Occuttm'on@Newstetter

Volume IV, Number 5 August, 1987 ISSN 0737-6766

Occultation Newsletter is published by the International Occultation Timing Association. Editor and compos- itor: H. F. DaBol); 6N106 White Oak Lane; St. Charles, IL 60174; U.S.A. Please send editorial matters, new and renewal memberships and subscriptions, back issue requests, address changes, graze prediction requests, reimbursement requests, special requests, and other IOTA business, but not observation reports, to the above.

FROM THE PUBLISHER IOTA NEWS

This is the third issue of 1987. It is the fifth David Id. Dunham '~.. issue of Volume 4. Paul Maley has made arrangements for this year's When renewing, please gfve your name and address exactly as they ap" IOTA meeting to be held in the Houston, TX, area on pear on your mi1ing )abe), so that we can locate your file; ff the label should be revised, tel) us how it should be changed. Saturday, October lOth, as noted on p. 58 of the last issue. The meeting, open to the public, will If you wISh, you may use your VISA or KasterCard for payrmts to IOTA; start at 9 am in the Hess Room of the Lunar and Include the account ntnber, the expiration date, and your sfgnature. Card users must pay the M) prices. If paying by cash, check, or Planetary Institute, 3303 NASA Road i, just east of money order, please pay only the discount prices. the johnson Spaceflight Center and about 35 miles Full Discount price price southeast of downtown Houston. The meeting will IOTA rmbership dues (incl. o.n. and arW swpments) break for lunch at noon, and will adjourn at 3 pm, for U.S.A.. Canada, and Kexico $12.50 $12.00 after which we may continue with some informal dis- for m others (to cover higher postage COStS) 17.71 17.00 cussions at another location. An agenda will not be Oceultation N~lettar subscMptionf (i year " 4 Issues) drawn up until shortly before the meeting, but it by surface mail will certainly include (but not be limited to) a for U.S.A., Canada, and Mexico? 8.33 8.00 very short business meeting, reports of this year's for al] others 8.17 7.84 by air (AO) mafj3 solar eclipse trips, plans for future solar eclips- for area 'A"' 9.96 9.56 es, showing of the better eclipse and occultation for area "g"S 11.38 10.92 fOr all other countries " 12.79 12.28 videotapes made during the past year, predictions and planning for lunar events (especially, Pleiades Back issues of q.n. by surface mail passages and grazes of lst-magnitude stars) and as- O.N.o.n. lj (14)(I) thruthruo.n.o.n. jq (13nl.. each 1.041.82 1.001.75 teroidal occultations during 1988, and status re- q.n. 4 (2) and later fssues. each 2.08 2.00 ports on the various computer projects. Unsuccess- Back issues of o.h. by air (AO) maf13 ful attempts were made to secure a meeting room for o.n. i (I) thru o.k. j ()3), each 1.51 1.45 q.n· : {!:)athru o.n. q ()), each 2.29 2.20 Sunday, Oct. 11, to bring the meeting time closer to o.n. nd later Issues, each 3.12 3.0'0 grdze of 1.8-mag. El Nath (Beta Tauri), which will (There are 16 Issues per volume, al) still availoble) " occur in the area around 4:18 am CDT Monday morning, Although they are avallable to IOTA members wIthout Oct. 12. Those who can stay untiNthen are invited charge, non-mdjers mst pay for the fo11owfng ft~: to join local efforts to observe the graze; those Local cfrcwstance (asteroidal appulse) predfctfons (entfre current list for your area) 1.04 1.00' travelling by plane may be able to'arrange to borrow Graze limit and profile prediction (each graze) 1.56 1.50 a local telescope to avoid bringing their own. But Papers explaining the use of the predictions 2.60 2.50 potential observers of this event are forewarned Supplements for South America wIll be available at extra cost through that the predicted profile is very smooth, promising Ignacio Ferrln (Apartado 700; Pkrida 5101-A; Venezuela), for Europe multiple occultations only for a very narrow range through Roland Bontnsegna (Rue dc Nrlembourg, 33; 8-638) DQURBES; whose location is hard to predict (that is, chances Belgium), for southern Africa, through K. d. Overbeek (Box 212; Eden- vale 1610; Republic of South Africa), for Australfa and New Zealand, of seeing only 0 or 1 occultation are high). If you through Graham Blow (P.0. Box 2241; Wellington; New Zealand), for Ja- are interested in attending the meeting, information 146,pem, japanj.throu h ToshfoSupplementsKSrose for(1-13a)) Shfmomarukoother areas l-chome;wfl] be Ota-ku,availableTokyofrom for out-of-town participants can be obtained from JIm Storm (Route )3, Box 109; London, KV 40741; U.S.A.) by surface Paul Maley; 15807 Brookvi11a; Houston, TX 77059; mall at the low prfce of' ).23 1.18 U.S.A.; telephone 713,488-6871. Also contact him if or by air (AO) mail at 2.04 ).96 you want to give a presentation, or have a specific Observers from Europe and the British Isles should joIn IOTA/ES, send- topic that you would like to see included in the ing DM SO.-- to the account 10TA/ES Bartold-knaust Strasse 8, 3000 agenda. Hannover 91, Postglro Hannover 555 829 - 303, bank-code-nuOer (Bank- 1eltuh1) 250 )00 30. Fu)) ~ership In IOTA/ES Includes the supple- Ment for European observers (total and grazing occultatfons). The "Universe '87" superconvention held at Pomona i Single issue available at k of price shown. College in Claremont, CA, was very successful, and 2 Price Includes any supp7ements for North Amerfcan observers. gave me a chance to meet some IOTA members for the 3 Not avaflab)e for U.S.A., Canada, or Mexico. first time, and see others whom I had not seen in 4 Area 'A" Includes Central America, St. Pierre and Mquelon, Carib- bean fslands, Bahamas, Bermuda, coicmm, and Venezuela. If desfred, many years. Members from all over the U.S.A. were area "A" observers may order the 5upp)ement for North Wrlcan observ- present, with a total attendance of about 900 (near- ers by surface mail @ 1.23 1.18 ly half of these were teachers who attended special or by air (AO) Ml) 0 1.56 1.50 5 Area "8" $nc1udes the rest of South America, Medfterranean Africa, teaching sessions during the weekend). One conven- and Europe (except Estonia, Latvia, Llthuanft, and U.S.S.R.)- tion participant (Tom Cragg) came from Australia. I

91 " " " "" t?

92 prepared a lO-minute videotape showing seven of the Europe just before or after the 1990 july eclipse, best grazes in my collection, along with my record- or in the U.S.A. or Mexico near the 1991 july large- ings of the 1983 occultation of 1 Vulpeculae by Pal- magnitude eclipse. Steven Edberg has already inde- las and the 1984 broken-annular eclipse. I showed pendently suggested an international superconvention this during one of my two talks, and discussed the in Mexico in 1991 july. pa11as occultation during the other. We also con- ducted a workshop on occultations, during which I On p. 58 of the last issue, I reported that a pro- went over the basics, Larry Dunn demonstrated his posal to close the Australian short-wave time signal realistic occultation simulation-reaction time test- station, VNG, had been dropped. Shortly after the ing software on a Macintosh computer, and Joan dis- issue went to press, I received a letter from S. C. cussed the status of the various IOTA pc projects Moon, secretary of Telecom Australia, which had (see p. 109). At the meeting, john Westfa11 passed polled seven Australian government departments about out some copies of a "Pomona Edition" of The Weekly their use of VNG. Moon said: Planet, produced by the Association of Lunar and Planetary Observers. This includes daily charts of "Only three out of the seven departments contacted the Moon outlining the maria and major craters, and responded indicating that VNG was currently being shows the terminator. \Aestfa11 produces these with used. One indicated that their future needs could his Apple computer, with input consisting of the be met by other technology. The others advised a date, time, and geographical coordinates for calcu- continuing need for VNG. lating topocentric librations. I think that this would be valuable for portraying important occulta- "In view of the use identified by the departments '" tions, especially for locating reappearing stars, concerned, Telecom will continue with the VNG serv- and Westfa11 said that he would send me a diskette ice for the time being. It will consult further with the software and database. The lunar features with the departments which have indicated future re- database probably can be transferred to an IBM PC, quirements for the time and frequency service. for which similar software could be written. "However, Telecom's position is clear in that whilst One of the topics to be discussed in Houston will be it will continue to negotiate with interested de- the time and location of the 1988 meeting. The of- partments, it cannot continue indefinitely meeting ficial meeting must be held in Texas, but the date the costs of a service for which it has no use it- does not need to be decided until a few months be- self nor any charter to provide." forehand, to publish in O.n. at least a month in ad- vance. At the symposium in Paris in June (see p. The section of Computer Sciences Corporation that I 113), the possibility of holding a joint I0TA-IOTA/ work for will be moving about 15 miles from Silver ES meeting was discussed. Iceland was suggested as Spring to the Greenbelt-Seabrook area of Maryland a possible location, a compromise between Europe and late this year. Shortly after that happens, joan North America. Bermuda, the Azores, and the Canary and I plan to move to the same area, and we will Islands might also be considered. But I don't know close P.0. Box 7488, Silver Spring, MD 20907. You if there is sufficient interest for enough people to may keep using it for the time being, since our mail travel farther than usual just for a joint occulta- will be forwarded to our new address. As soon as a tion meeting. Another possibility is to join a su- new address is determined, it will be published in perconvention of other astronomical societies, such o.n. and Sky and Telescope. Although his permanent as the ones just held in Paris and in Claremont, CA, address will remain unchanged, H. F. DaBo11 will be this year. It will probably be awhile before anoth- at his sumer home in Michigan's Upper Peninsula for er superconvention is.held, but if one is consid- a considerable fraction of each year. Whenever ap- ered, a compromise location like one of the ones propriate, first class mail will be forwarded, and "-" mentioned might encourage more international parti- phone calls to the St. Charles number will be refer- cipation. Another possibility is to organize the red to the Naubinway number by phone company record- meeting around a total solar eclipse, which many . ed announcement. IOTA members might want to observe, anyway. But few will be attempting the eclipse in March next year. We expect to publish the next issue of Occultation Possibilities might be to hold a joint meeting in Newsletter in November.

LET'S REPORT OCCULTATION TIMINGS ON DISKETTES sent to me at P.0. Box 7488; SilvEr Spring, MD 20907. lde can convert them to IBM-compatible files that we David Id. Dunham will send to ILOC and others who need them. hie en- courage as many observers as possible to report both Most occultation observers have experienced delays, total and grazing occultation data on diskette. In and found errors in, the residual calculations they some countries and regions, we hope that observers receive after reporting timings to the International can make arrangements so that those without comput- Lunar Occultation Centre (ILOC) in Tokyo. Recogniz- ers can send their written reports to those who have ing that these are caused primarily by ILOC'S limit- PCS, to send as many reports as possible to ILOC in ed staff for putting the written reports into ma- machine-readable form. If you have access to a PC chine-readable form for computer processing, I sug- and are willing to type reports for others in your gested to Akio Senda that the observers themselves area, contact me at the address above or telephone could do most of this job. He agreed, and sent me me at 301,585-0989, and we will publish your address the format for their card-image formats for the ob- in a future issue of o.n. for this purpose. The servations, which can be sent to ILOC on IBM-compat- more reports that are sent to ILOC on diskette, the ible 3js-, 5k-, and B-inch diskettes (or k-inch mag- faster will be the turnaround time for returning re- netic tape, but diskettes are much more comnon). siduals. Waiting for Earth-rotation observations Standard ASCII text files on 5!rinch diskettes writ- (UT1 - UTC corrections) delays distribution of ILOC ten with an Apple 11+, or equivalent computer can be residuals, but for preliminary results, predicted 93

D values can be used m mmmmmmmmmUUoUoUcjUUU that have much m . LtuljcrunmcqmcncrujUUUUUUUcjQ r· < smaller errors than ID ' other errors (star in u) W ' position, limb cor- r") mo CV Z rections, visual ~1 ·% timing) that affect C> m . O\ a the observations. W O'6 + a Consequently, as an m c'q Kr-r- incentive to those in cycnn % qq mmm who report data on R Z&& ^"^ diskette, ILOC c-l QH ODD hopes to set up its a >cZj >>>>>mmmpHHHHpppµp · Ob U)m= mcnr"j mHNHNHNNNNMNHN^NK^NK encl (However, he can m ·0DU (D K :Jww 0\ not read B-inch id net: 333 r-UD diskettes, and 54- in % W CJXQ inch floppies are rn ZD c'q^o0 CV cvcncv 2>-1 r" O 'cC ~cj·t >=:< c44DmlmDomNoo\u)olcjamu)lcnncja that the process is vo =hcj ~cq^ CjZU) oD\oNcna!bNmr·a'\oom|lnKc4wUn\oc4 CIr-l difficult at first, Ln MFJZ Q Nc")·t > U) DOODODDNU)C7DDDOOOOOOD - careful to avoid CV F-l · · ··0 ¢00¢o¢o©wwwwmwcDmmm©©co©© Cud

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Occultations and appu)ses by objects other than the The file should be a standard ASCII file readable by Moon (primarily by as teroids, planets, and comets) IBM, and equivalent, PCs; any word processor capable can also be reported cn diskette. But events in- of creating such a file can be used . It is impor- volving these 0ther objects shod d be sent to james tant to type all letters as capital s; if your com- Stann; Route 13 , Box 109; London, KV 40741; U.S.A.; puter has a Caps Lock key, keep it on as you type with a copy sen t to me for positi vc (actual occulta- the report. ILOC'S system correctl y interprets num- tion) events. Copies of these fi jes should not be bers and capital letters, but it in terprets small sent to ILOC or Stockbauer. Like Stockbauer, nei- letters as Japanese Katakana characters that have no ther Stam nor I can read B-inch diskettes. relation to what you typed. Hence, any small letter 94 on the written form must be capitalized in the ma- specify the column numbers, to be read vertically, chine-readable file. A copy of part of the corre- only to serve as a guide for specifying the columns sponding hand-written form is shown in Figure 2. for the data to be typed. You can include these lines in the file as you prepare it, but should de- The first two lines and the last two lines of Fig. 1 lete them from the copy that you send to ILOC and/or IOTA. By "IOTA," we mean here graze reports sent to

