LADIES AND GENTLEMEN: We enclose acopy of the CT^O/KPNO ... Long Range Plan FY 198… · The 4...

KITT PEAK NATIONAL OBSERVATORY

Operated by The

ASSOCIATION OF UNIVERSITIES FOR RESEARCH IN ASTRONOMY, INC.Under Contract With The

National Science Foundation

Member Institutions:UNIVERSITY OF ARIZONA

CALIFORNIA INSTITUTE OF TECHNOLOCY

UNIVERSITY OF CALIFORNIA

UNIVERSITY OF CHICAGO

UNIVERSITY OF COLORADO IN BOULDER

HARVARD UNIVERSITY

UNIVERSITY OF HAWAII

UNIVERSITY OF ILLINOIS

INDIANA UNIVERSITY

MASSACHUSETTS INSTITUTE OF TECHNOLOGY

UNIVERSITY OF MICHIGAN

OHIO STATE UNIVERSITY

PRINCETON UNIVERSITY

UNIVERSITY OF TEXAS AT AUSTIN

UNIVERSITY OF WISCONSIN

YALE UNIVERSITY

12 October 1983

LADIES AND GENTLEMEN:

We enclose a copy of the CTÔ/KPNO Long Range Plarj coveringthe period FY-1985-89 which is bein£ formally submitted tothe National Science Foundation by tTh€t^Corporate_ Office thisweek.

With best wishes.

GB/fed

Enclosure

Yours sincerely,

Geoffrey BurbidgeDirector

RECEIVEDNOAO

OCT 14 1983

DIRECTOR'S OFFICE

950 North Cherry Avenue

P.O. Box 26732

Tucson, Arizona 85726

AC 602 327-5511

Cable: AURACORP, Tucson

Telex: 666-484 AURA KPNO TUC

JOINT

CERRO TOLOLO INTER-AMERICAN OBSERVATORY

AND

KITT PEAK NATIONAL OBSERVATORY

LONG RANGE PLAN

FY-85 THROUGH FY-89

CONTENTS

I. LNTRODUCT ION I- 1

II. THE SCIENTIFIC FORECAST II- 1

III. THE PLAN Ill- 1

Observatory Operations Ill- 1

Scientific Staff HI- 8

Telescopes , Instruments And Computers 111-10

Research and Development 111-30

IV . NEW LARGE APERTURE TELESCOPE AT CTIO IV- 1

V. 15 METER NATIONAL NEW TECHNOLOGY TELESCOPE (NNTT) V- 1

I. INTRODUCTION

The Kitt Peak National Observatory and the Cerro Tololo Inter-American

Observatory are together responsible for filling a large part of the national

need of U. S. astronomers for optical and infrared observing facilities. The

Observatories' facilities comprise 7 telescopes on Cerro Tololo and 9 night

time telescopes on Kitt Peak. The 4 meter telescopes at both Observatories

are their most important instruments for night-time astronomy, and they are

used for a wide variety of observations at the very limit of the technology in

optical astronomy. This long-range plan will outline what is needed over the

next five years to maintain and improve these facilities. It will also

describe the new projects which are essential to the vitality of U. S.

astronomy.

The planning basis for normal operations is that the Observatories will

continue to operate at their current levels of effort. Note that these levels

have improved in relation to those of the last long range plan when the

Observatories were at their lowest point after the cutbacks of previous years

and were not able to operate all their existing equipment, let alone undertake

major new projects. At present, as a result of the improved funding for FY-

84, lowered world inflation, and a more favorable exchange rate in Chile, the

Observatories have been able to rebuild to the point that they can reopen and

support most of their previously closed facilities. Consequently, for their

long range planning, the Observatories are assuming the future availability of

staff and resources for the operation of the existing telescopes and

improvement of their auxiliary instrumentation. In addition, both

Observatories are planning major new projects, the 3-5 meter class telescope

at CTIO and the National New Technology Telescope (NNTT) at KPNO, to meet the

needs of their user community and to make the first major increase in

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telescope size since the completion of the Hale 5 meter telescope. Such

projects, of course, will require special funding, well in excess of the

normal operating budgets .

During the planning period KPNO intends to improve existing telescopes

and laboratory facilities and to continue the development of new

instrumentation. Telescope improvements include the installation of automatic

guiders, TV acquisition systems, computer control of pointing, finding and

instruments, automatic dome control, and console room observing at all

nighttime telescopes except the #4-0.4-meter and the Burrell-Schmidt . Effort

in the area of instrumentation will include the development of photon counting

detector systems, intensified CCDs and especially infrared arrays. Resources

will also be directed toward the development and improvement of existing

instrumentation. Improvements to the gratings laboratory and increased effort

in coatings research and techniques are also planned. The coating and grating

facilities at KPNO are unique national resources which must be maintained and

improved. Further development of remote observing techniques are anticipated,

and concomitant increases in the sophistication and capacity of KPNO computer

systems must be made. The major effort at KPNO during the period will of

course be continued work on the National New Technology Telescope. A detailed

description of the project is included as a separate section of this plan.

At CTIO the plans for improving existing instruments cover several

areas. Major efforts will continue in optical and infrared instrumentation to

keep the Observatory at the forefront of what is possible with modern

technology. Infrared detector arrays are expected to produce as large gains

as CCDs have for optical astronomy, with the result that factors of 10 to 100

or more improvement in observing efficiency can be expected for infrared

imaging and spectroscopic observations. Optical instrumentation efforts will

1-2

concentrate on making both higher spectral and angular resolution available

over what CTIO can now offer. It is anticipated that CCDs will be provided on

the smaller telescopes, thereby greatly increasing their power. To take full

advantage of the improved instrumentation, CTIO plans to complete its

modernization of the control and acquisition systems for the smaller

telescopes during the period. The increased use of two-dimensional detectors

will require expansion of CTIO's computing capabilities to handle the large

amounts of data produced by the devices . It is likely that recent

developments in microcomputers will enable data-handling needs to be met at a

cost below that of existing image processing.

CTIO's major project for 1985-1990 period will be the 3-5 meter class,

infrared-optimized telescope. A 5 meter telescope would be the world's

largest infrared telescope; at the same time it would double CTIO's light

gathering power for optical research. By basing the telescope structure and

building design on the Multiple Mirror Telescope (MMT) and by using a

lightweight mirror of the type being developed for the NNTT, engineering and

construction costs will be much lower than for a conventional design. It will

also be possible to build the telescope on a short timescale, so that it could

be ready soon after Space Telescope is launched.

All aspects of this plan are consistent with the conclusions reached by

the Astronomy Survey Committee of the National Academy of Sciences under the

Chairmanship of George B. Field. The Committee stated in its final report (p.

119):

"The National Centers face a difficult task in responding to the

diverse needs of a heterogeneous user community. They will continue

to need the strong support and encouragement of sponsoring federal

agencies in the decade ahead. The Centers must be funded at a level

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that not only provides for the maintenance of existing facilities and

staff but also permits the acquisition of appropriate new equipment

in addition to the major capital expenditures recommended by the

Astronomy Survey Committee."

Finally, it is important to note that this plan is being written at a

time when the AURA ground based observatories are being consolidated into a

single organization. This reorganization is not yet complete, and it is

possible that the final structure may require alteration of some aspects of

this plan. However, the principal features of the plan arise from the goal of

providing the best astronomy possible, and thus it is unlikely that the major

objectives of the Observatories described herein will change under the new

administrative structure.

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II. THE SCIENTIFIC FORECAST

While the prediction of future scientific directions is difficult, it is

possible to forecast trends in the technology and relate them to future

astronomical research and instrumentation. In addition, the NAS report

identifies priorities for support of existing programs and new facilities for

the decade of the 1980's.

One of the four major new projects which the NAS report recommended for

funding is a National New Technology Telescope (NNTT) of the 15 meter class .

In addition, a number of projects already underway will affect the operations

and require the support of the national nighttime observatories . The Space

Telescope and the associated Space Telescope Science Institute are already

using the observatories as they develop more precise photometry for lists of

selected guide stars in the northern and southern skies and for staff

research. After launch in 1986, the Space Telescope will undoubtedly generate

many new ground-based astrophysical and cosmological projects requiring new

observations at CTIO and KPNO.

Additional projects currently underway which will lead to new users for

the Centers include the Gamma-Ray Observatory, IRAS and other NASA level-of-

effort programs including research with aircraft, balloons and rockets. The

Explorer and Shuttle-borne Spacelab programs are currently being given high

priority by NASA and the Administration. The Shuttle Infrared Telescope

Facility, now under study by NASA, was strongly recommended by the Field

Committee and could represent a major advance in infrared astronomy.

Ground based optical measurements will continue to provide in most cases

the only tool by which distances, chemical compositions, temperatures,

densities, and velocity fields can be studied. Thus, although the fraction of

overall discoveries has naturally decreased at optical wavelengths as other

II-l

wavelength regimes have become accessible, the need for optical observations

as critical analytical tools has never been greater. The importance of

ground-based observations for understanding discoveries made in space has, for

example, been clearly shown by work on X-ray sources. There is no doubt that

both Observatories will play an important role once the new space instruments

are launched.

Another way to forecast the direction of astronomical research is to

consider the technological advances that are likely to occur and their effect

on the field. Already the application of solid state and electronic detectors

has increased the power of existing telescopes a hundredfold or more. In the

case of the infrared, an entirely new field of astronomy has been created. In

the next five years it is likely that infrared spectroscopy and imaging will

reach a level of sensitivity comparable to that of all but the most sensitive

optical techniques . It is imperative that both Observatories stay at the

forefront of infrared technology so that they can continue to play an

important role in this field.

In the field of optical detectors, there is no doubt that solid state,

two-dimensional arrays such as CCDs will dominate in the next few years, for

they are already being put into routine operation. To make full use of these

devices requires a strong effort and capability in computer hardware and

software. Single exposures from the arrays will produce a million data points

or more, and large computers with extensive image processing packages will be

as important as the detectors themselves. The Observatories must maintain and

strengthen their efforts in these areas.

