CERRO TOLOLO INTER-AMERICAN OBSERVATORY
AND
KITT PEAK NATIONAL OBSERVATORY
FY 1984 PROGRAM PLAN
Revision 1
November 18, 1983 TABLE OF CONTENTS
I. Introdu&frton ...... 1-1
II. FY1982 Research Highlights II-l
III. Scientific Projects and Programs
Highlights III-l
Scientific Projects - CTIO III-2 - KPNO III-5
Special Programs - KPNO 111-10
IV. Operations & Maintenance, Scientific Staff, and AURA Management
Operations & Maintenance - CTIO IV-1 - KPNO IV-4
Scientific Staff - CTIO IV-11 - KPNO IV-11
AURA Management IV-14
V. Construction V-l
VI. National New Technology Telescope VI-1
VII. Non-NSF Programs VII-1
VIII. FY-1984 Budgets and Staffing Tables VIII-l
APPENDIX 1 - Organization Charts - CTIO 1 - KPNO 2
APPENDIX 2 - Resident Staff and Primary Fields of Interest
- CTIO 3 - KPNO 4 APPENDLX 3 - User Data - CTIO 6 - KPNO 9
APPENDIX 4 - Preliminary Proposal for a Large Southern H5fl*sphere (3-5m) Telescope 15
APPENDIX 5 - The NNTT - A Status Report, April 1983 36 I. INTRODUCTION
In Fiscal Year 1984 CTIO and KPNO will continue ongoing programs of operation and support of the national optical and infrared telescopes. Both observatories-^ill-continue to maintain and improve instrumentation, upgrade the computing facilities, and in addition, each will move towards a major construction program.
At KPNO the time is ripe to prepare to construct the major ground-based optical/infrared telescope of the 20th century. The aim of this project, the National New Technology Telescope project, is to carry on advanced technology development and site assessment activities that can serve as the basis for future design and construction work on new large telescopes. This project, which is being carried out in collaboration with the University of California and the University of Arizona, requires a choice to be made between a segmented mirror telescope (SMT) design and a multiple mirror telescope (MMT) design during FY1984. To do this an extensive program of investigation involving both technical studies and scientific trade-offs together with site testing beyond that already carried out over the last 2 1/2 years will be carried out. Many astronomers, physicists and engineers from KPNO and throughout the community will be involved. This project is discussed in detail in Section VI and Appendix 5.
At CTIO plans are being laid to construct the first major telescope built since the 4-meter telescope was completed in 1975. In FY1984 concept studies directed towards the building of a 3-5-meter telescope that will complement the 4-meter and more than double CTIO's light gathering power will be carried out. The new telescope will keep CTIO at the front rank of southern hemisphere observatories, a position which the European Southern Observatory (ESO) has challenged in recent years by telescope and instrumentation projects that have given ESO the lead in light gathering power. This project is closely related to the NNTT program since mirror fabrication at that size is one of the technical developments required to decide between concepts in the NNTT program. A detailed discussion of the project appears in Appendix 4.
CTIO's plans for FY1984 are based on the continuation of the Chilean government's current exchange rate policy. This policy, under which the peso was devalued in FY1982 and subsequently pegged to the Chilean inflation so that it would maintain a constant real value against the dollar, allowed CTIO to undertake a rebuilding program in FY1983 to remedy the weaknesses caused by the layoffs of previous years and the postponement of maintenance and instrumention projects. CTIO will continue the rebuilding program in FY1984 by placing major emphasis on new instrumentation and improvement projects for the existing telescopes. Unfortunately, the reduced funding level of Revision 1 will slow these efforts considerably in comparison with what was orignally planned.
Although CTIO and KPNO are similar in the number and type of major facilities that are offered for nighttime astronomy there are differences between the two in operation and staffing and consequently in what is emphasized in each observatory's program. Cerro Tololo has seven telescopes, including the 4-meter, the largest in the Southern Hemisphere, and is the principal observatory in the South available to all U.S. astronomers. The summit is at 2200 meters elevation in the foothills of the Chilean Andes and
1-1 Rev. 1, 11/18/83 85 km from La Serena, where the main offices, laboratories, and library of the Observatory are located. La Serena, in turn, is 300 miles north of Santiago and Valparaiso, the main ports of entry for astronomers traveling to CTIO and for supplies being imported from the U.S. Operating a high technology observatory" at a* remote -site in a foreign country thousands of miles from the U.S. influences the style and type of work done. For example, the time and expense involved in travel to Chile results in visiting astronomers making fewer trips than they might to KPNO and receiving more observing nights per session. The distance from high technology centers makes it more difficult to develop and support sophisticated equipment at CTIO than at KPNO. Consequently, CTIO has fewer instruments and concentrates on making them as versatile and serviceable as possible. The CTIO efforts with vidicons, where the same detector can be used in a variety of spectroscopic and direct imaging applications, and the TOLNET network of interconnected computers are examples of this approach. Because of the geographical location of the observatory, CTIO is not an ideal place for developing the very forefront, experimental instruments; rather CTIO's efforts are directed towards acquiring and implementing instrumentation based on concepts that have already been shown to be promising. In view of the foregoing, it is best for CTIO to concentrate on providing excellent equipment in selected areas so that U.S. astronomers can do frontier work on the most important problems in Southern Hemisphere astronomy.
Kitt Peak offers 12 telescopes to U.S. astronomers in addition to providing sites and services for 6 telescopes operated by other institutions. The 4 meter telescope is outstandingly well equipped, and the McMath Solar Telescope is the largest solar telescope in the world. KPNO is the leading U.S institution for nighttime astronomy in terms of the facilities offered, visiting astronomers received, and range of programs covered. The Observatory is located 52 miles west of Tucson at an elevation of 2100 meters and has, in addition to the telescopes, extensive facilities including laboratories, workshops, dining rooms, dormitories and auxiliary instruments. The Tucson headquarters contains offices for staff and visiting astronomers, a library, laboratories, and computing facilities. In addition to equipment of the type provided by CTIO, KPNO has developed and installed the best fourier transform spectrometers in the world. A variety of low light detectors are available for work on faint objects and powerful computing facilities and display units for image processing are provided. These computing facilities are heavily used by visiting astronomers. The well- equipped smaller telescopes at KPNO are powerful enough for work on front-line problems. In addition, KPNO has important programs in detector development, optical coatings, and diffraction gratings that are for the benefit of the entire astronomical community.
1-2 Rev. 1, 11/18/83 II. FY1982 RESEARCH HIGHLIGHTS
CTIO VISITOR RESEARCH HIGHLIGHTS
A. Extragalactic Astronomy
1. The Magellanic Clouds. Using the SIT vidicon on the 1.5m telescope, P. Massey (Canada) and P. Conti (Colorado) observed faint Wolf-Rayet stars in the LMC. They conclude that spectroscopically similar W-R's span a range of 3 mag in absolute magnitudes, and hence their spectral subtypes cannot be used to infer their distances, as has often been done.
A. Cowley (Michigan), D. Crampton and J. Hutchings (Canada), in collaboration with several other groups, are making a complete survey of the stellar X-ray sources in the Magellanic Clouds. The B3V star identified with LMC X-3 was found to have a period of 1.7 days and a velocity curve with K = 235 +/- 11 km/s yielding a mass function of 2.3. The X-ray data was searched for eclipses in this period but none were found. The mass of the unseen companion is thus at least greater than 6 and most probably 10-11 solar masses making it the first extragalactic black hole and only the second well established case at all.
A major study of the optical emission line strengths in nearly 100 WN stars in the Galaxy and in the LMC was completed by Conti, Leep and Perry (Colorado). This body of data has been obtained over the last few years from observations on the 4m telescopes at KPNO and CTIO. The nitrogen and helium line ratios in these objects form an ionization sequence, but the strengths themselves are very different, even at similar subtypes. It seems inescapable that real abundance differences exist.
2. QSOs and Seyferts. B. Margon and R. Downes (Washington) obtained 4m spectra of an 18th magnitude blue object, discovered as an X-ray source, and located just north of the distant rich cluster of galaxies 0016 + 16 (z = 0.541). They find this object to be a QSO of redshift z = 0.55 +/- 0.01, essentially identical to that of the cluster. Although many QSOs have previously been found in small associations of galaxies, this is perhaps the best evidence to date for QSO membership in a rich cluster.
By now there are a significant number of cases of a quasar being near a galaxy with the same redshift. There is, up to now, only one case (3C 273) where there have been enough galaxies of similar redshift for a velocity dispersion to be reliably estimated so that a mass of the quasar could be estimated. New observations at CTIO of the southern hemisphere quasar PKS 0548-322 now allow another quasar mass estimate to be made. In November 1981, T. Kinman (KPNO) used the UV SIT vidicon spectrograph on the CTIO 4m telescope to get several spectra each of seven compact nebulous objects that surround this quasar. These observations showed that the nebulous objects are galaxies that have the same redshift as 0548-322; the redshift of the quasar was also confirmed. These observations support the idea that 0548-322 consists of an abnormally extended elliptical galaxy with a very compact non-thermal source
II-l at its center. A velocity-dispersion study for 0548-322 (with seven galaxies) gives 6.1 x 10E13 solar masses. The cluster around 0548-322 does seem to be more compact than that around 3C 273. Clusters with velocity dispersions as high as 800 km/s are frequently X-ray emitters and 0548-322 is a known X-ray source . —«*= -
3. Other Galaxies. S. Boughn (New Jersey) and P. Saulson (Massachusetts) performed a search for primeval galaxies using the InSb IR detector on the CTIO 4m telescope. They scanned 22 small patches of the sky which are devoid of stars and galaxies on deep plates, hoping to find light- at 2.2 microns. Such light might come from galaxies in a predicted bright phase of their early history. No statistically significant deflections were observed. The results allow some constraints to be placed on the nature of galaxies in the redshift range z = 10 to 20.
Outside of the Local Group, the nearest galaxies include those of the Sculptor Group. Of these galaxies, one of the closest and best resolved is the late-type edge-on system NGC 55. G. Da Costa (Connecticut) and J. Graham (CTIO) have studied the nature of the objects that might be globular clusters associated with this galaxy. The candidates all appear marginally non-stellar on 4m plates taken in excellent seeing and have magnitudes consistent with those expected for bright globular clusters in NGC 55. From the spectrophotometric observations, three candidates were found to have radial velocities that agree with that of NGC 55 and are therefore most likely to be globular clusters in this galaxy. The spectrum of the brightest cluster shows strong hydrogen lines which together with photoelectrically measured B-V and U-B colors suggests that this" cluster is a young (age < 10E8 years) globular cluster analogous to those found in, for example, the Large Magellanic Cloud. Thus NGC 55 becomes the fourth galaxy after the LMC, and SMC, and M33 to be shown to contain young globular clusters. Such clusters however, are not found in either our Galaxy or M31. The two other NGC 55 clusters appear, on the basis of their integrated spectra, to be old (ages > few Gyrs.) and moderately metal deficient and therefore they are probably similar to the old halo globular clusters of our galaxy.
B. Galactic
1. Clusters. 0. Levato, S. Malaroda and N. Morrell (Argentina) have continued their program on spectral morphology, axial rotation and percentage of binaries in open clusters. Among the most interesting results are the following: a) they discovered among the members of NGC 2287 three Hg-Mn stars, one star with a weak K line, one star with a composite spectrum, and eight double-line binaries, b) they found that the main-sequence members of NGC 6231 have an average axial rotation which is 65% of the rotation of field dwarfs, and also that the percentage of spectroscopic binaries among them is around 60%. c) they found several stars with broad hydrogen lines among the members of Trumpler 16 and Collinder 228. The broad-line stars are similar to one of the stars of the Trapezium system in the Orion Nebula Cluster, d) preliminary results based on more than 700 spectrograms of 60 stars in the Sco-Cen Association indicated a percentage of spectroscopics binaries for the Association of around 70%.
W. Harris, J. Hesser (Canada), and B. Atwood (CTIO) have begun a program of vidicon photometry in B and V for color-magnitude studies of several
II-2 galactic and LMC globular clusters. Applying van den Bergh's recent stellar models to the data, they find 47 Tuc to have an age in the range of 15 to 18 billion years at [Fe/H] ~ -0.5.
2. Stars-i—*&.-Stone (California) has collaborated with J. Baldwin (CTIO) in establishing a grid of 18 stars, generally in the declination band between -20 and -40 degrees, which are intended as flux standards for large southern hemisphere telescopes. The star's monochromatic magnitudes range between 10 and 14.5, and the observations cover the wavelength range from 3200 to 8280 angstroms.
A. Landolt (Louisiana) has completed the acquisition and reduction of UBVRI photoelectric data taken at the CTIO 0.4m and 0.9m telescopes. The 223 stars in the program are to be found mostly in an approximate two degree band centered on the celestial equator. The photometry is tied into Landolt's equatorial UBV standard stars and into Cousins ' E-region standard stars . The stars average 20.7 measures each on 12.2 different nights. These 223 stars fall in the magnitude range 7 < V < 12.5, and in the color index range -0.3 < B-V < +2.1. The mean error of the mean is ~ 0.003 magnitude for the magnitude and all color indices except for U-B, where is is ~ 0.005 magnitude.
A program of B, V photometry has been started to support development of the Guide Star Selection System (GSSS) at the Space Telescope Science Institute (STScI). The GSSS will select guide stars that the ST will use to locate and guide on astronomical targets. Positions and magnitudes of the guide stars will be measured from Palomar and SRC Schmidt plates. To achieve the required magnitude precision, photometric calibration sequences are needed at each plate center. The CTIO 0.6m and 0.9m telescopes are being used to observe stars in the approximately 800 sequences south of declination zero. In the first nine months of the program, 2834 observations of 1356 stars from 210 sequences were obtained, and the southern program is about 28% complete, with 90% completion expected at the end of 1983. The program is under the supervision of J. Russell and B. Lasker of the STScI.
3. Nebulae and Interstellar Material. D. Gezari (Maryland) has carried out a program of 1.0mm continuum observations of cool southern clouds, including the completion of a map of the entire NGC 6334 complex. The map covers a region about 30 arcmin long in the galactic plane, and shows six major centers of submillimeter emission. The northernmost peak, NGC 6334/1 (North), is a very cool (T = 19 =/- 5 degrees K) and dense star formation region in an extremely early stage of evolution. Each of the other peaks corresponds to a major molecular emission enhancement; however, two of the 1.0mm peaks are also associated with HII emission. The results confirm that the NGC 6334 complex is one of the most massive galactic molecular clouds, with visual extinctions in several peaks exceeding A(V) = 100.
During the past year R. Williams (Arizona) completed his studies of southern spatially resolved nova shells and spectroscopy of cataclysmic variables . The emission-line spectra of the shells around CP Pup and T Pyx were analyzed. The analysis shows that the CP Pup shell is relatively cold (T < 10E3 degrees K), yet moderately ionized. Its spectrum is unlike that of any nebula, consisting entirely of recombination lines of H, He, and N. The nitrogen abundance deduced from the N recombination lines yields N/H > 0.1, making the shell one of the most nitrogen-rich objects known. All of the nova
II-3 shells studied so far share this trait. The shell of T Pyx is similar to that of a planetary nebula, indicating that a strong source of UV radiation must still exist in this old nova. The extreme abundance enhancements in some nova shells raises the possibility that novae should be more important sources of Nitrogen for tlie^nterstellar medium of many galaxies than are planetary nebulae. Thus novae are likely to play a central role in the synthesis of some of the CNO in many galaxies. Nova models predict that the N produced in this manner should have an isotope ratio N15/N14 ~ 1 which should provide an interesting test of the idea.
4. X-ray Sources. J. Thorstensen (Vermont) and P. Charles (England) have completed a three-year investigation of the X-ray binary 2S 0921-630. This system generally shows a spectrum consisting of a nearly featureless continuum with high-excitation emission lines. Yet, the X-ray flux observed at earth is relatively weak; the apparent L(X)/L(opt) ratio is near unity. Systems with this low ratio tend to display evidence of binary behaviour and X-ray heating, which prompted the investigation, beginning in March 1979. The picture that has emerged is complex and not yet well-understood. Photometric measures on 26 nights, when combined with published results of other workers, yield a clear 9-day modulation. There is no long, deep eclipse in the light curve, though a 16-hour eclipse may be present if the period is near 9.013 days. The velocities, while consistent with the 9-day period, do not confirm it independently. The phasing of the velocities and light curve indicates that much of the emission probably arises from the gas stream between the two stars .
C. Solar System
1. Planets and Asteroids. J. Elliot, R. French, D. Mink and K. Meech (Massachusetts) and J. Elias (CTIO) observed a stellar occultation by Uranus simultaneously with the 4-m (at 0.88 microns) and 1.5m (at 2.2 microns) telescopes . These data will provide information about the sizes of ring particles and improve the kinematic model for the ring orbits. Using occultation data previously obtained at CTIO and other observatories, several of the Uranian rings were found, contrary to theoretical expectations, to be inclined a few-hundredths of a degree relative to the equatorial plane of Uranus . These are the first known examples of inclined planetary rings .
CTIO STAFF RESEARCH HIGHLIGHTS
J. Baldwin (CTIO) and M. Smith (Scotland) have studied a sample of QSOs having continuum absorption breaks near 912A in the emission-line rest frame. Of 3 QSOs which are sufficiently well observed to comment on the location of the absorbing material, 7 almost certainly have the absorbing material somewhere outside the emission-line region. The other case, though ambiguous, is also consistent with absorption by material external to the QSO. By including data from other samples, they conclude that the covering factor for large clouds of emitting material, espsilon < 0.09 and that the data are entirely consistent with epsilon < 0.02. The small observed values of the L alpha/H beta intensity ratio for QSO emission lines are therefore unlikely to arise from selective L alpha depletion. Three of the five quasars which they observed at Cerro Tololo showed broad absorption features in their
11-4 spectra. In one object they discovered a huge trough of Nitrogen V absorption which might be spread over a range of ejection velocities as large as 54,000 K/sec (0.18c).
By means -*fe»^small-dispersion near-infrared spectroscopic surveys of 29 SMC and 52 LMC sample regions, V. Blanco (CTIO) has studied the surface distribution of carbon and M-type giants in the Magellanic Clouds. The surveys achieved a high degree of completeness throughout the depth of the Clouds for the carbon stars and for the giants of type M5 or later, and a moderate degree of completeness for those of type M2 to M4. The total number of LMC carbon stars within the area sample in the surveys is about 8400, but an additional 2000 such stars may be found further out in the periphery for a total of 10,400. For the SMC, the corresponding figures are 2900, 600 and 3500. The ratios of carbon to M giants appears to be constant throughout each of the Clouds, but appreciably more C stars per M giant are found in the SMC than in the LMC. In particular, the ratio: Number of carbon/Number of giants of type M5 or later is 5.9 +/- 0.9 in the SMC, and 0.87 +/- 0.04 in the LMC.
0. Eggen (CTIO) has completed numerous studies, one of which is summarized here.
Pseudocepheids I. R Puppis, HR 4511 and AI CMi. The pseudocepheids (PC) are defined as supergiants in the Hertzsprung gap with light variations more erratic than those of cepheids. The present discussion includes four, high mass PC that are typical of some 20 observed on their present program. R Pup shows light variations that are not periodic but reach amplitudes of delta u = 0.4 mag and delta V = 0.2 mag. The color indices vary regularly with V but~H beta appears to vary independently. R Pup is located on the boundary of NGC 2439 but the cluster is apparently only the result of an absorption hole. The reddening of R Pup is E(b-y) = 0.142 mag and M(V) = -8.3 mag, giving a modulus of 14.3 mag. HR 4441 (omicron' Cen) has a reddening of E(b-y) = 0.149 mag and M(V) = -8.2 mag, giving a modulus of 12.65 mag and placing it in Car OBI which contains such objects in the immediate vicinity of HR 4441 as NGC 3293 (Mod. = 12.75 mag) and HR 4352 (FO la, Mod. = 12.55 mag). HR 4511 (V810 Cen) is a member of the cluster Stock 14 for which a modulus of 12.25 +/- 0.15 (sigma) and a mean reddening of E(b-y) = 0.178 +/- 0.018 (sigma) mag are derived. The observed color indices of HR 4511 are obviously affected by the presence of a blue companion and removal of these effects places the star very near R Pup and HR 4441 in the (M(Bol), Log T(eff) plane. The star may be quasi-periodic variable (~ 120 days) but there are large changes in the amplitude and the hot companion may be contributing to the variation. AI CMi is not a periodic variable but the cycle length is generally less than 100 days. Most of the color indices are not uniquely correlated with the V magnitude and the large reddening may be caused by circumstellar material.
During 1982, J. Elias completed observations for several major projects. The first of these was completion of identification and study of sources detected in near infrared surveys of portions of the Magellanic Clouds. Some results have been previously published, and a major portion of the data is incorporated in a detailed study of Magellanic Cloud K and M supergiants prepared with J. Frogel (CTIO) and R. Humphreys (U. of Minnesota). The final analysis of the survey results is underway.
II-5 The second project is a study of newly identified low-luminosity T Tauri stars in five southern dark clouds . Spectrophotometric and IR photometric observations indicate that a number of these stars are fainter than absolute visual magnitude +12, and may be stars of considerably less than a solar mass.
Elias and Frogel also completed, in conjunction with collaborators at Caltech and Mt. Stromlo, definition of the infrared standards system in use at CTIO and of the transformation between the system and that used at Mt. Stromlo and the AAO.
Among the projects completed by J. Frogel during the year is one he initiated six years ago to obtain infrared observations (JHK magnitudes and CO and water band indices) of giant stars in globular clusters. The initial objective was to assemble a library of infrared colors, magnitudes, and molecular band indices for globular cluster stars drawn from the entire range of cluster metal abundances . These data are of importance in the construction of stellar synthesis models and for a proper understanding of differences and similarities between the stellar populations of globular clusters and early type galaxies. In many cases, such as for clusters associated with nearby galaxies, only integrated light observations are feasible, and they must be calibrated by studies of nearby clusters for which both types of observations are possible. This work, done primarily in collaboration with J. Cohen of Caltech and S. Persson of Mt. Wilson and Las Campanas Observatories, has now been completed. They have prepared two major studies which present data on 26 clusters and a thorough analysis of these data plus those available from 7 previous papers on the subject which were already published. In a separate study, Frogel has examined the evolutionary status and pulsation characteristics of about 50 red variables in globular clusters .
J. Graham has taken new observational data for the dark globule ESO 210— 6A in which two Herbig-Haro objects were discovered by Schwartz. Images were obtained in H alpha, [S II] and near-IR light and new velocities as measured from spectrograms taken with the CTIO 4m telescope. Although it has not been possible to locate an obscured source, it seems very probable that in ESO 210- 6A we have a good case of bipolar material outflow from a young recently formed star causing shocks which are seen as H-H objects.
New optical observations by J. Graham demonstrate differential velocities of at least 800 km/s within a group of gaseous filaments near the middle NE radio lobe of the galaxy NGC 5128. These optical fragments are at a projected distance of 30 kpc from the main body of the galaxy and are associated with an extended source of soft X-rays. Compared with reasonable values for the average space velocity of the gas, the internal velocity spread is too high for it to have travelled in its present turbulent state over the full distance from the nucleus. The gaseous filaments, as observed, are evidently only temporary and will disperse over a time of the order of 10E6 - 10E7 years .