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and me. The rest of the data are arranged in the heading should contain "PLACE NAME" in columns l-lO five groups described below. The groups can and the name of the place of observation in columns 16 to be separated with blank lines, but these are 80. "ADDRESS" is in columns 1-7 and the address of the not required. report preparer ("representative"; your address, not IOTA'S address Or the address of the place of observation) 1. Heading Information. The first line of is in columns 16 to 80 of the second line. "REPRESENTA- TIVE" is in columns 1-4 and the name of the representative Fig. 28 (observer's name, or name of the graze expedition leader) is in columns 16 to 50 of the third line. "FORMS RE- « Bd r- QUIRED" is in columns 51 to 64 of the third line, "YES" or ~ - ^ ~ 4 "NO" in columns 71 to 73. "REPORTED TO" is typed in col- I . f I I I g umns 1 to 11 and the names of organizations (ILOC, IOTA, $ I — I , I I S any others) to which a copy of the report is sent should . ·4.qA ) SI I I - .J be given in columns 16 to 80 of the fourth (last lunar I t S , 0 header) line. For occultations by objects other than the :8 DJ h^ Moon, type a fifth header line with "OBJECT" in columns ·0 : 3 1-6 and the object's name starting in column 16. For as- q m\ _ » teroids, give the asteroid's number in columns 16-19 (I %0 (right-justified; leave blank for unnumbered asteroids) ~ and its name or designation starting in column 21. %02 -" t E !" 8 I - E 21 i & 2. Telescopes and Positions. These are the telescope ._ I')) I 0 ] t"t" " CJ specifications and geographical coordinates given in the " V 0 Se £:ElC ,I 4 i lower part of the heading of the front of the written U O b - O °c! ' I form. These lines do not need to be specified if ILOC has Kb i DJ u Zh 4.0 assigned you a Station/Tel/Obs code. All numbers in the ·d dC format below are right-justified: UJ El 1 I I I Description |j ill I I O Cm Yj Col umn 1 Always the letter "T"

I 0 Identifying letter, start with "A", a capital let- I I 2 2 I I ter corresponding to the small letters used in I I I I the heading and the "T" column of the written )i|!! I f I P d form. On the written form, spaces for only 3 I I Ch 6 I te1escope/positions are given, but in the ma- I I >1 X chine-readable file, you can use A through Z for ik4±". on up to 26 telescope/positions in a file. Use two 'V or more files if there are more than 26 tele- 3UUC qj >bO O scopes used in an expedition. ~0 =µµ E 5 Telescope type I I R = refractor I)!I b i 2~ ? N = Newtonian reflector :si I C = Cassegrain reflector, including Schmidt-Cass. & D I & CW 0 = Other, describe on a second line with the ·C "P" m VI t I VI same letters in col. 1 and 2, columns 3-5 G,b I 'A ENS Em E b-q % r- blank, and the description in col. 6-80. >: 1 = % a 6 Telescope mounting m + k1 q I E = equatorial I I X I I A = alt-azimuth m t 7 ,0 D Telescope drive g|iiU >4 % · O U Ell O © bo ·C D = clock-driven 3 u E 4) Cl 4 9-13 vi 4J ·t I M = manual 4D cn V) 0 0 E C W .Cl I q Telescope aperture in centimeters, to .I cm. Col- O m O ·Q I rd CI ry 3=j t ¢ ums 12 and 13 can be blank if the aperture is 0 I UJ I I given to the nearest cm. I I II " 15-20 Telescope focal length, in centimeters, to .1 cm. b II % I II Colums 19 and 20 can be blank if the focal II f (I K length is given to the nearest cm. Degrees of longitude from Greenwich. zl I . : 23-25 G m O M minutes'of arc of longitude wq 0 . g 27-28 Zl i &' U seconds of arc of longitude (hundredths of an arc W DJ dj Op - * 30-34 >' ' 00~ > " Q6 second can be specified, but tenths, as given in I (I1 !2 X ~ S Fig. 1 with col. 34 blank, are sufficient; the .jj 1 4J U :Z value needs to be accurate to I arc second or I ¶J 0 better). Zl Longitude East or West of Greenwich. Degrees of"1atitudC. f " i I!-:: minutes of arc of latitude. I 'ji ai 45-49 D seconds of arc of latitude. : g ~ Al C"b ,, &t !:-58 Latitude North or South of the equator. ¢5 © Height abOve sea 1Cvei, in meters, to 0.1; should 96

be accurate to ± 30 meters or better. 'Live data must be specified on every line. The eas- 59-70 Name Or abbreviation of geodetic datum, or iest procedure is to type the data on the first other type, of coordinates. line. Then, use your word processor to copy this ' 7]-75 ILOC station code, if known. line several times, as many as are needed for all of 76-80 ILOC telescope code, if known. the timings to be included in the file. Then, you just need to correct the data that change from line 3. observers and Recorders. These are the names of to line. observers and assistants that are given at the top of the back of the written forms. These lines do For coments, which can be specified on the back of not need to be specified if ILOC has assigned Sta- the written form, type a second line wIth columns tion/Tel/Obs/Rec codes for the observer-recorder- 1-4 blank. Type the comnent (remember to use all station-telescope combinations in question. The capital letters) in columns 5-80. The time station format is given below: call letters requested on IOTA'S written form should be specified here only if they are different from Column I: Always the letter "0." those specified in the second footing line described Column 2: Identifying letter, start with "A," a at the end, and should be given as a coment only capital letter corresponding to the for the first timing period. IOTA is no longer ask- small letters used on the written form. ing for the eyepiece power on the machine-readable On the written form, spaces for only 6 files sent to them. names are given, but in the machine- readable form, you can use A through Z 5. Footing Data. This consists of two lines, which """ for up to 26 observers and assistants should be included in copies of any files sent to in a file. Use two or more files if IOTA. ILOC does not use them, so they do not need there are more than 26 observers and to be included in the copies that you send to Tokyo. assistants in the expedition. Columns 5-30: The observer or recorder's (assis- The format of the first footing (map) line corre- tant's) name. sponds to the data at the bottom of the front of Columns 33-37: ILOC station code, if known. IOTA'S form for reporting occultations, and has the Columns 38-41: ILOC observer code, if known. following format: Columns 43-47: Estimated accuracy of latitude, in arc seconds. Column Description

4. Timings. This is normally the largest group, 1 Always the letter "M." including all of the event timings, given in the ta- 2 Blank if the positions for all stations were ble of the written form. Sequential numbers of the measured from the same map, in which case, events are given in colums 1 and 2 (integers, you need only one map line. Otherwise, the right-justified), corresponding to the numbers Telescope/Position letter (same as the let- printed on the left side of IL0C!S form for written ter in col. 2 of the Telescope/Position timings. You are not limited to 20 lines, as on the line) must be specified here, and you need written fom; you can include up to 99 timings in to have as many map lines as there are Tel- one machine-readable file. Use 2 or more files to escope/Position lines. report 100 or more timings. For the data in columns 4-34 Name or number of map from which the posi- I to 53 of the written form (column numbers given at tions were measured. the top of the table), add 4 to the written-form 36-39 Year of publication of the map. column number to obtain the corresponding column in 41-51 Scale of map, left-justified, such as the machine-readable file. Sq in the machine-reada- "1:24,000" or "1:50,000." """ ble file, the year is in colums 5 and 6, and the 53-80 Map publisher, such as "U.S.G.S." temperature is in columns 56 and 57. Column 73 (G, grazing occultation) of the written form is typed in. The format of the second footing (graze sumary) column 60 of the machine-readable file, and columns line corresponds to the data at the bottom of the SI, S2, and S3 of the written form are typed in col- back of IOTA'S form for reporting grazing occulta- umns 78, 79, and 80, respectively, of the machine- tions. It should not be included in any report that readable file. From the back of the written form, is not a lunar grazing occultation. The graze line the optional columns 56 (other phenomenon) and 57 has the following format: (lunar limb, D/B/U for dark/bright(sun7'it)/umbra during lunar eclipse) should be typed in columns 58 Column Description and 59, respectively, in the machine-readable file. The data to be entered in these columns are ex- 1 Always the letter "G." plained adequately in ILOC'S Guide to Lunar Occulta- 3- 7Predicted position angle of central graze, tion Observations. Remember that either Stationl to 0.1 degree. Tel/Obs codes (columns 28-36 of the machine-readable 9-12 Magnitude of star, to 0.1 magnitude. file) or T/O letters (in columns 78 and 79) must be 14-16 Percent of Moon sunlit. specified, not both. If the codes are unknown, (as 17 "+" for lunar waxing phase, "-" for waning is the case for all new stations, especially tempor- phase, "E" for lunar eclipse. ary sites for grazes), you need to specify the T/O 19-21 Cusp angle of central graze; letters, and the corresponding Telescope/Position umbral distance during lunar eclipse. and Observer/Recorder lines. 22 "N" for cusp angle measured from the north- ern cusp, "S" if it is measured from the In the written reports, repetitive data in some col- southern cusp, and "U" to indicate umbra) umns could be specified on the first line, and omit- distance during lunar eclipse. ted from the following lines, as specified in ILOC'S 24-26 Total number of stations in the graze expe- Guide. But in the machine-readable files, repeti- dition that obtained non-redundant data, 97

not just the number of stations in the file hand (odd-numbered) pages give declination, in a (in case there are more than 26 stations in format similar to Robertson's Z.C. But Sato's data the expedition). are for the new equinox J2000, rather than the 1950 27-30 Total number of contact timings made during equinox used by Robertson. Since Sato's catalog is the expedition, counting 1 for certainty arranged in order of equinox 2000 right ascension, code I (certain) events, js for certainty while Robertson's catalog was in 1950 R.A. order, code 2 (probable but not certain) events, the Z.C. numbers are in approximate, but not exact, and zero for certainty 3 (possible, but numerical order. Consequently, LG. 544 is listed probably spurious) events. It is not just before Z.C. 543 by Sato. In addition, Sato includes the number of timings in the file (in case ecliptic longitudes and latitudes, as well as SAD there are more than 99 timings in the expe- and AGK3 numbers. Sato's basic data are Robert- dition). son's, and he has reproduced one of Robertson's er- 32 Maximum sky steadiness (coIum 53 of timing rors that we discovered during the last series of line in machine-readable file, or col. 49 PIeiades occultations. Both catalogs incorrectly of written form) of all contacts (or of give the magnitude of Z.C. 549 (24 Tauri) as 8.1, central graze in the case of only one sta- when it is actually 6.3. Robertson apparently con- tion having a miss) in the expedition. fused this star, near Alcyone, with two nearby 8th- 34-36 Minimum te?escope aperture, in centimeters, magnitude non-Z.C. stars when he got its magnitude. reporting any contacts with the maximum sky steadiness given in column 32. An entry under the last (N) column in Fig. 2 indi- " 38 "C" if the graze is in the "Cassini" region, cates a note (usually D for double), showing that that is, if most contacts during the graze more data about the star are given in an auxiliary occurred in regions of the ACLPPP predicted table following the main table. The auxiliary table lunar profile defined by 2's, 3's, 4's, or gives proper names, Aitken double star (ADS) numbers, 7's. component magnitudes, separations, and position an- 39-41 Observed shift from the current ACLPPP pre- gles, periods of doubles with orbits, variable star diction, in arc seconds, to 0.1. information, and a reference to the source of the 42 "N" if the observed shadow was north of the additional data. Information on doubles discovered predicted shadow, and "S" if it was south from photoelectric occultation observations that of the predicted shadow (that is, the di- have been published during the last several years is rection of the shift, which is always mea- included. Part of the auxiliary data table is re- sured perpendicular to the predicted lim- produced in Fig. 3. Following this table are tables it). Leave this colum blank if no shift of zodiacal clusters, nebulae, galaxies, radio (0.0 shift) was observed. sources, and x-ray sources. 44-46 Watts angle of center of observed events on the ACLPPP profile, to the nearest degree. Following the tables are charts showing all of the It is the Watts angle of central graze if stars and other objects given in the tables. The the observations are symetric on the pro- charts are plotted with J2000 ecliptic coordinates; file, which is usually the case with dark- the chart showing the Pleiades, Hyades, and Aldebar- limb grazes far from the cusp. an is reproduced in Fig. 4. Sato's catalog can best 48-50 Predicted latitude 1ibration of the graze. be used with the new catalogs on equinox 2000, such It is given to the nearest 0.1 degree, but as those by. hL Tirion. If you have only the old the decimal is not typed, its location be- equinox 1950 catalogs, you can use Sato's charts, Ing understood to be between columns 49 and and the ecliptic coordinates in his tables, to use 50. star patterns to find objects on the old chart. " 52-60 Time station call letters, left-justified, for the time station of ultimate reference In an introductory section and in appendices, Sato (for example, give "\A\dV" and note in the shows how to compute apparent positions, lunar connents a local AM station, if the latter. eclipses, total and grazing occultations, and other madewas usedelsewherewith a tomasterobtaintapetheincludintimings?. W\AV information. Although the explanations are in japa- nese, some readers familiar with such calculations from sources such as the Explanatory Supplement to ZODIACAL CATALOG J2000 PRINTED IN JAPAN the Astronomical Ephemeris and Meeus' Astronomical Tables will probably be able to follow many of the David Id. Dunham fomulae Sato gives in these sections.

j. Robertson's Zodiacal Catalog was published by the Sato used a computer to produce the data for his U. S. Naval Observatory in 1939, but it has been out catalog, and it is available on floppy diskette for of print for the last several years. Last year, MS-DOS systems, along with software to perform the Isao Sato, a member of the Lunar Occultation Observ- calculations explained in his introduction and ap- ers Group in japan, republished the Z.C. after con- pendices. In addition, he has programs to simulate ' verting Robertson's data to the equinox J2000, but total and grazing occultations using special data- has added much new data, especially about double sets for events visible from japan. But Sato uses a stars, which makes the catalog more useful for mod- Japanese version of KS-DOS that utilizes japanese ern users. When I was in Japan in May, I bought 40 characters even in the diskette directories, so I copies of Sato's Z.C., so that I can sell them to was unable to read them with American P.C.'S. We readers who want them (see end of this article). have sent Sato an English version of MS-DOS, which he said he will use to produce versions of his data Parts of two pages of Sato's catalog, covering part and software that we can use on our machines and can of the Pleiades, are reproduced in Ficjs. 1 and 2. be distributed to other readers who may be interest- The left-hand (even-numbered) pages of the catalog ed. When I complete updating the USNO XZ catalog give right ascension information, while the right- (see p. 104), I will send a copy to Sato, which he ZC BD No. s tar Max R. Abc. ill mean ZC Dec. u ' mean longitude latitude sp. SAD ACX3 N 40 No. CD No. n am e mag (J2000. D) (s/lOOy) epoch No. (J2000. D) ("/100y) cpKjGfj (J2000. D) type No. No. m hmS ' ' " . 533 "19" 582 14 Tau E3. 34 3 43 47.227 +0.833 !901.8 533 ·19 39 54.82 -4. 92 1891.5 58. 178552" -0.091041 GS 93588 "19' 289 D 534 "20' 621 2?H. I Tau 6. 03 3 44 28.203 ·0.183 1905.2 534 ·20 55 42. 76 -I. 99 1898. 4 58.613487 ·1.105085 B9 78121 "20' 335 D 535 "27" 556 8. 71 3 44 37.235 -0.302 1914.9 535 '27 53 50.76 -7.65 1914.5 60. 203058 ·7. 891720 FO 78122 '27" 370 D 538 "23' SOS lf Tau 5. 43 3 44 48.197 ·0.11[ 1899.3 538 '24 17 22.27 -4. 39 1890.5 59. 434978 '4. 385292 BS 76128 ·24' 328 537 "23' 507 Tau 3. 81 3 44 52.538 +0.145 1900.8 537 "24 6 48. 38 -4. 29 1895. 9 59. 411940 '4. !89937 BSp 78131 ·23' 302 D?