Exciting progress has occurred in other fields as well. The development

of Fourier Transform Spectrometers (FTS) has enabled observations of

astronomical objects to be made at resolutions greater than were formerly

II-2

available in the laboratory. Indeed, the KPNO FTS is used for laboratory work

as well as for astronomy. Similarly, spectacular advances may occur in the

field of high resolution imaging. Should some of the interferometric devices

work as well as is expected, an order of magnitude or more improvement in the

optical or infrared may occur.

Last but far from least will be the scientific impact of the two major

new instruments proposed; the new large aperture telescope at CTIO and the

NNTT at KPNO. The probable scientific gains provided by the addition of a new

5 meter class telescope, in the southern hemisphere and open to all American

astronomers, are very great. Our understanding of H II regions, giant

molecular clouds, and the process of star formation itself will be enhanced

when such a telescope can be used to study objects such as the Magellanic

Clouds and the galactic center. Cosmology and the study of the nature of

active nuclei of galaxies will benefit from the extraordinarily good seeing at

CTIO. The benefits to all areas of astronomy afforded by the NNTT are widely

documented and generally recognized by the astronomical community; perhaps the

most exciting scientific results of this telescope will be those discoveries

which cannot be predicted.

Over the next decade, KPNO and CTIO expect and plan to develop telescopes

and instruments which will make unique and significant contributions to the

evolution of astronomical understanding. It is on this foundation that this

Long-Range Plan is based.

II-3

III. THE PLAN

In the Plan we consider what is required to maintain the Observatories at

their current operational level, allowing for the estimates of inflation over

the next five years . This plan assumes identical 5% inflation annually in the

U.S. and in CTIO's Chilean operating costs (as measured in dollars). It also

includes a number of small projects and R&D efforts which are considered

essential if the Observatories are to carry out their designated role in the

national picture. Such projects are also necessary to attract and keep the

high quality scientific and technical staff required to maintain the

Observatories at the forefront of astronomy. The major new projects, a large

aperture telescope for Cerro Tololo and the National New Technology Telescope

project at Kitt Peak, are discussed in the immediately following sections.

The role of the national observatories in contemporary astronomy is that

they are expected to provide state-of-the-art optical research facilities to

all qualified astronomers and support the efficient and effective use of these

facilities. They must also foster relevant and innovative research among

their engineering and scientific staff to ensure that the first requirement is

fulfilled at any future date. Finally, they must continually establish a

record of professional excellence and achievement in both service and

research, in order that the professional respect of the astronomical community

for them will be maintained. In order to fulfill this role our Long Range

Plan has several major components: Observatory Operations; Scientific Staff;

Telescopes, Instruments and Computers; and Research and Development.

Observatory Operations

Observatory operations include both the telescope and facilities

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operations areas. A major issue in telescope operations is the increase in

the number of visitors who use the telescopes each year. KPNO, in particular,

is facing a problem in this area as it does not have the facilities to handle

much more than the present load of visitors . At CTIO the recent

instrumentation improvements are attracting more observing proposals, and the

number of visitors is expected to increase. The causes of the growth of the

visitor load can be traced to increases in the number of telescopes on both

mountains in the last decade. In addition, at Kitt Peak the trend toward team

research, the growing use of telescopes during the daylight hours, and

comparatively short observing runs has accentuated the growth. CTIO is also

seeing an increase in the number of teams coming to observe .

The number of visitors at Kitt Peak increased from 172 in 1970 to 369 in

1982, with the 369 visitors actually making over 750 visits during the year.

During the decade, the 4 meter Mayall Telescope, the Stellar Fourier Transform

Spectrometer, the Burrell Schmidt, and the Coude feed have all been brought

into operation on the mountain. At the same time the annual appropriation to

the observatory in constant value dollars was decreasing at an average rate of

3% per year. Corresponding figures for CTIO show a similar pattern. In 1971

there were 70 visiting observers, and this number increased to 166 in 1980.

The 1.0 meter and 4 meter telescopes have been installed during the decade.

The annual rate of growth in visitor load has been nearly as large as at Kitt

Peak.

Although the observatories have made strenuous efforts to maintain the

quality of the support to visiting and staff astronomers, the quantity has

III-2

necessarily been reduced, particularly at CTIO. In addition, the balance

between user support and development programs has changed, and both program

areas are suffering from lack of funds . CTIO plans to restore the efficiency

that was lost on the smaller telescopes by the reduction of the night

assistant services with a program of modernizing the control systems and the

auxiliary instruments. KPNO has demonstrated how effective a small telescope

equipped with computer controls and modern detectors can be.

KPNO is now implementing a new policy designed to handle and reduce the

rate of growth of the visitor load. While continuing to provide the full

range of telescopes and instrumentation to visitors and staff in an effective

and efficient manner, so that scientific productivity is unimpaired, this

policy contains rules to limit the extent of team research, minimizes the

number of instrument changes, and encourages the development of remote

observing. Also, it should not be forgotten that public visitors visit both

KPNO and CTIO in large numbers. For example 86,696 people visited KPNO in

1982. The intention is to maintain public visitor facilities on both

mountains.

Remote Observing

Many astronomers now observe from an enclosed data room, collecting and

examining digital data. In many cases there is little reason why that room

need be on the mountain and not in the observer's home town. Modern

communications technology allows efficient and effective interaction with many

kinds of telescopic data at larger distances with real-time response to the

telescope operator. The obvious advantages to such "remote" observing include

less time and money spent on travel, less strain on the mountain's

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overburdened facilities, and the possibility of more efficient and adaptive,,

scheduling of telescopes depending upon weather and seeing conditions .

Moreover, such an observing mode will make possible the real time simultaneous

use of more than one observing facility, such as KPNO-VIA or KPNO-IUE. This

capability is of great importance when making multi-frequency observations of

rapidly varying serendipitous events such as supernovae, novae and comets at

perigee .

One possible disadvantage could be the reduced scientific interaction

between the KPNO scientific staff and visiting astronomers and a decreased

familiarity with instruments.

A series of remote observing experiments is presently under way at Kitt

Peak, and within the limitations imposed by the relatively slow telephone data

rate (one acquisition TV frame, every 30 seconds), the experiments have thus

far proved quite successful. They have proceeded to the point where the

Intensified Image Dissector Scanner will be available to visitors routinely

for remote observing in February' 1984. Further experiments are being made to

increase the video data transfer rate. At satellite data rates many of the

present inconveniences would disappear.

KPNO, therefore, is contemplating a proposal for a multi-observatory

time-shared observing link for use by a large number of users who would

receive but not transmit data. Observatories within the United States might

then be used by observers working from their home institutions. When

affordable satellite links become available, the service can be extended to

CTIO and to observers in Canada and Europe. Observers will communicate back

to observatories via land line voice and terminal links . Remote observing may

also be an essential feature for the most effective operation of the NNTT,

particularly since it must be located in a site of superlative seeing

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conditions where hypoxia can appreciably reduce appreciably the effectiveness

of the people working there.

The evolution of this facility is being approached conservatively since

the hardware and software available for such a system are changing rapidly.

Our cost estimates are likely to need revision, downward, it is hoped, with

future advances.

Facilities Maintenance

At CTIO, the major projects for the physical plant that need to be

carried out are the acquisition of a supplemental frequency converter for

Cerro Tololo, an extension to the astronomers' dormitory on the mountain, the

long-mentioned Tololo road improvements, replacement of Tololo temporary

buildings, and construction of a new visitors' center on Tololo. In La

Serena, a number of worn vehicles are scheduled for replacement and a new

full-capacity stand-by generator for the office/workshop area should be

purchased.

Tololo's electrical connection to Chilean power is via a 50 to 60 Hz

frequency converter now running close to its rated capacity; such a system

provides electricity at about half the cost of running diesel generators . An

additional converter will be required to meet the increased needs of the new

large telescope and to serve as a backup for the existing one.

With the installation of modern detectors such as CCDs, the number of

visitor requests for telescope time and the number of teams of observers (as

opposed to single observers) has increased notably. As the detectors are

installed on additional telescopes besides the 4 meter and 1.5 meter, CTIO

anticipates that the number of visitors will exceed the capacity of the

present dormitory facilities, and plans to build a ten room annex to meet the

needs .

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While it is unlikely that funds will be available in the early years of

this plan to pave the 23 mile long dirt road connecting Tololo to the public

highway, it should be feasible to install guardrails on the most dangerous 10

miles of the road, thereby reducing the hazards. This project now deserves

high priority.

The nearly 20-year-old "temporary" buildings on Tololo (powerhouse,

warehouse, garage, and workshops) are long overdue for replacement.

The present visitors' center also falls in the "temporary" category and

should be replaced with a new, well-equipped structure properly designed for

handling the growing numbers of visitors on the mountain. CTIO must presently

reject many requests for visits for lack of adequate and properly furnished

facilities .

CTIO projects that building maintenance will continue in the next six

years at its normal level, now that a main backlog of deferred projects will

soon be cleared .

CTIO's most pressing vehicle needs at the moment are: (1) replacement of

the Coquimbo-La Serena commuter bus (required by Chilean law if CTIO is not to

pay a transportation bonus to the entire Chilean staff); (2) a pick-up

delivery van for the Santiago Office; and (3) a stake-body pick-up for the La

Serena compound .

Finally, a supplementary emergency power generator is needed for the

offices, residences, shops and computer center of the La Serena Compound.

(The present generator is barely capable of supplying power needs for the

water system and computer center air-conditioning).

Kitt Peak National Observatory is now more than 20 years old. Many of

the basic facilities are in need of upgrading and general repair. In

particular, the water system is often pushed to its maximum capacity because

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it depends upon collecting runoff from rainfall and melting snow. A water

well and pumping stations are required to provide a dependable source of

potable water.

The dining room and kitchen need to be upgraded and enlarged. A modern

serving line is needed to comply with health code standards for a cafeteria.

The dining room must be enlarged to replace table space lost to improved

serving lines and to continue to accommodate usage by personnel from McGraw

Hill Observatory, Steward Observatory, Warner and Swasey Observatory, National

Radio Astronomy Observatory, and engineering and operations staff from Kitt

Peak National Observatory.

A second story addition to the // 1-0.9 meter telescope building is

needed. The approximately 600 square foot addition is to house increased

computer and electronics required by CCD systems and to provide a console room

and astronomers office. This telescope is currently as oversubscribed as the

KPNO 4.0 meter telescope.