P. Osmer (CTIO) continued his work on quasars near the apparent redshift limit at z ~ 3.5. He found that PKS 2000-330 (z = 3.78, the largest known redshift) was easily identifiable by its L alpha emission on a 4m grism plate of the type used earlier to search for quasars with z between 3.7 and 4.7. Spectra of PKS 2000-330 obtained with the SIT vidicon" confirm that L alpha is much stronger than CIV 1549A, as is the case for lower redshift quasars. Osmer obtained new grism plates with a wider bandpass (4950-6900A or 3.1 < z <
II-6 cr «; j> M rt o o O < ft) fD p- O rt Hi O pr id rt cr Hi fD 3 P- O <§ fD rt pf h P- o- Hi P-1 3" p- a. o rt rt a. 3 3" C fD H- fD o n o OP € ft> PG >•< B n> 0) < ft) ft> rt rt pr 3" fD PL p- rt a. fD rt ?0 rt fD p- 3 C-, rt O oq en O (D fD rt W fD rt ^j • P- 3 n 3 V rt 3 CO (X CO ft) CO P- oq m 3" 5-J" Hi £-• CO CO (D fD rt fD in ft) pr 3. 3 ft) c/) P- (_J P- . ft) rt CO p- ft) CD CO o o o ro O rt - JUL S 3- rt . ft) ^-n rt ft) fD P- rt rt p- O rt rt 3 -O rt 3 0 1— P1 in ^ OQ Oq CO rt rt rt
A new discovery in this field has been made at Kitt Peak by Chincarini, Rood and Thomp««B- using..the image Intensified Image Dissector Scanner (ITDS) on the 2.1-m telescope. Redshifts were obtained with this equipment for a random sample of 44 galaxies, selected from a complete population of 350 galaxies, brighter than 15.7 magnitude, in a 332-square-degree region between the Hercules group of clusters (A2151, A2152, A2147) and the A2199/2197 group. Here A2151 (for instance) is the identification of a rich cluster of galaxies in a catalog compiled by Abell. A plot of the redshift of these galaxies against position in the sky showed that there is a bridge of galaxies connecting the two groups of clusters. The redshifts of the galaxies vary smoothly by 2000 km s-1 in going from the Hercules region to the A2199/2197 region, and the bridge is tilted by 27° off the plane of the sky. There are rather few galaxies in the space between us and this bridge.
The suggestion that these groups of clusters might all be part of a giant supercluster was made by Abell twenty years ago. The new work, based on redshifts, is the first definite proof that this is the case. The result is significant because it is the first bridge that connects groups of Abell clusters as distinct from serial connections between single Abell clusters. It is also the longest bridge — from 50 to 100 Megaparsecs (depending on which distance scale is adopted). This is therefore the largest contiguous supercluster yet found, and it could be larger still if it is found to extend south beyond the Hercules region.
The tilt of the bridge to the plane of the sky is also of particular interest since, although this is entirely to be expected in a three- dimensional interpretation of the data, it is the first time that such a tilt has been observed. Most previously observed nearby clusters seemed to have major axes in the plane of the sky: this appearance now seems less significant.
2. The Luminosity of Serendipitous X-ray Quasars. Quasars were first discovered as radio sources, and the majority of those known were found this way. Their identity and nature was then confirmed by optical observations. Quasars can also be discovered by their peculiar optical properties even though they may not be observable as radio sources . Three astronomers (Margon, Chanan and Downes) have identified the optical counterparts of 47 serendipitously discovered X-ray sources with previously unreported quasars. These were X-ray sources that were discovered accidentally by the Einstein Observatory during observations made on other objects. It has been known for several years that many quasars are X-ray sources, but before these accidentally discovered sources could be identified with quasars, optical photometry and spectroscopy from ground-based observatories was needed. This has been done by Margon et al. at a number of observatories, including CTIO and KPNO: at Kitt Peak the 2.1-m telescope was used both for spectroscopy and multi-color photometry. It is found that about 50% of the X-ray sources can be identified optically to a limiting visual magnitude of 18.5, and that 70- 80% of these identifications are quasars whose spectra are indistinguishable from those found first as optical or as radio sources.
II-8 The surprising result of this investigation is that, although at a limiting magnitude of V = 18.5, a typical quasar (absolute magnitude M = -26) should have been detected with a redshift z = 0.9, the mean redshift or those found is only z = 0.42. In other words, this survey has revealed significantly -«a*e intrinsically faint quasars than other surveys to the same optical limit and there is a lack (relatively) of the more luminous quasars.
If one accepts a recently proposed value for the global value of the intrinsic X-ray to optical luminosities, these new observations could put severe constraints on the space density and luminosity function of quasars . Alternatively, the "typical" quasar, one that is optically luminous but not superluminous (absolute magnitude M > -27), may turn out to not be a strong X-ray source. This latter inference is not in conflict with the existing X- ray data on preselected quasars .
3. 0351+026: A QSO Spawned By Interacting Galaxies? If quasars (QSOs) are at the cosmological distances implied by their large redshifts, then they are the sources of enormous amounts of energy. There is increasing evidence that quasars are the ultra-luminous nuclei of distant active galaxies . These host galaxies are so distant however that it is difficult to investigate the source of this energy by finding out how the quasar phenomenon is triggered and maintained. This suggests that it would be profitable to study nearby quasars for which a more detailed view is possible. One of the nearest objects with quasar-like properties is 0351+026 which was identified earlier with a serendipitously discovered X-ray source (Bothun, G. D.; Romanishin, W.; Margon, B.; Schommer, R. A. and Chanan, G. A. 1982, Astrophysical Journal, 257 40). They showed that the quasar had a redshift of 0.036 and was a low-luminosity galaxy (l-L. = -18); this host galaxy was unusual in that it contained a large amount of neutral hydrogen that had a large (1500 km s~ ) velocity width.
New observations of this interesting object have now been made by Dr. Gregory Bothun (Harvard-Smithsonian Center for Astrophysics), Dr. Jeremy Mould (KPNO), Dr. Timothy Heckman (University of Maryland), Dr. Bruce Balick (University of Washington), Dr. Robert Schommer (Rutgers University), and Dr. Jerome Kristian (Mount Wilson and Las Campanas Observatories). New observations of the neutral hydrogen at Arecibo confirmed the unusually large amount of H I in this system and show that there are two sources present with a velocity spread of 1000 km s . The profile of the 21-cm line is strongly reminiscent of those found for pairs of interacting galaxies .
Direct evidence of the duplicity of this source comes from new deep images obtained with the 800 x 800 CCD detector at the prime focus of the KPNO 4-m Mayall telescope. These pictures show two nucleated galaxies embedded in a cloud of nebulosity. The brighter of these two galaxies (which has a luminosity of about that of the Large Magellanic Cloud) is the "host" of the quasar; the fainter companion galaxy has a luminosity similar to that of the Small Magellanic Cloud. The overall morphology is analogous to that in the examples of interacting pairs given by Arp. The small galaxy also has colors similar to those of the Small Magellanic Cloud although the larger "host" galaxy is somewhat redder than the Large Cloud.
New spectra of the system were obtained using the Cryogenic Camera with the Ritchey-Chretien spectrograph of the KPNO 4-m telescope. Three 20-minute
II-9 exposures were made using a Texas Instruments CCD as a detector. These spectra show that both galaxies are immersed in a highly excited gas. The [OIII] 5007 line (which is a convenient tracer of such gas) forms a bridge connecting the two nuclei. Excluding the QSO nucleus, the brightest [OIII] emission occurs, in the region between the galaxies although there is no enhancement of the-continuum emission in this region. This is taken as evidence of interaction between the galaxies. There is no evidence, however, that the interaction has produced appreciable amounts of star formation; thus neither galaxy is excessively blue as might have been expected if this had happened .
The spectroscopic data are consistent with the two galaxies being interacting systems; the object is also an unusually bright X-ray source - perhaps because of the interaction. Both galaxies appear to be hydrogen rich, and Bothun et al. raise the question as to whether a violent encounter between two hydrogen-rich systems could have triggered the quasar activity in the brighter galaxy. Certainly this remarkable system merits further study. As these authors point out, if 0351+026 had been three times farther away, the two galaxies would never have been noticed and it would have been just another unresolved QSO; if this quasar had been only twice as far away, then the companion galaxy would just have looked like a faint star.
B. Galactic
1. A New Determination of the Space Density of Very Low Mass Stars (VLM Stars). Determining the space density of very low mass stars (those with a mass less than one-tenth that"of the sun) is an exceedingly difficult observational problem because these stars are intrinsically very faint (M > +15): they have less than one ten-thousandth the intrinsic brightness of the sun. These VLM stars are very important since their properties bear on a number of interesting problems: the physics of protostellar fragmentation, the determination of the minimum stellar mass that can sustain hydrogen burning, the composition of galactic nuclei and also the composition of the halo of our galaxy.
The best surveys of VLM stars up to now have come from proper motion surveys. These have suggested a peak in the luminosity function at about absolute magnitude M = +13.6, but these surveys are incomplete at M = +15 so the character of the luminosity function is ill defined at this limit .
The faintest known stars are secondaries of binary systems and these faint stars are cool and therefore red. Probst and O'Connell have therefore searched for VLM stars as the companions of white dwarfs (which are intrinsically faint bluish stars). If a white dwarf has a faint red companion, it will produce quite a strong effect in the infrared because the white dwarf itself is weak in this part of the spectrum. Probst and O'Connell have therefore carried out an infrared photometric survey at Cerro Tololo and Kitt Peak where they used the KPNO 1.3-m and 2.1-m telescope for JHK photometry.
The JHK photometry was used together with existing UBVRI photometry and an automatic spectral synthesis technique, to show that only 15 out of 107 white dwarfs had composite spectra. In 8 of these cases, the anomalous colors were thought to be produced by accretion disks and only in 7 cases could the
11-10 colors be interpreted as being due to a faint red companion. Most of these faint companions had an absolute M of +13 or brighter. Only one object was found to have an M fainter than +15, while the limit of the Survey was computed to be M = +20.7. The new survey therefore provides strong support for a sharp -de«iXne_in the luminosity function for stars fainter than M = +14. It is calculated, that the total mass density of stars with absolute luminosities in the range 16 < M <_ 21 is no more than 0.005 solar masses per cubic parsec in the solar neighborhood. It therefore seems unlikely that these VLM stars make a substantial contribution to the mass of either the disk or massive halo components of the Galaxy.
C. Solar System
1. High Altitude Haze on the Dark Side of Venus. Infrared heterodyne spectroscopy is a relatively new technique. In order to work, it needs bright sources (such as planets), but it allows remarkable high spectral resolutions (106 - 107) to be achieved. These resolutions are less than the Doppler line widths in planetary atmospheres where the temperatures are 200°K or less. At this spectral resolution one can analyse the lines in the spectra of these atmospheres in ways that are not possible with more conventional spectroscopy. Heterodyne detection work by a number of astronomers using Kitt Peak facilities has led in the past to the discovery of natural laser emission in the mesosphere of Mars, the discovery of the failure of local thermodynamic equilibrium near the surface of Mars and also studies of the winds in the atmosphere of Venus .
Carbon dioxide has spectral lines in the infrared. A. Betz, M. Johnson, R. McLaren and E. Sutton first observed these by heterodyne spectroscopy in the atmosphere of Venus in 1976. In this CO2 spectrum, a line such as the 10.33 micron R(8) line (with a low J value) was found to have a strong non thermal emission core whose intensity was roughly proportional to the incident solar flux. On the other hand, the non-thermal core was negligible in the 10.86 micron P(44) line which has a high J value. These lines have now been further investigated by D. Deming, F. Espenak, D. Jennings, T. Kostiuk and M. Mumma using the Goddard Space Flight Center infrared heterodyne spectrometer interfaced with the Kitt Peak McMath Solar telescope. They considered that if the non-thermal emission in the 10.33 micron flux is produced by the solar flux, then it should be absent on the dark unilluminated part of the disk of Venus. If the emission-core is absent, then the profiles of the absorption lines can be used to work out the temperature structure and cloud properties in the region about 70 km altitude in the Venusian atmosphere.
D. Deming et al. observed both the R(8) and P(44) lines on both the illuminated and unilluminated parts of the planet's disk. They made a detailed comparison of the profiles of these lines as they observed them with the profiles that they calculated from models of the planet's atmosphere. To make both sets of profiles agree, they deduced that there had to have been a significant amount of an absorbing haze (possibly sulphuric acid aerosols) on the dark side of the stratosphere of Venus.
2. Discovery of Carbon Monoxide on Titan. Titan is the most massive satellite of the planet Saturn. As long as astronomers had to rely on ground- based observations alone there was considerable controversy over the constitution of Titan's atmosphere. When the large amount of Voyager 1 & 2
11-11 data became available, prospects brightened for untangling the problem of this state. The bulk composition now appears to be 82% nitrogen, 6% methane and 12% Argon. The largest trace constituent is hydrogen at 2000 parts per million while other hydrocarbons contribute less than 45 parts per million.
These observations suggest that Titan's atmosphere formed from the outgassing of the ices and rocky material that were accreted during the process of formation of the planets, rather than that the atmosphere is a remnant of a proto-nebula from which Saturn was formed. In this outgassing evolutionary picture, all the original or primordial oxygen would have been trapped in water-ices in the form of clathrates* and as hydrates of nitrogen, methane and argon. Slight heating would occur (from gravitation and radioactivity) which would allow the frozen hydrates to melt so that the trapped gases could escape, but the trapped water would be retained in its liquid form deep within the mantle of the satellite.
Very recently, this outgassing-picture ("clathrate-hydrate" model) appeared less likely when a weak emission in the infrared spectrum of Titan near 667 cm (15 microns wavelength) was tentatively identified as the n2 fundamental band of carbon dioxide (CO^). The photochemistry of Titan's atmosphere implies that as much as 0.5% carbon monoxide (CO) would also have to be present with this CO2 if this identification is correct. The puzzle was that CO had never been detected in the atmosphere of Titan.
Now, using KPNO's Fourier Transform Spectrometer at the 4m Mayall telescope, Drs. Barry L. Lutz (Lowell Observatory), Catherine de Bergh (Observatoire de Meudon, France) and Tobias Owen (State University of New York at Stony Brook) have recorded a series of spectra of the outer planets and of Titan in the 1.6 micron wavelength region where the second overtone of the vibration spectrum of carbon monoxide (CO) occurs . These spectra included one of Titan obtained in an integration time of seven and a half hours at a resolution of about 1 cm-1. The signal-to-noise ratio is greater than 50 to 1 and a number of the rotational P- and R-branch lines of the 3-0 vibration spectrum of CO are shown unambiguously.
Before one can extract a meaningful CO mixing ratio for comparison with the CO2 observations, detailed model calculations are needed because of complexities such as the photochemical smog and various cloud levels in Titan's atmosphere: such calculations are being carried out. Meanwhile we can say that the new observed line absorptions are quite strong and certainly confirm the identification of CO2. This demonstrates the existence of a non- trivial amount of oxygen on Titan; this changes our concept of and provides new insights into the formation and evolution of its atmosphere.
*Clathrates are "addition-compounds" formed by the inclusion of molecules in cavities formed by crystal lattices or that are present in large molecules. Such substances are used in laboratories as molecular sieves to absorb or separate specific molecules.
11-12 KPNO STAFF RESEARCH HIGHLIGHTS
A. Extragalactic Astronomy
1. The S*ailar_Population in the Dwarf Elliptical Galaxy NGC 147. For many years astronomers have thought that the stellar populations of both globular clusters and elliptical galaxies were relatively straightforward. They thought that in each of these types of systems, there had been a large initial burst in which stars were formed with a range of masses, and that, following this, little gas remained in these systems from which any later generations of stars could be produced. The subsequent history was simply that of the evolution of the individual stars - the evolution being faster for the more massive stars . The main differences between such systems were thought to be due to differences in the chemical compositions of their constituent stars (particularly the metal abundance) and in the total numbers of stars in each system.
Recently, it has been found that some globular clusters and the faintest dwarf elliptical galaxies appear to have more than one generation of stars present; they also have a spread in the chemical compositions of their giant stars. It is clearly of interest to see if such effects are also present in larger and brighter ellipticals but the only galaxies of this type that we know of are at such great distances that it is currently impossible to investigate their individual stars. NGC 147 is a dwarf elliptical galaxy that is thought to be a companion of the giant Andromeda spiral (Messier 31 or M31) - it lies 7 degrees away from it in the sky - and with a blue absolute magnitude of -14.5 is a much more luminous system than any of the globular clusters or dwarf elliptical galaxies associated with our own Galaxy. A color-magnitude diagram has now been determined for NGC 147 by Dr. J. R. Mould (Kitt Peak National Observatory), Dr. J. Kristian (Mount Wilson and Las Companas Observatories) and Dr. G. S. Da Costa (Yale University Observatory). They used an 800 x 800 format Texas Instruments CCD at the prime focus of the Kitt Peak 4-m telescope during November 1981 (using the new Kitt Peak Prime Focus Guider [now at CTIO]) to obtain high-quality calibrated pictures of NGC 147 in the visual (V), red (R) and infrared (I) colors. This digital data was processed on the Kitt Peak Interactive Picture Processing System (IPPS) to give R magnitudes and V - R and V - I colors of some 400 stars in a field on the edge of NGC 147 (the center of the galaxy being too crowded for analysis). An interesting part of their analysis consisted in measuring 400 artificial stars that were inserted into the data so that the measuring accuracy could be estimated.
Mould, Kristian and Da Costa found that the stellar population of NGC 147 resembles that of one of the globular clusters in our own Galaxy. If it is assumed that it is indeed at a distance of M31, then a metal-to-hydrogen ratio [M/H] = -1.2 ±0.2 is deduced. This is in fair agreement with that expected from the loose correlation that is thought to exist between the metal abundance and the total brightness of the system. On the basis of their careful evaluation of their photometric errors, Mould et al. conclude that there is a spread in the colors of the giant stars at a given magnitude (i.e., there is a "broad giant branch") which they interpret as a dispersion in metallicity of 0.3 dex for the stars in their field. However the absence of an extended giant branch in NGC 147 implies that less than 10% of the stars in NGC 147 sampled in this program were formed more recently than 12 billion
11-13 years ago. Mould et al. point out that their investigation of the outer parts of NGC 147 does not show evidence of star formation from the gas that is expected to be lost from dying stars . They conjecture that the gas may possibly escape from the system (the escape velocity is low) or it may aggregate in tfrtu center. ~of the galaxy. They suggest that a search for upper asymptotic giant branch stars in the central part of this galaxy would be interesting: it clearly would not be easy.
2. A Study of Low Surface Brightness Galaxies. Although in the past it has been proposed that all spiral galaxies have about the same surface brightness at their centers (21.6 B magnitudes per square second of arc) astronomers have found in recent years that there exist spiral galaxies with significantly lower surface brightness than this. A sample of sixteen of these low-surface-brightness (LSB) spirals has recently been studied at Kitt Peak by Drs. W. Romanishin (Goddard Space Flight Center), K. Strom and S. E. Strom (Kitt Peak National Observatory). They used the prime focus of the 4-m Mayall reflector to take plates from which the surface brightness distributions of these galaxies could be determined in detail. They were then able to calculate a variety of parameters for each galaxy such as the central surface brightness, the scale length (a measure of the compactness of the galaxy), disk-to-bulge ratios (which measure the shape of the galaxy and relate to its stellar content), and isophotal diameters. These last named are the sizes of the galaxies out to a specified surface brightness.
In the first place, it was found that these LSB galaxies were about a factor of three fainter at their centers than the standard surface brightness for spiral galaxies that had been proposed earlier. The scale lengths (averaging some 3 kpc) overlap with those of the brighter galaxies and agree with the previous idea that galaxies of later Hubble type (smaller bulge-to- disk ratios) have smaller scale lengths.
At a given absolute magnitude (the intrinsic brightness of the total light of the galaxy), these LSB spirals were found to be 1.5 times larger than normal spirals such as those found in the nearby Virgo cluster. Putting this another way, the LSB spirals were 1.1 magnitudes fainter (i.e., a factor of 0.36 in surface brightness) at their centers as normal spirals of the same radius. It is of interest to note that this work involved tracing out these faint galaxies to a surface brightness of about 29 B magnitudes per square second of arc or about one quarter of one per cent of the brightness of the dark night sky.
Romanishin et al. also obtained visible and infrared photometry of these LSB galaxies, and discovered the interesting fact that they are significantly bluer in the infrared than normal luminous spiral galaxies . Spectra of some of the HII regions (line-emitting gas surrounding hot stars) showed significant differences from those in normal spirals . The implication is that the star formation rate, initial mass function, and chemical abundances may be different in these LSB galaxies. A more detailed analysis that uses these data to investigate these matters is to appear in the future.
3. A New Distance to Messier 101. Messier 101 (M101) is the nearest giant spiral of the type known as Sc I. It is actually about 5 Megaparsecs (16 million light years) distant, but this is near enough for us to be able to distinguish some of the brightest individual stars in its spiral arms with
11-14 photographs taken with the largest telescopes . If we compare the apparent brightness of such stars with their known absolute brightness, we can calculate their distance. M101 is particularly important because it is sufficiently far away to have an appreciable redshift from the expansion of the Universe. —•'Hae rate -at which the redshift increases with distance (the Hubble constant) is extremely important to cosmologists because the redshift is essentially the only available distance indicator for distant galaxies. Astronomers are concerned about the correct value of the Hubble constant; hence any new information that can help in estimating its value is of great interest.
In recent years, the stars called M supergiants have become recognized as important distance indicators because the brightest of them in any galaxy always have the same brightness (absolute visual magnitude M = -8.0): this is about 135,000 times brighter than our Sun so it will be appreciated that they can be picked out as individual objects at great distances. Dr. Roberta Humphreys (University of Minnesota) has pioneered the study of these stars as distance indicators and now, in collaboration with Dr. S. E. Strom (Kitt Peak National Observatory), has discovered them in M101. These astronomers took a number of plates of M101 using the prime focus camera of the Kitt Peak 4-m telescope. The plates were sensitized and filtered so that they detected different regions of the spectrum from the green through the near infrared. A comparison of these plates then enabled them to pick out the red M supergiants in the spiral arms of M101.
The comparison and analysis of the plates was achieved by first scanning them with the Kitt Peak PDS microdensitometer; this measures the blackening at each point on the plate (which is roughly proportional to the amount of light received) and converts it into a number that can be processed by a computer. The computer programs are used to convert the plate blackening to true star brightnesses and measure the colors of the stars so that the red ones can be selected. The M supergiants were expected to be in the spiral arms of M101, and this enabled them to be distinguished from red foreground stars; 93 M supergiant candidates were picked out by this technique. An analysis of the brightness distribution of these candidates shows that there is a significant increase in numbers of these stars at an apparent magnitude V = 20.9. This must be the brightness of the brightest M supergiant - and so knowing their absolute brightness, the distance of M101 was deduced.
The new distance - 5.25 Megaparsecs - is somewhat smaller than previous estimates based on the brightest blue stars and on the sizes of ionized gas regions (known as H II regions). With this new distance the visual brightness of M101 becomes M = -20.9 and the local value of the Hubble constant (based v _ i _i on the M101 group of galaxies) is 76 (+4, -6) km s Mpc .
