
Blanco Telescope has been completed. The second phase of this project is underway and
involves the installation of control mechanisms that will automatically shut off all
ventilation equipment and shutters in the event of a fire, thus preventing potential
contamination from gases and fumes that might otherwise escape and spread throughout the
building. Funds permitting, we plan to install an automatic fire-fighting system for
unattended areas of this telescope.
In addition to the above, our personnel continue to be trained in modem fire-fighting
programs and fire prevention techniques.
La Serena Water System
During the month of March the installation of a new industrial-type water filter for the
water distribution system in La Serena was completed. This 5 urn activated-carbon filter
will completely eradicate particles, algae and other solids from the compound's drinking
water.
Support of the Gemini Project in Chile
Between 6-8 May, a delegation of NOAO and Gemini Management representatives met
with CTIO management staff members in La Serena to identify future management and
logistics requirements for the administration of the Gemini construction stage as well as for
the subsequent operational phase. During the course of these meetings the critical need for
common strategic administrative information systems, in order to seek full data
compatibility between Gemini, NOAO, and CTIO, was addressed.
Gemini assigned CTIO Logistics and Administration Division the responsibility of
conducting negotiations with the Irrigation Department, regional mining concerns, the
Public Works Ministry, and ultimately, with the Road Department, to reach an agreement
for the enlargement of the Puclaro Road tunnel, in order to allow the passage of large
cargoes of telescope components exceeding the width of the original tunnel design.
Attempts to persuade local companies, which might benefit from an increased tunnel width,
to join forces with us and seek financing for the enlargement of the tunnel proved
unsuccessful. After a long and difficult negotiation, an agreement between the Road
Department and AURA, Inc. (on behalf of Gemini) was reached whereby Gemini would
contribute the incremental financing required to enlarge the width of the tunnel, in strict
conformity with the requirements and interests of the project.
CTIO Operations personnel have been increasingly involved in assisting Gemini with the
logistics and administrative management of incoming ocean cargo consigned to the project
operations in Chile.
The Cerro Pachon road improvement was successfully completed, as specified by Gemini,
to allow for the passage of loads of up to 10 mts. wide.
16
2MASS
On 14 May CTIO scientific, engineering, and administrative staff members met with the
2MASS Project Manager to decide the most desirable site location for the southern 2MASS
telescope, explore practical construction solutions, and discuss the future operation of this
telescope on Cerro Tololo. These meetings included a visit to the telescope construction
site.
The University of Massachusetts accepted CTIO's proposal for the construction of the
enclosure building and control room for their telescope. This construction is expected to be
completed in December.
Robotic Camera
On 21 June a set of pictures, coordinates, and site plan drawings was sent to John E.
Gaustad for the installation of a Robotic Camera on CTIO. The installation schedule for
this instrument has been set for 11 October 1996.
B. Kitt Peak National Observatory
Both significant milestones and a critical failure marked FY 1996 for Kitt Peak National
Observatory. The WIYN Observatory completed a most successful first year of science
operation. The prime focus focusing mechanism of the Mayall 4-m was completely replaced
during Summer Shutdown to enable the CCD Mosaic to be installed in fall 1996. The high
resolution IR spectrometer, Phoenix, began commissioning and the Mayall 4-m was closed
from 30 October to 27 December because of a catastrophic failure of the dome shutter gearbox.
1.
New KPNO Programs in FY 1996
The WIYN Observatory began science operations in July 1995 (NOAO receives 40% of the
time on WIYN to schedule and operate for the astronomical community) and in its first
year has proven to meet its design goals and to enable excellent astronomical research.
NOAO time on WIYN is primarily scheduled for the Queue Observing Experiment where
KPNO support staff obtain observations for observing programs submitted to NOAO from
the astronomical community. The goals of this mode of operation are to complete highly
ranked proposals in a timely fashion, to provide new science opportunities by allowing a
wider range of program lengths, and to develop observing processes applicable to the
Gemini telescopes. In addition, the WIYN Queue is designed to match the observing
program to the observing conditions so as to increase telescope effectiveness. The first
semester—fall 1995—was very highly oversubscribed, reflective of the interest in the new
scientific opportunity which WIYN provides, and the WIYN Queue had a steep learning
curve to climb. As expected, the second semester—spring 1996—ran much more smoothly
and more productively. During spring 1996 nights were divided between classically
scheduled time, programs selected where it was advantageous to have the PI on site, and
the Queue. The WIYN Queue will continue to be fine tuned and optimized in the future to
maximize the scientific output (e.g., to provide scientifically useful partial data-sets when
100% program completion is not possible) and to define how queue and service operations
should be ran on Gemini before Gemini operations begin.
WIYN has now been fully integrated into KPNO operations, both in day-to-day operations
and maintenance and in improvement projects. An Operations Readiness Review (ORR) for
17
WIYN was held in February 1996 to review the as-built status of the telescope,
instruments, and enclosure. The WIYN ORR panel generated a list of actions considered
significant in bringing the observatory up to its full potential and to operate in a safe
fashion. Many of these action items have been incorporated as future improvement projects
for WIYN. The biggest challenge for WIYN is to achieve in a reasonable amount of time
and resources a steady state level of reliable operation comparable to other KPNO
telescopes.
The success of CTIO in improvement of image quality at the Blanco 4-m indicates that the
"old" technology telescopes like the Blanco and KPNO Mayall can be improved to deliver
better images—the Blanco now routinely averages sub-arc second images—if one is
willing to spend the time and resources. Two significant programs were initiated in
FY 1996 at the Mayall 4-m: to collimate the optics with wave-front curvature analysis and
to begin regular (several times a night), systematic measurement of the delivered image
quality (DIQ). WIYN aided in addressing an underlying question: is it worth the effort to
make the Mayall better? Since WIYN is designed not to degrade the free atmosphere seeing
conditions, the image size delivered by WIYN demonstrates that Kitt Peak is a much better
site than previously thought. Between September 1994 and June 1996 the average DIQ at
WIYN was 0.8 arcsec, with 24% of the time better than 0.7 arcsec and 11% better than 0.6
arcsec. For several months in spring 1996, the average measured DIQ at the Mayall 4-m
was 1.1 arcsec. The poorer DIQ at the 4-m relative to WIYN can be attributed to the effects
of turbulence in the dome and adjacent to the mirror and to optical collimation. As a part of
Summer Shutdown 1996 activities the primary mirror support system was refurbished and a
careful end-to-end alignment of the optics carried out. For several nights before resuming
operations the DIQ was measured at both the 4-m and WIYN at essentially the same time
and under optimal conditions where there was no mirror or dome degradation of the 4-m
DIQ. Within the precision of measurement and seeing variability, the measured DIQ was
exactly the same at both sites, indicating that under these circumstances the Mayall
delivered essentially site-limited seeing. The goal for FY 1997 is to decrease the average
DIQ and to increase the number of nights when excellent seeing conditions are achieved
because the free atmosphere seeing is better than average (e.g., less than 0.7 arcsec).
2. KPNO Observing Improvements
Improvement projects this year were severely set back by the catastrophic failure of the
dome shutter gear assembly. The root cause of the failure was wear over thirty years of use.
The original gears were cast-iron with a hardened surface. When the hardening wears
through, rapid wearing of the gears occurs with the teeth then easily breaking. All of the
gears showed pitting from wear, an indication of surface fatigue failure, but without signs
of scoring, which would indicate oil film failure due to excessive loads or aging lubricant.
All of the bearings in the gearbox showed similar wear and were replaced. The new gears
are made of solid steel with wear properties superior to cast-iron. In addition, the two
original motors—one for slow speed and one for fast—were replaced with a single DC
motor that ramps up to the set speed, thus placing less load on the gearbox when starting
and stopping. All astronomers affected by the closure were informed of the schedule for
repair and asked when they would like to be re-scheduled. By shortening the block assigned
for DLIRIM proposals, two canceled programs were scheduled. Five proposals canceled in
the fall were scheduled in early spring 1996. The remainder were given special
consideration for fall 1996.
18
Essentially all major improvement projects and summer shutdown activities in FY 1996
focused on the Mayall 4-m telescope. The prime focus mechanism (the "pedestal") and
ancillary electronics were completely replaced to support the Mosaic CCD imager. As
usual, all guiders and filter wheels were inspected, cleaned, and aligned, IRAF and
computer operating systems were brought up to the latest releases, and CCD dewars
cleaned and freshly evacuated with CCDs flooded for ultraviolet sensitization.
The multi-slit entrance masks for multi-object spectroscopy with the R-C Spectrograph or
Cryogenic Camera at the 4-m have been made from photographic film with a 10%
throughput loss in the film-base material. We have now developed a new technique using
thin etched stainless steel for the mask material which has zero throughput loss, effectively
increasing the speed by 10%. Other deficiencies corrected by this adaptation of integrated
circuit technology are occasional scale errors due to drifts in the film recorder electronics
and internal fringing in the film base.
Because oversubscription for imaging at the Mayall 4-m and at WIYN means that many
requests for moderately high resolution optical imaging must be rejected, imaging was
made available at the 2.1-m starting in fall semester 1996 with a Tektronix 1024 x 1024
CCD (TIKA). The ILS camera system, which replaced the venerable IDT guider as part of
making the 2.1-m user-friendly for astronomer operation, has been upgraded with a neutral
density filter and remote focus for efficient operation with imaging. The demand was quite
high for imaging at the 2.1-m with 32 nights scheduled in fall semester 1996.
The high demand for CCD imaging with the Burrell Schmidt during both KPNO and
CWRU time has resulted in the decision to offer only a CCD as a detector; photographic
plates will no longer be an option. Consequently, the opportunity arose to remove the plate
holder hardware which obstructs a significant fraction of the incoming starlight. Tests
indicate that a throughput gain of 60% was achieved. At the same time the lead screw in the
CCD focus mechanism was replaced to reduce sky-position-dependent focus variations and
a new collimation technique developed. The resulting images were less than two pixels
over the entire chip, i.e., under-sampled.
3. KPNO Instrumentation Improvements
Kitt Peak CCD controllers have used 15-bit analog-to-digital converters for many years
with a dynamic range of 32,767—a dynamic range which requires some compromises
between using all of the linearity range of the CCD and fully sampling the readout noise. A
related problem concerns the effects of saturated stars on the CCD electronics and on the
resulting data. While we have in recent past optimized the electronics for the gain which
minimizes these effects, a higher digitization limit would achieve a better compromise of
larger dynamic range and better sampling of the readout noise. With the start of the fall
1996 observing schedule, all of the KPNO CCD controllers now have 16-bit A-D
converters that allow either twice the dynamic range or two times better sampling of the
read noise at the previous dynamic range. An added benefit is that the new A-Ds operate
faster, and some 16 seconds will be trimmed from every 2048 x 2048 CCD readout. While
this does not seem a lot of time, the 16 seconds faster readout translates to an hour per night
over the various KPNO telescopes and 5-10 nights worth of telescope time over the course
of a year.
19
New imaging correctors to accommodate the 8K x 8K CCD Mosaic Imager were designed
and constructed for the 0.9-m and 4-m telescopes. The 0.9-m corrector, a simple doublet of
fused silica, with the Mosaic imager enables observations of a field 59 arcmin square with
0.43 arcsec pixels. The 4-m corrector, which includes atmospheric dispersion
compensation, with the Mosaic imager provides a field of view at the Mayall Prime Focus
of 36 arcmin square with 0.26 arcsec pixels. Both correctors are designed to maximize
transmission in the ultraviolet and to minimize scattered light. The correctors were
designed to produce spot sizes less than a single pixel over the whole field, and ontelescope tests indicate that off-axis images are not degraded by the corrector.
The new high-resolution IR spectrometer, Phoenix, has begun commissioning on the
mountain. With an instrument the scale of Phoenix—it is larger and more massive than
other IR instruments—a number of small, but significant improvements were required to
the 2.1-m telescope and facility. All of these have been completed and Phoenix will begin a
special opportunity observing process in the fall 1996 Telescope Schedule.
C. National Solar Observatory
1.
Kitt Peak
The McMath-Pierce Solar-Stellar Spectrograph
The community has made available resources from individual grants in order to renew the
nighttime program with the solar-stellar spectrograph. Nighttime operations at the McMathPierce facility will resume by the beginning of FY 1997. A resident observer will obtain
synoptic observations with the solar-stellar spectrograph. The mix of scientific programs
based on the contributed funding includes both solar-system studies and solar-stellar
investigations. In addition, approximately 30-40 nights of synoptic time will be available to
the general solar-stellar community on a competitive proposal basis.
The program was terminated in 1995 before the new cross-dispersion system could become
fully operational. The solar-stellar spectrograph will therefore continue to operate in a
single-order mode using the TI 800 x 800 CCD. We are still pursuing the possibility of
replacing the current CCD with a large-format (1Kx3K) device from the NOAO
instrumentation program. Thus far, ultra-thinned devices that may be unaffected by the
resolution degradation problem of the other 1Kx3K arrays have not been successfully
produced. Array development and testing continues.
Digital Library Development
During FY 1996, NSO began to populate its 300-disc CD-ROM jukebox with data from the
FTS and the KPVT. Currently, the jukebox holds a complete set of 39 discs of FTS
transformed spectra, eight discs of 512-channel magnetograph data, and three discs of
spectromagnetograph data, for a total of about 35 GB of on-line storage. The jukebox is
already being heavily used, with over 2000 files transferred in the period of 11 April-3
August 1996 in spite of the fact that there is no useful on-line search engine. The
development of the NSO Digital Library will accelerate in FY 1997. The addition of
resources from the NSF Space Weather Program and the NASA Space Physics Data
System will speed up migration of the data into the jukebox, and allow progress to be made
20
on a search tool and user interface. These improvements will further reduce both the delay
in the delivery of data to users, and the impact on scientific staff time to fill data requests.
NIM-2 (Near Infrared Magnetograph)
The NIM-2 project is constructing an imaging vector magnetograph based on a
piezoelectrically-tuned, servo-stabilized Fabry-Perot etalon. The existing Near Infrared
Magnetograph maps the true magnetic field strength in the deep solar photosphere, using
the McMath-Pierce Telescope, the 13.7-m vertical spectrograph, a liquid crystal
polarimeter, and an infrared array camera that records two Zeeman-sensitive iron lines near
1565 nm. Using the same infrared camera with an improved polarimeter and data system,
NIM-2 will achieve better time resolution and geometric stability (because the field of view
is imaged simultaneously rather than built up by scanning) with little sacrifice in spectral
resolution.
The project made major strides in FY 1996 and is ahead of schedule. The Fabry-Perot
etalon and the prefilter were received and tested. The mechanical and optical designs were
finalized. Mechanical fabrication is complete. The optics have been delivered and installed,
although they will be sent out for coating after the first-light tests. A fast liquid crystal
modulator was received which meets the primary switching-speed requirement but is being
reworked for ancillary improvements. The camera readout system has been modified to
almost double the exposure duty cycle. First light was achieved during August, and NIM-2
will be commissioned during FY 1997. The NIM-2 project is partially supported by a grant
from NASA.
Large-Format IR Array Camera
The McMath-Pierce facility offers capabilities that are unique in the world for infrared
solar observations: an unobstructed, all-reflecting light path (giving full wavelength
coverage with low thermal background) and large aperture (for angular resolution and
photon flux). These capabilities cannot be fully exploited without a state-of-the-art infrared
array detector at the focal plane.
The present detector is a commercial 256 x 256 InSb array from Amber Engineering, re
housed in a dewar from Infrared Laboratories. We chose this system because of its low
initial cost and 1-5 urn wavelength coverage. It has succeeded in jump-starting magnetic
observations with NIM and enabling a new class of results from CO spectroscopy.
However, the Amber system is becoming obsolete (this only takes 3-4 years in the realm of
infrared technology).
NSO plans to replace the Amber array with a state-of-the-art 1-5 urn camera by taking
advantage of NOAO's investment in the Aladdin array development project. The
performance of an Aladdin-based system will surpass the Amber system in every important
respect (dark current, readout noise, quantum efficiency, and immunity from electronic
interference); its 15-20 Hz frame rate is well matched to the requirements of NIM and
NIM-2.
During FY 1996, NSO prepared the way for the Aladdin era by purchasing a closed-cycle
cryogenic cooling system and proving it in use by hosting KPNO's Simultaneous Quadcolor Infrared Imaging Device (SQED) at the McMath-Pierce. During FY 1997 we will
take the next step by hosting the Aladdin-based Phoenix instrument for solar infrared
21
spectroscopy. Also during FY 1997 NSO will purchase an Aladdin controller from
NOAO/TPG, which has undertaken to produce a controller for NSO during FY 1998. Our
program assumes that NOAO will provide one or more science-grade Aladdin arrays
without cost to NSO.
Kitt Peak Vacuum Telescope Control Upgrade
FY 1996 was the second year of a long-term project to upgrade the 23-year-old control and
guiding systems of the KPVT. Maintenance of these systems is becoming difficult since
many of the components are no longer available. Performance problems also limit the
quality and quantity of data from the focal plane instruments.
The overall goals of the project include better control of image guiding and scanning,
reduction of unwanted image motion, replacement of obsolete computerized control
systems, and computer control of the Littrow spectrograph. The overall upgrade plan is
divided into small, stand-alone segments that provide prioritized, incremental
improvements.
To date, new gear boxes and motor drivers for the drive system of the No. 2 mirror have
been installed. These have greatly reduced the amount of backlash and improved the
reliability of these drives. A mounting and solenoid drive that will allow the No. 4 mirror to
be rapidly tilted to reduce image motion has been constructed and tested. It is scheduled for
installation in September 1996. The overall computer software and hardware architecture to
be used to control the telescope has been specified. A design for new sensors to replace
existing limb guiders and supporting electronics is underway. The design activities are
intended to be transferable to similar upgrades planned for the McMath-Pierce Telescope
and the proposed SOLIS project.
Milestones
FY 1995 - Design and start manufacture of new No. 2 mirror drive mechanical and
electronic systems. Design fast tip mounting for No. 4 mirror. Start electronic design of
No. 4 mirror drivers. Status: completed.
FY 1996 - Complete the fabrication and installation of the upgraded mechanical drive
assemblies on the No. 2 mirror. Complete the fabrication and installation of the mechanical
components of the image-motion compensation. Start the design and fabrication of the
image-motion compensation electronics. Start the design of the guider control electronics
and software. Specify the architecture of the telescope control software and hardware. The
bulk of the computer hardware required to complete the upgrade will be purchased in late
FY 1996.
FY 1997 - Complete the installation and testing of the image-motion compensation
electronics. Complete the installation and testing of the guider control electronics and
software. Complete computer control of the Littrow spectrograph.
22
2.
Sac Peak
Mark II Correlation Tracker
The development of the Mark U correlation tracker (CT) at NSO/SP has been mostly
finished during FY 1996. The CT system was integrated from off-the-shelf hardware
components, will be easily maintainable, and can be cloned for use at other observatories.