A first aid and fire station building is needed in a central location on

the mountain. The current first aid station is located in an old house

trailer across from the solar dormitory, and the fire station is located down

a hill in the maintenance area away from all telescope buildings . During the

winter with snow and ice on the road, it is difficult to drive the fire truck

up the hill. A combined first aid and fire station building located "on top"

near the Visitor Center would be the logical place for public visitors to go

to obtain emergency first aid treatment.

Larger, more spacious dormitory facilities are needed for the permanent

employees assigned to work at Kitt Peak. Permanent employees are currently

assigned a dormitory room only large enough to accommodate a single twin size

bed, and thus the rooms are too small for long term accommodations. A minimum

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of five dormitory rooms built as studio apartments are needed for resident

staff members.

Normal maintenance of the mountain facilities includes such items as

repainting the 4-meter telescope building, repair of mountain roads, and

replacing the two ten year old buses used to transport employees to the

mountain.

Funding for major maintenance projects has also been included for the

Tucson facilities. Typical projects to be considered are re-roofing,

replacement of heating and air conditioning equipment, and paving of parking

facilities. Recent studies have revealed significant deterioration of some of

the photographic plates in the KPNO plate collection. This collection is a

valuable national resource consisting of 6000 Palomar Sky Survey plates, about

4000 original KPNO plates, and the 660 plates of the recently acquired

Southern Sky Atlas. To prevent further damage, an environmentally controlled

plate storage facility is needed at the Tucson headquarters .

The Tucson library is one of the best astronomy libraries in the world,

but it has very nearly run out of shelf space. If no additional space is

found, older volumes of journals will have to be discarded to make room for

new ones, and the library's pre-eminence as a research facility will be

considerably diminished. A simple expansion to the library can be made which

utilizes existing structural members and thus greatly reduces the cost. Such

an expansion would provide the necessary shelf space for a period of about ten

years .

Scientific Staff

The Scientific Staff, which includes the tenure, tenure-track, support

Ill-i

scientists and postdoctoral fellows, takes an active part in the operation of

the observatories' research facilities in addition to carrying out independent

research. The activities include assisting visitors in the use of telescopes,

instrumentation, and data reduction equipment. The staff also assumes major

responsibilities in the development of new telescopes and instrumentation, the

improvement of existing research facilities, and in devising new methods to

increase the efficiency with which telescopic facilities can be used. In the

interval covered by this plan, the scientific staff at KPNO expects to be

increasingly involved with the development of systems and concepts that will

ultimately be related to the NNTT project. In order to fulfill this added

demand and at the same time maintain Observatory activities at their current

level, additional staff positions will have to be created during the planning

period. The plan also includes funding for a scientific meeting to be held

annually at KPNO, additions to the Visiting Research Scientist Program,

continuation of the summer student program, provision for a postdoctoral

program and increments to the staff and visiting observer travel budgets .

At CTIO the Visiting Resident Scientist Program will be continued and the

postdoctoral program will be restored; both programs contribute significantly

to the maintenance of a stimulating scientific atmosphere at CTIO's remote

location.

The advent of the new large telescope at CTIO will provide many new

research opportunities and increased operational responsibilities for the

Scientific Staff. As a result, at least two positions will have to be created

above the level planned for FY-84 as the telescope project gets underway.

Additional positions will be needed as the project proceeds.

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Telescopes, Instruments And Computers

The most spectacular advances in ground-based observations in the last

decade have come from the utilization of new detectors . Solid state

electronic detectors are replacing photographic plates and image tubes for a

wide range of observations in the optical and infrared. These devices achieve

an enormous gain in observational capability, allowing in many cases

measurements limited only by photon statistics of the faintest detectable

sources and of the sky. However, for the most efficient utilization, their

particular characteristics in most cases require substantial modification of

existing instruments, or even construction of new ones. They also place a

much heavier burden on instrument control and data analysis computers and on

the telescopes themselves. Many of the instrument projects for the 1980's

will involve either major upgrading of existing instruments by incorporation

of these detectors or development of entirely new instruments specifically

matched to them.

Telescopes

Both KPNO and CTIO plan to improve the capabilities of their existing

telescopes in order that the telescope facilities continue to be suitable to

the ever-increasing needs of the instrumentation. By the end of this period

all KPNO night-time telescopes, with the exception of the #4-0.4 meter and

Burrell-Schmidt telescopes, will be equipped as follows:

integrating acquisition TV systemautomatic guider

computer controlled pointing and finding

automatic dome control

console room observingfull computer control of all instruments/spectrographs .

111-10

Increasing oversubscription rates, improved detection efficiency and

increased complexity of instrumentation require that the efficiency of

observing be improved comensurately. The above features have existed for some

time at the 2.1 and 4 meter telescopes and, in part, at some of the other

telescopes . The plan is to carry out this program at most of the other

telescopes at a steady rate, duplicating existing equipment where appropriate

and taking advantage of new technology where cost effective.

Integrating acquisition TV systems have been constructed for the KPNO and

CTIO 4 meter telescopes and for the KPNO 2.1 meter telescope. Planned systems

for the small KPNO telescopes would be similar but would utilize the currently

available higher density (64k or 256k verses 16k) memory chips in order to

reduce costs. All KPNO acquisition TV's, currently intensified silicon

intensified target (ISIT) vidicons, will be replaced with commercially

available intensified CCD cameras. These will provide improved spatial

resolution and stability as well as reduced distortion and extended service

life.

New automatic guiders will utilize either image dissector tube sensors or

TV guiders. These will improve the quality of the data taken both by better

guiding than can be provided by individuals as well as by freeing the

astronomer for quick-look review of the data. At some facilities, initially

the Coude Feed, high band-width image stabilizers will be implemented to

remove seeing induced image jitter. Such a system has been in use at the

McMath telescope for over 10 years and has proven capable of providing

increases in the throughput of a high resolution spectrograph by up to one-

half order of magnitude.

Computer controlled pointing and finding has been in operation at the 4

meter and 2.1 meter telescopes for some time. Its availability at the other

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telescopes requires no new hardware, only completion of the software and

determination of the pointing error maps. This is being done as part of the

effort to replace the Varian computer systems .

Automatic dome control is a simple matter of adding a coarse encoder to

the dome track and implementing software developed for the larger

telescopes. This is also being done with the computer replacement.

Console room observing has become a necessity with array detectors such

as the CCDs. CCDs are currently in use at the 4 meter, 2.1 meter, Coude'

Feed, and #1-0.9 meter telescopes. Plans are currently underway to implement

similar detectors at the #2-0.9 meter telescope and to install infrared arrays

at the 1.3 meter telescope. Tne plan is to significantly increase the

observing room area at the #1-0.9 meter telescope and to construct a similar

room at the #2-0.9 meter facility.

Full computer control of the instrumentation spectrographs is necessary

if console room observing is to be fully implemented. As older instruments

are retired, their replacements are being designed and fabricated with this in

mind. With the distributed processing philosophy, most new instruments will

have either micro-computers or micro-processors built into them to provide

control and sequencing functions. The communication to the facility host

computer will be simple and strictly for the purpose of commands and data

recording. Existing spectrographs are being upgraded to provide remote

control of apertures, calibration sources, etc. Provision for more classical,

on-the-platform observing will be maintained at all facilities to permit the

testing and development of new equipment as well as the use of non-KPNO

equipment.

The above-listed improvements will achieve the following objectives:

maintain the facilities of the national optical observatory at thelevel of first rate capabilities;

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upgrade the capabilities of the telescopes to a level commensuratewith the increased requirements of the planned new instrumentation;

prepare these facilities for interactive remote observing.

The planned improvements to the #4-0.4 meter and the Burrell-Schmidt

include a subset of the above listed equipment. Given that the #4-0.4 meter

telescope has a computer for control of the photometer, it will be a simple

matter to implement automatic tracking of the dome as well as computer

controlled finding. The most pressing need for the Burrell-Schmidt is an

automatic guider. The combination of the better site (KPNO versus Cleveland)

plus improved optics (primary and prisms) have demonstrated the structural

deficiencies of the telescope. Users are now interested in fainter objects at

higher dispersion, so that longer exposures are required and as a result an

automatic guider has become necessary. Construction of an automatic guider is

more difficult at the Schmidt because the use of objective prisms dictates

that an auxilliary telescope be used for guiding. This necessitates some

system to ensure mutual collimation of the guide telescope and the Schmidt,

and this can be accomplished by servoed collimation of the telescope and guide

telescope. Proper automatic guiding would require replacement of the 30-year

old drives with more modern torque motor systems. Finally, we plan to

implement automatic tracking of the dome via use of a small microprocesser for

conversion of hour angle and declination to azimuth.

In FY 1983 KPNO began work devoted to the understanding of atmospheric

phenomena and its relation to and effects on imaging in ground based

telescopes. In FY 1984 a program of systematic monitoring of the telescope

and dome thermal and turbulence environment and of the image size and motion

will be begun. Midway through the period of this plan the results of these

two efforts will be used to improve the imaging properties of existing KPNO

telescopes and will be applied to the design of the 15 meter telescope. The

111-13

thermal and image monitoring program will very likely lead to additional

environmental conditioning equipment being installed at the telescopes. This

will presumably consist of heat rejection and air conditioning equipment. The

investigation of seeing phenomena will probably lead to the application of

active and/or adaptive optics at least at the major facilities. The

utilization of such devices is anticipated for the 15 meter telescope, and

thus the early implementation on existing telescopes would provide the double

benefit of improving the performance of those facilities while providing

valuable experience for the design of the large telescope.

At CTIO, the plan is to finish the small telescope drive modernization.

New drives on the 1 meter and 0.9 meter should be installed in FY 1984 but

may, along with the system on the 1.5 meter, require some additional effort in

order to maximize their usefulness .

CTIO plans to purchase additional acquisition TV systems . The existing

Quantex systems are growing old and unreliable. It is also difficult to

obtain spare parts for these obsolete units. The addition of remote control

capability for the small telescopes requires that TV acquisition systems be

purchased for the 1 meter and 0.9 meter as well. Current plans for the 1.5

meter remote offset guider call for its incorporation in a TV autoguider

system also, this in addition to the aperture-viewing TV. Thus, at least two

new acquistion TV systems should be obtained early in this period. (one is

budgeted for FY 1984).