B. Galactic Astronomy
1. Probing the Atmospheres of Giant Red Variable Stars in the Infrared. The Mira variables are huge, cool, giant stars whose radii are hundreds of times greater than that of the sun - if our sun were a Mira, the earth's orbit would be inside its atmosphere. They vary with well-defined periods of the order of several hundred days . At their brightest (maximum light) their light in the blue part of the spectrum (where conventional photographic spectra were mostly taken) is often over a hundred times brighter
11-15 than when they are at their faintest (minimum light). The spectra in the blue showed emission lines that occurred near maximum and which had velocity shifts that were consistent with the idea that the whole star was pulsating. Absorption lines in these spectra, however, failed to show the velocity changes that wattld have __been expected on such a model. A powerful probe of the atmospheres of cool stars are the vibration-rotation bands of the molecule CO in the infrared. Mira stars, being cool, are bright in the infrared and their infrared light amplitude is much smaller than in the visible. In fact, they are bright enough in the infrared to be observed at all phases in either day or night at high resolution with the Fourier Transform Spectrometer (FTS) at the Kitt Peak 4-m telescope.
K. Hinkle (KPNO), D. Hall (now at STScI), and S. Ridgway (KPNO) have just analysed an extensive (3 year) series of such observations of the Mira star x Cygni which has a period of 407 days . Their analysis gives detailed information about the photospheric kinematics and the energy balance associated with the optical variability. They also throw light on the complex circumstellar envelope that had previously been revealed by microwave observations. The new observations can be fitted to a picture consistent with both the optical and the microwave data.
It is found that the atmospheric structure of x Cygni is governed by a general stellar pulsation which propagates through the stellar photosphere just before and during maximum light. A shock front forms between the material being accelerated out by this wave and the material falling back in from the previous cycle. At this shock interface, the gas is heated and the molecules are dissociated; here the hydrogen is ionized and emission lines are produced. After the shock has propagated through the photosphere some two months after maximum, the material is uniformly accelerated inwards while it cools monotonically. The analysis shows that the stellar radius and the distance through the atmospheric layer where the infrared CO lines are formed are both about 250 R~. This makes x Cygni very extended and transparent compared to the sun—its radius is 1 R. (by definition) and its photosphere is about .001 R«. The stellar pulsation produces variations in radius of about ± 100 Rg. There is a stationary layer at a temperature of 800° K at a distance of about 10 R above the photosphere that dominates these circumstellar regions. In x Cygni, this layer was built up rapidly in 1975 and then diminished steadily over the next three pulsation cycles . During this interval, the layer appears to have acted as a reservoir both for material accelerated outwards (presumably by the pressure of the radiation on condensing dust) and for the material which may be draining back below it down to the photosphere. The various optical absorption lines arise in these two regimes associated with this stationary layer while the maser features (discovered by the microwave observations) are likely to originate in the outer boundary of this layer. The authors suggest that it will be interesting to look for correlations of the behaviour of this layer with the maser characteristics.
C. Solar System Astronomy
1. The Recovery of Halley's Comet. Last seen 71 years ago by Heber D. Curtis at Lick Observatory, Halley's comet was recovered on October 16, 1982 by D. C. Jewitt and G. E. Danielson (Cal Tech) using the 5m Hale telescope at a V magnitude of 24.2. The recovery was confirmed at Kitt Peak in observations
11-16 scheduled for the purpose of finding Halley on October 18 and October 20 by M. J. S. Belton and H. Butcher (Kitt Peak National Observatory) using the Cryogenic Camera on the 4m Mayall telescope. The recovery culminates a five- year search for the comet (the first attempts at KPNO to recover the comet were made in LftiZO,_and_begins a scientific program of observations that is expected to continue to 1989/1990. The recovery brightness is roughly 8 1/2 magnitudes fainter than was achieved at the recovery by Max Wolf in 1910. This factor is a direct measure of how the power of astronomical equipment has increased in modern times—a factor of 2.5 x 103!
There seems no doubt at the present that it is the nucleus of the comet, devoid of coma, that is being observed, and the current KPNO program (new observations were obtained at KPNO December 12, 1982) will concentrate on measuring its global properties, i.e., size, rotation, and color (the latter as an indication of surface chemistry). This is probably the first time that the nucleus of an active comet has ever been observed, and an important aspect of the ongoing program will be to watch for, and follow, this rise of atmospheric activity. This atmospheric "turn-on," which should be relatively abrupt, is not expected to occur until late 1984—but then again, comets are well known for surprising astronomers!
Belton and Butcher have re-evaluated physical models of Halley's nucleus in a paper recently published [Nature, 298, 249-251, (1982)] based on a limiting magnitude set at KPNO in December 1981 and modern analyses of the 1910 data, the optimum model plus the 1982 recovery magnitude indicate a nucleus roughly 4 km across with a visual albedo of about 22%.
2. Detection of Solar Flares When The Sun Is Observed As A Star. Solar flares are eruptions in the chromosphere of the Sun and as such are symptoms of solar magnetic activity. The strongest solar flares are associated with the ejection of particles from the Sun which can cause magnetic storms in the Earth's ionosphere severe enough to produce aurorae and disrupt radio communications. Most commonly, flares can only be seen as brightness enhancements in pictures of the disk of the Sun that are taken in the light of the strong chromospheric emission lines such as the Ha line of hydrogen or the K-line of ionized calcium. On rare occasions flares are powerful enough to be seen in white light. The Sun is of course a star, and it would be interesting to know whether other G-type stars like the Sun have the same kind of magnetic activity that produces flares. Unfortunately we can only observe the integrated light from the whole disk of a star: they are far too distant for us to be able to resolve surface with the equivalent of a spectroheliogram.
Recently Dr. W. C. Livingston (Kitt Peak National Observatory) and Dr. B. Ye (Yunnan Observatory, People's Republic of China and Visiting Astronomer at KPNO) have shown that it is possible to detect solar flares in the integrated (whole disk) light of the Sun. In an observatory laboratory in Tucson, they feed unfocused sunlight into an instrument called a K-index spectrometer. This is a high-dispersion spectrograph with two channels of detectors: light from a 1 Angstrom window centered on the ionized calcium K-line is fed to one photomultiplier tube, and light from a 0.1 Angstrom continuum window twenty Angstroms to the red is fed to another. The ratio of the two photomultiplier output signals is proportional to the K-index (i.e., the emission component of the calcium K-line). Daily observations have been made since September 1980, and two strong flares as well as numerous lesser events have been detected.
11-17 Could these flares be detected in the nearest solar-type stars? According to the known solar statistics of flare frequency, it would just be marginally possible to detect them with existing telescopes . The brightest flares could be detected, but these occur rather rarely (about once in every 500 hours) and—*££h_normal allocations of telescope time on large telescopes, one would be very lucky to catch a giant flare unless they occur much more frequently on other G stars than on the Sun. Less bright flares (that occur more frequently) would be too weak to be picked up with say a 1.5-m telescope. Livingston and Ye point out that a 15-m telescope could collect enough light for one to detect these faint, more numerous flares and suggest that the pursuit of these stellar flares in G-type stars may have to await such a telescope. Only then may we know whether or not the Sun is unique among G-dwarfs in terms of its 11-year activity cycle and the amplitude of underlying magnetic modulation that gives rise to it.
11-18 III. SCIENTIFIC PROJECTS AND PROGRAMS
Highlights of the FY1984 Program
FY1984 represents a major step forward in funding and activity for the 15 meter National New Technology Telescope (NNTT) Program at KPNO. It will be a year of transition from concept and feasibility studies to a full-fledged telescope design project. A Scientific Advisory Committee (SAC), established in FY1983, will have the task of reviewing the scientific and technical tradeoffs between the two competing concepts and making the recommendation on concept selection in mid-FY1984. Major efforts at concept evaluation will be carried out at KPNO and at the collaborating institutions: the Universities of Arizona and California. Following the concept selection, work will turn toward detailed design of the telescope. There will be a major increment in the activity related to the fabrication and polishing of the primary mirror for the selected concept. In addition, a site testing and selection program initiated in late FY1983 will be in full swing. The details of the NNTT Program plan of work for FY1984 are given in Section VI and in Appendix 5.
CTIO's instrumentation projects place the highest emphasis on obtaining the most powerful detector systems currently available. In the infrared, a joint effort with KPNO, begun in FY1983, to implement a working solid state infrared array for imaging and spectroscopy will continue in FY1984. Work with optical detectors, begun in FY1983, to obtain two-dimensional pulse- counting systems to succeed the SLT vidicons currently in use and to obtain large format CCDs to improve on the ones currently available will have high priority in FY1984. Related projects include the acquisition of new cameras and the adaptation of existing ones for optimal utilization of the new detectors. A new high-efficiency spectrometer is planned for the 4m prime focus for the same reason. Additional projects and the plans for improving the telescopes and computing equipment so that they will permit full use of the new instruments are described in the accompanying text .
Unfortunately, the reduced funds available for Revision 1 will slow substantially the instrumentation effort . It will not be possible to obtain the imaging Fabry-Perot originally planned, which would have been an extremely powerful device for mapping velocity fields and emission line objects . Plans were that a single instrument would be purchased and shared by CTIO and KPNO. An additional impact will be a substantial slowing of the effort to obtain large-format CCDs from British GEC. If additional funds can later be obtained, these projects should be restored to the Program Plan.
In addition to collaborative efforts with CTIO to procure and implement infrared detector arrays, KPNO is vigorously pursuing the deployment of two- dimensional photon-counting detectors for low and medium dispersion spectroscopy. The first of these systems will be put into service near the end of FY1984. KPNO will also continue the implementation of CCD detectors and related instrumentation, a program that was started in FY1980. Unfortunately the replacement of the Varian computer systems on the mountain will be delayed and the development of the Image Reduction and Analysis Facility (IRAF) will be slowed considerably in FY1984 due to the reduction in funding. A number of upgrades to existing facilities as well as the continuation of the seeing studies program begun in FY1983 are also planned.
III-l Rev. 1, 11/18/83 In March 1983, CTIO held its first meeting with representatives of the user community and experts in telescope design and technology to begin planning for the new telescope project. Several years ago CTIO envisioned a 2.5m telescope, but the project never advanced because of the tight funding situation. In The"meantime the demand for more light gathering power has increased and the technology for building large telescopes has advanced. Therefore, CTIO's intention is to take advantage of recent developments related to the NNTT to build a significantly larger telescope that will help the Observatory keep up with the anticipated pressure from projects such as IRAS and Space Telescope. A 3-5m class telescope optimized for the infrared will increase CTIO's capacity for many optical applications. The project description for the telescope is included below.
Work on the telescope project will also be greatly slowed by the reduction of funds for Revision 1 of the Program Plan. It will not be possible to make a detailed study of the telescope tube structure as had been planned originally. CTIO will be limited to obtaining updated cost estimates for the various components of the telescope and to the initial parts of a site survey to investigate locations on Tololo and Morado.
SCIENTIFIC PROJECTS (CTIO) $1,253K
Salaries $420K Infrared Instrumentation $152K Optical Detectors and Instrumentation $331K Small Telescope Improvement Projects $238K Visual Photometers $ 5K Telescope Project $107K
Infrared Instrumentation
In FY1983 the major infrared efforts were devoted to the mechanical and electronic fabrication of the cooled grating spectrometer, to beginning work on a new photometer for the 4m telescope, and to initiating efforts towards obtaining a new infrared array. These projects will continue in FY1984 and will be the major part of the infrared efforts. However, if the infrared array project is not bearing fruit, funds will be diverted to the construction of an infrared Fabry-Perot spectrometer which can be used with a single- channel detector. In addition, a device to measure radial velocities in the infrared, along the lines of that developed by Gunn and Griffin for the optical, will be considered. This can be a relatively simple device and will be used at the 1.5m Coude Spectrograph.
Optical Detectors and Instrumentation
We plan to obtain in FY1984 a large (1500 x 1500) GEC CCD, following work initiated in FY1983. This will be a 38mm-square device offering 25 micron resolution, 10 to 20 electron readout noise, and averaging 30% quantum efficiency in the 5000-10000A spectral region. This is the ideal format for spectroscopy and would be a natural complement to existing or projected detectors having about 20% quantum efficiency in the blue. Because of their large size and excellent cosmetic properties, these chips will also be very useful for Cassegrain direct work.
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In a continuing effort to modernize the existing small telescopes at CTIO, the following projects are planned: A new mount is needed for the secondary mirror of the' 1m telescope, since the present one offers only crude adjustments and has very poor long-term stability. The telescope must be realigned every few weeks. Because the lm and Schmidt telescopes have no automated systems at present, we will obtain two manually operated autoguiders, probably from outside sources. Depending on the outcome of test results for solving the image shift problem in the Curtis Schmidt telescope, it may be necessary to obtain a new support system for the primary mirror, including an airbag, pressure controller, and mercury edgeband. For the 1.5m telescope, the guider planned for FY1983 should be upgraded to provide autoguiding capabilities. Further interference filters will also be required for use with the CCD direct imaging systems on these telescopes .
Additional equipment required for the small telescopes includes another TV guiding system for the acquisition and observation of faint objects. A program of dome-seeing studies and improvements to all the CTIO telescopes is being undertaken. It will make use of an infrared TV camera the value of which has been demonstrated at the Steward and MMT observatories .
Telescope Project
In FY1983, a preliminary design study was reviewed at a special March meeting of CTIO users, CTIO staff, and a group of engineering experts at Tololo. The conclusion was that a 5m reflector can probably be achieved for under $10M pending further detailed design studies.
In FY1984 CTIO plans to work towards finalizing the design of such an optical/infrared telescope. This new instrument is needed right away. The role of large-aperture ground-based telescopes in the southern hemisphere will become even more critical because of the central part they will play in following up observations from orbiting telescopes of the Galactic Center and the Magellanic Clouds . The existing CTIO 4m telescope will not be adequate because it will not offer enough observing time and will not reach faint enough.
The new telescope will have an altitude-azimuth mounting and rotatable building patterned closely after the MMT, but will employ a monolithic lightweight primary mirror. In FY1984, CTIO plans to carry out the following phases of the project:
a. Send out the drawings of the MMT mount and building for bids from several contractors .
b. Study the 4m aluminizing facility on Tololo to see if costs can be saved by using existing pumps and electronics.
c. Finalize the optical design for optical and IR Cassegrain foci.
d. Study Tololo and Morado for optimal sites using microthermal towers.
e. Look for a backup mirror blank in the event a lightweight mirror
II1-4 Rev. 1, 11/18/83 cannot be obtained. The availability of conventional or lightweight mirrors in the 3-5m range will be explored.
SCIENTIFIC PROJECTS (KPNO) $1,256K
New initiatives $528K Optical Detector Implementation S154K Infrared Instrumentation $126K Telescope & Instrument Improvements $198K Computers $250K
New Initiatives
Studies toward the implementation of photon counting detectors were initiated in 1982. The intended use of these devices is for speckle imaging and moderate-to-high resolution spectroscopy (1000 < R < 10000) for the study of the structure and velocity fields of the outer atmospheres and shells around bright supergiants and nearby galactic nuclei. Thus far, we have used G. Timothy's multi-anode-microchannel-array (MAMA) detector at the 4m telescope in both linear and rectangular formats . Testing of the MAMA detector will continue during FY1984. This detector has the advantage that photon events are time-tagged with the high temporal resolution required for speckle work.
During FY1983 other photon counting systems were also studied. The result of that study was that it has been decided to implement a photon counting system utilizing an intensified CCD. This system will be based on a concept developed at the Carnegie Institution of Washington. The system will utilize the KPNO CCD Controller/Display system for data acquisition and "quick look" data reduction. The hardware will be constructed during FY1984 with the first engineering runs scheduled for the Fall of 1984. Regularly scheduled use with the 4 Meter R-C Spectrograph is planned for the Spring of 1985. The spectral range will be from 3200 to ~7000 A with resolutions varying from 1 to 10 A. The time resolution of this concept is somewhat lower than that of the MAMA. However, this concept has the advantage of being fully proven and thus its implementation will be a straightforward endeavor.
A third concept of a photon counting detector system will be studied during FY1984. This system, originally developed by Papaliolios and Mertz, utilizes a set of photomultiplier tubes behind an arrangement of encoding optical masks. This concept, if proven, will be capable of higher photon flux rates and greater time resolution than frame-read devices such as the IPCS. The FY1984 effort on this project will be primarily of an investigative nature with little hardware development beyond the construction of the optical masks. It is planned that most of the special electronic hardware developed for the IPCS would be utilized with this device.
Efficient utilization of such UV responsive detectors will require the construction of a new fast UV camera for the 4m R-C spectrograph. Such a camera would also be useful at this spectrograph and at the echelle spectrograph with existing un-intensified CCD detectors. A conceptual design study will be undertaken during FY1984 with construction planned for FY1985.
During FY1983 KPNO began a major effort directed toward the understanding of seeing phenomena and the determination of methods of image reconstruction.
III-5 Rev. 1, 11/18/83 This work will be continued during FY1984. The objectives of this activity include the development of techniques which will be applicable to the NNTT as well as to the near term improvement of the imaging properties of the 4m telescope.
A small-scale effort toward the study and implementation of interactive remote observing was begun during FY1981. Since that time, remote observations have been carried out with a number of KPNO instruments and telescopes, with the observers as far away as Great Britain. A total of 29 observing runs, utilizing eight different instruments at five telescopes, have taken place. In addition, a number of remote data reduction runs have been carried out. Remote observing runs and remote data reduction are now regularly scheduled. We plan to continue the remote observing studies during FY1984. The major thrust of the work during this year will be investigation of data compression algorithms and hardware with the objective of implementing high picture transmission rates . The overall goal of the remote observing program has been preparation for the use of the 15 meter NNTT which is quite likely to be located at a very remote site.
Optical Detector Implementation
The implementation of CCD detectors at Kitt Peak and Cerro Tololo telescopes has been the major thrust of the Instrument Systems Program since 1980. At the end of FY1983, the following detector systems were in service: CTIO 4m telescope (prime focus), KPNO 4m telescope (prime focus, echelle spectrograph, R-C spectrograph cryogenic camera, and R-C spectrograph intensified CCD), 2.1m telescope and Coude Feed (coude spectrograph) and #1- 0.9m telescope (cassegrain direct camera). Five CCD data acquisition systems plus four CCD data acquisition display systems are in service (one on Cerro Tololo, three on Kitt Peak, plus a laboratory development system). These instruments have become the work horses of KPNO. During FY1983, with two data acquisition systems available on Kitt Peak, 444 nights of CCD observations were scheduled. The addition of the third data acquisition system at the end of FY1983 has eliminated scheduling constraints, and usage during FY1984 is expected to increase.
During FY1984 we plan to continue this program of CCD detector implementation by completing the fabrication of replacements of equipment transferred to CTIO in FY1982 and implementation of a Texas Instruments Virtual Phase CCD in a Universal Dewar for use with all CCD instruments except the Cryogenic Camera.
Design and construction of an improved version of the 4m telescope prime focus CCD optical/mechanical interface, which was transferred to CTIO in FY1982, was begun during FY1983. The original plan of utilizing the prototype equipment at KPNO was found to be deficient. The new system will incorporate improved focusing hardware plus the drift-scan calibration technique developed by C. McKay. This project was partially finished at the end of FY1983 and will be completed midway through FY1984.
During FY1984 the Detector R&D Program will test a Texas Instrument CCD constructed of the new virtual phase technology. If this device proves to be satisfactory, it will be implemented in a new KPNO Universal Dewar for use with all CCD instruments except the Cryogenic Camera. This device, which has
II1-6 Rev. 1, 11/18/83 an 800 x 800 format, has the potential for lower read noise than the existing RCA detectors and, because of smaller pixels, higher spatial and spectral resolution when used with existing cameras.
Infrared Instrumentation
During FY1984 we plan to complete the project to replace the chopping secondary on the 2.1m telescope. This project, which was begun in late FY1982, will produce a 2-axis system with high positioning accuracy. During FY1983 a linear indium antimonide detector array was implemented in a prototype cryogenic spectrometer. This instrument is serving as a testbed for spectroscopic infrared arrays . This testing program will continue through FY1984 and when a high performance array has been found, it will be implemented in a user-class spectrometer.
Telescope & Instrument Improvements
The major planned improvement project during FY1984 will be an upgrade of the #2-0.9m telescope to implement the addition of an f/7.5 optical system. The availability of the CCD direct camera at the #1-0.9m telescope has generated an over-subscription of the dark time by a factor of three. Addition of the f/7.5 optical system at the #2-0.9m telescope will permit simultaneous scheduling of the IRS and the CCD direct camera. This work will also prepare the telescope for use with the planned CCD spectrophotometer.
New gratings are also scheduled for FY1984. These include a 790 line/mm 8000 A ruling for the 4 Meter R-C Spectrograph plus an echelle optimized for use with CCDs. Upgrade of the ruling engine will also continue.
Computers
The conversion of computers used for telescope control and data acquisition on the mountain and the replacement of the Interactive Picture Processing System (IPPS) and the batch downtown computer system continue to be high priority tasks. All three of these projects have been impacted by the recent budget reduction. We anticipate that Digital Equipment Corporation (DEC) will soon announce the release of their new "super-VAX," the computer in the DEC series most likely to replace the CYBER. Present funding levels will not permit us to commit approximately 3450,000 of FY1984 funds to replace the CYBER computer. The CYBER will continue to limit effective interactive computing at KPNO. Other effects of the budget reduction include delaying the implementation of new control and data acquisition computers on the mountain and the continuation of the use of inefficient data reduction procedures by visiting users .
Mountain Computers: The 12-year-old Varian computers are being replaced with the PDP line of DEC computers. During FY1983 the full conversion of the 2.1m and 4m telescopes to DEC computer systems was completed. Since it is possible to transport much of the software directly to the smaller telescopes, more than half the software conversion effort has also been completed.
During FY1984 we planned to complete the hardware and software conversions at the 1.3m and at the two 0.9m telescopes thereby completing the conversion of the KPNO nighttime facilities. However, because of the recent
III-7 Rev. 1, 11/18/83 reduction in funding, the conversion of the 0.9m telescopes will be delayed until FY1985. The subtle costs associated with yet another year of maintaining two different sets of hardware and software are not easy to determine but will certainly result in diminished resources available in other areas .
The capability to do data reduction has been part of the mountain computer plan since its inception. In order to ensure that the same reduction software will run in town and on the mountain, DEC computers have been implemented in both locations. During FY1984 we planned to construct a data reduction facility on Kitt Peak. This facility would initially house a small VAX computer for data reduction. In later years, after a high band-width link to the Tucson facility has been implemented, the facility would be a reduction center for observers using computers located in Tucson. As a result of the recent budget reduction, this facility has been removed from the plan. Thus, visiting scientists will continue to be required to extend their stay away from their home institutions to reduce data in Tucson.
Downtown Computers: An Image Reduction and Analysis Facility (IRAF) is being developed to replace the old Interactive Picture Processing System (IPPS) and to meet the greatly increased demand for computing facilities created by the new digital detectors . The IRAF software system is being written with the specific goal that it be transportable to other astronomical institutions. Portions of the basic system were released in late FY1983. The first four major applications packages will be available in FY1984. The system will be installed at CTIO in FY1984 and possibly at other sites in the astronomical community. During FY1984 another IRAF satellite computer, ordered in mid-FY1983, will be delivered and installed. It was planned that this system be upgraded in FY1984 to include a display unit. However, the recent budget cut has made that upgrade quite unlikely for FY1984.