A tip/tilt mirror system, purchased from the Kiepenheuer Institut fur Sonnenphysik using
Air Force Phillips Lab funds, was integrated into the system as a corrective element. The
servo loop was successfully closed in a test setup in the optical laboratory and the
performance of the CT system was characterized. The CT will see first light at the Vacuum
Tower Telescope (VTT) in September 1996. We anticipate that a minimal software effort
will be required in early FY 1997 in order to integrate the CT as a user-friendly instrument
into the VTT system. A permanent optical setup, that allows for easy alignment and
calibration of the CT was also installed during FY 1996.
Fast CCD Cameras
We are working toward replacing the custom-built MDA detector system with state-of-theart, large format CCD detectors. A Thomson IK x IK camera with 10-bit resolution and a
frame rate of up to 5 frames/sec and a KODAK Megaplus, with a 1317 x 1035 pixel format
and 8-bit resolution running at 6 frames/sec, are now available at NSO/SP. These cameras
can be used for high speed imaging and frame selection. A 2K x 2K 12-bit camera has been
ordered from Xedar. The prototype of the 2K x 2K CCD, developed for the RISE project,
has been delivered and is currently being tested and evaluated at NSO/SP. A second
2K x 2K camera will be delivered to NSO/SP in October 1997. Additional 2K x 2K CCD
detectors will be added as funds become available.
Image Quality Improvement at the VTT
In FY 1996 the optical performance of the VTT was measured, both by Shack-Hartmann
wavefront sensing using sunspots and stars as targets, and by interferometry. The results
show that the image degradation arising from the telescope alone can be worse than that
caused by atmospheric seeing at Sac Peak. Earlier work showed that solar heating of the
entrance window and its cell, which predominantly affects the edge of the window,
produces time-varying spherical aberration and higher order circular modes in the
wavefront. These effects have been studied in detail using interferograms made by
combining laser light reflected from the two sides of the window. Besides the circular
modes caused by the heated edge, these measurements also show considerable astigmatism
that may be temporarily variable, as well as some coma.
The thermal effects on the wavefront due to heating of the window have been greatly
reduced by an active cooling system that senses the gradient of temperature both across the
face of the window and through its 4-cm thickness by combining the measurements from
pairs of sensors on the outside and on the vacuum side of the window. The error signal for
the servo is derived by comparing the average of one pair of sensors at the edge of the
window to another pair 10 cm in from the edge. Interferograms show that the window
figure errors have been reduced from several waves to a fraction of a wave, implying that
the window temperature is now uniformly maintained to a few tenths of a degree. The
performance of the VTT has been significantly improved by this: frame selection
procedures now achieve diffraction limited resolution.
23
A Shack-Hartmann WFS was used to measure the aberrations of the entire telescope,
including the entrance window. Comparison of the wavefront errors produced by the
window alone to the overall wavefront measured with the Shack-Hartmann showed that a
significant portion of the image degradation coming from the telescope does not arise in the
window. Subsequent tests of the two 1.1-m diameter Cervit turret mirrors using a RitcheyChretien test set up with a 1.27 meter aperture sphere on loan from the KPNO optical shop
showed that the edge of one of the Cervit mirrors is turned down by at least two waves.
This mirror is being resurfaced and should be back in the telescope by the end of FY 1996.
Active Optics
Further improvement of the optical performance of the VTT can be achieved by using a
deformable mirror aimed at correcting fixed and slowly-changing aberrations. A relatively
slow system with a bandwidth of a fraction of a Hz, using a Shack-Hartmann wavefront
sensor with a limited number of subapertures, is faster and less costly to implement than a
high bandwidth adaptive system aimed at full atmospheric compensation. Such an "active"
optics system is currently under development at Sac Peak, based on a 97-actuator Xinetics
mirror purchased with USAF and NSO funds. This active optics system is regarded as a
stepping stone to the more elaborate adaptive optics system that has been under
development at Sac Peak for a number of years. Not only should it further improve the
performance of the VTT on an interim basis, but also it will provide experience and insight
into solar-related AO problems, such as wavefront sensing using solar granulation. In
FY 1996 a first successful active optics experiment was performed at the VTT in
collaboration with the Lasers and Imaging (LI) Directorate of the Air Force Phillips
Lab/Albuquerque using a 127-element LCD wavefront corrector provided by LI in
conjuction with the Hartmann-Shack wavefront sensor developed at NSO/SP. The active
optics development will continue through FY 1997.
Adaptive Optics
Since the successful demonstration of the Lockheed 19-segment adaptive mirror at Sac
Peak in 1991, there has been pressure by the users to build a facility AO system for the
VTT. Technical problems and lack of personnel have slowed the realization of this goal.
Progress has been made in all aspects of the supporting optical system, and much of the
optics for the innovative LCD wavefront sensor is in place.
The wavefront sensing problem in solar adaptive optics is more difficult compared to
nighttime AO because no point source is available on the solar disk. A solar wavefront
sensor has to function with solar granulation, an extended low-contrast scene. NSO is using
a 640 x 640 pixel thin-film transistor LCD display to create a spatial mask for filtering the
granulation scene and thereby encoding wavefront slopes as intensity variations at the
detector. The concept is not unlike the "knife-edge" or Foucault test, the generalizations
being that the edges are placed over intensity features (granules) everywhere in a scene,
and that the mask is dynamic, being updated as the granulation pattern changes. Because
the LCD display is large, the wavefront sensor optical system is placed in one of the large
instrument vacuum tanks in the VTT.
The NSO efforts during FY 1996 were concentrated on validating this wavefront sensor
concept and comparing its performance to the modified Shack-Hartmann wavefront sensor.
Evaluating and understanding the wavefront sensor is a crucial milestone to be achieved by
early FY 1997.
24
A second milestone for FY 1996 was achieved by finishing the mechanical and electrical
assembly of the 61 actuator continuous faceplate mirror.
Infrared Program
NSO/SP maintains two near-IR camera systems which were developed by outside
collaborations (with Michigan State University, Wyoming Infrared Observatory, and
Haverford College). These cameras account for about 25% of the user time allocated at the
VTT and the Evans coronagraph. Some year-end funds were allocated last year for IR
optics and the purchase of an IR array. During the coming year we will develop a 1-2.5 um
camera system that is available year-round at NSO/SP. The system will be developed in
collaboration with MSU and Starfire Optical Range, Albuquerque.
In collaboration with the USAF, we have obtained two near-IR Fabry-Perot etalons and an
additional controller. The etalons will be used in tandem for narrowband imaging between
1-1.8 um. Current projects include: coronal imaging in 1083.0 nm, velocity and magnetic
field maps of the corona, and development of a prototype imaging vector magnetograph for
possible use in an upgrade of the AF solar observing network. The etalons will be available
for user programs during 1997.
D. US Gemini Program
The US Gemini Program (USGP) serves as a liaison between the International Gemini Project
Office (IGPO) and the US community. The Gemini Project is an international consortium to
build two 8-m telescopes, one on Mauna Kea, Hawaii, and one on Cerro Pachon, Chile, in
which the US maintains a 50% share. The USGP is led by the US Gemini Project Scientist, and
currently includes one Astronomer, a Project Engineer, and a Technical Administrator.
A major part of the work of the USGP during the past year has been connected with
procurement of the Gemini instruments assigned to the United States. The United States is
responsible for three instruments, a near-IR (1-5 um) imager, a near-IR spectrograph, and a
mid-IR (8-30 um) imager. The near-IR imager was assigned by the NSF to the University of
Hawaii; the USGP is responsible for the procurements of the other two instruments. The nearIR spectrograph was assigned to the NOAO instrumentation group through a competitive
selection in FY 1995. The mid-IR imager is still in the selection process. At the request of the
IGPO, the USGP has taken on the management of these instruments as the Gemini IR
Instrument Program. This approach allows one group, the USGP, to look out for interface
issues, areas of commonality among instruments, and to identify and help to solve problems in
areas of budget, schedule, and risk.
During FY 1996, the USGP defined a plan for the procurement of the mid-IR imager, involving
a two-stage competitive selection open to the entire US community. The first phase of this was
a competition for an award to conduct a conceptual design study. This was carried out in
FY 1996, and negotiations are underway with two groups to do this work. This work will be
completed in early 1997 and will be followed by another open competition to produce a
detailed design and fabricate the instrument.
In addition to these instruments, the United States has been asked to provide the optical and
infrared detectors and controllers for the Gemini instruments. The USGP has been monitoring
25
development programs at a number of CCD vendors, and a plan for procurement of these and
the CCD controllers is being finalized. The specified near-IR arrays are the 1024 x 1024 InSb
ALADDIN arrays being developed jointly by NOAO, the US Naval Observatory, and the Santa
Barbara Research Center. The USGP has worked with the NOAO instrumentation group and
Gemini representatives to develop a plan by which a foundry ran following the ALADDIN
effort will provide Gemini with the detectors it needs.
After the selection of a supplier for each instrament is made, the USGP remains responsible to
the Gemini Project in seeing through the successful design, fabrication, and delivery of each
US-allocated instrament. This activity includes day-to-day monitoring of progress by each of
the instrament suppliers, identifying concerns that have implications for cost, schedule, or risk,
and helping the groups work out solutions to these concerns. During FY 1996, USGP personnel
worked with the University of Hawaii near-IR imager group to develop a realistic schedule and
management plan for that instrament. USGP staff have coordinated discussions and testing of
common aspects such as cryogenic motors, software, and on-instrament wavefront sensors. The
USGP works with the Gemini Project in organizing and conducting design reviews and
acceptance tests.
In August 1996, the USGP organized a workshop on the US interests in future instruments for
the Gemini telescopes. The discussion was focused on the science that the community will want
to do with the Gemini telescopes and in the context of the entire suite of facilities available to
the US community. About 25 astronomers from around the country participated in this two-day
meeting in Tucson. Major elements of the plan endorsed by the group are an aggressive
adaptive optics program, ultra-high resolution optical spectroscopy, and Near-IR spectroscopy
with spatial multiplexing, either with multiple slitlets or with an integral field feed.
In order to encourage a better understanding of the Gemini capabilities by the South American
partners and to foster collaboration between southern hemisphere and northern hemisphere
Gemini partners, the USGP organized and carried out a Gemini workshop at the 7th Regional
Latin American Astronomy meeting held in Montevideo, Uruguay in November 1995. This
workshop included a Gemini display, a session of talks on the Gemini telescopes,
instrumentation, operations plans, and a question and answer session. The meeting was
attended by a number of astronomers and national project office staff from the US, the UK, and
Canada.
The USGP is responsible for keeping the community informed about Gemini's progress and
fostering community support for Gemini. Displays are regularly presented at AAS meetings and
USGP staff contribute status information to both NOAO and Gemini newsletters. The USGP is
also in the process of developing a World Wide Web site to provide all the information and
support that US astronomers will need to use the Gemini telescopes effectively.
Another USGP responsibility is the monitoring of technical developments within the project.
The US Gemini Project Scientist serves on the Gemini Science Committee (GSC) and
represents there the views of the US scientific community. In addition to the GSC and project
scientist team teleconferences, formal input is contributed through participation in reviews and
working group meetings organized by the project. The USGP also solicits membership for US
participants in these reviews and meetings and organizes the US participation in the GSC. One
such meeting held in May 1996 was a scientific review of the High-Resolution Optical
Spectrograph (HROS), an echelle spectrograph being designed in the UK for the southern
Gemini telescope. A group of four US astronomers participated in a two-day meeting at
26
University College London where they helped to define the performance requirements for this
instrament. HROS is now proceeding toward a conceptual design review late in 1996.
In a similar way, the national project managers meet regularly to discuss procurements and
other management issues. USGP staff take part in these discussions, and the US Project
Scientist represents US issues in these matters at semi-annual national project managers'
meetings and the Gemini Director's review.
In a less formal sense, the USGP personnel interact frequently and directly with the Gemini
Project to provide scientific and technical feedback, to identify scientific performance issues
and to help define technical solutions to meet the science requirements, to evaluate
implementation plans, and to participate in source selection for critical systems and
components.
The USGP has participated intensively in the development of a plan for the evolution of
responsibilities in the operations phase of Gemini. It is clear that the international Gemini
Office will continue to depend on the national Gemini offices for a great deal of assistance in
interacting with the user communities of the partner countries. The national Gemini offices will
solicit proposals, perform technical evaluations, run national time allocation committees and
national users committees, and will provide assistance to astronomers in writing Gemini
proposals and reducing Gemini data. The USGP has begun to plan for these activities as well as
other possibilities such as providing a remote observing center and developing tools to support
queue observing with Gemini.
E. NOAO Instrumentation Program
The purpose of the Instrament Projects Group (IPG) is to develop and produce major
instruments for the NOAO nighttime telescopes at both CTIO and KPNO. The NOAO
scientific staff initiates, directs, and prioritizes projects, while the engineering managers are
responsible for meeting schedule, budget, and performance requirements. NOAO astronomers
generate new instrament projects in response to user requests, scientific staff interests, and
advances in technology, particularly with the development of new detectors.
As in all of NOAO, dedicated and effective individuals are responsible for the success of the
program. Neil Gaughan is the engineering projects manager. The IPG reports to him, and he
reports to Larry Daggert, the Manager of ETS. Neil brought a background of detailed planning
for projects including low-light sensor development. The Instrament Projects Advisory
Committee has scientific oversight responsibility for the program, and the task of
recommending priorities for major instrament development to the NOAO Director. The
committee consists of Taft Armandroff, Bob Schommer (CTIO), Todd Boroson (US Gemini
Program Scientist), Dave De Young (KPNO), Jay Elias (Gemini Near-IR Spectrograph Project
Scientist), Richard Elston, and Richard Green (NOAO Deputy Director and Chair). The group
meets monthly with the technical managers to review schedules, resource management issues,
and priorities. It conducts quarterly reviews of the program, and holds an annual open meeting
to discuss plans for activities for the next fiscal year. IPAC works with Neil Gaughan and Larry
Daggert to produce the detailed plan for the annual allocation of technical resources that is
recommended to the Director and the NSF. It also organizes and participates in non-advocate
design reviews for major projects. A system of review gates controls the rate at which
resources are released to a project, subject to successful completion of the previous stage.
27
Each approved instrumentation project has a project scientist responsible for the scientific
performance and a project engineer who leads the instrament technical team in meeting
performance requirements, cost, and schedule. The ETS technical group itself was formally
reorganized in April 1995, to merge the former IR and O/UV Groups into a single Instrament
Projects Group. The two wavelength ranges demand separate dedicated engineering expertise,
but the design, drafting, and fabrication resources are fully integrated. Two major new
instruments were neared completion during the reporting period, and two IR instruments were
in the process of upgrades to new large-format arrays.
One of the major accomplishments of the joint program was the successful testing on the
telescope of the new CCD Mosaic Imaging system. The imager has a detector mosaic of eight
CCDs with 2048 x 4096 format of 15 micron pixels. It has a large filter transport mechanism
holding 14 six-inch filters and a pneumatically controlled shutter mechanism that gives 1%
timing accuracy in 1-second exposures. Accommodation of the Mosaic Imager at the Mayall
4-m prime focus required a nearly complete rebuilding of the pedestal and focus mechanism. A
new multi-element corrector with atmospheric dispersion correcting prisms was designed,
polished, and integrated in the optical shop. The technical team at CTIO had to multiplex
together four ARCON controllers for rapid read-out and image reassembly. An initial telescope
test ran in June led to a summer of intense activity, particularly on the electronics of the
controller system. The entire system was integrated successfully for a ran at the end of
September, and both engineering and scientific images were collected. Remaining work is
primarily in software, mostly related to user and telescope interface issues and more rapid
image reassembly and display. The Mosaic Imager will be made available to KPNO users on a
shared risk basis during Spring semester. At the end of the fiscal year, NOAO joined with the
Carnegie Observatories for a mass buy of scientific grade CCDs, which will replace the
engineering grade arrays currently being used for commissioning. The replacement should take
place during calendar year 1997. Longer term plans call for production of a clone, so that the
twin 4-meter telescopes can offer such an imager in each hemisphere. The capability of widefield surveying is necessary for support of follow-up programs suitable for the Gemini
telescopes.
Equally impressive progress was made on the high-resolution near-infrared spectrograph,
Phoenix. Phoenix operates from 1-5 microns, using two quadrants of a new ALADDIN InSb
array detector. Spectral resolution delivered by the echelle grating is designed to be 100,000 for
two-pixel sampling of the slit. This instrament resides in the largest cryogenic dewar yet
integrated by NOAO, and includes foreoptics to cold stop the pupil, slit and pupil viewing,
dichroic beam splitting for optical guiding on the target, and a double-pass collimator-camera
optical system. After first light on the telescope in June, the summer was spent tackling issues
of thermal control and very low-noise performance of the ALADDIN array and new mounting.
A return to the telescope in September has given confidence that the instrament is close to
meeting all its performance goals. It will be available to users as a facility instrament on the
2.1-m in the spring semester.
The ALADDIN program mentioned above is a joint development effort among NOAO, the US
Naval Observatory Flagstaff Station, and Hughes Santa Barbara Research Corporation. Its goal
is to develop the technology for producing 1024 square InSb arrays for astronomical use.
Failure modes can be benign in that arrays can have a smaller number of working quadrants
which can still be useful for science. The initial investment may produce between 12 and 16
28
arrays to be shared by NOAO and USNOFS. Technical progress has been slow but steady; as of
this reporting seven hybrids have been produced, and three are working in astronomical
instruments.
At the same time, NOAO has been advancing its development of array controllers to handle the
vastly increased number of near-IR pixels in these arrays. A hardware architecture was
produced to handle the multiplexing of four quadrants read as rapidly as the array capacitance
will allow, around 20 frames per second. The core of the digital system is the Datacube Digital
Signal Processor, which was the basis of the DLIRIM real-time shift-and-add experiment.
Several improvements have also been made in the analog front end of the controllers, with a
design that supports four ADCs per card with significant noise immunity.
The two other arrays have been deployed in upgrading two existing instruments. One is COB,
the Cryogenic Optical Bench. This multiple purpose imager had been used at KPNO with a 256
square InSb array to conduct the shift-and-add experiment, sampling the point spread function
with 0.1" pixels. Those optics will remain in place, while the detector has been replaced by an
ALADDIN array with a single working 512 square quadrant, and a suitable upgrade to the
WILDFIRE controller. An initial telescope ran showed a number of minor problems to be
resolved as of the end of this FY. The instrament will be shipped to CTIO in November. There
it will be used with the new f/14 secondary just delivered from the Tucson optical shop. The
tip/tilt capability of the secondary designed and implemented at CTIO combined with the fine
angular sampling will provide an early taste of Gemini image quality to CTIO users of the
Blanco Telescope.