538 '24' 546 18 Tau S. 83 3 45 9.881 '0.084 1903.6 538 '24 SO 21.09 -4. 92 1894. I 59. 638909 '4. 883228 B8 78137 "24' 328 D 539 "24" 547 19 qTau 4. 37 3 45 12.527 ·0.172 1898.5 539 "24 28 2. 33 -4. 33 1888.5 59. 564818 '4.518198 B5 76140 '24' 329 D 540 "22' 544 8. I 3 45 39.934 "0.177 1911.8 540 '22 41 41. 39 -3.08 1912.6 59. 274896 '2. 788357 AO 76154 "22' 343 541 "23' S 16 20 Tau 4. 02 3 45 49.581 '0.128 1899.0 541 '24 22 3.47 -4. 91 1889.4 59. 680252 +4. 389921 B5 78155 '24" 335 542 "24" 553 21 Tau S. 85 3 45 54.429 ·0.101 1898.4 542 '24 33 16.07 -5.03 1884. 2 59.739550 '4.568106 B8 78159 '24' 336

544 "18' 537 8. 4 3 48 1.186 '0.183 1911.5 544 '18 34 0.81 -0.41 1910.4 58. 447984 -I. 278864 B8 93587 +18' 288 543 "24" 558 22 Tau 6. 48 3 46 2.930 '0.164 1905.8 543 '24 31 40.65 -4. 41 1896. 3 59. 765222 '4.535154 B9 78164 '24' 337 D 545 "23" 522 13 Tau 4. 25 3 48 19.586 '0.148 1897.1 545 "23 56 54.10 -4. 47 1889. B 59. 699330 '3. 955828 BS 76172 '23' 309 547 "13' 594 6. 80 3 46 26.289 '0.191 1911.1 547 "13 30 32.29 -2.74 1909.5 57. 4320[5 -6. 235171 AO 93590 +13" 297 546 "23' 523 6. 98 3 46 27. 263 "0.130 1914.9 546 '24 IS 18.21 -4.54 1910.6 59. 795398 '4. 248831 AO 76173 '24' 340

548 "24" 582 El. 88 3 46 59.381 "0.137 1916.1 548 '24 31 12.30 -4. 77 1906. 9 59.972912 '4. 480504 B9 76183 "24' 341 D 550 "23' 537 6. 82 3 47 20. 951 "0. 103 1923. 8 550 "23 48 13.44 -2. 97 1922. 9 59. 898267 ·3.763540 AO 76193 '23' 321 549 "23" 538 2( Tau 8. I 3 47 21.030 "0.135 1891.4 549 ·24 6 58. 85 -4. 31 1883. 2 59.964905 ·4.068583 AO 76192 "23" 320 551 "23' 538 7. 10 3 47 24.373 '0.074 1913.4 551 "23 54 53.01 -3. 84 1895. I 59. 933278 '3. 869018 B9 76197 D 552 "23" 541 25 n Tau 2. 96 3 47 29. 083 '0. 145 1900. 0 552 '24 6 18.37 -4.59 1894.6 59. 992411 "4. 050912 BSp 76199 D

Figure 1. Part of p. 30 of the main part of Sato's Figure 2. Part of p. 31 of Sato's catalog, giving catalog, giving right ascension information. declination information.

80" 75" 70" 65" 60"

'8" I 00 I ID II I I I , II I t I I ' I :I I I I ·8" 0 +

+ 0 + 0

" p 0 + +

0 0 " 0 P P O. 0 + I 0 2 0"4" -" ." ." -" · .". ·- · .P - +4' 3 0 0 0 P 0 + ~ " D " + P + 4 0 + 0 + + ' ·

ZC BD No. star Dooe N DATA S ·+ + 0 0 00 + · + P + _ B "· O . + - < ,, 0 + 533 ·19' 582 ]4 Tau D 7 · 0' 0 0 0' 534 '20' 621 ~" p . , 221Ll Tau D 8 " + 0 0 0 , 535 "27' 556 D ADm3s 6-6 d·ll7" P·43' (1920) - 0, . + + · + a " , . 538 '23" SOS 16 Tau Celm 9 · D 537 +23° 507 ~ 17 Tau D? Electra DBL -0- 0 ' 0 00 O ~ " + , , , + 0 m X, 0 0 538 '24' 546 VAR O . ' O + " ·' I! qTau D Tamta6.4-6.4 d-0.05'4.4-9 d·69'(1974)P·330° 0 . 0 + 0 0O + 0 + 539 '24" 547 NEB O -4" , + O+ "4" . . + . 0 0 54! +23' SIB 20 Tau ki8 0 p + + 542 '24" 553 RAD O 0 0 0 0 21 Tau A8tcixjpe " " D ' +1 " 0 543 '24° 556 22 Tau D 7.3-7.3 d-o.r p-80" (19u) Xry x 0 " " 0 " m " QO " , ¢' - ~- ", , ~ 0 545 '23" m 23 Tau Ikmpe 0 0 , D + 0 + 0 0 0 548 +24' 562 D 6.8-9.8 d·0.299" p·m' (!971) 0 0 D 0 + 0+ 0 551 '23" 538 D ADG1781 7-9 d·6.1' P·265' (1952) -8" I I II I t I I I I d6 I I I I h I |'1 -8' 552 '23" 541 25 n Tau D Alcm 3.0-4.6 d·0.031' P·207' (1971) 556 '22' 563 1048. Tau D 5.7-7.7 d·0.05' (1974) 80" 75' 70" 85" 60"

Figure 3. Part of p. 132 of Sato's catalog, Figure 4. Ecliptic-coordinate map showing the including part of the table of auxiliary data. PIeiades and Hyades, from p. 152 of Sato's catalog. 99 will use to extract the best current data for the from the American Embassy in Tokyo to USNO, and some Z.C. stars for his database. were damaged in transit (mostly, frayed and soiled edges). Although none of the information in these Sato sells his catalog for 2000 yen. Unfortunately, copies was destroyed or made illegible, I am selling I was in Japan when the do11ar/yen conversion was 6 lightly damaged copies for $13.50, and 3 moderate- the most unfavorable for Americans for many years, ly damaged copies for $10.00. I will probably re- so I need to sell my copies for $14.70. I bought turn to Japan in October, and can then buy some more them, not IOTA, so checks should be payable to me in copies from Sato, if my current supply is sold out American currency. Several of my copies were sent or runs low. He still has about 200 more copies.

THE SEPTEMBER 13TH PLEIADES PASSAGE with o.n. 4 (3) late last year., This time, there should be more time to request special predictions, David W. Dunham such as for detailed USNO total occultation predic- tions for planned graze expedition sites. For such The last issue was devoted to the Pleiades, with a requests, send approximate coordinates to me at P.0. major article starting on p. 58. Readers are refer- Box 7488; Silver Spring, MD 20907; phone 301,585- red to that article for general information about 0989. During the September 13th passage, the Moon the current series of passages, especially the sec- will be slightly gibbous, 61% sunlit. Those with 8- tions on value, predictions, observing considera- inch (and perhaps 6-inch) telescopes will probably tions, Pleiades charts, and double stars. Pleiades still be able to time occultations of 9th-mag. stars passages occur each month, and a list of this year's if conditions are good, but a USNO observability (D) passages was published on p. 69 of last January's code of 2 is needed to ensure all of these events issue of Sky and Telescope. But o.n. readers can will be predicted at this phase (the O-code calcula- learn about passages visible in their area by exam- tions penalize moderate gibbous phases more than ining the Alcyone (Z.C. 552) graze paths in the they should). So if you have USNO predictions, you Grazing Occultation Supplement that was distributed should check your O-code limit to see if you might

m .Cl tC,j e ' "Z ?,' - "d_ D '< ,,i m

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V? e " C) " . :" @@ D el) " ° " erjn m 0 0 0 £ +a EJ ) · ~4nm" " · " " :" F) "/ : m ! CJ o m 42 2e) D °r,) LC) Lil) ® "d_ 'o " 7 C'J % C"J W ' c\i+ + -I- 100 need a lower limit for this passage. If you rely on on p. 61 of the last issue, and described on pages Walter Morgan's total occultation predictions using 59-61. The scale of the chart has been modified the a and b factors, they are limited to an O-code slightly so that the Moon figure on p. 60 of the of 6, which includes stars only down to about mag. last issue can be used. During the September 13th 7.6 at the 61% sunlit phase of this passage. passage, the Moon's apparent radius will be 15:37 when its altitude is 20° above the horizon. For or- Grazing Occultation Expeditions. Please send or ienting the Moon figure, the position angle of the phone me information about any graze expeditions lunar north pole (0° on left side of the figure) planned in your area, so that I can put this infor- will be 348° The position angle of the north cusp will be 346°'(the same as in March) and the center mation on the IOTA occultation line telephone mes- sage center, 301,495-9062. Sky and Telescope will of the sunlit limb will be at 76°. publish an article about the passage in their Sep- tember issue, and will give this number as a source The Moon will pass centrally across the cluster for of more information. There will probably be expedi- observers in northern South America, as shown by the tions for grazes of Alcyone near Houston, TX; in path for Caracas. The circled A shows the Moon's northern AL; central KV; near Pittsburgh, PA; and center at moonrise, while a circled S terminates a near Montreal, Que. Other probable expeditions will path at sunrise. The passage will end near sunrise be north of Detroit for Merope and north of Washing- for western Europeans; the paths for Rome; Hannover, ton, DC for 24 Tauri. I need to have information to German Federal Republic; and Tromso, Norway are es- contact expedition leaders for these, and other pecially short. The path for St. john's, Newfound- planned, graze expeditions to include on the IOTA land lies close to that for Miami, FI. W , ,_ occultation line, which you are also encouraged to call for information about plans in your area. Graze Predictions. The northern limits for the qc- cultations of Merope (23 Tauri), Alcyone (Eta Tau- Results from the March Passage. As far as I know, a ri), Pleione (27 Tauri), and Atlas (28 Tauri) are large Pacific storm prevented any observations from shown on the map on p. 68 of the january issue of being made anywhere west of the Rocky Mountains dur- Sky and Telescope. Shifts expected for the three ing last March's favorable passage. But many ob- brightest stars are noted above. The limits for servers in the central and eastern U.S.A. were quite three other Pleiades grazes of sixth-magnitude stars successful, in spite of the poorer geometry for are shown in the RASC Observer's Handbook. But them. I trave11ed to Tyrone, CO, east of the Sand eight grazes of Pleiades stars, as long as other Dunes National Monument, since clouds from the ap- favorable grazes during September, are shown in the proaching storm threatened the latter area. Near map, and accompanying table, of the northeastern Tyrone, I tried to videorecord the Merope (Z.C. 545) graze, but failed when the camera came loose while 1987 GRAZES. attempting a minor adjustment just before the graze began. I succeeded with Atlas (Z.C. 560) near [5 " J Hoehne, 15 miles down the road, 1.5 hours later, and ,1 'Kj' experienced a 0!'25 south shift, close to what was ¶ expected (see p. 89 of the last issue). But a zero shift occurred for Paul Maley's large expedition r south of Corpus Christi for the Alcyone (Z.C. 552) « graze, videorecorded from a few of the stations. « Although I failed for Merope, Benny Roberts succeed- : G . '9 ?g ·1' , ed and had a O:'i north shift, as noted in the table T b « on p. 103. It is clear that the expected 0!'25 south ] , gb shift is not universal, with the bright stars so far " _ 0 T averaging closer to zero. Errors of the proper mo- U tions in Eichhorn's catalog, now over 30 years old, D seem to be accumulating, so that we will need to ' E 75 ¢b keep track of the observed shifts for individual stdrs to get very accurate (to O':i) predictions for " \b' future grazes of Pleiads. A new survey like Eich- horn's would be useful for further refinement of the cluster positions. pleiades Chart. The apparent-place chart of the 1iu%\gz :_m. Pleiades, showing topocentric paths of the Moon's center for several cities, is similar to the chart LONGITUDE yo, YE.A.R Eq DAY USNO SAD E WAG 7.SKL .L HN.T, LOXG I,AF SXAR, KANE KAGI 11AG2 SV u

14 1987 SEP 1 233U 18U262 7.5 U9+ S1k3371 -78" 37" IS 1987 SEP 2 2496 185278 6.8 60+ S2 58.8 -78 37 17 1987 SEP ¶2 435 75662 5.8 76- X6 U6.7 -76 uo 117 ARIETIS 19 1987 SEP 13 sus 76172 U.2 67- Xu 3.0 -83 uu 11erope (23 tauri) 91 1987 SEP 13 X U895 76188 8.3 67- Xu 23.0 -75 39 92 1987 SEP 13 X U899 76191 8.2 67- Xu 2U.7 -75 39 20 1987 SEP 13 5U9 76192U 6.3 67- X u 24.0 -77 uo 24 TAURt 7.1 8.2 0"01 205" 21 1987 SEP 13 552 76199K 3.0 67- X u 28.9 -80 41 ALCYOXE (ETA TAURI) 3.0 u.6 0:03 207 22 1987 SEP 13 562 76236X 6.6 67- X 5 30.2 -74 38 7.u 7.4 0.1 90 23 1987 SEP 13 X 4981 762U9 7.3 67- X5 U6.9 -81 U2 24 1987 SEP 13 X U995 76259 7.3 66- X6 5.9 -75 39 25 1987 SEP 15 X 7352 77397 8.0 U7- X6 39.2 -77 uo 26 1987 SEP 16 X 9379 7853ort 8.0 37- K6 19.5 -78 'to 8.5 9.0 0.30 19 27 1987 SEP 16 1022 78593K 5.8 37- K 8 19.6 -83 uu su aurigae 6.0 7.8 0.90 36 29 1987 SEP 18 X12718 80165 7.3 19- X 8 35.9 -78 U1 30 1987 SEP 30 X2UU82 186186 7.6 45+ S0 39.6 -80 U1 101

