NATIONAL OPTICAL ASTRONOMY OBSERVATORIES

QUARTERLY REPORT

January 1, 1984 - March 31, 1984

The period ending March 31, 1984, was a very active period with the formation of NOAO and several of its component parts. Each of the Observatories—Cerro Tololo Inter-American Observatory (CTIO), Kitt Peak National Observatory (KPNO), and National Solar Observatory (NSO)—has prepared separate quarterly reports which are included in this packet. Because the Advanced Development Program (ADP) was just starting up during the last month of the reporting period, a report was not required for that division. The only other units which were formed during the reporting period—the NOAO Director's Office and Central Administrative Services—are covered in the following report (Central Offices).

Director's Office

The NOAO Director's Office was officially established on February 1, 1984. During this first quarter efforts were centered on reorganization of the management of the three ground- based observatories—CTIO, KPNO, and NSO—and the formation of the NOAO Central Offices. Search Committees which we established for the NOAO Associate Directors/Directors of KPNO and NSO completed their separate searches and recommended candidates for the positions. Consistent with their recommendation Drs. Sidney Wolff and Robert Howard were selected by NOAO Director Jefferies, for KPNO and NSO respectively, for recommendation to the AURA Executive Committee whose approval was subsequently obtained. In addition, selections were made for the following positions: NOAO Associate Director/Director ADP, Manager Central Administrative Services/Controller, Assistant to the Director NOAO, Manager of NOAO Engineering and Technical Services, and Manager of NOAO Central Computer Services.

The newly formed NOAO Management Committee met several times concentrating mainly on the FY 1985 budget and program plan.

Construction and preparation of offices in the Warren Avenue building were carried out during this quarter. In addition to the NOAO Director and his staff, the Manager of Central Administrative Services/Controller, Budget Manager, and Personnel Office staff are housed in this building.

Central Administrative Services

The quarter ending March 31, 1984, was an extremely busy one for the newly-formed Central Administrative Services, primarily due to the on going NOAO reorganization. Because the addition of each division to NOAO requires extensive reprogramming and -2- substantial effort for all CAS departments, especially the accounting and budgeting staff.

The office of the CAS Manager/Controller continues to play an active part in the reorganization, particularly in the area of budgeting. Several budget exercises related to the FY 1984 Program Plan were prepared, including a breakdown of Revision 1 into mission and support components and reassessments of carryover. As requested by the NSF, preparation of an addendum to the FY 1984 Program Plan was begun. Work was also begun on formulation of the FY 1985 Provisional Program Plan.

With the January closing, the NOAO subledger was established and accounting procedures/programs changed to reflect organizational changes, i.e. the addition of the NOAO Director, CAS, and ADP.

In February, the Chile Support Office Manager spent two weeks at CTIO assisting the Procurement Department with specific problems and coordinating and streamlining the procurement process to make it more compatible with that of the Tucson Office.

With the assistance of the Chile Support Office, a new AURANET Telemail System was established between AURA-operated facilities. It is anticipated that CTIO will be on-line by the end of the next quarter, thereby eliminating the need for the inefficient radio-telex communications link currently in operation.

The Personnel Department has continued to be involved in unusually heavy recruiting activity due to the NOAO reorganization and, in addition, has finalized the Summer Research Assistant recruitment. Statistical salary information, requested by the AURA president, was prepared for a presentation at the March 21, 1984 meeting. Negotiations were finalized resulting in a change of health and life insurance carriers from Blue Cross/Blue Shield/TIAA to Massachusetts Mutual.

In addition to the unusually heavy load of purchase requisitions processed, six major subcontracts or amendments to existing subcontracts were processed, all of which are in support of the NNTT project. QUARTERLY REPORT

CERRO TOLOLO INTER-AMERICAN OBSERVATORY

January-February-March 1984

INDEX

I. SCIENTIFIC HIGHLIGHTS 1

II. TELESCOPE OPERATIONS, INSTRUMENTAL WORK,

RELATED ACTIVITIES 4

III. ADMINISTRATIVE AND FACILITIES HIGHLIGHTS 6

IV. USAGE OF CTIO TELESCOPES 10

V. CTIO PUBLICATIONS 18

VI . MISCELLANEOUS 22 I. SCIENTIFIC HIGHLIGHT

An active field of research is the search for the so-called

missing mass in galaxies. The term comes about because observations of motions in galaxies indicate that a significantly larger amount of mass is present than can be accounted for by the light distribution. The missing mass is not really missing, just non-I urninous. Speculations on the nature of the missing mass span the range of massive neutrinos, mini-black holes, objects of planetary mass like Jupiter, and low-mass, cool stars. G. Gilmore and P. Hewett report new results on this topic based on observations made at CTIO. As they point out, a widely assumed, and logical, candidate for the missing mass is a population of low luminosity M dwarfs. Such stars have very little luminosity for their mass and are consistent with the observations of mass- to-light (M/L) ratios inferred from galactic rotation curves. The stars do exist in large numbers, yet it has been difficult to determine their space density because of their low intrinsic luminosity and low temperatures, which makes them faint at the. visual and blue wavelengths used in previous surveys. Consequently, Gilmore and Hewett have been carrying out a new survey using the UK Schmidt telescope in Australia and red sensitive photographic plates. The wide area and faint limit of the survey at wavelengths favorable for the detection of cool stars allows them to make a much improved search for stars with masses down to the limit at which nuclear hydrogen burning occurs. Using automatic techniques to cover the huge amount- of information on their plates, they identified some 50 very red stars, which are candidates for having very low mass (0.1 solar mass or less). These stars would all be within

200 parsecs of the Sun.

However, the survey observations alone are not sufficient to determine the nature of the stars. Spectroscopic data are needed to estimate the temperature and luminosity of the stars; then their mass can be inferred. Gilmore and Hewett used the CTIO 4m telescope and CCD spectrometer to observe a subset of their candidates and compare them with stars rof^nowrr :\ umi nos ities The CCD system, then just newly installed, offered- the on Iy means of obtaining red spectra of such stars, as previously available detectors did not have adequate sensitivity. The spectra showed that none of the candidate stars was significantly less luminous than their comparison stars (the faintest of which is 1/300,000 as luminous as the Sun), despite the fact that they had sampled a volume of space 50 times larger than had been covered before.

Therefore, Gilmore and Hewett conclude that either the faint limit of stellar luminosity has been reached, or that the space density of very low luminosity stars is substantially less than expected. In either case, very Iow-I urninosity stars do not account for the missing mass in the solar neighborhood. They also go on to argue that such stars do not account for the missing mass problem that occurs on larger scales in the gaIaxy.

The problem of the missing mass remains, nevertheless, and the search for it will continue at other wavelengths and with other techniques. Its nature continues to be a tantalizing problem in modern astronomy. II. TELESCOPE OPERATIONS, ENGINEERING AND TECHNICAL SERVICES,

AND INSTRUMENTAL WORK

TeI ops

In the period Jan-Mar 1984 the telescope statistics were quite good. On the 4m, 1.3^ of the time was lost to instrument failure and 6.3% to poor weather. On the 1.5m, the percentages were 2.7 and 10.6 respectively. There were 78 instrument changes on all telescopes during this period.

The instrument group repaired a number of cold boxes and installed a new collimator on the 4m RC spectrograph. A number of small maintenance items on various instruments were performed. There were no serious problems or breakdowns reported by TELOPS during this period. A good quarter!

ETS and Generaj Instrumentat1 on

Work continues on the Vidicon electronics boxes in order to identify and fix some recurrent causes of failures and to increase their reliability.

Two new CCD dewars were completed and testing of the new GEC chips is proceeding. The Air-Schmidt camera was tested on the

4m telescope. It looked very good and will be made available as soon as the new GEC chip situation is sorted out.

Work continues on the IRS. A number of small mechanical pieces were fabricated in the shop to aid optical testing. The electronics are producing smoothly. The computer peripherals problems are sorting themselves out.

Plotting packages are installed and available on the PRINTRONIX.

The Cipher tape drive problems are almost all cured. The new big disks have not yet been received, though, nor has a replacement for the V ICOM "mouse". V ICOM software implementation is making progress. A library has been set up to store and catalogue magnetic tapes. III. ADMINISTRATIVE AND FACILITIES HIGHLIGHTS

P_iil£ e_o1_+he_DJ_ rector_o f__ Adm_i_ nJ_ strat_i_ ve Services (DAS) During the quarter the DAS was primarily occupied with budget changes for FY84 and budget preparations for FY85, with the Conference Board Price Survey, and with travel to the U.S. for the annual AURA Board meeting and associated NOAO meetings. There was an extraordinarily large amount of budget work owing to the implementation of new NOAO procedures and the consequent changes that had to be made. Similarly, the price survey, which was being done as part of AURA's study of the overseas compensation package for U.S. hires, was time consuming, and the DAS had little assistance available. The results of the survey are

awaited from the Conference Board. The technicalities of the Chilean income and social security withholding tax situation raised by the auditors in 1983 are still unresolved. CTIO will continue to follow its present procedure until the auditor's lawyer provides a definite recommen dation to the contrary. The cumulative inflation in Chile for the first quarter of CY84 was 2.A%. The government continues to predict that the inflation for all of CY84 will be 20$.

!^nil.§2o-_.9_iilc_e.• The usage of the guest quarters at the Santiago office doubled from the first quarter to the second quarter of FY84. Comments from visiting astronomers and CTIO staff indicate that +he quarters are much appreciated. Operations.

Construction and other projects. The completion of the

La Serena Lab extension has been delayed by lack of receipt of materials ordered from the U.S. However, the offices on the second floor will be ready by April (and indeed have been occupied by the time of writing), and the laboratory facilities should also be completed by the end of the next quarter.

The La Serena water system and fire station project is progressing, with the piping, 24 fire stations, and fire hoses having been installed and tested. Work is now concentrated on the new storage tank and pump system. It should be completed during the next quarter.

Work continues satisfactorily on the construction of House

26, with the main structure and rafters now in place.

For the laundry building project on Cerro To IoIo, the site work, foundations, framing, and exterior walls are all complete. At present work is being done on the columns, beams, and joists.

The concrete slab for the NASA mobile laser ranging station is being prepared on a site near the Lowell telescope on a cost- reimbursement basis with NASA.

The new telephone system, based on ITT plants on To IoIo and at the La Serena office, went into operation during the quarter. It has performed satisfactorily, except for the Serena-

ToIoIo link, which is hampered by the manufacturer's failure to provide the proper software. The company has provided a temporary solution to serve until the proper software arrives. A major failure of the switching system for the Tololo powerhouse occurred February 25. It has left the frequency converter disabled, which means that the mountain is running on the power supplied by the backup diesel generators. Because the replacement components are not normally stocked by the manu facturer, a delay of at least two months will occur before the frequency converter can be restored to service. In the meantime, the power costs are double their normal value because of the inefficiency of the backup system. As this is the second major failure in two years, the acquisition of a backup frequency converter system should be considered. The new liquid nitrogen plant was put into operation during the quarter on Tololo. Its production is exceeding the manufacturer's specifications and gives CTIO sufficient capacity for its cryogenic needs at present. The previous ancient system did not, and CTIO had had to make supplementary purchases of commercial liquid nitrogen at high cost. The usage of liquid nitrogren has nearly doubled in the last two years because of the installation of more electronic detector systems at the telescopes, all of which require coo ling.

Maintenance and renovation work confined during the quarter on the Tololo dining-dormitory building, the visitor center, the water plant, the Schmidt telescope building, the technician's dormitory, and the road to the San Carlos well. The long term program to bring the physical plant back to a state of good repair is nearly finished. To improve the food service on Tololo, the shifts have

been reorganized. The head cook will be on a Monday-Friday

schedule and will be responsible for the preparation of the

menus and the ordering of the food. Training courses for some of the employees are also planned. 10

IV. USAGE OF CTIO TELESCOPES

A; Statistics of telescope usage during the period January

1 through March 31 , 1984:

: 53 nights for visitors, 33 nights for staff, and

5 nights for engineering.

1 .5m : 54 nights for visitors, 33 nights for staff, and 4 nights for engineering.

1m : 65.5 nights for visitors, 14.5 nights for staff, 5 nights for engineering, and 6 nights closed.

0.9m : 67 nights for visitors, 14.5 nights for staff, 5 nights for engineering, and 6 nights closed.

0.6/0.9m : 37 nights for visitors, 8 nights for staff, 5 nights for tests, and 41 nights closed during the bright

of moon.

0.6m : 23 nights for visitors, 1 night for staff, and 67

n ights cIosed.

0.4m : This telescope remained closed during the quarter.

During the report period, 89 investigators from 50 different institutions participated in 62 research programs carried out at CTIO. 11

B. Individual telescope assignments are listed below.

Graduate Students are indicated by an asterisk after their name.

Nights assigned, hours worked, and telescope used are included.

B. Blanco and V.M. Blanco, CTIO: A Survey for RR Lyrae Stars

in the LMC, 6(39)1.5, 3(5)MS.

M.F. Bode, W.P.S. Meikle, J.R. Graham, A. Evans, and G. Pearle, Los Alamos National Lab: Infrared Mapping of X-ray Bright

Supernova Remnants in the LMC, 5(50)1.5. N. Caldwell, CTIO, and G. Bothun, California Institute of Technology

Schmidt Plates of Virgo Cluster Dwarfs, 4(10)MS. N. Caldwell, CTIO, R. Kirshner and D. Richstone, University

of Michigan: Dynamics of Gas and Stars in Elliptical Galaxies,

1 .5(14)4, 2(21 )1 .5. N. Caldwell, CTIO, B.A. Twarog and B.J. Anthony-Twarog, University

of Kansas: Astrometric and Photometric Studies of Intermediate

Age CIusters, 4(42)1 .

N. Caldwell and M. Phillips, CTIO, The Nature of the Peculiar

Galaxy NGC 5253, 1(11)4, 1(10)1.5. L. Celis, Universidad Catolica de Chile: UBVRI and H/3Photometry

of Mira Stars, 5(20)0.6. G. Chanan and D. Helfand, Columbia Astrophysics Lab., and S. Reynolds, NRAO: Optical Synchroton Nebulae Surrounding

Radio PuIsars, 2(21)4. J.J. Claria and E. Lapasset, Universidad de Cordoba, and H. Levato, Universidad Nacional de La Plata: CMTIT2 Photoelectric 12

Photometry of Red Giants in Old Intermediate Age Open Clusters

5(54)0.9.

P. Conti, University of Colorado, P. Massey, KPNO, and C. Garmany,

University of Colorado: Initial Mass Function of Massive

Stars in the Magellanic Clouds, 4(33)4.

D. Crabtree and H. Richer, University of British Columbia:

Pop II Carbon Stars in the LMC, 4(41)1.5.

G. Da Costa, Yale University: The Mass Functions of LMC and

SMC Young Globular Clusters, 2(17)4. R. Dufour, Rice University, K. Davidson, University of Minnesota, and N. Walborn, NASA Goddard Space Flight Center: Spectroscopy

of Ejecta From Eta Carinae, 3(31)4, 4(40)1.5. O.J. Eggen, CTIO: Photoelectric Photometry, 16(62)1.5, 11(61)1,

15(49)0.9.

F. Fekel, Vanderbilt University, J. Africano and P. Schmidtke, KPNO, and R. Quigley, Western Washington University: Occultation Observations of YSgr, 2(21)0.9.

J. Frogel, CTIO: a) CCD Spectroscopy of M Giants in the Field of the Large Magellanic Cloud, b) Infrared Photometry and Spectroscopy of Stars, c) Infrared Photometry and Color Magnitude Diagrams for E and SO Galaxies, d) Photometry and Spectroscopy of Luminous Stars in Magellanic Cloud

Clusters, e) The Stellar Population of the Nuclei of Late Type Spirals from Infrared Photometry, 12(116)4. J. Frogel, CTIO, and R. Cohen, Institute for Space Studies,and M. Rubio, Universidad de Chile: An Infrared Survey of a 13

Molecular Cloud in the Large Magellanic Cloud, 4(28)1.5.

D. Geisler*, University of Washington: An Investigation of Anomalous

Stars in Melotte 66, 5(40)1, 6(51)0.9.

J. Graham, CTIO: Near IR Spectroscopy of Southern Herbig-Haro

Objects and their Sources, 3(25)4.

J. Graham, CTIO, and J. Nemec, Dominion AstrophysicaI Observatory:

Variable Stars in the Intermediate Age Clusters of the

Magel Ianic Clouds, 3(19)1.

M. Hamuy* and J. Melnick, Universidad de Chile: UBVRI Photometry

of Faint Globular Clusters, 4(16)0.9.

G. Hartig and J. Baldwin, CTIO: CCD Spectrophotometry of BAL

QSO's, continued, 2(21)4.

P. Hodge and M. Mateo, University of Washington: Color-Magnitude

Diagrams of Intermediate-Age Globular Clusters in the

LMC, 3(26)4, 6(36)0.9.

R. Humphreys, University of Minnesota, and J. Graham, CTIO:

The Stellar Content of M83 and Distance to the NGC 5128

Group, 2(18)4.

B. Jarvis, CTIO: Photometry of Rapidly Rotating Elliptical Galaxies,

3(24)4.

T.D.Kinman, KPNO, and J. Baldwin, CTIO: Velocity Dispersion

of the Galaxy Group Associated with the Black Object 0521-365,

1.5(14)4.

R. Kirshner, University of Michigan, and P. Winkler, Middleburry College: Chemistry and Kinematics of Young Supernova Remnants,

5(45)4. 14

H. Levato, N. Morrell, and S. Malaroda, Universidad Nacional

de La Plata: Binary Frequency Among CNO Stars, 14(144)1.

D.J. MacConnell, Michigan State University, and R. Wing, Ohio

State University: Eight-Color Wing Photometry of Southern

M Supergiant Candidates, 5(28)0.9.

R.D. McClure, NSF, J.E. Hesser, Dominion AstrophysicaI Observatory,

and R.A. Bell, NSF: High Precision Photometry of Globular

Clusters, 3(29)4.

P. Massey, KPNO, and P. Conti and C. Garmany, University of

Colorado: Absolute Spectrophotometry of Wolf-Rayet Stars,

5(46)1.5.

J. Melnick, Universidad de Chile, and M. Copetti, Rio Grande

do Sul, Brasil: Infrared Photometry of: Wl Galaxies,

4(35)4, 13(96)0.6.

J. Melnick, Universidad de Chile, R. Terlevich, Royal Greenwich

Observatory, and M. Moles, Instituto de Astrofisica de

Andalucia: Spectrophotometry of HII Galaxies, 3(30)4, 1(2)MS.

H. Moreno and A. Gutierrez-Moreno, Universidad de Chile: Secondary

Spectrophotometric Standard Stars, 10(45)0.9.

J. Mould, California Institute of Technology, and G. Da Costa,

Yale University: Turnoff Luminosities in LMC and SMC Interme

diate Age Clusters, 4(18)4.

J. Mould, California Institute of Technology, and J. Graham,

CTIO: Are There Carbon Mixed Stars in CO Car Binaries?,

2(19)4. 15

J.M. Nemec and J.E. Hesser, Dominion AstrophysicaI Observatory:

Metal Abundances for the RR Lyrae Stars in and Around the

Remote LMC Cluster NGC 2257, 4(36)4.

V. Niemela, Instituto de Astronomia y Fisica del Espacio: OB

and WR Bi nari es, 7(51)1.

P. Osmer, CTIO: The Clustering Properties of Quasars at

Z -2, 4(41 )4.

J. Patterson, R. Remillard, and W. Roberts, Smithsonian AstrophysicaI

Observatory: Optical Identification of X-Ray Sources,

4(33)1.5, 4(32)1, 8(40)MS.

M.M. Phillips, CTIO: a) A Search for Supernovae in Starburst

Nuclei, b) Supernovae and Supernovae Remnants in Galaxies

with Starburst Nuclei, 1(9)4, 7(38)1.5.

J.J. Puschell, TITAN Systems, Inc., J. Burns and M. Zeilik,

University of New Mexico, and J. Frogel, CTIO: Near-Infrared

Observations of Knots in the Cen+aurus A Jet, 5(53)1.5.

A.E. Ringuelet, J. Sahade, and J.M. Fontenia, Universidad Nacional

de la Plata: Models for the Envelopes of Be Stars,

5(50)1.5.

M.T. Ruiz, Universidad de Chile: Spectroscopy and Direct Photography

of SNR, 1(7)4, 3(30)1.5.

J. Sahade, Instituto Argentino de Radioastronomia, 0. Ferrer,

C. Hernandez, E. Brandi, and L. Garcia, Universidad Nacional

de La Plata: Investigation of Southern Interacting Binaries,

6(54)1.5. 16

P. Schechter, Mt. Wilson and Las Campanas Observatories, M. Aaronson,

University of Arizona, and V.M. Blanco, CTIO: Galactic

Rotation and Disk Size from Carbon Stars Viewed Through

Windows in the Plane, 4(35)4.

J.A. Tyson, Bell Labs, P. Boeshaar, Rider College, and P. Seitzer,

KPNO: CCD Faint Object Survey, 2(21)4.

R. Wade, Northwestern University, and K. Home, Institute of

Astronomy, Cambridge: A Near-Infrared Radial Velocity Study

of the Dwarf Novae Z Cha and OY Car, 3(14)4.