Cyber Replacement and VAX Operations. Unfortunately the November 1983 budget reduction will complicate planning for replacing the Cyber computer and increasing VAX computer operations. The Cyber 170/720 computer system in Tucson serves two purposes. First it serves as a batch data reduction and analysis system for the entire observatory and second it runs the IPPS system, along with the Varian V74. The Cyber system, despite its large computing capability, is becoming a hindrance in fulfilling the computing requirements of the observatory. The hardware is leased from Control Data Corporation for a combined leasing and maintenance cost of S210,000 per year. Despite the "number crunching" capability, this is a high fee to pay just for leasing the system. Furthermore, the architecture of the system is archaic and 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 should replace the Cyber with a system that is more compatible with other data collection and data reduction systems at the Observatory and throughout the national and international community. Simply using the lease costs alone, we could purchase several VAX-class machines per year and give KPNO far more computing resources than is currently available with the Cyber. Based on the estimated time required for conversion of software, the Cyber lease was extended until December 1984.
Until about a year ago, it was assumed the IRAF host and the Cyber replacement computers would be independent systems. Since then it has become
III-8 Rev. 1, 11/18/83 apparent that, with the decreasing price of computer technology, it is possible to obtain both functions in a single machine at the price originally estimated for the IRAF host alone. It is expected, for both software portability and hardware portability, that the Cyber replacement will be the same architecture as the IRAF, i.e. a VAX-11. This will provide a uniform architecture for both software and hardware throughout the observatory. This concept offers tremendous simplification and unification of the KPNO computer plan.
The specific computer under consideration is the "super-VAX." Digital Equipment Corporation has provided, under a non-disclosure agreement, some details of performance, cost, and probable availability. Based on this discussion, and on communication with theoreticians who have considerable VAX 11/780 experience, we estimate that the super-VAX will be 4-8 times as capable as the Cyber for typical astrophysical computations. Equally important, numerous expansions, such as very large memory, large disks, array processors, bulk storage media, etc., will be available from numerous sources, while with the Cyber they are either unavailable or extraordinarily expensive.
As a result of this merging of IRAF host and Cyber replacement, the distinction between IRAF and other observatory computing becomes substantially blurred.
Well before the removal of the Cyber, we must stop all new development of programs on the Cyber and must provide other computing facilities to allow staff members to start converting their programs from the Cyber. In order to do this, a VAX-11/750 has been purchased and will be used as a general purpose data reduction machine. This process is well underway, as several major reduction facilities have been moved to this computer, and it is under intensive use. This system will slowly grow as more and more programs migrate from the Cyber to it. The memory, disk and other peripherals will be steadily upgraded until the Cyber replacement is available.
In addition, interim use of the Tucson 11/44 has drawn a substantial share of the transitional computer load. As described in the Mountain Hardware plan, we intend to delay the implementation of a mountain host to provide an 11/750 to take over the 11/44 burden in Tucson at least until the Cyber replacement becomes available. In a climate of uncertain funding levels, it is difficult to establish methodology to cope with increased and changing demands for computational facilities at the observatory. However, the needs discussed above must be addressed to avoid a bottleneck in scientific data processing.
Finally, a peripheral aspect of the implementation of VAX computers and the UNIX operating system at KPNO has been the remarkably rapid spread of computer usage. A number of general purpose capabilities, such as data base management and text manipulation, which were available in a limited fashion previously, are now in widespread use in all areas of the observatory. The major problem in supporting this usage, which is not very demanding on cpu cycles, is in providing the terminals and terminal connections. Much of this has been done, but a number of requirements remain to be filled.
Networking of computers is becoming a cost-effective way of minimizing duplication of computers and peripherals. It is likely that some form of
III-9 Rev. 1, 11/18/83 networking will be implemented on the mountain- and in Tucson, possibly with a connecting link, in FY1984.
SOLAR PROJECTS (NSO) $35K
A portion of" the scientific project budget has been assigned for support of the new scientific projects of the KPNO Solar Program staff. A description of these projects is included in the National Solar Observatory Program Plan.
SPECIAL PROGRAMS (KPNO) $540K
Gratings Laboratory $ 63K Coatings Laboratory $ 68K Detector R&D $378K Visitor Program-Foreign Telescopes $ 30K Dark Sky Site Survey $ IK
Gratings Laboratory
The KPNO Gratings Laboratory provides large ruled diffraction gratings to the AURA Observatories and to the general astronomical community. The Harrison C Ruling Engine, obtained from MIT in 1973, has a maximum capacity of 400 mm ruled length and 600 mm ruled width, making it the largest of its type in the U.S. The engine is operated as a national facility in that rulings are performed for other institutions on a cost reimbursement basis. An archival submaster is made from each successful ruling. Replicas made from these submasters are available to the astronomical community on a cost reimbursement basis .
During FY1983 the Gratings Lab produced a 200-line-per-millimeter ruling for the CTIO 4m telescope R-C spectrograph and a cross-disperser for the KPNO 4m telescope echelle spectrograph. A new echelle will be ruled in FY1984 after a major upgrade of the ruling engine has been completed. The planned FY1984 rulings also include three for the KPNO 4m telescope R-C spectrograph and possibly a CCD optimized ruling for the 2.1m telescope coude spectrograph.
Coatings Laboratory
The KPNO Coatings Laboratory has the capability of performing high uniformity, multi-layer, vacuum-deposited coatings on substrates up to 2 meters in diameter. Four coating chambers are operated in support of KPNO O&M and project activities. In addition, coating services are provided to other institutions on a cost-reimbursement basis . One of the major activities of the Coatings Laboratory is associated with providing master blank coatings for the Gratings Laboratory.
Detector R&D
The major efforts of the detector R&D group in FY1984 will be directed towards the evaluation of new IR and visible array detectors as they become available to us. Work during FY1982 and 1983 has not led to an obvious IR array candidate for implementation in a common user instrument. The cryogenic IR array spectrometer is, however, now ready for mountain use as a testbed for the arrays, and at the very least will be used with one or more of the
111-10 Rev. 1, 11/18/83 available devices during FY1984 to try to define the science which can be done with the current state of technology.
In FY1984_, a somewhat greater emphasis will be placed specifically on the IR array work." "Potentially important devices to be studied include the Schottky barrier chips for work below 2.5 microns, and the Si: In photoconductor hybrid CCD and Si :Bi CID's for longer wavelengths. During FY1983 a reticon-scanned indium-antinimide array was purchased by CTIO for evaluation by the KPNO R&D Program. This array will be delivered in late FY1983 or very early FY1984. In addition, KPNO and CTIO have jointly funded a request for proposal to obtain special infrared arrays optimized for astronomical use. The responses to this RFP will arrive in early FY1984 with the actual arrays expected to be delivered in mid-FY1984. As soon as a satisfactory IR array detector is identified, it will be made available for scientific use at both KPNO and CTIO.
Efforts will continue to evaluate new CCD arrays for the visible wavelengths . Any actual implementation will take place through the Instrument Systems Program.
Visitor Program - Foreign Telescope
These funds will be used to help defray travel expenses for U.S. observers who have been assigned observing time on certain large foreign telescopes .
Dark Sky Site Survey
A small amount of funds have been carried over to pay residual expenses
III-ll Rev. 1, 11/18/83 SCIENTIFIC PROJECTS
(Amounts in Thousands)
FY1984 FY1983
KPNO
CTIO NIGHTTIME DAYTIME TOTAL TOTAL
Personnel Costs $ 420 $ 798 $ $1,218 $ 914
Supplies & Materials 646 249 35 930 453
Purchased Services 109 109 32
Domestic Travel 6 6 10
Foreign Travel 13
Equipment 72 209 281 845
Total $1,253 $1,256 $ 35 $2,544 $2,267
Staffing Schedule (in FTE)
FY1984 FY1983
KPNO CTIO NIGHTTIME DAYTIME TOTAL TOTAL
Scientific 1.50 1.50 1.50
Technical Professional 4.00 9.00 13.00 14.00
Professional Administrative & Supervisory 2.00 2.00 2.00
Administrative & Clerical .50 .50 .50
Technical & Others 6.00 12.00 18.00 17.50
Total 14.00 21.00 35.00 35.50
111-12 Rev. 1, 11/18/83 SPECIAL PROGRAMS
(Amounts in Thousands)
KPNO NIGHTTIME
FY1984 FY1983
GRATINGS LABORATORY Personnel Costs 38 34 Supplies & Materials 7 17 Purchased Services 3 2 Equipment 15 39 $ 63 $ 92
COATINGS LABORATORY Personnel Costs $ 38 26 Supplies & Materials 23 26 Purchased Services 1 Domestic Travel 1 Equipment 5 $ 68 $ 53
DETECTOR RESEARCH & DEVELOPMENT Personnel Costs $ 304 218 Supplies & Materials 39 132 Purchased Services 4 2 Domestic Travel 4 2 Foreign Travel 5 1 Equipment 22 $378 $374
VISITOR PROGRAM-FOREIGN TELESCOPES Foreign Travel $ 30 20 30 S 20
DARK SKY SITE SURVEY Personnel Costs 22 Supplies & Materials 1 Purchased Services 5 Domestic Travel 3 Equipment
$ 1 $ 32
$540 $571
111-13 Rev. 1, 11/18/83 SPECIAL PROGRAMS
Staffing Schedule (in FTE)
KPNO NIGHTTIME
FY 1984 FY1983
GRATINGS LABORATORY Technical & Other 1.00 1.00
COATINGS LABORATORY Technical & Other 1.00 1.00
DETECTOR RESEARCH & DEVELOPMENT Professional Administrative & Supervisory 1.00 Technical Professional 2.00 3 .00 Technical & Other 5.00 5 .50
Sub-total 8.00 8 .50
Total 10.00 10 .50
111-14 Rev. 1, 11/18/83 IV. OPERATIONS AND MAINTENANCE SCIENTIFIC STAFF AND AURA MANAGEMENT FY1984
OPERATIONS AND MAINTENANCE
CTIO $4,955K
Operations Support $2,020K Engineering & Technical Services $ 509K General & Administrative $2,426K
Under CTIO's organizational structure, the above budget categories are represented by the following CTIO divisions :
Operations Support: 1) Telescope Operations 2) Operations/Cerro Tololo
Engineering & Technical Services 1) Computer Applications 2) Mechanical/Facilities Engineering
General & Administrative 1) Director's Office 2) Library 3) Business Office/La Serena 4) Business Office/Santiago 5) Business Office/Tucson 6) Operations/La Serena
Operations Support
Telescope Operations - The Telescope Operations Department, with 30.5 FTE, provides visitor and staff observer assistance and carries out the day- to-day operation and routine maintenance of the telescopes and research instruments. The personnel in Telescope Operations are supported in special tasks by employees from the Engineering and Technical Services Division.
The Observer Support Group is charged with assisting visiting astronomers in preparing the telescopes for their observing programs, setting up instrumentation packages including those provided by visitors, and operating the telescopes and data-acquisition systems for both visitors and staff.
The Photographic Specialists ensure that visitors are provided with required photographic or other data-processing materials along with information on how to use and process plates.
The Telescope Mechanics Group is responsible for routine maintenance of telescopes and auxiliary equipment. They change instrumentation packages to correspond to different observing programs and service equipment as required. A small machine shop on Tololo is operated by this group to provide an emergency facility for repairs or modifications . The Electronic and Data Systems Group is responsible for the operation and maintenance of all the computers, peripherals, and electronic components
IV-1 Rev. 1, 11/18/83 of the telescopes and instruments on the mountain.
Operations/Cerro Tololo maintains the 23-mile-long, unpaved access road to the mountain, the housings of eight telescopes, five houses and four dormitories with 68 rooms and associated kitchen facilities for visiting observers and mountain staff members. In the area of utilities, OperationsyCerw Tololo must maintain a water system drawing from the San Carlos well which-is over 4,000 meters distant from, and over 1,000 meters lower than, the water treatment plant on the mountain. The permanent laundry annex to the Technicians' Dorm (and serving all other dorms, the kitchen and the infirmary) could not be completed in FY1983 because of delays in design and bad weather on Tololo. With the advent of summer weather in December, the laundry annex will be completed in FY1984 with funds carried over from FY1983.
Like Operations/La Serena, Operations/Cerro Tololo has its own fleet of vehicles to fuel and service. An ambulance is on order and four trucks, long overdue for replacement, will have been purchased using FY1983 funds. The staff of Operations/Cerro Tololo is composed of 37 FTE's, all Chileans.
Engineering & Technical Services
The Engineering and Technical Services Division is responsible for non- routine visitor and staff observer support; non-routine maintenance of the telescopes and research instruments; programming of the telescope control and data acquisition computers and the La Serena Computer Center; and electronic and mechanical design, fabrication and maintenance of instrumentation. Engineering and technical assistance is given to Operations/Cerro Tololo and Operations/La Serena. This group is also responsible for the maintenance and upgrading of the La Serena-based computer systems, measuring engines and all other electronic systems, and the design and manufacture of printed circuit cards .
The Computer Applications Group is responsible for systems-level programming of the Tololo Network (TOLNET) and the La Serena Computer Center, for programming the telescope control computer system, and for user-oriented data acquisition and data reduction programs.
The Mechanical and Facilities Engineering Group is responsible for the mechanical design and drafting involved in all instrument, telescope and facilities projects, supplies electrical engineering expertise, and provides engineering supervision for major telescope maintenance.
The FY1984 staffing schedule for ETS is 25.0 FTE's. It is to be noted that half of these positions and the related payroll costs will be charged to ETS, and half to Scientific Projects. Staffing schedules and budget summary pages are calculated accordingly.
General & Administrative
Director's Office - The Director and his staff have the overall responsibility for the operation and planning of the Observatory. The Director represents CTIO to AURA, the NSF, and the scientific community. The Assistant to the Director plays an important role in preparing the plans and reports required by contract and in assisting with the operational and administrative work in the office. Scientific Public Relations is also managed by the Assistant to the Director. The Administrative Assistant,
IV-2 Rev. 1, 11/18/83 Secretary, and Radio Operator handle the recordkeeping associated with the telescope usage, the processing of applications for telescope time, and communications with the Tucson Business Office. They also work with the scientific staff as necessary. Funds for the Director's travel and for the Users Committee" and- Telescope Assignment Committee travel are managed by this office. CTIO's share of the expenses associated with the NOAO Director's Office is also budgeted here. The office staff consists of 5.0 FTE on board and 1.0 FTE clerical vacancy.
Library - The CTIO librarian is responsible for the operation of the CTIO research libraries in La Serena and on Cerro Tololo. The funds for the library cover the cost of subscriptions to scientific journals, the acquisition of new books, and all charges associated with staff and visitor publications .
Business Office, La Serena - The Business Office, La Serena, is the seat of operations of the Director of Administrative Services (DAS) who supervises business offices in three cities and the Operations Department on Cerro Tololo and in La Serena. Also under his supervision, the Office of Budget and Accounting, with the assistance of a counterpart office in KPNO, handles all financial matters. The Business Office in La Serena is staffed by 14 Chileans and one U.S. hire, the DAS.
Business Office, Santiago - The Santiago Office is responsible for the purchase of supplies and equipment more economically obtained in that metropolitan center than in the United States or in La Serena. It processes both incoming and outgoing shipments through the Chilean customs in Santiago, Valparaiso and other ports of entry or departure. The office serves as the Observatory's liaison with a variety of ministries and agencies of the Chilean Government and provides assistance to CTIO's visitors in passing through Customs, obtaining lodging in Santiago, and procuring transportation to La Serena.
In two successive reductions in force, the Santiago Office has been cut to a bare minimum for operational utility, especially when one considers that its personnel are traditionally on call to aid visitors 24 hours/day, 365 days per year. The office has one U.S. professional administrator and two Chilean hires, both in the Administrative/Clerical category.
Business Office, Tucson - This office is responsible for procurements in the United States . The office coordinates the receipt and shipment of supplies and equipment through a number of freight forwarders in major ports and expedites deliveries by these agencies. The Tucson office is also the Observatory's main communications link in the United States. The Tucson Office radio room processes an average of 297 messages from Chile, and an average of 340 messages to Chile each month. Although the staffing schedule for the Tucson Office shows no vacancies at the moment, it, too, is operating at a "bare bones" level. The 4 FTE's, all U.S hires, are all Professional and Administrative/Clerical in classification.
Operations/La Serena - Under supervision of the DAS, this department, with 18 FTE's, is responsible for the operation and/or maintenance of the offices, shops, laboratories, twenty-five houses, 10-room dormitory, recreational facility, San Joaquin well and water system, and all surrounding roads and grounds of the La Serena Compound.
IV-3 Rev. 1, 11/18/83 KPNO $9,025K
Operations Support Division $4, 202K Engineering & Technical Services $2,001K General & Administrative $2 ,822K
Operations Support
The Operations Support Division (OSD) is made up of three departments and the Division Director's office. The departments are Observing Support, Kitt Peak Operations, and Computer Support. The purpose of the Division is to provide direct user assistance 363 days and nights per year to well over 750 users of KPNO facilities. The users consist of visiting and staff astronomers, graduate students, and others qualified to use the facilities. The assistance rendered is in the form of support for all the KPNO telescopes, data acquisition and reduction software and equipment, and KPNO mountain dining, lodging, and physical plant facilities. The total division staffing level is 101 .00 FTE.
Observing Support Department - The 31 .50 FTE personnel in this group include telescope operators for the 2.1m and 4m telescopes, technical assistants, instrument specialists, darkroom assistants, observers, support scientists, and supervisory personnel.
The two major functions of this department are to insure that all telescopes are "astronomer-ready" for day and night observing, and to instruct all users in the proper use of the more than 50 instruments and 12 telescopes available to them. In addition, this group of people provides: 24 hour/day call-out service for instrument and telescope problems; preventative maintenance and mechanical repair of instruments; coordination and direct assistance to visiting astronomers in reduction of scientific data; preparation and revision of Observatory instrument manuals; help in preparation and revision of the telescope schedule during the year; and help in defining and developing new scientific instruments . In addition, personnel in this department provide assistance and support to scientists using remote observing instrumentation and equipment techniques.
Kitt Peak Operations - The 43.00 FTE personnel in this department consist of mechanics, electricians, cooks, medical technicians, carpenters, painters, secretaries, tour guides, custodians, and supervisory personnel.
This department is responsible for the physical plant maintenance of all 48 buildings located on Kitt Peak. It is also responsible for all of the basic utility distribution systems and services associated with operating the equivalent of a small town in an isolated area. A few of these services include such things as preparation of four meals per day, lodging, fire protection, first aid, and snow removal. During FY1984 two new four-door sedans will be purchased to replace worn-out vehicles .
IV-4 Rev. 1, 11/18/83 Kitt Peak Operations is also responsible for the Visitor Center which features exhibits, the sale of Papago Indian handicrafts, and tour guides who handle almost 100,000 public visitors each year.
Computer-Support Department - The 21.00 FTE personnel in this department consist of scientific and systems programmers, support scientists, secretarial support and supervisory personnel. The group's primary responsibilities are to provide software for telescope control, data acquisition, data reduction and analysis, and data reduction support. In addition, this group is responsible for defining, planning and implementing existing and future scientific computational facilities requirements.
Office of Operations Support Division Director - The 5.50 FTE include a secretarial staff, a support scientist assigned to assist in development of new instrumentation, a parttime employee to support observatory efforts to protect observational facilities on Kitt Peak from light pollution, and the division Director.
Engineering & Technical Services
The Engineering & Technical Services Division (ETS) consists of three functional areas, the Office of the Director of ETS, the Telescope Systems Program and the Instrument Systems Program, plus two research programs, the Detector R&D and the National New Technology Telescope (NNTT) Programs (described in other sections). The total level of staffing devoted to O&M activities is 38 FTE engineering, administrative, technical, and clerical personnel.
The Office of the Director of ETS provides general management, as well as secretarial support, for the four ETS programs for all O&M, Scientific Project, and Special Program activities.
The Telescope Systems Program's (TSP) O&M responsibilities include the diagnosis and repair of the electronic and mechanical components of all KPNO telescopes and instrumentation including computers, guiders, rotators, control systems, and drive systems. A workforce of seven highly trained electronic and mechanical technicians is on-site at all times to service equipment breakdowns. In addition, these individuals also carry out preventative maintenance programs (both independently and in conjunction with KPNO Operations personnel) and assist Operations Support personnel in performing instrument changes on the larger telescopes. The Telescope Systems Program provides vacuum-deposited coatings for all large optics. This service is available to other astronomical institutions on a cost-reimbursement basis . The TSP also operates the drafting room and electronic supply room facilities. In the area of scientific projects, the TSP is responsible for all telescope-related projects and for the engineering aspects of the implementation of the new mountain and IRAF computer systems .
The Instrument Systems Program (ISP) is responsible for the engineering maintenance and modification of all KPNO instrumentation. The primary function of the ISP is the design and construction of new instrumentation. During FY1982 the ISP carried out the transfer of the KPNO 4m telescope prime focus CCD system to CTIO. The people in this program also operate a mechanical fabrication and welding facility, as well as the Staff Shop, which
IV-5 Rev. 1, 11/18/83 provides direct support for the personal research of the scientific staff. Design, analysis, fabrication, and testing of optical systems and elements are also provided in this program. Lastly, the Coating and Gratings Laboratories (described in another section) are administered by the ISP.
General & Administrative
Director's Office - The Observatory Director and his staff have overall responsibility for the operation and planning of the Observatory. The Director represents KPNO to AURA, the NSF, and the scientific community. The Associate Director assists in all aspects associated with the operation of the Observatory and acts as Chairman of the Scientific Staff. The Assistant to the Director is responsible for the preparation of the plans and reports required by contract and by AURA and assists with the operational and ' administrative work in the office. The Information Services Office, staffed by the Information Services Coordinator and an Assistant is also managed by the Assistant to the Director. This office is discussed below. The Administrative Supervisor performs secretarial duties for the Director and supervises the secretaries who are involved with work for the scientific staff. Travel funds for the Director's Office staff, the User's Committee, the Telescope Allocation Committee and U.S. astronomers observing at foreign telescopes are administered through this office. KPNO's share of the expenses associated with the NOAO Director's Office is also budgeted here.
The Information Services Office is staffed by 2 FTE's. The Information Services Manager is primarily responsible for making available photographs, slides, films and other astronomy-related items to teachers, science writers, film makers, and publishers, both directly and indirectly through Hansen Planetarium. In many of the above activities, the office works closely with CTIO and NSO. At the request of the general public, the office also provides speakers (from the staff), exhibits, and a program of Public Evenings. The preparation of news releases and interaction with the news media will be handled through the NOAO Director's office.
The Director of Administrative Services is responsible for the management of all General & Administrative activities other than the Observatory Director's Office. Responsibilities include the activities of the Photographic Laboratory, Library, Tucson Facilities & Operations Department, Controller's Office, and Personnel and Procurement Departments. Each of these is discussed below.
Photographic Laboratory - Staffed by 3.0 FTE's, the Photographic Laboratory provides for staff and visiting scientists a complete custom photographic service in the form of publication-quality prints, finding charts, dicomed reprints and transparencies and other materials associated with data reduction.
Library - The Librarian and full-time assistant are responsible for acquiring, cataloging and maintaining books, journals, preprints and other publications . The budget for acquisition of journals suffered a 30% cut in FY1981 and remains at this reduced level. Page charges account for more than one-third of the Library's budget, and the rates continue to escalate.