The other instrament upgraded with an ALADDIN array is being made available through a
cooperative arrangement with the Ohio State University and the Michigan-Dartmouth-MIT
Observatory. OSU built their MOSAIC instrament to cover the J-K bands with cold
interchangeable cameras for imaging, and slit spectroscopy with single grisms for each band.
The optics were designed with large-format detectors in mind, so NOAO has provided an
ALADDIN array with two (adjacent) working quadrants for the upgrade. An initial engineering
ran of the TIFKAM (The Instrament Formerly Known as Mosaic) in September provided a
good basis for final optimization of the system. It will be available to KPNO users on the 2.1-m
and 4-m telescopes during spring semester.
Work for the Gemini Project represents the highest priority of the instrament program. NOAO
won the competition to build the Gemini Near-IR Spectrograph, and began design work in
FY 1996. Jay Elias is the NOAO Project Scientist and Dan Vukobratovich, formerly of
University of Arizona Optical Sciences, is the Project Manager. The instrament will be the
largest cryogenic device produced by NOAO, with a length of some 2 meters. It successfully
passed its Conceptual Design Review in the spring. The Preliminary Design Review will be
held in October. The bulk of FY 1997 will be spent bringing the design to the level of detail
required for constraction and the Critical Design Review, which will be held in October 1998.
Design progress also advanced on a second-generation near-IR multi-color imager/
spectrograph. The plan calls for an instrament that can ultimately accommodate four fullformat ALADDIN arrays. Since the IR opto-mechanical team is fully occupied with the
Gemini spectrograph, NOAO is working in partnership with the Ohio State University for
development and fabrication of this instrament. A successful conceptual design review was
29
held in May, and a Preliminary Design Review will be held in first or second quarter of
FY 1997.
The Instrament Projects Group is fully committed for the activities planned for FY 1997. The
first quarter will see final commissioning of the CCD Mosaic Imager, Phoenix, and the
Cryogenic Optical Bench. Besides the high priority design work on the Gemini Near-Infrared
Spectrograph, the Gemini Project has delegated to NOAO the responsibility for procurement of
ALADDIN-type near-infrared arrays, and the production of controllers for the Gemini imager
and spectrograph. The controllers effort is an upgrade of the WILDFIRE architecture to
compatibility with Gemini software standards, particularly EPICS, and routine use of the
Datacube DSP for image reassembly and real time shift-and-add accumulation. On the
completion of the first controller system and delivery to Gemini in July 1997, a comparable
system will be adapted to the upgrade of SQIID, the four-color imager, to one-quadrant
ALADDIN arrays and deployment on Kitt Peak. On the optical/UV side, the joint CTIO/KPNO
Users Committee recommended as their highest priority a version of the Hydra robotic multifiber positioner for the CTIO 4-m Blanco Telescope. That project also includes the production
of a wide-field corrector with atmospheric dispersion compensation for the R-C focus. For the
longer term, the optical/UV scientific group is investigating the technology for a novel
approach to high-throughput optical spectroscopy. The further enrichment of the IR
complement at CTIO and Gemini South leads to a plan for a clone of the Gemini IR
Spectrograph that NOAO will produce for the Gemini North telescope.
V.
MAJOR PROJECTS
A. Global Oscillation Network Group
The Global Oscillation Network Group (GONG) is an international, community-based project
to conduct a detailed study of the internal structure and dynamics of the closest star by
measuring resonating waves that penetrate throughout the solar interior. To overcome the
limitations of current observations imposed by the day-night cycle at a single observatory,
GONG has deployed and is now operating a six-station network of extremely sensitive and
stable solar velocity mappers located around the Earth to obtain nearly continuous observations
of the "five-minute" pressure oscillations. GONG has also established a distributed data
reduction and analysis system to facilitate the coordinated analysis of these data. GONG data
are available to any qualified investigator whose proposal has been accepted, but active
membership in a GONG Scientific Team will allow early access to the data and the
collaborative scientific analysis that the Teams have already initiated.
FY 1996 marked the first year of operations for the full six-site GONG network. The project
has already collected more data on a wider range of oscillation modes than any preceding
program. These have been provided to the Science Teams who have been aggressively
analyzing them. Seven first-results papers were published by the Teams in the 31 May 1996
issue of Science magazine, and presented at various sessions at the June Meeting of the AAS in
Madison.
A Scientific Advisory Committee—consisting of P. Gilman (Nat. Center for Atmospheric
Research), R. Noyes (Harvard-Smithsonian Center for Astrophysics), A. Title (LockheedMartin Palo Alto Research Lab.), J. Toomre (U. of Colorado, Chair), and R. Ulrich (U. of
30
California, Los Angeles)—continues to provide overall scientific guidance to the Project. In
addition, the Data Management and Analysis Center Users' Committee—consisting of Philip
Stark (U. of California, Berkeley/Chair), Rachel Howe (Queen Mary and Westfield College),
Sylvain Korzennik (Harvard-Smithsonian Center for Astrophysics), Jesper Schou (Stanford U.),
and Steve Tomczyk (High Altitude Obs.)—provides important community input in the
development of this critical part of the Project.
In the instrument realm, the field stations are operating at the Big Bear Solar Observatory in
California, the High Altitude Observatory's site on Mauna Loa in Hawaii, the Learmonth Solar
Observatory in Western Australia, the Udaipur Solar Observatory in India, the Observatorio del
Teide on Tenerife in the Canary Islands, and the Cerro Tololo Inter-American Observatory in
Chile.
The Project's operations group maintains daily contact with the automatically operating
instruments, largely through the internet. Daily status reports and sample images are obtained
from the instruments' computer systems, with e-mail or telephone contact with the host sites'
support groups as required. A database of the some 200 different instrament operational
parameters is being compiled for each system. Routine analyses of these data are conducted to
verify performance and detect trends. Small technical teams are dispatched to roughly one site a
month in a routine cycle of on-site preventative maintenance.
The technical performance of the network has been excellent, especially considering that these
new systems are in their initial year of remote operation. The data duty cycle including both
weather and downtime has hovered at about 90% (as high as 93%)—nominally the value
predicted by the site survey. Of all the possible images that could be obtained at the individual
sites, only about 0.4% have been lost to equipment difficulties, and many of these were backed
up by images taken at adjacent sites.
The instrument-support arm of the operations group continues to operate the Tucson prototype
station as a "ground simulator" for hardware and software enhancements that eventually
propagate to the field stations. The group is also in the early stages of a feasibility study to
explore the possibility of incorporating a higher resolution camera into the existing stations.
The Data Management and Analysis Center is processing the incoming data at a furious pace to
keep up with the more than one gigabyte per day of data coming in from the field, and satisfy
the voracious appetites of the GONG science community. These data are reduced to 36-day
time series (a "GONG month") of oscillation-mode coefficients and transformed to obtain the
frequency spectram for each mode and, finally, tables of mode-frequency peaks. The data from
each of these and several other intermediate steps are archived as defined data products in the
Data Storage and Distribution System.
The distribution of archived data to the science community is proceeding at a good rate as well.
Data requests are received by e-mail, the World Wide Web, and by other forms of
communication. Data distributions have exceeded five gigabytes per working day. The recent
distributions have been at a rate approaching 1.5 million files per year.
The data group is continuing to provide support to the Data Scientist's in-house team and
interested contributors from the community in the ongoing effort to improve understanding of
the data themselves and enhance the quality of the data reduction processes. A number of such
31
enhancements have already been developed and will be incorporated into the current data
pipeline and a planned reprocessing of early data to produce a more homogeneous data set as
time goes on.
The Annual GONG Meeting was held in conjunction with the June AAS Meeting in Madison,
Wisconsin. It was very well attended and featured a separate poster session to provide peeks at
many interesting works in process. A series of Science Team meetings engaged in organization
and planning for several Team science papers expanding on the first results. These papers will
be sent to appropriate archival journals early in FY 1997.
Representatives from the sites participated in a separate meeting following the Annual Meeting,
and we have had several-month-long scientific visitors from three of the sites participating in
the development of analysis techniques in Tucson.
Observations have now established convincingly that the solar internal structure and
dynamics—as measured by the p-mode frequencies that GONG utilizes—vary significantly
during the solar activity cycle. Thus, the Project and the community are beginning to look
seriously at the technical and scientific milestones leading up to a decision on whether to
continue GONG operations beyond the baseline of three years. The exciting scientific
possibilities and technical feasibility of an upgrade to a high-resolution square-pixel camera
format are also being explored.
B. Precision Solar Photometric Telescope (PSPT)
The PSPT program is part of the NSF SunRISE project, which is devoted to understanding the
mechanisms of solar luminosity variations. NSO began development in FY 1994 of a small
network of photometric telescopes to measure solar surface brightness variations. The
instruments are designed around a 15-cm objective, a 2K x 2K pixel CCD, and fast frameselection electronics. Full-disk surface photometry with 0.1% per pixel accuracy with a onehour cadence will be obtained.
Highlights from this year include: (1) Deployment of a prototype PSPT instrament in Rome,
(2) Completion of the 2K x 2K photometric camera, and (3) Construction of the final PSPT
instrument at NSO/SP.
The project is actively working to minimize development costs by seeking other scientific
partners interested in the PSPT hardware. For example, the Kiepenheuer Institut fiir
Sonnenphysik is currently duplicating the lKx IK prototype camera for their observatory.
NSO will also share in the software development for the 2K x 2K Thomson camera system.
The new camera will be useful for a broad range of high-spatial and photometric dynamic range
problems, and we expect the instrument/camera costs to decrease as additional partners are
identified.
C. SOLIS
Improved long-term measurements of solar activity are key to any scientific strategy for
understanding the solar cycle. NSO is already the acknowledged world leader in full-disk
synoptic measurements. SOLIS, proposed to NSF in February 1996 as part of the "Renewing
NOAO" proposal, represents a new generation of instruments that will form the core of the US
32
synoptic capability for the next twenty years and can serve as a prototype for a worldwide
synoptic network.
In order to relate measurements from GONG, RISE/PSPT, and other space- and groundbased
instraments to the overall pattern of solar activity, it is necessary to make daily measurements
of magnetic and velocity fields, as well as chromospheric and coronal structure, with a stable
suite of well-calibrated instraments. The data provided by the SOLIS instruments will be
dramatically improved in quality, quantity, and network availability compared with what is
currently available. SOLIS will be cheaper to operate because of consolidation, automation, and
modernization. SOLIS will replace NSO's existing synoptic facilities.
SOLIS comprises four instrament packages: a Vector Spectromagnetograph that measures the
strength and direction of the magnetic field in the photosphere over the full solar disk every 15
minutes, which is of prime importance for understanding the dynamics of magnetic fields and
their relation to chromospheric and coronal structure (the present spectromagnetograph only
measures the net magnetic flux along the line of sight, typically once a day); a Full Disk Patrol
that delivers digital full-disk images of the Sun in various spectral lines at high cadence (the
present instraments typically deliver one image per day on film with a very limited selection of
spectral lines); a Coronal Emission-line Imager and Photometer that provides intensity and
velocity images of the corona in at least five spectral lines with high spatial resolution (the
current coronal photometer performs intensity scans around the solar disk at coarse resolution
once per day in three lines); and a Sun-as-a-star Precision Spectrometer that delivers very
precise spectra of integrated sunlight over a substantial spectral range (current measurements
are performed in a labor-intensive manner with a heterogeneous collection of older instruments
using just a few spectral lines).
It is important to build and operate SOLIS soon to study the next solar maximum around the
year 2000 and to support SOHO, TRACE, GONG, RISE, and other ground- and spacebased
observations.
During FY 1996, NSO prepared for SOLIS by using its existing synoptic telescopes as testbeds
for state-of-the-art hardware and software concepts applicable to SOLIS; by reaching out to the
solar physics community through the SOLIS Web page, the NSO Users' Committee (which has
strongly endorsed SOLIS), AAS/SPD meetings, and the community-based Solar Magnetism
Initiative; and by pursuing the possibility of partnerships. Potential partners include the US Air
Force, the NCAR High Altitude Observatory, and the NOAA Space Environment Center.
D. CLEAR Feasibility Study
Large solar telescopes are needed to answer a number of important science issues. Among these
are (1) high angular resolution needed to resolve the scales at which most of the action is in
solar magneto-hydrodynamics, (2) access to the infrared part of the solar spectram wanted to
extend the range of physical conditions over which the solar atmosphere is studied, (3) accurate
polarization observations needed to measure solar magnetic fields, (4) high sensitivities,
essential to study variations in these and other solar conditions, and (5) coronagraphic
capability to observe magnetic fields and small scale stractures in the solar corona. The
Coronagraph and Low Emissivity Astronomical Reflector (CLEAR) is a concept which
attempts to combine these qualities in one telescope.
33
This year saw major progress in the development of the CLEAR project. A technical and
budgetary feasibility study of the CLEAR project has so far shown no showstoppers. This study
focuses on a strawman CLEAR concept which has the following technical requirements:
Mount:
Optics:
Spectral Range:
Image Quality:
alt-az, off-axis Gregorian
4 m. f/3.75 parabolic primary, f/30 Gregorian/Nasmyth/coude foci
0.38 to 15 um minimal, 0.35 to 35 um optimal
0.1 arcsec over 5 arcmin field-of-view (FOV)
FOV:
5 arcmin diameter
Polarimetry:
Adaptive Opt:
0.01 % accuracy; 0.001 % sensitivity (photon flux allowing)
Tip-Tilt secondary mirror, adaptive optics designed for 1.6 um
wavelength at 1 arcsec seeing (100 actuators). Allow in design for future
growth to shorter wavelength and laser beacon use.
Coronagraphic quality
Scatter:
The cost model is considering various down-scoping options including relaxing the diameter
and scattered light requirements. It also will include estimates of constraction and operation
costs depending on site choice.
The study includes the design, modeling, analysis and costing of the telescope. Among these
are modeling of the telescope structure and co-rotating telescope envelope, of the primary
mirror support and thermal behavior, of the airflow in the telescope tube, and of the prime
focus heatstop. Ahead of us are the constraction and testing of a 1/6 scale mock-up of the
telescope enclosure to study issues related to seeing and dust control.
Parallel with the feasibility study, the CLEAR project is reviewing the suitability of existing
solar observatory sites for the location of the facility. Site parameters of interest are the amount
of time during which good seeing and/or coronal sky conditions are satisfied. The GONG site
survey data are used as a uniform data base for sunshine hour values and extinction/sky
conditions. Solar scintillometers, as seeing monitor proxies, are being installed on Hawaii, Big
Bear Solar Observatory, Sac Peak, and La Palma (Canary Islands) to compare seeing
conditions.
Outreach includes the CLEAR Web page (www.nso.noao.edu:80/~nsoclear/), lectures, and
workshops.
VI. CENTRAL COMPUTER SERVICES
Central Computer Services consists of two groups: the IRAF (Image Reduction and Analysis
Facility) group, and the Tucson computing support group.
The first bug fix patch for IRAF V2.10.4 was released early in FY 1996 for SunOS, Sun Solaris,
and OSF/1. Most of the bug fixes were minor, although a serious world coordinate system bug fix
was included that affected writing QPOE files in the PROS/XRAY package.
IRAF V2.10.4 for PCs ranning Linux was released at the same time (the initial release included the
patch mentioned above). The IRAF V2.10.4 port to Linux was done using the Slackware 2.3 Linux
distribution and the version 1.2.11 Linux kernel. The initial testing for the port was done on two
34
platforms, a high end Pentium system and a more modest 486DX2 66 MHz system. The distribution
includes Linux versions of xgterm and ximtool as well as an option to ran gzexe-compressed
executables on those systems with limited diskspace.
The IRAF V2.10.4 distribution for PCs ranning Linux has been a hot item since its release. In the
first several months since the release there have been roughly 275 distributions of PC-IRAF, either
from the network archive or by purchase of a CD-ROM (there have been about 2500 total copies of
IRAF V2.10 downloaded from our serverfor all platforms in the past couple years).
The second patch to IRAF V2.10.4 (V2.10.4-p2) was completed for the SunOS, Solaris, Linux
(Slackware), and DEC Alpha OSF/1 platforms. There were some minor bug fixes as well as
enhancements to support specific outside projects, but from the viewpoint of most users the main
reason for its release was platform support, i.e., to support changes to operating system software or
compilers. For Solaris/TRAF the patch adds support for Solaris 2.5 and the SunSoft version 4
compilers. This same distribution also supports Solaris 2.3 and 2.4. For Linux/IRAF the patch
includes support for ELF-based versions of Linux, but still uses the a.out format binaries. For
OSF/1, patch 2 was simply a bug fix upgrade since we are still ranning an older OSF/1 V2.0
operating system on our DEC Alpha. The current OSF1/IRAF release should ran fine under OSF/1
V3 but not the newly released Digital Unix 4.0. IRAF V2.10.4-p2 is also available now for
SGLTRIX. This was essentially a new port and is a major upgrade for this platform. The port was
done under IRDC 5.3. XI IIRAF binaries were also released for this platform, including support for
ximtool, xgterm, and xtapemon. We would like to thank Wisconsin and the WIYN Observatory for
letting us use their SGI for IRAF support.
The IRAFUsers' Committee, which met in Tucson in February (see below), made a strongplea that
we upgrade our support for those platforms neglected by recent IRAF software introductions and
patches. In particular we plan to make the XI IIRAF utilities (xgterm and ximtool), which have
been in use for one to two years now, available on all supported platforms. A new release of
XI IIRAF is due out soon and this version will be made available for all IRAF platforms. We have
begun negotiations with the vendors to update our platforms in preparation for the V2.ll release.
This includes updating hardware where necessary and obtaining and installing the current versions
of ADC, HPUX, IRDC, Digital UNIX, and OpenVMS (and a few others). This process is already
underway. Support for some older platforms will be dropped; support for Apple A/UX has already
been discontinued, as our A/UX Macintosh has died. Sun 386i support was dropped previously.
Unless we hear pleas from users we will probably drop support for the VAXstation running Ultrix
(not to be confused with DECstation Ultrix, which is still supported, although it is slated for
eventual retirement).
IRAF V2.10.4 is
now available for distribution on a
CDROM that includes
all V2.10.4
distributions, all IRAF documentation (mostly as PostScript files), selected NOAO layered
packages, and other miscellaneous items. These CDROMs are intended mainly as an alternative to
tape or network distributions.
Work continues on IRAF V2.ll, currently ranning on all the IRAF development systems. V2.ll
will add the FITS image kernel and the latest versions of all applications, and will upgrade all the
remaining IRAF platforms not already supported by V2.10.4-p2.
We are pleased to announce that a mirror of the IRAF network archive and Web pages at the
Rutherford Appleton Labs in the UK is now operational, as part of a collaborative effort with the
Starlink group at RAL. The FTP archive is available via anonymous FTP to starlink-ftp.rl.ac.uk,
35
directory pub/mirrors/iraf. The URL for access to the IRAF Web pages is http://starwww.rl.ac.uk/iraf. We expect this site will be popular with UK IRAF users who have found the
network connections to the US to be very slow. We are still learning how to operate a mirror
efficiently; once things are ranning routinely we hope to set up additional mirrors at other locations,
especially overseas.