During the period CTIO will finish the remote offset guider for the 1.5

meter telescope (start FY 1984).

Leaky memory autoguider units will be purchased for all the small

telescope acquisition TV systems.

CTIO will continue efforts to improve local dome seeing. Insulation,

111-14

heat control, ventilation, and monitoring equipment will be used in a

concentrated effort at measurement and seeing improvement .

The 5 meter telescope project should be at a stage where it requires most

of CTIO's resources in the area of telescope engineering very early in this

period. Additional support personnel will be required as the project

develops.

Instrumentation'

The plan for the FY 1985 - FY 1989 period is to maintain the present

level of emphasis on instrument development relative to other observatory

programs. However, the increasing sophistication, complexity, and cost of

modern systems makes the state-of-the-art more expensive each year. Thus,

unless a substantial infusion of funds is obtained, the real level of activity

in this area can be expected to decrease. It is particularly important that

the national observatories provide instrumentation at least as modern as that

provided at university observatories . In recent years this has not been the

case. The first imaging photon counting detector systems will not be put into

service at the national observatories until late in calendar year 1984, but

other observatories, including U.S. institutions as well as foreign national

centers, have had such systems available to their users for over half a

decade. During the remainder of the 1980's it is planned that the national

optical observatories improve their competitive position in instrumentation in

order that the nation's astronomers be provided with the very best, most

modern equipment.

During the remainder of this decade KPNO will attempt to maintain

intensive efforts in the area of optical instrumentation while intensifying

111-15

its activities in the application of self-scanned infrared detectors. In

addition, KPNO will emphasize the improvement of instrumental efficiency, from

the point of view of throughput as well as spectral and spatial utilization.

Lastly, work on speckle techniques will commence.

In the area of optical detectors, KPNO will implement intensified CCDs

operated in an integrating mode for imaging at the 4 meter and 2.1 meter

telescopes and for medium and high-resolution spectroscopy at the 4 meter

telescope. This work was begun in early FY 1983 with the first instrument

being put in service for visitors in mid-FY 1983. Un-intensified CCD imagers

have been in service at the 4 meter telescope prime focus and the #1-0.9 meter

telescope for a number of years. In addition, un-intensified CCDs are in

service as spectroscopic detectors at the 4 meter R-C and echelle

spectrographs and at the 2.1 meter coude spectrograph. A CCD

spectrophotometer will be constructed for use at the #2-0.9 meter telescope

during the period FY 1984 - 1985. At this point, five of the KPNO telescopes

will be equipped with integrating CCDs. Efforts will continue for the testing

and implementation of new CCDs as they become available. The KPNO CCD

controller/display system can operate CCDs with formats up to 4096 square, and

currently there are three such controller/display systems available for use on

KPNO. Depending upon user demand, it may be necessary to construct one or

more additional units, given that CCDs will be useable on five of the

nighttime telescopes by the end of FY 1985.

An intensified CCD operated in a photon counting mode will become

available at KPNO in late 1984. This instrument will be used with the 4 meter

R-C spectrograph and will be similar in concept to that developed at the Mount

Wilson and Las Companas Observatories. Investigation and testing of other

photon counting concepts is expected to lead to the deployment of higher

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performance systems later in the period of this plan. Multi-anode-

microchannel-array (MAMA) detector systems offer the potential of higher

photon flux rates and greater time resolution than intensified CCDs . The

latter property makes them more suitable for speckle observations. Other

concepts, such as those utilizing encoded optical feeds to sets of

photomultiplier tubes offer the potential for even greater count rates and

time resolution. Instruments employing these or other types of photon

counting detectors will be developed first for spectroscopic use and later as

speckle systems .

The availability of both blue and red sensitive detector systems at KPNO

provides the opportunity for more efficient utilization of the telescopes via

such devices as double spectrographs and the array-equivalents of multi

channel photometers. During FY 1984 KPNO will construct a fast blue-optimized

spectrograph camera for use with the 4 meter R-C and echelle spectrographs .

Later during the period of this plan a double spectrograph will be constructed

to utilize that camera, or a version thereof, to feed a two-dimensional photon

counting detector for blue sensitivity and a red-optimized camera to feed an

integrating CCD detector for red sensitivity. Such a spectrograph could be

fed using the currently available aperture plate/slit technique or remotely

controllable fiber-optic feeds. KPNO also has planned a multi-color prime

focus camera to permit simultaneous multi-band CCD photometry. This system

would be similar to a 3-channel photometer but would utilize three CCD

detector heads .

KPNO also plans to take advantage of the higher sensitivity of

integrating intensified CCDs and two-dimensional photon counting detectors by

implementing very narrow band imagers. These will be developed utilizing both

Fabry-Perot and tuneable Lyot type filters.

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The level of resources applied to the implementation of infrared array

detectors at KPNO will be increased during the period of this plan. A 32-

element linear indium-antimonide (InSb) charge injection device (CID)

currently being evaluated by the KPNO Detector and R&D Program is the first

major effort in this area. KPNO and CTIO have undertaken joint efforts in the

evaluation of this type of array and in the procurement of other similar

devices. The utilization of other technologies (CCDs, hybrid devices, etc) by

manufacturers has made the availability of area arrays with sensitivities out

to 20 microns imminent. Recognizing that KPNO is an excellent site for 10

micron observations, a high resolution cryogenically cooled echelle conceptual

design has been developed for the utilization of such an array.

Lastly, KPNO plans to continue the development and improvement of

existing instrumentation. This will include the production of new gratings

for existing instruments, the implementation of high reflectivity coatings as

they become available, and the upgrade of "work-horse" type instruments such

as photometers and polarimeters. Further improvements to the 4 meter Fourier

Transform Spectrometer (FTS) are planned, including the implementation of

array detectors and a multiband slicer. This combination will permit

simultaneous high resolution spectra to be obtained.

At present CTIO is directing its main efforts in optical detectors at

present toward improving its CCDs and making them available on the smaller

telescopes and toward obtaining two-dimensional photon-counting systems. CTIO

will construct three complete CCD systems which can be used at the 1.5 meter,'

1 meter, and 0.9 meter telescopes and at the Cassegrain focus of the 4 meter

telescope. A substantial effort to take full advantage of new, large-format

CCDs currently under development is planned. Such a device would have an

order of magnitude larger number of pixels than CCDs currently in use at

III-l*

C-.C. _i replace the vidicon detectors, CTIO is presently beginning the

c:ns:r.::i3n of two-dimensional photon-counting systems for use at the 4 meter

and -.: nezer or 1.0 meter telescopes. It is likely that these projects will

ay-a-d :-:d 1985.

3-:= these very basic instruments and detector systems are brought up to

state-::-trie-art efficiency, CTIO plans to add a number of somewhat more

specialized instruments so as to allow its Southern Hemisphere observational

studies :o branch out into new directions. This is an important thing for

CTIC t: do because there is only one major private U.S. Observatory in the

S:ut'~, vhich might otherwise have been able to provide this more specialized

Tr.ise new instruments would include:

- A high-resolution, high signal-to-noise optical spectrometer foruse on the 4 meter telescope. At this telescope it is presentlypossible to obtain a maximum resolution of about 8-10 km/sec withdigital detectors and using a wide enough slit to observe fainterobjects. About four times higher resolution would provide areasonable match to the widths of the absorption lines in the spectraof dwarf stars, and thus permit line profile studies and betterdetection of weak absorption lines. CTIO is studying a pier-mounted,Cassegrain fiber-optics fed echelle spectrograph for this purpose.

- A spectropolarimeter device to be added to the complement ofexisting spectrographs. This should be designed to work at quitehigh resolution, for detailed studies of the profiles of emissionlines in the spectra of active galaxies.

- A multi-object, remotely controllable fiber optics feed for usevith the 4 meter and possibly the 1.5 meter spectrographs. This willoffer a great increase in the efficiency of these telescopes for sometypes of observing.

- A speckle interferometer.

Irvards the end of the 1985 - 1989 period CTIO will be fully occupied

producing the instruments for the 5 meter telescope. These instruments

include:

- A double spectrograph, similar to the one designed by Oke for useon the 200 - inch telescope.

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- CCD and 2D photon counting detectors for the double spectrograph.

- A CCD direct-imaging system.

- A duplicate multi-object, fiber-optics spectrograph feed system.

- A duplicate high-resolution, high signal-to-noise spectrometer.

The infrared program at CTIO has five main goals for the 1985-1989

period, namely:

(1) To upgrade the performance of existing telescopes until they arenearly competitive with similar telescopes at otherobservatories which were optimized for infrared observations abinitio.

(2) To provide the required instrumentation for the proposed newtelescope when its design is finalized.

(3) To take advantage of new detector technology as it becomesavailable. In this regard CTIO will try to stay competitivewith northern hemisphere observatories, while not attemptingmajor technological development which is beyond CTIO'sresources.

(4) To provide support or follow-up for space-based observations(both in the infrared and at other wavelengths).

(5) Within the constraints of major projects, to undertake smallerprojects of a highly opportunistic nature, in accordance withcurrent developments in astronomy.

These goals can be achieved by means of several projects, some of them

already underway:

(1) The 4 meter LR photometer performance will be upgraded. Thisincludes replacement of the 4 meter wobbling secondary andconstruction of an IR photometer optimized for the CTIO 4meter. The wobbling secondary is nearing completion and isscheduled for installation in January 1984. Design work isbeginning on photometer optimization. Construction will notbegin, though, until current major IR projects are completed,which will be in the early part of FY 1984. This represents

about a one year delay over previous time estimates because of

limited human resources at the Observatory.

(2) CTIO plans to develop instruments which use infrared arrays. Anarray of 32 infrared detectors has recently become availablecommercially. CTIO has begun a joint program with KPNO, andwill proceed to implement it in a system usable on a telescope

so that its performance can be judged. This will take placearound the middle of FY 1984 and continue into FY 1985.

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Implementation of near-infrared arrays is likely to be thedominant activity within the IR program during the first yearsof the plan period. Obvious uses of such arrays are in twoareas:

Spectroscopy. The CTIO IR spectrometer, to be completed in

FY 1984, has been designed to accept a small (8-element)

array initially, and should be adaptable in the future to

somewhat larger arrays as they become available.