R. Wade, Northwestern University, G. Berriman and K. Home,

Institute of Astronomy, Cambridge, and M. Cook, University

of Leicester: High Speed Photometry of Eclipsing Dwarf

Novae, 3(20)1.5, 16(126)0.9.

A. Wilson, University of Maryland, J. Baldwin, CTIO, and K. Adney*,

University of Maryland: Long-Slit and Direct Imaging Studies

of Gas in Seyfert and Radio Galaxies, 5(52)4, 2(21)1.5.

R. Wing, Ohio State University, and S. Yorka, Denison University:

Molecular Band Strengths in Peculair Red Giants, 6(53)0.9.

D. Westpfahl and M. Chester, Montana State University: a) OB Stars at J. = 240°, b) Variable Stars at J= 240°, 5(32)1.5,

16(99)1, 9(32)MS.

MICHIGAN PROGRAMS: a) D.J. MacConnell, Michigan State University,

J.C. Mermilliod, Universite de Lausanne, K. Steven, Mankato

State University, and N. Houk, University of Michigan: A

Search for Flare Stars in two Poor, Young, Nearby Clusters and three other short Schmidt Programs; b) F. Miller, 17

University of Michigan, and W. Liller, Instituto Isaac

Newton: Comet Crommelin Observations, 7(52)MS.

YALE PROGRAMS: M. Gregg, J. Yamanaka, and A. Oemler, Yale Uni

versify, a) Main Sequence Luminosity Functions in Open

Clusters, b) Red Spectroscopy of Early-Type Galaxies,

14(99)1. 18

CTIO PUBLICATIONS

The following papers by staff and visiting scientists at

CTIO were published or accepted for publication during January, February, March 1984. Complete publication information is given when available.

C-2618 van den Bergh, S. (1983). "The Flattening of Globular Clusters." Publ. Astron. Soc. Pac. 95, 639.

C-2619 Janes, K.A., and Smith, G.H. (1984). "The Giant Branch of the Old Open Cluster M76." Ap . J .

C-2620 Hutchings, J.B., Crampton, D., and Cowley, A.P. (1983). "A Spectrographic Orbit for LMX X-1: Another Massive X-Ray Source? Ap. J. Lett. 275, L43.

C-2621 Gilmore, G., and Hewett, P. (1983). "A New Limit on the Nature of the Galactic Missing Mass." Nature, 306, 669.

C-2622 Schober, H.J. (1983). "The Large C-Type Asteroids 146 Lucina and 410 Chloris, and the Small S-Type Asteroids 152 Atala and 631 Philippina: Rotation Periods and Lightcurves." Astron. 4 Astrophys. Suppl. 53, 71.

C-2623 Cohen, M., and Schwartz, R.D. (1984). "The Geometry of "The Infrared Nebula" in Chal." Astron. J. 87, 277.

C-2624 Twarog, B.A. (1984). "UVBY Secondary Standards Near the South Galactic Pole." Astron. J.

C-2625 Bell, R.A., Hesser, J.E., and Cannon, R.D. (1984). "Spectroscopy over a Range of 5 Magnitudes in NGC 6752." Ap . J.

C-2626 Harris, H.C., and Wallerstein, G. (1984). "Kinematics of Field Type II Cepheid Variables." Astron .J. 19

C-2627 Carney, B.W., and Latham, D.W. (1984). "The Baade-WesseIink Method and the Distances to RR Lyrae Stars. I. The Field Star VY Serpentis." Ap. J. 278, 241 .

C-2628 Szkody, P., and Mateo, M. (1984). "An Unprecedented UV/Optical Flare in TV Col." Ap. J.

C-2629 Turner, D.G., and Drilling, J.S. (1984). "LS M+34°26, An Unusual B Supergiant Located Near the Outer Edge of the Galaxy." Publ. Astron. Soc. Pac. C-2630 Schechter, P.L., Ulrich, M.H., and Boksenberg, A. (1984). "NGC 4650A: The Rotation of the Diffuse Stellar Component." Ap. J. 277, 526.

C-2631 Caldwel I, C.N. (1984) . "A Survey of [01 IJ Emission in Elliptical Galaxies." Publ. Astron. Soc. Pac.

C-2632 Aaronson, M., Schommer, R.A., and Olszewski, E.W. (1984). "AM-1: A Very Distant Globular Cluster." Ap. J. 276, 221.

C-2633 McAlary, C.W., Madore, B.F., and Davis, L.E. (1984). "The Distance to IC 1613 from Infrared Photometry of Cephe ids."

C-2634 Grindlay, J.E., Petro, L.D., and McClintock, J.E. (1984). "Optical Identification of 2S 1417-62." Ap. J. 276, 621 .

C-2635 Wampler, J.E., Gaskell, CM., Burke, W.L. and Baldwin, J.A. (1984). "Spectrophotometry of Two Complete Samples of Flat Radio Spectrum Quasars." Ap. J. 276, 403.

C-2636 Wing, R.F., and Dean, CA. (1983). "Spectral Classification of Nearby Stars." in IAU Colloquium No. 76 "The Nearby Stars and the Stellar Luminosity Function," eds. A.G.D. Philip and A.R. Upgren (Van VI eck Obs. Contribution No. 1).

C-2637 Graham, J.A., and Nemec, J.M. (1984). "A Survey of Magellanic Cloud Clusters," in IAU Symposium No. 108 , Structure and Evolution of the Magellanic Clouds; eds. S. van den Bergh, and K.S. de Boer (D. Reidel Dordrecht) p. 20

C-2638 Graham, J.A. (1984). "RR Lyrae Stars and Novae in the Magellanic Clouds." in IAU Symposium No. 108, The Structure and Evolution of the Magellanic Clouds; eds. S. van den Bergh, and K.S. de Boer (D. Reidel: Dordrecht) p.

C-2639 Melnick, J., and Quintana, H. (1984). "Optical Studies of Southern Clusters of Galaxies III: of Photoelectric Photometry of Galaxies in 15 Clusters." Astron .J.

C-2640 Carney, B.W. (1984). "Nova Normae 1983." IAU Circu lar No. 3888.

C-2640 Garrison, R.F., Schild, R.E., Hiltner, W.A., and Krzeminski, W. (1984) . "CPD -48°1577: The Brightest Known Cataclysmic Variable." Ap. J. Lett. 276, L13.

C-2642 Hesser, J.E., Harris, H.C., van den Bergh, S., and Harris, G.L.H. (1984). "The NGC 5128 Globular Cluster System." Ap. J. 276, 491.

C-2643 Blanco, V.M., McCarthy, M.F., and Blanco, B.M. (1984). "Giant M Stars in Baade's Window." Astron .J.

C-2644 Conti, P.A., and Garmany, CD. (1984). "SK-71°34: A New Wolf-Rayet Star in the Large Magellanic Cloud." Publ. Astron. Soc. Pac.

C-2645 Demers, S., Beland, S., and Kunkel, W.E. (1983). "The Structure of the Carina Dwarf Elliptical Galaxy." Publ. Astron. Soc. Pac. 95, 354.

C-2646 Osmer, P.S. (1984). "Observatory Report Cerro Tololo Inter-American Observatory." Bull. Am. Astron. Soc.

C-2647 Schmidt, E.G. (1984). "Yellow Giants in Young Clusters I. Photometric Observat ions." Ap. J. Supp I.

C-2648 Schaeffer, B. et al. (1984). "An Intercontinental Baseline Coincidence Search for Optical Flashes with Two Schmidt Telescopes." Ap. J. 21

C-2648 Eggen, O.J. (1984). "A Systematic Search for Members of the Hyades Super- cluster I. The White Dwarfs." Astron . J.

C-2650 Eggen, 0. J. (1984). "The A0 Stars." Ap . J. Supp I.

C-2651 Eggen, O.J. (1984). "A Systematic Search for Members of the Hyades Super- cluster II. The Visual Binaries." Astron .J.

C-2652 Kodaira, K., and Philip, A.G.D. (1984). "On the Metallicity of Blue HorizontaI-Branch Stars in M4 and NGC 6797." Ap. J. 278, 201.

C-2653 McCarthy, M.F., and Blanco, V.M. (1984). "Cool Stars in the Magellanic Clouds and in the Direction of the Galactic Center." Memoirs del la Societa Astronomica Italiana 54, 65, and Proceedings of the Frascati Workshop 1982, held at Vulcano, September 6 to 10. Istituto di Astrofisica Spaziale Consiglio Nazionale delle Ricerche.

C-2654 Kodaira, K., and Philip, A.G.D. (1984). "High-Dispersion Spectroscopic Investigation of Field HorizontaI-Branch, High-Luminosity, and Main-Sequence Stars." Ap. J. 278, 208.

C-2655 Ringuelet, A.E., Sahade, J., Rovira, M., Fontenia, J.M., and Kondo, Y. (1984). "Simultaneous IUE and Ground-Based Observations of V923 A q u i Iae ." Astron. & Astrophys. 131, 9. 22

VI. MISCELLANEOUS

A. Personnel Notes

P; Seitzer, Assistant Astronomer, left CTIO on January

14 to take up a new post on the scientific staff at KPNO.

R. Donoso, Administrative Specialist in charge of the Tololo

Warehouse died of heart failure on January 15. Sr. Donoso had worked at CTIO for 15 years.

T. Ingerson of the University of Idaho joined the CTIO staff on March 1 as Senior Support Scientist, after spending

8 months as Consultant on Observatory Projects.

J. Graham, Astronomer, was elected Vice President of the

AAS and will take over this office at the June meeting.

B. Visitors

P. Conti, JILA, University of Colorado, and Mrs. Conti arrived on January 21 to spend 3 1/2 months at CTIO under the

Visiting Resident Scientist program.

P. Schechter, Mt. Wilson and Las Campanas Observatories visited CTIO on January 16 and gave a talk at the weekly staff tea. M. Dennefeld, European Southern Observatory also gave a talk at the staff tea on February 1.

P. de Yonge of the Max-Planck Radio Telescope in Grenoble and R. Booth, Nuffield Radio Astronomy Laboratories, Jodrell

Bank visited CTIO and the Columbia University radio telescope installations on February 9. N. Carleton, Harvard-Smithsonian Center for Astrophysics, 23

spent February 13-24 at CTIO as Consultant on the new 4m Telescope

Project. M'. Roberts and R. Havlen of the National Radio Astronomy

Observatory visited CTIO March 19-22. C. Enterline, Manager of the CTIO Support Office in Tucson, visited CTIO February 26 - March 5.

R. Williams , ESO and NASA Ames Research Center, and Mrs. Williams arrived at CTIO on March 27 to spend two months here under the Visiting Resident Scientist program.

C. MEETINGS J. Graham and P.S. Osmer attended the 163rd Meeting of the AAS in Las Vegas January 8-11. Dr. Osmer presented a paper on the CTIO new telescope project. P.S. Osmer attended the NOAO Management Committee meetings in Tucson together with J. Frogel and J. Way on January 7 and

March 26,27. In March Dr. Osmer also attended the Annual AURA Board meeting on March 21-23 accompanied by J. Way, and the KPNO/CTIO Standing Committee meeting on March 19-20. J. Graham attended the Workshop on Halos of Galaxies at KPNO on January 16-20. He also attended the meeting, "Protostars and Planets" and gave a poster paper. B. Atwood and M. Phillips attended the Supermicro Workshop in Chapel Hill on January 20-22. Part of the AURA Observatories Visiting Committee met in La Serena February 14-16. The committee members who attended 24

were: Chairman, R. Gehrz, University of Wyoming; G.A. Newkirk,

National Center for Atmospheric Research; and G. Preston, Mt. Wilson and Las Campanas Observatories. Also present for this meeting were J. Jefferies, NOAO, and N. Carleton, Harvard-Smithsonian

Center for Astrophysics.

KITT PEAK NATIONAL OBSERVATORY

MEMO TO John Jefferies DATE: 30 April 1984 RECEIVED FROM: Geoffrey Burbidge ' /2 NOAO

SUBJECT: Quarterly Report MAY 0 i 1984

DIRECTOR'S nenre

Attached is the KPNO Quarterly Report for the period 1 January 31 March 1984 for distribution by you to:

NSF J. Teem Visiting Committee KPNO/CTIO Standing Committee

We have distributed copies to the appropriate staff at KPNO, and P. Osmer, J. Way, J. Zirker, F. Hegwer, J. Beckers, and R. Giacconi.

fed

Enclosure

KITT PEAK NATIONAL OBSERVATORY

NATIONAL OPTICAL ASTRONOMY OBSERVATORIES*

QUARTERLY REPORT

JANUARY - MARCH 1984

*Operated by the Association of Universities for Research in Astronomy, Inc. under Contract No. AST 78-27880 with the National Science Foundation.

TABLE OF CONTENTS

Page

I. SCIENTIFIC HIGHLIGHTS 1

A. JETS IN A REGION OF STAR FORMATION 1

B. FLASHES IN THE SKY 2

C. THE COLORS OF GIANT EARLY-TYPE GALAXIES 3

D. ABUNDANCE - LUMINOSITY EFFECTS IN LATE-TYPE GALAXIES 4

E. THE FIRST SPECTRUM OF THE NUCLEUS OF COMET HALLEY 5

II. DIRECTOR'S OFFICE 7

A. LIBRARY 7

B. PHOTOGRAPHIC LABORATORY 17

C. INFORMATION SERVICES 18

III. SCIENTIFIC STAFF AND VISITORS 23

IV. TELESCOPE USAGE STATISTICS 27

V. ENGINEERING AND TECHNICAL SERVICES 35

A. GENERAL ACTIVITIES 35

B. RESEARCH AND DEVELOPMENT (R&D) PROGRAM 35

C. TELESCOPE SYSTEMS PROGRAM (TSP) 37

D. INSTRUMENT SYSTEMS PROGRAM (ISP) 39

E. NON-KPNO WORK 42 VI. OPERATIONS SUPPORT DIVISION 44

A. OFFICE OF THE DIRECTOR, OPERATIONS SUPPORT DIVISION (OSD) 44

B. TUCSON OPERATIONS DEPARTMENT 44

. C. KITT PEAK OPERATIONS DEPARTMENT 44

D. OBSERVING SUPPORT DEPARTMENT 46

E. COMPUTER SUPPORT DEPARTMENT 47

APPENDIX A- OBSERVATIONAL PROGRAMS 55 KITT PEAK NATIONAL OBSERVATORY

QUARTERLY REPORT

January - March 1984

I. SCIENTIFIC HIGHLIGHTS

A. JETS IN A REGION OF STAR FORMATION

Collimated, high-velocity outflows of gas are often found in regions of recent star formation. Signs of these outflows include broad molecular emission-line profiles, shock-excited emission lines and high-velocity H20 maser activity. Recently, highly collimated and oppositely directed optical emission jets have been observed towards several young stellar objects, and this frequent occurrence of outflows suggests that this phase is a characteristic of the pre-main sequence evolution of most, if not all, stars. One of the best examples of collimated outflow that is known is centered on the infrared source IRS-5 which is in the dark cloud L1551. This object has been the subject of observations by R. L. Snell (Five College Radio Observatory, University of Massachusetts), J. Bally (A.T. & T. Bell Laboratories) and S. E. Strom and K. Strom (University of Massachusetts) at both the VLA and at Kitt Peak.

The Kitt Peak observations were made with a CCD at the 0.9-m telescope using V,R,I and an H-a filter. The main idea was to map the shock-excited gas associated with the mass outflow and also to chart the regions dominated by scattered light from the embedded young objects. The pictures of IRS-5, that were taken through the V and I filters, map the scattered light component, while those taken through the R and H-a filters trace the images of the shocked gas. The VLA radio observations showed that there are two oppositely directed jets that extend for more than 10 arcsec from IRS-5 along the direction of the previously known bipolar molecular outflow. The optical images, obtained with the CCD at Kitt Peak, reveal an optical jet that comes from the southwest of IRS-5 and which coincides with this new radio jet. There is no optical emission, however, associated with the radio jet on the northeast side.

The absence of the optical emission on the northeast side is best explained by the presence of a dense disk of gas that lies perpendicular to the outflow axis in such a way that it obscures the jet on the northeast side but not that to the southwest. This disk whose density is estimated to be 10 atoms cm-^, may also be responsible for collimating the outflow into the two oppositely directed jets. Additional evidence for this disk has been provided by Nagata, Sato and Kobayashi who deduced that a disk oriented perpendicular to the bipolar outflow might be producing (by anisotropic scattering) the polarization that they observed.

Snell et al. observed an extended reflection nebulosity in their broadband R and I images of IRS-5 which seems to delineate the walls of a cavity that is formed by the interaction of the collimated wind from IRS-5 with the ambient molecular cloud. Near IRS-5, the cavity has a diameter of only about 6 arcsec, but some 10 arcsec from it there is a region of rapid expansion; then the jet is recollimated farther out - probably when the pressure in the jet decreases to the point where equilibrium with the pressure in the ambient medium is re-established.

B. FLASHES IN THE SKY

Gamma-ray bursters are a new and mysterious class of object whose nature is unknown. Optical counterparts of these gamma-ray bursts have recently been identified on archival astronomical photographic plates that were taken for some other purpose at the time that the gamma-ray burst occurred. Such identifications must remain rather uncertain, however, until it can be shown that it is highly unlikely that these optical bursts were not caused in some other way. Optical emission of short duration could be produced by astronomical sources such as meteors, flare stars or x-ray bursters. The emission might also be caused by some non- astronomical source such as an aircraft light or the momentary reflection from an artificial satellite at an unusual angle; besides these, there are various kinds of defects that can occur in a photographic emulsion that could mimic an optical burst from the gamma-ray source. Clearly, the detection of a burst is a formidable problem; the bursts are probably rather infrequent, and so a lot of observing is needed, and ways must be found to distinguish the real burst from a variety of imitators.

This observational challenge has recently been taken up by B. E. Schaefer, R. Vanderspeck, H. Bradt and G. Ricker (Massachusetts Institute of Technology). It happens that there are two very similar Schmidt telescopes at the National Optical Astronomy Observatories at Kitt Peak and Cerro Tololo. In Arizona, Kitt Peak has the Burrell Schmidt of Case Western Reserve University, while in Chile, Cerro Tololo has the Curtis Schmidt of the University of Michigan. These Schmidt telescopes take wide-field (5.5 degrees square) photographs of identical scale that can easily be compared. The artificial sources that might be mistaken for the gamma-ray optical emission are all relatively nearby and so could not possibly produce similar effects on plates taken from observatories that are thousands of miles apart. It would also, of course, be extremely unlikely for any image-defects to be mistaken for a "burst" when two plates are available. The problem of distinguishing a burst from an astronomical source was solved by trailing the plates slightly - in other words, introducing a small error into the tracking so that the star images were slightly elongated. Any very rapid

-2- event would show up as a circular image, but a slower change in the star's brightness would produce an elongated image. Schaefer et al. used these relatively simple techniques to conduct the first survey of its kind for these celestial flashes; they accumulated simultaneous photographs from the two telescopes for nine days in October 1982. These plates were then examined to look for- unelongated images. None were found.

These new data, although giving a negative result, have put a limit on the possible frequency of occurrence of these flashes that is three orders of magnitude lower than was possible from previous studies. This new limit will be most useful to the number of groups around the world who are currently planning to build flash detectors which work electronically. Secondly, the new data has been used to assess the probability that the bursts that were found on the archival plates could have been produced by other astronomical sources; the probability of this has been found to be extremely low.

C. THE COLORS OF GIANT EARLY-TYPE GALAXIES

The colors of early-type galaxies are known to depend on their absolute brightness: the brighter ones are redder. Studies of clusters of early-type galaxies some years ago by Sandage and Visvanathan suggested that this relationship between color and luminosity might be the same for all of these galaxies. It has become doubtful whether such a universal color- magnitude exists; however, various factors such as the environment, ellipticity, and internal velocity dispersion may produce deviations from a simple relation between color and luminosity.

One particular effect is described by the Hausman-Ostriker cannibalism model. Clusters of galaxies are characterized by what is called their Bautz-Morgan type; those of early Bautz- Morgan type show a larger brightness difference between the brightest and second-brightest galaxy in the cluster than those of later Bautz-Morgan type. It has been suggested that the brightest galaxies in the early-type clusters have been built up by cannibalizing smaller galaxies in the cluster. These smaller clusters would be bluer, and so one might expect that the brightest galaxies in clusters of early Bautz-Morgan type would be bluer than those of equal brightness in clusters of late Bautz-Morgan type. The prediction is that they should be about 0.1 magnitude bluer.

P. Lugger (Harvard-Smithsonian Center for Astrophysics) has been trying to see whether this prediction of the Hausman- Ostriker model actually holds. Originally, using galaxy colors from the literature, she did find an effect of the right order; the photometry came from more than one source, however, and it was not certain whether or not systematic errors were affecting this result. Lugger therefore undertook to measure the colors herself using the Mk II computer photometer on the 1.3-m

-3- telescope at Kitt Peak. Her new work gives UBVR photometry for twenty-six, first-ranked cluster members, 14 fainter cluster members and two field galaxies. Many of these galaxies had been measured by other groups of observers, and it was possible to draw some conclusions about systematic differences between the measurements of different observers. These amounted, in some cases, to as much as 0.08 magnitudes; this showed up the difficulty of trying to solve the problem in hand by using the existing data.