IV-6 Rev. 1, 11/18/83 Controller's Office - The Controller's Office with a complement of 12.5 FTE's provides full accounting, financial reporting and payroll services for KPNO, CTIO (excluding transactions in Chile), NSO and the Corporate Office.
Procuremaat^Department - This department staffed by 5.5 FTE's, performs all purchasing and ."subcontracting services for KPNO.
Personnel Department - The Personnel Department with 3 FTE's is responsible for developing, implementing and coordinating personnel policies and programs including employment, wage and salary, benefits, equal employment and affirmative action, and employee services. It serves all of AURA's employees at the ground-based observatories, excluding Chilean hires at CTIO.
Tucson Facilities & Operations Department - This department is staffed by 24 full-time and one part-time position. It provides a broad range of services related to the operation and maintenance of 120,000 square feet of laboratory, shop and office space. It also provides shipping and receiving services, property control, mail room services, switchboard operations, photocopier and print shop services, motor pool operations, and operates the central office supply stockroom. Utilities and telephone services are provided for KPNO's Tucson headquarters, CTIO's Tucson Business Office, and the Corporate Office by this department.
KPNO Operations Support, ETS and Administrative Services support 6 telescopes located on Kitt Peak operated by other institutions and a variety of programs and projects funded by other agencies and institutions. Administrative Services also provides reimbursed support to CTIO, NSO and the AURA Corporate Office. The resources required to support these activities in FY1983 were equivalent to 15 FTE.
IV-7 Rev. 1, 11/18/83 OPERATIONS & MAINTENANCE
(Amounts in Thousands)
FY1984 FY1983
KPNO- CTIO NIGHTTIME DAYTIME TOTAL TOTAL
Personnel Costs $2,256 $5,962 $374 $ 8,592 $ 7,122
Supplies & Materials 1,103 1,195 85 2,383 2,207
Utilities & Communication 468 736 48 1,252 1,059
Purchased Services 795 <140>(I) 478 1,133 601
Domestic Travel 49 102 2 153 111
Foreign Travel 115 39 1 155 74
Equipment 169 138 5 312 1,177
Real Estate 62
Total $4,955 $8,032 $993 $13,980 $12,413
Staffing Schedule (in FTE)
FY1984 FY1983
KPNO-
CTIO NIGHTTTME DAYTIME TOTAL TOTAL
Scientific 2.50 12.50 15.00 14.50
Technical Professional 11.00 18.50 29.50 30.00
Professional Administrative & Supervisory 22.00 29.75 .25 52.00 52.00
Administrative & Clerical 20.50 33.75 1.00 55.25 53.00
Technical & Other 32.00 40.75 11.25 84.00 81.50
Maintenance & Service
Workers 39.00 49.00 2.00 90.00 89.00
Total 127.00 184.25 14 .50 325.75 320.00
*• 'The credit results from indirect cost recoveries for support provided to daytime programs, CTIO, NSO and non-NSF programs.
IV-8 Rev. 1, 11/18/83 ALLOCATION OF OPERATIONS & MAINTENANCE BY MAJOR FUNCTIONAL AREA
(Amounts in Thousands)
FY1984 FY1983
CTIO NIGHTTIME DAYTIME TOTAL TOTAL
OPERATIONS SUPPORT Personnel Costs $1 ,037 $2 888 $204 $ 4,129 $ 3,390 Supplies & Materials 615 557 51 1,223 1,206 Utilities & Communication 202 233 47 482 419 Purchased Services 72 146 <20>1 198 176 Domestic Travel 14 1 15 16 Foreign Travel 13 Equipment 94 79 2 175 720 Sub-total $2 ,020 $3 ,917 $285 $ 6,222 $ 5,940
ENGINEERING & TECHNICAL SERVICES Personnel Costs 345 $1,318 $118 $ 1,781 $ 1,439 Supplies & Materials 99 392 34 525 375 Purchased Services 17 85 102 <40> Domestic Travel 17 17 13 Foreign Travel 7 7 6 Equipment 41 35 2 78 190 Sub-total $ 509 $1,847 $154 $ 2,510 $ 1,983
GENERAL & ADMINISTRATIVE Personnel Costs $ 874 $1,756 $ 52 $ 2 ,682 S 2,293 Supplies & Materials 389 246 635 626 Utilities & Communication 266 503 1 770 640 Purchased Services 706 <371>2 498 833 465 Domestic Travel 49 71 1 121 82 Foreign Travel 108 39 1 148 55 Equipment 34 24 1 59 267 Real Estate 62 Sub-total $2 ,426 $2,268 $554 $ 5 ,248 $ 4,490
TOTAL O&M $4,955 $8,032 $993 $13,980 $12,413
Anticipated funding from NASA for support of Vacuum Telescope operations The credit results from indirect cost recoveries for support provided to daytime program, CTIO, NSO and non-NSF programs.
IV-9 Rev. 1, 11/18/83 OPERATIONS & MAINTENANCE
Staffing Schedule (in FTE)
FY1984 FY1983
KPNO-._—____ CTIO NIGHTTIME DAYTIME TOTAL TOTAL
OPERATIONS SUPPORT Scientific 1.50 9.50 11.00 10.50 Technical Professional 7.00 12.50 19.50 19.00 Professional Administrative and Supervisory 5.00 11.00 16.00 16.00 Administrative & Clerical 3.00 8.00 1.00 12.00 12.00 Technical & Other 24.00 18.50 4.50 47.00 45.50 Maintenance & Service Workers 27.00 34.00 2.00 63.00 62.00
Sub-total 67.50 93.50 7.50 168.50 165.00
ENGINEERING & TECHNICAL SERVICES Technical Professional 4.00 6.00 10.00 11.00 Professional Administrative and Supervisory 2.00 3.00 5.00 5.00 Administrative & Clerical .50 4.00 4.50 4.50 Technical & Other 6.00 18.00 6.00 30.00 29.00 Maintenance & Service Workers 1.00 1.00 1.00
Sub-total 12.50 32.00 6.00 50.50 50.50
GENERAL & ADMINISTRATIVE Scientific 1.00 3.00 4.00 4.00 Professional Administrative and Supervisory 15.00 15.75 .25 31.00 31.00 Administrative & Clerical 17.00 21.75 38.75 36.50 Technical & Other 2.00 4.25 .75 7.00 7.00 Maintenance & Service Workers 12.00 14.00 26.00 26.00
Sub-total 47.00 58.75 1.00 106.75 104.50
TOTAL OPERATIONS & MAINTENANCE 127.00 184.25 14.50 325.75 320.00
IV-10 Rev. 1, 11/18/83 SCIENTIFIC STAFF AND SUPPORT
CTIO $952K
For reporting purposes*, CTIO's on board scientific staff presently consists of 9_.0_FTE Astronomers, 1.0 FTE Associate in Computer Support, 1.0 FTE Research Assistant"II, and 1.0 FTE secretary. 1.0 FTE Astronomer is expected to join the staff on 1 December 1983, bringing the total on board to 13.0 FTE's. There will remain 4.0 FTE vacancies in the allotted complement of 17.0 FTE's. *CTI0's 3.0 FTE Support Scientists must be counted elsewhere as described below.
KPNO $ 1,592K
Twenty-six scientific staff positions are budgeted in this Plan and efforts will be made in FY1984 to recruit an additional astronomer for FY1985 to replace a staff member who departed at the end of FY1983. This number does not include 11 FTE Support Scientists assigned to the Operations Support Division, Engineering & Technical Services, and the Director's Office. Post- Doctoral positions are increased to 6 FTE, up from 5 FTE in FY83. Four FTE secretaries provide support for the scientific staff and for the visiting scientists who come to Kitt Peak to reduce data and do longer term research projects. This area also includes support for the Summer Student Program.
CTIO and KPNO Scientific Staff
The staff astronomers divide their time equally between their personal research and a wide variety of tasks associated with the operation of the Observatories and the development of new equipment . Their research work has been essential to the development of CTIO and KPNO as first class research institutions . It is perhaps less well known how important their other activities are to the operation of the Observatories . The telescope scheduling process occupies all the non-research time of one staff member at each Observatory and requires substantial involvment by other staff as well. Most of the CTIO staff participate in assisting visiting astronomers with preparation for observing and with instruction in the use of equipment and computer programs. The supervision of the library and photographic group at CTIO comes from the staff.
The three Support Scientists on the CTIO scientific staff are experimental physicists and play key roles in instrument development. The development and implementation of modern detectors, and instruments that utilize them, and the related telescope control and computing systems are essential in modern observational astronomy, and Support Scientists devote most of their time to CTIO's efforts in these areas, with the remainder often going for research programs involving equipment they have developed. For the purposes of the Plan, the positions are counted half in Telescope Operations and half in Scientific Projects . The eleven Support Scientists on the KPNO staff are fully committed in the areas of instrument development and visitor support. They are budgeted in the Observatory operations area.
At present the Advisory Committee for Technical Resources (CTIO) and the Scientific Overview Committee (KPNO), which are each made up of five staff members, oversee the telescope operations and all the engineering and technical services. The committees assign priorities to instrument
IV-11 Rev. 1, 11/18/83 development projects and monitor their progress. There are staff advisors for all projects, and the staff participate actively in the development of new instruments and computer programs .
The Visitia^ Resident Scientist program is included in this area. This program has been very successful in bringing outstanding scientists to the Observatories for periods from one to several months. It stimulates the scientific atmosphere for the resident staff by having people with a wide range of research interests visit and interact and it has offered the participants a chance to do longer term projects than are possible in short visits .
Travel funds for this area include support for the resident scientific staff and the visiting astronomers who come to observe. The staff travels to scientific meetings in the U.S. and abroad, and to work with their colleagues in other observatories and universities in order to keep up in the field. They must also travel on Observatory business . The Observatories also provide travel support to visiting astronomers who are granted time on the telescopes .
IV-12 Rev. 1, 11/18/83 SCIENTIFIC STAFF & SUPPORT
(Amounts in Thousands)
FY1984 FY1 ?83
KPNO- CTIO NIGHTTIME DAYTIME TOTAL T(DTAL
Personnel Costs $752 $1,145 $260 $2 157 $1 684
Supplies & Materials 11 16 27 69
Utilities & Communication 3
Purchased Services 22 1 23 20
Domestic Travel 19 70 13 102 83
Foreign Travel 181 25 3 209 169
Equipment 26 26 30
Total $952 $1,299 $293 $2,544 $2,058
Staffing Schedule (in FTE)
FY1984 FY1983
KPNO-
CTIO NIGHTTIME DAYTIME TOTAL TOTAL
Scientific 14.00 23.00 4.00 41.00 36.00
Technical & Professional 1.00 1.00
Administrative & Clerical 1.00 4.00 5.00 5.00
Technical & Other 1.00 1.00 1.00
Total 17.00 27.00 4.00 48.00 42.00
IV-13 Rev. 1, 11/18/83 AURA MANAGEMENT FEE
MANAGEMENT F"EETT»r..-.. ..-. $408K
CTIO $136K KPNO $272K
Fee provided to AURA, Inc. by NSF for the management oversight of the two Observatories' operations .
IV-14 Rev. 1, 11/18/83 V. CONSTRUCTION
FY1984 ctio :..rrr...... $i2iK
It is to be noted that these are carry-over funds from the following projects approved in FY1983 and not completed.
1) (1) House in La Serena $ 60K This item is not to be confused with the 2 houses in the FY1984 Provisional Program Plan.
2) Tololo laundry building 25K
3) ETS Lab wing, La Serena 36K
KPNO <$236K>
Visitor Center Addition
Unfortunately, the November 1983 funding reduction requires that work in progress on the Visitor Center Addition be suspended and that funds committed for this purpose in FY1983 be disencumbered. The site has been cleared of trees and boulders, leveled, and a ventilation system for use of propane heating systems installed. The site will be stabilized to prevent erosion, and engineering drawings for structural design of the building will be completed this fiscal year.
A study will be conducted to determine how much work can be completed using funds from public contributions and other non-NSF sources .
V-l Rev. 1, 11/18/83 CONSTRUCTION
(Amounts in Thousands)
FY1984 FY1983
CTIO KPNO TOTAL
Personnel Costs $ 32
Supplies & Materials 88
Purchased Services $121 <$236>(L> <$115> 259
Equipment 1
TOTALS $121 <$236>(L) <$115> $380
(1) The credit is the result of cancellation of the Visitor Center Addition committed in FY1983.
V-2 Rev. 1, 11/18/83 VI. NATIONAL NEW TECHNOLOGY TELESCOPE
FY 1984
FY1984 wtt^f consti-tute a transition of the 15 meter telescope program from concept and feasibility studies to a full-fledged telescope design project. During FY1983 a Scientific Advisory Committee (SAC) was established to review the scientific and technical tradeoffs of the two competing concepts: the Segmented Mirror Telescope (SMT) and the Multiple Mirror Telescope (MMT). This committee will have the task of recommending which of the two concepts should be chosen for the 15 meter NNTT. It is planned that this decision be made near mid-1984. The work of the NNTT Program during the early part of FY1984 will center about the completion of initial concepts for the SMT and MMT designs. As the first task, the scientific potential of both approaches will be explored and each design optimized according to the scientific priorities envisioned by the SAC. In addition, the relative cost and risk of each approach will be determined. When the choice has been made, work will turn toward detailed design of the telescope with emphasis on those technical areas which are most in need of better definition. A complete telescope proposal will be generated in late FY1986.
A site selection program will be carried out in parallel with the telescope definition and selection process. The effort during FY1983 was to set up identical measuring stations at the candidate NNTT sites. The FY1983 budget was increased to allow the purchase and installation of the site evaluation equipment. A synoptic data collection effort will commence early in FY1984 and carry on into FY1985. The site selection will be made toward the end of FY1985.
The NNTT program of work in FY1984 is being carried out in collaboration with the Universities of Arizona and California. Much of the work will thus be subcontracted to these institutions . There are seven major elements to the FY1984 work. These are described below. The history of the NNTT Program as well as a detailed description of the FY1984 plan is given in Appendix 5.
NNTT PROGRAM (KPNO) $2,198K
Telescope Design $359K Instrument Design & Validation $226K Telescope Enclosure Design $ 83K Active Optics $164K Primary Optics $995K Optical Polishing Facility $158K Site Evaluation $189K Scientific Advisory Committee Travel $ 24K
Telescope Design
Telescope design activities will be a major element of the NNTT Program for FY1984. The engineering work in this area will progress logically through two stages :
Completion of comparative analyses of the two concepts. This work was begun in FY1983. Particular emphasis will be placed on the
VI-1 Rev. 1, 11/18/83 optical and infrared imaging properties of the designs and on the design of the structures and their response to wind dynamics.
After the concept selection, work on the final design of the 15 meter NNTTiym. begin.
The majority of this work will be carried out at KPNO with strong interaction with scientists from the collaborating institutions. Two items will be subcontracted: analysis and testing of the SMT mirror cell and control system will be performed by the University of California and production of durable, broad-band, high reflectivity coatings will be done by the University of Arizona's Optical Sciences Center.
Instrument Design & Validation
Prior to concept selection, a representative selection of instruments for each approach will be studied to the level where performance for the critical scientific goals specified by the SAC can be estimated. Instrumentation Planning Groups made up of the KPNO scientific staff, along with NNTT Program technical staff, will be heavily involved in this effort. Following the concept selection, more refined designs will be completed. The specific instrumentation issues to be addressed include:
Design of spectrographs covering two decades of wavelength from 0.3 to 30 microns at low, intermediate, and high resolution with capability for simultaneous spectra of many objects .
Design of systems for direct imaging at optical and infrared wavelengths .
Projection of the performance characteristics of point and area detector systems for the 0.3 to 30. micron region which might be available for this telescope.
Application of interferometric instrumentation.
Telescope Enclosure Design
Prior to concept selection, estimates of the relative costs of enclosures for the SMT and MMT will be completed. In addition, studies of the effects of the enclosure upon telescope seeing and wind dynamics will be continued. After the concept selection, preliminary architectural design will commence. The major architectural design work will begin in FY1985.
Active Optics
Because of the physical size and stringent imaging requirements (1/4 arc- second) of the NNTT, existing methods of passive alignment of telescope optical systems will need to be supplemented with active alignment systems. The major problem areas are:
VI-2 Rev. 1, 11/18/83 Primary-to-secondary mirror position control.
Alignment of mirrors and optical path distance control to allow phased and interferometric operation.
Chopping -methods for observations in the thermal infrared.
The major differences between the primary mirror configurations of the SMT and MMT concepts will require very different solutions to the above problems. The initial work will be associated with comparative feasibility analyses of methods applicable to the two concepts as well as the performance of limited hardware testing, particularly related to sensing devices. The majority of this work will be carried out at KPNO.
Primary Optics
The development of methods for the manufacture and polishing of the primary optics of the SMT and MMT concepts has been a major activity of the NNTT Program since FY1981. Work has progressed in two areas:
Development of methods for casting one-piece, light-weight, ribbed (honeycomb) mirror blanks from borosilicate glass is being carried out at the University of Arizona. Two 1.8 meter diameter blanks were completed during FY1983.
The stressed-mirror polishing method for making off-axis aspheric mirror surfaces has been extended to a full-scale test on a 2 meter blank at KPNO. The first full-size off-axis parabola mirror will be completed in early FY1984.
During the early part of FY1984, i.e. prior to concept selection, these activities will be extended as follows:
The 1.8 meter borosilicate blank will be figured for subsequent installation in the UA/SAO Multiple Mirror Telescope on Mt. Hopkins.
A second 2 meter off-axis segment will be polished by the stressed- mirror polishing method in order to determine cost and reproducibility factors .
In addition, major funding will be allocated to the extension of the borosilicate casting facility at the University of Arizona to a 3 to 4 meter capacity. This will be done irrespective of the concept selection. A significant slippage in the overall schedule for production of the 7.5 meter blanks would occur if funding is not available in early FY1984. Even by providing funds in the most timely fashion the first 7.5 meter blank will not be completed until late FY1986. The primary mirror for the CTIO 3-5 meter telescope may be provided by this facility, possibly in FY1985.
In the event that the SMT concept is chosen, a portion of the mirror casting facility funding will be reprogrammed to efforts related to the completion of final designs for the SMT primary mirror segment position sensor
VI-3 Rev. 1, 11/18/83 and actuator hardware This work would be done primarily at the University of California.
Optical Polishing Facility
This area is most dependent upon the concept selection. In the case of the SMT the task is the fabrication of 60 off-axis paraboloidal segments whereas in the case of the MMT the task is the polishing of four 7.5 meter diameter mirrors. Optical polishing facilities do not exist in either case. After the concept selection, planning for the polishing facility will commence. The options include modification of the existing 4 meter facility at KPNO as well as subcontracts with commercial organizations .
Site Evaluation
A minimum-level two-year program of site testing was begun in late FY1983. This program and the sites to be tested were defined by the Ad Hoc NNTT Site Survey Committee in the spring of 1983. The basic site requirements are as follows:
Elevation above 3000 meters to minimize atmospheric water vapor for infrared astronomy.
Distance from major or growing population centers to eliminate light- pollution .
Minimal cloud cover .
Availability within a suitable time period for development as a scientific facility.
On the basis of the above requirements, two potentially superior sites have been selected for further study and testing: Mauna Kea on Hawaii: Elevation 4100 meters Latitude 20 degrees
The Pinaleno Mountains in Southern Arizona: Elevation 3200 meters Latitude 33 degrees
Preliminary testing of these sites has determined no significant detrimental factors. As conditions warrant, e.g. should one of the sites appear unacceptable during early testing and/or a potentially superior site be proposed, sponsored and confirmed on the basis of preliminary tests, the number and identity of the sites under parallel test might change and appropriate budget adjustments would be requested. However, we do not intend to enlarge or prolong the intensive site evaluation any more than is necessary to guarantee the identification of a superior, acceptable site.
During FY1983 equipment for the monitoring of optical images, atmospheric turbulence and atmospheric water vapor was prepared and installation was initiated at the Hawaii and Southern Arizona sites. Comparative testing will commence in early FY1984. The testing will be performed under subcontracts to
VI-4 Rev. 1, 11/18/83 the Universities of Arizona and Hawaii. This testing program will continue into FY1985 with the actual site selection being made in late FY1985. In addition, site testing equipment will be installed and operated at CTIO, either on Cerro Tololo or Cerro Morado. These results will provide a comparison of -a-southern hemisphere site as well aid in the selection of a site for the proposed CTIO 3-5 meter telescope.
Scientific Advisory Committee Travel
Funds have been allocated to provide for the travel of the Scientific Advisory Committee. It is expected that this committee will meet every two months during most of the fiscal year.
VI-5 Rev. 1, 11/18/83 NATIONAL NEW TECHNOLOGY TELESCOPE
(Amounts in Thousands)
KPNO NIGHTTIME
FY 1984 FY1983 Program Actual Plan Expenses
Personnel Costs $ 419 $ 451
Supplies & Materials 190 90
Subcontracted Services 1,300 327
Purchased Services 62 8
Domestic Travel 52 37
Foreign Travel 10 7
Equipment 165 152
Total $2,198 $1,072
Staffing Schedule (in FTE)
KPNO NIGHTTIME
FY1984 FY1983
Scientific 1.00 1.00
Professional Administrative
& Supervisory 1.00 1.00
Technical Professional 5.00 5.00
Technical & Other 5.00 5.00
Total 12.00 12.00
VI-6 Rev. 1, 11/18/83 VII. NON-NSF PROGRAMS
KPNO ,$445K
A number of KPNO staff scientists participate as co-investigators, team members or guest observers in a variety of astronomy programs funded by NASA. These programs involve observations using space vehicles and generally complement the scientists' work with ground-based instruments. KPNO also contracts with NASA and other government agencies to make use of KPNO's unique facilities and talents to provide ruled gratings, coatings and data.
NASA: Infrared Astronomy Satellite (IRAS) $11 IK
NASA: Project Galileo (Formerly Jupiter Orbiter/Probe Mission) , 32K
NASA: Wide Field Camera Project 11IK
NASA: International Ultraviolet Explorer (IUE) Observations 6K
NASA: A Circumstellar Environment of Young Stellar Objects: A Search for Disks IK
NASA Vacuum Telescope Operations 59K
NASA Support of On Site NASA Personnel 15K
NASA Solar Optical Telescope Project.. 8K
NASA Laboratory Fourier Transform Spectroscopy of Planetary Molecules 6K
NOAA: Variation of Solar Call Emission, IK
DOE: Battelle-Pacific Northwest Laboratories Terrestrial Monitoring Project 70K
NASA: UV Project for Spacelab .., 6K
NASA: Space Telescope Grating.. 4K
USAF: High Reflectivity Coating, 15K
NASA: Infrared Astronmy Satellite (IRAS)
Dr. F. C. Gillett has been participating on the Science Team of the NASA Infrared Astronomy Satellite Project since 1975. The satellite was launched in early FY1983, and results so far have been better than expected. As expected, Dr. Gillett's involvement has increased, requiring his presence in England at least through January 1984 and possibly longer.
VII-1 Rev. 1, 11/18/83 NASA: Project Galileo (Formerly Jupiter Orbiter/Probe Mission)
Dr. M. J. S. Belton is participating in Project Galileo, which is NASA's successor project to the Jupiter Orbiter/Probe 1981/1982 Mission. He is serving as Teaa—Leader of the Orbiter Imaging Science Team. The funding support is used primarily to cover the cost of consultants and Dr. Belton's travel to team meetings.