U.S.A., which is favored during this passage. The manpower to produce reduction pPofiles of observed favorable graze of 6.3-mag. Z C. 549 (24 Tauri) is grazes, as was done by HMNAO, so IOTA'S efforts in not included in the RASC Handbook map, since it is this direction are important. based on the Zodiacal Catalog, which incorrectly lists it at 8th mag., fainter than the 7.5-mag. lim- Mitsuru SOma was especially helpful during my vis- it for their map. Z.C. 549 is incorrectly listed as its, leading me through the intricacies of the Tokyo a variable star, wIth mag. at minimum = 8.1, in train system to get to various destinations on time. USNO's XZ catalog. Messages about the bogus varia- In November, we visited the Tokyo Astronomical Ob- bility are consequently given in USNO'S total occul- servatory, where I gave a presentation about IOTA'S tation predictions; Morgan's, Bode's, and Fabrin's work. SOma gave us a comprehensive tour of the pho- predictions based on them; and in IOTA'S graze pre- toelectric meridian telescope, where he works. dictions. The 8.1-mag. minimum was put in the XZ due to the Z.C. error, but it is wrong, and\ the cor- In March, I timed my arrival in Tokyo to be nearly rect, constant magnitude of the star is 6.3. half a day before a graze of Spica in Okinawa, which I hoped to videorecord. Toshio Hirose met me at Na- The northern limits of Electra, Taygeta, and Maia rita Airport, but I noticed that clouds thickened as are shown in western Europe in the o.n. Eastern Hem- my flight approached japan. Hirose drove me to Ha- isphere grazing occultation supplement. Notice that neda Airport, where I was to catch a flight to Okin- the northern limit for Taygeta intersects the south- awa to join SOma and many other members of the main- ern limit for Alcyone (with graze near sunrise, and ly amateur Lunar Occultation Observer Group (LOOG), 'b~. on the bright limb) in southern Spain, a good place japan's version of IOTA. But heavy rain accompanied to be. our arrival at Haneda, and a phone check of the weather forecast was discouraging. So I decided not ILOC/LOOG NEWS to fly to Okinawa, which is not such an interesting place to visit when it is raining. SOma later re- David W. Dunham ported that 33 stations were set up for the Spica graze, the largest effort to date for any graze in My business trips to Japan last November and March Japan, but he also confirmed the forecast; it rained were briefly noted in previous issues. In May, Iat central graze time. needed to make even a third business trip to japan. Altogether, I made six week-long business trips, We had better luck for the March 20th graze of 5.1- four of them overseas, during the first half of mag. Z.C. 2298 near Mito, about 100 km northeast of 1987. This unusual activity in my job made it very Tokyo. Brian Marsden had recently arrived in Tokyo, difficult to keep up with even the most essential and we were both treated to a special dinner honor- occultation work, and I have not had time to answer ing those for whom asteroids had been named, in a many letters received during the past several rooftop restaurant overlooking the grounds of the months. But the distant journeys gave me opportuni- Imperial Palace, the evening before the graze. ties to meet many foreign occultation observers and Prof. Tomita drove me to Mito, where a 20-cm have long discussions with them. The trips to japan Schmidt-Cass. telescope was set up for use with my have been most rewarding, and have resulted in two video equipment. All but one of the 15 stations other important articles in this issue, on reporting succeeded in timing the graze; Hirose's reduction occultation timings in machine-readable form (see p. profile is reproduced here. It was Tomita's first 92 ) and on a newly published Zodiacal Catalog (see graze observation. I obtained the first videore- P. 97 ). Other aspects of these trips are described cording of a graze in Japan, but there was a north below. shift. The star was occulted twice in only 14 sec- onds at my site, making it the shortest videotaped During each of the trips, I was able to spend at lunar occultation, from first D to last R, as far as least half a day at the Geodesy and Geophysics Divi- I know. When we met after the graze, a tape record- sion of the Hydrographic Department, which includes er was passed around as each observer gave his or the International Lunar Occu1tation Centre (ILOC). ' her impressions (number of events, special circum- In March, I gave a presentation there about observ- stances, any difficulties, etc.) of the graze. ing occultations and grazes with video equipment. Graze expedition leaders in other countries may want Members of the division described their work with to adopt this practice. solar eclipses, and gave me a manuscript'of an arti- cle analyzing their photoelectric observations of a jnomn lWb CV lunar occu1tation of Vesta. We also discussed some 3."0 - CR. OBS. ZC 2298 of the items discussed by D. Biittner in o.n. 4 (2), p. 35. Concerning item 4, I gave ILOC a copy of my double star files on magnetic tape, also including a 2. 0 " zodiacal subset of comprehensive double star data maintained at USNO. But as of May, they did not r :% have time to work with the numerous inhomogeneous I, 0 " ' ' ' r, · Q , .· . datasets; Don Stockbauer's work described on p. 104 " ' ...... " "' ~~^ should help get this underway. Concerning item 9, ILOC stressed that they want to collect grazing oc- 0. 0 " cultation observations, but confirmed that they were not very useful for their main task of determining Delta-T (Dynamical Time - Universal Time) from all -I. 0 _ reported timings. Their support for grazes is de- monstrated by their continued production of graze

maps for various publications, such as the annual "1'?or 102 b;3 104 IDS 1% 107 m m 200 ?01 RASC Observer's Handbook. But they do not have the Paa1t1am ^rmgle From F'alor Axzb 102

The chart of the graze of Z.C. 2298 observed in tation observations (station number SN 211) which March near Mito City, Japan, was provided by Toshio arrived earlier this year, and the Report of Lunar Hirose. Occultation Observations for 1984, which was re- ceived last week. After only a few hours of sleep following the graze, Tomita met me again, so that we could travel with There are some discrepancies between the two which I Brian Marsden on the bullet train to Shizuoka, 200 wish to discuss. I will refer to the individual re- km southwest of Tokyo, to attend the 17th annual ductions as reduction R1 and the report reductions meeting of japanese comet observers. At Shizuoka, as R2. Also, I do carry out reductions for the Oc- we were met by the mayor and other local dignitar- cultation Section of the Royal Astronomical Society ies. In the afternoon, under a banner proclaiming of New Zealand; the reductions I produced for my own "Welcome Dr. Marsden," Brian gave a talk on comet 1984 observations I will refer to as R3. orbit determination. The next morning, I gave a brief talk emphasizing the astrometric and observa- I have made fairly detailed comparisons of the fol- tional contributions that attendees could make lowing items: towards asteroidal occultations. Both Marsden's and my talks were translated, and I learned later that (a) Residual distances including limb correction, brief parts of both were shown on the noon news on O-C. national television! Later that day, I was given (b) Watts' limb corrections, or vertical profile of the opportunity to play parts of njy occultation vid- the lunar limb, (Hid in Rl, WH in R2). eotape of various grazes (including the one at Mito) (C) Simple residues, that is, without limb correct- on a large-screen monitor. There were about 200 in tion, calculated for ILOC reductions by adding the room at the time; it remains the largest and the limb profile value to O-C. most enthusiastic audience that I have had for my (d) Position angles of events (KM in R1, K in R2). video presentations. Overall, I was very impressed at the high level of accomplishments by the Japanese I. Differences Arising from a Possible Discrepancy amateurs at the meeting. Besides discovering numer- in Declination. ous comets, many of them routinely take and measure astrometric plates. Several of them have computer The individual reductions, R1, were received before programs to calculate orbits, including three with the report, R2, so I made fairly detailed compari- numerical integration programs to take into account sons of R1 with the reductions (R3) I had carried planetary perturbations for precise orbit work. out. This showed that all items compared, (a), (b), There is virtually no American amateur counterpart (C), and (d) are in moderate agreement (if the same to this activity, especially in astrometry. But star catalogue has been used). However, detailed this is perhaps balanced by a greater emphasis on comparisons showed that there is a position angle photoelectric and CCD work by American amateurs, (d) difference which is declination-dependent. This mainly on variable stars and some on asteroidal is zero for zero declination, but about O:JS at dec- lightcurves. lination 25° and -0?15 at declination -25° for dis- appearances, in the sense Rl - R3, and similar dif- ' LETTER TO THE EDITOR ferences with opposite signs for reappearances.

Dear Mr. DaBo11, Also, the small differences in the simple residues (C) show a position angle dependence (graphing sug- Having recently received the ILOC Report of Lunar gests the difference is proportional to the sine of Occultation Observations for 1984 after earlier re- the position angle, as might be suspected). ceiving their reductions of my own observations for that year, I have been making comparisons between However, comparisons of R2 with R3 show that these the two, and with the reductions I carry out myself differences no longer exist, and that there are sim- for the RASNZ Occultation Section. This has shown liar differences between R1 and R2 as there are be- , up some discrepancies which are of sufficient magni- " tween R1 and R3. tude to prompt me to write about them to ILOC. I thought the matter might be of interest to IOTA and Both of the differences can be accounted for by as- possibly the menbership, so enclose a copy of my suming that the calculated declinations of the Moon letter to ILOC. are the same for a zero declination, but are up to about 2" farther north in Rl than R2 for extreme Graham Blow has let me have a copy of the 1983 re- northerly declinations and a similar amount farther· port, which I wasn't sent directly by ILOC. Inter- south for extreme southerly declinations. estingly, this also contains discrepancies with the reductions of tqy own observations which ILOC sent 2. Differences in Vertical Limb Profile. me, a\thouyh cjf a dlflerent nature. I have unly made brief mention of them, as I suspect they may As mentioned above, there is fairly close agreement have been picked up already. I did not carry out my in limb profile corrections between R1 and R3, al- own reductions of 1983 observations, so cannot make though it was felt they could have been closer. a comparison in that direction. Differences are generally less than 0!'2 in magni- tude, and frequently less than 0!'1. These may part- Sincerely, Brian Loader ly arise from the position angle differences. Limb corrections for R3 were obtained by manual look-up To the Director, ILOC, in "The Marginal Zone of the Moon," by C. B. Watts, published by the Nautical Almanac Office , U.S.N.O., Reduction of Lunar Occultations 1984 1963.

Thank you for the reductions of njy 1984 lunar occul- However, there are gross discrepancies between the 103 limb corrections used in Rl and R2 (and therefore, would appear to relate at least in part to the R2 and R3). There appears to be no correlation be- change in position angles noted on part 1. tween them at all. As an example, the limb correc- tions given for the first few observations at SN 211 I can see no obvious reason for the large and appar- in 1984 are: ently random differences in the limb correction val- ues between R1 and R2, and wonder if they are in er- Date Star Hid as in R1 KIH as in R2 ror in the Report of Lunar Ckxmltation Observations Jan 9S 146940 0!'84 -0!'04 for 1984. jan 9S 146943 0:'70 0!'02 Jan 9S 146944 0!'82 -O:'OS 1983 Reductions and Report jan 12 S 110328 0!'23 0!'03 Jan 13 S 93179 -0!'53 -0!'49 In 1983, there appears to be close agreement of the jan 13 S 93183 -0'.'68 -0!'95 limb profile corrections between R1 and R2. Howev- jan 16 S 77513 1!'30 1':44 er, the O-C values show considerable differences, as do the values for K-R, the position angle of the As a result, there are considerable differences be- event referred to the direction of the Moon's motion. tween the O-C values (a) in R) and R2 (and also R2 and R3). However, there are only small differences Yours sincerely, B. Loader between the simple residues (C) in R1 and R2. These

GRAZING OCCULTATIONS DateY Star % # # S Ap Sta Tm. S fm, Organizer p # Mag Sn1 .C,A. Location C S'. !!A I! Don Stockbauer 1986 Reports of successful lunar grazing occulta- 0727 0184 6.2 62- 17N Hubbe11, NE 2 6 115 Richard P. Wilds 342 12 tions should be sent to 0728 0290 6.1 53- ION Pleasanton, CA 9 53 2 8 Rick Baldridge 3N349 -1 me at 2846 Mayflower 0803 1093 6.4 5- 20N Bruceville, CA 8 47 2 8 Rick Baldridge )N350-61 Landing; Webster, TX 0827 076493 8.3 49- 16N Redwood City, CA 3 21 1 20 Steve Ba11aron 343-42 77598; U.S.A. Also 0831 1181 6.8 14- 14N Manteca , CA 11 58 2 15 Rick Baldridge 45352-65 sending a copy to ILOC 1030 X17749 )0.0 ]2- 6S Tisvildeleje, Den. I 4 2 31 N. P. Wieth-knudsen 190-22 is greatly appreciated; 1]09 3160 7. 0 52+ 15S King City, CA 4 9 18 Rick Baldridge 55164 66 their address is: In- 1111 3419 4. 5 73+ 12S Willits, CA 2 20 1 20 Rick Baldridge 0165 46 ternational Lunar Occu1- 1112 3535 5. 2 82+ 11S Morgan Hill, CA 6 20 1 20 Rick Baldridge 2N165 32 tation Centre; Geodesy and Geophysics DiVision; 1987 Hydrographic Department; Tsukiji-5, Chuo-ku; 0102- 3175 4.8 11+ us jackson, MS 2131 20 Benny Roberts IS163 58 Tokyo, 104 japan. 0125 2366 1.2 22--18N Baker, CA 2182 20 David Paul Werner 2N 16 61 0204 0232 8. 5 34+ 9S Afton, MN 314115 james H. Fox 170-12 Copies of Pleiades 0210 1105 6.5 91" Dinant, Belgium 1 5 1 20 Yvon Thirionet graze reports should be 0218 1925 1.2 79- 14S St. George, UT 215120 David Paul Werner 0196 20 sent to me and, if pos- 0305 076001 8.5 35+ 3N Tisvildeleje, Den. 1101 31 N. P. blieth-knudsen IN 1-42 sible, ILOC. Reports of 0306 076103 8.1 36+ IN Perronville, MI 1 7 1 20 Homer DaBo11 IS 0-47 Pleiades total occulta- 0306 0545 4.2 37+ 6N Sidon, MS 430115 Benny Roberts IN 4-49 tions need only be sent 0306 0550 6.8 37+ N Concord, NY 1 5 I 15 Adrienne Morris to ILOC if all stars are 0310 1206 5.9 80+ 6N Hundested, Denmark 1 52 6 N. P. Nieth-knudsen 2N 10-60 in the SAD; if any are 0320 2251 7.5 75- 13S Pleasanton, CA 213 220 Rick Ba1dridge 25197 56 not, David Dunham (P.0. 0320 2298 5.1 72- 13S Izumosaki, japan I 22 9Masashi Hiroki 2N196 60 Box 7488; Silver Spring. 0320 2298 5.1 72- 13S 'Mito City, japan 740 27 Hideo Takahashi 2N196 60 MD 20907; U.S.A.) should 0320 2298 5.1 72- 13S Mito City, japan 11 84 1 10 David W. Dunham 2N196 60 also receive a copy. 0405 078042 7.8 39+ 11N Lomita, CA 1 0 1 20 David Paul Werner >15 -66 Many observers send cop- 0501 076841 7.5 9+ N Rio Vista, CA I 0 I 20 Tony Freeman ies of the limit and t profile predictions with their reports; this is al- profile, thus quickly establishing the consistency ways greatly appreciated. and quality of the observations. Residuals can be seen innediately, and the important "overall residu- The shift requested on the report form is defined as al" (the shift value) can be easily measured and re- the shift of the observed shadow from the shadow ported. I have a paper detailing the whole process shown on the original predicted profile. Empirical which I will provide free upon request. corrections as suggested by David Dunham or others should not be applied to the predicted profile be- Some reports have arrived which test the empirical fore calculating the final shift. Please send me a corrections detailed on p. 89 of the last issue. In corrected shift if this was done for any of your ex- the article "Corrections to 80H Grazing Occultation peditions. Predictions," David Dunham suggests that northern- limit profiles should be adjusted 0:'3 south for Several people have asked me to send them the resid- stars at the northernmost declinations, 0!'2 north uals of their grazes. ILOC routinely mails residu- for the southernmost declinations, linearly going to als to the address entered on their form with each no correction at the celestial equator. I general- graze contact treated as a total occultation, but it ized his guidelines, but these rules match his takes quite a while due to their work load. A bet- closely. It seems that shifts for stars in Taurus, ter method is to plot the contacts on the predicted Gemini, Aries, and Cancer have either been close to 104 the 80H predictions or have shown slight (0!'1) north ules of the various computors, the mailing was much shifts. Unfortunately, this affected expedition too late, and many observers received their predic- leaders who positioned stations too deeply into the tions for July - December well after July lst. I shadow during the Pleiades passage on March 6. In apologize for this; don't blame the individual com- my opinion, given the current state of the art, it putors. Perhaps one advantage of the situation is is unrealistic to expect graze predictions to be that we have one consistent prediction system for more accurate than 0!'2, even with trend factors (em- all of 1987. Although the catalog changes will im- pirical corrections) applied. Spacing stations prove the prediction accuracy for many mainly south- closely together has many advantages if all goes ern stars, it is probably not a good idea to change well; those advantages become liabilities if a rou- the prediction basis in the middle of the year. I tine shift occurs. promise to provide more lead time in the future.