Members of the IRAF Group attended the ADASS '95 Conference in Tucson in late October 1995,
and presented various papers on current IRAF projects. The IRAF BOF held on Monday during the
conference had a new format this year, emphasizing ERAF development by user sites. A number of
interesting contributed talks were given, followed by a presentation on IRAF system development,
and concluding with a group discussion of IRAF priorities and plans. An IRAF Developer's
Workshop was held on Thursday following the conference and was attended by over 60
participants. Software developers from around the world attended the workshop to discuss their
various IRAF projects. Special topics for this year included Pipeline Software, Archiving, and Data
Stractures. The workshop concluded with a group discussion of future directions and priorities for
IRAF development.
The IRAF User's Committee met in Tucson on 6 February to review the status of the IRAF project
and to advise NOAO in setting priorities for the IRAF project during the coming year. The IRAF
User's Committee is appointed by the NOAO Director to provide a communication link between
NOAO and the IRAF user community. The current committee members are Jeff Pier (USNO)
(Chair), Peter Eisenhardt (JPL), Andrea Prestwich (CfA, Harvard), Bill Romanishin (Oklahoma),
Bill Sparks (STScI), and Steve Walton (CalState, Northridge).
A major development for the ERAF project in this fiscal year was the award of a three-year NASA
ADP grant to IRAF to support the Open ERAF initiative. The Open IRAF initiative will evolve and
enhance IRAF in many ways to allow better integration of IRAF with non-IRAF software and data
formats, and improve the support for user software development. These enhancements will include
improved facilities for host execution of IRAF tasks and scripts, multi-language support, support
for host-callable IRAF libraries, and support for dynamically loadable modules. The multi-language
support will give the developer a choice of any of several different programming languages
including C, Fortran, and probably C++. The Open IRAF funding will also aid our efforts to
develop ERAF support for distributed objects and messaging and object component technology.
This project represents a collaboration of the ERAF group at NOAO and all the major ERAF
development sites within NASA, including HST, AXAF, SAO, and CEA.
A major development project for IRAF will be software support for the NOAO mosaic. The NOAO
Mosaic is an 8K x 8K CCD mosaic generating 128 MB (64 megapixel) images. Work thus far has
concentrated on keywords and the data dictionary, the Mosaic archival FITS data format, and
design of the messaging system and the real time display and mosaic viewer. The real time display
and mosaic viewer will provide near real time display and quick look analysis of single frame or
mosaic data during readout. The facility will be highly extensible to support integration with local
instrumentation, to support various messaging systems for data capture, custom data formats,
permit on the fly calibration, and so on.
Another current ERAF systems project is the transparency monitor, an automated camera that
continually observes Polaris to monitor the transparency of the sky (or at least a portion of the sky).
This is a high priority for KPNO and WIYN for monitoring observing conditions during
photometric rans and to help manage queue observing. It is an important and interesting project for
ERAF involving developing new capabilities which are important for the future evolution of ERAF,
36
such as distributed objects and messaging, support for heterogeneous systems (integrating ERAF
and non-IRAF components), and other elements of the Open IRAF initiative.
Lindsey Davis has continued work on the new world coordinate driven image matching package, a
first version of which was released early in FY 1996. The celestial coordinate transformations are
performed using the Starlink positional astronomy library SLALEB which has recently been ported
to IRAF. Lindsey has also begun work on defining the requirements for the new ERAF Astrometry
package, which will be a collaborative effort of Lindsey and others in the ERAF group, working
with astronomers and astrometric catalog providers from the general community.
Rob Seaman has been busy this fiscal year with the planned expansion of the NOAO "Save the
Bits" archive to include a dedicated CD-ROM based archive and data distribution system for the
WEYN telescope. We are also in the process of installing Save the Bits at CTEO, working with the
CTIO staff. CTIO data will be saved to dual Exabytes as is currently done at KPNO. Updates to the
ICE CCDACQ CCD data acquisition package and to the prototype FINDER package for generating
plate solutions from the image display using the HST Guide Star Catalog are in various stages of
completion.
Frank Valdes has been working on tools for the automated identification of arc-line spectra. The
task allows various types of constraining information such as approximate central wavelength and
dispersion. A minimum input to the task would be the arc line spectram, a line list, and an optional
wavelength-calibrated template spectram. The new auto-identification facilities should greatly
simplify the process of spectral dispersion calibration. Frank is currently extending the algorithms
to multi-order echelle spectra. Other recently completed projects include improvements to the
astronomical image header editor and a new astronomical calculator tool. The calculator tool may
be used for many purposes, one of which is a new task that identifies, from a large set of images, a
subset of images within a specified distance of a point in the sky. Frank has also enhanced the
EMEXAMENE and PSFMEASURE tasks for fitting stellar profiles to include Moffat profiles. Since
many groundbased stellar profiles are a better match to a Moffat profile than a Gaussian profile, the
new fitting model gives better full-width at half-maximum values.
The downtown Tucson computing facilities continue to evolve as older systems are replaced by
newer, more cost-effective and easier-to-maintain systems. In particular, the machines Gemini
(used as a Server on the Scientist Workstation Network) and Ursa (used for data reduction and
analysis by staff and visitors) were significantly upgraded during FY 1996. Also, several older disk
drives on various CCS systems failed during the year and were replaced by more reliable, and also
larger, disks. Similarly, older laser printers were replaced by newer, more capable printers.
The proliferation of desktop workstations, PCs and X-terminals to scientists' and engineers' offices
has slowed as saturation is approached; however, many desktop systems were upgraded to faster
systems over the course of the year. The network infrastructure in the downtown Tucson office
building was upgraded with the addition of several special purpose networks (including a Fast
Ethernet subnet) and the implementation of switched Ethernet on the building backbone network.
During FY 1996, a project was begun to completely rewrite the 14-year old Addresses, Lists and
Proposals System (ALPS) used to manage observing proposals and telescope usage statistics. ALPS
currently rans on a Sun system while the new version will utilize networked PCs. Enhanced
functionality and maintainability is the goal of the new project.
37
VII. SCIENTIFIC STAFF
A. CTIO Scientific Staff Changes
Alejandro Clocchiatti, one of the first recipients of a Gemini Fellowship, is spending a year at
CTIO carrying out supernova research.
Jack Baldwin is spending close to a year on sabbatical at the Institute of Astronomy,
Cambridge, UK. Jack's sabbatical ends in December.
Jay Elias transferred to Tucson in January to take on the role of Project Scientist for the ER
Spectrometer being built for Gemini by the NOAO.
Alistair Walker was promoted from Associate Astronomer with tenure to Astronomer during
October.
Richard Elston was promoted from Assistant Astronomer to Associate Astronomer, also
during the month of October.
Following his sabbatical here in FY 1996, Ron Probst has transferred to CTIO from KPNO for
three years commencing in August. Ron will be a member of the ER program team here, with
initial responsibilities for the f/14 tip tilt-system (after Richard Elston leaves) and for the
cryogenic optical bench.
B. KPNO Scientific Staff Changes
Hired
Date
Name
Position
10/1/95
Arjun Dey
Research Associate
03/1/96
Michael Corbin
Assistant Scientist
07/1/96
Paul Smith
Assistant Scientist
Completed Employment
Date
Name
Position
11/17/95
Stephane Chariot
Research Associate
11/30/95
David Crawford
Astronomer/Tenure
12/19/95
Paola Sartoretti
Research Associate
12/31/95
Helmut Abt
Astronomer/Tenure
12/31/95
Lloyd Wallace
Astronomer/Tenure
04/15/96
Michael Corbin
Assistant Scientist
38
Change of Status
Date
Name
Position
10/1/95
Tod Lauer
Promotion from Assistant Astronomer
10/1/95
Philip Massey
Promotion from Assistant Astronomer/Tenure
02/1/96
Taft Armandroff
Promotion from Associate Astronomer
07/1/96
David Silva
Promotion from Assistant Scientist
08/1/96
Ronald Probst
Transfer from KPNO to CTEO
to Associate Astronomer
to Astronomer/Tenure
to Associate Astronomer/Tenure
to Assistant Astronomer
C. NSO Scientific Staff Changes
Michael Dulick joined NSO/T as an NSF/Chemistry-funded Assistant Scientist, on 31 January
1996.
Rudolf Komm joined NSO/T as an SOI-funded Jr. Scientist on 15 August 1996.
John Varsik joined NSO/SP as a Research Associate on 9 October 1995.
During the reporting period, the following people visited NSO and stayed for a month or more:
H.M. Antia (Tata Inst, of Fundamental Research), T. Alan Clark (U. of Calgary), Irene
Gonzalez and Jesus Patron (Inst, de Astrofisica de Canarias), Jinghao Sun (Beijing
Astronomical Obs.), Sushant Tripathy (Udaipur Solar Obs.), Li Yan (U. of Sydney), and
Binxun Ye (Yunan Obs.).
VIII. DIRECTOR'S OFFICE
The current management stracture for NOAO consists of the following employees: Sidney
Wolff, NOAO Director; Richard Green, NOAO Deputy Director; Malcolm Smith, CTIO
Director/NOAO Associate Director; Mark Phillips, CTIO Assistant Director; Brace Bohannan,
KPNO Assistant Director; Robert Barnes, Assistant to the KPNO Director; Jacques Beckers,
NSO Director/NOAO Associate Director (Douglas Rabin served as Acting NSO Director during
FY 1996); Todd Boroson, USGP Project Scientist/NOAO Associate Director; Glen Blevins,
Manager, Central Administrative Services; Larry Daggert, Manager, Engineering and Technical
Services; John Dunlop, Manager, Central Facilities Operations; Yvette Estok, Manager, Public
Information Office; Steve Grandi, Manager, Central Computer Services.
The NOAO Director is responsible for the overall operation of NOAO, which includes providing
scientific leadership for NOAO, determining priorities, planning budgets, and allocating
resources. The Director represents NOAO, and in particular, the four scientific divisions (CTIO,
KPNO, NSO, and USGP) to AURA, NSF and the scientific community.
39
IX. NOAO STATISTICS
A. CTIO Statistics
During the period of 1 October 1995 through 30 September 1996, a total 198 separate
observing programs involving 417 scientists (223 visitors, 194 collaborators) were carried out
at CTIO. In the same period, 194 papers were published based on the use of Cerro Tololo
facilities. The number of nights CTIO scientific staff spent on CTIO during this period was
201. The number of public visitors to CTIO during this same period is estimated to be 5,960.
Breakdown of CTIO Observational Statistics
The figures in the following table reflect the number of observers/users physically present at
the Observatory and do not include multiple visits by a single observer/user. This table does
not include NOAO staff. The total number of visits including multiple ones is 328. Visiting
astronomers were assigned 93.2% of the observing time and the remaining 6.8% was assigned
to the staff.
Foreign
Total
Observers/Users
US
PhDs
105
17
37
159
41
2
11
54
Graduate Students
Technicians & Research Students
Total Visitors
Latin A.
4
6
150
25
48
223
10
134
8
52
194
32
102
-
Collaborators who were not
physically present
Institutions represented by
the above visits
63
USA Institutions (63)
Lawrence Livermore Nat. Lab.
Alma College
Louisiana State U.
Arizona State U.
Maria Mitchell Obs.
At&T Bell Labs.
Massachusetts Inst, of Tech.
Benedictine College
Brigham Young U.
Michigan State U.
Caltech, IPAC
NASA Ames
Carnegie Inst, of Washington
NASA Goddard
Millikin U.
Columbia U.
NASA Johnson
Cornell U.
New Mexico State U.
Darmouth College
Ohio State U.
Drew U.
Pennsylvania State U.
Pomona College
Fermi Nat. Accelerator Lab.
Franklin & Marshall College
Georgia State U.
Georgia Inst. Tech.
Princeton U.
Purdue U.
Rice U.
Rutgers U.
Saint John's College
Space Telescope Science Inst.
Harvard-Smithsonian
Imperial College, UK
Johns Hopkins U.
40
Foreign Institutions (32)
Anglo-Australian Obs., Australia
Armagh Obs., Ireland
State U. of New York
U. of Alabama
U. of Alaska
DAO, Canada
Durham U., UK
U. of Arizona
U. of California, Berkeley
U. of California, Los Angeles
Edinburgh U., UK
European Southern Obs., Germany
U. of California, Santa Cruz
U. of Chicago
Leicester U., UK
McMaster U., Canada
U. of Colorado
U. of Hawaii
Max-Planck Inst., Germany
U. of Illinois
MSSSO, Australia
U. of Kansas
Nagoya City U., Japan
Nat. Astron. Obs., Japan
U. of Maryland
Nat. Central U., Taiwan
Oxford U., UK
SAAO, South Africa
U. of Massachusetts
U. of Michigan
U. of Minnesota
U. of Missouri
Sternberg Astron. Inst., Russia
U. of North Carolina
Stockholm Obs., Sweden
U. of Pennsylvania
U. of Oregon
U. College London, UK
U. of Birmingham, UK
U. of Texas
U. of British Columbia, Canada
U. of Washington
U. of Cambridge, UK
U. of Wisconsin
U. of Central Lancashire, UK
US Naval Obs.
U. of Lisbon, Portugal
Western Connecticut State U.
U.
U.
U.
U.
U.
Yale U.
Latin American Institutions (7)
Las Campanas Obs., Chile
Obs. Astron. La Plata, Argentina
of Montreal, Canada
of Sussex, UK
of Toronto, Canada
of Victoria, Canada
of Wales, UK
U. of Waterloo
U. Nac. Mexico, Mexico
Yonsei U., Korea
York U., Canada
Obs. Nacional, Brazil
U. de Sao Paulo, Brazil
UFRGS, Brazil
U. de Chile
U. de La Serena, Chile
B. KPNO Statistics
During the period 1 October 1995 through 30 September 1996, a total of 254 observing
programs were carried out by visitors and the NOAO staff at Kitt Peak. Associated with these
programs were 492 individual scientists, and 42 programs were identified as graduate theses.
Visiting astronomers were assigned 83% of the scheduled telescope time and the remaining
17% was assigned to the staff.
Astronomers using Kitt Peak telescopes in this period represented 86 US institutions and 28
foreign institutions. The top five represented are:
1) Space Telescope Science Institute (18);
2) University of Arizona (15);
41
3) Johns Hopkins University (10) and University of Colorado (10);
4) NASA Goddard Space Flight Center (8) and Pennsylvania State University (8);
5) University of Maryland (7), and Harvard-Smithsonian CfA (7).
Observers/Users
PhDs
US
243
Graduate Students
92
Technicians & Research Students
28
Total Visitors
Foreign
36
6
—
Total
279
98
28
363
42
405
86
28
114
Institutions represented by
the above visits
The number of public visitors to Kitt Peak in this period is estimated to be 35,000. This
estimate is based on the number of visitors attending two daily scheduled tours on Kitt Peak
and does not factor in visitors taking self-guided tours or visitors scheduling special tours
through the Public Information Office.
C. NSO Statistics
During the period of 1 October 1995 through 30 September 1996, a total of 211 observing
programs, involving 138 individual scientific visitors and 33 staff were carried out at NSO
facilities. Astronomers using NSO facilities during this period represented 42 US institutions
and 25 foreign institutions. Visiting astronomers were assigned 33% of the scheduled telescope
time and the remaining 67% was assigned to the staff.
During the reporting period a total of 914 outside users from 1020 institutions accessed the
main NSO/Tucson data archive and distribution area a total of 11,025 times. A total of 30,425
data files were transferred during these accesses. In addition, 23 distributions per observing day
are made automatically to outside users, adding approximately 5500 distributions per year for a
total of over 36,000 data distributions annually to about 950 users. During this same time
period, NSO web pages were accessed by outside users a total of 36,384 times. Note that these
statistics are for NSO/Tucson only.
During the reporting period a total of 11608 scientific data files were transferred via
anonymous ftp from NSO/Sac Peak.
Observers/Users
US
PhDs
110
35
2
3
5
19
98
2
21
40
138
42
25
67
Graduate Students
Technicians & Research Students
Total Visitors
Foreign
Total
145
Institutions represented by
the above visits
D. NOAO Tucson Headquarters Building Statistics
During the period 1 October 1995 through 30 September 1996, a total of 1,777 visitors signed in
at the NOAO Tucson headquarters building.
42
APPENDIX A
National Optical Astronomy Observatories
October 1995 to September 1996 Technical Reports
The following papers were published by CCS personnel:
Barnes, J. (Editor) 1996, ASP Conf. 101: Astronomical Data Analysis Software and Systems V, ed. G.H.
Jacoby, J. Barnes (ASP).
Bell, D.J., et al. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.451, "An Automated System for
Receiving KPNO Proposals by Electronic Mail"
Bell, D.J. 1996, PhD Thesis (U. of Illinois at Urbana-Champaign), "A Kinematic and Abundance Survey
in the Galactic Rotational Directions"
Bragaglia, A., et al. 1996, ASP Conf. 92, ed. H. Morrison (ASP), p.175, "Definition of a Pure Sample of
Nearby BHB Stars"
Cotton, S.D., Tody, D., Pence, W.D. 1995, A&AS, 113, p.159, "Binary Table Extension to FITS"
Davis, L.E. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.147, "World Coordinate System Based
Image Registration Tools for IRAF"
Fitzpatrick, M., Tody, D. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.68, "Datastream Compression
for IRAF Image Display"
Gillies, K., Walker, S. 1996, ASP Conf. 101, ed. G.H. Jacoby, p.347, "The Design of the Gemini
Observatory Control System"
Heim, G.B., Buchholz, N., Fowler, A.M. 1995, SPEE, 2475, p.118, "Controlling an ALADDIN IK x IK
Array with Wildfire"
Kinman, T.D., et al. 1996, AJ, 111, p.1164, "A Preliminary Discussion of the Kinematics of BHB and
RR Lyrae Stars Near the North Galactic Pole"
Marshall, B., Gillies, K., Lewis, J. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.408, "The Integration
of Telescopes, Instruments, and User Interfaces at KPNO and WIYN"
McGehee, P.M., Wampler, S.B., Gillies, K.K. 1996, SPEE, 2479, p.193, "Command Completion Within
an EPICS Database"
Mills, D. 1996, SPEE, 2479, p.50, "The WIYN Telescope Graphical User Interfaces"
Mills, D. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.233, "BOF Session-Linux Users"
Seaman, R., Bohannan, B. 1996, ASP Conf. 87, ed. T.A. Boroson (ASP), p. 114, "Alternate Observing
Options at Kitt Peak National Observatory"
Seaman, R. 1996, ASP Conf. 87, ed. T.A. Boroson (ASP), p.229, "Save the Bits at the Kitt Peak National
Observatory"
Seaman, R., Bohannan, B. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.432, "Remote Observing and
Automatic FTP on Kitt Peak"
Tody, D., Fitzpatrick, M. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.322, "PC-ERAF: The Choice of
a GNU Generation"
Valdes, F.G., et al. 1995, PASP, 107, p.1119, "FOCAS Automatic Catalog Matching Algorithms"
Valdes, F.G. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.33, "Automated Arc Line Identifications in
IRAF"
The following papers were published by ETS personnel:
Fowler, A.M., et al. 1995, SPIE, 2475, p.27, "ALADDEN, the 1024 x 1024 InSb Array: Test Results"
Fowler, A.M. (Editor) 1995, SPEE v.2475: Infrared Detectors and Instrumentation for Astronomy, ed.