NASA: Wide Field Camera Project
Dr. C. R. Lynds, co-investigator of the Space Telescope Wide Field Camera Project, will continue development of software for analysis of the laboratory and observational test data obtained with CCDs of the type to be used during flight and will provide an operating system based on FORTH running under VAX- VMS.
NASA: International Ultraviolet Explorer (IUE) Observations
Dr. M. J. S. Belton has been a guest observer since May 1, 1980 for his project "Stability of S02 Frost and Vapor on Io and an Investigation of Longitudinal Asymmetry in the Lyman Alpha Albedo of Jupiter." Funding is provided through October 31, 1983 to support travel and publication costs.
NASA: The Circumstellar Environment of Young Stellar Objects: A Search for
Disks
This is the second year of a two-year program of Dr. S. E. Strom in which it is hoped to gain a deeper understanding of the circumstellar environment of Young Stellar Objects (YSOs). Funding is provided for the support of a Research Associate and a modest amount for travel. Dr. Strom has accepted a position on the faculty of the University of Massachusetts where the balance of this project will be done under subcontract.
NASA: Vacuum Telescope Operations
Kitt Peak has provided the solar physics community with full-disk, high- resolution magnetograms and He 10830 spectroheliograms for a number of years using the Vacuum Telescope for synoptic observations. Since 1979 NASA, a primary user of this data, has been providing funding to assist in the operational support and improvement of the telescope.
NASA: Support of On Site NASA Personnel
Funds are provided for the secretarial, computer, and miscellaneous support of Goddard Space Flight Center personnel stationed at KPNO using the Vacuum Telescope.
VII-2 Rev. 1, 11/18/83 NASA: Solar Optical Telescope Project
Dr. J. W. Harvey is the principal investigator for the definition phase of this project. His activities will include the preparation of an updated proposal wh-irh rjaflpr-rs the approved facility and scientific instrument performance capabilities. The science program will be defined to the extent required to accurately estimate all activities planned for the investigation and the resources needed to carry it out. He will also participate in three Science Working Group meetings.
NASA: Laboratory Fourier Spectroscopy of the Planetary Molecules
Dr. James Brault is responsible for a two-year program to provide laboratory spectra of molecular gases which are needed for analyzing observed spectra of planetary atmospheres . The infrared spectra to be provided will be used in creating line lists for heterodyne and FTS searches, modelling of vibration-rotation bands which occur in planetary spectra, and derivation of molecular parameters. These projects have been terminated and action initiated to return the unused funds .
NOAA: Research on Variation of Solar Call Emission
Dr. W. C. Livingston is involved in a Call observing program complete with the necessary data reduction and archiving of the Call chronology. These data will be made available to the Space Environment Laboratory (NOAA) for use in its own study of variability in the UV spectrum of the sun. Analysis and study of the chronology will continue according to a research plan for examining each season of the solar cycle. Funds provided have been used for the temporary support of a part-time research assistant to assist in reduction and archiving of the data and for partial support of the co-investigator, Dr. 0. White.
DOE: Battelle-Pacific Northwest Laboratories
As part of the U. S. Department of Energy's (DOE) effort to evaluate solar absorption spectroscopy as a tool that can be used in the study of atmosphere CO2 abundances, KPNO is providing, on a monthly basis, spectra of the sun using the 1-meter Fourier Transform Spectrometer (FTS) at the McMath Telescope. Once the data has been received, the KPNO computers are used to transform the spectra to a linear wavenumber scale. The data is then transmitted to Battelle-Pacific Northwest Laboratories for further reduction and analysis.
NASA UV Project for Spacelab NASA Space Telescope Grating USAF High Reflectivity Coatings
These projects have been terminated and action initiated to return the unused funds.
VII-3 Rev. 1, 11/18/83 KITT PEAK NATIONAL OBSERVATORY
NON-NSF PROJECTS
(Amounts in Thousands)
FY1984 FY1983
NIGHTTIME DAYTIME TOTAL TOTAL
Personnel Costs $201 $201 $ 200
Supplies & Materials 23 $ 20 43 45
Purchased Services 102 102 86
Domestic Travel 34 34 14
Foreign Travel 16 16 39
Equipment 10 39 49 13
Total $386 $ 59 $445 $ 397
Staffing Schedule (in FTE)
FY1984 FY1983
NIGHTTIME DAYTIME TOTAL TOTAL
Technical Professional 2.00 2.00 2.00
Technical and Other 2.50 2.50 3.50
Total 2.00 2.50 4.50 5.50
VI1-4 Rev. 1, 11/18/83 VIII. FY1984 BUDGETS AND STAFFING
FY1984 PROGRAM PLAN
By Source of Funding
(Amounts in Thousands)
—ruriNu
CTIO NIGHTTIME DAYTIME TOTAL TOTAL
NSF FUNDING
Operations & Maintenance $4,955 $ 8,032 $ 993 $ 9,025 $13,958
Scientific Staff & Support 952 1,299 293 1,592 2,544
Scientific Projects 1,253 1,256 35 1,291 2,544
Construction 121 <236>(1) <236> <115>
Management Fee 136 243 29 272 408
Sub-total $7,417 $10,594 $1,350 $11,944 $19,339
Special Programs 540 540 562
NNTT 2,198 2,198 2,198
Total NSF Funding $7,417 $13,332(2) $1,350(3) $14,682 $22,099
NON-NSF FUNDING 386<4> 59(5) 445 445
TOTAL FUNDING $7,417(6) $13,718 $1,409 $15,127 $22,544
^ 'The credit is the result of cancellation of the Visitor Center addition committed in FY1983, *i2)Includes $795K carryover from FY1983 (3) Includes $98K carryover from FY1983. (4)Includes $74K carryover from FY1983. ^)Includes carryover of $19K and new funds of $40K from NASA for partial support of the Vacuum Telescope operations. (6)Includes $706K carryover from FY1983.
VIII-1 Rev. 1, 11/18/83 CERRO TOLOLO INTER-AMERICAN OBSERVATORY
COMPARISON OF PROGRAM PLAN WITH PRIOR YEARS
FY1982 FY1983 FY1984 Program Plan
Actual Actual New Expenses Expenses Carryover Funds Total
Operations & Maintenance $ 4,280 $ 4,734 $ 274 $ 4,681 $ 4,955
Scientific Staff & Support 522 649 952 952
Scientific Projects 644 1,104 311 942 1,253
Construction 114 121 121
Management Fee 105 107 136 136
Total $ 5,551 $ 6,708_ $ 706 $ 6,711 $ 7,417
VIII-2 Rev. 1, 11/18/83 KITT PEAK NATIONAL OBSERVATORY
COMPARISON OF PROGRAM PLAN WITH PRIOR YEARS
FY1982 FY1983 FY1984 Program Plan
Nighttime Dayti me 1
Actual Actual New New Expenses Expenses Ca rryover Funds Can yover Funds Total
Operations & Maintenance $ 6,695 $ 7,679 $ 513 $ 7,519 $ 48 $ 945 $ 9,025
Scientific Staff & Support 1,333 1,409 67 1,232 15 278 1,592
Scientific Projects 1,189 1,163 100 1,156 35 1,291 pa (1) fD Construction 266 14 <250> <236> <
Management Fee 223 228 243 29 272
Special Programs 393 571 101 4 39 540
NNTT 568 1,072 2,198 2, 198 00 Sub-total NSF Funds $10,401 $12,388 $ 795 $12,537 $ 98 $ 1,252 $14,682
Non-NSF Funds 192 397 74 312 19 40 445
Total $10,593 $12,785 869 $12,849 117 $ 1,292 $15,127
(l^The credit is the result of cancellation of the Visitor Center addition committed in FY1983. 1*1984 Program Plan Summary of NSF Funding by Coat Category (Amounts In Thousands)
Opers. Scl. Staff Scl . AURA Special I * Halnt. & Support Projects Construction Mgt • Fee Programs NNTT To t a 1 a ii CTIO KPNO CTIO KPNO CTIO KPNO CTIO KPNO CTIO KPNO— CTIO KPNO— CTIO KPNO CTIO KPNO Night Day Night Day Night Day Night Day Night Day Night Day • Night Day Night Day
Personnel Costs $2,256 $5,962 $374 $752 $1,145 $260 $ 420 $ 798 $ $ $ $ $ $ $ $ $380 $ $ $ 419 $ $3,428 $ 8,704 $ 634
Supplies & Materials 1,103 1,195 85 II 16 646 249 35 70 190 1.749 1,715 136
Utilities & Communications 468 736 48 468 736 48
795 <140>' 478 22 1 109 Purchased Services 795 <140>' 478 22 I 109 121 <236>2 136 243 29 1,362 1,161 1,259 508
Domestic Travel 49 102 2 19 70 13 6 52 74 229 15
Foreign Travel 115 39 1 181 25 3 35 10 296 109 4
169 138 5 26 72 Equipment 169 138 5 26_ 72 209 42 165 241 580 5 TOTA1.S $4.955 $B.032 S993 $952 $1.299 $293 $1,253 $1,256 $35 $121 $<236> $ $136 $243 $29 $ $540 $ $ $2,198 $ $7.AI 7a $13,332*- $1,350s
The credit results from Indirect cost recoveries for Bupport services provided to the daytime program. CTIO. NSO and non-NSF projects. The credit Is the result of cancellation of the Visitor Center addition committed in FY1983. 3Includes $706K carryover from FVI983. ''Includes $795K carryover from FY1983. CERRO TOLOLO INTER-AMERICAN OBSERVATORY
FY1984 SPENDING PROJECTIONS BY QUARTER
(Amounts In Thousands)
1st Qtr 2nd Qtr 3rd Qtr 4th Qtr Estimated Estimate Estimate Estimate Estimate Carryover
Operations & Maintenance $1 238 $1 ,238 $1,239 $1,240
Scientific Staff & Support 238 238 238 238
Scientific Projects 313 313 313 314
Construction 48 48 25
Management Fee 34 34 34 34_
Total ii,_8j_i_ $1 ,871 $1,849 $1,826 $ 0
VIII-5 Rev. 1, 11/18/83 KITT PEAK NATIONAL OBSERVATORY
FY1984 SPENDING PROJECTIONS BY QUARTER
(Amounts In Thousands)
1st Qtr 2nd Qtr 3rd Qtr 4th Qtr Estimated Estimate Estimate Estimate Estimate Carryover
NSF FUNDING
Operations & Maintenance $2,367 $2 211 $2 218 $2,229
Scientific Staff & Support 369 399 399 425
Scientific Projects 255 307 409 320
Construction <236>(1)
Management Fee 68 68 68 68
Special Programs 125 129 137 149
NNTT 1,004 355 355 484
Sub-Total NSF Funds 3,952 3 ,469 3 ,586 3,675
Non-NSF Funds 125 120 100 100
TOTAL $4,077 $3 ,589 $3 ,686 $3,775
(1)The credit is the result of cancellation of the Visitor Center addition committed in FY1983,
VIII-6 Rev. 1, 11/18/83 CTIO PROGRAM PLAN, FY84
ESTIMATED DISTRIBUTION OF EXPENDITURES, UNITED STATES AND CHILE
(Amounts in Thousands)
To be spent in U. S.: To be spent in Chile: TOTAL U.S. Dollars DIVISION Dollars % Obs. Total $ Equiv. % Obs. Total Dollars % Obs. Total
OPERATIONS/MAINTENANCE
Operations Support: Telescope Operations $ 300 4.0 $ 551 7.4 $ 851 11.5 Operations/Tololo 182 2.5 987 13.3 1,169 15.8 Subtotal, Ops. Sup. 482 6.5 1 ,538 20.7 2,020 27.2
M
^1 ENGINEERING & TECHNICAL SERVICES 186 2.5 323 4.4 509 6.9
GENERAL & ADMINISTRATIVE Director's Office (incl . Cont . Fund) 456 6.2 125 1.7 581 7.8 pa fD Library 55 0.7 32 0.4 87 1.2 < Bus. Off ./La Serena 160 2.2 478 6.4 638 8.6 Bus . Off ./Santiago 43 0.6 54 0.7 97 1.3 Bus. Off./Tucson 379 5.1 4 0.1 383 5.2 Operations/La Serena 128 1.7 512 6.9 640 8.6
1,221 16.5 1 ,205 16.2 2,426 32.7 CO Subtotal, G&A
O&M TOTAL: 1,889 25.5 3 ,066 41.3 4,955 66.8
SCIENTIFIC STAFF & SUPPORT 863 11.6 89 1.2 952 12.9
OBSERVATORY PROJECTS 916 12.4 337 4.5 1,253 16.9
CONSTRUCTION 30 0.4 91 1.2 121 1.6
AURA FEE 136 1.8 136 1.8
TOTALS: $3,834 51.7 $3 ,583 48.3 $7,417 100.00 STAFFING SCHEDULE BY BUDGET CLASSIFICATION
(IN FTE)
FY1984 FY1983
KPNO CTIO NIGHTTIME DAYTIME TOTAL TOTAL
OPERATIONS & MAINTENANCE 127.00 184.25 14.50 325.75 320.00
SCIENTIFIC STAFF & SUPPORT 17.00 27.00 4.00 48.00 42.00
SCIENTIFIC PROJECTS 14.00 21.00 35.00 35.50
CONSTRUCTION
Sub-total 158.00 232.25 18.50 408.75 397.50
SPECIAL PROGRAMS 10.00 10.00 10.50
NNTT 12.00 12.00 12.00
TOTAL-NSF 158.00 254.25 18.50 430.75 420.00
NON-NSF PROJECTS 2.00 2.50 4.50 5.50
TOTAL 158.00 256.25 21.00 435.25 425.50
VIII-8 Rev. 1, 11/18/83 STAFFING SCHEDULE BY FUNCTION
(IN FTE)
FY1984 FY1983
KPNO- CTIO NIGHTTIME DAYTIME TOTAL TOTAL
Scientific 18.00 36.50 4.00 58.50 53.00
Technical Professional 16.00 34.50 50.50 52.00
Professional Administrative & Supervisory 24.00 31.75 .25 56.00 55.00
Administrative & Clerical 22.00 37.75 1.00 60.75 58.50
Technical/Other 39.00 64.75 11.25 115.00 112.50
Maintenance & Service Workers 39.00 49.00 2.00 90.00 89.00
TOTAL 158.00 254.25 18.50 430.75 420.00
VIII-9 Rev. 1, 11/18/83 APPEND".
CERRO TOLOLO INTER-AMERICAN OBSERVATORY ORGANIZATION CHART ASSISTANT USERS' L TO DIRECTOR COMMITTEE I ."! (H.J.Wood) I— CTIO DIRECTOR TELESCOPE RADIO ( P. S. Osmer) ALLOCATION COMMITTEE V LIBRARY I 1 ADVISORY COMMITTEE ADMINISTRATIVE SCIENTIFIC STAFF TECHNICAL RESOURCES SERVICES (J.Baldwin, Chair.) (J.B.Way, Jr.)
fD < EN6. 8 TECHNICAL TELESCOPE FACILITIES BUSINESS OFFICE SERVICES OPERATIONS OPERATIONS LA SERENA (B.Gregory) ( 0. Saa) (E. Figueroa) (L.H.Meneses)
MECH.aFAC. OBSERVER OPERATIONS BUSINESS OFFICE CO i>j ENGINEERING SUPPORT LA SERENA SANTIAGO (G.Perez) (R.Venegas) ( P.Zamorano) (J.Guarini)
COMPUTER TELESCOPE OPERATIONS BUSINESS OFFICE APPLICATIONS MECHANICS CERRO TOLOLO TUCSON (P. Schaller) (J. Briones) (L.Garvizo) (W.C. Enterline)
ELECTRONICS ELECTRONICS 8 INVENTORY PURCHASING DATA SYSTEM CONTROL LA SERENA ( R. Schmidt ) (G.Brehmer) (H. Bustos) ( J. Aguilar)
PHOTOGRAPHIC ACCOUNTING SUPPORT ( L. Pinto) 20 June 1983 (T.Ponce) KITT PEAK NATIONAL OBSERVATORY ORGANIZATION CHART
ACCOCIATE niRFrTno ASSISTANT KPNO UIKLUIOK D. DE YOUNG TO DIRECTOR i G. BURBIDGE A. HEWItJt USERS COMMITTEE _|
1 ' 1 TELESCOPE ALLOCATION 1 COMMITTEE 1 1 INFORMATION 1 SERVICES NNTT SCIENTIFIC ADVISORY I COMMITTEE S.MESZAROS
ADMINISTRATIVE OPERATIONS SCIENTIFIC ENGINEERING B SERVICES SUPPORT STAFF TECHNICAL SERVICES J.KATTINGE, Director B.POWELL,Director D.De YOUNG,Chairman D.SCHRAGE, Director
RESEARCH S COMPUTER LIBRARY CONTROLLER DEVELOPMENT SUPPORT A. FOWLER C.VAN ATTA G.BLEVINS 0 PEN
TELESCOPE SYSTEMS R.NAGEL PHOTOGRAPHY KITT PEAK PROCUREMENT (acting) LABORATORY OPERATIONS
M.HANNA C.JOHNSON R DOANE INSTRUMENT SYSTEMS A.ABRAHAM (acting) TUCSON OBSERVING FACILITIES a PERSONNEL NATIONAL NEW SUPPORT OPERATIONS TECHNOLOGY J.RUFFINO R.BARNES TELESCOPE M. RHOADES PROGRAM L. BARR OCTOBE =« 17, 198 3 APPENDIX 2
Resident Staff and Primary Fields of Interest
CERRO TOLOLO INTER-AMERICAN OBSERVATORY
Bruce Atwood T^Ph^D. Wesleyan University, 19 75. Senior Support Scientist. Experimental'physicist with wide background in electronics. Responsible for CTIO's SIT-vidicon and CCD detectors.
Jack Baldwin. Ph.D. University of California, Santa Cruz, 19 74. Tenured astronomer. Spectroscopy of quasars and Seyfert galaxies. Winner of the Pierce Prize of the American Astronomical Society. Chairman Advisory Committee for Technical Resources (ACTR). Responsible for spectrographs and reduction software for vidicon spectroscopy.
Victor Blanco. Ph.D. University of California, 1949. Tenured astronomer and former director of CTIO. Low dispersion spectra of late type stars in the galactic center and Magellanic Clouds. Photometry of variables in Baade's window. Currently responsible for telescope scheduling at CTIO.
Olin Eggen. Ph.D. University of Wisconsin, 1948. Tenured astronomer. Stellar photometry and galactic structure. Serves as Acting Director in Osmer's absence, adviser for telescope operations, adviser for library, member of ACTR, assists with telescope scheduling meetings.
Jay Frogel. Ph.D. California Institute of Technology, 1971. Tenured astronomer. Infrared properties of cool stars and stellar systems. Infrared instrumentation.
John Graham. Ph.D. University of Sidney, 1964. Tenured astronomer. Magellanic Clouds, nearby galaxies, RR Lyrae and Cepheid variables. Adviser for telescopes and for photographic operations. Liaison with Columbia University radio project.
Brooke Gregory. Ph.D. Brown University, 1972. Associate support scientist. Low temperature physicist working on infrared instrumentation. Vice Chairman of ACTR and Executive Officer for Engineering and Technical Services.
George Hartig. Ph.D. Johns Hopkins University, 1978. Assistant Support Scientist. Experimental physicist working on telescope upgrading. Previously worked on space experiments and observations of quasars. Member of ACTR.
Patrick Osmer. Ph.D. California Institute of Technology, 19 70. Director and tenured astronomer. Spectroscopy and space distribution of quasars.
Mark Phillips. Ph.D. University of California, 1977. Assistant astronomer. Seyfert galaxies and quasars. Adviser for La Serena Computing Center. Visitor support for vidicon observations and data reduction. Member of ACTR.
Patrick Seitzer. Ph.D. University of Virginia, 1982. Assistant astronomer. Globular cluster dynamics. Staff for prime focus CCD and data reduction.
Rev. 1, 11/18/83 Resident Scientific Staff and Primary Fields of Interest
KITT PEAK NATIONAL OBSERVATORY
H. A. Abt -^-&£ellar spectroscopy; binary stars; stellar rotation. M. J. S. Belton - Planetary spectroscopy; theory of planetary atmospheres. J. W. Brault - Solar spectroscopy; solar atmosphere models. G. R. Burbidge - Extragalactic astronomy, cosmic rays, nucleosynthesis. D. L. Crawford - Photoelectric photometry; galactic structure; telescope construction. R. L. Davies - The dynamics of chemistry and stellar populations in early type galaxies; the stellar component of active galaxies.
D. S. De Young - Theoretical astrophysics; active galaxies and QSO's, galaxy clusters; astrophysical plasma processes and hydrodynamics. F. C. Gillett - Infrared photometry and spectroscopy of solar system, interstellar, and extragalactic objects. R. Green - Quasars; white dwarfs; extragalactic astronomy. J. W. Harvey - Solar magnetic fields and velocity fields. G. Illingworth - Dynamics of early-type galaxies and globular clusters, structure and models of globulars, optical structure of radio sources. T. D. Kinman - RR Lyrae variables, planetary nebulae, globular clusters; dwarf and emission-line galaxies; photometry of QSO and BL objects. W. C. Livingston - Eleven-year solar cycle; solar rotation; coronal heating; prominences. B. T. Lynds - Dust and H II regions in spiral galaxies; galactic structure. C. R. Lynds - Observational cosmology; galactic morphology. P. Massey - Wolf Rayet stars; stellar spectroscopy. A. K. Pierce - Solar limb darkening, energy distribution, rotation, and line profiles. C. A. Pilachowski - Stellar abundances and evolution; chemical composition of globular cluster stars; chemical evolution of the galaxy. S. Ridgway - High-resolution spectroscopy of late-type stars and outer planets. P. Seitzer - Extragalactic astronomy; instrumentation, globular cluster dynamics. L. V. Wallace - Temperature structures of outer planets.
Rev. 1, 11/18/83 Support Scientists
J. W. Goad - Kinematics and chemical composition of galaxies.
L. E. Goad - Planetary Nebulae, Galaxy dynamics; digital image processing.
D. S. Hayes - Stellar spectrophotometry; optical properties of the earth's atmosphere; optical properties of interstellar dust; atmospheres of early type stars.
K. H. Hinkle - Infrared spectroscopic studies of late-type and variable stars.
G. Jacoby - Planetary nebulae, chemical evolution of galaxies, Local Group galaxies.
R. Joyce - Infrared photometry and spectrophotometry of regions of star formation.
V. Junkkarinen - Spectroscopy of absorption and emission lines in QSOs and spectral energy distribution and time variability of QSOs and BL Lac Objects.
M. Merrill - Infrared photometry and spectrophotometry of solar system, galactic, extragalactic objects; interstellar and circumstellar dust.
R. Probst - Infrared astronomy; instrumentation.
F. Valdes - Statistical cosmological and galactic structure studies using automated image analysis; the theory of molecular cloud formation; the search for extraterrestrial intelligence (SETI).
Postdoctoral Research Associates
P. Allan - Quasar theories: radio jets, energy sources, winds, accretion; optical and infrared variability of quasars; infrared observations of radio sources; the early universe.