Mapping (Imaging). Either 1- or 2-dimensional arrays willradically improve the efficiency and resolution of infraredmapping, making it more directly comparable with visualwavelength imaging. The chief difficulties withinstrumentation of this sort are likely to be dataacquisition hardware and software, since reductionprocedures will in all probability resemble those currentlyused for visual wavelength CCD imaging.

(3) New infrared instrumentation for the large aperture CTIOtelescope must be developed. This telescope will be optimizedfor IR performance. It should have dedicated infraredinstrumentation. Construction would begin toward the end of theplan period. The instrumentation would have capabilitiesresembling that of existing 4 meter and 1.5 meter telescopeinstruments.

(4) A number of smaller projects will be of value. Some maycomplement or support space-based observations . These are seenas small, specialized instruments which can be constructed with

a relatively modest effort. Work on some of these may begin atthe start of the plan. They include:

Mm./sub-mm. detector. This would be a state-of-the-art(helium-3 cooled) far infrared detector which would beoperated at the Cassegrain focus of the 4 meter telescopetogether with the other 4 meter infrared detector

systems . Since millimeter observations can be carried outduring dry but non-photometric conditions, this wouldprovide a considerable amount of "free" time for millimeter

work. Millimeter and sub-millimeter observations in theSouthern Hemisphere are likely to become of increasinginterest as observations from IRAS and from several

Southern molecular-line surveys become available .

High spatial resolution. Interest in achieving neardiffraction-limited spatial resolution in the infrared hasincreased in recent years, and a number of Northern

observatories have already implemented one-dimensional"speckle" systems in the near-infrared. Such a system maybe implemented at CTIO by the end of FY 1984. Considerable

111-21

improvement in efficiency (though not in resolution) shouldbe achievable with infrared arrays of modest size .

Long range planning for visual photometers must take into account the

expected utilization of CCDs. For applications involving either crowded field

photometry and/or stars fainter than 14th magnitude, CCD photometry is clearly

superior to classical single or multiple channel photoelectric work. This

does not mean that one should abandon the old ways: photoelectric photometry

will continue to have several applications .

(1) monitoring of objects with very fast time variability and foroccultations .

(2) work in spectral regions where CCDs are not sensitive (ultravioletand infrared, for example).

(3) setting up bright standards for checking calibration of CCD fields(especially if CCD data were obtained on non-photometric nights).

(4) work on individual stars widely scattered over the sky

Therefore, needs for visual photometers during the period FY 1985-1989

are dominated primarily by the necessity to maintain existing photometric

equipment at a level of high reliability. Visual photometry represents

roughly 40% of total telescope usage at present, primarily on the smaller

telescopes. As the older equipment wears out, it is desirable to replace it

with equipment with greater efficiency, as has been done in the past. As

computers are made available on all but the smallest telescopes, the manual

photometers should be replaced by automatic photometers . Two of these are now

in service, but in the face of increased demand a third may be required during

the period of this plan.

Another minor improvement would be provision of a capability of quasi-

simultaneous visual and infrared observations. On the new 4 meter photometer

this can be accomplished simply by the construction of an appropriate f/30

visual coldbox.

111-22

A third improvement would be the construction of a modern 2-channel

visual photometer for the 1.5 meter (also usable on the 0.9 meter). This

represents a greater development effort than those listed above, and would be

justified only by strong user interest in such an instrument. It should be

flexible enough to be used as a faint star photometer (star and sky channels)

and also as a 2-color photometer. Such a device would require a staff

scientist to devote his support effort to optical photometry.

Finally, fiber optics can be used to develop a multiple object

photometer. This instrument would be useful for monitoring variability of

objects against a reference star, especially on nights when thin clouds would

ordinarily preclude such observations .

Computers

New computer systems are being implemented at the Kitt Peak National

Observatory, both on the mountain and downtown. The new mountain facilities

are designed to replace the Varian 620 systems with a system of computers

which will provide reliable data acquisition and process control along with

augmented data reduction and real time processing capabilities . The Tucson

computers are designed to replace the Interactive Picture Processing System

(IPPS), the Varian V74, the Hewlett Packard 2100, and the Cyber 170/720

systems with a facility that can better handle the current and anticipated

volume of two dimensional data. The new computer systems for both the

mountain and downtown will be based upon using Digital Equipment Corporation

(DEC) systems. This will provide benefits of both hardwark and software

compatibility.

On the mountain, the Varian computers will be replaced with DEC 11/24 or

111-23

11/44's depending on the need of each telescope facility. The replacement

computers will operate independently in a stand alone mode for data

acquisition and telescope control . The new computers are required to handle

the increased volume of data supplied by array detectors. The systems will be

equipped with much greater disk and memory to accommodate the needs of two

dimensional data. Data reduction capability will be provided at the

telescopes to provide many basic reductions in full and quick look reductions

in all cases. In the continuing development of research capabilities, the

most important features of the mountain computer systems are the capacity for

expansion and availability of the peripherals, since these are the most common

limiting features .

A VAX 11/750 will be installed in the mountain administration building to

serve as a central data reduction facility. The observatory has included

funding for a limited facility in the FY 1984 Program Plan. Future

requirements include connecting the central data reduction computer to all

telescope computers by a network system. By providing hardware that is

equivalent to the downtown data reduction, all of the interactive reduction

and analysis facility (IRAF) software will thus be available for use on the

mountain. The VAX 11/750 may serve as a full IRAF satellite, which would

require the purchase of additional peripherals .

Eventually, there should be a high speed data link (possibly microwave)

between Kitt Peak and Tucson. This will provide the full power of the

downtown computer systems to the domes, and reduce the need for additional VAX

class computers on the mountain where they are difficult to maintain. The

data link will also be needed if remote observing is to be supported

efficiently on a regular basis .

All computer systems, both on Kitt Peak and downtown need to be connected

111-24

by a network such as Ethernet . This will permit sharing of expensive

peripherals and provide extensive computer power at all facilities .

In the FY 1984 Program Plan we discussed the importance of replacing the

Cyber 170/720 computer with a system more compatible with current observatory

needs . Funding limitations may not allow us to replace the Cyber facility

during FY 1984. In this case it should be replaced in early FY 1985.

The Cyber computer system serves two purposes . It serves first as a

batch data reduction and analysis systems for the entire observatory and

second as a host for the IPPS system. The Cyber, despite its large computing

capability, is becoming a hindrance in fulfilling the computing requirements

of the observatory. The architecture of the system is archaic and it is a

major obstacle in providing portable code that visitors can run at their home

institutions, or that the observatory can run on Kitt Peak. We need to

replace the Cyber with a system that is more compatible with the other data

collection and data reduction systems at the observatory and throughout the

national and international community. For the Cyber lease costs alone, we

could purchase several VAX-class machines per year and give KPNO far more

computing resources than are currently available with the Cyber. Thus, we

need to replace the Cyber with a "host" computer of the super VAX class.

The downtown IPPS facility was developed in 1975, and, it is no longer

able to cope with the increased volume of data coming from an increased number

of digital detectors. To illustrate the need, we note that the IPPS was

unable to completely fill the demand for image analysis, even in 1975. In

1975 no digital arrays were in regular use at KPNO. Today, the 5 CCD systems

are in use and a 6th is under construction. The need for image analysis

exceeds the available facilities by a factor of 3 or 4. Even more important,

astronomers cannot now explore reduction techniques, but are forced to

111-25

concentrate on a few minimal operations . In order to manage the increasing

volume of image data and to allow Kitt Peak to exchange image processing

software with other astronomical centers, the development of the IRAF is

underway.

The IRAF will consist of satellite computers dedicated primarily to a

single image reduction user. Each satellite will be capable of driving an

image display for interactive image processing and general data reduction and

analysis. The VAX 11/750 has been selected as the first IRAF satellite

computer and two of these systems have been installed in Tucson. These

satellite computers will be connected to a large host so that expensive

peripherals (array processors, large disks, group encoded magnetic tapes) may

be concentrated on one system, and so that the interactive user on a satellite

can spawn large numbers of batch reductions (on the host) without destroying

the interactive usefulness of his satellite. Tnis is a very important

feature, needed to permit the visitor who is resident in Tucson for only a few

days to complete reductions which are partially interactive and partially

computation intensive. Implementation of these major software and hardware

programs on Kitt Peak and in Tucson will require that additional staff

positions be filled in the Computer Support Department.

With the introduction at CTIO of new instrumentation such as the 2D

Photon Counting Devices, large-format CCD chips, IR arrays, and an Imaging

Fabry-Perot, CTIO expects that by 1985 the data reduction and analysis load

both in La Serena and on the mountain will have suffered a several-fold

increase. The experience at other major observatories indicates that the

MV/8000 in La Serena will not be able to handle more than two users

simultaneously reducing 2D data, and most likely only one user at a time

carrying out reductions of 3D data (such as produced by an Imaging Fabry-

111-26

Perot) or sophisticated programs such as RICHFIELD. On Cerro Tololo, of

course, not even this capability is currently available. The instrumentation

currently planned will produce, by 1985, a quadrupling of the data output on

the mountain as well as the need for facilities to allow simultaneous

reduction of 2D and 3D data by six to eight users. By 1989, we anticipate yet

another factor of two increase in demands on the computers. Hence, thre will

be an urgent need by 1985 to significantly increase CTIO's computing

facilities.

Within realistic funding constraints, two options exist for increasing

the capacity for data reduction and analysis in La Serena and Cerro Tololo.

These are (a) the purchase of another large, multi-user computer such a the

MV/10000 or VAX-11/780, or (b) acquisition of several of the new generation of

super-micro computers such as the Sun Workstation. Under option (a), CTIO

would very likely install the new computer in La Serena, and relocate the

MV/8000 on Cerro Tololo. A fast data transfer link between the MV/8000 and

the central S230 Eclipse computer in TOLNET would allow the former to be used

for on-line data reduction by observers on the various telescopes included in

TOLNET (although the practical limitation of two simultaneous 2D users will

probably still apply). In La Serena, the new computer replacing the MV/8000

would handle the same number of users as before, but most likely at a 50-100%

increase in speed.