If the Moon's observed profile as determined from a The graze data for 1988 were generated at USNO early graze expedition contains an improbable feature, try in July, and will be sent to the computors in early removing all vertical exaggeration from the plot. August. He will send the computors IOTA station da- USNO profiles are typically elongated 30-fo1d verti- ta and address labels early in October, to give them cally, and some expedition leaders even increase more time to make the prediction runs. Some have that in order to show more separation between close- reported that map orders to U.S.G.S. often take more ly spaced stations. If, for example, a tiny out- than a month, so detailed predictions for the first cropping of rock on the observed plot becomes a raz- half of 1988 should be distributed by mid-November. or-thin ledge a hundred feet thick and several miles In any case, you should have 1:250,000-scale maps long, on an undistorted graph, it would probably be covering your region, since careful plots on them best to assign the questionable timings certainty usually suffice for preparation of graze expedi- code 2 ("possibly spurious") as a flag to those ul- tions, although more detailed maps are needed for timately reducing the data. Other types of of anom- reporting accurate coordinates. If you want to alies include large tunnels bored scores of miles change your travel radii or if your address has through the Moon's interior, or long, thin arches of changed, please send a correction to Mr. DaBo11 at lunar rock. Such features must be justified by the address in the masthead as soon as possible. their purported origin and current stability; if they really exist, then future lunar explorers will Corrections to graze predictions. Small corrections behold some truly magnificent scenery. to the current system, the 80H prediction basis ACLPPP profiles, 1986 December version, were recom- I am designing a program which will read the USNO mended for northern-limit grazes on p. 89 of the double star file and automatically provide this in- last issue. The small shifts listed in the table on formation to the graze program. Formerly, graze p. 103 show that there is no strong observational computors had to enter the data by hand; I hope to evidence for my proposed corrections, so for the have it ready for the 1988 predictions. Don Oliver time being, I now propose that no corrections be ap- is designing software to read Thomas Van Flandern's plied, except for observed shifts reported during tape of occultation observations and complete the previous grazes of the same star (see, for example, machine-readable graze list project for the pre-oc- p. 100 for Pleiades stars). I thank observers who cultation Newsletter era. have reported recent graze observations promptly to Stockbauer and me. In particular, I thank Gunther Corrections — in o.n. 3 (13), p. 274, the graze on Neue for his preliminary report of timings of the Feb. 6, 1984 involved Z.C. 106}, not Z.C. 0106. In May 8th graze of the FK4 star Sigma Leonis (Z.C. o.n. 4 (4), p. 63, the shift for SAD 184191 observed 1644) near Dortmund, German Federal Republic, and Sept. 10, 1986 should be 1.15, not 1.65. his reduction profile of the observations, shown "--" here. My analysis showed a north shift of 0'!26; the Thanks for the reports received. Their volume has latitude 1ibration was n:os. Also, Dr. N. P, dropped off quite severely over the past year or . Wieth-knudsen sent a report of his two timings of two, so every one received is more valuable than the graze of Beta Virginis (Z.C. 1712) made in Spain on june 5th. His timings indicated a 0!'17 north ever. shift, at latitude 1ibration -0?79. GRAZE PREDICTIONS AND XZ CATALOG IMPROVEMENTS Z.C. magnitude errors. On june 22nd, Harold Poven- David w. Dunham mire observed a graze of Z.C. 439 = SAD 93221. The catalogs list 8.0 as the magnitude of the FO spec- tral type star, giving the graze a marginal rating. Graze prediction schedule. Most of the grazing oc- cultation predictions for IOTA members for the sec- But Povenmire said the graze was favorable, and es- ond half of 1987 were computed in May, but I pur- timated the star's true magnitude as 7.2. Wayne posely held up the calculations of the limb correc- Warren, at the Astronomical Data Center at Goddard tion data needed to produce the ACLPPP profiles, Space Flight Center, found the star in the French hoping that I could complete my updates to the XZ SIMBAD on-line computer database, which listed an catalog before doing them. At the beginning of article by Eric Craine and Werner Scharlach, "VI June, it became clear that I could not finish the XZ Photometry of Selected SAD Stars," in Publ. Astron. catalog work, described below, before my June 6th Soc. pacific 94, p. 67 (1982 February issue). They departure on a week-long business trip (see p. 112). list a photoelectric V magnitude for SAD 93221 as The limb-correction data were consequently generated 7.33, in good agreement with Povenmire's estimate, with the current version (BOll) of OCC at the U. S. and I plan to update this magnitude in the XZ during Naval Observatory, and sent to computors june 4-8. rqy catalog improvement work described below. Z.C. Unfortunately, considering mailing times, time to 549 is a PIeiades star whose erroneous Z.C. magni- compute the profiles and prepare the mailing for all tude was corrected in USNO's database during the of the predictions, and business and vacation sched- last series of PIeiades passages; see p. 101. 105

XZ catalog improvement. Late in May, I completed a - complex function of lunar ephemeris, star posi- computer comparison of USNO's zodiacal XZ with the tion, limb correction, observer's position and Perth 70 catalog. I found 394 southern Perth 70 timing result of observation stars that are also in the XZ, but which were not - many other influences: e.g., shape and size of matched in the original comparison done several Earth's body, mean radius of Moon, etc. years ago. This gives a total of 2833 southern At the moment of occultation, the following geomet- stars that are in both catalogs, and a new version rical exactly defined relation between the positions of the XZ including the Perth 70 positional data was of star, observer, and lunar limb (from position of written. I am working slowly on a more difficult lunar disc's center, radius of the Moon and limb program that will merge Yale Catalog (for the poor correction) is valid: As seen from the observer, position G.C. stars) and Lick Voyager catalog posi- the star is situated just at the limb of the Moon. tional data into the XZ; see discussion of the com- - henceforth, true distance of the star to the lunar bined catalog for asteroidal predictions in o.n. 4 limb is equal to zero (3), p. 46-48. When this is completed, probably - residual is the theoretical distance and gives the sometime this month, I will update the XZ stellar sumary error of all above components database at USNO to create the 801 version of the - ideal case: Residual equal to zero, if all com- OCC program, which will be used to compute the limb ponents are free of error (not achievable practi- corrections and final prediction adjustments for cally) or if all errors compensate together acci- ACLPPP profiles for the 1988 graze predicted pro- dentally files. I will also then finally send copies of this - typical values: -2" to +2" ~ improved XZ catalog to those who requested it from Interpretation of residuals: me, some over a year ago (sorry for the delay). - single large O-C does not denote a timing error in . every case, as bad star position or poor limb cor- ?\, rection may also be the cause - in case of very large O-C (e.g., 9:'99): Mostly er- ror in star number, date, or time (e.g., differ- ,., )987 May 8 ,' r \, I ence between UT and local standard time) t X r0 C t %,f \:\ p"" - many O-C of one observer large: Probably error in \ ( I t geographical coordinates of observer \ I 6I iI - single residuals can be checked for coarse errors I \\ 0t II \ II t "" only (see above) : j I,r/}¶ 46,~ /\4/ - evaluation useful only with statistical methods tbud V for determining numerous corrections of influenc- ing quantities; statistical evaluation needs many observations (some 1000 or 10000) Ii' 1,;· / \ Hid or WH (LC): Limb correction - height of real lunar limb at the point of occulta- tion above mean limb in case of positive value, or depth below mean limb for negative value. The mean limb represents the zero line in Watts' charts of the moon's marginal zone and exists the- oretically only for an ideal circular outline of the Moon's disc. Both abbreviations (Hid and m are used with identical meaning by the ILOC. " - input data for reading Hid from Watts' charts: to- pocentric 1ibration in longitude and latitude and The reduction profile for the graze of 4.1-mag. Sig- Watts angle (WA) ma Leonis " Z.C. )644 near Dortmund, German Federal - given to 0!'01 (like O-C), corresponding to about Republic, was sent by Glinther Neue. ' 19 m at Moon's limb (for mean distance) - mean uncertainty ±0!'05, in some cases uncertain by EXPLANATION OF LUNAR OCCULTATION ±0!'5; * denotes uncertainties greater than ±0!'3 OBSERVATION REDUCTIONS - errors in profile corrections are mainly known from comparisons of observed and theoretical limb Dietmar Biittner in case of grazing occultations (see reduction profiles published in O.N.) This article should provide any facts for making the - typical values of HW: -2" to +2" reduction results of lunar occultation observations more understandable. The symbols used refer to re- KM (PA):'Position angle of contact point ductions by the ILOC; deviating ones in parentheses - counted starting at north point of Moon's disc denote symbols used by the HMNAO. through E, S, Id, to N - corresponds to PA in USNO total occultation pre- O-C: residual; difference 'observation - computa- dictions tion' - theoretical radial distance between the star and K-R (not given by HMNAO): the real lunar limb at the reported time of obser- angle between the direction of the Moon's motion and vation the point of occultation - lunar limb profile is considered - 0° for central disappearance, 180° for central re- - O-C is given in seconds of arc appearance, 90° for southern limb graze, and 270° - positive values denote the star to be outside of for northern limb graze lunar limb and negative values denote star inside - K-R is comparable with CNTCT ANGLE in USNO predic- of lunar limb tions (for photoelectric observers only); however, 106

CNTCT ANGLE is expressed in another way: Positive (373) Melusina SAD 189336 Nov 07 ScHtAn values from 0 to 180° for occultations north of (191) Kolga SAD 163997 Nov 08 E10vCp the Moon's center and negative values from 0 to (349) Dembowska SAD 190516 Nov 10 ScHtAn 180° for points south of this path (0° central (397) Aquitania SAD 191017 Nov IQ ScHtAn disappearance, ±180° central reappearance, -90° (779) Nina AGK3 +34 0176 Nov 12 Fr southern graze, +90° northern graze) (9) Metis AGK3 "20 0417 Nov 13 BcDyOmGwGsLpMoMjRhwk (261) Prym AGK3 +18 0830 Nov 14 Th Both KM and K-R are counted from 0 to 360° counter- (191) Kolga SAD 164199 Nov 21 OvSmGyCp clockwise. (778) Theobalda AGK3 +24 0073 Nov 27 ElGyCp (210) Isabella SAD 189826 Nov 28 Sc REPORTS OF ASTEROIDAL APPULSES AND OCCULTATIONS (104) Klymene AGK3 +24 0437 Nov 28 Ly (125) Liberatrix AGK3 +06 0220 Dec 02 21 Observers 7 Jim Stam (233) Asterope SAD 157658 Dec 04 DmK1MjMo (ii) Parthenope SAD 96444 Dec 04 St Reports of all appulses and occultations should be (676) Melitta SAD 165128 Dec ]3 StLy sent to me at Rt 13 Box 109; London, KV 40741; (509) Iolanda AGK3 '05 0712 Dec 14 CbCrMsMzMoPo U.S.A. If the target star was monitored near the 1145) Adeona AGK3 +11 0301 Dec 17 Gg?a predicted time of an event, then the observation was 877) ldalkure SAD 93900 Dec 22 Ly valid, and a report should be sent to IOTA — even if (242) Kriemhild AGK3 "08 0362 Dec 23 sjslMkMpMy nothing was seen. We use the negative reports more (17) Thetis AGK3 +17 0486 Dec 24 Sm than we do the positive ones. (87) Sylvia SAD 77917 Dec 28 SaMpMyFr (43) Ariadne AGK3 +21 0753 Dec 28 Sa Table 1. Asteroidal appulses and occultations ob- (946) Poesia SAD 80322 Dec 30 MpMyLyFr served from july through Decenber 1986. Notes: Events from July through December, 1986, Minor Planet Star Date Observers Notes referenced in Table 1.

(306) Unitas SAD 161893 Jul 04 Rb I) Observers monitoring this event were BhBgCnGzCsCo (187) Lamberta AGK3 +09 1363 jul 04 CpCm DcDgMiG1GuGsjgLcLhMtNpRdTsThTdVsVvZm. Zinnermann (287) Nephthys SAD 141631 jul 10 HtAn recorded a blink of 0.4 to 0.5 sec. duration. (19) Fortuna AGK3 +14 0219 jul 12 HtAn 2) Tregaskis reported a "definite" disappearance at (415) Palatia SAD 159637 Jul 12 NtMoPoPi 19:46:47.1, and a reappearance at approximately (741) Botolphia SAD 187699 Jul 16 LdBwOdMfldh 19:46:49, under good sky conditions. This obser- (679) Pax SAD 189278 jul. 18 ScAnl¢yHt vation indicates a southward shift of about 0!'5. (741) Botolphia SAD ]87571 Jul 23 Ldwh 3) Observers were OvKtkgMcHIMbE1BjFtVnMeSmGyFs. (46) Hestia AGK3 +15 0246 Jul 26 OvGyMeFsVb 4) Observers were AgBhBrBfBnDIGsInLpMsMzMoPmRnSbTpHl (697) Gali1ea AGK3 +10 0227 Jul 27 SmGyOkSpLkMbVb cpsmE10vBj. The two French observatories report- (52) Europa SAD 146840 Jul 31 Mt ed that the event occurred one hour sooner than (377) Campania AGK3 +18 0265 Aug 02 24 Observers 1 predicted. None of the other observers reported (41) Daphne AGK3 "03 2032 Aug 06 LdMxBaNsScAn a different time. (409) Aspasia AGK3 "24 0406 Aug 07 TgScAn 2 5) A 2-magnitude drop from 1:28:31.5 to ):28:38.9 (232) Russia SAD 163645 Aug 10 PvCuLWhScAn was reported, along with some fluctuations around (213) Lilea SAD 185266 Aug 21 AmGaGcLbPIRn 1:25 by Lipski. The observatories reported that (145) Adeona SAD 111430 Aug 29 Mo the shift placed the path over central Africa, (705) Erminia AGK3 '41 0840 Sep 06 TpRnOrNpPoMoLpGv and that it was about 10 minutes later than pre- (1115) Sabauda SAD 211769 Sep 07 ScAnHtRg dicted. (393) Lampetia AGK3 +04 2577 Sep 07 ScAn 6) Observers were BrCsCvGmGbGpGflnLtMhMrMtMuNMwNzPn (385) Ilmatar SAD 208293 Sep 13 14 Observers 3 RzSiSsSrVf. The asteroid passed north of the (104) Klymene AGK3 "23 0457 Sep 17 D1EINp star at Stuttgart, German Federal Republic, and (932) Hooveria AGK3 +28 0489 Sep ]7 ScAnHt south of the star at Mostoles, Spain and Locarno, (332) Siri SAD 146545 Sep 21 22 Observers 4 Switzerland. Germann reported a "non-instantane- (2363 Cebriones AGK3 +11 2151 Sep 23 StFr ous disparition at 19:26:47.5 during 16 seconds." (431) Nephele AGK3 "21 0763 Sep 24 AnHt See R. Boninsegna's article. (190) Ismene SAD 162468 Sep 29 StFr 7) Observers were AjBhBrBiCsCbOyGolnIvLpMsMqMzMoMwNP (148) Gallia SAD 167259 Sep 29 FrLn OzPmRnVf. Ortiz reported a possible occultation (598) Octavia SAD 166016 Oct 01 StLx beginning at 18:27:09.5 and lasting 7.6 seconds. (38) Leda SAD 75363 Oct 04 StLyFrLnRbMpMY Pie du Midi reported that the minor planet passed (487) Venetia AGK3 +13 0491 Oct 13 CsOyGbLpMoPmNp north of the star. See R. Boninsegna's article. PoTNkZm 5g) This event was the first from which Australasian (613) Ginerva AGK3 +13 0491 Oct 18 DbPm and Lowell observatory updates were to be ob- (676) Melitta SAD 164583 Oct 21 StRb tained. Lowell had problems, but Craig Bowers at Perth Observatory obtained plates on December 9, · (405)(417) SueviaThia SAD 164275SAD 161462Oct 22 BucdGiGjGxGcNcRpRuTiTfOct 22 ElOvSm 15, and 16. Warwick Kissling in Wellington com- (597) Bandusia AGK3 +19 0229 Oct 26 8cBhBnGbRnTh puted a path shift of 3!'4 N from the Dec. 9th (818) Kapteynia SAD 210004 Oct 27 Cm plate, and 2!'8 N from the other two plates. Gra- (597) Bandusia AGK3 +19 0227 Oct 27 Sc ham Blow and David Herald notified a large number (93) Minerva AGK3 +02 0008 Oct 27 22 Observers 6 of observers in the area. A definite miss was (222) Lucia AGK3 "19 0870 Oct 29 EtFzMvNpTiZw reported from Hobart, Tasmania, and Martin George (94) Aurora SAD 79994 Nov 04 StLykhWrMpMyAzWz in Launceston reported a 0.2-sec. blink with 50% (583) Klotilde AGK3 +02 1392 Nov 04 An certainty, at 12:31:25.5 — which is near the up- (297) Caecilia SAD 164457 Nov 06 LyMpMy dated time and position. All other locations (597) Bandusia AGK3 +19 02)1 Nov 07 El were clouded out. 107