A.M. Fowler (SPIE).
Gregory, B., et al. 1995, SPEE, 2475, p.318, "Design of an Efficient Infrared Spectrometer for Large
Telescopes"
Heim, G.B., Buchholz, N., Fowler, A.M. 1995, SPEE, 2475, p.118, "Controlling an ALADDIN IK x IK
Array with Wildfire"
Roddier, N., et al. 1995, SPIE, 2479, p.364, "The WIYN Telescope Active Optics System"
APPENDIX B
Cerro Tololo Inter-American Observatory
October 1995 to September 1996 Publications List
Agostinho, R., et al. 1995, The Formation of the Milky Way, ed. E.J. Alfaro, A.J. Delgado (Cambridge
U. Press), p. 211, "UVW Components, Proper Motions, Age and Chemical
Composition of Disk Stars at the South Galactic Pole"
Alcock, C, et al. 1996, ApJ, 463, L67, "Real-Time Detection and Multisite Observations of Gravitational
Microlensing"
Allain, S., et al. 1996, A&A, 305, p. 498, ARotational Periods and Starspot Activity of Young SolarType Dwarfs in the Open Cluster IC 4665"
Bailyn, CD., et al. 1995, Nature, 378, p. 157, "Dynamical Evidence for a Black Hole in the Eclipsing XRay Nova GRO J1655-40"
Baldwin, J., et al. 1995, ApJ, 455, LI 19, "Locally Optimally Emitting Clouds and the Origin of
Quasar Emission Lines"
Baldwin, J.A., et al. 1996, ApJ, 461, p. 664, "Very High Density Clumps and Outflowing Winds in QSO
Broad-Line Regions"
Baldwin, J.A., et al. 1996, ApJ, 468, LI 15 "Physical Conditions in Low- Ionization Regions of the Orion
Nebula"
Balona, L.A., Krisciunas, K. 1995, ASP Conf. 83, ed. R.S. Stobie, P.A. Whitelock (ASP), p. 341,
"Slowly Variable Early F-Type Stars"
Bautista, M.A., Pogge, R.W., DePoy, D.L. 1995, ApJ, 452, p. 685, "The Nebular Extinction in the Orion
Nebula"
Beers, T.C., et al. 1996, AJ, 112, p. 1188, "Additonal Emission-Line Candidates From the HK Survey"
Berdnikov, L.N., Turner, D.G. 1995, Astonomy Letters, 21, p. 803, "Photoelectric Observations of
Southern Cepheids in 1995"
Berdnikov, L.N., Turner, D.G. 1995, Astronomy Letters, 21, p. 534, "Photoelectric UBV(RI)C
Photometry of Southem-Sky Cepheids"
Bica, E., et al. 1996, ApJS, 102, p. 57, "Integrated UBV Photometry of 624 Star Clusters and
Associations in the Large Magellanic Cloud"
Blum, R.D., DePoy, D.L., Sellgren, K. 1996, IAU Symp. 169, ed. L. Blitz, P. Teuben (Kluwer), p. 225,
"A Comparison of Near Infrared Spectra of the Galactic Center HE I Emission Line Sources and Early
Type Mass Losing Stars"
Boesgaard, A.M. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p. 327, "Light Element
Abundances in the Halo"
Brown, J.A., Wallerstein, G., Zucker, D. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p.
355, "Echelle Spectroscopy and Abundances in Ruprecht 106 and Pal 12"
Buta, R., Purcell, G.B., Crocker, D.A. 1995, AJ, 110, p. 1588, "Intrinsic Bar/Ring Misalignment and a
Starburst Nuclear Ring in the Peculiar Spiral Galaxy ESO 565-11"
Caldwell, N., et al. 1996, AJ, 111, p. 78, "Spatial Distribution of the Starbursts in Post-Starburst Coma
Cluster Galaxies"
Campusano, L., Hardy, E. 1996, IAU Symp. 173, ed. C.S. Kochanek, J.N. Hewitt (Kluwer), p. 125, "A
Luminous Arc in A Z=0.042 Cluster of Galaxies, The Nearest Gravitational Arc Known?"
Carney, B.W., et al. 1995. AJ, 110, p. 1674, "The Distance to the Galactic Center Obtained by Infrared
Photometry of RR Lyrae Variables"
Carswell, R.F., et al. 1996, MNRAS, 278, p. 506, "The High-Redshift Deuterium Abundance: The z =
3.086 Absorption Complex Towards Q 0420-388"
Cellone, S.A., Forte, J.C. 1996, ApJ, 461, p. 176, "Washington Photometry of Low Surface Brightness
Dwarf Galaxies in the Fornax Cluster: Constraints on Their Stellar Populations"
Churchwell, E., et al. 1996, ApJ, 469, p. 209, "The Western Rim of the Vela Shell"
Ciardullo, R., Bond, H.E. 1996, AJ, 111, p. 2332, "A Survey for Pulsations in O VI Nuclei of Planetary
Nebulae"
Claria, J.J., Piatti, A.E., Osbom, W. 1996, PASP, 108, p. 672, "DDO Metal Abundances of HighLuminosity Late-Type Stars in Galactic Clusters"
Colbert, J.M., et al. 1996, ApJS, 105, p. 75, "Large-Scale Outflows in Edge-On Seyfert Galaxies. I.
Optical Emission-Line Imaging and Optical Spectroscopy"
CAU, P., et al. 1995, ApJ, 454, p. 788, "Dynamics of the Galactic Globular Cluster NGC 3201"
CAU, P., et al. 1996, ASP Conf. 90, ed. E.F. Milone, J.C. Mermilliod (ASP), p. 222, "Searching for
Spectroscopic Binaries in the Globular Clusters M4 and M22"
CALJ, P., et al. 1996, AJ, 112, p. 565, "Spectroscopic Binaries in Globular Clusters. I. A Search for UltraHard Binaries on the Main Sequence in M4"
CAtJ, P., et al. 1996, AJ, 112, p. 574, "Spectroscopic Binaries in Globular Clusters. II. A Search
for Long-Period Binaries in M22"
Cowley, A.P., et al. 1995, PASP, 107, p. 927, "X-Ray Discovery of a Hot PG 1159 Star, RX J0122.97521"
Crocker, D.A., Baugus, P.D., Buta, R. 1996, ApJS, 105, p. 353, "The Distribution and Properties of H H
Regions in Early-to-Intermediate Hubble Type Ringed Galaxies"
Diaz, M.P., Steiner, J.E. 1995, AJ, 110, p. 1816, "The Nova-Like Variable WX Centauri and the V
Sagittae Phenomenon"
Diaz, M.P., et al. 1995, MNRAS, 277, p. 959, "Recent Observations of Nova GQ Mus 1983"
Dinshaw, N., Impey, CD. 1996, ApJ, 458, p. 73, "Two-Point Velocity and Spatial Correlation Functions
of the C IV Absorption Systems Toward the Tololo Quasar Group: Evidence for Superclustering at z • 2"
Dixon, W.V., Davidsen, A.F., Ferguson, H.C. 1995 ApJ, 454, L47, "Observations of the UltravioletBright Star in 47 Tucanae with the Hopkins Ultraviolet Telescope"
Djorgovski, S.G., et al. 1996, Nature, 382, p. 234, "Identification of a Galaxy Responsible for a HighRedshift Lyman- " Absorption System"
Dottori, H., et al. 1996, ApJ, 461, p. 742, "Spatial Distributions of Young Large Magellanic Cloud
Clusters as Tracers of a Bar Perturbation"
Drilling, J.S., Bergeron, L.E. 1995, PASP, 107, p. 846, "An Extension of the Case-Hamburg OB-Star
Surveys"
Drilling, J.S., Beers, T.C., Heber, U. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R.
Upgren, C.J. Adelman (Cambridge U. Press), p. 182, "Very Hot Subdwarf O Stars"
Durrell, P.R., et al. 1996, ApJ, 463, p. 543, "Globular Cluster Systems in Dwarf Elliptical Galaxies. I.
The dE,N Galaxy NGC 3115 DW1"
Eggen, O.J. 1995, AJ, 110, p. 1749, "Pre-Main-Sequence Stars in the Pleiades Supercluster"
Eggen, O.J. 1996, AJ, 110, p. 2862, "Reality Tests of Superclusters in the Young Disk Population"
Eggen, O.J. 1996, AJ, 111, p. 466, "Distribution and Correlation of Age, Abundance, and Motion of
Lower Main Sequence Stars"
Eggen, O.J. 1996, AJ, 111, p. 1313, "Photometric Parameters for Short-Period Cepheids"
Eggen, O.J. 1996, AJ, 111, p. 1615, "The Stellar Content of Star Stream I"
Ellingson, E., et al. 1996, ApJ, 466, L71, "Optical-IR Spectral Energy Distribution of the Protogalaxy
Candidate MS1512-cB58"
Elston, R., et al. 1996, ApJ, 456, L13, "A Redshift 4.38 Mg II Absorber Toward BR 1202-0725"
Ferland, G.F., et al. 1996, ApJ, 461, p. 683, "High Metal Enrichments in Luminous Quasars"
Ferguson, A.M.N., et al. 1996, AJ, 111, p. 2265, "Diffuse Ionized Gas in Spiral Galaxies: Probing Lyman
Continuum Photon Leakage from H II Regions?"
iii
Ford, H.C, et al. 1996, ApJ, 458, p. 455, "The Stellar Halo of M104. I. A Survey for Planetary Nebulae
and the Planetary Nebula Luminosity Function Distance"
Francis, P.J., et al. 1996, ApJ, 457, p. 490, "A Group of Galaxies at Redshift 2.38"
Friel, E.D., et al. 1995, The Formation of the Milky Way, ed. E.J. Alfaro, A.J. Delgado (Cambridge U.
Press), p. 189, "New Results for the Oldest Open Clusters: Kinematics and Metallicities of the Old Disk"
Fullton, L.K., Carney, B.W. 1996, ASP Conf. 92, ed. H. Morrison A. Sarajedini (ASP), p. 265, "New
Age and Abundance Estimates for NGC 6723: Clues Regarding Formation of the Inner Halo"
Gebhardt, K., et al. 1995, AJ, 110, p. 1699, "Fabry-Perot Observations of Globular Clusters. B. 47 Tuc,
NGC 6397, and M30"
Geisler, D. Sarajedini, A. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p. 524, "Standard
Giant Branches in the Washington System: Calibration and Application to the Draco, Ursa Minor and
Sextans Dwarf Spheroidal Galaxies"
Giridhar, S., Rao, N.K., Lambert, D.L. 1996, ASP Conf. 96, ed. C.S. Jeffery, U. Heber (ASP), p. 171,
"Spectral Variations of DY Cen"
Gonz<lez, G., Wallerstein, G. 1996, MNRAS, 280, p. 515, "ST Pup: A Binary Type EE Cepheid with a
Peculiar Chemical Composition"
Graham, M.J., Clowes, R.G., Campusano, L.E. 1996, MNRAS, 279, p. 1349, "A Quasar with
Ultrastrong, Ultraviolet Fe II Emission"
Gregory, B., et al. 1995, Proceedings of the SPEE, Vol. 2475, p. 318, "Design of an Efficient Infrared
Spectrometer for Large Telescopes"
Haller, J.W., et al. 1996, ApJ, 456, p. 194, "Stellar Kinematics and the Black Hole in the Galactic
Center"
Hartkopf W.I., et al. 1996, AJ, 111, p. 936, AICCD Speckle Observations of Binary Stars.
Measurements During 1989-1994 from the Cerro Tololo 4 M Telescope®
XUI.
Hartkopf, W.I., Mason, B.D., McAlister, H.A. 1996, AJ, 111, p. 370, "Binary Star Orbits From Speckle
Interferometry. VIII. Orbits of 37 Close Visual Systems"
Hazen, M.L. 1996, AJ, 111, p. 1184, "A Search for Variable Stars in the Globular Clusters NGC 5694
and NGC 6558"
Heathcote, S.R., et al. 1996, AJ, 112, p. 1141, "Hubble Space Telescope Observations of the HH47 Jet:
Narrow Band Images"
Henry, T.J., et al. 1996, AJ, 111, p. 439, "A Survey of CA II H and K Chromospheric Emission in
Southern Solar-Type Stars"
iv
Hill, G.J., Goodrich, R.W, DePoy, D.L. 1996, ApJ, 462, p. 163, "Observations of Paschen " in a
Complete Sample of Radio Galaxies"
Hill, R.S., et al. 1996, AJ, 112, p. 601, "UJT: New Ultraviolet Stellar Photometry and Surface Brightness
Profiles of the Globular Cluster M79 (NGC 1904)"
Huchra, J.P., et al. 1996, ApJS, 102, p. 29, "Extragalactic Globular Clusters. IV. The Data"
Hunter, D.A. 1996, ApJ, 457, p. 671, "Supershells and Chimneys: The Giant Ionized Gas Filaments in
NGC 1800"
Hunter, D.A., Plummer, J.D. 1996, ApJ, 462, p. 732, "Sextans A: A Case Study of Star Formation and
Gas Densities in Irregular Galaxies"
Hutchings, J.B., et al. 1995, PASP, 107, p. 931, "An X-Ray Selected White Dwarf + M Dwarf Binary:
RX J0458.9-6628"
Hutchings, J.B., et al. 1995, AJ, 110, p. 2394, "UV Spectra of the Eclipsing LMC X-Ray Binary CAL
87"
Irwin, M., et al. 1996, ASP Conference Series 92, ed. H. Morrison, A. Sarajedini (ASP), p. 84, "The
Space Motion and Extent of the Sagittarius Dwarf Galaxy"
Jewitt, D., Luu, J., Chen, J. 1996, AJ, 112, p. 1225, "The Mauna Kea-Cerro- Tololo (MKCT) Kuiper Belt
and Centaur Survey"
Johansson, S., et al. 1995, A&A, 300, p. 521, "Fluorescence Lines of Mn EI in the Red Spectram of 0
Carinae"
Kassis, M., Friel, E.D., Phelps, R.L. 1996, AJ, 111, p. 820, "CCD Photometry of the Old Open Cluster
092-SC18"
Kennefick, J.D., Djorgovski, S.G., Meylan, G. 1996, AJ, 111, p. 1816, "A Multicolor CCD Survey for
Faint z > 4 Quasars"
Kinman, T.D., et al. 1996, AJ, 111, p. 1164, "A Preliminary Discussion of the Kinematics of BHB and
RR Lyrae Stars Near the North Galactic Pole"
Kinman, T.D., Suntzeff, N.B., Kraft, R.P. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R.
Upgren, C.J. Adelman (Cambridge U. Press), p. 353, "A Survey for Field BHB Stars Outside the Solar
Circle"
Kinney, A.L., et al. 1996, ApJ, 467, p. 38 "Template Ultraviolet to Near-Infrared Spectra of StarForming Galaxies and Their Application to A'-Correction"
Kochanski, G.P., Tyson, J.A., Fischer, P. 1996, AJ, 111, p. 1444, "Flickering Faint Galaxies: Few and
Far Between"
Krisciunas, K., et al. 1995, MNRAS, 277, p. 1404, "A Search for ( Doradus-Type Variable Stars in the
Hyades"
Kuchinski, L.E., Terndrup, D.M. 1996, AJ, 111, p. 1073, "Infrared Photometry and Dust Absorption in
Highly Inclined Spiral Galaxies"
Landsman, W.B., et al.
