Binorbit.dbf is a disabled version of data contained now on NSDAC/SAC CD-ROM. The conversion into *.dbf took place from an older version of these data, and I do not have the source data nor my conversion algorithm any more. The dBase file is meant almost only as an input into our programme Tr_Bin computing and showing trajectories of binaries. It does not contain full original information. Coordinates of stars are mostly missing here, and the original file with notes to individual fixed stars cannot be used therefore and is not included in the archive. The contents of the dBase file is explained in another dBase file, BinOrbi_.dbf (or BinOrbc_.dbf, in Czech). Please buy the NASA CD-ROMs to have the full information. Jan Hollan, N. Copernicus and Planetarium in Brno 1996-12-02 INTRO.DAT from the CD-ROM follows: FOURTH CATALOG OF ORBITS OF VISUAL BINARY STARS C.E. Worley and W.D. Heintz INTRODUCTION This catalog continues the series of catalogs of visual binary orbits previously published by W.S. Finsen (1934, 1938), C.E. Worley (1963), and jointly by Finsen and Worley (1970). The combination of the independent resour- ces and opinions of two authors results, we believe, in a more complete, accu- rate, and consistent catalog. The Finsen-Worley Catalog, supplemented by all subsequently published orbits known to us, formed the basis for the present compilation. During the past decade, practically all stars having visual orbits have been observed, often repeatedly, either by us with micrometers at Washington, Swarthmore, and Cerro Tololo, or by H. A. McAlister with the speckle interferometer at Kitt Peak. This new data, combined with the extensive data now resident in the ob- servation catalog maintained at the U. S. Naval Observatory, provides a firm basis for judging the quality of the visual orbits. In each instance, orbital residuals were computed for all significant observations by the aid of a desk- top computer. In numerous cases we have investigated whether the most recent elements were satisfactory, and whether they provided a distinct improvement over earlier and also satisfactory solutions; orbits predating the entries in the 1970 catalog were also frequently examined. Nevertheless, there remain cases where it has been impossible to choose between several orbits of the same pair; in such instances both orbits are listed. The spread of hand calculators and desk-top computers has obviated the need for publication of the Thiele-Innes constants, which are therefore no longer listed. As in the Finsen-Worley catalog, we continue to list astrometric solutions, but we have now restricted their inclusion to those cases considered relatively certain. Dubious astrometric solutions, along with other orbits re- jected for various reasons, are listed in a brief "for-the-record" list in Table 1, which also tabulates the reason for rejection, R. In particular, per- iods over 4000 years and hyperbolic solutions have been rejected as being too unreliable. The few parabolae which had remained in the 1970 catalog have been replaced by elliptic elements. Except for five Hopmann orbits for which refer- ences are given in the table, all references to rejected orbits may be found in the Finsen-Worley catalog. Table 1. ORBITS REJECTED FROM THE CATALOG R.A. Dec. ADS Name R Author 00307+2927 497 STF 42 1 J.Hopmann, 1967. 01226+8846 1477 Alpha UMi 7 A.Wyller, 1957. 01315-3025 HJ 3447 3 S.Arend,R.F.Mourao, 1968. 02208+6657 1860 Iota Cas Aa-C 1 J.Hopmann, 1960. 02472+5251 2202 Tau Per 7 P.van de Kamp,S.Andersen, 1969. 04298+4104 58 Per 8 A.Wyller, 1957. 04548+4341 Epsilon Aur 7 K.Strand, 1959. 06491+3018 5570 STF 981 2 J.Hopmann: Mitt. Wien Nr. 7, 1971. 08032+3231 6623 STF 1187 2 J.Hopmann: Mitt. Wien Nr. 7, 1971. 09365+7632 Ross 434 8 H.Alden, 1951. 10142+2022 +20 2465 8 D.Reuyl, 1943. 10579+3638 +36 2147 8 S.Lippincott, 1960. 11056+3100 8083 STT 231 1 J.Hopmann, 1960. 11084+2041 8094 STF 1517 2 J.Hopmann: Mitt. Wien Nr. 5, 1970. 11217+0333 8162 STF 1540 2 J.Hopmann, 1960. 12106-2248 8481 BU 920 3 A.Bespalov, 1961. 12255+1016 8575 STF 1647 2 J.Hopmann, 1964. 13118+1733 8841 BU 800 1 J.Hopmann, 1960. 13499+1854 Eta Boo 7 Z.Daniel,K.Burns, 1939. 14516-2058 9446 H 28 1 J.Hopmann, 1967. 14542-2136 -21 4009 8 H.Alden, 1938. 14560-0342 9476 A 14 5 J.Hopmann: Mitt. Wien Nr. 14, 1973. 16086+1348 9969 STF 2021 2 J.Hopmann, 1964. 17334+1837 Ci 18,2347 8 G.Bieger, 1964. 17370+6826 Ci 18,2354 9 S.Lippincott, 1967. 17529+0425 Ci 20,1069 9 P.van de Kamp, 1969. 18140-6132 Gale 2 7 H.Alden, 1946. 19039-1958 12096 B 427 6 N.Voronov, 1934. 20154-1506 Beta(2) Cap 9 H.Alden, 1936. 21068-1524 14736 H 47 2 J.Hopmann: Mitt. Wien Nr. 17, 1974. 21514+3821 15454 A 1449 4 P.Baize 21538+6309 VV Cep 7 L.Fredrick, 1960. _________________________________________________________________________ KEY TO REASONS FOR REJECTION R = 1 Hyperbolic orbit. 2 Period over 4000 years. 3 Orbits completely faulty and irreparable. 4 Rescinded by the author (omitted from publication). 5 Optical pair. 6 Probably not double. 7 Amplitude below noise level. 8 Not confirmed by subsequent observations. 