D. Hunter - Star formation; evolution of galaxies; irregular galaxies.
W. C. Keel - Galactic nuclei, active systems, QSOs; Gravitational lenses; Interstellar medium.
J. Pier - The structure and evolution of the Galaxy; stellar populations; stellar kinematics.
A. Saha - RR Lyrae stars; stellar spectroscopy.
N. Sharp - Galaxies and their evolution.
Rev. 1, 11/18/83 APPENDIX 3
CERRO TOLOLO INTER-AMERICAN OBSERVATORY
INVESTIGATORS - FY1983
ASTRONOMERS ASTRONOMERS WHO OBSERVED PARTICIPATING GRADUATE INSTITUTION AT TOLOLO IN PROGRAM STUDENTS
ARGENTINA
Instituto Argentino de Radioastron. 1 Instituto de Astronomia y Fisica del Espacio 3 1 Universidad Nacional de Cordoba 1 1 Universidad Nacional de Cuyo 1 Universidad Nacional de La Plata 2 1
AUSTRALIA
Mt. Stromlo & Siding Spring Observatories 1 4 University of Sydney 1
AUSTRIA diversity of Vienna 1
BRAZIL
Universidad de Sao Paulo 1 1
CANADA
David Dunlap Observatory 1 1 Dominion Astrophysical Observatory 5 2 Universite de Montreal 1 University of Toronto 3 University of Waterloo 1 University of Western Ontario 1
CHILE
Instituto Isaac Newton 1 Universidad de Chile 4 2 Universidad Catolica de Chile 1
GREAT BRITAIN
Cambridge University 4 University of Canterbury 1 'diversity College, Cardiff 1 iyal Greenwich Observatory 2 1 Royal Observatory Edinburgh 2
6 Rev. 1, 11/18/83 ASTRONOMERS ASTRONOMERS WHO OBSERVED PARTICIPATING GRADUATE INSTITUTION AT TOLOLO IN PROGRAM STUDENTS
JAPAN ~—°*-
Gifu University 1 Tokyo Astronomical Observatory 1
SOUTH AFRICA
University of Cape Town 1
SWEDEN
Copenhagen University 1
USA
University of Alaska 1 University of Arizona 5 Arizona State University 2 1 Bell Labs 1 Boston University 1 Brigham Young University 1 University of California, Berkeley 3 1 iversity of California, San Diego 1 .iversity of California, Santa Cruz 2 California Institute of Technology 2 2 Carnegie Institution of Washington 1 1 Case Western Reserve University 1 Computer Science Corporation 1 Palo Alto California 1 Clemson University 1 1 University of Colorado 2 Franklin Marshall College 1 University of Georgia 1 Goddard Space Flight Center 1 Harvard Smithsonian 4 2 Harvard University 1 University of Hawaii 1 1 University of Illinois 2 1 University of Kansas 1 Kitt Peak National Observatory 2 2 Los Alamos National Laboratory 1 1 Louisiana State University 2 1 University of Maryland 1 1 Massachusetts Institute of Technology 3 2 University of Michigan 3 1 Middlebury College 1 University of Missouri 2 Montana State University Mount Wilson & Las Campanas Observatories 1 illard Space Science Lab. 1
Rev. 1, 11/18/83 ASTRONOMERS ASTRONOMERS WHO OBSERVED PARTICIPATING GRADUATE INSTITUTION AT TOLOLO IN PROGRAM STUDENTS
National Research Laboratory 1 University of Nebraska 1 University of New Mexico 1 1 State University of New York 1 University of North Carolina 1 Northwestern University 2 1 Ohio State University 3 Pennsylvania State University 2 3 University of Pittsburgh 2 Princeton University 1 Rensselaer Polytechnic Institute 1 Rice University 1 1 University of Rochester 1 Rutgers University 1 Smithsonian Astrophysical Observatory 2 Southwest Missouri State University 1 Space Telescope Science Institute 2 Swarthmore College 1 University of Texas 2 U.S. Naval Observatory 1 University of Virginia 1 University of Washington 4 4 rT~2sleyan University 1 liversity of Wisconsin 2 4 Yale University 4 2
TOTALS 122 69 10
Astronomers 191 Graduate Students 10 Total Investigators 201 U.S. Institutions 59 Latin Americans Institutions 9 Other Countries 18 Total Institutions 86
During fiscal year 1983, 79% of the telescope time scheduled for observations was assigned to visiting astronomers, most of whom came from the United States. During the fiscal year, a total of 201 different investigators, including 10 graduate students, carried out 144 observational programs at CTIO. Among the institutions represented by these investigators, 59 are in the United States, 9 in Latin America, and 18 in other countries.
During the report period, 201 scientists were involved in 144 separate investigations using the Cerro Tololo telescopes. Of these scientists, 70% were U. S. based, 11% were from Latin American countries, 8% from Canada, and 11% from other countries.
Rev. 1, 11/18/83 KITT PEAK NATIONAL OBSERVATORY
USER INSTITUTIONS FY1983
Institution Ph.D. GS Neither
Aarhus University" Aerospace Corporation Arizona State University 2 Atmospheric & Environmental Research, Inc. 1 Ball State University 1 Bates College 1 Battelle Northwest Laboratories 3 Bell Laboratories 2 California Institute of Technology 7 California State College/San Bernadino 1 Carnegie Institution of Washington 1 Center for Astrophysics 8 College of William & Mary 1 Computer Sciences Corporation 1 Cornell University 1 Corralitos Observatory 1 Denison University 2 Doane College E.G. and G. Edinboro State College Emory University Franklin & Marshall College 2 Georgia State University 6 Harvard University/Center for Earth & Planet Harvard-Smithsonian Center for Astrophysics 2 High Altitude Observatory 3 Howard University 1 Illinois Wesleyan University Indiana University 2 Jet Propulsion Laboratory 2 KPNO Summer Student 1 Kitt Peak National Observatory 35 11 Lawrence Berkeley Laboratory 1 Lawrence Livermore Laboratory 2
Lockheed Palo Alto Research Labs. 1 Logicon 1 Los Alamos National Laboratory 6 Louisiana State University 2 Lowell Observatory 2 Massachusetts Institute of Technology 11 McDonnell Douglas Research Laboratories 2 Michigan State University 2 Mt. Wilson & Las Campanas Observatories 3 NASA Ames Research Cener 1 NASA/Goddard Space Flight Center 17 National Bureau of Standards 1 National Radio Astronomy Observatory 4 National Radio Astronomy Observatory, VLA 1 Naval Research Laboratory 2
Rev. 1, 11/18/83 Institution Ph.D. GS Neither
New Mexico State University 1 1 Ohio State University 2 Orange Coast College 1 Pennsylvania State University 1 2 Planetary Sci-ewee- Institute 4 3 1 Princeton Univers-ity 3 Rensselaer Polytechnic Institute 1 Rice University 3 1 SUNY at Stony Brook 5 1 Sacramento Peak Observatory 2 1 San Diego State University 1 Solar Physics Research Corporation 1 Southeast Missouri State University 1 Space Telescope Science Institute 6 1 Stanford University 3 Steward Observatory/University of Arizona 14 2 TRW, Inc. 1 U.S. Naval Observatory Flagstaff 2 U.S. Naval Academy 1 University of Alabama 1 University of Arkansas 2 University of California, Berkeley 4 3 University of California, Los Angeles 3 1 University of California, San Diego 2 University of California, Santa Cruz 3 University of Chicago • 2 1 University of Cincinnati 1 University of Colorado 5 3 University of Hawaii 1 1 University of Illinois 7 2 1 University of Iowa 1 1 University of Louisville 1 University of Maryland 4 1 University of Massachusetts 3 University of Michigan 6 1 University of Minnesota 1 2 University of Missouri, Columbia 1 University of Nebraska 1 University of Nevada 1 University of New Mexico 3 4 University of North Carolina 1 1 University of Pennsylvania 1 University of Pittsburgh 1 University of Rochester 2 2 University of Texas, Austin 2 1 University of Toledo 1 University of Virginia 2 University of Washington 7 8 1 University of Wisconsin 3 2 1
10 Rev. 1, 11/18/83 Neither Institution Ph.D. GS
University of Wyoming 1 Van Vleck Observatory 1 Vanderbilt University 1 1 Vassar College 3 Villanova Uni,9>«*slty .. 1 Washington University 1 Wesleyan University 1 1 Western Washington University 1 Wheaton College 1 Williams College 1 Wright Patterson Air Force Base 1 Yale University 3 2
284 68
Total of 110 institutions
11 Rev. 1, 11/18/83 Institution Country Ph.D GS Neither
Centro de Investigacion de Astronomia VENEZUELA 1 Copenhagen University Observatory DENMARK 1 Dominion Astrophysical Observatory CANADA 4 European Space Agency NETHERLANDS 1 Inst. Nacional~"cTe;"Astrofisica Optica y Elec. MEXICO 1 Instituto de Astrofisica de Canarias SPAIN 2 Instituto de Astronomia (UNAM) MEXICO 2 Kiel University WEST GERMANY 1 Kiepenheuer Institut fur Sonnenphysik WEST GERMANY 1 Leicester University ENGLAND 2 Max Planck Institut fur Astrophysik WEST Germany 1 Mullard Radio Astronomy Observatory ENGLAND 2 1 Observatoire de Paris Meudon FRANCE 1 Royal Greenwich Observatory ENGLAND 1 Royal Observatory SCOTLAND 1 1 Simon Frazer University CANADA 1 Stockholm Observatory SWEDEN 1 Tel-Avis University ISRAEL 1 Universitat Hannover WEST GERMANY 2 Universite de Paris-Sud FRANCE 1 University of Calgary CANADA 1 1 University of Gottingen WEST GERMANY 1 University of Leicester ENGLAND 1 University of Montreal CANADA 1 1 University of Oslo NORWAY 2 University of Toronto CANADA 3 1 University of Victoria CANADA 1 1 Yunnan Observatory CHINA 2
39
Total of 28 institutions
12 Rev. 1, 11/18/83 KITT PEAK NATIONAL OBSERVATORY
VISITOR TELESCOPE USAGE - FY 83
Domestic Foreign Total
Visiting Astronomers 243 43 286 (Ph.D. )
Graduate Students 66 7 73 (Thesis Projects) (39) (5) (44)
Other Technicians, 21 0 21 (Res. Assts., etc. )
Total Visitors 330 50 380
Institutions 125 31 156
All numbers given are unduplicated; this means that the count does not take into consideration the number of visiting telescope users who came more than once.
13 Rev. 1, 11/18/83 .USE OF KPNO REDUCTION FACILITIES IN FY83
Visiting Scientists Number of
Institutions Ph.D. Student Oth er Total
CDC 640 0 Computer *97 121 9 12 239
Grant Comparator - 1 axis * 4 3 0 0 7
Grant Comparator - 2 axis *22 29 7 0 58
PDS Microdensitometer *36 21 7 _2 66
TOTALS *159 174 23 14 370
* These totals are for FY82 and are not available for FY83 at this time. Upon tabulation of the FY83 figures the totals will be updated. All other totals reflect unduplicated usage of our reduction facilities for FY83.
14 Rev. 1, 11/18/83 APPENDIX 4•
PRELIMINARY PROPOSAL
FOR A LARGE
SOUTHERN HEMISPHERE (3-5M) TELESCOPE
I. INTRODUCTION
This preliminary proposal describes the many reasons for immediately constructing a large (3-5m) class telescope for southern hemisphere optical and infrared astronomy. These center around the major role which will be played by large-aperture, ground-based telescopes in complementing the work of instruments in space, on the preferred position of a southern-hemisphere telescope for observing many of the most fundamentally important celestial objects, and on the need for an infrared optimized telescope in the southern hemisphere.
The basis for an undertanding of stellar structure and evolution and of stellar populations comes mainly from studies of stars in our own galaxy and in the nearest external galaxies. The center of our galaxy and its accompanying concentration of bulge-population stars, globular clusters, X-ray sources, H II regions, and planetary nebulae pass directly overhead at Cerro Tololo Inter-American Observatory, whereas it only skims the southern horizon at most northern observatories. The galaxies nearest to as, the Magellanic Clouds, are even further south at -70° declination and can only be studied to advantage from a southern-hemisphere site. Much of the observing time on new space-borne telescopes (Space Telescope, IRAS, EUVE, etc.) will go towards studying these fundamentally important objects in new passbands or at higher angular resolution than was previously possible. Many of these observations from space will be made because of previous studies by southern-hemisphere ground-based observers. In turn, these observations will lead to many basic new discoveries, and to an explosion of demand for ground-based follow-up observations.
Yet in spite of the great scientific interest in the objects visible in the southern hemisphere, most of the telescopes are in the north. U.S. astronomers have routine access only to a total of 28m2 of aperture in the south, about 25% of that available to them in the north. Furthermore, che existing 4m telescopes in the south were not designed with optimization for infrared observations in mind, so that the deficit in telescope aperture is even more serious in this spectral region. A 5m telescope optimally designed for infrared work could be 30 to 40 times faster than the 4m in the 10 micron wavelength region.
The above arguments, which will be developed in Section II, make che case that the next major U.S. ground-based telescope should be built in the southern hemisphere. This telescope is badly needed right now, as the Field Committee has recognized in recommending support for optical/infrared 15 Rev. 1, 11/18/83 -elescopes in the 2-5m ciass. It should be a 3-5m telescope, fully optimized for infrared observing and designed to provide better imaging in both the optical and infrared than does the existing 4m. CTIO argues that the proper strategy is to select a telescope design which can be started on immediately, using funds vhre^ are annually available in the NSF astronomy budget, without undermining the support required for the existing southern-hemisphere observing facilities. The general specifications which should be met by this telescope are given in Section III. Finally, Section IV of this proposal briefly describes a preliminary design concept for such a telescope. It indicates that a telescope as large^ as 5m could be built for under $10 million including an initial complement of instruments. It would be built on one of the finest dark-sky sites in the world, and as an extension of CTIO which has ready-made support infrastructure, so that its operating costs would be modest. Except in the all-important area of trying out the new lightweight-mirror technology the project would not use untested concepts, so the risk of it not working to specification would be minimal. This telescope project would, however, apply existing design methods at the lowest possible cost, and for this reason would be scientifically highly cost-effective. In short, CTIO proposes to build a telescope on a rapid time scale which will in one stroke double the U.S. capability for southern-hemisphere ground- based astronomy and provide an unmatched ability for making observations of the faintest objects in both the infrared and optical passbands.
It should be stressed that this project is not competing with the NNTT project to build a very large groundbased telescope. Rather the two are complementary. The heart of the southern telescope is a lightweight mirror based on a technology being developed for the NNTT. It will provide a good demonstration of the feasibility and economy of the new technique, which may spur the building of 3-5m class telescopes by organizations for whom conventional designs would be far too costly. The southern telescope can be viewed as a logical step in the progression of the NNTT project.
II. THE CASE FOR A LARGE SOUTHERN TELESCOPE
A. The Special Importance of the Southern Sky
American astronomers need access to additional large telescopes in che southern hemisphere. This is because of the many unique objects of fundamental astrophysical importance which are located in the southern sky. A primary reason for this concentration of especially interesting objects is that the center of our own galaxy is at declination -30°. Thus all objects whose distributions are centered on the Galactic nucleus: open clusters, H II regions, globular clusters, planetary nebulae, and Galactic X-ray sources, as well as the nucleus itself, can best be observed from a southern observatory site. These are the classes of objects which can tall us the most about such fundamental problems such as the birth and evolution of stars, cheir interaction with their environment, the dynamical evolution of our galaxy and of its various components, and the nature of the compact sources which exisc in the galaxy's center. The distribution on che sky of some of chese types of objects is illustrated in Figures 1 and 2, where the shaded areas mark che zone of the southern declinations.
16 Rev. 1, 11/18/83 GLOBULAR CLUSTER
M3 M5 MI3
roR
ii k ij (I i 'j l:r 1 liul 1 mi at i| luliiildi i lust u r s N362 4 7TUC I h i.- southern h >:t\\ l s |> It e r e is hhI ic>iU'(l Itij I'ross li a t, c li i Hij . a no the annudl path of (. f I H ' t; zenith l ;> -ilioiim h tj the ilouhli; broken I l n i' "i ~r~~ TOLOLO ZENITH .-I iii c o 3eyond our own galaxy, our closest extragalactic neighbors, the Magellanic Clouds, can be studied only from the southern hemisphere. These two dwarf galaxies have often been referred to as the Rosetta Stones for understanding many aspects of stellar evolution and of the chemical history of galaxies. Thi*^is because they are sufficiently close to us that it is possible to make detailed studies of many of their individual components, yet astronomers can study their constituent populations on a galaxy-wide scale. The Clouds also play a unique role in astrophysics because they are at just the right distance. On the one hand they are close enough to allow studies of individual stars, yet they are far enough away that all their contents are at affectively the same distance from earth. This means that in the Clouds the determination of intrinsic luminosities can be extended to new classes of objects by simply comparing their apparent magnitudes to those of objects of known luminosity. This technique has made the Clouds a vital link both in measuring the dimensions of our own galaxy and for calibrating the cosmological distance scale.
In addition to the Magellanic Clouds, the southern sky contains three of the nearest and brightest dwarf spheroidal galaxies: the Sculptor, Fornax, and Carina systems. Studies of these objects give important insight into the earlier stages of the chemical and dynamical evolution of galaxies.
Finally, only from the southern hemisphere is it possible to survey a truly representative sample of extragalactic space out to a distance of 25 Mpc. This is because the northern sky is dominated by the extensive cloud of galaxies which are members of the Virgo supercluster.
B. The Future of Southern-Hemisphere Astronomy
The southern hemisphere thus offers our best opportunities for accacking many of the basic areas of research involving che central parts of our own Galaxy and other nearby galaxies. Many of these investigations require large amounts of time on large telescopes. For example, spectroscopic studies or accurate radial velocity determinations of stars like the sun at che discance of the center of our Galaxy requires a telescope of at least 4m aperture. In the specific direction of the Galactic Center, heavy absorption by interstellar dust further compounds the problem at optical wavelengths. The Magellanic Clouds are five times further away, so even without heavy absorption, detailed studies of individual stars is a problem requiring large telescopes. The existing CTIO 4m telescope could (and will) be kept heavily occupied for many decades into the future just continuing with "classical" optical and infrared studies.
At the same time, a new era is opening up in the investigation of chese southern-hemisphere objects; the era of space astronomy. This has already been heralded by the International Ultraviolet Explorer and che Einstein X-ray satellite, and has just been carried another step along the way by che successful launching of the Infrared Astronomical Satellice (IRAS). The special objects in the southern sky are just as important Co scudy with space telescopes as with ground-based telescopes, and will continue Co be a focus of attention.
But these space observatories do not replace ground-based telescopes. Rather, they open up exciting new fields which can then only be fully studied
18 Rev. 1, 11/18/83 THE FOURTH UIIURU CATALOG
Coma Virgo 3C2M
lltr X-l
Cm X-i
Crol.
EOUATOH
Cyg X-l
H(iC 6624 r~ = r TOLOLO ZENITH rj -I ,1 i 5tr ih nt ion of X-r iij s our c i.'s . fi I; ij i s i n il itat e il li ij 3!)lJtllLTH l.e.in SplMMl! .,.... , I pat i' :»r ,-s halcliini). «•>'• tin* ,. 11 e il nol) 1 ' r i I i I ' s M.'n 1 Lli it, s h oiisit using large ground-based instruments. As an example, follow-up observations of X-ray sources discovered with the Einstein satellite have over the past few vears accounted for almost a quarter of the visitor use of the CTIO 4m and 1. 5m telescopes. This rate of usage continues even though the satellite stopped functloTTtrtg- two-years ago. Some specific fields in which large bursts of ground-based observations were ignited by observations made from past or •resent satellites include: the study of chemical abundances in the galactic halo and nearby intergalactic space via observations of absorption lines in superluminous stars in the Magellanic Clouds; the search for regions of star formation in the MC's with IRAS which is going to require extensive subsequent IR observations from the ground; and the search for X-ray sources in globular clusters coupled with subsequent ground-based investigations of the dynamics of che clusters and their chemical abundances.
The real impact, however, will come with the 1986 launch of the 2.4m- aperture Space Telescope and of up to ten additional space-astronomy satellites during the next decade. These space observations will work at all wavelengths from the X-ray to the far infrared. To see the role which large ground-based telescopes will play in complementing space astronomy, we need only list some of the areas in which the capabilities of satellite observations will be relatively limited:
a) high resolution spectroscopy, both IR and optical, where one is limited only by the ability of the telescope to collect photons and not by any sources of background noise;
b) observations at the highest possible angular resolution, where the larger aperture of ground-based telescopes can be combined with speckle interferometry to give a factor of two improvement over what can be done from space;
c) very wide field imaging and photometry, and
d) targets of opportunity and observations which require semi-continuous monitoring of sources over extended periods of cime, boch types of which are difficult from space vehicles because of the constraints imposed by orbital parameters.
In all cases the first two of these areas, and in many cases che lasc two as well, require telescopes of the largest possible aperture, as well as optimization for observations in infrared passbands.
The other way in which space astronomy is complemented by large ground- based telescopes is of course that the latter can be constructed at very much lower cost to provide the photon-collecting capability for the huge variety of optical and infrared programs which in principle could be done equally well from space or the ground.
3ased on the view of the future outlined above a continuation of che present fundamental studies of Galactic objects and the Magellanic Clouds, combined with an explosion of new problems generated by observations made from space CTIO expects that during the coming few decades some of che important problems to be tackled with large ground-based telescopes in che southern hemisphere will include:
20 Rev. 1, 11/18/83 — ;v
'•>- - _
"* . *-.. •«•»•• ,'J r
...';•»,: .'••..
"ML.
"laure 2. Recently obtained -00 micron m a o c f a strip in t Large Magellanic Cloud. The many new sources discovered by IR A3 !j i L I irr.m ed lately be::~e 1". : j .". -priority targets far fallaiu-up observations at CTIQ. The 5m telescope could provide up to 100 times the resolution of the IRAS map. (CTIO Curtis Schmidt photo •+• NASA JPL IRAS map)
21 Rev. 1, 11/18/83 - High resolution spectroscopy of globular cluster stars to provide atmospheric parameters such as abundances, microturbulent velocities, and rotational velocities. - Studies "ar^hi-gh resolution of interstellar absorption lines seen in the spectra of distant stars within our own galaxy, in its halo, and in nearby dwarf companions in order to probe interstellar and intergalactic space to learn atomic abundances, ionization levels, temperatures and gas densities.
- High resolution infrared spectroscopy of ordinary cool stars in order to study molecular abundances. Many molecules, for example CO, have absorption lines only in the IR.
- High resolution spectroscopy and speckle imaging of regions of star formation and of protostellar sources in order to understand the processes involved in star formation itself.
- Medium to high resolution infrared spectroscopy of absorption bands which are characteristic of interstellar grains and dust.
- Radial velocity determinations of obscured galactic sources in order to probe the dynamical structure of distant regions of the galaxy.
- Detailed study of the chemical enrichment history of the Magellanic Clouds via observations of their various stellar and non-stellar components.
- Detailed photometric and spectroscopic studies of individual stars in the Fornax, Sculptor and Carina dwarf spheroidal systems.
- Follow-up studies of external galaxies, galaxy clusters, and quasars in the southern sky which are found to be of special interest as a result of observations made from space.