The raw colors of the various galaxies had to be corrected for interstellar reddening and also for the K-term. The latter corrects for the effect on the colors of the differing redshifts of the observed galaxies. Galaxies also may contain color gradients within themselves, and so comparisons need to be made in such a way that compensates for this effect. When these had all been taken into account, no difference was found between the brightest galaxies in clusters of different morphologies. The errors of the observations were such that the color difference that was predicted from the cannibalism model can be ruled out at the level of five standard deviations.

D. ABUNDANCE - LUMINOSITY EFFECTS IN LATE-TYPE GALAXIES

For the past several years, W. K. Ford, Jr., and V. C. Rubin (Department of Terrestrial Magnetism, Carnegie Institute of Washington) have been using the RC spectrograph on the 4-m telescope at Kitt Peak to obtain spectra of late-type galaxies at high velocity resolution and high spatial resolution. Late-type galaxies are spirals, and the spectra enable the rotations of these galaxies to be determined from the Doppler displacements of their emission lines. From these rotations, galaxy masses have been deduced as a function of luminosity and morphological type. The other important topic that can be studied from these galaxy spectra is their chemistry - the variations in the elemental abundances within them and as a function of their other properties.

In their new work, Rubin, Ford and B. C. Whitmore (Department of Terrestrial Magnetism) have discovered a correlation between line strengths and luminosity in the spectra of galaxies with prominent spiral disks (Sb and Sc Hubble types). The emis6\s)on line intensity ratio of the forbidden ionized nitrogen lines [Nil] XX 6548+6583 relative to the forbidden ionized sulfur [SII] XX 6717+6731 averaged over a spiral disk (but excluding its nucleus) increases with galaxy luminosity. The [Sill lines are strong in the disks of low- luminosity spirals; the [Nil] lines are strong in the disks of high-luminosity sprials. Now the ratio of the strengths of these lines is a good approximation to the actual ratio of their abundances in the excited gas. Rubin et al. therefore infer that the enhancement of nitrogen by secondary nucleosynthetic processing is greater in the disks of more luminous spirals than less luminous ones; they can also say that it is greater in more massive than less massive spiral galaxies.

-4- It is well established from the early work of Baum, and more recent work by de Vaucouleurs and de Vaucouleurs; Faber and Visvanathan; and Sandage, that elliptical galaxies of high luminosity have redder colors and stronger absorption lines than those of lower luminosity. These observations have been interpreted as showing that the more luminous elliptical galaxies are more- metal rich than the fainter ones. Analogous relations, however, had not been established for spiral galaxies, although within some spiral disks there had been evidence for a decrease in metal abundance with increasing radial distance from the center of the galaxy. The new luminosity-dependent parameters that have been identified by Rubin, Ford and Whitmore should offer valuable tools for studying the chemical history and evolution of spirals; possibly they may also help in establishing the distances to galaxies of earlier type.

E. THE FIRST SPECTRUM OF THE NUCLEUS OF COMET HALLEY

The first spectrum of comet Halley during this apparition, and probably the first ever of the surface of its nucleus, has been obtained with the cryogenic camera at the 4-m telescope by H. Spinrad (U.C. Berkeley), P. Wehinger (Arizona State University) and M. Belton (KPNO).

At the time that the hour-long exposure was made in February 1984, the visual magnitude of the comet was about 23.2, and it was moving at about 19 arcsec per hour against the background of stars on which the telescope tracks. The telescope was therefore guided manually through instructions that were relayed by the astronomers to the telescope operator. The cryogenic camera - which has a cooled CCD at the focus of the spectrograph camera as its detector - is particularly suitable for this type of work; Hyron Spinrad, one of the investigators, described the Kitt Peak telescope-spectrograph combination as "the hottest system available anywhere for faint object spectroscopy in the red."

There was enough signal in the spectrum between wavelengths 0.58 and 0.68 microns to show that the nucleus of the comet is very red. This observation appears to support a conjecture, made previously, that the rocky material in comets is similar to that found on the dark side of Iapetus (a satellite of the planet Saturn) and some of the Trojan asteroids. It is currently thought that these materials can be identified with kerogen that is found in the matrix of carbonaceous chondrite meteorites.

Other Comet News

The periodic comet Giacobini-Zinner was recovered by S. Djorgovski and H. Spinrad (U.C. Berkeley) and M. Belton and G. Will (KPNO) at the prime focus of the 4-m telescope using a new Texas Instruments CCD as the detector. On recovery, the comet had a red magnitude of about 23. This comet has been searched for since well before NASA redirected the ISEE-3 spacecraft (renamed The International Cometary Explorer) on a trajectory

-5- toward the general vicinity of the comet in December 1983. The scientists and engineers who are responsible for this spacecraft were glad to find that the comet (now at a distance of 4.6 astronomical units) was only 4 arcsec from its predicted position; only minimal corrections will be required for the trajectory of the International Cometary Explorer. Until now, there had been questions about the accuracy of the predicted orbit of Giacobini-Zinner because its orbit had previously been known to show the effects of erratic non-gravitational forces.

In August 1983, the periodic comet Crommelin was recovered at Kitt Peak by P. Wehinger and S. Wycoff (Arizona State University) using the RCA CCD on the 0.9 (#1) telescope; the comet had a visual magnitude of about 20. This was well ahead of the International Halley Watch "trial run" on this comet. These, and subsequent observations by several visiting and staff observers, showed that the comet behaved unusually in that it developed an ion tail composed of H20+ rather than the normally dominant C0+ ion.

-6- II. DIRECTOR'S OFFICE

On 3 January 1984 the Kitt Peak Director's office became responsible for the activities of the Photographic Laboratory and the Library in addition to its supervision of the Information Services office.

A. Library

1. During this quarter the library staff compiled the FY- 198 3 publication record for the annual report and updated the card catalog and records of Observatory publications.

2. Kitt Peak National Observatory Papers

The Kitt Peak National Observatory Papers list consists of papers that have been published or have been accepted for publication and will appear in print within two or three months.

The papers are by KPNO staff and visitors or papers that acknowledge use of KPNO facilities.

The list is compiled from preprints, notices by authors, literature searches of astronomical journals, related journals, books and proceedings of meetings, symposia, etc., received during the period January - March 1984.

-7- KITT PEAK NATIONAL OBSERVATORY PAPERS

January 1984

K-4608 Star formation in the M8E region. M. Simon, L. Cassar, M. Felli, J. Fischer, M. Massi, and D. Sanders. (1984, Ap. J.: pt.l, 223., 170-175)

K-4609 Chemical abundances in a new halo planetary nebula. T. Barker and K.M. Cudworth. (1984, Ap. J.: pt.l., 223., 610-614)

K-4610 Near-infrared spectrophotometry of Crab Nebula filaments. R.B.C. Henry, G.M. MacAlpine, and R.P. Kirshner. (1984, Ap. J.: pt.l, 223, 619-629)

K-4611 Stellar populations in local group dwarf ellipticals. II. NGC 205. J. Mould, J. Kristian, and G.S. Da Costa. (1984, Ap. J.: pt.l, 223, 575-581) K-4612 Speckle interferometric measurements of binary stars. IX. H.A. McAlister, W.I. Hartkopf, B.J. Gaston, E.M. Hendry, and F.C. Fekel. (1984, Ap. J. Suppl., 5_4, 251)

K-4613 The incidence of infrared excesses among G-type stars in the direction of the Orion Ic association. A.E. Rydgren and F.J. Vrba. (1984, A. J., fi9_r 399-405)

K-4614 A high resolution infrared spectrum of the Wolf-Rayet star HD 193793. D.L. Lambert and K.H. Hinkle. (1984, PASP, 21, 222-225) K-4615 The cool DC white dwarf Stein 2051B. G. Wegner and F.H. Yackovich. (1984, Ap. J.: pt.l, 221, 240-246) K-4616 The age and compostition of the LMC red globular cluster NGC 2121. P. Flower, D. Geisler, P. Hodge, and E. Olszewski. (1984, Ap. J.: pt.l, 221, 15-34) K-4617 The stellar kinematics and dynamics of barred galaxies. I. NGC 936. J. Kormendy. (1983, Ap. J.: pt.l, 215., 529- 548)

K-4618 The structure and emission spectrum of a nonradioactive shock wave in the Cygnus Loop. J.C. Raymond, W.P. Blair, R.A. Fesen, and T.R. Gull. (1983, Ap. J.: pt.l, 275. 636-644) K-4619 Photometric molecular indices in warm carbon stars: NH, CN, CH and C2. S.R. Yorka. (1983, A. J., £3, 1816-1824) K-4620 Photoelectric photometry of selected SAO stars. III. W.W.G. Scharlach and E.R. Craine. (1983, PASP, 9_5_, 876-877)

-8- K-4621 The period of the intermediate polar V1223 Sgr. A.R. King and G.A. Williams. (1983, R.A.S. Mon. Not., 233, 57-60)

K-4622 V0332 + 53. R.K. Honeycutt and E.M. Schlegel. (1984, IAU Cir. No. 3899)

K-4623 CCD parallax astrometry. D.G. Monet. (1983, The nearby stellar luminosity function, IAU Col. No. 76, ed. by A.G.D. Philip and A.R. Upgren; L. Davis Press: Schenectady, N.Y., pp.435-477)

K-4624 New limits on the surface density of M-dwarfs from CCD and photographic data. P.C. Boeshaar and J.A. Tyson. (Ibid., pp. 85-91)

K-4625 Observational basis for velocity fields in stellar atmo spheres: summaries. L. Goldberg. (1983, Observational basis for velocity fields in stellar atmospheres, ed. by R. Stalio; Trieste Astronomical Obs., pp. 435-477) K-4626 CO emission from the star-burst irregular galaxy NGC 1569 J.S. Young, J.S. Gallagher, and D.A. Hunter. (1984, Ap. J.: pt.l, 223, 476-479)

K-4627 Two new extremely hot pulsating white dwarfs. H.E. Bond, A.D. Grauer, R.F. Green, and J. W. Liebert. (1984, Ap. J.: pt.l, 221, April 15) K-4628 Optical spectrophotometry of the M87 jet and its environs, W.C. Keel. (1984, Ap. J.: pt.l, 223., April 15)

K-4629 HD 46703: A high-luminosity population II F-type star. R.E. Luck and H.E. Bond. (1984, Ap. J.: pt.l, 279. April 15)

K-4630 The kinematics of giant extragalactic H II regions. E.D. Skillman and B. Balick. (1984, Ap. J.: pt.l, 280. May 15)

K-4631 Dense cores in dark clouds: young embedded stars at 2 micrometers. P.J. Benson, P.C. Myers, and E.C. Wright. (1984, Ap. J.: pt.2, 221, April) K-4632 Induced nuclear line activity in interacting spiral galaxies. R.C. Kennicutt, Jr. and W.C. Keel. (1984, Ap. J.: pt.2, 221, April) K-4633 Anomalous emission regions in irregular galaxies. D.A. Hunter. (1984, Ap. J.: pt.2, 223, L35-L39) K-4634 Continuum distributions of an X-ray observed sample of BL LAC objects. I. Cruz-Gonzales and J.P. Huchra. (1984, A. J., Ql, April) K-4635 Radio and infrared observations of optically invisible type II hydroxyl masers. J.D. Fix and R.L. Mutel. (1984, A. J., ££, 406-410)

K-4636 UBVRI & H(alpha) photometry of FK COM. J.A. Holtzman and H.L. Nations. (1984, A. J., £9_, 391-398)

K-4637 X-Ray observations of M33 with the high resolution imager on the Einstein Observatory. T.H. Markert and A.D. Rallis. (1983, Ap. J.: pt.l, 225., 571-577)

K-4638 Infrared observations of the eclipse of Epsilon Aurigae: direct measurements of the 700K secondary at 5,10, and 20 (mu)m. D.E. Backman, E.E. Becklin, D.P. Cruikshank, R.R. Joyce, T. Simon, and A.T. Tokunaga. (1983, AAS Bull., Abst., 23., 925)

K-4639 Spectrophotometry of QSOs in two fields in Hercules. E.M. Burbidge, H.E. Smith, V.T. Junkkarinen, and A.A. Hoag. (1983, AAS Bull., Abst., 15., 959)

K-4640 The National New Technology (NNTT) Telescope Project. G. Burbidge. (1983, AAS Bull., Abst., 15., 1003)

K-4641 The importance of density waves in generating cosmic rays in spiral galaxies I: NGC 3310. N. Duric, E.R. Seaquist P.C. Crane, R.C. Bignell, and L.E. Davis. (1983, AAS Bull., Abst., 15., 944)

K-4642 The suitability of an acoustic sounder as an observatory site evaluation tool. F.F. Forbes. (1983, AAS Bull., Abst., 15., 999)

K-4643 Observations of the 1982 eclipse of 31 Cyg. W. Hagen, R.E. Stencel, J.L. Hopkins, R. Fried, P.C. Schmitdke, Y. Kondo, and R.D. Chapman. (1983, AAS Bull., Abst., 15., 925) K-4644 Variations of total solar irradiance during rapid sun- spot growth. H.S. Hudson, H. Jones, and P. Mcintosh. (1983, AAS Bull., Abst., 15, 950)

K-4645 IUE observations of amorphous galaxies. S.A. Lamb, J.S. Gallagher, M.S.H. Jellming, and D.A. Hunter. (1983, AAS Bull., Abst., 15, 921) K-4646 Variation of solar limb darkening. L.D. Petro, P.V. Foukal, W.A. Rosen, R.L. Kurucz, and A.K. Pierce. (1983, AAS Bull., Abst., 15., 951) K-4647 The cluster of galaxies associated with the quasar 3C 206. H.K.C. Yee. and R.F. Green. (1983, AAS Bull., Abst., 15., 957)

-10- K-4648 Splitting of CIV lines in a Z=1.79 QSO absorption line system. J. Bechtold, D.G. York, R.F. Green, and F.H. Chaffee. (1983, AAS Bull., Abst., 15., 986)

K-4649 Growth of scientific journals. H.A. Abt. (1983, Science, 222, 1280)

K-4650 1240-057: giant jet or colliding galaxies? W. Romanishin. (1984, PASP, 23, 24-27) K-4651 Spectrophotometry of the RS CVn stars. II. A Study of seven systems from (lambda) 4000 - (lambda) 11000 angstrom. S.N. Shore and S.J. Adelman. (1984, Ap. J. Suppl., 51, 151-165)

February 1984

K-4652 AM-1: A very distant globular cluster. M. Aaronson, R.A. Schommer, and E.W. Olszewski. (1984, Ap. J.: pt.l, 223, 221-228) K-4653 PS 1012-029: A high-excitation eclipsing cataclysmic variable. W.R. Penning, D.H. Ferguson, J.T. McGraw, J. Liebert, and R.F. Green. (1984, Ap. J.: pt.l, 276. 233-242)

K-4654 LSS 4300, a hot counterpart of Upsilon Sagittarii and KS Persei. D. Schonberner and J.S. Drilling. (1984, Ap. J.: pt.l, 216., 229-232)

K-4655 The response of chromospheric emission lines to flares on YZ Canis Minoris. S.P. Worden, T.J. Schneeberger, M.S. Giampapa, E.E. Deluca, and L.E. Cram. (1984, Ap. J.: pt.l, 223, 270-280) K-4656 Main-sequence photometry for three galactic globular clusters. W.E. Harris, J.E. Hesser, and B. Atwood. (1983, PASP, £5, 951-966)

K-4657 SIT vidicon photometry for four old Magellanic Cloud clusters. W.E. Harris, J.E. Hesser, and B. Atwood. (1983, PASP, 9_5, 967-978) K-4658 Differential photometry and absolute spectrophotometry of CH Cygni. J.B. Kaler, S.J. Kenyon, and J.P. Hickey. (1983, PASP, 23, 1006-1011) K-4659 Coherent scattering in the solar spectrum: survey of linear polarization in the range 4200-9950 (angstrom). J.O. Stenflo, D. Twerenhold, J.W. Harvey, and J.W. Brault. (1983, A. & A. Suppl., 51, 505-514)

-11- K-4660 High-resolution observations of the 6815 (angstrom) band of methane in the major planets. K.H. Baines, W.V. Schempp, and W.H. Smith. (1983, Icarus, 56., 534-543)

K-4661 Spectroscopic observations of supernova remnant candidates W28, CTBI, and DR4. J. Bohigas, M.T. Ruiz, L. Carrasco, L. Salas, and M.A. Herra. (1983, Rev. Mex. de A. & A., 1, 155-161)

K-4662 Optical and infrared photometry of late-type stars in the Pleiades. J.R. Stauffer. (1984, Ap. J.: pt.l, 280. May 1)

K-4663 A spectroscopic study and mass determination for the cataclysmic variable AC Cancri. E.M. Schlegel, R.H. Kaitchuck, and R.K. Honeycutt. (1984, Ap. J.: pt.l, 280. May 1)

K-4664 The variability of Alpha Orionis. L. Goldberg. (1984, PASP, 23, May)

K-4665 An interpretation of the near-ultraviolet absorption spectrum of SO (sub. 2): implications for Venus, Io and laboratory measurements. M.S.J. Belton. (1983, Moon & The Planets, 21, 250-251)

K-4666 Galaxies: spindle-like galaxies. P.L. Schechter, R. Sancisi, H. van Woerden, and C.R. Lynds. (1983, Mt. Wilson & L. Campanas Obs. Annual Report, pp. 627-630)

K-4667 UBV light curves of the eclipsing binary RS Cephei. D.S. Hall, R.O. Cannon, and C.G. Rhombs. (1984, A. J., 01, April) K-4668 A study of the galaxy W 371 and a nearby companion. J.F. Scholl and E.J. Grayzeck. (1984, PASP, 96., May) K-4669 LSII+34 (degrees) 26, an unusual B supergiant. D.G. Turner and J.S. Drilling. (1984, PASP, 9_6_, May)

K-4670 The NGC 5128 globular cluster system. J.E. Hesser, H.C. Harris, S. van den Bergh, and G.L.H. Harris. (1984, Ap. J.: pt.l, 223, 491-508) K-4671 The distance to IC 1613 from infrared photometry of Cepheids. C.W. McAlary, B.F. Madore, and L.E. Davis. (1984, Ap. J.: pt.l, 223, 487-490) K-4672 Accuracy of spectral classification. H.A. Abt. (1983, Current techniques in double and multiple star research, IAU Col. No. 62, ed. by R.S. Harrington and O.G. Franz; Lowell Obs.: Flagstaff, pp. 118-119)

-12- i.

K-4673 Five years of double star interferometry and its lessons. H.A. McAlister. (Ibid., pp. 125-144)

K-4674 Astrometric properties of the KPNO 4m telescope-prime focus CCD detector system. D.G. Monet. (Ibid., p. 219)

K-4675 Spectral classification of composite spectrum stars. P.C. Schmidtke (Ibid., p. 228)

K-4676 Fourier techniques for binary star orbit determination. D.G. Monet. (Ibid., p. 286) K-4677 Spectroscopic studies of Wolf-Rayet stars with absorption lines. VIII. HD 193793. P.S. Conti, D. Roussel-Dupre, P. Massey, and M. Resing. (1984, Ap. J.: pt.l, 231, June 15)

K-4678 The kinematics of the narrow line region in active galaxies and quasars III: correlations with the broad- line region and radio emission. T.M. Heckman, G.K. Miley, and R.F. Green. (1984, Ap. J.: pt.l, 281, June 15) K-4679 The chemical composition of globular clusters: global trends. CA. Pilachowski. (1984, Ap. J.: pt.l, 2JL1, June 15)

K-4680 Absolute spectrophotometry of northern Wolf-Rayet stars: how similar are the colors? P. Massey. (1984, Ap. J.: pt.l, 231, June 15) K-4681 Photometric study of NGC 2023 in the 3500 (angstrom) to 10000 (angstrom) region: confirmation of a near- infrared emission process in reflection nebulae. A.N. Witt, R.E. Schild, and J.B. Kraiman. (1984, Ap. J.: pt.l, 231, June 15) K-4682 The triple nature of the short period RS CVn system HD 86590. S.C. Barden. (1984, A. J., 01, May) K-4683 The giant branch of the old open cluster M67. K.A. Janes and G.H. Smith. (1984, A. J., 01, April) K-4684 A long-period orbit for the binary Wolf-Rayet star HD 193793, W7 + 04-5. R. Lamontagne, A.F.J. Moffat, and W. Seggewiss. (1984, Ap. J.: pt.l, 221, 258-262) K-4685 Deep CCD photometry in globular clusters. I. The main sequence of M4. H.B. Richer and G.G. Fahlman. (1984, Ap. J.: pt.l, 222, 227-234) K-4686 AU Pegasi, the binary Cepheid outside the instability strip. H.C. Harris, E.W. Olszewski, and G. Wallerstein. (1984, A. J., 01, 119-125) -13- K-4687 An investigation of T Tauri variability. J.T. Schmelz. (1984, A. J., 01, 108-114)

K-4688 .Alfven waves and turbulence in quiescent prominences. E. Jensen. (1983, Solar Phys., 01, 275-285)

K-4689 Digital imagery of the x-ray Pulsar 2259 + 586. B. Margon and S.F. Anderson. (1984, Astrop. Letters, 21, 211-215) ttaicii 1984

K-4690 Interstellar absorption lines in the infrared spectrum of NGC 2024 IRS 2. J.H. Black and S.P. Willner. (1984, Ap. J.: pt.l, 221, April 15)

K-4691 An upper limit to the shell size of (zeta) Tauri. P.C. Schmidtke and A.L. Africano. (1984, A. J., 89, May)

K-4692 Periodic Comet Crommelin (1983n). H. Spinrad, P. Wehinger, S. Wyckoff, and M. Belton. (1984, IAU Cir. No. 3914)

K-4693 Spiral galaxies in clusters V: radical gradients in Coma and A1367. G.D. Bothum, R.A. Schommer, and W.T. Sullivan, III. (1984, A. J., 01, April)

K-4694 Photometric solutions for U Cephei. E.C. Olson. (1984, PASP, 23, 162-166) K-4695 Modeling National New Technology Telescopes. J.M. Yarborough. (1984, Sky & Tel., £2, 225)

K-4696 GD 323: A white dwarf with a stratified H/He atmosphere. J. Liebert, F. Wesemael, E.M. Sion, and G. Wegner. (1984, Ap. J.: pt.l, 222, 692-699)

K-4697 Optical properties of the knots in NGC 73 85. S.M. Simkin, G.V. Bicknell, and A. Bosma. (1984, Ap. J.: pt.l, 222, 513-525)

K-4698 H and K Ca II plage profiles obtained with a Fourier transform spectrometer. P. Lemire. (1984, Solar Phys., M, 31-34) K-4699 Further photometric surveys for white dwarfs in Praesepe, B.J. Anthony-Twarog. (1984, A. J., 01, 267-273) K-4700 Periodic Comet Crommelin (1983n). P.A. Wehinger, H. Spinrad, S. Wyckoff, and M.J.S. Belton. (1984, IAU Cir. No. 3927)

-14- K-4701 Preliminary results from eclipse coronal velocity observations. W. Livingston and J. Harvey. (1982, Total solar eclipse of 16 February 1980; results of observations, ed. by S.K. Trehan; Indian Natl. Science Academy: New Delhi, pp. 18-28).