Table 2. Observers and locations of events reported M. Kohl Kl Uster, Switzerland I from July through December 1986. C. Lake Lk Pietermaritzburg, South Africa 1 Thomas Langhans Ln San Bruno, CA 2 Observer jp. Location Reports Rec'd J.-F. Leborgne Lb S. F. dc Guixois, Spain 1 J. Lecacheux Le Obertraun, Austria ) f. Aljama Al Sabade11, Spain 1 j. Lecacheux Lt Meudon,'France I m. Alufji Ag Genova, Italy 1 H. Le Tallec Lt Toulouse, France I C. Amengual Am Palau-Sabardera, Spain 1 A. Lheureux Lh Brussels, Belgium 1 Peter Anderson An The Gap, Queensland, Australia 14 P. Lipski Lp Dresden, German Democratic Rep. 5 John Asztalos Az Milwaukee, ldl I Brian Loader Ld Blenheim, New Zealand 3 Lindsay Ball Bd Coopers Plains, Qnslnd, Austr1. 1 Dennis Lowe Lw Bundaberg, Qnslnd, Australia 1 J. Barthes Bh Castres, France 4 Greg Lyzenga Ly Altadena, CA 7 P. Barufetti Br Massa, Italy 3 Alistair MacOonald Mx Townsvi)1e, Australia I F. Basslni Bf Bologna, Italy 1 C. Mahot Mv Vauvenargues, France I A. Battare)1i Bi Trento, Italy 1 S. Maksymowicz Ms Chapet, France 2 J. Begbie Bj Harare, South Africa 2 Patrick Manly My Tempe, AZ 6 C. Blanchart Be Brussels, Belgium 2 Peter Manly Mp Tempe, AZ 6 Graham Blow Bw Wellington, New Zealand I M. March Mh Mataro, Spain 1 Roland Boninsegna Bn Dourbes, Belgium 2 B. Margesin Mg Trento, Italy 1 J. Bourgeois Bg Conneux, Belgium i hi. Marinello Mr Brescia, Italy I J. Bourgeois Bu Bagneres, France I J. Marti Mt Mataro, Spain 3 J. Cano Cn Puigcerda, Spain 1 H. Marx Mu Stuttgart, German Federal Rep. 1 N. Cardie1 Cd Madrid, Spain I P. Mazalrey Mz Vernon, France 3 R. Casas Gs Sabadel}, Spain 4 F. Mazzanti Mi Puigcerda, Spain 1 M. Cavagna Cv Cajvignano, Italy 1 A. McRae Mc Johannesburg, South Africa I joe Chums Cm Cape Town, South Africa 2 jeff Medkeff Mk Hartvi11e, OH 1 A. Colomba Gb Reggio Calabria, Italy 2 Meudon Obs. Mo Meudon, France 9 F. Comeron Co Argentona, Spain I D. Michie Me Johannesburg, South Africa 2 Tim Cooper Cp Sasolburg, South Africa 5 J.-P. Michon Mi Element, France 2 F. Courbin Cr Vernon, France I Milano Obs. m Merate, Italy 1 Don Currie Gu Bundaberg, Qnslnd, Australia 1 E. Mirco Mw Trento, Italy 2 G. DeBenedetto Ob Reggio Calabria, Italy I A. Morrisby Mb Bulawayo, South Africa 2 M. Deconinck Dc Limal, Belgium 1 Noel Munford Mf Palmerston North,. New Zealand 1 F. Delahaye Dy Bordeaux, France 3 G. Napolitano Np S. Maria D. Mole, Italy 6 j. Delgado DB Puigcerda, Spain I Nat'l. Astro. Lab. Nt Itajuba, Brazil 1 J. dc Klerk Ok Potchefstroom, South Africa I E. Nazry Nz Toulouse, France 1 M. Dentel cm Bernau, German [Mocratic Rep. 2 Nice Obs. Nc Nice, France ) R. DI Luca DI Bologna, Italy 2 Gary Nielsen Ns Coopers Plains, Qnslnd, Austrl 1 Tony Dodson Dd Wellington, New Zealand 1 L. Orsi Or Bologna, Italy 1 G. Earle El East Rand, South Africa 6 E. Ortiz Oz Vitoria, Spain 1 A. Elliott Et Leeds, United Kingdom 2 Danie Overbeek Dv East Rand, South Africa 6 Filipowicz Fz Otwock, Poland 1 Paris Obs. Po Paris, France 4 R. Fleet Ft Harare, South Africa 1 R. Pe11o PI S. F. dc Guixois, Spain I B. Fraser Fs johannesburg, South Africa 2 S. Piana Pn Vara11o, Italy 1

. Tony Freeman Fr Berkeley, CA 7 pie du Midi Obs. Pm Pie du Midi, France 4 C. Gallart G1 Puigcerda, Spain 1 J. Piriti Pi Nagykanizsa, Hungary 1 C. Gallart Gi Igualada, Spain 1 Norm Plever Pv West Footscray, Australia 1 J. Ga11ego Gj Madrid, Spain 1 G. Raspadori Rp Bologna, Italy 1 J. Garcia Ga Lisboa, Portugal I G. Regheere Rh Grenoble, France 1 M. Genovese Gy Prafonevoso, Italy I' A. Renou Rn Brissac, France 5 M. Genovese Go Torino, Italy 1 Benny Roberts Rb Jackson, MS 3 Martin George Gg Launceston, Tasmania 1 D. Rodriguez Ru Vi11aba, Spain I R. Gemann Gm Wald, Switzerland 1 D. Rodriguez Rz Mostoles, Spain I M. Geyser Gy Pretoria, South Africa 5 J. Rodriguez Rd Guadalajara, Spain 1 A. Gomez Cx Madrid, Spain 2 D. Rogers Rg Wynnum West Brisbane, Australia I j. Gomez Gz Puigcerda, Spain 1 D. Schieb Sb Mulhouse, France 1 R. Goncalves Gc Lisboa, Portugal 1 D. Schieb Si I11furth, France 1 C. Gros Gb Besancon, France 3 J. Smit Sm Pretoria, South Africa 6 C. Grunnet Gw Virum, Denmark I Charlie Smith Sc ldoodridge, Qnslnd, Australia 12 Gruppo list. Savonesi Gp Savona, Italy 1 Specola S. Ticinese Ss Locarno, Switzerland 1 A. Grycan Gf Toulouse, France 1 j. Spoelstra Sp Potchefstroom, South Africa 1 J. Guarro Gu Puigcerda, Spain I Billy Stann $1 Cuyahoga Falls, OH 1 J.-D. Guerisse Gs Brussels, Belgium 3 jim Stam St London, KV 8 A. Hi)ton HI Johannesburg, South Africa 2 Jim Stann Si Akron, OH 1 Steve Hutcheon Ht Sheldon, Queensland, Australia 9 Jim Stamn Sa Westfield, MA 2 M. Inghirami In Massa, Italy 3 L. Strabia Sr Brescia, Italy 1 Z. Ivica Iv Rijeka, Yugoslavia 1 E. Tassi Ts Forli, Italy 1 jungfraujoch Obs. Jg jungfraujoch, Switzerland 1 Y. Thirionet Th Brussels, Belgium 3 Philip Kearney Ky Bundaberg, Qnslnd, Australia 1 P. Todini Td Siena, Italy 1 L. Keith Kh Milwaukee, kll 1 P. Todini Ti !so1a d'Arbia, Italy 2 j. Knight Kt East Rand, South Africa I Bruce Tregaskis Tg Mt. Eliza, Victoria, Australia 1 S. Knight Kg East Rand, South Africa I F. Tulipani Tp Bologna, Italy 2 108

F. Tulipani Tf Tizzano, Italy 2 pp 8 Milano Obs. (I - Merate) F. Vaissiere Vf St. Genest-Lerp, France 2 9 W. Marinello - L. Strabla (I - Manerbio) P. van B1omnestein Vb Cape Town, South Africa 2 10 M. Cavagna (I - Calvignano) E. Velasco Vs Guadalajara, Spain 1 11 Gruppo Astrof. Sav. (I - Savona) J. Vi11averda Vv Puigcerda, Spain I 12 P. Barufetti - M. [nghirami (I - Massa) J. Vincent Vn Harare, South Africa 1 13 M. March - j. Marti (E - Mataro) Sally Waraczynski Wz Milwaukee, WI 1 14 R. Casas (E - Sabade11) David Paul Werner Nr Lakewood, CA 1 David Wheeler \Ah Corrima1, N. S. W., Australia 3 2. (125) Liberatrix and AGK3 +6 0220, 1986 Dec. 2. N. P. Nieth-knudsen Wk Tisvildeleje, Denmark 2 Zawilski Zw Lodz, Poland 1 Again, a total occultation was reported by only one L. Zimmermann Zm Brussells, Belgium 2 observer. Here, the case is more critical: The di- ?a Hobart, Tasmania 1 ameter of Liberatrix is not accurately known, vary- ing from 103 km (Gehre1s) to 47 km (Pilcher). MORE INFORMATION ON NO ASTEROIDAL APPULSES · 1 Roland Boninsegna

The positions of the stations presented in the fig- ures have been moved onto a single line, in the fun- 2 100 km damental plane, perpendicular to the motion of the · 3 minor planets. "=> '

1. (93) Minerva and AGK3 +2°0008, 1986 October 27.

Most of the stations are presented in Fig. 1. One total occultation was recorded by station 3, lasting about 16 seconds. The diameter of (93) Minerva is ' o;'i well-known (see Mi11is, R. L., 1985, Icarus 61, 124 5 or Note Circulaire GEOS 450): 170.8 ± 1.4 km. E M Figure 2 8 , C4 ·% a The chord reported by station 4 is presented in Fig. 2, with the position of Liberatrix assuming a north or south chord and a }03-km diameter. If the north- ern track is more unlikely, we cannot rule out the reality of the southern one: No station could con- tradict E. Ortiz' observation. It is noteworthy W ta re)" that Pic-du-Midi Observatory reported a north shift h t ~na mo r·"aj aT rC4T"r" t using visual control. D I: I j. Barthes (F - Castres) Gtu 2 G. Napolitano (I - St Maria Della Mole) tv 3 Pic-du-Midi Observatory '(F - BagnCres) 4 E. Ortiz (E - Vitoria) 5 F. Aljama (E - Sabade11)

Conclusions.