1996, ASP Conference 99, ed. S.S. Holt, G. Sonnebom (ASP), p.199,
"Spectroscopic Constraints on the Helium Abundance in Globular Cluster Stars"
Lavery, R.J., et al. 1996, ApJ, 467, LI, "Distant Ring Galaxies as Evidence for a Steeply Increasing
Galaxy Interaction Rate with Redshift"
Lavery, R.J., et al. 1996, ASP Conference 98, ed. C. Leitherer, U. Fritze-v. Alvensleben, J. Huchra
(ASP), p. 333, "HST/WFPC2 Imaging of the Tucana Dwarf Galaxy"
Lawrence, C.R., et al. 1995, AJ, 110, p. 2570, "MG 0414+0534: A Dusty Gravitational Lens"
Layden, A.C, 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini, (ASP), p. 141, "Kinematics of RR
Lyrae Stars in the Inner and High Halos"
Layden, A.C. 1994, Hot Stars in the Galactic Halo, ed. S.J. Ademan, A.R. Upgren, C.J. Adelman,
(Cambridge U.Press), p. 287, "Metallicities and Kinematics of the Local RR Lyrae Stars: Lukewarm
Stars in the Halo"
Lehnert, M.D., Heckman, T.M. 1996, ApJ, 462, p. 651, "Ionized Gas in the Halos of
Edge-On Starburst Galaxies: Evidence for Supernova-Driven Superwinds"
Leibundgut, B., et al. 1995, Messenger, 81, p.19, "Discovery of a Supernova (SN 1995K) at a Redshift of
0.478"
Leibundgut, B., et al. 1996, ApJ, 466, L21, "Time Dilation in the Light Curve of the Distant Type la
Supernova SN 1995K"
Lu, P.K. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R. Upgren, C.J. Adelman, (Cambridge
U.Press), p. 124, "Hot Stars at the South Galactic Pole"
Luhman, M.L., Jaffe, D.T. 1996, ApJ, 463, p. 191, "Ultraviolet-Excited H2: A Comparison with LargeScale Tracers of Molecular Clouds"
Magalhnes, A.M., et al. 1996, ASP Conference 97, ed. W.G. Roberge, D.C.B. Whittet (ASP), p. 118,
"High Precision CCD Imaging Polarimetry"
Magnier, E.A., et al. 1996, ApJ, 464, p. 829, "X-Rays From Superbubbles in the Large Magellanic
Cloud. IV. The Blowout Stracture of N44"
Mason, B.D., McAlister, H.A., Hartkopf W.I. 1996, AJ, 112, p. 276, "Binary Star Orbits From Speckle
Interferometry. IX. The Nearby Solar-Type Speckle-Spectroscopic Binary Fin 347 Aa"
vi
Massey, P., et al. 1995, AJ, 110, p. 2715, "Hot, Luminous Stars in Selected Regions of NGC 6822, M31,
and M33"
Matthews, J.M., et al. 1996, ApJ, 459, p. 278, AOpening a New Window on Ap Star Atmospheres: A T J Relation for HR 3831 From its Limb-Darkened Pulsation Amplitudes®
Maza, J., et al. 1995, Rev.Mex.Astron.Astrofis., 31, p. 119, "Cal<n-Tololo Survey. VI. One Hundred
New Southern Quasars"
Maza, J., et al. 1995, Rev.Mex.Astron.Astrofis., 31, p. 159, "Cakn-Tololo Survey. VIE. One Hundred
Southern Quasars"
McAlister, H.A., et al. 1996, AJ, 112, p. 1169, "ICCD Speckle Observations of Binary Stars. XEV. A
Brief Survey for Duplicity Among White Dwarf Stars"
McNamara, B.R., et al. 1996, ApJ, 466, L9, "Optical Stracture in the Abell 1795 Cluster Central Galaxy:
Evidence for Stripping and Deflection of Radio Jets"
McNamara, B.R., et al. 1996, ApJ, 469, p. 66, "U-Band Polarimetry of the Radio-Aligned Optical
Continuum in the Abell 1795 Cluster Central Galaxy"
Minniti, D. 1995, A&AS, 113, p. 299, "Abundances and Velocities for Open and Globular Cluster
Giants: The Data"
Minniti, D., et al. 1995, MNRAS, 277, p. 1293, "The Metallicity Gradient of the Galactic Bulge"
Minniti, D. 1996, ApJ, 459, p. 175, AField Stars and Clusters of the Galactic Bulge: Implications for
Galaxy Formation®
Minniti, D., et al. 1996, AJ, 112, p. 590, "Background Giants in the Field of the Globular Cluster M22:
Kinematics of the Galactic Bulge"
Montgomery, K.A., Janes, K.A. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R. Upgren,
C.J. Adelman (Cambridge U. Press), p. 136, "Population II Horizontal Branches: A Photometric Study of
Globular Clusters"
Mulchaey, J.S., Wilson, A.S. 1995, ApJ, 455, L17, "An Alignment Between Optical Continuum and
Emission-Line Structures in the Circumnuclear Regions of Seyfert Galaxies"
Mulchaey, J.S., Wilson, A.S., Tsvetanov, Z. 1996, ApJS, 102, p. 309, "An Emission-Line Imaging
Survey of Early-Type Seyfert Galaxies. I. The Observations"
Mulchaey, J.S., Wilson, A.S., Tsvetanov, Z. 1996, ApJ, 467, p. 197, "An Emission-Line Imaging Survey
of Early-Type Seyfert Galaxies. II. Implications for Unified Schemes"
Netzer, H., et al. 1996, MNRAS, 279, p. 429, AOptical Monitoring of Luminous AGN - I. Radio-Loud
Quasars®
vn
Niemela, V., et al. 1996, ASP Conf. 90, ed. E.F. Milone, J.C. Mermilliod (ASP), p. 133, " The Open
Cluster RU 55: OB Members, Search for Binaries, and the Surrounding ISM"
Niemela, V., et al. 1996, ASP Conf. 90, ed. E.F. Milone, J.C. Mermilliod (ASP), p. 224 "A Search for
Spectroscopic Binaries in the Magellanic Clouds"
Nugent, P., et al. 1995, ApJ, 455, L147, "Evidence for a Spectroscopic Sequence Among Type la
Supernovae"
Oey, M.S., Massey, P. 1995, ApJ, 452, p. 210, "Triggered Star Formation and the Dynamics of a
Superbubble in the LMC: The OB Association LH 47/48 in DEM 152"
Oey, M.S. 1996, ApJ, 465, p. 231, " Stellar Content of Superbubble H H Regions in the Large Magellanic
Cloud"
Orosz, J.A., et al. 1996, ApJ, 468, p. 380, "Improved Parameters for the Black Hole Binary System XRay Nova Muscae 1991"
Orsatti, A.M. 1995, AJ, 110, p. 1728, "Ruprecht 55 or the Two-In-One Cluster"
Oswalt, T.D., et al. 1995, Nature, 382, p. 692, "A Lower Limit of 9.5 Gyr on the Age of the Galactic
Disk From the Oldest White Dwarf Stars"
Pandey, G., Rao, K.N., Lambert, D.L. 1996, ASP Conf. 96, ed. C.S. Jeffery, U. Heber (ASP), p. 167,
"MV Sgr-The Emission Line Spectram"
Pandey, G., Kameswara Rao, N., Lambert, D.L. 1996, MNRAS, 282, p. 889, "The Emission-Line
Spectram of the Hot R Coronae Borealis Star MV Sgr"
Patterson, J., et al. 1995, PASP, 107, p. 1183, "Superhumps in Cataclysmic Binaries. VIII.
V1159 0rionis"
Phelps, R.L., Janes, K.A., Montgomery, K.A. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman,
A.R. Upgren, C.J. Adelman (Cambridge U. Press), p. 175, "Population I Horizontal Branches: Probing
the Halo-to-Disk Transition"
Piatti, A.E., Clari<, J.J., Abadi, M.G. 1995, AJ, 110, p. 2813, "Chemical Evolution of the Galactic Disk:
Evidence for a Gradient Perpendicular to the Galactic Plane"
Pogge, R.W., et al. 1995, PASP, 107, p. 1226, "The Ohio State Imaging Fabry-Perot Spectrometer
(IFPS)"
Porto de Mello, G.F. 1996, Ph.D. Thesis (CNPq, Brazil), "A DistribuiH>o de Abund>ncias em Estrelas
de Tipo Solar Na VizinhanHa Solar"
Prosser, C.F., Randich, S., Stauffer, J.R. 1996, AJ, 112, p. 649, "Photometry in the Open Clusters IC
2602 & NGC 6475"
Vlll
Purcell, G.B., Buta, R. 1996, ASP Conf. 91, ed. R. Buta, D.A. Crocker, B.G. Elmegreen (ASP), p. 244,
"Photometry and Kinematics of the Ringed Barred Galaxy NGC 3081"
Quintana, H., RamRrez, A., Way, M.J. 1996, AJ, 111, p. 603, " Spectroscopy of the NGC 4782/3
Dumbbell Dominated Group of Galaxies: Dark Haloes and Merger of Subgroups"
Quintana, H., RamRrez, A., Way, M.J. 1996, AJ, 112, p. 36, "Dynamics of the Cluster of Galaxies
A3266 (SERSIC 40/6). I. Spectroscopic Data"
Reed, B.C. 1996, PASP, 108, p. 61, "H$ Photometry of Southern Luminous Stars"
Remillard, R.A., et al. 1996, ApJ, 459, p. 226, ADynamical Evidence for a Black Hole in X-Ray Nova
Ophiuchi 1977"
Ribeiro, A.L.B., et al. 1996, ApJ, 463, L5, "HCG 16: A High Concentration of Active Galaxies in the
Nearby Universe"
RodrRguez-Ardila, A., et al. 1996, ApJ, 463, p. 522, "The Nucleus of C16.16: Another Case of a DoublePeaked Active Galactic Nucleus"
Rose, J.A. 1996, ASP Conf. 86, ed. A. Buzzoni, A. Renzini, A. Serrano (ASP), p. 157, "The Role of
Environment on the Stellar Content of Early-Type Galaxies"
Rosen, S., et al. 1995, ASP Conf. 85, ed. D.A.H. Buckley, B. Warner (ASP), p. 279, AEUVE
Spectrophotometry of QS Tel (RE1938-461): The Second Pole Becomes Active®
Rosen, S.R., et al. 1996, MNRAS, 280, p. 1121, "Accretion Mode Changes in QS Tel (RE 1938-461):
EUVE, ROAST and Optical Observations"
Rubenstein, E.P., Bailyn, CD. 1996, AJ, 111, p. 260, "A W UMa Contact Binary in the Globular Cluster
NGC 6397"
Ruiz, M.T., et al. 1995, ApJ, 455, L159, "The Extremely Low Luminosity White Dwarf ESO 439-26"
Ruiz, M.T. 1996, AJ, 111, p. 1267, "New Cool Degenerate Stars"
Ryan, S.G., Deliyannis, C.P. 1995, ApJ, 453, p. 819, "Lithium in Short-Period Tidally Locked Binaries:
A Test of Rotationally Induced Mixing"
Sadler, E.M., Rich, R.M., Terndrap, D.M. 1996, AJ, 112, p. 171, "K Giants in Baade's Window. B.
The Abundance Distribution"
Sandquist, E., Bolte, M., Stetson, P. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p. 293, "
The Composition and Stellar Populations of M5"
Santiago, B.X., et al. 1996, ApJ, 461, p. 38, "The Optical Redshift Survey. B. Derivation of the
Luminosity and Diameter Functions and of the Density Field"
Sarajedini, A., Layden, A. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p. 297,
AMetallicities and Reddenings for Young Globular Clusters®
ix
Sarajedini, A. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R. Upgren, C.J. Adelman
(Cambridge U. Press), p. 100, "Recent Progress on a Continuing Survey of Galactic Globular Clusters for
Blue Straggler Stars"
Schachter, J.F., et al. 1996, ApJ, 463, p. 747, "Optical and X-Ray Characteristics of Stars Detected in the
Einstein Slew Survey"
Schaefer, B.E. 1996, ApJ, 460, LI9, "The Peak Brightness of SN 1960F in NGC 4496 and the Hubble
Constant"
Schmidtke, P.C, et al. 1996, AJ, 111, p. 788, AA Supersoft X-Ray Binary in the Small Magellanic
Cloud®
Schmidtke, P.C, Cowley, A.P. 1996, AJ, 112, p. 167, "Optical Identification and Photometry of the
LMC Supersoft X-Ray Source RX J0439.8-6809"
Schmidtke, P.C, et al. 1996, PASP, 108, p. 668, "UV Observations of Three LMC Be-Star/X-ray
Binaries"
Schweitzer, A.E., et al. 1995, AJ, 110, p. 2747, "The Absolute Proper Motion and a Membership Survey
of the Sculptor Dwarf Spheroidal Galaxy"
Shaw, M., et al. 1995, MNRAS, 274, p. 369, "Nuclear Bars and Blue Nuclei Within Barred Spiral
Galaxies"
Smette, A., et al. 1996, IAU Symp. 173, ed. C.S. Kochanek, J.N. Hewitt (Kluwer), p. 103, "A Common
High-Column Density LY-" Line in the Spectra of Q 1429-008 A & B"
Smith, E.O., et al. 1996, AJ, 111, p. 1596, "Fomax GlobularClusters 1 and 5: A Confirmed Extragalactic
Second Parameter Pair"
Smith, L.F., Shara, M.M., Moffat, A.F.J. 1996, MNRAS, 281, p. 163, "A Three-Dimensional
Classification for WN Stars"
Smith, V.V., Cunha, K., Lambert, D.L. 1995, AJ, 110, p. 2827, "The Chemical Composition of Omega
Centauri. I. Heavy-Element Abundances of Seven Warm Giants"
Sneden, C, et al. 1995, PASP, 107, p. 997, "Stellar Population and Abundance Studies at High
Resolution with Very Large Telescopes"
Sneden, C, et al. 1996, ASP Conf. 92, ed. H. Morrison, A. Sarajedini (ASP), p. 387, "A Detailed
Analysis of N-Capture Elements in the Ultra-Metal-Poor Halo Giant CS22892-052"
Sneden, C, et al. 1996, ApJ, 467, p. 819, "The Ultra-Metal-Poor, Neutron-Capture-Rich Giant Star CS
22892-052"
Soderblom, D.R., et al. 1996, ApJ, 460, p. 984, "The Age-Related Properties of the HD 98800 System"
Stauffer, J.R., Hartmann, L.W., Barrado y Navascues, D. 1995, ApJ, 454, p. 910, "An Age Estimate for
the $ Pictoris Analog HR 4796A"
Storchi-Bergmann, T., Wilson, A.S., Baldwin, J.A. 1996, ApJ, 460, p. 252, "Nuclear Rings in Active
Galaxies"
Storchi-Bergmann, T., et al. 1996, A&A, 312, p. 357, "Excitation and Temperature of Extended Gas in
Active Galaxies "
Storm, J., et al. 1994, Hot Stars in the Galactic Halo, ed. S.J. Adelman, A.R. Upgren, C.J. Adelman
(Cambridge U. Press), p. 298, "Baade-Wesselink Analyses of Field vs. Cluster RR Lyrae Variables"
Suntzeff, N.B. 1995, PASP, 107, p. 990, "Properties of Echelle Spectrographs: The Transition from 4-m
Telescopes to Very Large Telescopes"
Suntzeff, N.B., Walker, A.R. 1996, PASP, 108, p. 265, "The CTIO Prime-Focus Charge-Coupled Device:
System Characteristics from 1982-1988"
Suntzeff, N.B., Kraft, R.P. 1996, AJ, 111, p. 1913, "The Abundance Spread Among Giants and Subgiants
in the Globular Cluster T Centauri"
Suntzeff, N.B. 1996, IAU Colloquium 145, Supemovae and Supemovae Remnants, ed. R. McCray, Z.
Wang (Cambridge U. Press ), p.41, "Observations of Type la Supemovae"
Szkody, P., et al. 1996, AJ, 111, p. 2379, " IUE and Optical Spectra of AL Comae Berenices During a
Rare Superoutburst"
Taylor, B.J., Joner, M.D. 1996, AJ, 111, p. 1338, "The Cousins VRI System: A Consistency Test of
Equatorial and Southern Standard Stars"
Terndrap, D.M., Sadler, E.M., Rich, R.M. 1995, AJ, 110, p. 1774, "K Giants in Baade's Window. I.
Velocity and Line-Strength Measurements"
Thorstensen, J.R., Vennes, S., Bowyer, S. 1996, ApJ, 457, p. 390, "The 0.8 Day Orbit of the
Precataclysmic Binary EUVE J1016-053"
Van Dyk, S.D., Hamuy, M., Filippenko, A.V. 1996, AJ, 111, p. 2017, "Supemovae and Massive Star
Formation Regions"
Vennes, S., Thorstensen, J.R. 1996, AJ, 112, p. 284 "An Ephemeris for the Pre-Cataclysmic Binary
EuveJ0720-317"
Vrba, F.J., et al. 1995, Ap&SS, 231, p. 85, "An Optical-IR Counterpart for SGR B1900 + 14?"
Vrba, F.J., et al. 1996, ApJ, 468, p. 225, "The Double Infrared Source Toward the Soft Gamma- Ray
Repeater SGR 1900+14"
Wakamatsu, K., et al. 1996, ASP Conf. 91, ed. R. Buta, D.A. Crocker, B.G. Elmegreen (ASP), p. 83, "A
Nuclear Ring in the Sa(r!) Galaxy NGC 7742"
xi
Walker, A.R. 1995, ASP Conf. 83, ed. R.S. Stobie, P.A. Whitelock (ASP), p. 198, "Pulsating Stars and
the Distance Scale -1"
Walker, A.R. 1995, IAU Symp. 167, ed. A.G.D. Philip, K.A. Janes, A.R. Upgren (Kluwer), p. 123, "CCD
Photometry - Present and Future"
Walker, A.R. 1995, IAU Symp. 167, ed. A.G.D. Philip, K.A. Janes, A.R. Upgren (Kluwer), p. 339, "The
NOAO CCD Controller - ARCON"
Wallerstein, G. 1996, PASP, 108, p. 408, "The Spectram of Wakuda's Eraptive Star Near the Time of
Outburst"
Wallin, J.F. 1995, ApJ, 453, p. 641, "AM 1354-250: Photometric Observations and Models of
Collisional Ring System"
a
Walter, F.M., Wolk, S.J., Neuh@user, R. 1996, Nature, 379, p. 233, "Discovery of a Nearby Isolated
Neutron Star"
Wang, L., et al. 1996, ApJ, 466 p. 998, "Hubble Space Telescope Spectroscopic Observations of the
Ejecta of SN 1987A at 2000 Days"
Weiner, B.J., Williams, T.B. 1996, AJ, 111, p. 1156, "Detection of H" Emission from the Magellanic
Stream: Evidence for an Extended Gaseous Galactic Halo"
Williger, G.M., et al. 1996, ApJS, 104, p. 145 "Large-Scale Structure at z ~ 2.5"
Williger, G.M., et al. 1996, ASP Conf. 94, ed. P. Coles, V.J. Martinez, M.J. Pons-Borderia (ASP) p. 183,
"Large-Scale Stracture at z - 2.5"
Xu, J., Crotts, A.P.S., Kunkel, W.E. 1995, ApJ, 451, p. 806, "A Three-Dimensional Study Using Light
Echoes of the Stracture of the Interstellar Medium in Front of SN 1987A"
Zacharias, N„ et al. 1995, AJ, 110, p. 3093, "A Radio-Optical Reference Frame. VHE. CCD Observations
from KPNO and CTIO: Internal Calibration and First Results"
Zinn, R., Bames, S. 1996, AJ, 112, p. 1054, "The Horizontal Branches of Globular Clusters. I. The
Color-Magnitude Diagram of NGC 6426"
xu
Publications by Telescope FY 1996
Blanco 4-m
=
91
1.5-m
=
45
0.9-m
=
42
1-m
=
14
C.Schmidt
=
9
0.6-m
=
8
Staff
=
.25
Total
=
234
These figures include usage of more than one telescope per publication.
Total Publications FY 1996: 194
Xlll
APPENDIX C
Kitt Peak National Observatory
October 1995 to September 1996 Publications List
Abt, H.A. 1995, ApJ, 455, p.407, "Some Statistical Highlights of the Astrophysical Journal"
Abt, H.A. 1996, ASP Conf. 90, ed. E.F. Milone (ASP), p. 15, "Keynote Address: Questions for the
Present and Future"
Abt, H.A., Willmarth, D.W. 1996, ASP Conf. 90, ed. E.F. Milone (ASP), p.105, "Observational Evidence
of Binary Evolution in Open Clusters"
Abt, H.A., Zhou, H. 1996, PASP, 108, p.375, "What Fraction of Astronomers Become Relatively
Inactive in Research after Receiving Tenure?"