With option (b), CTIO envisions employing super-micro computers as

satellite workstations to the MV/8000 in La Serena, connected in a limited

network such as Ethernet. Each super-micro would have its own large (80-160

MByte) disk, an inexpensive image display device, and possibly a magnetic tape

drive. The VICOM image display system would be left on the MV/8000 for users

requiring it's sophisticated facilities. The super-micros would run UNIX,

111-27

offering considerable software compatibility with other astronomical

institutions. The implementation of super-micros on the mountain could also

take the form of satellite workstations of TOLNET or as stand-alone data

acquisition and reduction systems.

CTIO, in consultation with KPNO, is presently studying both options (a)

and (b) in further detail, and expects to reach a decision by the middle of FY

1984 as to which it will pursue. In fact, a combination of both options may

eventually be required to meet the expected data reduction and analysis

burden .

By 1985, CTIO expects to have the 4 meter, 1.5 meter, 1 meter and 0.9

meter telescopes included in TOLNET, and to be using this as the data

acquisition system for the optical photometers, IR photometer/spectrometer,

SIT Vidicon, and CCD. However, for new instrumentation CTIO will most likely

begin to utilize the new, more-powerful, stand-alone super-micro computers.

In the period 1985-1989, CTIO expects to improve communications between

La Serena and Cerro Tololo to allow for the possibility of remote observing.

This would probably entail the purchase or leasing of a multi-channel

microwave link. This link might also be feasible for data transmission

between the Cerro Tololo and La Serena computer systems.

Software support requirements can be expected to increase in direct

proportion to any increase in hardware. Hence, for the increase in computing

facilities outlined above, an additional four to five programmers should be

added to the staff. At least two more electronics engineers will also

probably be needed to support the hardware increases .

111-28

Laboratory Improvements

While the KPNO optical fabrication facilities are excellent, continual

improvement is required if the needs of sophisticated new instrumentation and

of the 15 meter NNTT are to be met. Most of the optical polishing equipment

is nearly 20 years old and more capable equipment is now available.

Similarly, better test equipment, primarily that associated with digitally

recorded interferometric testing, has decreased the amount of art while

increasing the amount of science, and thus the cost-effectiveness, of the

optical polishing process. During the period of this long range plan, KPNO

will procure new large aperture interferometric test equipment, probably a

ZYGO interferometer, as well as implement computer controlled polishing,

either by the modification of existing equipment or by procurement of a

complete system.

The KPNO Gratings Laboratory is a unique national resource which can

produce gratings which are unavailable from any other source. This equipment

is also over 20 years old and recent attempts to rule large, high blaze angle

gratings have demonstrated the need for improvements to this facility.

Planned improvements include replacement of the bell-crank operated diamond

carriage with a linear motor stroker and implementation of closed-loop

positioning of the diamond.

Research and development performed under the Technology Development

Program for a National 15 meter Telescope has demonstrated the need for

improvement of KPNO's optical coating facilities. Again, these facilities

must meet requirements which cannot be met cost-effectively by commercial

sources. The efforts will be directed to two areas: the first toward solving

the problems associated with providing multiple layer coatings on large

111-29

surfaces and the second toward research on the coatings themselves . NNTT

conceptual designs include the utilization of refractive elements to obtain

large fields of view. Tnus the study of broad band anti-reflection coatings

must also be included.

Research and Development

The Observatories will continue to take a leading role in Research and

Development for the Optical/IR community. The purpose of the R&D program at

KPNO is to provide the technological basis for advanced planning of new

telescopes, such as the NNTT and the CTIO Large Aperture telescope, and for

the upgrading of existing facilities. The direction, emphasis and goals of

this program are based on our current understanding of the scientific needs of

astronomy and of current technological capabilities and potentials . Thus the

plan emphasizes basic technology, particularly in the detector field, and work

toward development of an NNTT.

There are two necessary ingredients for a successful R&D program.

First, there must be a very tight coupling between the scientific goals of the

community, the scientific staff, the instrumentation program, and the R&D

effort. This coupling will be provided by the users committees of the two

Observatories and by strong scientific staff involvement in all phases of

these activities. Secondly, since virtually all the R&D effort is at or

beyond the technological state-of-the-art, a knowledgeable, creative and

imaginative engineering and technical group will be maintained in the

Observatories.

In the following exposition, research and development will be subdivided

under the following subheadings: Basic Technology, including detectors,

111-30

cryogenics, and optical coatings, Prototype Instrumentation, and NNTT

Instrumentation.

Basic Technology

Included in this area is the development, adaptation and evaluation of

optical/IR detectors, development of cryogenic capabilities, and possibly

grating and coating improvement. In general, this effort should be directed

toward applications of clear scientific need, either for improvements in the

efficiency, capabilities or performance of existing instrumentation or for new-

instrumentation for existing telescopes.

It is anticipated that the adaptation and evaluation of both linear and

two-dimensional IR detectors will be a major, high priority effort over the

next 5 years at KPNO and CTIO. The application of high quantum efficiency,

multi-detector arrays to IR spectroscopy and mapping will result in enormous

gains in sensitivity and efficiency over our present techniques which, in

virtually all cases, utilize single detectors.

The relatively small IR arrays (32 x 32, 32 x 1) are expensive ($20K

each) compared to silicon CID's and CCDs, and the evaluation and application

costs are still dominated by manpower. Nevertheless, every attempt will be

made to incorporate LR arrays into effective, usable instruments for staff and

visitor use in the near future. It is a major Observatory goal to use solid

state arrays as the primary detectors on most instruments. Their compactness,

high quantum efficiency, geometric stability and large dynamic range make them

the clear choice for foreseeable detector applications. In order to reach

this goal, it is most important to continue the R&D evaluation and

adaptation of silicon CCDs into the near future. In addition, R&D work on

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high speed, two-dimensional detectors with application in advanced sub seeing

instruments and possible spectroscopic systems is necessary. Tnis work would

include techniques for cryogenic temperature control, efficient use of

cryogens, cryogenic actuators, etc., as required.

Prototype Instrumentation

At present the R&D program at KPNO is working on a prototype cryogenic

spectrometer. Two examples of areas for future prototype instruments are IR

cameras and spatial interferometric devices:

IR Cameras

With the availability of two-dimensional IR arrays comes the possibility

of vastly improved mapping capabilities . The scientific potential and

importance of efficient "picture taking" in the IR cannot be overestimated.

It is comparable to the importance of optical imagery to all of astronomy and

heretofore has been unattainable. Prototype cameras for rapid picture taking

on a variety of spatial scales and spectral regions will be required in order

to demonstrate observing techniques and background suppression approaches, as

well as the limitations and scientific utility of such devices.

Spatial Interferometry (both optical and IR)

The next frontier in optical astronomy is probably the development of

very high spatial/angular resolution capability. This area is also of high

scientific interest in the IR. R&D work will begin on the development of

111-32

fast two-dimensional photon counting arrays and on-line processing hardware.

The capability has clear application to spectroscopy as well as imaging.

NNTT: National New Technology Telescope Instrumentation

In addition to work on the NNTT itself, which is described in Section V,

the R&D effort must aim toward defining the instrumentation needs and

understanding the required associated technology. In order to take full

advantage of the potential capabilities of an NNTT, virtually all

instrumentation will require careful design and development. Included in this

are the following:

1. larger area and pixel size detectors2. large gratings3. spatial and spectral interferometry techniques4. seeing studies

In the case of detectors, whether applied to imagery or spectroscopy, a

problem exists in a resolution mismatch between the best currently available

solid state detectors and the image forming characteristics of a 15 meter

class telescope. It is part of our Long Range Plan to start a special program

in detector and instrument development that will address this problem and

assure the availability of appropriate detectors and instrumentation when the

telescope is placed in operation. It is clear that detector developments

should proceed in two distinct areas: large-scale CCDs and large-scale event-

sensitive photoelectric detectors. In both cases, significant departures from

current and anticipated technology are involved. Moreover, until there is

secure knowledge of the technological possibilities, there will be no

competent basis for predicting the level of performance that is desired and

required. Therefore, serious attention to the subject of detectors will begin

in FY 1984.

111-33

IV. NEW LARGE APERTURE TELESCOPE AT CTIO

If the United States is to maintain a balanced astronomical program in

the next decade, it is important that small to moderate projects be funded in

addition to the major ones. For example, the major project currently under

way, Space Telescope, and the first priority project recommended by the NAS

Committee, AXAF, have a total cost between 1.5 and 2.0 billion dollars.

Unquestionably both instruments will depend heavily on ground-based telescopes

and will increase the demand for their use. Being space instruments, both

will have all-sky coverage. For the U.S. to take full advantage of their

potential, it must ensure that adequate ground-based facilities are available

in both hemispheres . If we consider that CTIO can double its light-gathering

power in the optical and increase its infrared capability by more than a

factor of ten for about one tenth of the cost of the NNTT and one hundredth of

the cost of Space Telescope, the conclusion is inescapable that a relatively

small project such as CTIO's planned 3-5 meter class telescope deserves

serious consideration. Indeed the NAS Committee and its panels recognized

this fact. Examination of the Committee's recommendation and the report of

the panel on Ultraviolet, Optical, and Infrared Astronomy shows that the

highest ranked groundbased optical/IR projects are first, the NNTT, and second

a 4 meter class IR telescope in the Southern Hemisphere.

It is also important to realize that ground-based telescopes offer

capabilities in certain areas that are far superior to the current generation

of space instruments. A 5 meter telescope on the ground has more light

gathering power than the Space Telescope and is superior for high resolution

spectroscopy of objects brighter than the night sky. Space Telescope will

have no infrared instruments at all initially and SIRTF missions will only

last a week. Thus, ground-based telescopes will offer the only long term,

IV-1

continually available infrared facilities for many years. Finally, of course,

ground-based telescopes have a much wider field of view than does Space

Telescope.

As a result of the improved outlook for funding in FY 1984. CTIO has been

carrying out studies together with its users and outside consultants of an

infrared-optimized telescope with an aperture as large as 5 meters. The

concept, which has the enthusiastic support of the users and staff, is based

on the lightweight mirror technology being developed for the NNTT and the

Multiple Mirror Telescope (MMT) mount and building design. A single,

lightweight 5 meter mirror in an altitude-azimuth (alt-az) mount and building

similar to that used for the MMT would be much less expensive to build and

requires a considerably smaller engineering effort that a telescope and dome

of conventional design. The MMT has proven that it meets the stringent

tracking and pointing requirements for a modern infrared telescope; therefore,

it is logical to utilize as much of the design effort and expertise that went

into it as possible. First estimates indicate that such an instrument would

cost about SIOM and could be built in three years after a mirror blank became

available.