C. The Present Situation
We have seen that many of the most important astrophysical problems can be tackled best with large ground-based telescopes in che southern hemisphere. Indeed, if there could be only one ground-based Celescope , most astronomers would agree that it should be sited in the southern hemisphere. Yet the present situation is that most of the telescopes are in the north. US astronomical institutions presently operate ten large (greater Chan 2m) aperture telescopes in the north, but only two in che south — the 4m at CTIO and the Carnegie Institution's 2.5m on Cerro Las Companas. As of 1980, che total light gathering power in all countries in the Northern Hemisphere was about 280m2, whereas in the southern hemisphere it was only about 70ra2.
Both the Greenstein Committee and the Field Committee recommended adding new telescopes in the 2 to 5m class, because of cheir general utility and versatility. To date, only a very small start has been made on chese recommended programs. Our European counterparts also recognize telescopes in chis size range to be an exceptionally good scientific investment. As Joseph Wampler pointed out in a recent Physics Today article "... the US national
22 Rev. 1, 11/18/83 centers have four telescopes with apertures exceeding 2 meters, and no firm commitment to increase this number. The Common Market countries, with a comparable population, and smaller gross national product than the United States, have five large telescopes operating on good sites, two more under construction and an additional two funded and in their initial phase of engineering."
D. A New Large Telescope
There is a clearly expressed world-wide need for 4 - 5m class telescopes, and there is a far greater shortage of such telescopes in the south. CTIO therefore proposes that high priority be given to immediately starting the construction in the southern hemisphere of the largest such telescope which can be funded and which could then be operated without undermining the continued operation and maintenance of CTIO's present observing facilities. In particular, CTIO needs a telescope larger than the existing 4m, capable of doing new things. For reasons which will be explained in Section IV, CTIO feels that a 5m telescope can be constructed over the next few years for under S10 million.
A 5m telescope fully optimized for infrared observing with a clean infrared profile, diffraction-limited optics at lOum, a relatively wide field for infrared work, and accurate pointing and tracking would be far superior to any existing southern-hemisphere telescope in terms of its performance. At 10ym its sensitivity would be about six times better than that of CTIO's 4m, which translates into a gain of a factor of 30 to 40 in integration time. Such a telescope would clearly open up new realms of scientific investigation.
For the first time, all stars with absolute lOum magnitudes brighter than -8m could be studied in the Magellanic Clouds. This is precisely the sensitivity level needed to look at dust formation and mass loss processes in stars, as well as regions of star formation and even novae. It would therefore be possible to study, in a very powerful way, the interplay between stars and the interstellar medium in the Magellanic Clouds.
For IR spectroscopy, CTIO expects that detector improvements over che next few years will allow background-limited observations even at intermediate resolutions in the 2-5um region, thus realizing the full factor of 40 gain in integration time. At the highest resolutions, the gains in integration cirae from an infrared-optimized 5m telescope will still be at least a factor of two over the 4m. These tremendous improvements in sensitivity will permit IR spectroscopy of objects hitherto unreachable — distant protostars, faint main sequence dwarfs, giants in nearby galaxies, and the integrated light of distant galaxies.
No space telescope will be capable of approaching the infrared imaging performance of a properly designed 5m telescope for decades to come. Large IR arrays will be available by the time the telescope is built, and they will be used extensively to study dark clouds and H II regions, both in our own Gaiaxy and in the Magellanic Clouds. The structure of the [Ne II] clouds seen at 12.8um in the Galactic Center could be studied in detail, to investigate cheir size, structure, and relationship to active galactic nuclei. A search could
23 Rev. 1, 11/18/83 be made for similar clouds in nearby active galactic nuclei, the closest of which (Cen A) is a southern-hemisphere object. IR speckle imaging would allow detailed studies of dust emission and non-thermal IR sources in other active galactic nuclei.
A 5m telescope would also represent a very significant increase in our capabilities for optical observations. 3esides offering 50% more aperture Chan any other southern hemisphere telescope, it would be housed in an optimum structure which would significantly reduce dome-seeing effects. The resulting combination of larger aperture with smaller images would allow photon-limited observations of objects at least one magnitude fainter than is possible with the 4m telescope. This capability would translate into previously impossible observing programs such as:
a) Spectroscopic study of main sequence stars in the Magellanic Clouds. The present 4m telescope can just reach the globular cluster giants, but spectra of the fainter main-sequence stars would allow us to uniquely determine the elemental abundances without needing to correct for the stars' evolutionary states.
b) Determination of the Mass-Luminosity relation in the Magellanic Clouds. With the 4m telescope it has only been possible to measure the masses of two stars in the Large Magellanic Cloud (LMC X-4 and LMC X-3) and one in the Small Magellanic Cloud (SMC X-l). Not a single "normal" spectroscopic binary has been analyzed. It is of fundamental importance to determine if the. mass-luminosity relationship in the Clouds is the same as in our Galaxy, especially given the abundance differences. This would become a practical project with the 5m telescope.
c) Time Variability Studies. The 4m telescope can only do broad-band photometry of faint X-ray "bursters" while maintaining che necessary time resolution. With a 5m, these sources could be monicored in narrower bandpasses isolating emission lines (cf. He II X4686) which are predicted to be strong from an X-ray heated accretion disk. Alternatively, the cime resolution could be increased significantly. For example, it would be possible to search for the ~1 msec flickering which is predicted from che faint X-ray sources in the Galactic bulge if they are really black holes. High-resolution spectra could for che first cime be caken of these same X-ray sources to search for velocity variations indicating binary systems.
d) Study of fainter X-ray sources. Over the next decade a series of orbiting X-ray observatories (EXOSAT, ROSAT, ASTRO-C, XTE and AXAF) will push X-ray detection limits to 102 - 103 times fainter Chan chose of che Einstein Satellite. ASAV, for instance, will be launched around 1990 to become a permanently orbiting observatory capable of detecting galaxy clusters at z ~ 1-2, and QSOs with the luminosities of Seyfert galaxies out to z ~ 4. At least half of these distant sources will be in che southern sky. A telescope larger Chan che 4m is needed Co make any real progress in following up with optical observations of these very fainc objects.
e) Galaxy Counts to 25th-26th magnitude. The combination of good seeing and moderately wide field would allow CCD imaging of very faint gi'axies
24 Rev. 1, 11/18/83 - /L -• cc - - .9 ~ -\Qn. /"^i Schrm'df N :G "- .CE2RO TQLOLO sur.w CER 30 TO l. O LC T/^, •n — j.'0T'1O ^OQC Rev. 1—LU/18/83 Si ~£ C for comparison with the Northern Hemisphere surface density in the direction of the Virgo Supercluster. The obvious location for a new telescope is CTIO. There exists a choice of excellent sTTSs on the CTIO property. With some crowding, another celescope could be placed on Cerro Tololo itself or on a tower adjacent to the summit platform. An excellent alternative is to place the telescope on Cerro Morado, a large flat-topped mountain 6 miles to the south of Cerro Tololo and with essentially the same altitude. Extensive testing shows that Cerro Morado is just as good as Cerro Tololo; i.e. it is one of the very best sites in the world, with <0.55 arc-sec seeing 22% of the time, and with a very high percentage of both photometrically and spectroscopically usable nights throughout the year. Both Cerro Tololo and Cerro Morado are sufficiently high (over 7000 feet) that the resulting low values of precipitable water vapor and iOum sky noise, combined with the good seeing and clear skies, cause them to rank among the best infrared sites in the world. The extra cost of modest development of Cerro Morado to permit operation of a 5m telescope there would only be about 5200,000, which is comparable to the extra cost of putting the telescope on a pier next to Cerro Tololo. In summary, a new large telescope is badly needed in the southern hemisphere. A preliminary study has shown that the required engineering techniques are available. A first-class site is available. CTIO therefore proposes to start detailed studies towards the development of such an instrument in the immediate future. III. SPECIFICATIONS To build a 5m telescope for under S10M, CTIO must obviously build inexpensively. Yet the telescope must meet some basic, strict performance requirements. This section sets out those underlying requirements. CTIO envisions a new telescope operated as part of che observatory, and thus complementing the existing 4m telescope. The present 4m has Ritchey- Chretien optics giving a wide (40 arc-minute) field, and also has a well- instrumented prime focus. The RC optics and prime focus features could reasonably be left out of the new telescope in favor of a simpler design. On che other hand, the present 4m is not optimized for infrared observing, and is heavily oversubscribed for optical spectroscopy. These are the areas where che new telescope should perform well. In addition, what will be che largest telescope in the southern hemisphere should clearly not sacrifice che abilicy for high-quality optical and infrared direct imaging over modest (5-10 arc- minute diameter) fields. The most important advance in the capabilities of this telescope over che present 4m would be its optimization for infrared work. This requires a small chopping secondary and a clean infrared profile, and also a fairly small hole in the primary mirror. A focal ratio of f/30 is preferred, Co maintain compatability with other CTIO telescopes. This focus would be equipped with an assortment of infrared spectrometers and photometers. A key aspect of the optimization for infrared observing, and also for faint optical observing, is that the telescope must be capable of precise pointing, tracking and offsetting. Because of the current lack of imaging 26 Rev. 1, 11/18/83 capability in the infrared, accurate pointing and trading are essential for IR spectroscopy or photometry on invisible IR sources. It should have an r.m.s. pointing arror^PXl arc-sec for < 60° zenith distance. Its tracking errors should be less than 1 arc-sec per hour and less than 0.2 arc-sec maximum excursion per 10 minutes. The telescope should be able to offset over 3 degrees with an absolute error < 0.8 arc-sec, and over 10 arc-min with < 0.2 arc-sec error. While these specifications significantly exceed the performance of many existing large telescopes, they are neither impossible nor so strict as to impose a major cost burden. An interchangeable top end will be required to provide a faster focal ratio for optical observations. The most desirable plate scale for optical direct imaging is about 5 pixels (of ~25 microns each) per arc-second, but as a matter of convenience in the design of future instruments, CTIO prefers the same f/7.8 focal ratio that currently exists at the RC focus of the present 4m telescope. This gives 7.6 pixels/arc-sec, which only slightly oversamples good-seeing images. A 1500 x 1500 pixel2 detector would have a 3 x 3 arc-min2 field, similar to that obtained with the present 4m prime focus CCD system. The f/7.8 Cassegrain focus would be equipped with an array of direct imaging devices and low to intermediate-dispersion optical spectrographs, since these are the workhorses of observational optical astronomy. The spectrographs should be capable of long-slit and multi-aperture observing. A high-dispersion echelle spectrograph for high signal/noise observations of stellar objects would be provided later, using either a fiber-optic feed to a floor-mounted instrument or a semi-stationary (cf. Nasmyth) focus. Although CTIO is not aiming to duplicate the very large optical field of the 4m telescope, an extremely important capability of the new telescope will be direct imaging of the highest quality over intermediate-sized fields at both the f/7.8 and f/30 foci. This will require careful optical design to give uniformly good images over a field of 5 - 10 arc-min diameter at the f/7.8 focus, and also over a field of the same linear size at the f/30 focus. In order to take advantage of these good optics, a telescope enclosure designed with very close attention to the elimination of dome seeing problems will be required. CTIO hopes to build upon the careful seeing studies (and good results) gained with the enclosure for che Multiple Mirror Telescope. IV. A PRELIMINARY DESIGN CONCEPT After reviewing a number of potential designs1, CTIO believes chat a high-quality 5m telescope can be constructed for under 310 million. Based upon the March 1983 review and preliminary cost estimates, CTIO proposes co '•Design concepts including, besides the alt-az configuration described here, 5m equatorial fork-mounted telescope, a full duplication of the MMT, and an "upgrading" of the CTIO 4m telescope to 8m, were discussed by members of the CTIO scientific and engineering staff along with representatives of che user community and telescope designers at a meeting held on Cerro Tololo in March 1983. From these talks, CTIO is convinced that the alt-az design concept presented here gives the best chance of building a large low-cost telescope with good pointing and tracking performance. 27 Rev. 1, 11/18/83 /' \ I a ~z;i'i gure 5 Sketch of tne proposed 5m Teiesc 28 Rev. 1, 11/18/83 build an alt-az telescope borrowing heavily from the experience gained with the Multiple Mirror Telescope, but utilizing a single 5m-diameter, f/2.0 primary mirror ,-«^rhe_ drive system, telescope control software and azimuth mount would be taken almost directly from the MMT design and are thus proven quantities of known cost. The remaining parts of the telescope structure are clearly a tractable design problem. A stripped-down version of the MMT's rotating building would probably also be used, although this will be compared against the possibility of using at a lower cost a commercially-available 75- foot dome with a very simple concrete building. The low-cost telescope envisioned here would use a lightweight primary mirror of the type being developed at the University of Arizona. CTIO estimates that the lower weight of this mirror would lead to a cost saving of Sl-1.5 million over a telescope employing a more conventional mirror. However, this is the one area where the design would depend on unproven concepts, and CTIO intends over the next months to search for an alternate source for a mirror blank, to which it could fall back in case the University of Arizona project runs into trouble. In the event a 5m, lightweight mirror cannot be obtained, it may be necessary to reduce the aperture to keep the project costs within bounds. Alternatives that have been mentioned include approaching the Canadians to see if their 4m mirror blank could be used, investigating with Corning or Schott the possibility of a conventional thin mirror in the 3-5m range, or making use of a smaller lightweight blank produced in the NNTT development program. The proposed design offers a good combination of high performance and low cost. The MMT is known to point and track to well within the specifications outlined in Section III. This is in large part due to the greater simplicity of the structural requirements posed by an alt-az mount compared to an equatorial mount, but is also a product of the MMT's use of on-axis direct encoding of the telescope's position. The new 5m telescope will exactly duplicate these MMT features, and should therefore perform just as well. Another positive feature of the alt-az configuration is that the lightweight primary mirror can be used in the simplest possible mirror-support configuration. It appears that the lateral support of these mirrors must be carried to a large number of points inside of cheir "egg-crate" structure, and this is far easier to do when the lateral force will occur in only one direction, as is the case with an alt-az mount. This telescope would initially be equipped with only f/30 and f/7.8 Cassegrain foci, using interchangeable top ends. A precise, computer- controlled instrument rotator and a two-axis chopping secondary would be used to compensate for field rotation. The initial complement of instruments would be interchangeable with those on the present 4m telescope. CTIO would in fact develop and test the new instruments on the 4m telescope, in advance of che completion of the new telescope. This means that the new telescope would be able to immediately start producing a wide range of top-quality observational results soon after first light, contrary to the normal situation for a major new telescope. A design criterion would be to leave ample space for the eventual implementation of a remotely controlled prime focus (on a future chird cop end) and of the Nasmyth foci. The f/2 prime focus is of great potential use 29 Rev. 1, 11/18/83 for wide-field direct imaging, although at possibly less than the full angular resolution of the telescope. The Nasmyth foci, in addition to cheir obvious advantage as non-tilting mounting points for quite large instruments, can be used with a rapidly-changeable, remotely operated tertiary mirror, thus giving in a very straightforward way the possibility of mixing during a single night observations with more than one large instrument. Based on the actual costs of the various components of the MMT and on commercial estimates for most of the other items, a tentative budget for the construction of the new telescope is as follows:2 - Azimuth mount, azimuth and altitude drives, ... S 1.5 M control system. - Altitude tube + mirror support s 1.2 M - Site, building, dome ••• s 2.0 M - Mirror (blank + polishing) s 2.0 M - Aluminizing tank s 0.5 M - Instrumentation s 0.7 M - Freight s 0.6 M - Contingencies (15%) s 1.3 M TOTAL (1983 dollars) ... S~~9.8 M The cost of operating this additional telescope will depend to some extent on whether it is sited on Cerro Tololo or on Cerro Morado. CTIO estimates that the annual costs for a Cerro Tololo site will be 3373,000, broken down as follows: - Labor 3 night assistants ••• 3 24 K 2 electronic technicians ••• S 32 K. 1 mechanic ••• S 11 K. 1 electronics engineer ••• S 21 iC 0.5 mechanical engineer ••• S 10 K 2 facilities personnel ••• S 22 K 2 astronomers ••• SL00 K - Expendable Supplies (water, electricity cryogenics, etc). ••• S /0 '< - 52 round trips per year for visiting astronomers from U.S.A. ••• S 33 -^ TOTAL ... S373 K Operation of the telescope on Cerro Morado would require approximately cwo more technical personnel and one more facilities person, for an added cost of S57K/yr. In order to prepare a final proposal for the construction of chis telescope, CTIO plans during the next few months to obtain up-co-date cose ^The basis for these estimates is outlined in che Appendix, 30 Rev. 1, 11/18/83 estimates for duplication of the MMT yoke, drives and building, and for the other components of the proposed telescope. CTIO will make a preliminary optical design -which optimizes the tradeoff between moderately wide fields at both f/30 and f/7.8, and it will also look for a source for a backup mirror blank. A modest repeat program of detailed site testing on Cerro Morado and on Cerro Tololo will be initiated. In the meantime, the purpose of this preliminary proposal has been to acquaint the National Science Foundation with the pressing need for a southern-hemisphere 5m telescope, and to outline CTIO's ideas about how to go about building one. CTIO hopes to receive the NSF's comments in return. 31 Rev. 1, 11/18/83 Basis for Cost Estimates 1. AzimuHrmount ,• azimuth and altitude drives, control system. The MMT base and yoke structure plus its on-axis encoders cost S426K in 1973. Allowing for 217% inflation (based on Consumer Price Index statistics) raises this to S925K in 1983. CTIO estimates that the remaining computers, electronics and motors in the control system can be duplicated for S100K. The MMT software would require only slight modification. The above items total to only 31,025K. CTIO is estimating the whole subsystem at S1,500K to allow for uncertainty in the large inflation correction. 2. Altitude Structure & Mirror Support. Included here are S200K engineering costs, and material and fabrication costs including those for two interchangeable top rings with spider assembles. It is assumed that the svstem will require fifty mirror support actuators similar to those recently designed for the University of Arizona 72-inch lightweight mirror. Total cost: 31.2M. 3. Site, Building, Dome. The quoted costs are based on a commercially manufactured 75-foot dome on top of a simple concrete building, since price information is available. If it is not significantly more expensive, a stripped-down version of the MMT rotating building would probably be used instead. 75-foot dome ... S1.200K Concrete building, including special measures to minimize dome-seeing, utility connections (water, power, telephones •.. 3 600K Special site costs (tower next to Cerro Tololo, or Cerro Morado development ••. S 2Q0K TOTAL COST ... 32,000K 4. Mirror. Conversations with Dr. Roger Angel of che University of Arizona suggest that if other funding leads Co che produccion of a 3.5m mirror blank, the additional step to a 5m blank would cost approximately 31M. CTIO estimates that polishing will cost an additional SIM. These estimates include the cost of the f/7.8 secondary mirror. Total cost: S2M. 5. Aluminizing Tank. A 5m tank fully equipped with all vacuum and aluminizing gear could cost up to SIM from a commercial manufacturer. Instead, CTIO plans to purchase just the tank, and Co cransfer che vacuum and electrical equipment back and forth between the 5m cank and our presenc 4m facility. CTIO would expect to aluminize each mirror every other year, so che Cransportation of the auxiliary equipment is not a major problem. Estimaced cost: S500K. 32 Rev. 1, 11/18/83 6. Instrumentation. Because of the far better infrared performance of the new telescope over the present 4m telescope, CTIO plans to transfer the existing 4m IR photometer and spectrometer to the new telescope. The top ring and spider for the f/30 chopping secondary are included under item (2) above, but the cost of the;chopping mechanism and optics are included here. The following estimates are based on the cost of ongoing projects at CTIO, including salary costs at present levels: - Chopping secondary S120K - Remotely controlled offset guider 3 50K - Acquisition TV, with digital memory and autoguiding 3 45K - CCD direct imaging system $ 60K - Optical spectrograph 5100K - Optical 2D photon counting detector S100K - High throughput camera for CCD spectrometer 5 40K - Data acquistion computer system, with full backup system S150K - Incidentals $ 35K TOTAL COST S700K 7. Freight. Our estimate is for inland shipping plus ocean freight charges for transporting 325 tons (including dome and telescope) from central Kansas to Cerro Tololo. 8. Operating Costs. Estimated labor costs assume that all positions, except that of the astronomer, are filled by Chileans who are paid at the midpoints of current salary ranges. CTIO has assumed an exchange rate of 100 pesos per dollar, plus a 25% cost-of-living increase over January 1983 pay scales. If the present pay scales and current exchange rate of 75 pesos per dollar are used, the Chilean costs would be increased 7%. 33 Rev. 1, 11/18/83 :l o < in a c > cr o < > cr Ld CO CD O < o cr o -J o o cr cr 34 Rev. 1, 11/18/83 = I u c O 3 i < in •J! '' I -I i,n o a. i Q 00 cr o en LLl CO CD o "Z. < CO cr LU cr LLl 1- O _J O _J o O cr cr LU 35 Rev. 1, 11/18/83 CO APPENDIX 5 NATIONAL NEW TECHNOLOGY TELESCOPE (NNTT) PROGRAM STATUS REPORT & DETAILED PLAN The following document is a report of the history and detailed plans for the 15 meter National New Technology Telescope Program. This document was prepared in April of 1983 for presentation to the NS7 during a site visit and program review held at KPNO in May of 1983. The document contains a very detailed description of the planned FY1984 work along with a preliminary description of the FY1985 work. Since the writing of this document changes in che FY1983 KPNO Program Plan have resulted in changes in the FY1984 Plan that have produced minor revisions to the NNTT plan. These changes are listed below". In addition a revision to the detailed FY1984 NNTT budget given in the Status Report (Table IV) is provided. This revised budget reflects the changes listed below. a) Support Scientist: A support scientist has been added to the program to provide the necessary interface with the Scientific Advisory Committee (SAC). The result is an increase of the FY1984 staffing level to 12 full- time-equivalents (FTE's). b) Payroll Costs: The planned FY 1.984 labor rates have changed. The FY1984 budget table has been revised to reflect this change. c) SAC Travel: Domestic travel funds have been added to provide for che cost of the Scientific Advisory Committee meetings. d) Site Evaluation: In late FY1983 KPNO core budget funds were re- programmed to allow site testing activities to begin in a timely fashion. The availability of these funds in FY1983 has permitted che early procurement of site testing equipment and its subsequent deployment at the two selected sites prior to the onset of winter weather. The FY1984 site evaluation funds have been reduced co reflect chese expenditures. 36 Rev. 1, 11/18/83 f * TABLE IV NNTT FYI984 BUDGET SUMMARY (PRELIMINARY 4/15/83, REVISED 6/24/81) ITEM TEL. INSTR. TEL. ACTIVE PRIMARY OPTICS SITE SCI. TOTAL DESIGN DESIGN ENCLO. OPTICS MIRROR FABRJ. EVAL ADV. & VALID DEVEL. FACIL. COMM. LABOR COSTS 99 76 13 34 95 7 95 419 CONSULTANTS 5 15 10 5 8 4 47 ^J DOMESTIC TRAVEL 10 5 3 10 24 52 FOREIGN TRAVEL 5 5 10 CONFERENCE 10 5 15 n> < SUPPLIES 60 50 30 50 190 - SUBCONTRACTS 230 30 60 10 870 40 60 1300 c EQUIPMENT 40 65 _50 10 165 00 TOTALS 359 226 83 164 995 158 189 24 2198 00