K-4702 A study of extreme carbon stars—I. Silicon carbide emis sion features. M. Cohen. (1984, R.A.S. Mon. Not., 206. 137-147)

K-4703 Optical region elemental abundance analyses of B and A stars - I. PI Ceti, 134 Tauri, HR 2154, HR 5780, 21 Aquilae and NU Capricorni. S.J. Adelman. (1984, R.A.S. Mon. Not., 233, 637-648)

K-4704 Optical region elemental abundance analyses of B and A stars - II. The hot AM stars (omicron) Pegasi and (sigma) Aquarii and the marginal peculiar A star (nu) Cancri. S.A. Adelman, J.M. Young, and H.E. Baldwin. (1984, R.A.S. Mon. Not., 233, 649-660) K-4705 Ca II emission surface fluxes in active chromosphere stars. B.W. Bopp. (1984, Ap. J. Suppl., 51, March)

K-4706 The bright end of the color-magnitude relation for early- type galaxies in clusters. P.M. Lugger. (1984, Ap. J.: pt.l, 223, 51-60) K-4707 Absolute spectrophotometry of Wolf-Rayet stars from 1200 to 7000 (angstrom): a cautionary tale. CD. Garmany, P. Massey, and P.S. Conti. (1984, Ap. J.: pt.l, 278. 233-240)

K-4708 The Infrared Astronomical Satellite (IRAS) Mission. G. Neugebauer, H.J. Habing, R. van Duinen, H.H. Aumann, B. Baud, CA. Beichman, D.A. Beintema, N. Boggess, P.E. Clegg, P.C. Gillett, T. de Jong, J.P. Emerson, T.N. Gautier, S. Harris, M.G. Hauser, J.R. Houck, R.E. Jennings, F.J. Low, P.L. Masden, G. Miley, F.M. Olnon, S.R. Pottasch, E. Raimond, M. Rowan- Robinson, B.T. Soifer, R.G. Walker, P.R. Wesselius, and E. Young. (1984, Ap. J.: pt.2, 223, L1-L6) K-4709 The IRAS minisurvey. M. Rowan-Robinson, P.E. Clegg, CA. Beichman, G. Neugebauer, B.T. Soifer, H.H. Aumann, D.A. Beintema, N. Boggess, J.P. Emerson, F.C Gillett, T.N. Gauter, M.G. Hauser, J.R. Houck, F.J. Low, and R.G. Walker. (1984, Ap. J.: pt.2: 221, L7-L10)

-15- K-4710 Infrared Cirrus: new components of the extended infrared emission. F.J. Low, D.A. Beintema, T.N. Gautier, F.C Gillett, CA. Beichman, G. Neugebauer, E. Young, H.H. Aumann, N. Boggess, J.P. Emerson, H.J. Habing, M.G. Hauser, J.R. Houck, M. Rowan-Robinson, B.T. Soifer, R.G. Walker, and P.R. Wesselius. (1984, Ap. J.: pt.2: 278. L19-L22)

K-4711 Discovery of a shell around Alpha Lyrae. H.H. Aumann, F.C. Gillett, CA. Beichman, T. de Jong, J.R. Houck, F.J. Low, G. Neugebauer, R.G. Walker, and P.R. Wesselius, (1984, Ap. J.: pt.2, 278. L23-L27)

K-4712 Far-infrared observations of the Crab Nebula. P.L. Marsden, F.C Gillett, R.E. Jennings, J.P. Emerson, T. de Jong, and F.M. Olnon. (1984, Ap. J.: pt.2, 27 8. L29-L32)

K-4713 The formation of solar type stars: IRAS observations of the dark cloud Barnard 5. CA. Beichman, R.E. Jennings, J.P. Emerson, B. Baud, S. Harris, M. Rowan-Robinson, H.H. Aumann, T.N. Gautier, F.C. Gillett, H.J. Habing, P.L. Marsden, G. Neugebauer, and E. Young. (1984, Ap. J.: pt.2, 221, L45-L48)

K-4714 Unidentified point sources in the IRAS minisurvey. J.R. Houck, B.T. Soifer, G. Neugebauer, CA. Beichman, H.H. Aumann, P.E. Clegg, F.C. Gillett, H.J. Habing, M.G. Hauser, F.J. Low, G. Miley, M. Rowan-Robinson, and R.G. Walker. (1984, Ap.J.: pt.2, 221, L63-L66)

K-4715 Infrared galaxies in the IRAS minisurvey. B.T. Soifer, M. Rowan-Robinson, J.R. Houck, T. de Young, G. Neugebauer, H.H. Aumann, CA. Beichman, N. Boggess, P.E. Clegg, F.C. Gillett, J.P. Emerson, H.J. Habing, M.G. Hauser, F.J. Low, G. Miley, and E. Young. (1984, Ap. J.: pt.2, 221, L71-L74) K-4716 Diagnostics of solar magnetic fluxtubes using a Fourier transform spectrometer. J.O. Stenflo, J.W. Harvey, J.W. Brault, and S. Solanki. (1984, A & A, 121, 333-346) K-4717 On the periods of RZ Comae and V1073 Cygni. Z. Asian and T.J. Herczeg. (1984, IAU Inf. B. on V. Stars, No. 2478)

-16- B. Photographic Laboratory The photo lab was involved in tests in preparation for two papers to be presented by Mark Hanna at the I.A.U. meeting in Scotland in early April. The first paper titled "Using a Gossen Light Meter to Produce Enlarged Interpositive's Film Copies from Glass Plates" describes a technique whereby an ordinary light meter can be used as a film plane light meter to produce consistent interpositives with minimal waste.

The second paper titled "Unsharp Masking at the Enlarger" describes how the unsharp masking technique (usually confined to contact printing) could be done at the enlarger with enlarged images, making registration much less critical. The process was worked out using very simple inexpensive tools so minimally equipped dark rooms could afford to try this technique.

A wide-angle, large-format lens was ordered for use in taking photos of telescope interiors and instrumentation.

During this quarter 264 work orders were received and 5,900 print units were produced.

-17- In January the Information Services Office hosted a two-day conference for Public Information personnel from major U. S. Observatories and National Centers. Attending were representatives from:

National Astronomy & Ionosphere Center Harvard-Smithsonian Center for Astrophysics Yerkes Observatory Cerro Tololo Intei—American Observatory Sacramento Peak Observatory McDonald Observatory National Center for Atmospheric Research Space Telescope Science Institute The agenda included such topics as Observatory publica tions, reproduction policies and fees, copyright policies and procedures, pricing policies and marketing of Observa tory photographic materials.

About 275 photo entries have been received in the 1985 NOAO Calendar competition. This publication should be in press by mid-summer.

The Visitor Center is now under the supervision of this Office, having been transferred from Operations Support in January. Joe Underwood retired on February 29. Don Karl Is serving as acting manager of the Visitor Center. Tony Enci- nas was hired as a tour guide in mid-March.

Stephen Meszaros resigned in March to return to NASA, Greenbelt, Maryland. Del Hewitt is the Acting Information Services Coordinator.

2. Media Suppgct/c

a. Newspaper and Magazine Coverage:

Ninety-four press clippings were sent to us by the Luce Press Clipping Service and other sources. Of these, 30 referred to light pollution. "Rings around other stars" was the topic of 18, and 16 were about super clusters of galax ies.

-18- Eric Brus, of Science Almanac conducted a phone intei— view with Geoffrey Burbidge on the subject of the NNTT pro ject.

b. T.V./Radio Coverage:

Fred Gillett was interviewed by two Tucson T.V. chan nels in early January about his discovery of a possible solar system around the star Vega.

Geoffrey Burbidge was interviewed "live" from the Observatory for a local T.V. Channel news program on the proposed space station and how it relates to the future of astronomy.

David Crawford was Interviewed by a Phoenix T. V. Chan nel on the dark sky ordinances being considered by Phoenix. The taping was done locally and relayed to Phoenix.

On Thursday, March 8, a Tucson T. V. Channel did its weather report from Kitt Peak and interviewed Caty Pllachowski.

Stephen Meszaros gave an ovei—the-phone interview to KAIR Radio, Tucson, concerning President Reagan's State of the Union Address in which Reagan proposed the building of a space station by NASA.

Helmut Abt gave a phone interview to a Community Col lege radio station in Centerville, Iowa about the dedication of Kitt Peak on March 15, 1960.

3_. Hansen Planetarium Activities

The Hansen Planetarium announced the selection of a new director. Von Del Chamberlain. He arrived on March 1 to replace former director, Mark Littmann, who had vacated the post last summer.

-19- 4. Mountain Visitor Center

Visitors Jan.-March

31,030 1984 31,145 1983 27,008 1982 28,508 1981

In the period December 1, 1983 through March 31, 1984, 72 regularly scheduled guided tours were given to visitors to the mountain. In addition, 76 special tours were given. They included the following:

Elementary and Junior High School Groups - 19 High School Groups (including schools from California, Colorado, Connecticut, Tempe, and Phoenix) - 6 Gifted Classes - 2 Universities (including Iowa, A.S.U./Tempe, N.A.U./ Flagstaff, U of A, and Pima Comm. College) - 5 Senior Citizen Groups - 6 Elderhostel - 3 Church Groups - 5 Indian Groups - 3 Mexican Groups - 3 Public Nights - 3 VIP Request Tours - 11 Cub Scouts - 2; Boy Scouts - 1; YMGA - 1; Museums - 2; Drug, Alcohol Rehab. - 4

The mountain tour guides also gave 7 presentations to classes at local schools.

5. Office Sales $575.20 — Catalog cash and Invoiced sales. $1,604.15*— Non-catalog cash and invoiced sales,

$2,179.35 — Total

♦Includes the sale of six films at $250 ea.: five calories and one Science: Woman's Woxk..

-20- £. Pictfi Requests, Ellm Orders, and Written Responses £s Entile Inquiries.

1984 1983 1982 Photo Requests 26 54 59 Films Distributed* 71 77 32 Written Responses 196 308 379

*Summary si Ella Lsan Program: 20 Journey into Light 3 Skies of the Andes 18 Stars, Galaxies, and Southern Skies 10 Science: Woman's Work 20 The Observatories

71 Total

Tourist information brochures distributed this quartei 6,400.

1• Miscellaneous

Several members of the Kitt Peak staff visited local organizations to give presentations about astronomy and Kitt Peak. The groups checked out slides from Information Ser vices' slide loan program and all expressed appreciation for this valuable resource. Those using the slides and slide projector from the office included: Peter Allan, Richard Green, Bill Keel, Jeff Pier, and Paul Schmidtke.

Myron Smith presented a "Space" talk to first graders in Austin, Texas.

Stephen Meszaros attended the AAS Meeting in Las Vegas in early January to present a Kitt Peak exhibit of photos and the NNTT models.

A Kitt Peak photo exhibit was shown at the Fourth Annual Space Symposium held at the University of Arizona in late February.

Visitors hosted by this office included: Anthony Y. T. Chan and Kwong Siu Cheung, Assistant Curators from the Hong Kong Space Museum.

-21- Allen Freeman, Managing Editor for Architecture Maga zine.

Bill Knight, a free lance reporter from Peoria, Illi nois, who is writing a series of articles on the space pro gram and is including Kitt Peak in one of the articles. He interviewed astronomers David Crawford and Dave De Young and visited the mountain.

-22- III. SCIENTIFIC STAFF AND VISITORS

Scientific staff and administrative changes for this quarter were as follows: John S. Gallagher, III was hired as an Astronomer/tenure on January 16, 1984.

Philip Massey was hired as an Assistant Astronomer on January 16, 1984.

Stephen Meszaros resigned as Information Services Coordinator on March 22, 1984.

Visitors who arrived during this quarter were:

G. Aldering The University of Michigan February 1984

S. Anderson University of Washington February 1984

T. Armandroff Yale University January 1984

T. Beers California Institute of Technology January 1984

*J.-F. Blavier Universite de Liege January 1984

D. Carbon Lick Observatory February 1984 - March 1984

B. Carney The University of North Carolina January 1984

E. Craine E/ERG, Inc. March 1984

R. Culver Colorado State University January 1984, March 1984

-23- R. Fesen University of Colorado January 1984

D. Fraquelli The University of Georgia January 1984

W. Freedman University of Toronto January 1984

D. Hamilton The University of Chicago January 1984 - August 1984

J. Hewitt Massachusetts Institute of Technology February 1984

P. Hintzen NASA/Goddard Space Flight Center January 1984

E. Hu Space Telescope Science Institute March 1984

A. Jakobsen Aarhus Universitet February 198 4 - June 1984

C. Kellett National Science Foundation March 1984

J. Kormendy Dominion Astrophysical Observatory January 1984 - February 1984

M. Kurtz Center for Astrophysics February 1984

A. Lasenby Jodrell Bank March 1984 - June 1984

J. Mahoney Massachusetts Institute of Technology February 1984

-24- B. Margon University of Washington March 1984

M. McCarthy Vatican Observatory February 1984 - May 1984

R. Milkey Association of Universities for Research in Astronomy, Inc. March 1984

D. Morton Anglo-Australian Observatory January 1984

J. Narlikar Tata Institute of Fundamental Research February 1984 - June 1984

E. Olszewski Dominion Astrophysical Observatory January 1984 - February 1984

*G. Penrod Lick Observatory February 1984

R. Peterson Lockheed Palo Alto Research Laboratories January 198 4 - June 198 4

W. Romanishin NASA/Goddard Space Flight Center March 1984

E. Sadler European Southern Observatory March 1984

G. Schievn University of Massachusetts March 1984

*W. Smith Washington University in St. Louis March 1984

*R. Stalio Trieste Observatory January 1984 - July 1984

-25- K. Strom University of Massachusetts March 1984

S. Strom University of Massachusetts March 1984

G. Steigman Bartol Research Foundation January 1984 - February 1984

P. Thejll University of Delaware March 1984 - April 1984

S. van den Bergh Dominion Astrophysical Observatory January 1984

S. Van Dyk University of Washington March 1984

R. Walker U. S. Naval Observatory January 1984

P. Wehinger Arizona State University February 1984, March 1984

*G. Williams Commonwealth Scientific and Industrial Organization February 1984 - March 1984

S. Wolff University of Hawaii March 1984

♦Visitor to National Solar Observatory

-26- IV. TELESCOPE USAGE STATISTICS

1 January through 31 March 1984

4m telescope

Sched Usabl e Sched Usable Nights * Hours $ Days $ Hours *

Visitor 71 .24 82. 4 661 .57 83-3 10.80 71.1 70.86 73.1 Staff 15-26 17- 6 132. 48 16.7 4.40 28.9 26.04 26.9 subtotal 86.50 100. 0 794. 05 100.0 15-20 100.0 96-90 100.0

Engineering 4-50 4. 9 49. 00 5-8 0.00 0.0 0.00 0.0 Shutdown 0.00 o. 0 0. 00 0.0 0.00 0.0 0.00 0.0 Open Time 0.00 o. 0 0. 00 0.0 0.00 0.0 0.00 0.0 Oper. Train 0.00 0. 0 0. 00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0 0 0. 00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0 0 0 00 0.0 0.00 0.0 0.00 0.0 Request Obs 0.00 0 .0 0 00 0.0 0.00 0.0 0.00 0.0 Test & Eval 0.00 0 .0 0 .00 0.0 0.00 0.0 0.00 0.0 Public Info 0.00 0 .0 0 .00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0 .0 0 .00 0.0 0.00 0.0 0.00 0.0 total 91 .00 4 •9 843 •05 5.8 15.20 0.0 96.90 0.0

Night Down Time

Reason Hours

Weather 219-45 20.4 Other 6.50 0.6 KPNO I nstrument 2.00 0.2 Computer 5-25 0.5 Software 1 .50 0.1

Total 234-70 21 .8

Day Down Time

Reason Hours

Weather 31.00 23-6 Computer 1 .00 0.8 KPNO I nstrument 2.00 1 -5 Software 0.50 0.4

Total 34.50 26-3

-27-

2.1m telescope

Sched Usable Sched Usable Nights $ Sours * Days % Hours *

Visitor 69-99 80-9 592.63 79-8 0.00 0.0 0.00 0.0 Staff 16.51 19-1 149-67 20.2 0.00 0.0 0.00 0.0 subtotal 86-50 100.0 742.30 100.0 0.00 0.0 0.00 0.0

Engineering 4-50 4-9 44.00 5-6 0.00 0.0 0.00 0.0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Open Time 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 o.o Test & Eval. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 91 .00 4-9 786.30 5-6 0.00 0.0 0.00 0.0

Night Down 1'ime

Reason Hours %

Weather 250.20 23-4 Computer 1 •50 0.1 KPNO Instrument 8 •50 0.8 I elescope 8 •75 0.8 Other 1 1 •50 1 .1 Software 1 •50 0.1

Total 281.95 26-4

-28- CF telescope

Sched Jsable Sched Usable Nights * ]iours * Days % Hours %

Visitor 54.68 79-2 446.36 77-1 0.00 0.0 0.00 0.0 Staff 14-32 20-8 132.64 22.9 0.00 0.0 0.00 0.0 subtotal 69-00 100.0 579-00 100.0 0.00 0.0 0.00 0.0

Engineering 9-00 11-5 63-50 9-9 0.00 0.0 0.00 0.0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Open Time 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Test & Eval. 0.00 o.o 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 78.00 11-5 642.50 9-9 0.00 0.0 0.00 0.0

Night Down 1'ime

Reason He urs

Weather 208 •50 23-5 Software 6 •50 0.7 KPNO Instrument 5 •50 0.6 Other 14 •50 1 .6 1 elescope 6 •50 0.7 Computer 3 •50 0.4

Total 245.00 27.6

-29- 1.3m telescope

Sched Usable Sched Usable Nights * Hours % Days * Hours %

Visitor 63-02 81 .8 396.79 79-0 11 .00 100.0 33-00 100.0 Staff 13-98 18.2 105-71 21 .0 0.00 0.0 0.00 0.0 subtotal 77-00 100.0 502.50 100.0 11 -00 100.0 33-00 100.0

Engineering 8.00 9-4 73-00 12.7 0.00 0.0 0.00 0.0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 o.o Open Time 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 o.o Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Test & Eval. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 85-00 9-4 575-50 12.7 11 .00 0.0 33-00 0.0

Night Down Time

Reason Hours

Weather 330.00 34-6 KPNO Instrument 10.50 1 .1 Other 24-50 2.6 Software 6.50 0.7 Telescope 5-50 0.6 Computer 1 -50 0.2

Total 378-50 39-7

Day Down Time

Reason Hours %

Weather 49-00 54-4 KPNO Instrument 8.00 8.9

Total 57-00 63-3

-30- 1-36 telescope

Sched Usable Sched Usable •*• Nights # Hours * Days % Hours %

Visitor 57-40 82.0 458.45 83-9 0.00 0.0 0.00 0.0 Staff 12.60 18.0 87-76 16-1 0.00 0.0 0.00 0.0 subtotal 70.00 100.0 546.20 100.0 0.00 0.0 0.00 0.0