A preliminary proposal for the project has been prepared and submitted to

the NSF with the FY 1984 program plan; consequently, the full details of the

project are not repeated here. Since the submission of the proposal, CTIO has

been fortunate to have the assistance of the project scientist for the MMT

from the Harvard-Smithsonian Center for Astrophysics, Dr. N. Carleton, and the

project engineer, Mr. T. Hoffman, in beginning a study of how the MMT design

can be modified to accept a single, lightweight 5 meter mirror (Figure IV-

1). The availability of alternate mirrors is also being investigated. The

main work for FY 1984 and FY 1985 will be as follows: to establish the

IV-2

Figure IV-1. Perspective view of proposed 5 meter telescope for CTIO,

IV-3

optical and mechanical specifications of the telescope and carry out the

corresponding optical and structural design studies, to obtain detailed cost

estimates, to test and select a site for the telescope on Tololo or Cerro

Morado, and to begin design work on the auxiliary instrumentation. Once these

steps are carried out, actual construction can be initiated.

As an illustration of how the MMT design can be modified to accept a 5

meter single mirror, Figure IV-2 shows two views of the resulting telescope

and building. The modifications to the mount mean that the yoke base would be

shortened by 36 inches . The azimuth bearing support height would be reduced

by 16 inches and a 12 inch high spacer would have to be added under the

elevation bearings. However, the rest of the design can be taken over

virtually unchanged, so that a minimal amount of engineering work (less than

or equal to two months) would be needed before the mounting fabrication could

go out for bids .

The side view of the mount and building in Figure IV-2 indicates that the

building profile would change from rectangular to a more oval form because the

shutters would have to be reconfigured. Otherwise the only building

modifications would be to replace the existing bridge crane with a shutter-

supported crane and to increase the width of the side rooms . It would not be

necessary to develop the building interior as extensively as was done for the

MMT because laboratory and shop facilities already exist on Tololo; this would

reduce the building costs somewhat.

IV-4

?&

o^1 v

H^

s

^

Figure IV-2. Elevation views of proposed 5 meter telescope for CTIO,

IV-5

Mr. Hoffman has developed a time schedule, shown in Figure IV-3, that

illustrates how the telescope could be completed in three years after funding

became availble. As mentioned above, the modification to the mount and

building would be minor and both could go out to bid within the first months

of the project. The telescope tube structure, mirror cell, and head rings

would, of course, require new designs, but they are all conventional and

should not cause any difficulties. The lightweight, honeycomb mirror will be

strong, and will not require a special mirror mount to maintain its optical

figure .

Under the assumption that funding started in FY 1986, then the telescope

could be ready in FY 1988. The availability of the mirror blank is, of

course, crucial. As it will depend on the progress of the NNTT project, it is

also important to investigate other sources for mirrors . To date two

possibilities are known for backup mirrors: a Canadian 4 meter blank and an

Italian 3.5 meter blank. Should a lightweight 5 meter mirror not be produced,

then it would be logical to see if the Canadian 4 meter blank could be

obtained as an interim solution. First conversations suggest that this may be

possible .

In any case, the budget tables consider that the project will start in FY

1986 and follow the schedule described in Figure IV-3. Note, however, that

the project could get under way earlier if funding were available and the

production of lightweight mirrors could be accelerated. Given the success of

IRAS and the need for ground-based observations of the new infrared sources it

is finding, there is ample justification for building the telescope now. For

the same reason it would be desirable to have the telescope ready as soon

after the launch of Space Telescope as possible.

IV-6

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V. 15 METER NATIONAL NEW TECHNOLOGY TELESCOPE (NNTT)

During the next decade the role of the national ground-based observatory

will change. Implementation of the VIA to its fullest capability, successful

launching of the Space Telescope, and the data from IRAS will all serve to

place unprecedented demands upon ground-based observatories for complementary

investigations and observations of newly-discovered phenomena. The case for

these investigations and the new, ground-based telescope required to make them

has been set forth by the Strittmatter Committee and, more recently, by the

NAS Astronomy Survey Committee. These committees, and other important groups

in astronomy, have shown the need for a 15 meter class telescope on the ground

optimized for optical and IR observations. Furthermore, there is a stated

need for the National Observatory to assume leadership in the quest for its

completion.

During FY 1984 the 15 meter National New Telescope project will pass one

of the most important milestones along the path to completion: a final

selection of the telescope concept. This decision will be the product of five

years of concept studies (FY 1975 through FY 1980 through the Next Generation

Telescope Program), three years of technical feasibility activitis (the 15

Meter Technology Development Program), and innumerable contributions from

individuals and groups in and out of KPNO concerned with telescope design. In

mid-FY 1983 the Universities of Arizona and California joined with KPNO to

form a consortium to work toward the final concept selection. The major

activities of these groups will be the completion of technical feasibility

studies initiated under the Technology Development Program and the comparison

of the two competing concepts. A Scientific Advisory Committee (SAC) composed

of astronomers from throughout the United States has been established. The

Committee has been given the task of recommending which of the two concepts

should be chosen for the NNTT:

V-l

The Multiple Mirror Telescope (MMT) concept with four 7.5 metertelecopes mounted on a common structure and feeding light toeither separate foci or to a central optical beam combiner. Theexisting six-mirror MMT on Mt. Hopkins serves as a prototype formany of the important design features .

The Segmented Mirror Telescope (SMT) which differs from moreconventional telescopes principally in using a primary mirrorcomprised of segments held in position by a system of sensorsand acutators. The University of California has adopted this

approach for their Ten-Meter Telescope. The UC design is in arelatively advanced state of completion.

Figure V-l shows scale models of the two concepts along with a model of

the KPNO 4 meter telescope. For comparison purposes the three models were

constructed to the same scale.

It is planned that the concept decision be made in mid FY 1984.

Following the choice, the work will turn toward detailed design of the

telescope with emphasis on those technical areas most in need of better

definition. The telescope enclosure as well as the optical polishing facility

will be designed during this period. This work will carry on through FY 1985

and 1986. A major portion of the detailed engineering and architectural

design work will be carried out under subcontract. Only modest increases in

the NNTT Program staffing will be required to monitor such contracts and to

carry out the conceptual design of the telescope and instrumentation. A

complete telescope proposal will be generated in FY 1986.

Concurrent with the telescope design work in FY 1986 we intend to carry

out plans developed earlier for building an optics facility that will serve,

at a minimum, as the means for making the NNTT primary optics. At present,

none of the optical fabrication facilities available anywhere in the world are

really suitable for making all of the off-axis aspherics for the SMT or for

polishing the 7.5 meter mirrors for the MMT. A substantial investment in the

V-2

The Segmented Mirror Telescope(SMT)

FIGURE V-l.

15 METER NNTT CONCEPT SCALIi MODELS

The KPNO 4-Meter Telescope The Multiple Mirror Telescope

(MMT)

development of new optical technology has been made in recent years . There is

a follow-on need for a facility to produce optics taking advantage of this

technology and, in particular, to fabricate the NNTT optics. Properly

planned, the cost of this facility will be offset by reductions in the cost of

the NNTT optics that might otherwise have to be produced at high risk with

inadequate facilities or under subcontracts that would be inflated to include

the cost of new facilities. In order to avoid costly delays in the NNTT

completion, it is important to have the optics facility ready at the outset.

As with most large telescopes, the special nature of the primary mirrors

mandates special equipment and talent. Thus it is planned that the

construction of the optical fabrication/polishing facility be started in FY

1986. The cost of this in FY 1986 is modest and is felt to be cost effective

in that early availability of the facility will serve to shorten the duration

of the project.

It is planned that construction of the telescope commence in FY 1987 with

completion in FY 1992. Further increases in the staffing level will be

required to monitor the construction contracts as well as complete the design

and construction of the instrumentation.

Efforts are also being devoted to the selection of a site for the 15

meter telescope. A minimum-level two-year program of critically needed tests

was begun in mid FY 1983. This program and the sites to be tested were

defined by the Ad Hoc NNTT Site Survey Committee in the spring of 1983. On

the basis of the requirements set down by the committee, two sites were

selected for testing: Mauna Kea on Hawaii and the Pinaleno Mountains in

Southern Arizona. Preliminary testing of these sites has determined no

significant detrimental factors . The testing program will continue into late

FY 1985 with the actual site selection being made in late FY 1985.

The details of the plan for the 15 meter NNTT for the period of this long

V-4

range plan are given in Table V-l. This Table shows the progress of the

project from 1982 along with plans through the end of FY 1989. Table V-2

gives the details of the spending schedule through this period while Table V-3

shows the staffing schedule.

It is recongized that the 15 meter telescope will be instrumented and

operated in a fashion significantly different than current facilities .

Certainly, the telescope will be scheduled quite a bit differently than most

present facilities . More remote observing and queue scheduling will

undoubtedly be done. The scale of the instrumentation will be very much

different form that in use today. Study of these areas is necessary and is a

vital element of the large telescope program. KPNO, with its expertise and

experience in the construction and operation of major astronomical facilities

is in a unique position to lead and participate in the development of

telescope technology while at the same time pushing foward in the related

areas of detectors and instrumentation that will serve both present day and

future astronomers.

V-5

Table V-l

NNTT 15 Meter Telescope Project - Planning Schedule

Activity

SEGMENTED MIRROR TELESCOPE:

Segment Fab. DevelopmentSegment Control Tests

MULTIPLE MIRROR TELESCOPE:

Borosilicate Blank Devlp.Mirror Support Devlp.