The chord reported by station 3 is presented as the None can really be drawn, especially for the Libera- position of Minerva assuming a north or south chord. trix event. Double stations would have improved the As the figure shows, other stations should have re- conclusion. Be careful in reporting information on ported the occultation, especially if the track of a minor planet's position relative to a star, during MinerVa was the southern one. The observer at sta- appu1se: It is not so easy when the path is nearby. tion 2 interrupted his observation during some in- stants around the moment of station 3's event. So For the complete list of observers for these events, only two stations contradict R. German's report, if see Note Circulaire GEOS 518. the track of Minerva was the northern one. All the observers were further questioned; they were all CORRECTION sure of star identification. Last important detail: Station 6 and Diego Rodriguez (148 km below station David KL Dunham 14) reported that Minerva passed south of the star, while station ] reported it north. On p. 58 of the last issue, I said that a graze of 107 B. Tauri had been observed in the Soviet Union 1 H. Marx (D - Stuttgart) in 1986. This star is not in the Z.C. In a recent 2 D. Schieb (F - I11furth) letter, Alexander Osipov said that the star was ac- 3 R. German (CH - Nahren) tually Z.C. 840 = 107 B. (Aurigae). Bode assigned 4 C. Gros (F - BesanCon) the star to Auriga, but after the I.A.U. later spec- 5 E. Mirco (I - Trento) ified official constellation boundaries, the star pp 6 Specola Sol. Ldc. (CH - Locarno) ended up in Taurus. Osipov said that 825 occulta- 7 S. Piana (I - Vara11o Sesia) tions were timed at 17 Soviet observatories in }986. 109

ASTRONOMY AND PERSONAL COMPUTERS to some of them. Also, we would like to hear about other projects that IOTA members think would be use- Joan Bixby Dunham ful.

projects Updates: Now that we have had some experi- 1. Write a program to use when entering, editing, or ence with the PC projects, as well as coments and correcting occultation observations data to go to discussions on them at the Universe '87 meeting, we the ILOC. See David's article (p. 92 ) in this is- have reorganized the projects list to be more use- sue for the format. Data can be entered in the ILOC ful. Some of the projects are removed as completed, format with a simple editor, but it would be better others because we do not think they are going to be to have software to check entries for obvious errors very productive or useful. Let me know if you are and to help in editing or correcting the entries. interested in doing some of the following projects, Peter Manly has written software earlier, before the or if you think you have done some work that applies format was defined, and perhaps that could be modi- i S. O'MEARA LUNAR F'ROFILE: GRAZE OF ,1986-8-29 z-e- 885 CENTRAL GRAZE AT HOLLYWOOD M!) j..-- "" "'"' .....L,.CoDRMUMM ,9 2j3 }] 4 " " j""""·: 6: AQ9E' '~ ,? Em ,X""' , , ' .,: -Fj2 " ..- ""'"" "j=<:>4""" L '" " - " k""" i-<: ' "m" "" fi'tt!9,:t' =, ""' ·--=--""_"""' -"z=-E4'i ' '":;j ..i' 'eic_;,""'"'"""" '" ,^ "" ' J. DUNHAM _ _ X X " " "==':—··'· ,"K.1CAZMECIAK E. SCHEIDKER —- :1 .. : -" '"'""" ";yurj lj i.,.£= D HX..~ .-- l- .' J. IITVER — A_ X X .- " " '. , . .="=C" I L—J I——.- . — '·'-- ·&":T; —— R. BOLSTER "==·T " "':_"" "" W j" . . lj I . , . -...... ".,"=_N. LANG Y. NISSEN =*T- - --—- """Z... "=iq'I yit'd - X " -.--=.--""" ' -- —r,-— KNIGHT L""" 5uY—._~__ , I'. 1RUEBL00D -_C>':8_ . '." -..::==.-=:_FI,9: b6W""Iq 11 chell

" ' B U\ - _J L,x """-- ~.. D. MOORE u. 2 X

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VERSION 80H. LjBRATIMS: LONG.r .24 LAT. H -S. 74 SHIFT - -.44 ARC SEC. PLOT BY R.N. BOLSTER Robert Bolster prepared this reduction profile of light. Paths for the Maryland observers are hori- the graze of Z.C. 885 on 1986 August 29 using his zontal, with observer names on the left. Scheidker Apple II computer and observer track data computed called out "R" for what was actually a flash, caus- with the OCC program at USNO. Central graze for the ing the discordant line near the center of the plot. four expeditions are indicated with vertical lines Slanting lines show paths for other expedition ob- under "HOLLYWOOD" in the heading: servers, who are named on the right. The names for P. Donbrowski and L. Robinson are printed on top of No. Place Expedition 1eader(s) each other. Dombrowski, whose path has the smallest slope of the two, timed 22 events. For the observ- I Hollywood, MD D. Dunham and R. Taibi ers outside of Maryland, the path slopes, caused by 2 Plymuth, MA j. Maltsberger differences in position angle of central graze, are 3 Narragansett, RI P. Dombrowski large due to the factor of 31 exaggeration of verti- 4 Reidsville, NC M. Lang cal distances over horizontal distances. The shift given at the bottom does not include the empirical The curve is the Moon's mean limb, and x's are correction applied to northern-limit profiles by the points from Watts' limb correction charts. Unfor- ACLPPP prediction program. Using the current Decem- tunately, Bolster's platter draws the paths too ber 1986 version of ACLPPP, the effective shift was quickly, so that parts of them are invisible or very -0';jg. 110

fled. seems to show that there is a difference in reaction times between asteroid and lunar occultation events. 2. Search occultation reports for double star data, A simulator is one way to see whether there really report the observations, and put the information in- is a difference, and what it is. A project would be to a machine-readable format for inclusion in the to use Larry's simulator, or write one for other ma- graze predictions. Don Stockbauer is defining the chines, and collect the difference in reaction times format. for simulated grazes, as compared to simulated as- teroid occultations, from many different people. 3. Bob Bolster wrote a program for the Apple II to The simulators also are useful for showing inexperi- create reduction profiles of grazing occultations enced observers what to expect. based on the observations and on the occultation prediction data available for PCS. Now what is 8. Convert ALPO president John Hestfall's Moon plots needed are options to format the USNO OCC output for from an Apple II" to a PC XT. These are used by the Apple and to add the ability to retrieve data ldestfall to plot daily charts of the Moon for ALPO, from the new format for electronic reporting of outlining the maria and major craters, and showing grazing occultation observations. Also, it would be the terminator. The project is to see whether this nice to have this software converted to work on oth- would be useful for portraying important occulta- er computers. tions, especially reappearances.

4. Write software to help in planning observations, project Status: The following is a sumary of what given a particular observing site's location and was done for some of the projects we had listed in limitations. The software would have a "mask" it the past. would apply to the sky that describes the viewing blockages from buildings, trees, etc. It could scan Don Oliver has converted the GRAZE, ACLPPP, and the prediction data and tell observers which events MEEUSMAP programs to PCS, and is in charge of dis- might not be possible from the observing location, tributing them. Several computors are now using PCS and might include times of Sun and Moon rise/set, to do the graze predictions. with an option to enter coordinates of any object and compute its rise/set/culmination. It could be Bob Bolster, as mentioned earlier, has written soft- combined with the precise predictions software des- ware for an Apple II to do reduction profiles of the cribed later. grazes.

5. Write a PC program to compute total occultation Don Oliver and Pat Trueblood each worked on arrang- predictions for local regions to use the regular it- ing David's graze computor papers into a graze com- erative method for determining occultation times. putor manual. I am now in the process of combining This could be done by converting a part of the Evans what they did and updating it, and have a prelimin- program used to compute the USNO total predictions ary user's guide for the GRAZE program, but not to run on a PC. Part of the project would be to de- ACLPPP or MEEUSMAP. Pat also entered David's list termine a means of reducing the size of the input of local occujtation observers into a PC-Fi1e+ data- data set needed sq that the data will fit conven- base, to give us some practical experience in using iently on a few floppies. There is a BASIC program that DBMS. to compute totals from a.and b factors, similar to the FORTRAN program Walter Morgan uses to answer re- For double stars, Walter Nissen is deriving a method quests for standard coverage predictions. David for determining separation, position angle, and Herald has written a program with the more accurate their rates of change from speckle interferometry occultation computations for the Commodore C64/C128, data on stars for which orbital elements are not _ but he needs the star catalog data on a floppy be- known. Don Stockbauer is standardizing the formats fore he can use it. A connercia1 program, PC Alman- used for storing double information and writing a ac, also does computations of occuitations this way,, program to read the data files and automatically in- but also has a very limited amount (about 30 stars) sert the double star information into the graze in- of catalog data. put data sets.

6. Write software to help in leading grazes. One On the project to create a data base of observatory project in particular would be to investigate the information: Several volunteered to do data entry use of PC mice in measuring the coordinates of ob- of the observatory information, and have ideas on servers. Are they accurate enough? Are they prac- how to do the data storage and retrieval. However, tical? Graze leaders might have more ideas for first we must have data on the observatories, and we software. do not have a good plan for getting that yet,

7. Larry Dunn has written a graze and asteroid oc- Software: The software available from me is listed cultation simulator for the Macintosh, which he dem- below. For each, send the number of diskettes indi- onstrated at Universe '87. He generates graze cated and a self-addressed mailer with sufficient events next to a gibbous Moon with a random fence of postage for the mailer and diskettes, approximately obstructions, trying to generate a view similar to 22¢ for the mailer and 17¢ for each diskette in the what is seen through a telescope. He included op- U.S. These are MS-DOS 54 DSDD diskettes. tions to simulate atmospheric turbulence or not, and to show the obstructions or not. Larry's address is 1. Generate total occultation predictions, written given at the end, for those Mac owners who would in GWBASIC (2 diskettes) like a copy. (Send him a disk and an addressed and stamped mailer.) 2. Computerized !L0C forms, in Microsoft Basic under CP/M, provided to us as text files Oh an MS-DOS Data reduction of the Pa11as asteroid occultation diskette. (Peter Manly's software, discussed in Ill

project #1, 1 diskette) America, and performed this function up to the time of his death. 3. Six diskettes of public domain or shareware as- tronomy software. Under his auspices, regional meetings were organ- ized, and he stimulated astronomical clubs and soci- Addresses: eties. He also proposed several observational pro- jects involving occultations visible from Brazil. joan Bixby Durham; PO Box 7488; Silver Spring, MD 20907 In 1972, Polman founded the "Clube Estudanti1 dc As- Larry Dunn; 34625 Seavey Loop Road; Eugene, OR 97405 tronomia," at Recife, which is one of the best- Don Oliver; 13173 CIarewood; Houston, TX 77072 equipped amateur societies in Brazil. It is still active, with introductory courses, practical work HUBBLE SPACE TELESCOPE AMATEUR PROPOSAL DEADLINE and publications. EXTENDED TO NEXT SHUTTLE LAUNCH Polman was born in Amsterdam, on January 7, 1927, David KL Dunham and took root in Brazil during 1952. Here, he was clergyman and professor. His fascination for as- At the Universe '87 convention in California, Steven tronomy, particularly for observing, his talent for Edberg met with other members of the Amateur Astron- small inventions, and his mastery captivated every- omers Working Group (A.A.W.G.) for H.S.T. proposals. one who knew him. He was dynamic, indefatigable, \._ With the current launch delays, the original June jovial, and possessed by a notable sense of good hu- 30th deadline was considered unrealistic. In order mor. At the same time, he was simple and sympathet- to avoid the need to change the deadline again in ic. His death opened an enormous void, very diffi- case of further delays, the deadline for receipt of cult to fill. the preliminary proposals has now been set as the date of the next American Space Shuttle launch. But THE 1983 NORTH AMERICAN DATUM as a reward to those who met the June 30th deadline, al] of those proposers will be accepted for the sec- David W. Dunham ond round of more detailed proposals. The A.A.W.G. plans to have the second-round proposal forms ready Articles in several North American newspapers during for distribution by the end of the year. Also, for- the past month have told how several landmarks have eign amateurs can be co-investigators, but not prin- "moved" 50 meters or more as the result of a new cipal investigators, for the H.S.T. This is partly survey using modern techniques. These changes are to save costs, since the Space Telescope Science In- large enough to be of interest to occultation ob- stitute will pay travel expenses for the principal servers. Most North American maps use the 1927 investigator to be present when his or her observa- North American datum for their survey reference. tions are made. Another decision, which I objected The comprehensive new survey was undertaken to de- to but was overridden, was the definition of profes- fine the improved 1983 North American datum. Recent sional astronomers, who are excluded from the ama- maps published by the U. S. Geological Survey have teur proposals, even as co-investigators. A person tickmarks in the corners showing the offsets between is considered a professional astronomer if, at the the two datums, and list the numerical values. time he submits his proposal, he either earns a ma- jority of his income from an astronomical profes- We do not yet have the corrections needed to convert sion, or if he has an advanced degree (either Mas- 1983 North American datum coordinates to the I.A.U. ters or Ph.O.) in astronomy. I objected to the de- ellipsoid world geodetic system used for analysis of - gree part because some advanced degree holders do occultation observations, but we will soon try to not earn their incomes as astronomers, and conse- get this information. About ten years ago, results quently, unlike professionally employed astronomers, of preliminary work for the 1983 datum allowed new they usually can not use the resources of the insti- corrections to be determined for different parts of tutions where they work to submit professional (Gen- " the 1927 datum to permit more accurate calculation eral Observer) H.S.T. proposals. As of late July, of the I.A.U. ellipsoid coordinates from 1927 datum Paul Maley informs me that IOTA has received five coordinates. These were incorporated into the OCC occultation-related proposals for H.S.T. amateur ob- program geodetic database at 1JSNO by Van Flandern. servations. These corrections are nearly equivalent to the shift to the 1983 datum, which will give relatively small JOHANNES MICHAEL ANTONIUS POLMAN (1927-1986) changes from them. So the lack of 1983 datum con- version factors should not be as serious a problem Luiz Augusto L. da Silva as the newspaper articles might imply for our work. We will try to convert everything to the 1983 datum On June 2, 1986, Prof. johannes M. A. Polman, known when we get sufficient information to do so. Al- as Jorge Polman, living at Recife, Brazil, passed though unlikely, we may need some help in tracking away at age 59. down this information for specific areas, and will let you know if that is the case. Polman was an IOTA member, chairman of the Asteroid- al Occultations Section of the Iberian-American SOLAR ECLIPSE NEWS League for Astronomy (an intercontinental society founded in 1982), and a former coordinator of the David kl. Dunham Occultation Comission of the Brazilian Union of As- tronomy, as well as an ex-president of this same so- 1987 March 29, broken annular: This eclipse was to- ciety. tal over parts of the Atlantic Ocean. The best land view was seen from Gabon, on the Atlantic coast of In 1981, he was elected the IUAA adviser for Latin central Africa, where the eclipse was broken annu- 112