Engineering 9-00 1 1 .4 56.00 9-3 0.00 0.0 0.00 0.0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Open Time . 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 o.o Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Test & Eval. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 79-00 11 .4 602.20 9-3 0.00 0.0 0.00 0.0

Night Down 1 ime

Reason Hours

Weather 225 -70 . 26.1 KPNO Instrument 1 1 .00 1 -3 1 elescope 6 .00 0.7 Other 16 -70 1 -9 Software 4 .00 0-5 Computer 0 -50 0-1

Total 263-90 30-5

-31- 2-36 telescope

Sched Usable Sched Usable Nights % Hours % Days % Hours %

Visitor 75-18 94-0 424-42 92.1 0.00 0.0 0.00 0.0 Staff 4-82 6.0 36.28 7.9 0.00 0.0 0.00 0.0 subtotal 80.00 100.0 460.70 100.0 0.00 0.0 0.00 0.0

Engineering 7-00 8.0 38.00 7.6 0.00 0.0 0.00 0.0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Open Time 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Test & Eval. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 87-00 8.0 498.70 7.6 0.00 0.0 0.00 0.0

Night Down T Lme

Reason Hours

Weather 428 •25 45.5 KPNO Instrument 2 .00 0.2 Other 12 •25 1.3

Total 442.50 47-0

-32- 4-16 telescope

Sched Usable Sched Usable Nights * Hours % Days % Hours %

Visitor 48.00 100.0 243-00 100.0 0-00 0.0 0.00 0.0 Staff 0.00 0.0 0-00 o.o 0.00 0.0 0.00 o.o subtotal 48.00 100.0 243-00 100.0 0.00 0.0 0.00 o.o

Engineering 2.00 4-0 6.00 2.4 0.00 0.0 0.00 o.o Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Open Time 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 o.o 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Test & Eval. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Public Info. 0.00 o.o 0.00 0.0 0.00 0.0 0.00 0.0 Other 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 total 50.00 4-0 249-00 2.4 0.00 0.0 0.00 0.0

Night Down Time

Reason Hours

Weather 260.50 50.8 Computer 2.50 0-5 Other 1 .00 0.2

Total 264-00 51 .5

-33- Schm telescope

Sched Usable Sched Nights % Hours Days % HoursUsable % Visitor 29-00 100.0 161.50 100.0 0.00 0.0 0.00 0 0 Staff 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 subtotal 29-00 100.0 161-50 100.0 0.00 0.0 0.00 0.0 Engineering 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0 0 Shutdown 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0 0 Open Time . 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Oper. Train. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Soft. Engr. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Sys. Check. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0.0 Request Obs. 0.00 0.0 0.00 0.0 0.00 0.0 0.00 0 0 0.00 0.0 0.00 0.0 0.00 0.0 Publicle%* Info.w1' 0.00n'SS °'°0.0 °-000.00 °-°0.0 °-000.00 0.0o.6 0.00o oo -"o!o Other °-000.00 °-°0.0 0.00o-oo 6.60.0 60.00".00 0.0o'.O o'.OOv,.w o!o total 29-00 0.0 161.50 0.0 0.00 0.0 0.00 0.0

Night Down Time

Reason Hours #

Weather 108.00 39-0 Other 7.00 2-5 KPNO Instrument 0.25 0.1

Total 115-25 41-6

-34- V. ENGINEERING AND TECHNICAL SERVICES

A. GENERAL ACTIVITIES The major activities during this quarter were related to the Scientific Overview Committee and User's Committee reviews of the proposals for FY1985 observatory projects and the preparation of materials for the KPNO and NOAO Management Committees reviews of the proposed FY1985 ETS O&M budget and KPNO projects. In addition, the first steps were taken for the ETS portion of the NOAO reorgani zation.

NOAO Reorganization

Dale Schrage was appointed Manager, ETS, NOAO, effective May 1, 1984. In addition, the scientific technical illustration function was transferred to the KPNO Director's Office, the Facilities Engineering Department was transferred to ETS from KPNO Administra tive Services, and the NOAO Advanced Development Program (ADP) was established with responsibility for the NNTT Program.

Personnel Changes

During this quarter J. Machaln, Design Drafter in the Telescope Systems Program resigned. The following individuals were hired duj— ing this quarter:

Ken Dowdney, Engineering Associate, Instrument Systems Program. Mr. Dowdney had been employed by KPNO for 19 years until his resignation a year ago.

Brian Fisher, Design Drafter, Telescope Systems Frogram.

Recruitment is in progress for the following positions, with the exception of the two program manager positions. These are being left open pending the planned reorganization of the observatories.

R&D Program: Electronics Engineer Telescope Systems Program: Program Manager Instrument Systems Program: Program Manager Optical Engineer

B. RESEARCH AND DEVELOPMENT (R&D) PROGRAM

The major activities continue to be the testing and evaluation of IR arrays. The resignation of Steve Marcus has caused a temporary termination of the testing and evaluation of visible arrays.

-35- IR Array Projects

Cinclnatti Electronics InSb Array: This is a joint project with CTIO. Preliminary tests have shown the dark current to be high, and this results in a prob able maximum integration time of 1000 seconds. Although this will limit the performance of the array short of 2 microns, this deficiency is not severe. With new electronics it appears that the read noise may be reduced to approximately 1000 elec trons.

The detector is being installed in a new dewar, the CTIO/KPNO IR Imaging Camera. The conceptual design was completed at CTIO with the detail design and fabrication being carried out at KPNO.

Hughes 58x62 Schottky Barrier Array: The dewar and electronics were completed and the array was installed during the last week of the quarter. The device is cosmetically good with no bad columns or rows and only a few bad pixels.

Aerojet Si:Bi Array:

The second 2x64 pixel device was installed in the dewar for testing. The prototype CCD controller has been used to operate the system. This array is inferior to the first in that it has four dead pixels, whereas the first array had none, and the noise is somewhat higher. The first array is being modified by Aerojet to include reset switches to change the readout mode. This scheme will be tested next. The better array has less than 200 electrons read noise and good uniformity.

Array Procurement:

We have begun verbal negotiations with the Santa Barbara Research Corporation, a Hughes Aircraft subsidiary, regarding the procurement of a 58x62 element InSb array.

Visible Array Projects

Galileo Virtual Phase CCD:

Work on this project ceased with the resignation of Steve Marcus. The performance of the array was found to be inferior to devices currently in service at KPNO.

GEC CCD:

Further GEC CCDs will be procured through Cambridge Imaging Electronics in England. This firm will provide initial screen ing and testing.

-36- Data Acquisition & Control Computer System The system delivered in the fall of 1983 is now In operation and is being used for the infrared array testing. This system utilizes the multi-tasking FORTH operating system developed for the CCDs. This software is not entirely suitable for use with Infrared arrays given the small format, high readout rate, and co-adding requirements of infrared arrays. Further software development is underway subject to the availability of person nel . A second system has been ordered in preparation for the removal of the Varian lab computer system.

C. TELESCOPE SYSTEMS PROGRAM (TSP)

The major activities during this quarter were related to shut downs and maintenance and to matters concerning the implementation of the Digital Equipment Corporation (DEC) computer systems on KPNO and to infrared chopping secondary projects for the KPNO 2.1 meter and CTIO 4 meter telescopes.

O&M Support Activities The following optics were aluminized or cleaned during this quarter:

Telescope Optics Service

1.3 Meter Tel. Primary Aluminized

Burrell-Schmidt Primary Aluminized 5 Prisms Cleaned

Improvement Projects

4 Meter Telescope:

Installed a new CAMAC A/D converter in the FTS crate.

1.3 Meter Telescope:

Installed new drive preload motor controls and modified the control system for use with the autoguider.

#1-0.9 Meter Telescope: Construction of new colllmation drive assemblies for the f/7.5 and f/13.5 secondaries is in progress. Installation is planned for early summer.

-37- Grant Measuring Engine: . Began installation of a new "Falcon" single-board microcomputer for control and data acquisition.

Dicomed: Replaced floppy discs with a 5 Mbyte Winchester to improve reliability.

Observatory Projects

Instrument & Computer Power:

Completed specifications and RFQ for rotary UPS for #2-0.9 meter telescope. Bids have been received and an order has been placed.

Mountain Computer Implementation:

It will be necessary to add CAMAC memory modules to each com puter system involving construction of at least two dozen more units. It has been decided that these should be constructed on printed wiring boards. A vendor has been selected to provide the artwork.

Additional Kinetic Systems branch drivers have been ordered for the remaining site on Kitt Peak.

Downtown Computer Implementation:

The downtown DEC PDP 11/44 has been replaced with a VAX 11/750 system. The PDP 11/44 has been installed in the 1.3 meter telescope.

The Western Peripherals controllers for the Kennedy tape drives used with the VAXs have been found to be unreliable. These are being replaced with units from Emulex.

A second DEC PDP 11/23+ system has been ordered for the R&D Program. This unit will be identical to the system which was installed during the first quarter and will be dedicated to the evaluation of infrared arrays.

2.1 Meter Chopping Secondary:

The final design review was completed, and fabrication of t n."3 mechanical hardware is underway. The installation of the hardware will be delayed until late fall due to the need for subcontracting the figuring of the secondary mirror.

-38- 4 Meter Seeing Monitor:

Hardware and software development for the data acquisition com puter system is continuing. The hardware is nearly complete with the pre .otype software roughly 75% finished. The in-dome image motion sensor system will be installed early during the next quarter. There has been one "engineering run" attempt to acquire microthermal data.

#2-0.9 Meter Telescope Modifications:

Construction of the new computer room began very late in the quarter. The architectural design of the console room is nearly complete. Construction of mechanical hardware for the conversion of the telescope from f/13.5 to f/7.5 is underway. This project is scheduled to be completed during a shutdown in August.

D. INSTRUMENT SYSTEMS PROGRAM (ISP)

The major activities during this quarter centered around the initiation of the FY1984 instrumentation projects.

O&M Support Activities

The Coatings Lab provided coatings on 52 surfaces for KPNO jobs.

R. Reed traveled to Falrchild Instruments in Palo Alto, Cali fornia, to receive technical instructions concerning the CCD detec tor for the Spectroscopic Event Counting System. He also traveled to JPL in Pasadena, California, to obtain the Texas Instruments 3- phase 800x800 CCD Array. The Universal CCD Dewar was tested for direct imaging use at the 2.1 meter telescope. This system utilizes the optical/mechanical Interface which was constructed for the #1-0.9 meter telescope in FY1982.

Improvement Projects

Acquisition TVs: An integrating acquisition TV memory/gulder was delivered by Digital Television Imagery (DTI). Three identical units were obtained for CTIO at the same time. This device was tested at the Coude' Feed, 1.3, 2.1, and 4 meter telescopes and has been put into service at the 1.3 meter telescope. Four additional units have been ordered for KPNO. These will be placed into service at the Coude' Feed, #1-0.9, #2-0.9, and Burrell-Schmidt telescopes.

-39- A search for a solid-state acquisition TV is being carried out jointly by OSD and ETS staff as an eventual replacement for the ISIT cameras currently in use. A prototype consisting of a Litton dual-microchannel plate intensifier, fiber-optically coupled to a Fairchild model 222 CCD camera, has been tested using both the KPNO and DTI acquisition TV memory/gulders. The sensitivity is at least equal to that of the ISIT, and guiding can be achieved provided that the image is at least 30M FHWM.

#1-0.9 Meter CCD Optical/Mechanical Interface:

Design work to implement more repeatable filter positioning was complete. The hardware modifications will be completed at the end of April.

Observatory Projects

Universal CCD Dewars:

The Texas Instruments (TI) 3-phase 800x800 CCD, which was received via an NSF Astronomy Instrumentation Grant, has been installed in a Mark II Universal Dewar. The first engineering night is scheduled in April at the 2.1 meter telescope.

A new-type RCA CCD has been received, and most of the camera head electronics have been fabricated. Installation and test ing will commence following the evaluation of the TI chip. High Resolution Imaging Spectrometer (HRIS):

The Rlsley prisms have been delivered by the coating vendor. Another engineering run with G. Timothy's multl-anode- microchannel-array (MAMA) detector is scheduled for June.

R-C Spectrograph Grating:

This ruling was completed prior to the end of the calendar year. Testing by KPNO and Bausch & Lomb has shown the ruling to be acceptable for use in the 4 meter telescope R-C spectro graph. Both KPNO and CTIO have ordered replicas. The ruling shows a small error of run, indicating that the engine is not yet capable of the more demanding high blaze angle rulings.

Spectroscopic Event Counting System (SECS):

It has been difficult to obtain the tapered fiber optic plugs. Most manufacturers have difficulty in meeting the shear distoi— tion specification of <5M. It has been difficult to obtain quotes on the 25 millimeter dual microchannel plate intensifi er. This is a non-standard item. A Fairchild #222 CCD detec tor with zero defects has been obtained for this instrument.

-40- Mechanical design of the camera head is underway. Fabrication of the camera head and interface electronics is in process. Hardware and components for the controller and memory processor are on order.

Seeing Studies: There were three observing runs at the 4 meter telescope during this quarter. Data were obtained on binary stars.

4 Meter Prime Focus CCD Mounting:

With the exception of the scan mechanism, the major mechanical sub-assemblies have been assembled and have passed environmen tal tests. The design of the electronics is underway. A pro totype scanning device is being designed.

Echelle Intensified CCD:

The fabrication of hardware to mount an intensified CCD on the 4 Meter Echelle Spectrograph will be complete early in the next quarter. It is planned to make this system available for scheduling during the fall semester.

Ruling Engine Improvements:

During this quarter the engine mounting was modified to imple ment a kinematic arrangement, and a new diamond carriage bush ing was installed. Implementation of a humidity control in the engine room is underway.

2-Dimensional Photon Camera:

The results of preliminary layout of the encoding masks and 19 photomultipliers have shown that the required diameter of the system will be in excess of 75 millimeters. The design of the optics is underway.

UV Fast Camera:

A design layout study is in progress to determine the physical constraints associated with the 4 meter Echelle and R-C Spec trographs within the Cass cage.

IRS @ #2-0.9 Meter Telescope:

Mechanical design of modifications to the existing guider is nearly complete and fabrication is underway. Provisions for the eventual implementation of a two-star photometer have been included. The use of the Intensified Reticon Scanner at the #2-0.9 meter telescope will be scheduled in the fall of 1984. Due to personnel shortages, the system will be manually operated during most of the semester.

-41- f/7.5 Automatic Filter Photometer (AFP): The KPNO Scientific Overview Committee Initiated this project in January to make an AFP available at the #2-0.9 meter tele scope after its conversion to f/7.5. This project, which con sists of modifications to an existing manual photometer, is currently 80% complete.

E. NON-KPNO WORK

National Solar Observatory

O&M Activities

During this quarter the McMath #2 Main Mirror was aluminized, and the #3 Main Mirror was cleaned.

Improvement Projects

McMath Telescope:

A new Main Optical System focus encoder was Installed.

Fabrication of mechanical and electronic hardware for the installation of a high resolution encoder for the Main Heliostat Declination axis is continuing. This system will be completed in late summer. The new McMath vertical spectrograph interferometric grating position system was interfaced to the computer.

Vacuum Telescope: The delivery of hardware for the DEC PDP 11/73 computer system has begun. This system will be the Varian computer replacement for this facility. Installation is planned for the sumr.er.

Instrumentation:

Efforts continued toward the implementation of a new interface of the 512 Channel Magnetograph to the computer. The hardware has been installed in the telescope and test ing is underway.

-42- Cerro Tololo Inter-American Observatory

Projects 4 Meter Chopping Secondary: The KPNO-supplied electronic hardware and CTIO-supplied mechanical hardware was assembled in Tucson and tested. The mirror was delivered by the subcontractor, and the KPNO Coating Lab provided a gold coating. All items have been shipped to CTIO. Installation Is scheduled for May. Bob Nagel, Acting Program Manager of the TSP, will travel to CTIO for the installation and testing. Acquisition TV Memories:

Three commercial acquisition TV memory/guider units were delivered, tested, and shipped to CTIO. An RCA ISIT TV ca-era was also purchased, modified, and shipped.

CCD Computer System:

KPNO has begun the assembly of a CCD computer system to be used to operate the CTIO Vldicon-Electronics-Box based CCD systems. This will permit the CTIO-constructed CCD sys tems to utilize the same software as the RCA CCD system which KPNO delivered to CTIO in 1982.

University of Hawaii

Coatings

The Coatings Laboratory coated ten Infrared beamsplitters for the Institute of Astronomy.

-43- VI. OPERATIONS SUPPORT DIVISION

A. OFFICE OF THE DIRECTOR, OPERATIONS SUPPORT DIVISION (OSD)

1.- During this quarter responsibility for the Tucson Operations Department was transferred to OSD.

2. The external Computer Advisory Committee held a final meeting and submitted its report.

3. There were 260 observing proposals received for the Fall 1984 semester.

/4. The Papago Tribal Utility Authority agreed to replace all mercury vapor outdoor lights within a 12-mile radius of the Observatory with low-pressure sodium fixtures. Implementation will begin as soon as NSF approval for financing the project is received.

5. The University of Arizona announced their commitment to begin replacing outdoor lighting with low-pressure sodium fixtures.

B. TUCSON OPERATIONS DEPARTMENT

The following are the major projects and other work undertaken by Tucson Operations during the quarter (in addition to routine maintenance and other work).

1. Constructed three new offices in the NOAO Director's Office building for CAS personnel. This work included modifying the lighting, air conditioning ducts, installing two windows and removing and reinstalling existing carpeting.

2. Constructed a skid for and shipped one of two "Pima" tower domes to Hawaii for NNTT site survey testing.

3. Modified and painted the other Pima tower dome and constructed a base for same. This dome is scheduled to be shipped to Mt. Graham for NNTT site survey testing.

4. Completed the design for a computer room on the ground floor of the #2 0.9-meter telescope building. Design of the console room for this building is 50% complete.

C. KITT PEAK OPERATIONS DEPARTMENT

1. Projects undertaken by Mountain Operations during the quarter included:

a. Added incandescent lighting in 4-meter FTS observing room; fluorescent lighting was too bright.

-44- b. Replaced three dome truck driver rollers at 84" telescope.

c. Replaced drive wheels on 50" dome.

d. Began repainting Solar interior. Completed to date: front entrance, two offices, machine shop, spectrograph hall to observing room, and observing

room.

e. As a result of losing a guide roller on 4-meter upper shutter, retainers were added to all guide rollers.

f. Sealed all light leaks from 84" coude observing room into telescope area.

g. As a result of heavy rainfall in 1983, the old road became impassable. The road was completely rebuilt during this quarter.

h. Installed a new pressure tank at the pump house at NRAO and McGraw Hill to increase water pressure at the new McGraw Hill telescope.

2. Telescope Support

a. Aluminized 50" primary mirror.

b. Aluminized Solar #2 main mirror.

c. Aluminized Burrell-Schmidt primary mirror.

d. Assisted in aluminizing U. of A. mirror.

e. Assisted in repairing broken water line at NRAO.

f. Assisted with equipment and manpower in installing McGraw Hill telescope.

3. General

a. Received four trucks from Excess Property at Fort Huachuca. These will replace older vehicles in the mountain fleet.

b. Processed water in storage: 580,000 gals.

c. Water processed: 250,000 gals.

d. Water used: 470,300 gals.

e. Precipitation: 1.69 in. Last precipitation: Jan. 14, 1984 (77 days)

f. Meals served: 12,577

-45- g. Lodgings (aggregate): 2,311

h. Among the special guests who visited the Observatory during this quarter were:

(1) Twenty members of the Illuminating Engineers Society of Arizona to study light pollution problems (January 26).

(2) Public information officers from major U.S. observatories and national centers attending conference in Tucson.

D. OBSERVING SUPPORT DEPARTMENT

1. Telescope Support

a. During the second quarter of FY84, there were 88 instrument changes, which included three visitor instruments.

b. Kim Gillies transferred from the Telescope Support group to Computer Support. He is currently working as a mountain programmer.

c. Dean Hudek, University of Iowa, has been hired as a replacement for the open telescope operator/technical assistant.