Adelman, S.J., Philip, A.G.D. 1996, ASP Conf. 92, ed. H. Morrison (ASP), p.347, "Elemental
Abundances of Eight Field Horizontal-Branch A Stars"
Adelman, S.J., Philip, A.G.D. 1996, MNRAS, 280, p.285, "Elemental Abundances of Field Horizontal
Branch Stars - IV. HD 74721, 86986 and 93329"
Adelman, S.J., Philip, A.G.D. 1996, Baltic Astronomy, 5, p.l 17, "Some Superficially Normal Stars with
Stromgren Photometry Similar to That of Field-Horizontal-Branch Stars"
Ajhar, E.A., et al. 1996, AJ, 111, p.l 110, "Hubble Space Telescope Observations of Globular Clusters in
M31. I. Color-Magnitude Diagrams, Horizontal Branch Metallicity Dependence, and the Distance to
M31"
Albright, G.E., Richards, M.T. 1996, ApJ, 459, p.L99, "Doppler Tomography of Accretion Disks in
Algol Binaries"
Andreon, S., et al. 1996, A&AS, 116, p.429, "Morphological Classification and Stractural Parameters for
Early-Type Galaxies in the Coma Cluster"
Armandroff, T.E., Olszewski, E.W., Pryor, C. 1995, AJ, 110, p.2131, "The Mass-To-Light Ratios of the
Draco and Ursa Minor Dwarf Spheroidal Galaxies. I. Radial Velocities from Multifiber Spectroscopy"
Armandroff, T.E. 1995, ASP Conf. 84, ed. J.M. Chapman (ASP), p.21, "The Use of CCDs on Schmidt
Telescopes"
Baggett, S.M., MacKenty, J.W. 1996, ASP Conf. 91, ed. R. Buta (ASP), p.224, "Box/Peanut Galaxies in
the Near-IR"
Bally, J., et al. 1995, ApJ, 454, p.345, "Twin Herbig-Haro Jets and Molecular Outflows in L1228"
Barden, S.C, Armandroff, T. 1995, SPEE, 2476, p.56, "The Performance of the WIYN Fiber-Fed MOS
System - Hydra"
Barden, S.C. 1995, SPIE, 2476, p.2, "Review of Fiber Optic Properties for Astronomical Spectroscopy"
Barden, S.C, Armandroff T.E., Pryor, CP. 1996, ASP Conf. 90, ed. E.F. Milone (ASP), p.89, "The
Frequency of Binary Stars Near the Tumoff in the Globular Cluster M71"
Barden, S.C. (Editor) 1995, SPEE v.2476: Fiber Optics in Astronomical Applications, ed. S.C. Barden
(SPEE).
Barrado y Navascues, D., Stauffer, J.R. 1996, A&A, 310, p.879, "Lithium Abundance in Binaries of the
Hyades Open Cluster"
Barrientos, L.F., Schade, D., Lopez-Craz, O. 1996, ApJ, 460, p.L89, "Luminosity Evolution in Cluster
Galaxies from z=0.41 to z=0.02"
Baum, W.A., et al. 1995, AJ, 110, p.2537, "Globular Clusters in Coma Galaxy NGC 4881"
Bazan, G., Sneden, C, Yoss, K. 1996, ASP Conf. 92, ed. H. Morrison (ASP), p.351, "High Resolution
Spectroscopy of Metal-Rich Halo Stars"
Beers, T.C., et al. 1996, ApJS, 103, p.433, "A Catalog of Candidate Field Horizontal-Branch and A-Type
Stars. II"
Beers, T.C., et al. 1996, AJ, 112, p.l 188, "Additional Emission-Line Candidates from the HK Survey"
Bell, D.J. 1996, Ph.D. Thesis (University of Illinois at Urbana-Champaign), "A Kinematic and
Abundance Survey in the Galactic Rotational Directions"
Bell, D.J., et al. 1996, ASP Conf. 101, ed. G.H. Jacoby (ASP), p.451, "An Automated System for
Receiving KPNO Proposals by Electronic Mail"
Belton, M.J.S., et al. 1996, Icaras, 120, p.l, "Galileo's Encounter with 243 Ida: An Overview of the
Imaging Experiment"
Belton, M.J.S., et al. 1996, Icaras, 120, p.185, "The Discovery and Orbit of 1993 (243)1 Dactyl"
Bernstein, G.M., et al. 1995, AJ, 110, p.1507, "The Luminosity Function of the Coma Cluster Core for 25 < MR < -9.4"
Bianchi, L., Hutchings, J.B., Massey, P. 1996, AJ, 111, p.2303, "The Winds of Hot Stars in External
Galaxies. III. HST UV Spectroscopy of O and B Supergiants in M31 and M33"
Blanton, E.L., et al. 1995, AJ, 110, p.2868, "Observations of the Type II-P SN 1991G in NGC 4088"
Boroson, T. 1996, ASP Conf. 87, ed. T.A. Boroson (ASP), p. 13, "Queue Scheduling - One Approach
Toward Evaluating Gains and Drawbacks"
Boroson, T. (Editor) 1996, ASP Conf. 87: New Observing Modes for the Next Century, ed. T. Boroson,
J. Davies, I. Robson (ASP).
ii
Borra, E.F., et al. 1996, AJ, 111, p.1456, "Spectroscopy of Quasar Candidates Found with Slitless
Spectroscopy. II. Six Northern Fields"
Bragaglia, A., et al. 1996, ASP Conf. 92, ed. H. Morrison (ASP), p.175, "Definition of a Pure Sample of
Nearby GHB Stars"
Brooke, T.Y., Sellgren, K., Smith, R.G 1996, ApJ, 459, p.209, "A Study of Absorption Features in the 3
Micron Spectra of Molecular Cloud Sources with H2 Ice Bands"
Burstein, D., Willick, J.A., Courteau, S. 1995, The Opacity of Spiral Disks, ed. J.I. Davies (Kluwer),
p.73, "Inclination-Dependence of Spiral Galaxy Physical Properties: History and Tests"
Byun, Y-L, et al. 1996, AJ, 111, p.1889, "The Centers of Early-Type Galaxies with HST. n. Empirical
Models and Stractural Parameters"
Callanan, P.J., et al. 1996, ApJ, 461, p.351, "Observations of GRO J0422+32. UI. A Low-Inclination
Black Hole X-Ray Nova"
Calzetti, D., et al. 1995, AJ, 110, p.2739, "An Atlas of Ha Emitting Regions in M33: A Systematic
Search for SS433 Star Candidates"
Calzetti, D., Kinney, A.L., Storchi-Bergmann, T. 1996, ApJ, 458, p.132, "Dust Obscuration in Starburst
Galaxies from Near-Infrared Spectroscopy"
Calzetti, D. 1996, RevMexAA, Serie de Conferencias 3, p.173, "Dust in Starburst Galaxies: Insights from
Near-Infrared Spectroscopy"
Campbell, J.M., et al. 1995, ApJS, 101, p.237, "Infrared Absorption and Emission Spectra of SiO"
Cecil, G., Morse, J.A., Veilleux, S. 1995, ApJ, 452, p.613, "Spectral Evidence for Shock-Ionized Gas
Along the Jets of NGC 4258"
Chaboyer, B., Demarque, P., Sarajedini, A. 1996, ApJ, 459, p.558, "Globular Cluster Ages and the
Formation of the Galactic Halo"
Chapman, C.R., et al. 1996, Icaras, 120, p.231, "Cratering on Gaspra"
Chariot, S., Worthey, G., Bressan, A. 1996, ApJ, 457, p.625, "Uncertainties in the Modeling of Old
Stellar Populations"
Chariot, S. 1996, ASP Conf. 98, ed. C. Leitherer (ASP), p.275, "Comparison of Models of Young/StarForming Galaxies"
Ciardullo, R., Bond, H.E. 1996, AJ, 111, p.2332, "A Survey for Pulsations in O VI Nuclei of Planetary
Nebulae"
Claria, J.J., Piatti, A.E., Osbom, W. 1996, PASP, 108, p.672, "DDO Metal Abundances of HighLuminosity Late-Type Stars in Galactic Open Clusters"
iii
Colless, M., Dunn, A.M. 1996, ApJ, 458, p.435, "Structure and Dynamics of the Coma Cluster"
Connolly, A.J., et al. 1995, AJ, 110, p.2655, "Slicing Through Multicolor Space: Galaxy Redshifts from
Broadband Photometry"
Cote, P., Fischer, P. 1996, AJ, 112, p.565, "Spectroscopic Binaries in Globular Clusters. I. A Search for
Ultra-Hard Binaries on the Main Sequence in M4"
Cote, P., et al. 1996, AJ, 112, p.574, "Spectroscopic Binaries in Globular Clusters. H. A Search for LongPeriod Binaries in M22"
Courteau, S., Holtzman, J. 1995, The Opacity of Spiral Disks, ed. J.I. Davies (Kluwer), p.211, "Color
Gradients in Spiral Disks"
Courteau, S., de Jong, R.S., Broeils, A.H. 1996, ApJ, 457, p.L73, "Evidence for Secular Evolution in
Late-Type Spirals"
Courteau, S. 1996, ApJS, 103, p.363, "Deep r-Band Photometry for Northern Spiral Galaxies"
Cowan, J.J., et al. 1996, ApJ, 460, p.L115, "First Detection of Platinum, Osmium, and Lead in a MetalPoor Halo Star: HD 126238"
Craig, N.,et al. 1996, IAU Colloq. 152, ed. S. Bowyer (Kluwer), p.491, "The EUVE Optical
Identification Campaign II: Late-Type and White Dwarf Stars"
Crawford, D.L., Craine, E. 1996, ASP Conf. 89, ed. J.R. Percy (ASP), p.183, "GNAT: A Global Network
of Small Astronomical Telescopes"
Crawford, D.L. 1996, Baltic Astronomy, 5, p.247, "Philosophy of Standard Stars as Tools in
Astronomical Photometry"
Crawford, D.L., Craine, E. 1996, Baltic Astronomy, 5, p.255, "A Global Network of Small Telescopes as
a Resource for Photometry"
Crawford, D.L. 1996, Baltic Astronomy, 5, p.263, "Light Pollution: The Problem and the Potential
Solutions"
Currie, D.G., et al. 1996, AJ, 112, p.l 115, "Astrometric Analysis of the Homunculus of t| Carinae with
the Hubble Space Telescope"
da Costa, L.N., et al. 1996, ApJ, 468, p.L5, "The Mass Distribution in the Nearby Universe"
Davies, M.E., et al. 1996, Icaras, 120, p.33, "The Direction of the North Pole and the Control Network of
Asteroid 243 Ida"
De Young, D.S., Charles, R.D. 1995, AJ, 110, p.3107, "Numerical Simulation of Airflow Over Potential
Telescope Sites"
IV
De Young, D.S. 1996, ASP Conf. 100, ed. P.E. Hardee (ASP), p.261, "Boundary Layer Development,
Entrainment, and Energy Transport in Radio Sources"
Dempsey, R.C, et al. 1996, AJ, 111, p.1356, "Multiwavelength Observations of Two Moderate Rotation
RS CVn Systems: V815 Herculis and IM Pegasi"
Dobrzycka, D., et al. 1996, AJ, 111, p.2090, "The Hot Component of RS Ophiuchi"
Duncan, D.K., Rebull, L.M. 1996, PASP, 108, p.738, "Lithium in Young Solar-Type Stars in the Orion
Nebula Region"
Dunlop, J., et al. 1996, Nature, 381, p.581, "A 3-5-Gyr-Old Galaxy at Redshift 1.55"
Durrell, P.R., et al. 1996, AJ, 112, p.972, "Globular Cluster Systems in Dwarf Elliptical Galaxies. B. The
Virgo Cluster"
Dyck, H.M., et al. 1996, AJ, 111, p.1705, "Radii and Effective Temperatures for K and M Giants and
Supergiants"
Elmegreen, D.M., Chromey, F.R., Johnson, CO. 1995, AJ, 110, p.2102, "Near-Infrared Observations of a
Central Bar in M81"
Elmegreen, D.M., et al. 1996, AJ, 111, p.1880, "Near-Infrared Observations of Isophotal Twists in
Barred Spiral Galaxies"
Elmegreen, D.M., et al. 1996, ApJ, 469, p. 131, "Star Formation in the Outer Resonance Ring of NGC
1300"
Feibelman, W.A., et al. 1995, PASP, 107, p.914, "Variability of EUE Spectra of the Pulsating Nucleus of
the Planetary Nebula K 1-16"
Fekel, F,C 1996, AJ, 112, p.269, "Chromospherically Active Stars. XV. HD 8357=AR Piscium, an
Extremely Active RS CVn System"
Fekel, F.C., et al. 1996, ApJ, 462, p.L95, "HDE 233517: Lithium and Excess Infrared Emission in Giant
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Silva, D.R. 1996, Spiral Galaxies in the Near-ER, ed. D. Minniti (Springer), p.3, "When Do Near-ER
Colors Help in Studying Stellar Populations"
Simonelli, D.P., et al. 1996, Icaras, 120, p.38, "Ida Lightcurves: Consistency with Galileo Shape and
Photometric Models"
Simpson, C, et al. 1996, ApJ, 457, p.L19, "An Ionization Cone and Dusty Disk in Markarian 348: The
Obscuring Torus Revealed?"
Smith, D.A., et al. 1996, ApJS, 104, p.217, "Starburst Galaxies. B. Imaging and Spectroscopy of a RadioSelected Sample"
Sneden, C, et al. 1996, ApJ, 467, p.819, "The Ultra-Metal-Poor, Neutron-Capture-Rich Giant Star CS
22892-052"
Soffner, T., et al. 1996, A&A, 306, p.9, "Planetary Nebulae and HII Regions in NGC 300"
Stepanian, J.A., et al. 1996, A&A, 309, p.702, "SBS 1425+606: A Bright, High-Redshift QSO.
Illuminating a Damped Lya Absorber"
Straizys, V., Crawford, D.L., Philip, A.G.D. 1996, Baltic Astronomy, 5, p.83, "The Stromvil System: An
Effective Combination of Two Medium-Band Photometric Systems"
Sullivan, R., et al. 1996, Icaras, 120, p. 119, "Geology of 243 Ida"
Szomoru, A., van Gorkom, J.H., Gregg, M.D. 1996, AJ, 111, p.2141, "An H I Survey of the Bootes Void.
I. The Data."
Szomoru, A., et al. 1996, AJ, 111, p.2150, "An H I Survey of the Bootes Void. II. The Analysis"
Thomas, P.C, et al. 1996, Icaras, 120, p.20, "The Shape of Ida"
Thorbum, J.A., Hobbs, L.M. 1996, AJ, 111, p.2106, "Beryllium Abundances of Six Halo Stars"
Thomley, M.D. 1996, ApJ, 469, p.L45, "Uncovering Spiral Stracture in Flocculent Galaxies"
Tolstoy, E., et al. 1995, AJ, 110, p. 1640, "Variable Stars in the Irregular Galaxy NGC 2366 (DDO 42)"
xv
Tolstoy, E. 1995, Ph.D. Thesis (Rijksuniversiteit Groningen), "Modelling the Resolved Stellar
Populations of Nearby Dwarf Galaxies"
Tolstoy, E. 1996, ApJ, 462, p.684, "The Resolved Stellar Population of Leo A"
Tripp, T.M., Lu, L., Savage, B.D. 1996, ApJS, 102, p.239, "High Signal-to-Noise Echelle Spectroscopy
of Quasar Absorption-Line Systems in the Direction of HS 1946+7658"
Usher, P.D., Mitchell, K.J., Huang, K.-L. 1995, ApJ, 454, p.654, "Faint Blue Objects at High Galactic
Latitude. VB. Spectroscopy of Narrow-Line Objects and the Morphological Selection Criterion of the US
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Van de Steene, G.C, Jacoby, G.H., Pottasch, S.R. 1996, A&AS, 118, p.243, "Optical Observations of
Planetary Nebula Candidates from the Northern Hemisphere"
Van de Steene, G.C, Jacoby, G.H. 1996, ASP Conf. 102, ed. R. Gredel (ASP), p.299, "Spectroscopy of
New Planetary Nebulae Close to the Galactic Center"
van Dokkum, P.G., Franx, M. 1996, MNRAS, 281, p.985, "The Fundamental Plane in CL 0024 at z=0.4:
Implications for the Evolution of the Mass-to-Light Ratio"
Veilleux, S., Cecil, G., Bland-Hawthorn, J. 1996, Sci. Am., 274, no.2, p.98, "Colossal Galactic
Explosions"
Vennes, S., Thorstensen, J.R. 1995, White Dwarfs, ed. D. Koester (Springer), p.313, "White Dwarfs in
Close Binaries in the Extreme Ultraviolet Explorer All-Sky Survey"
Veverka, J., et al. 1996, Icarus, 120, p.66, "Ida and Dactyl: Spectral Reflectance and Color Variations"
Veverka, J., et al. 1996, Icaras, 120, p.200, "Dactyl: Galileo Observations of Ida's Satellite"
Vrba, F.J., et al. 1995, Ap&SS, 231, p.85, "An Optical-IR Counterpart for SGR B1900+14?"
Vrba, F.J., et al. 1996, ApJ, 468, p.225, "The Double Infrared Source Toward the Soft Gamma-Ray
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Wallace, L., Hinkle, K. 1996, ApJS, 103, p.235, "An Infrared Spectral Atlas of Arcturas for the Range
10750-11500 cm"1 (8690-9300 A)"
Wallace, L., et al. 1996, APJS, 106, p.165, "Infrared Spectral Atlases of the Sun from NOAO"
Weintraub, D.A., Kastner, J.H., Whitney, B.A. 1995, ApJ, 452, p.L141, "In Search of HL Tauri"
Weintraub, D.A., et al. 1996, ApJ, 468, p.L45, "Diffraction-Limited 3.8 Micron Imaging of Protostellar
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White B, J.C, Schlegel, E.M., Honeycutt, R.K. 1996, ApJ, 456, p.777, "BT Monocerotis: Another
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xvi
Willick, J.A., et al. 1996, ApJ, 457, p.460, "Homogeneous Velocity-Distance Data for Peculiar Velocity
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Willmer, C.N.A., et al. 1996, ApJS, 104, p. 199, "A Medium Survey of a Minislice at the North Galactic
Pole. II. The Data"
Wise, M.W., Silva, D.R. 1996, ApJ, 461, p.155, "The Effects of Dust on Broadband Color Gradients in
Elliptical Galaxies"
Wolk, S.J., Walter, F.M. 1996, AJ, 111, p.2066, "A Search for Protoplanetary Disks Around Naked T
Tauri Stars"
Woolf, V.M., Tomkin, J., Lambert, D.L. 1995, ApJ, 453, p.660, "The r-Process Element Europium in
Galactic Disk F and G Dwarf Stars"
Yang, H., et al. 1996, AJ, 112, p. 146, "The Violent Interstellar Medium of NGC 604"
Zacharias, N., et al. 1995, AJ, 110, p.3093, "A Radio-Optical Reference Frame. VBI. CCD Observations
from KPNO and CTIO: Internal Calibration and First Results"
xvn
APPENDIX D
National Solar Observatory
October 1995 to September 1996 Publications List
Altrock, R.C, Henry, T.W. 1996, Solar-Geophysical Data, Part 1, Prompt Reports 607, ed. H.E. Coffey,
"Sacramento Peak Coronal Line Synoptic Maps, 1995"
Altrock, R.C, Henry, T.W. 1996, Solar-Geophysical Data, Part 1, Prompt Reports 607, ed. H. E. Coffey,
"Coronal Line Emission (Sacramento Peak), 1995"
Altrock, R.C, Henry, T.W. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N.