TELESCOPE DESIGN STUDIES:

Comparative Design Studies

Comparative Instrument Studies

Final Concept Selection

TELESCOPE DESIGN:

Telescope MountingInstrumentation

Telescope Enclosure

Optics Polishing Facility

CONSTRUCTION:

TelescopeMirror Blank Mfg

Optical Polish Fac .Optical PolishingMirror Supports

Telescope EnclosureInstrumentation

Computers & Controls

SITE SELECTION:

Select Test Sites

Site Evaluation

Site Selection

Site Preparation

1982 1983 1984

-#

-#

-1.8m

V-6

Fiscal Year

1985 1986 1987 1988 1989

-3 .5m- -7 .5m

-#

-#

-#

»

#

•#>>

»

»

»

»

Tabic V-2

NNTT PROGRAM - SPENDING LEVELS

(amounts in thousands)

Fiscal Year

Category 1982 1983 1984 1985 1986 1987 1988 1989

Personnel $ 363 $ 450 $ 460 $ 757 $ 893 $1280 $1630 $1746

Supp. & MatIs . 30 39 190 145 200 200 200 200

Other Services 157 336 1362 1470 1500 500 200 200

Dom. Travel 5 22 52 40 40 50 60 60

For . Travel 1 6 10 15 15 20 30 30

Equipment 12 159 165 440 1000

Construction 2000 10000 20000 30000

TOTALS $ 568 $1012 $2238 $2867 $5648 $12050 $22120 $32236

Notes: 1. Project scientist & site survey scientist are budgeted underthe KPNO scientific staff.

2. 5% inflation assumed for FY 1985, no inflation assumed thereafter

V-7

Category 1982

Table V-2

NNTT PROGRAM STAFFING PROJECTION

1983

Fiscal Year

1984 1985 1986 1987 1988 1989

Scientific 1 1 2 2 3 4 4

Tech. Prof. 3 5 5 8 9 12 13 14

Prof. Admin . 1 1 1 2 2 3 3 3

Admin/Clerical 1 2 2 2

Tech/Other 5 5 5 8 9 14 20 22

Maint/Service

TOTALS 9 12 12 20 23 34 42 45

Notes: 1. Authorized staffing level at end of fiscal year.2. Does not include project scientist (R. Lynds) and

Site Survey Scientist (M. Merrill), both arebudgeted under KPNO scientific staff.

V-8

TAIII.K 1

CLKKO Tlllillil INTLK-AMKKICAN 1Hi S i: l( V All IKY

AND

KITT I'KAK NATIONAL oh.SF.KVATOHY

I.ONO KANI.TC I'Ij\N SUMMARY

(FY I'JII.'. - FY 1989)

(An, d:; In Til,hi:,,11,(1:, )

FY-84 FY-85 FY--H6 FY-H7 FY-Ml FY-89

CTIO KI'NO CTIO KI'NO CTIO KI'NO CI 10 KI'NO CTIO KI'NO CTIO KI'NO

OBSERVATORY OPERATIONS 5 '.,951 5 9.1)5 5 5,(.8'. 5 9,901 5 6,255 510,57'. 5 h,'.:)2 511,015 5 6,'.II 511,'..15 5 (,,70/ 511,995

SCIENTIFIC STAFF 4 SUITOKT 952 1,465 1,000 1,656 1,050 1,7)9 1,101 1,1)26 1,157 1,917 1,215 2,01)

OBSERVATORY, 1'RO.ItCTS 1,397 1,382 1,64'J 1,1)09 5,6)1 2,024 6,1148 1,843 1,564 1,765 2,414 1,891

OTHER I'ROC-RAMS 2,643 3,445 6,249 12,682 22,7111 32,9)1

TOTAL I'UN $ 7 3(.)0 514,825 5 8,3)3 $16,813 512,916 520,586 $14,381 527,166 511,112 517,898 $10,356 $48,830

TOTAL CTIO 6, KI'NO $22,125 $25,146 5)3,522 541,749 549,030 $59,186

Inflation Rate: 5Z

OBSERVATORY OPERATIONS

Operations 4 Maintenance

TABLE 2

CERRO I'OLOIJl I (ITER-AMERICAN OBSF.HVA I'OKY

AMU

KITT I'EAK NATIONAL OBSERVATORY

I.ONC RANCE I'l.AN SUMMARY

(FY 1984 - FY 1989)

(Amounts In Thou;;au<Ls )

FY-84 FY-85 FY-86 FY-87 FY-88 FY-89crl0 KI'NO CTIO KI'NO CTIO KI'NO CTIO KI'NO (.Til) KI'NO (.Til) KI'NO

"''pay rol l\ Payroll Expenses $1,037 $ 2,988 $1,089 $ 3,142 5 1,143 5 3,299 51,200 5 3,464 5 1,260 $ 3,637 5 1,324 S3,8194 10 614 441 645 46) 677 486 711 511 747 5)6684 420 725 441 761 463 799 486 839 511 8IH

$1 ,037

585

400

52 ,02 2

5 333

98

62

5 493

Materials 4 SuppliesServices 4 Other Costa

Sub-total

Eiii'lneerlng 4 Technical Services .Payroll 4 Payroll Expenses 5 333 5 1.436 $ 350 $ 1.508 $ 367 $ 1.583 $ 3115 5 1.662 $ 405 5 1./45 $ 425 5 1,813

y 360 11)3 378 108 397 113 417 119 438 125 459199 65 209 68 219 72 2)0 75 242 79 254

Materials 4 Supplies

Services 4 Other Costs

Sub-tot a I

5 4,082 52,123 $ 4,308 $2,229 $ 4,523 $2,340 ?_^'49 W,_457_ $ 4.987 5 2.582 i_J_.JT±

5 493 $ 1,995 5 518 5 2.095 $ 543 $ 2,199 $ 570 S^09 S_ J>99_ $ 2,425 $ 629 5^546

Intlac Ion Kate: it

TAHI.F. 2 (Coiitlnueil)

l'.i|;e 2 of 4Inflation Kate: 57.

Administrative Services

Payroll 4 Payroll ExpensesMaterials 4 SuppliesServices 4 Other Costs

Sub-total

Suh-totnl 04M

Management Fee

Total OSM

FY-84

CTIO KPNO

$ 866 $ 1,7 73

117 205

983 755

$2,166 $ 2 733

$4,681 5 8 RIO

5 150 $ 300

54,831 $ 9 1 10

Construction 4 Major Maintenance Projects

Mountain Facilities $ $

City Facilities 120225

Sub-total

TOTAL OBSERVATORY OPERATIONS

5 120 $ 225(1)

54.951 5 9,335

(1) To be funded from FY 03 carryover

~~"

- .- .__

5 909 $ 1,875 5 95 5 $ 1,969 SI 00 1 $ 2 06/ $1 05 1 5 2 1 71

33 1 215 14 9 2 26 16 7 2 1/ 18 5 2'.9

1 0 32 799 1 084 8 19 1 1 18 8111 1 1 9'", 92 5

$2 2 74 $ 2,889 $2 1118 $ 1,014 $2 508 5 1 1 8 5 $2 6 ) 1 5 1 14 5

$4 915 $ 9,2 92 $5 160 5 9,/56 $5 4 18 510 24 ) $5 6119 $10 7 57

5 158 $ 315 $ 165 $ 111 $ 174 5 14 7 5 182 C; 16 5

55 073 $ 9,607 $5 12 5 $10,087 $5 592 $10 ,590 55 87 1 $11 12 2

$ 320 5 20 7 $ 860 $ 300 $ 840 e 150 $ 540 s 2 50

291 89 70 187 75 63

5 611 $ 282 $ 930 $ 3 7 5 $ 840 $ 4 2 5 $ 540 $ 113

$5 684 $ 9,901 $6 2 55 $10,574 $6 412 $i i ,015 56 .411 $11 415

FY-89

CI 10 KPNO

$1,105 $ 2,279

405 262

1,255 971

$2,765 $ 1,512

5 5,976 $11,294

$ 191 $ IHI

56,167 $11,677

5 540 $ 2 52

66

$ 540 $ 118

$6,707 $11,995

TABLE 2 (Cml Inued)

Page 3 of 4Inflation Rate: 57.

SCJE_NT 1FIC STAKE 4 SUPPORT

Payroll 4 Payroll ExpensesMaterials 4 SuppliesServices 4 Other G.sts

FY-84

CTIO KPNO

FY-85

CTIO KI'NO

752 $ 1.278 $ 790 $ 1,46027 28

200 160 210 168

FY-86

CTIO KI'NO

FY -87

CTIO KPNO

FY-88

CTIO KI'NO

829 5 1,533 $ 871 5 1,610 $ 914 S 1.69030 31 33

221 176 232 185 243 194

FY-89

CTIO KPNO

$ 960 $ 1,77534

255 204

TOTAL SCIENTIFIC STAKE 4 SUPPORT 5 952 5 1.465 5 1,000 $ 1,656 $ 1.050 $ 1.739 S 1,103 5 1.826 5 1,157 $ 1.917 5 1,215 $ 2.013

OBSERVATORY PROJECTS

New lnlt1 at ives

Coiupul e rs

l-irge Aperture Telescope

TOTAL OBSERVATORY PROJECTS

$1,081 $ 1,020 $362

316

915 $ 1,309 $ 1,381 5 1.174 $ 1,518 $ 1,443 $ 1,809 $ 1.515350 500 350 650 300 400 100 250384 3,900 5.030 1,655

$ 1,804 5 1.591

200 300

4 30

1.397 $ 1.382 $ 1,649 $ 1.609 5 5,631 $ 2,024 $ 6,848 5 1.843 $ 3,564 5 1,765 $ 2.434 $ 1,891

ft

TABLE 2 (Continued)

Pa£e 4 of 4Inflation Rate: 57.

FY-84 KY-85 KY-86 i'Y-87 KY-IIII FY-89

CTIO KPNO CTIO KPNO CTIO KPNO CTIO KI'NO CTIO KI'NO CTIO KI'NO

OTHER I'ROCRAMS

Detector Research & Development $ $ 278 $ $ 397 5 5 417NN1T Program 2,198 2,872 5,648Coalings Lib 70 74 77Oral logs Lib 67 70 74Visitor Pi ograin-Fore I gn Travel 30 12 II

TOTAL OTHER I'ROCRAMS 5 5 2,641 5 $ 1,445 $ $ 6,249

$ 418 S $ 4 5912,050 2 2,120

111 85

78 HI

15 16

SI 2,682 $ $22,781

$ 4 82

32, 216

119

86

18

$32, 911

TOTAL PI AN $ 7,300 $14,825 $ 8,333 $16,813 $12,936 $20,586 514,383 527,366 511,132 537,898 $'0,356 $48,8)0

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