2. Instrument Support Group

a. Conversion of the #2 0.9-meter telescope to f/8: Several members of the Instrument Support Group have been working with the Engineering Department to ensure that this conversion goes smoothly and that the results are compatible with present oberving techniques. In addition to the conversion project, Instrument Support personnel have worked on the design of a new automatic filter photometer and combination auto guider/two-star photometer to go with the new f/8 telescope. These additions will increase our photometric capabilities on the smaller telescopes and increase scheduling flexibility.

b. "Film" multi-aperture plates: The production of multi-slit aperture plates for doing limit- spectroscopy with the cryogenic camera has been an expensive and difficult task. Most of the fabrication was done by outside vendors, thus increasing the time required for completion. We now have developed a procedure for complete "in-house" fabrication of these plates using photographic film and our Dicomed film recorder. The result is a piece of film, which is used at the telescope focal plane,

-46- with an array of slits corresponding to the actual positions of galaxies and QSOs. Observers report that they are very happy with the results and that they cannot even detect the loss of light in the film base since it is usually masked by seeing variations.

c. A new developmental project was begun to investigate a new generation of acquisition television systems. Laboratory and on-telescope tests have been made, in conjunction with the Engineering Department, on the latest micro-channel plate intensifiers and CCDs which show promise for field acquisition work. Present tests involve a Litton Industries dual- microchannel plate and Fairchild 222 CCD. In addition, a working group has been formed to review methods of upgrading a number of instruments so they will be available for auto guiding with our new leaky memories/auto guiders.

d. New optics for the cryogenic camera: Early in the quarter the installation of a new corrector plate for the cryogenic camera was completed. The new optics, after an initial debugging period, show improved imaging for the whole field available (5 arc- minutes). The camera still suffers from the wavy surface of the chip which will continue to be the major drawback of the instrument.

e. New user instrumentation documentation: Updated versions of an "Observers Manual for the Intensified Image Dissector Scanner," and the "IIDS/IRS Mountain Reduction Manual" were completed.

f. The new photomultiplier tube test bench is nearing completion. First tests with this device are projected for mid-May. The test bench will be used in Tucson for the first few months before it is sent to the mountain.

g. The "barefoot" TI CCD/universal dewar on the 4-meter R.C. spectrograph was successfully tested on the 4- meter telescope January 10. It is now available for regularly scheduled use.

E. COMPUTER SUPPORT DEPARTMENT

1. Highlights

a. The IRAF system was released for internal use within NOAO-Tucson on March 19. While this first release of the system did not include any major scientific packages, it did include 10 system and utilities packages containing about 100 tasks of varying sizes. This first release of IRAF contains

-47- approximately 110K lines of code, 35K lines of which were imported.

b. ; Steve Grandi was appointed Acting Manager of the Computer Support Department effective February 28. c. Suzanne Hammond was promoted to Scientific Programmer on March 1 and has moved to the IRAF group.

d. A new DEC VAX-11/750 replaced the PDP-11/44 (which was sent to the mountain) as the downtown Class 1 computer. A new version of UNIX was installed on the machine, and on March 28 it was made available for document processing, database transactions and other general-purpose activities. The new VAX features two 456 Mbyte disks, a slow 800 bpi tapedrive and a fast 800/1600 bpi tapedrive.

e. The 1.3-meter was converted to run with a DEC PDP- 11/44 as of February 1 and has not been switched back to the Varian since. This implies that the new photometry program made a successful debut.

/ f. Doug Tody, Steve Grandi and Dave De Young (with Bruce Atwood and Mark Phillips of CTIO) attended the January conference on Supermicrocomputers in Astronomy at Chapel Hill, North Carolina. It was concluded that supermicrocomputers will make excellent and cost effective IRAF workstations, though the floating point performance of most models currently on the market is poor.

2. Equipment

a. New 456 Mbyte disks were installed on the Class 2 and Class 5 VAXes.

b. A second Unibus channel was installed on the Class 2, Class 3 and Class 5 VAXes. These upgrades should increase the efficiency of large i/o transfers involved in image processing.

c. A new Versatec V-80 printer/plotter replaced the Versatec 1200 attached to the Class 2 and Class 3 VAXes.

d. A memory upgrade card was added to the Imagen Imprint-10 laser printer to enable the creation of more complex plots.

e. A new 32-line terminal controller card was added to the Class 1 VAX, and a new 16-line card was added to the Class 3 VAX.

-48- f. New tape controller cards for the Kennedy high-speed tape drives were ordered for all four VAXes.

g. A new 5 Mbyte Winchester disk was obtained for the PDP-11/03 computer that runs the Dicomed image- hardcopy system and is in the final stages of installation.

h. Two unibus branch drivers were received for the mountain 4-meter and 2-meter 11/24 systems.

3. Software Documentation

a. A number of extensions and revisions were included in the "CCD Software Observing Manual."

b. A new manual for the Photometry program was released.

c. A number of extensions and revisions were made to the TCP manuals, including specific instructions on loading the 4-meter PDP-11/24 system from bootable task images.

d. The "Cryogenic Camera Long-Slit Batch Reduction Manual" has been rewritten. A number of errors were corrected from the previous version of the manual, and more information has been added.

e. The "Video Camera Reduction Manual" has been updated. VCAM reduction software remains unchanged, but changes have occurred in the VCAM data tape format since the previous version of the manual.

f. The "IPPS RV Manual" has been extensively rewritten. The manual describes how to use the routines available on the IPPS for the reduction of two-dimensional spectral data.

g. A draft version of the "Intensified CCD Spectrometer Long-Slit Batch Reductoin Manual" has been written. The manual will be completed after more is learned about data reduction for this instrument when the ICCD is used on the 4-meter telescope in May.

h. The "IRAF Project List and Program Implementation Plan" was issued on February 12.

i. The "User's Guide to the IRAF Command Language" has been completed.

j. A "Bibliography of IRAF Documentation" has been written to describe the collection of IRAF documents; the database of documents is available on-line via telephone modems.

-49- 4. Systems/Software Support Group

a. Systems Support—Operating Systems and Utility Programs:

(1) VAX/VMS version 3.5 and VMS C compiler were installed on the Class 3 VAX.

(2) The MONGO interactive plotting package was installed on the Class 3 VAX.

(3) The 15Sep83 version of AIPS was installed on the Class 3 VAX.

(4) Berkeley UNIX 4.2 was installed on the new Class 1 VAX incorporating numerous local bug fixes and upates.

(5) The TeX82 text processing system was installed on the Class 1 VAX.

(6) The Ingres database system was moved to the new Class 1 VAX.

(7) KPNO Forth has been brought up under UNIX 4.2 on the Class 1 VAX.

(8) The IMSL numerical subroutine library was obtained and is installed on the Class 2 and Class 5 VAXes.

(9) The portion of the NCAR plot package which plots on a device has been improved to conform more closely to the actual device. The package can now produce plots tailored to a terminal, the Versatec, the Imagen and even the Calcomp.

(10) Several improvements have been made to the ALPS telescope scheduling system.

(11) Several Cyber utility programs have been adapted to attempt to remove a bad block on the SCRATCH disk from active use.

(12) The Whitesmith's C compiler is now available on the 11/03 Dicomed system.

b. Software Support—Program Conversions

(1) The conversion of the Spotbox PDS program from the Cyber to the VAX was completed.

(2) A new package aimed at replacing the Cyber LFORTH/XFORTH package (used to list and cross-

-50- reference Forth progrmas) has been written in VAX/UNIX Forth. It is being ported to stand alone Forth and should be portable to any Forth system.

(3) The Cyber package PLOTLIB has been added to the VAX NCAR plot package. It is actually a simulation using NSPP calls.

c. Software Support—Data Acquisition, Reduction and Analysis.

Two new programs have been added to the Tololo- Vienna spectral package. One performs a cross- correlation on two spectra to determine the wavelength difference between two observa tions. The other program is a continuum estimator which will also remove the low- frequency modulation from a spectrum to "flatten" it.

d. Miscellaneous

(1) Various versions of KPNO Forth have been exported to 21 institutions.

(2) The UNIX of the NCAR/NSPP plotting package was exported to one institution.

(3) The Cyber program FINDER and the SAO catalog it reads have been exported to one institution.

5. Mountain Programming Group

a. Personnel: Kim Gillies joined the group at the '•••--" beginning of the quarter. He is assigned to the data-logging program which will run on the DEC systems and replace a number of Varian codes.

b. Conversion. The major group activity over the quarter continued to be conversion.

(1) The hardware for the 4-meter FTS and for the data-logging program became available just before the end of the quarter, so those activities are no longer waiting for equipment.

(2) A distributed processing implementation was inaugurated at the 4-meter with the installation of an 11/24 as the telescope control computer. The instrumentation computers (11/44 or 11/23) communicate commands and received status over an RS232 link at the 9600 baud.

-51- c. NSO Activities. One-and-a-half FTE were used on solar activities in the period. The efforts were devoted to the Vacuum Telescope (75%), solar FTS (15%) and the solar Reticon (10%).

(1) The Vacuum Telescope Varian Forth program was used for real observing tests of the new Mortara hardware interface unit. The program needs some additional calibration codes but is otherwise near the end of the varian development stage. It will be converted to the DEC 11/73 as soon as it is installed. (2) The Solar FTS activity involved rapid observing sequences and tailoring the observing informa tion block to make it more applicable to the observing modes in use at this instrument.

(3) A new release of the software was prepared for the Reticon system. The release date of the new version is April 1, coinciding with a major break in the schedule including a telescope maintenance shut-down.

d. Administrative Activities. The mountain programming group is to be transferred to thec CAS-division effec tive May 1, 1984. A number of group meetings have been conducted with the manager-designate of the CAS to discuss this aspect of the NOAO reorganization.

6. Data Reduction and Analysis (IRAF) Group

a. The IRAF group spent most of this past quarter on applications software development, documentation, and planning. The IRAF system was released for internal use within NOAO on 19 March.

(1) The core system software received only a small amount of attention this past quarter. The TTY (terminal control) interface was finished early in the quarter. The system package was completed shortly thereafter, adding the stty program for terminal setup, and the lprint program for driving the line printer (both depend upon TTY for device independence). With the completion of this software, the IRAF system can now be used from virtually any type of terminal, and can be used remotely via a modem.

(2) The UNIX Yacc compiler utility was modified to produce SPP/Fortran parsers, making it possible to build very nice user interfaces for IRAF applications programs.

-52- (3) A week was spent designing the internals of the image calculator program, but the project had to be set aside to meet the deadline for the internal pre-release.

(4) The help program, used to provide online docu mentation facilities, was completed in time for the pre-release, though a large backlog of manual pages remain to be written for the system packages.

(5) The new package tv was added to improve the user interface for image display control.

(6) The mtexamine and reblock programs were added to the dataio package, and coding of the FITS writer was underway by the end of the quarter.

(7) The utilities package was brought online with half a dozen or so programs, and a new package local was added to provide a place within the system for user-generated software (software of general utility not yet integrated into the main system nor supported by the IRAF group).

(8) It was unacceptable to have the first release of IRAF without some graphics facilities for looking at data, so a basic version of the plot package was brought online for the pre release. The plot package includes programs for generating contour and surface plots of image data, for plotting lines and columns of images, and a very general program for graphing vectors input as either lists or image sections. The new graphics software is nonproprietary and system and device independent, and may be used to generate plots on the graphics terminal or on any NOAO graphics output device. There is as yet no provision for graphics input (cursor readback). The implementation uses the NCAR graphics software, and will be modified internally during the next quarter to use the new NCAR implementation of the ISO standard Graphical Kernal System (GKS) for the device interfaces.

(9) Paul Schmidtke left the IRAF group early in the ""--- quarter. The filter photometry package, originally assigned to Paul, has been set aside for the moment in favor of higher priority projects. We have imported an existing photometry package from Paul Stetson at DAO; this package should help meet our needs until

-53- the matter of the IRAF photometry package is resolved. We are also in the process of importing Stetson's new digital stellar photometry package, and are very encouraged by the reports we have been hearing about the package. The package will be brought up initially with minimal modifications on the VMS VAX. It seems likely that Stetson's package will be integrated into IRAF as a fully supported package within the next year. (10) Suzanne Hammond joined the IRAF group late in the quarter. Suzanne has begun work on the lists package, which should be completed during the next quarter.

(11) Doug Tody represented NOAO at a conference of the national astronomical centers held in Boulder on January 13 to discuss graphics standards. NOAO and STScI agreed to adopt both the NCAR graphics software and the GKS standard. Cliff Stoll of STScI will be visiting Tucson in April and May to bring up the NCAR/GKS software within IRAF.

7. Computer Usage Statistics. a. The IPPS system was scheduled for the following number of hours based on a full month, including weekends and holidays.

Month Comtal 4010-1 4010-2 January 12.9 hrs/day 4.7 hrs/day 2.9 hrs/day February 8.9 hrs/day 6.4 hrs/day 2.9 hrs/day March 9.7 hrs/day 4.6 hrs/day 1.6 hrs/day

b. The computer usage statistics for the past three months were as follows:

Cyb«r CI»M 1 VAX CIam I VAX Claw 6 VAX Class a vms vax

CP hour. % Hag % viator. CP hour. CP how. CP how, 1 CPhoar. Jan 501 i6% 5395 22.0(11/44) 238.7 213.0 185.5 Feb 321 60?6 37% Nooe AraiUble* NoQt AvjuUblef 227.5 155.1 Mar 357 31% 68°5 63 7(11/750) 3482 210.4 131 4

11/750r,/^ClM*system' 7""^,statis'ic9(new Class 1) availableavailablefor forpublicFebruaryuse 3/28/84.1984. PDP-I1/44 dismantled and sent to the mountain,mountain- VAX-vaa- t Class 2statistics not available for the month of February 1984 due to system failure.

-54-

APPENDIX A- OBSERVATIONAL PROGRAMS

Summary of Executed Proposals 01/01/84 - 03/31/84

Nights Hours Days Hours 5136 M Aaronson, University of Arizona J Mould, G Bothun, California Institute of Technology Determination of the Distance Scale & Expansion Rate via... 2.1 meter 4.00 26.00 0.00 0.00

5137 M Aaronson, University of Arizona J Mould, G Bothun, California Institute of Technology CCD Surface Photometry of Cluster Spirals Nr. 1 0.9 meter 4.00 37.00 0.00 0.00

4685 H Abt, Kitt Peak National Observatory Rotational Velocities of A-type Stars 2.1m Coude Feed 1.00 11.00 0.00 0.00

5006 H Abt, Kitt Peak National Observatory Rotational Velocities of A-Type Stars 2.1m Coude Feed 3.00 29.00 0.00 0.00

4851 P Allan, W Keel, Kitt Peak National Observatory Low Level Variability of Quasars 1.3 meter 1.00 6.00 0.00 0.00

4851 P Allan, w Keel, Kitt Peak National Observatory Low Level Variability of Quasars 1.3 meter 1.00 7.00 0.00 0.00

4852 B Anthony-Twarog, University of Kansas A Stromgren Photometric Investigation of Hyades Subdwarf... Nr. 2 0.9 meter 6.00 15.00 0.00 0.00

5073 H Arp, Mt. Wilson & Las Campanas Observatories J Sulentic, University of Alabama Investigation of Peculiar High Redshift Objects 4 meter 7.00 83.50 0.00 0.00

-55-

,_,„„ Nights Hours Days Hours 4770 B Balick, University of Washington T Heckman, University of Maryland G Bothun, Center for Astrophysics Low-Redshift Quasars as the Active Nuclei of Interacting... 4 meter 2.00 12.20 0.00 0.00

4853 T Balonek, Williams College J Puschell, Titan Systems, Inc. P Smith, M Zeilik, University of New Mexico P Heckert, Doane College Simultaneous Infrared, Visual, Millimeter & Centimeter 2.1 meter 4.00 29.00 0.00 0.00

4695 T Barker, Wheaton College A Spectrophotometric Survey of Planetary Nebulae Nr. 1 0.9 meter 3.00 8.00 0.00 0.00

5010 T Barker, Wheaton College A Spectrophotometric Survey of Planetary Nebulae 2.1 meter 4.00 33.00 0.00 0.00

4995 M Belton, Kitt Peak National Observatory H Spinrad, University of California, Berkeley P Wehinger, S Wyckoff, Arizona State University D Yeomans, Jet Propulsion Laboratory Characterization of the Physical & Chemical Properties 4 meter 2.00 22.50 0.00 0.00

4994 M Belton, Kitt Peak National Observatory H Spinrad, University of California, Berkeley International Halley Watch (IHW) Trial Run & Investigation Nr. 1 0.9 meter 3.50 28.00 0.00 0.00

-56- Nights Hours Days Hours 4832 M Belton, Kitt Peak National Observatory H Spinrad, University of California, Berkeley P Wehinger, S Wyckoff, Arizona State University D Yeomans, Jet Propulsion Laboratory Characterization of the Physical & Chemical Properties of.. 4 meter 2.00 14.00 0.00 0.00

4966 P Bernath, University of Arizona S Ridgway, Observatoire de Lyon Molecular Constituents of the IRC + 10216 Shell 4 meter 2.00 22.00 1.20 8.00

5058 B Bohannan, D Hummer, D Abbott, University of Colorado Precision Spectrophotometry of Early Type Stars 2.1m Coude Feed 6.00 32.00 0.00 0.00

5165 H Bond, Louisiana State University J Bahcall, Institute for Advanced Study Photometry of a Complete Sample of Stars in the Direction.. Burrell Schmidt 6.00 28.00 0.00 0.00 Nr. 2 0.9 meter 6.00 35.00 0.00 0.00

5166 H Bond, R Luck, Louisiana State University CNO Abundances in Subgiant CH Stars 2.1 meter 3.50 40.00 0.00 0.00

5147 B Bopp, University of Toledo B Goodrich, Kitt Peak National Observatory L Palmer, Simon Frazer University Photometric Study of Active-Chromosphere & Composite F+Be.. Nr. 2 0.9 meter 4.00 16.00 0.00 0.00

4804 B Bopp, University of Toledo J Africano, B Goodrich, Kitt Peak National Observatory L Palmer, Simon Frazer University Photometric Study of New Active-Chromosphere stars Nr. 2 0.9 meter 5.00 48.00 0.00 0.00

-57- 1 Nights Hours Days Hours 4976 B Bopp, University of Toledo Spectrodcopy of F + Be Binaries 2.1m Coude Feed 4.00 24.00 0.00 0.00

5167 K Borne, Carnegie Institution of Washington J Hoessel, Space Telescope Science Institute Photometry of Interacting Galaxies Nr. 1 0.9 meter 3.50 29.50 0.00 0.00

5187 S Boughn, J Uson, Princeton University Infrared Observations of the Integrated Light from the 1.3 meter 4.50 44.00 0.00 0.00

5236 H Bradt, R Remillard, Massachusetts Institute of Technology W Roberts, Center for Astrophysics Optical Identification of HEAO-1 X-Ray Sources Burrell Schmidt 7.00 50.00 0.00 0.00

4957 L Brown, R Toth, Jet Propulsion Laboratory R Poynter, Jet Propulsion Lab, T-1166 FTS Laboratory Spectroscopy in Support of Remote Sensing... McMath FTS Lab 3.00 27.00 3.00 30.00

4856 J Burns, D Batuski, University of New Mexico Mapping the 3-Dimensional Distribution of Two Super 2.1 meter 4.00 36.00 0.00 0.00

5285 R Campbell, U.S. Naval Academy Photometric Study of Eclipsing Variable Nr. 4 0.4 meter 7.00 43.50 0.00 0.00

-58- Nights Hours Days Hours

5189 H Campins, University of Maryland Infrared Photometry of Periodic Comet Encke 1.3 meter 0.00 0.00 7.00 16.00

5264 B Carney, University of North Carolina D Latham, Center for Astrophysics Survey of Stars in the Lowell Proper Motion Catalog !-3 meter 2.00 0.00 0.00 0.00

4915 C Chapman, D Davis, S Weidenschilling, D Levy, R Greenberg, Planetary Science Institute Photometric Geodesy of Main-Belt Asteroids Nr. 2 0.9 meter 4.50 18.50 0.00 0.00

4344 C Chapman, D Davis, S Weidenschilling, R Greenberg, Planetary Science Institute Photometric Geodesy of Main-Belt Asteroids Nr. 2 0.9 meter 4.00 24.00 0.00 0.00

5032 Y Chu, Washburn Observatory, University of Wisconsin G Jacoby, Kitt Peak National Observatory J Kaler, K Kwitter, University of Illinois Radius-Expansion Velocity Relationship for Single Shell.... 4 meter 4.00 37.00 0.00 0.00

4967 N Comins, J Hayes, University of Maine A Study of Double Galaxies 4 meter 2.00 25.00 0.00 0.00 Nr. 1 0 9 meter 2.00 20.00 0.00 0.00

4737 L Connolly, Southeast Missouri State University J Wilson, Georgia State University Stromgren Photometry of BL Herculis Variables Nr. 2 0.9 meter 7.00 47.50 0.00 0.0C

-59- Nights Hours Days Hours 5263 P Conti, A Torres, University of Colorado P Massey, Kitt Peak National Observatory Measure WC Type Stars Nr. 1 0.9 meter 4.00 17.50 0.00 0.00

5035 C Corbally, Vatican Observatory R Garrison, David Dunlap Observatory G Coyne,. Vatican Observatory Research Group Survey for G-Dwarfs at the North Galactic Pole Burrell Schmidt 2.00 11.00 0.00 0.00

5202 A Cowie, J Blades, L Cowie, Space Telescope Science Institute D York, University of Chicago Mass Flow onto the Galactic Disk: the Origin,Distance 4 meter 4.00 38.10 0.00 0.00

5036 P Crane, European Southern Observatory Photometry of the Cors of E and SO Galaxies Nr. 1 0.9 meter 4.00 37.20 0.00 0.00

4738 S D'odorico, European Southern Observatory R Becker, Virginia Polytechnic Inst, and Student Univ. J Dickel, A Silverman, University of Illinois K Long, Johns Hopkins University Spectroscopy of Optical Counterparts of Non-Thermal Radio.. 2.1 meter 1.00 6.50 0.00 0.00

5013 G Da Costa, C King, Yale University Evolutionary Synthesis of the Stellar Population in Spiral. 1.3 meter 5.00 42.50 0.00 0.00