1ar. The beads phenomena were even better than dur- ences to make preliminary arrangements to observe ing the 1984 May 30 eclipse, since the Moon's appar- this eclipse from the northern U.S.S.R. ent radius was about 1" larger relative to that of the Sun. Observers from the United States, France, 1991 july 11, total: Ma1ey notes that the southern Germany, and japan gathered at POrt Gentil to ob- limit passes very close to Puerto Va11arta. serve the eclipse from three locations in an effort coordinated by Paul Maley. Maley published an arti- IOTA/ES NEWS cle about their efforts in the July issue of Sky and Telescope. Torrential rain dampened spirits the David N. Dunham morning of the 29th, but the clouds thinned as the central eclipse approached. The thickness of the My plans to visit Europe, to attend a comet symposi- clouds changed rapidly during the central eclipse at um in Brussels, Belgium, were briefly described on Maley's and Hans Bode's sites, allowing video re- p. 58 of the last issue. After spending the first cordings of only brief glimpses of Baily's beads. night at Hans-joachim Bode's house in Hannover IOTA/ES was given official notification of their (where I gave him copies of IOTA graze and total oc- group's status as a scientific organization about a cultation software on diskette for his IBM-compati- week before the eclipse, so that the travel expenses ble PC), we traveled to Kiel on April 5th, where we of members from the German Federal Republic are de- had a meeting of mostly German members of IOTA/ES. ductible from the income that they report for tax Kyri1 Fabrin and Leif Kristensen traveled from Den- purposes, just as is the case for the parent IOTA in mark to attend the meeting. Hans gave a report of the U.S.A. The japanese team was fortunate to have his expedition the previous week to Gabon, where he the thinnest cloud cover at their site, but the bat- joined Paul Maley in efforts to videorecord the tery powering their video equipment failed right at March 29th eclipse (see p. Ill). Shortly before his central eclipse! Fortunately, they got complete trip, IOTA/ES was officially recognized by the gov- photographic records of Baily's beads, both with an ernment of the German Federal Republic as a scien- B-m movie camera and a 35-m camera with automatic tific research organization. So like American mem- winder taking pictures at half-second intervals. bers of IOTA, German members of IOTA/ES can now de- Reiko Morufushi showed me their records while I was duct the costs of their travels for eclipses and qc- in Tokyo on May 1]th. They have just begun the cu1tations from their income taxes. Hans also pro- analysis of their material, with help from ILOC. posed an expedition to the vicinity of Alma Ata, U.S.S.R., to observe the annular eclipse of Septem- Plans for expeditions to time Baily's beads near the ber 23rd near the southern limit, but few expressed edges of future eclipse paths are mostly preliminary any interest in such an effort; a total eclipse and are briefly described below: would be more popular. I discussed the status of IOTA's various projects. Fabrin discussed the ar- 1987 September 23, annular: Paul Maley and Hanssen rangements for the sixth annual European Symposium Tours travel agency have worked with astronomers at on Occultation projects (ESOP-VI), to be held in Purple Mountain Observatory and Beijing Observatory Aalborg, Denmark, at the end of August. This will to set up an expedition to observe this eclipse from probably reach readers too late to make new arrange- China. The planned tour will leave San Francisco on ments to attend, but anyone interested can get more Sept. 18 and return on Oct. 4. Several IOTA members information from Dr. Kyril W. Fabrin; Raadsherrevej plan to be in the tour, including me. While in Chi- 2, Hasseris; 9000 Aalborg, Denmark; telephone (DB) na, the tour will visit Beijing, Shanghai, Xian, and 181513. I'm sure that a separate mailing about Guilin, as well as sites at both limits in two sep- ESOP-Vl was distributed to IOTA/ES members some time arate groups in and south of Taiyuan on eclipse day. ago. Hans Bode has made plans to observe the eclipse from the southern limit in the south-central U.S.S.R., During one evening while I was in Belgium, a dinnerl """ which is much less expensive for Europeans to travel meeting was arranged at the Urania Observatory in to than China. Hove, a suburb of Antwerp. I met most of those at- tending the meeting for the first time, including Edwin Coffin, Roland Boninsegna, and Henk Bulder 1988 March 18, total, The only land crossed by the edges of this path are in Sumatra, Borneo, and the from the Netherlands. Also there were Eberhard southern Philippines, as shown on maps that have Bredner from Germany (he met me in Brussels and been published now in both Sky and Telescope and as- drove me to the observatory) and jean Meeus, whom I had last seen nearly 20 years ago. Coffin had just tronomy. Maley is planning to go to the latter lo- cation, if the limit areas are reasonably safe by completed selection of his asteroidal occultation predictions for 1988, and was starting to print eclipse time. The Hanssen Tours expedition will de- part Los Angeles on March 12th and return on the them. jim Stann received Coffin's package of 1988 25th, with cost $2680, double occupancy. Observa- events in May, and David Werner has already begun tions will be made from, and north of, General San- annotating the charts that we will publish in the tos on Mindanao. Those interested should contact North American asteroidal occultation supplement for Paul Maley; 15807 Brookvilla; Houston, TX 77059. 1988, which we probably will distribute with the Hans Bode is planning to observe from the east coast next issue. I had lunch with jean Meeus at the of Borneo, and David Herald and other Australians Brussels airport where he works, a few hours before hope to observe from Banka Island near Sumatra. Un- my return flight. He demonstrated his lunar ephem- fortunately, Fiala's attempt, to obtain U.S. Naval eris program, which achieves an accuracy of 0!'01 us- support to get to the southern limit, where it cros- ing a subset of Chapront's lunar theory ELP2000. ses two rather inaccessible islands south of Minda- From some 37,000 terms, Meeus combined several and nao, seems to have failed. eliminated the majority of terms with very small co- efficients to produce his subset of nearly 6000 1990 july 22, total: Maley has contacted astrono- terms. He repeated his long-standing request for mers in Leningrad and in the Soviet Academy of Sci- the XZ catalog, the updating of which I would have 113

completed by now if I had trave11ed less this year! Paul Maley and Charles Herold represented IOTA'S in- terests at the colloquium in Paris on june 20 to 24. In early June, I returned to Europe, to attend a Paul gave a talk on videorecording eclipses, and spacecraft mission planning meeting at E.S.A.'S Eu- Hans Bode discussed his trip to Gabon for the March ropean Space Technology Centre (ESTEC) in Noor&ijk, 29th eclipse. He also gave my talk on videorecord- the Netherlands, on the 9th, and a symposium on ing grazes (I had given him a 7-minute tape of 4 of problems in astrodynamics and celestial mechanics in the best events), while Wolfgang Beisker gave my Turin, Italy, the rest of the week. I first visited presentation about the 1983 occultation of 1 Vulpec- Hans Bode in Hannover again on the 7th. After a ulae by Pa11as. Many occultation observers through- fine outdoor dinner, we got ready for an occultation out western Europe, as well as Prof. Tomita from Ja- of Spica. Hans set up his video camera on a 20-cm pan, were at the colloquium, and I am sorry that I Schmidt-Cass. while Wolfgang Beisker attached his couldn't attend it myself. It provided an opportun- photoelectric photometer to a 25-cm Newtonian re- ity for members of IOTA, IOTA/ES, and GEOS to get flector. Hans had an B-cm refractor, to which we together to discuss some mutual problems, and con- were able to attach my RCA Ultricon camera. A large sider ways for increasing future coordination. The cloud bank in the west threatened us for two hours possibility of holding a future intercontinental before the occultation, but it moved towards us only meetinp. 92 ?. of occultation observers was discussed (see very slowly, with the wind blowing some low clouds from the south. The partly cloudy sky provided dra- ma, but we were lucky; the Moon was in the clear ASTEROIDAL, COMETARY, AND JOVIAN " when Spica disappeared, and all of our equipment OCCULTATIONS DURING 1987 worked, making it perhaps the best-recorded occulta- tion by IOTA/ES. Unfortunately, everyone else that David Id. Dunham I met during the rest of my trip was clouded out that night. This is a continuation of the article started in o.n. 4 (3), 41 and continued on p. 66 of the last This was the last of my six business trips during issue. David Werner prepared all of the finder the first half of 1987. It was two weeks before the charts in this issue, usually annotating charts 1° International Astronomical Union Colloquium No. 98, and 3° on a side that I generated with a computer. "The Contribution of Amateur Astronomers to Astrono- I made a modified version of the A.C. 1° chart pro- my," in Paris. My frequent travelling had put me gram to produce similar charts from combined catalog far behind with many projects, so I decided not to data. Werner and I hope to prepare all or most of go to Paris for the colloquium. But I was already the 1988 finder charts for North America early scheduled to give papers there. Since I knew that enough so that they can be distributed, along with Hans Bode planned to be at the Paris meeting, I gave some of SOma's world maps, with the North American him material for my two presentations while I was in asteroidal occultation supplement (based mainly on Hannover, so that he could read my papers. Edwin Goffin's material) for 1988.

On the 8th (Whit Monday), I trave11ed to Leiden, the A list of priority asteroidal occultations, identi- Netherlands, where I was met by Henk Bulder. Before fied by Robert Mi11is (Lowell Obs.) and Roland Bon- dinner at his home, he showed me his 25-cm reflec- insegna (GEOS), was published in o.n. 4 (3), p. 49. ' tor, with which he timed 268 occultations during one I propose that some other events, listed in the last year, in spite of Holland's bad weather (only about issue, also deserve at least preliminary astrometry, 50 clear nights a year). We then went to Leiden Ob- and should be added to the priority list. These ad- servatory, where we held a meeting on occultations ditional eVents are listed below: ~- attended by about 50 people. I showed some of my videotapes, including the Spica occultation recorded Date Asteroid Star Notes the night before. Henk discussed plans for future grazes, and described observations of two grazes on , Aug 30 247 Eukrate SAD 213992 Dec. -31° consecutive nights early in May. One was the May Nov 13 313 Chaldea BD +4° 1281 Nov 14 7 Iris L 5 3047 Om = 0.3 . 8th(see grazep. 104).of SigmaBut Leonis,in Holland,also theobservedevent occurredin Germany Nov 25 2060 Chiron · Anonymus exactly at sunset. Even so, observers had little Nov 27 336 Lacadiera BD +18° 527 problem seeing the star, and one even videorecorded Dec 11 160 Una SAD 77137 the graze, the first in Europe, as far as I know. Dec 16 250 Bettina SAD 61705 But due to the bright background, contrast was poor, so the graze events are hard to see on the video. Observers are encouraged to monitor all of the pri- ority events that are observable at their locations My flight to Italy landed in Milan, where I was met with predicted miss distances of 3" or less, even if by Marco Cavagna, holding a sign that read in part, no astrometry is obtained to improve the predic- "(3123) Dunham now flying-by Milan." He and a tions. This is not just to check for secondary oc- · friend drove me to the train station, where we had cultations. Uncorrected predictions can have large time for a sandwich before my train left for Turin. errors, and even if you are very close to a path im- In Turin, I met IOTA/ES member Francesco Cerchio, proved with astrometry, we might not be able to no- who was also at the celestial mechanics symposium. tify you in time. Usually, last-minute results are He is the director of the Occultation Section of the obtained less than a week in advance. The only Italian Union of Amateur Astronomers. Francesco practical way to notify a large number of observers Cerchio and workers at the Turin Polytechnic Insti- is by mail, and those in outlying areas have a good tute, which sponsored the symposium, did a great job chance of receiving the mailed notices after the in making my visit to Turin very enjoyable. Both event. When we get a good astrometric update for an Cavagna and Cerchio planned to be in Paris, where event in the U.S.A., I try to telephone as many ob- they could see my graze videotape shown by Bode. servers as possible, but this is time-consuming and 114

expensive, so that often only a few regiond1 coordi- a satellite which is usually several Earth radii nators can be contacted this way. Besides the pri- distant, I needed to modify my occultation search ority events, you are also encouraged to monitor program to generate a list of geocentric appulse da- other observable appulses with predicted closest-ap- ta for all events where the minimum separation was proach distances less than 1", since there is then a less than two arc minutes as seen from the Earth's reasonable chance for an occultation; those with center. distances less than 2" also have some chance and al- so should be considered. I have not heard whether any of Prof. Evans' planned IUE observations were successful, but he did write On p. 69 of the last issue, the angular diameter of thanking me for the predictions. The changes in the Jupter is incorrectly given as 24:'53. The correct computed orbits described above show the great dif- diameter is twice that value. The values for the ficulties in trying to predict occultations by new diameter in km, and the predicted central duration comets, especially to the accuracies needed to see on the previous page, are correct. diming by dust near the nucleus.

None of the occultations by Comet Wilson (19861), The numerous trips that I have made this year, and listed on pages 66 and 67 of the last issue, were other pressing obligations, delayed resumption of my visible from the Earth's surface. I kept in contact work on the 1983 May 29th Pa11as occultation. I be- with Brian Marsden and Daniel Green at the Smithson- gan working on it again only recently, but hope to ian Astrophysical Observatory in Cambridge, MA, to have a manuscript ready for formal publication well keep track of the latest astrometric observations before the end of 1987. I also hope to complete and new orbit determinations of both Comet Wilson analyses of other asteroidal occultations reported and Comet 1987c. As of mid-April, they still had no to IOTA, especially the 1983 Nemausa event, before new observations of Comet 1987c, or of Comet Wilson the Asteroids II meeting that will be held in Tuc- since its conjunction with the Sun, so I telephoned son, AZ, next March. David Herald to ask for Australian help to get crit- ically needed positions of these southern comets. Graham Blow sent me a copy of the 7-page Newsletter By late April, observations of both comets had been No. 3 of the Australasian Asteroidal Astrometric reported to Cambridge by David Herald and by astrom- Group, working under the auspices of I.A.U. Connis- etrists in Chile, allowing Marsdeh to update the or- sion 20'S Working Group on Occultations. The news- bits, which I then used to compute new occultation letter, dated June 26th, "updates asteroidal event predictions. The orbit of Comet Wilson differed by results during the first half of 1987." The news- over 20" in the cross-track direction from the one letter documents vigorous activity by astrometrists that I used for the predictions in the last issue, and observers in New Zealand and Australia, discus- and that for Comet 1987c changed by a large fraction sing in detail astrometry obtained by the Black of a degree from the first orbit that I had used for Birch, Perth, and Lowell observatories for five ap- that comet for predictions computed in March. pu1ses, one (511 Davida on March 16th) that resulted Around May lst, I sent the updated predictions for in the first videorecording of an asteroidal occul- urgent events to regional coordin'ators, most of them tation from Carter Observatory in Wellington, and in the Southern Hemisphere. In early May, I was in another (Hermione on March 26th) that may have pro- Tokyo on business, and took the opportunity to de- duced a long dimning (like the "cloud" of particles liver a magnetic tape with the new occultation data around Pa11as proposed by Russian astronomers, see to Mitsuru SOma, who generated world maps for the o.n. 3 (8), p. 167). Coordinator Graham Blow closes events. In mid-May, I sent copies of the maps and with a sad note: "I think we are all aware that predictions for events, primarily in late May and Perth (Observatory) is currently facing closure. june, to regional coordinators in the appropriate Perth has been a highly active contributor to the network, and it would be a great loss if their input areas. Around May 20th, new orbits for both comets were issued by Marsden, and I updated the predic- was removed. Carter Observatory's future is also tions again. Again, the new orbits showed that the under threat, the observatory having effectively run previously distributed Occultations either were not ' out of money and now being subject to a funding and visible at all from the Earth, or took place far organisational review." It will indeed be unfortun- from the regions to which I had sent predictions. I ate if any more Southern-Hemisphere observatories - distributed a last round of predictions for the few engaged in astrometric observations follow the clos- remaining events to regional coordinators in late ures of the Republic and Sydney observatories. Per- haps considering this situation, and the difficulty May. Two of the events were potentially visible from the U.S.A. and Europe, one perhaps from Florida of asteroidal occultation astrometry in general, the and one possibly from southern Europe, but the group should add "Research" between "Astrometric" chances were not large. and "Group" to provide an appropriate acronym! ._ CV ·r This activity was partly the result of a request to D · W ~ Don Yeomans of the International Halley Watch for ' " ' ""-' i '% " ! · " . ·'7 "?1,'?· " , % °:· .'" ' ".0 . 8 D (J D UDd -DD am 2" dO . Wilsonpredictionsto earlyof occultationstype stars byandProf.appulsesNye Evansby Cometat the Oi " :', ' ,0'. " , "i .: g' 0 °OO y () ° : University of Keele in England. He wanted to ob- ' """ "" , i cb d o—g-cr g) ' " a serve some of the better appulses with the IUE sat- :k: ' '" 'b, "' :' ! "3 ° jo° " j: ' " ellite, and coordinate the observations with ground- °% U\ D Ej O G m ; based observations of the same events. Don sent the .· ' %, , .,· ! . , -J G, request to Lowell Observatory, where Ted Bowell " : t . ·· 'i . O D OOO "' bn . 0 . rj .. apologized that his software could not handle hyper- " t QC8 "'® '· 47y~—0. " 2_«°;_:_n_:b,p :· ? bolic orbital elements input, and asked if I could

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A2257333 by Ophelia 1987 Dec 1 Anonymous by Ophelia 1987 Dec 1 +21°1371 by Ludmilla 1987 Dec 2

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SAD 61705 by Bettina 1987 Dec 16

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SAD 109103 by Athor 1987 Dec 20 L 2 3421 by Metis )987 Dec 25 SAD ]89335 by Venus 1987 Dec 25

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