Smartt, (ASP), p.324, "Prediction of Coronal-Hole Solar Wind Velocities at Ulysses from NSO/SP
Coronal Data"
Andretta, V., Giampapa, M.S., Jones, H.P. 1995, Irish Astronomical Journal, 22, p. 177, "Helium in the
Spectram of the Sun and of Solar-Type Stars"
Aschwanden, M.J., et al. 1995, ApJ, 454, p.512, "Solar Rotation Stereoscopy in Microwaves"
Balasubramaniam, K.S., Keil, S.L. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil,
R.N. Smartt, (ASP), p. 189, "A Search for Large-Scale Photospheric Flows as Drivers of Mass Ejections"
Balasubramaniam, K.S., Keil, S.L., Smartt, R.N. eds. 1996, ASP Conference 95, 628 pp.
Balasubramaniam, K.S., Keil, S.L., Smartt, R.N. 1996, ASP Conference 95., viii-x, "Solar
Drivers of Interplanetary and Terrestrial Disturbances: Preface"
Beck, J.G., Hathaway, D.H., Simon, G.W. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L.
Keil, R.N. Smartt, (ASP), p.196, "Observing Large-Scale Solar Surface Flows with GONG: Investigation
of a Key Element in Solar Activity Buildup"
Beck. J.G., Hill, F., Ulrich, R.K. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema,
(ESA), Vol. 2, p.401, "A Study of the Background Solar Velocity Spectram Using GONG Data"
Benner, D.C., et al. 1995, J. Quan. Spectr. Rad. Trans., 173, p.705, "A Multispectram Nonlinear Least
Squares Fitting Technique"
Berger, T.E., et al. 1995, ApJ, 454, p.531, "New Observations of Subarcsecond Photospheric Bright
Points"
Bemasconi, P.N., et al. 1995, A&A, 302, p.533, "Direct Measurements of Flux Tube Inclinations in Solar
Plages"
Bocchialini, K., Koutchmy, S. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA),
Vol. 2, p.499, "Chromospheric Oscillations from Simultaneous Sequences of He I 1093 and Ca B K
393.4 Spectroscopic Measurements"
Bogart, R.S., et al. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 2,
p.147, "Plane-WaveAnalysis of Solar Acoustic-Gravity Waves: a (Slightly) New Approach"
Bogart, R.S., et al. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 2,
p.151, "Preliminary Results from Plane-Wave Analysis of Helioseismic Data"
Bogdan, T.J., Braun, D.C. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA) Vol.
2, p.31, "Active Region Seismology"
Brajsa, R., et al. 1996, Solar Phys., 163, p.79, "Helium 10830 A Measurements of the Sun"
Braun, D.C. 1995, ApJ, 451, p.859, "Scattering of p-Modes by Sunspots. I. Observations"
Brynildsen, N., Kjeldseth-Moe, O., Maltby, P. 1996, ApJ, 462, p.534, "Quiet-Sun Connection Between
the C iv Resonance Lines and the Photospheric Magnetic Field"
Chang, E.S., Deming, D. 1996, Solar Phys., 165, p.257, "Observation of Infrared Lines in a Prominence
at 1-5 Microns"
Christensen-Dalsgaard, J., et al. 1996, Science, 272, p.1286, "The Current State of Solar Modeling"
Cliver, E.W., et al. 1995, 24th International Cosmic Ray Conference, Vol. 4 (International Union of Pure
and Applied Physics), p.257, "Extreme Propagation of Solar Energetic Particles"
Coulter, R., Kuhn, J.R., Rimmele, T. 1996, Solar Phys., 163, p.7, "Using Scintillation Measurements to
Achieve High Spatial Resolution in Photometric Solar Observations"
D'Silva, S. 1996, ApJ, 462, p.519, "Measuring the Solar Internal Rotation Using Time-Distance
Helioseismology: I. The Forward Approach"
Dupree, A., Penn, M.J., Jones, H.P. 1996, ApJ, 467, L121, "He I 10830 A Wing Asymmetry in Polar
Coronal Holes: Evidence for Radial Outflows"
Duvall, T.L. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 1, p.107,
"Other Groundbased Observations"
Duvall, T.L., et al. 1996, Nature, 379, p.235, "Downflows Under Sunspots Detected by Helioseismic
Tomography"
Esser, R„ et al. 1995, J. Geophys. Res., 100, p.19829, "Using Fe X 6374 A and Fe XEV 5303 A Spectral
Line Intensities to Study the Effect of Line of Sight Integration on Coronal Temperature Inferences"
Fan, Y., Braun, D.C, Chou, D.Y. 1995, ApJ, 451, p.877, "Scattering of p-Modes by Sunspots. B.
Calculations of Phase Shifts from a Phenomenological Model"
Fan, Y., Fisher, G.H. 1996, Solar Phys., 166, p.17, "Radiative Heating and the Buoyant Rise of Magnetic
Flux Tubes in the Solar Interior"
Fisher, G.H., et al. 1996, IAU 153, eds. Y. Uchida, T. Kosugi, H. S. Hudson, (Kluwer), "The Dynamics
of Magnetic Flux Tubes in the Solar Convection Zone — a Study of Active Region Formation"
Frohlich, C, et al. 1995, Solar Phys., 162, p.101, "Virgo: Experiment for Helioseismology and Solar
Irradiance Monitoring"
Giampapa, M.S., Craine, E.R., Hott, A. 1995, Icaras, 118, p.199, "Comments on the Photometric Method
for the Detection of Extrasolar Planets"
Giampapa, M.S., et al. 1995, ApJ, 463, p.707, "The Coronae of Low Mass Dwarf Stars"
Giampapa, M.S., Craine, E.R. 1995, Icarus, 118, p. 199, "The Photometric Method for the
Detection of Extrasolar Planets"
Giver, L.P., et al. 1996, J. Mol. Spectr., 175, p.104, "The Rovibrational Intensities of the (40°1) <- (00°0)
Pentad Absorption Bands of !2C1602 Between 7284 and 7921 cm"1"
Gough, D., et al. 1996, Science, 272, p.1281, "Perspectives in Helioseismology"
Gough, D., et al. 1996, Science, 272, p.1296, "The Seismic Stracture of the Sun"
Gu, Y. 1995, Chinese Science, 46, no. 6, "The Sun Never Sets: an Introduction to the Global Oscillation
Network Group"
Guelachvili, G., et al. 1996, Spectrochimica Acta, 52A, p.717, "High-Resolution Wave-Number
Standards for the Infrared"
Haber, D.A., et al. 1995, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), p.141, "Local Area
Analysis of High-Degree Solar Oscillations: New Ring Fitting Procedures"
Hanaoka, Y. 1996, Solar Phys., 165, p.275, "Flares and Plasma Flow Caused by Interacting Coronal
Loops"
Harvey, J.W. 1995, Phys. Today, 43, p.32, "Helioseismology"
Harvey, J.W. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 1, p.9,
"Helioseismology: the State of the Art"
Harvey, J.W., et al. 1996, Science, 272, p.1284, "The Global Oscillation Network Group (GONG)
Project"
Harvey, K.L., et al. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N. Smartt,
(ASP), Vol. 2, p.100, "Comparison and Relation of He I 1083 nm Two-Ribbon Flares and Large-Scale
Coronal Arcades Observed by Yohkoh"
Hathaway, D., et al. 1996, Science, 272, p.1306, "GONG Observations of Solar Surface Flows"
Hathaway, D.H. 1996, ApJ, 460, p.1027, "Doppler Measurements of the Sun's Meridional Flow"
iii
Hick, P., et al. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S. L. Keil, R.N. Smartt, (ASP),
p.358, "The Coronal Temperature Stracture and the Current Sheet"
Hill, F. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 1, p.127,
"Resolution and Error Trade-Offs in Velocity Fields Inferred from Ring Diagrams"
Hill, F. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 1, p.63, "Local
Probes of the Solar Interior"
Hill, F., et al. 1996, Science, 272, p. 1292, "The Solar Acoustic Spectram and Eigenmode Parameters"
Hofmann, J., Deubner, F.L. 1995, A&AS,113, p.583, "The Effect of Limited Spatial Resolution on the
Observed Power of Solar Oscillations"
Hofmann, J., et al. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2, p.493,
"Phase Analysis of the K-Grain Excitation Pattern"
Hofmann, J., Steffens, S., Deubner, F.L. 1996, A&A, 308, p. 192, "K-Grains as a Three-Dimensional
Phenomenon. II. Phase Analysis of the Spatio-Temporal Pattern"
Howard, R.F. 1996, Solar Phys., 167, p.95, "Tilt-Angle Variations of Active Regions"
Howard, R.F. 1996, Ann. Rev. Astron. Astrophys., 34, p. 75, "Solar Active Regions as
Diagnostics of Subsurface Conditions"
Jones, H.P. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema, (ESA), Vol. 2, p.227,
"Tracking Magnetogram Proper Motions by Multiscale Regularization"
Kankelborg, C.C., et al. 1996, ApJ, 466, p.529, "Observation and Modeling of Soft X-Ray Bright Points.
I. Initial Results"
Kariyappa, R. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2, p.525,
"The Relation Between the Period of Oscillations and Brightness in Chromospheric Bright Points"
Kariyappa, R. 1996, Solar Phys., 165, p.211, "Solar Oscillations in Strong and Weak Fraunhofer Lines
Over a Quiet Region"
Kariyappa, R., Pap, J.M. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2,
p.521, "Intensity Oscillations in Nal Dl and D2 Lines"
Kariyappa, R., Pap, J.M. 1996, Solar Phys., 167, p.115, "Contribution of Chromospheric Features to UV
Irradiance Variability from Spatially-Resolved Ca B K Spectroheliograms. I. A New Method of Analysis
and Preliminary Results"
Kariyappa, R., et al. 1995, ESA SP 376, Fourth SOHO Workshop, et al. J.T. Hoeksema (ESA), Vol. 2,
p.429, "Preliminary Results of the Analysis of Ca II K Spectroheliograms"
Keil, S.L., et al. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N. Smartt (ASP),
p.158, "The Solar Mass Ejection Imager (SMEI): Development and Use in Space Weather Forecasting"
iv
Keller, CU. 1996, Solar Phys., 164, p.243, "Recent Progress in Imaging Polarimetry"
Keller, C.U., Smartt, R.N. 1996, Solar Phys, 166, p.311, "Imaging Coronal Emission Lines Under High
Sky-Background Conditions"
Kononovich, E.V., et al. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N. Smartt
(ASP), p.251, "Two-Dimensional Model of a Rotating Solar Prominence. I. Observations and
Preliminary Approach"
Kuhn, J.R. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 1, p. 145, "Solar
Variability in Irradiance and Oscillations"
Kuhn, J.R., Penn, M.J., Mann, I. 1995, ApJ, 456, p.L67, "The Near Infrared Coronal Spectrum"
Kuhn, J.R., Stein, R.F. 1996, ApJ, 463, p.L117, "Accounting for the Solar Acoustic and Luminosity
Variations from the Deep Convection Zone"
Lantos, P., Alissandrakis, CE. 1996, Solar Phys., 165, p.83, "Coronal Sources at Meter and Optical
Wavelengths During the Declining Phase of the Solar Cycle"
Latushko, S. 1996, Solar Phys., 163, p.241, "Meridional Drift of the Large-Scale Solar Magnetic Fields
in Different Phases of Solar Activity"
Latushko, S. 1996, Solar Phys., 166, p.261, "Rotation of the Large-Scale Solar Magnetic Fields in the
Equatorial Region"
Learner, R.C, et al. 1995, J. Opt. Soc. Am. A, 12, p.2165, "Phase Correction of Emission Line Fourier
Transform Spectra"
Leibacher, J.W. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2, p.401,
"A Study of the Background Solar Velocity Spectram Using GONG Data"
Linsky, J., et al. 1995, ApJ, 455, p.670, "Stellar Activity at the End of the Main Sequence: GHRS
Observations of the M8 Ve Star VB 10"
Lites, B.W. 1996, Solar Phys., 163, p.223, "Performance Characteristics of the Advanced Stokes
Polarimeter"
Lites, B.W., et al. 1996, ApJ, 460, p. 1019, "Small-Scale Horizontal Magnetic Fields in the Solar
Photosphere"
Livingston, W.C, Ban, L. 1996, Mirror Substrate Alternatives Workshop, eds. J.P. Rozelot and
W.C. Livingston, p. 121, "McMath-Pierce Upgrade: Achieving Stealth Optics to Yield a
Thermally Invisible Telescope"
Lorrain, P., Koutchmy, S. 1996, Solar Phys., 165, p.l 15, "Two Dynamical Models for Solar Spicules"
Lynch, D.K., Livingston, W.C, 1995, Color and Light in Nature, (Cambridge U. Press)
v
Marquez, I., et al. 1996, A&A, 305, p.316, "Numerical Modeling of Spectral Line Asymmetries in
Photospheric Stractures. I. Quiet Sun"
Montague, M., Muller, R„ Vigneau, J. 1996, A&A, 311, p.304, "The Photosphere of the Sun: Statistical
Correlations Between Magnetic Field, Intensity and Velocity"
Nesme-Ribes, E., Meunier, N., Collin, B. 1996, A&A, 308, p.213, "Fractal Analysis of Magnetic Patterns
from Meudon Spectroheliograms"
November, L.J. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N. Smartt (ASP),
p.375, "Dark-Thread Thermodynamics and the Coronal Temperature Structure"
November, L.J., Koutchmy, S. 1996, ApJ, 466, p.512, "White-Light Coronal Dark Threads and Density
Fine Stracture"
O'Neal, D., Saar, S.H., Neff, J.E. 1996, ApJ, 463, p.766, "Measurements of Starspot Area and
Temperature on Five Active, Evolved Stars"
Orton, G., et al. Science, 272, p.839, "Earth-Based Observations of the Galileo Probe Entry Site"
Pap, J.M., Vigouroux, A., Delache, P. 1996, Solar Phys., 167, 125, "Study of the Distribution of Daily
Fluctuations in Observed Solar Irradiances and Other Full-Disk Indices of Solar Activity"
Patron, J., et al. 1995, ApJ, 455, p.746, "Velocity Fields Within the Solar Convection Zone: Evidence
from Oscillation Ring Diagram Analysis of Mt. Wilson Dopplergrams"
Paxman, R.G., et al. 1996, ApJ, 466, p.1087, "Evaluation of Phase-Diversity Techniques for Solar-Image
Restoration"
Penn, M.J., Jones, H.P. 1996, Solar Phys. 168, p. 19, "Limb Observations of He I 1083 nm"
Radick, R.R., et al. 1995, ApJ, 452, p.332, "A Twelve Year Photometric Study of Lower Main-Sequence
Hyades Stars"
Radziemski, L.J., Engleman, Jr., R., Brault, J.W. 1995, Phys. Rev. A, 52, p.4462, "FTS Measurements in
the Spectra of Neutral Lithium, 6Li I and7Li I"
Ram, R.S., Bemath, P.F. 1996, J. Chem. Phys., 104, p.6444, "Fourier Transform Emission Spectroscopy
of New Infrared Systems of LaH and LaD"
Ram, R.S., Bemath, P.F., Davis, S.P. 1996, J. Chem. Phys., 104, p.6949, "The Low-Lying Electronic
States of CoF"
Ram, R.S., Bemath, P.F., Davis, S.P. 1996, J. Mol. Spectr., 175, p.l, "Fourier Transform Emission
Spectroscopy of the A3 <b - X3 <(> System of CoH"
Ram, R.S., et al. 1996, ApJS, 103, p.247, "Infrared Spectra of Hot HF and DF"
vi
Rieger, E., et al. 1996, Solar Phys., 167, p.307, "The Role of High-Energy Protons and Electrons in
Powering the Solar White Light Flare Emission"
Rimmele, T.R., et al. ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2, p.329,
"Dark Lanes in Granulation and the Excitation of Solar Oscillations"
Rimmele, T.R., Radick, R.R. 1996, Adaptive Optics Workshop, OSA Technical Digest Series 13
(Optical Society of America), p.247, "Experimental Comparison of Two Approaches for Solar
Wavefront Sensing"
Rozelot, J.P., Livingston, W.C, eds. 1996, Mirror Substrate Alternatives Workshop, pp.238
Riiedi, I., Keller, C.U., Solanki, S.K. 1996, Solar Phys., 164, p.265, "Measurement of the Full Stokes
Vector of He I 10830 A"
Riiedi, I., Solanki, S.K., Livingston, W.C. 1995, A&A, 302, p.543, "Infrared Lines as Probes of Solar
Magnetic Features. XI. Stracture of a Sunspot Umbra with a Light Bridge"
Rust, D.M., et al. 1996, Solar Phys., 164, p.403, "Balloon-Borne Polarimetry: the Flare Genesis
Experiment"
Schmieder, B., et al. 1996, ApJ, 467, p.881, "Differential Magnetic Field Shear in an Active Region"
Schrijver, C.J., et al. 1996, ApJ, 468, p. 921, "Dynamics of the Chromospheric Network:
Mobility, Dispersal, and Diffusion Coefficients"
Seiden, P.E., Wentzel, D.G. 1996, ApJ, "Solar Active Regions as a Percolation Phenomenon. II."
Shcherbakov, A.G., et al. 1996, A&A, 309, p.655, "He I A.10830 A Line as an Indicator of Solar
Chromospheric Activity"
Sheeley, N.R. 1996, ApJ, 469, p. 423, "Elemental Abundance Variations in the Solar
Atmosphere"
Simon, G.W., et al. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T. Hoeksema (ESA), Vol. 2,
p.223, " Warning: Local Correlation Tracking May Be Dangerous to Your (Scientific) Health"
Simon, G.W., Jones, H.P., Hurlburt, N.E. 1995, ESA SP 376, Fourth SOHO Workshop, ed. J.T.
Hoeksema (ESA), Vol. 1, p.205, "Surface Flows and Feature Tracking: MDI/GONG Joint Working
Group Report"
Smartt, R.N. 1996, Australian Optical Society News vol. 10, no. 2, p.27, "Development of NewTechnology Coronagraphs"
Smartt, R.N. 1996, MacMillan Encyclopedia of Earth Sciences, vol. 2, p. 1052, "Sun"
Smartt, R.N., et al. 1996, ASP Conference 95, eds. K.S. Balasubramaniam, S.L. Keil, R.N. Smartt (ASP),
p.531, "White-Light Reflecting Coronagraph for the SWATH Mission"
vii
Smartt, R.N., et al. 1996, Mirror Substrate Alternatives Workshop, eds. J. Rozelot and W.C.
Livingston, p. 127, "Application of New-Technology Objective Mirrors in Reflecting
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