5015 K Davidson, University of Minnesota T Kinman, Kitt Peak National Observatory Long-Integration-Time Spectrophotometry to Determine 2.1 meter 4.00 44.00 0.00 0.00

-60- Nights Hours Days Hours 5014 K Davidson, University of Minnesota T Kinman, Kitt Peak National Observatory High-Resolution Spectroscopy of I Zw 18 & Other Objects.... 4 meter 4.00 32.75 0.00 0.00

5118 R Davies, S Hurley, Nuffield Radio Astronomy Laboratories T Kinman, Kitt Peak National Observatory Improved Mass to Light Determinations of Galaxy Groups..'... 2.1 meter 3.00 31.00 0.00 0.00

4861 L Davis, R Davies, G Illingworth, Kitt Peak National Observatory M Cawson, Cambridge University CCD Surface Photometry of Ellipticals and Disk Systems Nr. 1 0.9 meter 1.00 10.00 0.00 0.00

5104 L Davis, J Barnes, D Hayes, J Africano, G Jacoby, D Ketelsen, Kitt Peak National Observatory Imaging Detectors Standards Consortium Nr. 1 0.9 meter 1.00 5.00 0.00 0.00

4861 L Davis, R Davies, G Illingworth, Kitt Peak National Observatory M Cawson, Cambridge University CCD Surface Photometry of Ellipticals & Disk Systems with.. Nr. 1 0.9 meter 3.00 29.00 0.00 0.00

5119 J Eaton, Indiana University C Poe, University of Wisconsin BVRI Photoemtry of RS Canum Venaticorum: the Temperature... Nr. 4 0.4 meter 2.00 8.50 0.00 0.00

-61- L Nights Hours Days Hours 4237 F Fekel, Goddard Space Flight Center Spectroscopy of Close Multiple Stars 2.1m Coude Feed 6.00 67.50 0.00 0.00

4806 F Fekel, Goddard Space Flight Center J Africano, K Gillies, Kitt Peak National Observatory Spectroscopy of New, Chromospherically Active stars 2.1m Coude Feed 2.00 4.00 0.00 0.00

5038 G Fontaine, F Wesemael, P Lacombe, University of Montreal R Green, KPNO Stromgren PHotometry of Hot B Subdwarfs in the Palomar-.... 1.3 meter 4.00 28.50 0.00 0.00

4895 W Forrest, J Pipher, A Moneti, C Woodward, University of Rochester Astronomical Infrared CCD Imaging 1.3 meter 7.00 83.50 0.00 0.00

5240 P Foukal, Atmospheric & Environmental Research, Inc. W Rosen, Vassar College L Petro, Atmospheric Environmental Research A Pierce, Kitt Peak National Observatory SOLAR-An Investigation of Time-dependent Variations in... McMath Main 0.00 0.00 5.00 32.00

5239 P Foukal, W Chiang, Atmospheric & Environmental Research, Inc. T Duvall, Jr., NASA Goddard Space Flight Center Photospheric Photometry Solar Vacuum 0.00 0.00 2.00 19.00

-62- Nights Hours Days Hours 4779 D Fraquelli, University of Georgia Short Period Eclipsing Binaries 2.1m Coude Feed 2.00 10.00 0.00 0.00

5124 J Gallagher, University of Illinois D Hunter, Kitt Peak National Observatory A Sandage, Mt. Wilson & Las Campanas Observatories Properties of Virgo Cluster Irregular Galaxies 1.3 meter 6.00 37.00 0.00 0.00

4679 W Gieren, Universidad de Los Andes Coude Spectroscopy and UBVRI Photometry of 3 very Short.... 2.1m Coude Feed 11.00 111.50 0.00 0.00 Nr. 2 0.9 meter 5.00 29.00 0.00 0.00

5126 R Green, KPNO H Yee, Dominion Astrophysical Observatory Multi-aperture Spectroscopy of Galaxies Associated with.... 4 meter 3.00 33.00 0.00 0.00

4898 D Hall, Space Telescope Science Institute K Hinkle, Kitt Peak National Observatory A Search for Dark Companions of K and M Giants 4 meter 0.00 0.00 2.00 16.20

5207 D Hall, Space Telescope Science Institute K Hinkle, Kitt Peak National Observatory A Search for Dark Companions of K & M Giants 4 meter 0.00 0.00 4.00 17.00

3790 J Harvey, National Solar Observatory/Kitt Peak SOLAR-Vacuum Telescope Synoptic Program Daily Magnetograms Solar Vacuum 0.00 0.00 50.50 257.00

-63- » i Nights Hours Days Hours 3790 J Harvey, Kitt Peak National Observatory Synoptic Program Daily Magnetograms Solar Vacuum 0.00 0.00 27.50 123.00

5141 D Hayes, Kitt Peak National Observatory V Straizys, Lithuanian Academy of Sciences JHKL Observations of Stars in the Taurus Dark Cloud Region 1.3 meter 4.00 22.00 0.00 0.00

5262 A Heiser, Vanderbilt University Search for Monoceros OBI and 0B2 Nr. 4 0.4 meter 5.00 12.00 0.00 0.00

5071 K Hinkle, Kitt Peak National Observatory F Clark, T Troland, University of Kentucky W Scharlach, D Johnson, National Bureau of Standards Coordinated SiO Maser and CO Absorption Line 4 meter 0.00 0.00 1.50 17.20

5211 E Hu, L Cowie, Space Telescope Science Institute Z Wang, Boston University Optical Emission Studies of Gas Systems in the Central 4 meter 4.00 33.50 0.00 0.00

4971 R Humphreys, M Sitko, University of Minnesota A Comparison of the Stellar Content, Luminosity Function... Nr. 1 0.9 meter 4.00 45.00 0.00 0.00

4981 P Ianna, B McNamara, University of Virginia Photometry of McCormick Parallax Stars Nr. 4 0.4 meter 7.00 48.50 0.00 0.00

-64- Nights Hours Days Hours 5229 G Illingworth, Kitt Peak National Observatory M Aaronson, K Cook, University of Arizona A Search for Cepheids & the Distance to M101 4 meter 1.00 0.00 0.00 0.00

4953 D Jennings, NASA Goddard Space Flight Center SOLAR-Nasa Contract—Laboratory FTS of Planetary Molecules McMath FTS Lab 0.00 0.00 1.00 7.00

4170 D Jennings, A Weber, NASA Goddard Space Flight Center J Keady, Los Alamos National Laboratory SOLAR-Long Term: Laboratory Infrared Spectroscopy of Planet McMath FTS Lab 3.00 18.00 3.00 28.00

3744 H Jones, T Duvall, Jr., NASA Goddard Space Flight Center SOLAR-NASA Contract, SMM Area Scans - Vacuum Telescope Solar Vacuum 0.00 0.00 1.50 12.00

3744 H Jones, T Duvall, Jr., NASA Goddard Space Flight Center SOLAR-NASA Contract, SMM Area Scans - Vacuum Telescope Solar Vacuum 0.00 0.00 3.50 33.00

4982 R Joyce, G Jacoby, J Africano, P Schmidtke, Kitt Peak National Observatory M Siegel, Steward Observatory Stellar Angular Diameters 4 meter 0.50 3.00 0.00 0.00

4913 R Joyce, G Jacoby, S Ridgway, P Schmidtke, J Africano, G Jacoby, Kitt Peak National Observatory M Siegel, Steward Observatory Stellar Angular Diameters 4 meter 0.34 0.00 0.00 0.0L

-65- Nights Hours Days Hours 5170 V Junkkarinen, Kitt Peak National Observatory Are there QSOs with Infalling Absorption Systems? 4 meter 4.50 35.75 0.00 0.00

4887 V Junkkarinen, Kitt Peak National Observatory Velocity Differences of QSO Emission Lines 4 meter 2.00 16.50 0.00 0.00 2.1 meter 3.00 14.50 0.00 0.00

4998 W Keel, Kitt Peak National Observatory Wolf-Rayet Stars in NGC 5430 2.1 meter 2.00 20.00 0.00 0.00

4705 W Keel, Kitt Peak National Observatory J Condon, National Radio Astronomy Observatory Extragalactic H II Regions with Enhanced Nonthermal Radio.. Nr. 1 0.9 meter 2.00 12.00 0.00 0.00

4890 T Kinman, C Mahaffey, Kitt Peak National Observatory H-alpha Survey for Emission-Line Galaxies 1.3 meter 2.00 5.50 0.00 0.00

4254 R Kron, University of Chicago D Koo, Carnegie Institution of Washington R Windhorst, Leiden Observatory Redshift Distribution of Faint Extragalactic Objects 4 meter 5.00 49.50 0.00 0.00

4839 R Kron, D Hamilton, University of Chicago An Observational Test for Galaxy Evolution 4 meter 3.00 0.00 0.00 0.00

-66- i Nights Hours Days Hours 5247 S Kukolich, University of Arizona SOLAR-Laboratory Spectroscopy on Molecular Complexes of... McMath FTS Lab 3.00 18.00 3.00 27.00

5173 D Lambert, V Smith, University of Texas, Austin CNO in Cool Red Giants 4 meter 5.00 41.00 2.50 15.00

5041 A Landolt, Louisiana State University UBV Photometry of Stars Useful for Checking Equipment Nr. 2 0.9 meter 4.00 6.00 0.00 0.00

4972 A Linnell, Michigan State University\Visitor KPN0til6/l/ High Speed UBVRI Photometry of W Ursae Majoris Stars Nr. 2 0.9 meter 8.50 66.50 0.00 0.00

4963 J Linsky, J Timothy, C Joseph, University of Colorado T Simon, University of Hawaii S Worden, University of California, Los Angeles M Giampapa, Sacramento Peak Observatory (KPNO) Monitoring Magnetic Fields and Active Regions on Late-type. McMath Main 8.00 63.00 0.00 0.00

4936 W Livingston, J Leibacher, National Solar Observatory/Kitt Peak 0 White, High Altitude Observatory SOLAR-Solar Cycle Variations of Sun as a Star... McMath Main 0.00 0.00 5.00 26.00

4936 W Livingston, J Leibacher, Kitt Peak National Observatory 0 White, High Altitude Observatory Solar Cycle Variations of Sun as a Star .... MMcM 0.00 0.00 3.00 16.00

-67- L Nights Hours Days Hours 5042 M Longair, Royal Observatory S Lilly, Princeton University Observatory J Allington-Smith, Mullard Space Science Laboratory Spectroscopy of a Statistical Sample of Faint Radio Galaxie 4 meter 2.50 28.75 0.00 0.00

5193 B Madore,- W Freedman, University of Toronto C McAlary, University of Arizona L Davis, Kitt Peak National Observatory The Distance to NGC 2403 4 meter 3.00 31.50 0.00 0.00

4706 B Margon, S Anderson, University of Washington The Contribution of OSOs to the Diffuse X-ray Background 4 meter 3.00 26.00 0.00 0.00

4706 B Margon, S Anderson, University of Washington The Contribution of QSOs to the Diffuse X-ray Background 4 meter 1.00 11.50 0.00 0.00 2.1 meter 1.00 12.50 0.00 0.00

4179 H McAlister, H Miller, W Hartkopf, Georgia State University 0 Franz, Lowell Observatory Speckle Interferometry with the GSU Speckle Camera 4 meter 5.00 58.50 0.00 0.00

5231 S McLaughlin, Space Telescope Science Institute\CSC Continuing Study of Algol Variables with UBV and H-Beta.... Nr. 4 0.4 meter 8.00 58.50 0.00 0.00

-68- L Nights Hours Days Hours 4840 K Merrill, R Joyce, K Gillies, F Gillett, Kitt Peak National Observatory Infrared Monitoring of Late Type Stars & Protostellar 1.3 meter 2.00 21.00 0.00 0.00

5001 K Merrill, R Joyce, K Gillies, F Gillett, Kitt Peak National Observatory Infrared Monitoring of Late Type Stars & Protostellar 1.3 meter 4.00 43.00 0.00 0.00

4841 K Mitchell, Virginia Polytechnic Institute & State Univer A Warnock, Pennsylvania State University\NASA Goddard Surface Density of Medium-Bright QSOS 2.1 meter 5.00 62.50 0.00 0.00

4743 D Monet, Mt. Wilson & Las Campanas Observatories C Dahn, U. S. Naval Observatory, Flagstaff Trigonometric Parallaxes of Intrinsically Faint Nearby 4 meter 3.00 14.50 0.00 0.00

5093 K Nordsieck, C Anderson, University of Wisconsin Doppler-Resolved Spectropolarimetry of Reflection Nebulae 4 meter 1.50 14.50 0.00 0.00

5094 K Nordsieck, R Myers, University of Wisconsin Infrared Polarimetry of Comets, Asteroids & Supergiant 2.1 meter 4.00 21.00 0.00 0.00

5045 C O'Dell, H Castaneda, Rice University Internal Velocity & Density Fluctuations in HII Regions 2.1m Coude Feed 5.00 47.00 0.00 0.00

-69- L Nights Hours Days Hours 5096 A Oemler, Jr., M Gregg, Yale University Spectral Synthesis of SO Disks 1.3 meter 3.00 14.50 0.00 0.00

4984 E Olsen, Copenhagen University G-Dwarf Problem - Metallicity Distribution in the Nr. 2 0.9 meter 8.00 51.50 0.00 0.00

5216 F Owen, National Radio Astronomy Observatory, VLA R Laing, Royal Greenwich Observatory CCD Surface Photometry of Bright Radio Galaxies Nr. 1 0.9 meter 5.00 45.50 0.00 0.00

5232 J Percy, University of Toronto Photometric Variability of Be Stars Nr. 4 0.4 meter 8.00 34.00 0.00 0.00

4260 D Peterson, State University of New York, Stony Brook Long-Period Spectroscopic Binaries in the Pleiades, Hyades 2.1m Coude Feed 3.00 30.00 0.00 0.00

4260 D Peterson, State University of New York, Stony Brook Long-Period Spectroscopic Binaries in the Pleiades 2.1m Coude Feed 5.00 37.00 0.00 0.00

4728 R Peterson, Lockheed Palo Alto Research Labs. Abundances in Globular Clusters of the Remote Hal° 4 meter 4.00 48.00 0.00 0.00

-70- i Nights Hours Days Hours 5249 B Pettersen, University of Texas, Austin SOLAR-Chromospheric Lines in Active Red Dwarf Stars McMath Main 5.00 54.00 0.00 0.00

4952 A Picard-Bersellini, Laboratoire de Photophysique Moleculaire Infrared Spectrum of N0C1 at 1800 cm -1 and 924 cm -1 McMath FTS Lab 0.00 0.00 2.00 14.00

5112 J Pier, C Pilachowski, Kitt Peak National Observatory Velocity Dispersion of Subdwarfs Near the Galactic Anti.... 2.1 meter 4.00 41.00 0.00 0.00

4939 A Pierce, National Solar Observatory/Kitt Peak SOLAR-Solar Rotation in High Level Lines; Nal & Solar Spect McMath Main 0.00 0.00 9.00 43.00

4939 A Pierce, Kitt Peak National Observatory Solar Rotation in High Level Lines; Nal and Solar Spectrum McMath Main 0.00 0.00 8.00 60.00

5218 C Pilachowski, Kitt Peak National Observatory H-alpha Emission in Metal Poor Giant Stars 2.1m Coude Feed 2.00 22.00 0.00 0.00

4905 J Pipher, A Moneti, University of Rochester Infrared Polarimetry Sources in the Taurus Cloud 2.1 meter 5.00 18.50 0.00 0.00

-71- L Nights Hours Days Hours 5143 R Probst, Kitt Peak National Observatory P Ianna, University of Virginia Photometric Selection of Astrophysically Interesting Faint. 2.1 meter 5.00 38.50 0.00 0.00

5234 L Ramsey, S Barden, Pennsylvania State University Starspot & Investigations for Short Period..- 2. lm Coude Feed 12.00 86.00 0.00 0.00

5266 K Rao, Ohio State University J Manheim, Wright Patterson Air Force Base SOLAR-Fourier Transform Spectroscopy of Ammonia McMath FTS Lab 3.00 30.00 3.00 32.00

5097 T Robertson, T Jordan, Ball State University Selection of Late Type Equatorial Photometric Standard Burrell Schmidt 7.00 47.00 0.00 0.00

5048 W Romanishin, NASA Goddard Space Flight Center S Strom, K Strom, University of Massachusetts An Abnormal Initial Mass Function in Low Surface 1.3 meter 5.00 31.50 0.00 0.00

4988 W Romanishin, NASA Goddard Space Flight Center Systematic Imaging Survey of Intrinsically Large Spiral.... Nr. 1 0.9 meter 4.00 36.50 0.00 0.00

5099 W Romanishin, NASA Goddard Space Flight Center Using J-K Color Profiles to Measure Stellar 1.3 meter 5.50 13.50 0.00 0.00

-72- L Nights Hours Days Hours 4748 A Rydgren, D Zak, Rensselaer Polytechnic Institute Photometric Search for Rotation Periods of Late-Type 1.3 meter 4.00 19.00 0.00 0.00

5180 A Saha, California Institute of Technology Photometry of Faint Variable Stars Nr. 1 0.9 meter 9.00 52.00 0.00 0.00

4914 W Scharlach, National Radio Astronomy Observatory, Tucson E Craine, University of Arizona Photometric Calibration for IRAS Mini-Survey Fields Nr. 4 0.4 meter 4.00 0.00 0.00 0.00

5113 E Schlegel, R Honeycutt, R Kaitchuck, Indiana University Time Resolved Spectroscopy of Accretion Disks in Short-.... 2.1 meter 5.00 53.50 0.00 0.00

5049 P Schmidtke, J Africano, Kitt Peak National Observatory Lunar Occultations of Double Stars Nr. 2 0.9 meter 0.50 4.00 0.00 0.00

4814 P Schmidtke, J Africano, Kitt Peak National Observatory Lunar Occultations of Double Stars Nr. 2 0.9 meter 0.50 3.00 0.00 0.00

4749 S Simkin, University of Wisconsin H Su, Purple Mt. Observatory Surface Photometry of Nearby Seyfert Galaxies Nr. 1 0.9 meter 4.00 40.00 0.00 0.00

-73- t Nights Hours Days Hours 5265 M Simon, SUNY at Stony Brook Measure Radial Velocities and the Halpha [N II] and Hbeta.. Nr. 1 0.9 meter 5.00 41.00 0.00 0.00

5222 T Simon, University of Hawaii K Hinkle, Kitt Peak National Observatory Eclipse Observations of Epsilon Aurigae 4 meter 1.50 21.00 1.00 4.00

5223 D Smith, University of Nevada Stromgren 4-Color and HB Photometry of Peculiar Upper Main. Nr. 4 0.4 meter 7.00 38.00 0.00 0.00

4989 M Smith, (KPNO) National Solar Observatory ASpectrographic Search for Nonradial Pulsation AmongJ 2.1m Coude Feed 7.00 68.00 0.00 0.00

4769 S Strom, C Pilachowski, Kitt Peak National Observatory K Strom, R Mundt, Max Planck Institut fur Astrophysik C Lada, J Stocke, University of Arizona Spectra of Exciting Stars & Shock-Excited Regions 2.1 meter 2.00 24.30 0.00 0.00

4750 S Strom, Kitt Peak National Observatory K Strom, J Stocke, University of Arizona A CCD Survey of Herbi-Haro Objects: The Search for Nr. 1 0.9 meter 8.00 53.00 0.00 0.00

4267 P Szkody, University of Washington A Study of the Disks in Short Outburst Period, High 2.1 meter 4.00 44.50 0.00 0.00

-74- Nights Hours Days Hours 5114 P Szkody, M Mateo, University of Washington Time Resolved Spectroscopy of the DQ Her Variables 2.1 meter 3.00 27.00 0.00 0.00

4267 P Szkody, University of Washington A Study of the Disks in Short Period, High Excitation 2.1 meter 4.00 44.00 0.00 0.00 1.3 meter 4.00 17.00 0.00 0.00

4813 M Ulmer, J Loughlin, Northwestern University P Hintzen, NASA Goddard Space Flight Center Optical Studies of Low X-Ray Luminosity Clusters of Galaxie 2.1 meter 2.00 4.50 0.00 0.00

4818 A Upgren, E Weis, Wesleyan University H Nations, Pennsylvania State University Calibration of Radial Velocities Obtained from Objective... Burrell Schmidt 7.00 25.50 0.00 0.00

5161 G Wallerstein, D Geisler, University of Washington Abundances & Improved Color-Magnitude Diagrams for 1.3 meter 4.00 9.00 0.00 0.00

4733 P Wannier, R Sahai, California Institute of Technology 4.6 Micron Carbon Monoxide Lines in Extended 4 meter 4.66 40.50 3.00 19.50

4820 G Wegner, Dartmouth College Spectroscopy of DB White Dwarfs 2.1 meter 4.00 31.00 0.00 0.00

-75- L Nights Hours Days Hours 4991 W Wehlau, J Matthews, University of Western Ontario A Search for Rapid Oscillations Among Cool Northern AP Star Nr. 2 0.9 meter 10.00 50.20 0.00 0.00

5102 E Weis, Wesleyan University A Photometric Search for Nearby Dwarf M Stars Nr. 2 0.9 meter 7.00 46.50 0.00 0.00

4942 0 White, High Altitude Observatory W Livingston, J Leibacher, National Solar Observatory/Kitt Peak SOLAR-Ca II Variability McMath Main 0.00 0.00 2.00 7.00

4942 0 White, High Altitude Observatory W Livingston, Kitt Peak National Observatory Ca II Variability McMath Main 0.00 0.00 1.00 0.00

4822 R Wing, Ohio State University L Palmer, TRW, Inc. Narrow-Band Photometry of Red Giants in Galactic Clusters 1.3 meter 5.00 24.00 0.00 0.00

5005 A Witt, University of Toledo Spectroscopic Studies of Extended Red Emission in 2.1 meter 2.00 12.50 0.00 0.00

5004 A Witt, University of Toledo Survey for Presence of Extended Red Emission in Reflection 1.3 meter 4.00 34.00 0.00 0.00

5116 M Zeilik, R Elston, University of New Mexico Infrared Photometry of RS CVn Stars with Large Optical 1>3 meter 0i00 0<00 4-0g 17,00

5184 N Zotov, Gannon University Spectra of Case Western Survey Blue Stellar Objects 2.1 meter 4.00 27.00 0.00 0.00

-76-

&L*J ecr^ National Qptica! RECEIVED Astronomy NOAO Observatories JUNO 8 1984 May 15, 1984 DIRECTOR'S OFFICE

Dr. John M. Teem National Solar Observatory President, AURA, Inc. Sunspot, NM 88349 Suite 820 (505) 434-1390 2100 Pennsylvania Ave., N.W. Telex: 0666-484 Washington, D.C. 20037 AURA KPNO TUC Dear John, Here are two copies of NSO's Quarterly Report for the second quarter of FY 1984, January - March 1984. Copies have also been sent to those below. This quarterly report covers activities at both NSO/Sacramento Peak and ' NSO/Tucson.

Sincerely,

-s~iyt^£*^ >t>^ Jack B. Zirker, Acting Director

Enclosures

xc: (with enclosures) Dr. J. Jefferies - Dr. P. Bautz Dr. J. Beckers Dr. K. Rieqel Dr. G. Burbidge Mr. S. Tuttle (5 copies) Dr. T. Hagfors Mr. C. Frost Dr. K. Pierce AURA Solar Standinq Committee NSO/Tucson Library AURA Visiting Committee Dr. P. Osmer NSO Users' Committee Dr. M. Roberts

JBZ:mhr

Operated by the Association of Universities 'of Research in Astronomy. Inc under contract with the N.'itionnl Science Foundation

NATIONAL SOLAR OBSERVATORY QUARTERLY-REPORT January 1, 1983 - March 31, 1984

I. Telescope Usage The following table summarizes the use of NSO's telescopes during the first quarter of FY 1984. The telescopes in Table A are at NSO/Sacramento Peak, and those in Table B are at NSO/Tucson.

Table A: SUMMARY INSTRUMENT USAGE - 2nd QUARTER FY 1984 (Scheduled Hours)

Tower Big Dome Total

Visitors 503.5 (64.4%) 534.5 (33.8%) 1038.0 (43.9%)

AURA Staff 115.0 (14.7%) 135.5 ( 8.6%) 250.5 (10.6%)

USAF Staff 108.5 (13.9%) 502.0 (31.8%) 610.5 (25.9%)

Community1 0 168.0 (10.6%) 168.0 ( 7.1%)

Monitoring^ 0 179.0 (11.3%) 179.0 ( 7.6%)

Engineering-' 40.0 ( 5.1%) 0 40.0 ( 1.7%)

Shut Down4 15.0 ( 1.9%) 61.0 ( 3.9%) 76.0 ( 3.2%)

TOTAL 782.0 (100%) 1580.0 (100%) 2362.0 (100%)

Synoptic observations for Solar Geophysical Data 2 Sporadic activity observations ^Includes time used in interfacing instruments, testing, and minor maintenance Maintenance and major repair.

2nd Quarter, FY 1984 Table B: SUMMARY INSTRUMENT USAGE - 2nd QUARTER, FY 1984 (scheduled hours)

Part 1: FTS Laboratory Nights Days Visitor 321.0 (87.4%) 243.4 (90.2%) Staff 30.9 ( 8.4%) 26.3 ( 9.8%) Engineering 0.0 ( 0.0%) 0.0 ( 0.0%) Shutdown 15.3 ( 4.2%) 0.0 ( 0.0%) Total 367.2 (100%) 269.7 (100%)

Part 2: McMath Nights Days Visitor 752.0 (18.3%) 874.5 (40.2%) Staff 432.0 (10.5%) 1091.5 (50.2%) Engineer! ng 40.0 ( 1.0%) 26.1 ( 1.2%) Shutdown 2886.0 (70.2%) 182.5 f 8.4%) Total 4110.0 (100%) 2175.0 (100%)

Part 3: Solar Vacuum Telescope Nights Days Visitors 0.0 (0.0%) 744.0 (31.2%) Staff 0.0 (0.0%) 1362.0 (57.1%)

Community 0.0 (0.0%) 0.0 ( 0.0%) Engineering 0.0 (0.0%) 52.2 ( 2.2%) Shutdown 0.0 (0.0%) 226.0 ( 9.5%) Total 0.0 (0.0%) 2384.0 (100%)

2nd Quarter, FY 1984 II. Visitor Research

During the second quarter of FY 1984 the following visitors used NSO's instruments (NSO staff collaborators shown in parentheses).

A. NSO/Sacramento Peak

Hilltop P. Wilson, University of Sydney Sunspot survey H. Yoshimura, University of Tokyo Birth and evolution of sunspots

Tower H. Beebe, New Mexico State University, and H. Yun, Seoul National University (F. Hill) Sunspot spectra R. Canfield, University of California, San Diego Flare H-alpha extreme wing observations G. Elste, University of Michigan Solar photospheric network D. Haber, JILA/University of Colorado (F. Hill)

Acoustic waves J. Malville and G. Toot, University of Colorado Velocity fields in prominences R. Smithson, Lockheed Research Laboratories Lockheed Active Mirror J. Thomas, University of Rochester (B. Lites) Umbra oscillations in the photosphere P. Wilson, University of Sydney (G. Simon) Magnetic and velocity intensity fields G. Withbroe and S. Habbal, Center for Astrophysics Study of bright points

2nd Quarter, FY 1984 Big Dome T. Brown, High Altitude Observatory (J. Evans) Debugging Fourier Tachometer J. Kuhn, Princeton University Intermediate-scale global oscillations D. Landman, Institute for Astronomy (R. Smartt) Line profiles in prominences Spectroheliograms in the oxygen lines at 7775A and 8446A L. Petro and P. Foukal, Atmospheric & Environmental Research, Inc. Velocities in sunspots E. Seykora, East Carolina University (R. Smartt) Differential photometry - limb darkening S. Worden, USAF/OUSDRE (S. Keil), jolar Rotation, 3898A to 3954A

B. NSO/Tucson

FTS Laboratory J. Black and P. Bernath, University of Arizona (J. Brault) Spectroscopy of CS+ L. Brown, R. Toth and R. Poynter, Jet Propulsion Lab FTS laboratory spectroscopy in support of remote sensing of the stratosphere and planetary atmosphere R. Engleman, L. Faires and B. Palmer, Los Alamos National Laboratory Atomic oscillator strengths from the inductively couple plasma and other laboratory Fourier transform spectroscopy D. Jennings, NASA-Goddard Space Flight Center Laboratory FTS of planetary molecules D. Jennings, NASA-GSFC; A. Weber, National Bureau of Standards; and J. Keady, Los Alamos National Laboratory Laboratory infrared spectroscopy of planetary molecules S. Kukolich, T. Tipton, and J. Choe, University of Arizona Laboratory spectroscopy on molecular complexes of astrophysical interest

2nd Quarter, FY 1984 J. Lawlor, D. Duquette and P. Chevako, University of Wisconsin Atomic oscillator strengths of the transition metals A. Picard-Bersellini, Laboratoire de Photophysique Moleculaire Infrared spectrum of N0C1 at 1800cm"1 and 924 cm"1 K. Rao, Ohio State University; and J. Manheim, Wright Patterson AFB Fourier transform spectroscopy of ammonia E. Worden, Lawrence Livermore National Laboratory; and J. Conway, Lawrence Berkeley Laboratory To measure frequencies and intensities of emission lines of Actinide elements for determination of energy levels and branching ratios

McMath Telescope P. Foukal and L. Petro, Atmospheric & Environmental Researach, Inc.; and W. Rosen, Vassar College (A. Pierce) An investigation of time-dependent variations in photospheric limb darkening as a diagnostic for changes in solar luminosity W. Kalkofen, Smithsonian Astrophysical Observatory; and I. Furenlid, Georgia State University Chromospheric wave heating J. Linsky and S. Saar, JILA Studies of magnetic fields in late-type stars J. Linsky, S. Saar, C. Joseph, JILA; J. Timothy, Stanford University; T. Simon, Institute for Astronomy; and S. Worden, USAF/OUSDRE (M. Giampapa) Monitoring magnetic fields and active regions on late-type stars by coordinated KPNO-IUE observations J. LoPresto, Edinboro University (A. Pierce) Solar gravitational redshift wavelengths of solar lines versus laboratory lines G. O'Brien, Indiana University (M. Smith) A search for ^10830 line variations in late-type stars, phase I B. Pettersen, University of Texas Chromospheric lines in active red dwarf stars

2nd Quarter, FY 1984 G. Stokes, Battelle Northwest Laboratories Telluric absorption spectroscopy S. Vogt and G. Penrod, Lick Observatory Doppler imaging spectroscopy of RS CVn stars and studies of nonradial oscillations on B stars 0. White, HAO and Lazy FW Ranch (W. Livingston) Ca II variability 0. White, HAO and Lazy FW Ranch (W. Livingston and J. Leibacher) Solar cycle variations of Sun as a star S. Worden, USAF/OUDRE (M. Giampapa) Measurement of magnetic fields on late-type stars

Solar Vacuum Telescope P. Foukal and W. Chiangi Atmospheric & Environmental Research, Inc.; and T. Duvall, Jr., NASA-GSFC Photospheric photometry H. Jones and T. Duvall, Jr., NASA-GSFC SMM area scans

III. Visitor and Staff Research Highlights

The National Solar Observatory has actively supported and encouraged research connecting solar and stellar phenomena. Recent progress in this area promises to enhance our understanding of solar and stellar activity and the processes involved in nonradial oscillations. M. Giampapa (NSO/Tucson) and R. Rosner (Harvard) have investigated the nature of activity and magnetic fields on main sequence F stars, and submitted a paper on their work to Ap. J. Letters. These stars have convection zones which are shallower than the Sun's and rotation rates considerably higher than the Sun's. Observations of Ca H and K emission from these stars show little if any variations on a stellar cycle time scale and little rotation modulation. Yet, the level of Ca II, Mg II, and transition region line emission is several times the solar level as is the x-ray luminosity. Giampapa and Rosner suggest that these data indicate the presence of magnetic activity without the

2nd Quarter, FY 1984 6 formation of large isolated active regions or cyclic activity. They suspect that these stars have a uniform network of magnetic fields. If any spots exist at all, they must be small and uniformly scattered. They also suggest that the flux ropes produced in these shallow convective zones tend to be smaller than those produced in the Sun and do not expand as much when they rise to the surface. Observations such as these can help constrain solar and stellar dynamo theory.

M. Smith and D. Jaksha (NSO/Tucson) continue to refine and improve the instrumentation for the nighttime use of the McMath. In his own research with these instruments Smith has investigated nonradial pulsations in hot stars and has made some fascinating discoveries which may have implications for the solar oscillations. He has monitored line profile variations in Persei and finds three commensurate periods in the ratio 1:4:6. This result suggests the presence of an "autoresonance" phenomena in which stray modes are excited by resonance of a basic long period mode, presumably deep inside the star. If similar phenomena are found in other stars, they might suggest the excitation mechanism for solar oscillations, which is highly uncertain at present. A seven night observing run on <*Virginis showed hints of a correlation between line profile distortions (nonradial pulsations) and orbital phase. The prob able "bisynchronism" of this star in its orbit (two rotations per revolution) suggests that the periods of the pulsations can be directly compared to the star's rotation period. Here, too, it appears that an all important long period mode is excited in these stars -- it may well coincide with the rota tion period. Smith suggests that resonances between rotation and convection currents in the stellar cores may be the excitation mechanisms for these oscillations in B stars.

Work related to the solar global oscillations quickened its pace during the last quarter. Several NSO staff members studied the performance of a glo bal oscillation observing network. Under the leadership of J. Leibacher (NSO/Tucson) the Global Oscillation Network Group (GONG) was formed to inves tigate the scientific goals and instrumental requirements of such a network (see section VI, on meetings). F. Hill, R. Stebbins (NSO/Sac Peak) and G. Newkirk (High Altitude Observatory) used data on the meteorological

2nd Quarter, FY 1984 7 characteristics of several Dossible observing sites in order to estimate the performance of different possible networks. They found that a 93% duty cycle could be expected with a network of six sites. Fewer sites, or a poor selec tion of sites, decreased this duty cycle and introduced additional artifacts in the frequency spectrum. NSO plans to install sunshine monitors at five sites during FY 1985 and to compare the actual and predicted duty cycles of possible networks. R. Stebbins has selected and ordered some of the necessary equipment. In collaboration with J. Toomre and B. Merryfield (U. Colorado) and D. Gough (Cambridge), Hill has simulated the effects of seeing on the analysis of the solar p-mode oscillations. They find that for the large scale modes (spherical harmonic degree 1< 150) the analysis is largely unaffected by seeing. However, the smaller modes, 1,> 150, can be severely degraded. Analy ses such as this will be useful in providing criteria for global oscillations observing instruments, jR. Smartt (NSO/Sac Peak) and J. Harvey (NSO/Tucson) have explored a Fabry-Perot concept of a Doppler analyser for the network instruments. They simplified their original optical system and verified the existence of an effect on imaging through a Fabry-Perot that will require special strategies to compensate. After careful comparison of a solid etalon with a Zerodur-spaced etalon, they now favor the solid etalons. The details of an observing network will be settled during the upcoming quarters.

J. Harvey and T. Duvall (NASA affiliate) obtained a superb set of data on solar oscillations during a 17 day run at the McMath telescope in May, 1983. The analysis of this data in collaboration with J. Leibacher, W. Dziembowski (Warsaw), P. Goode (U. Arizona) and D. Gough (Cambridge) has provided a deter mination of solar rotation variations with depth. The results indicate that the rotation of most of the interior is quite close to that of the surface. The major exceptions are a local maximum in the convection zone, an apparent minimum around r = 0.25 R, and a rapidly rotating core below r = 0.2 R. The quadrupole moment of the Sun was established with an accuracy which was lim ited equally by solar model uncertainties and by the observational noise but in any event J2 was too small to affect tests of the theory of relativity that involve the perihelion advance of Mercury.

2nd Quarter, FY 1984 K. Pierce (NSO/Tucson). and J. LoPresto (Edinboro State College) have monitored solar differential rotation with the double pass spectrograph on the McMath telescope using lines of Fe, Mg, Na, K, Si and 0 in the wavelength interval AA3820 - 10827. The results were analysed using both Legendre poly nomials and a power series representation. The differential rotation they found for 1979 - 1983 is very close to the result obtained by Howard and Har vey in 1966 - 1968 at Mt. Wilson but with a slightly greater amplitude. They note that day to day variations in the rotation rate occur in the equatorial zone but a steady rotation rate is found outside of the sunspot zone. B. Lites (NSO/Sac Peak) has completed an analysis of chromospheric oscillations in sunspots. Simultaneous observations of the profiles of the He I 10830 line and the Ca II H line in a sunspot umbra were obtained with the Tower telescope, Echelle spectrograph, and Multi-Diode Array. The time sequence shows that the He I line is in weak absorption over the sunspot umbra and undergoes periodic Doppler shifts with a 17 km/s peak-to-peak amplitude. The amplitudes and waveforms of these line shifts suggest that the oscillations are nonlinear in the upper chromosphere and lend support to the mechanism of resonant transmission of oscillations excited from below the chromosphere. The phase differences between the Ca II H line and the He I line are not easily interpreted. Lites suggests that nonlinear interactions between the oscilla tions and the upper chromosphere, in combination with radiative transfer effects in Ca II, may produce much of the observed phase differences. If Lites' future computations are successful in reproducing the oscillatory nature of the He I and Ca II lines, he will apply a similar analysis to the quiet solar chromosphere.

R. Smartt (NSO/Sac Peak) has studied observations of post-flare loops obtained with the 20-cm emission line coronagraph of post-flare loops. The record consists of coronal photographs in Fe XIV (5303 A), Fe X (6374 A) and Ha, and the disc in H«, which show the development of the loops over an 8-hour period. The coronal images appear to show evidence of localized heating in the region where the tops of several the loops aoproach each other. This result is consistent with explanations of flare radio emission, in which mag netic reconnection, and localized heating, can occur between closely related

2nd Quarter, FY 1984 9 loop systems. Smartt will study his data to try to establish if they are con sistent with this interpretation. Using data obtained with the Tower telescope and the Echelle spectro graph on Sac Peak, R. Canfield and T. Gunkler (UCSD) have examined electron heating and chromospheric evaporation during a flare also observed from the Solar Maximum Mission (SMM). They have compared the observed flare H« pro files to theoretical H« profiles based on physical models of chromospheric flare processes and model parameters inferred from the SMM x-ray observations. They find that the observed H* profiles show the theoretically predicted enhanced wing signature of nonthermal electrons. They infer coronal pressures above the flare which agree well with the values inferred from the soft x-ray data. They conclude that nonthermal electron heating is insufficient in driv ing chromospheric evaporation — thermal conduction appears to be the dominant mechanism. This process successfully accounts for the measured coronal pres sure at the time of maximum emission measure. R. Altrock (AFGL/Sac Peak) has successfully produced the first full disc map of Ca XV 5694 A coronal emission using the three line coronal photometer in the Big Dome. This line is significant for its high excitation tempera tures (-3,000,000° K) and is associated with active regions having a high level of activity. Whenever Ca XV emission is detected a full-disc map is produced and sent to the space forecasting centers in Boulder, Colorado, and Offutt AFB, Nebraska.

IV. Status of Projects

The Fourier Tachometer II has been installed and has been exercised dur ing several engineering runs. The filter ovens were installed and calibrated and a new modulator rotator was built. All the electronics work and most of the optics are ready to go. Replacement of the Sac Peak Tower computer (a Sigma 3) has started. The 68000 computer is available and its interface to CAMAC has been purchased. Most of the modules have been bought or are on hand. This project still

2nd Quarter, FY 1984 10 requires a few more modules to be selected and purchased and will then require a considerable amount of programming. Work has proceeded on the Correlation Tracker. Arrambide and Healy wrote a Fortran program to model the bit-slice processor on the Correlation Tracker. This program proved that the hardware design will do the Fast Fourier Transform in the time allowed. It further showed that a discrete two- dimensional transform can be linearized so that existing algorithms can be used. Also, existing hardware sequences can be used to do the 2-D transforms without great changes. Additional work in modelling the bit-slice processor is expected. Improvements have been installed on the McMath's main spectrograph. An interferometer was installed to control the grating rotation. The original grating drive showed slight irregularities. While tjhe improvement has reme died this problem, small errors have now shown up. The grating mount vibrates and phase delays in the electronics introduce distortion and wavelength shifts in the recorded spectra. Solutions to these problems are being sought.

V. Administration and Facilities

The Corona Cafe was reopened on a regular schedule for lunch on 21 March with the return to work of Patti Rentschler. Several informal meetings have been held with representatives of the Astrophysical Research Corporation (ARC) concerning their proposed Apache Point Observatory. Matters such as roads, water, electricity, telephone, et cetera, have been discussed. ARC will have a meeting at Sunspot on 10 April to further refine their plans. A contract for the reconstruction of a portion of the Sunspot road, near Sunspot, has been awarded to Sunrise Services, an El Paso, Texas, small disad vantaged business. Work is expected to begin early in the next quarter. The remainder of the road construction has been divided into two parts, with the portion which goes through the Top of the Pines subdivision being scheduled to be done after all other work has been completed. This will allow the State of

2nd Quarter, FY 1984 u New Mexico more time to acquire right-of-ways through this subdivision. The FHWA has scheduled a construction meeting at Sunspot on 11 April.

VI. Meetings J. Zirker and R. Dunn attended meetings of SOT co-investigators in Washington, D.C. (Jan. 16) and Baltimore (Feb. 23-24) In January, Zirker held a staff meeting of NSO/Tucson personnel, and attended a meeting of the NOAO Management Committee in Tucson. Another NSO/Tucson staff meeting was held in February, as was ameeting on the pro posed Global Oscillations Network project. In March, Zirker and F. Hegwer attended meetings in Tucson of the AURA Board, Executive Committee, and Solar Standing Committee. Zirker and other NSO staff members attended a meeting of the NOAO Management Committee to dis cuss project priorities for FY 1985.

2nd Quarter, FY 1984 1?