9 Objects still suspected to be binary by some, but no even approximately reliable or complete elements yet available. _________________________________________________________________________ Combined magnitudes were selected in the following order of preference: (a) Photoelectric V magnitudes taken from various sources. (b) Photometric visual magnitudes (two-decimal) from the Henry Draper Catalogue. (c) Durchmusterung magnitudes corrected to the Harvard system. (d) Uncorrected Durchmusterung magnitudes, plus a few values from miscellaneous sources. Because the binaries included in this catalog are generally close pairs, determination of individual photoelectric magnitudes for the components is im- possible in most instances. For these cases one must know the difference of magnitude in order to assign the individual magnitudes. In many cases photo- metric determinations of magnitude difference were found, obtained by a variety of techniques. In other cases visual estimates were used, emphasizing, where possible, recent estimates made by experienced observers using large tele- scopes. The magnitudes so derived are given in the catalog as follows: (a) If there are individual photoelectric magnitudes, or a photo- electric combined magnitude and photometric difference of magnitude, then two-decimal values are given for both com- ponents. (b) In all other cases, one-decimal values are given. Spectral types are given in the following order of preference: (a) MK (Yerkes) types, taken from various sources. Values follow- ed by an asterisk have been classified by Christy and Walker (1969). For these cases the procedure was to observe the com- posite spectrum and to infer the individual spectral types from the known magnitude difference. While this procedure is open to several objections, the ordinary practice of quoting only a single spectral type is also flawed. (b) Mt. Wilson types. (c) Henry Draper types. The orbital elements are listed according to the definitions set forth in the Introduction to the 1970 catalog, or, for instance, by Heintz (1978). In a few cases the elements given by the original author have been rewritten in compliance with these conventions. Also in a few cases, the elements have been rounded when the author gave more than three decimals in the dynamical, and more than two in the angular elements; otherwise the decimals are as given in the original paper, and therefore their number has no relation to the degree of reliability. The orbits have been graded into five classes on a scale of 1 (definitive) to 5 (indeterminate). The grade assigned to an orbit takes into account the length and curvature of the observed arc, the number, distribution, and consistency of the observations, and (most importantly) also the size and distribution of the residuals. An approximate guide to the criteria used is given below: Grade 1 Definitive Well-distributed coverage exceeding one revolution; no revisions expected except for minor adjustments. 2 Good Most of a revolution, well observed, with sufficient curvature to give considerable confidence in the de- rived elements. No major changes in the elements likely. 3 Reliable At least half of the orbit defined, but the lesser coverage (in number or distribution) or consistency of the data leaves the possibility of larger errors than in Grade 2. 4 Preliminary Individual elements entitled to little weight, and may be subject to substantial revisions. The quantity (3loga - 2logP) should not be grossly erroneous. This class contains: orbits with less than half the ellip- se defined; orbits with weak or inconsistent data; orbits showing deteriorating representation of recent data. Many of the Grade 4 cases could be called pre- mature, as higher-grade solutions may be attainable with additional data before long. 5 Indeterminate The elements may not even be approximately correct. The observed arc is usually too short, with little curvature, and frequently there are large residuals associated with the computation. It may be noted that, aside from the period, other elements have a se- lective influence on the grade, in particular high eccentricities and/or in- clinations which limit the positionally observable arc, thus rendering a high- grade solution more difficult to obtain. In cases where the difference of magnitude is small and there is doubt regarding the quadrant interpretation, so that two or more widely differing sets of elements are possible, the ambiguity is indicated by the symbol A pre- ceding the grade. For example, for ADS 450 (A 111) two solutions have been of- fered with periods of 10.755 and 21.30 years, each graded A3, and each grade being assigned on the assumption that the ambiguity has been resolved. (Thus these grades do not indicate if and which one of the alternatives is more likely). In a few cases the possibility of ambiguity has been indicated even though the alternative interpretation has not been tested by orbit computation. DESCRIPTION OF THE CATALOG Table 2 lists the orbit catalog, where most of the data presented are identifiable by the column headings. Each orbit requires two lines of data ar- ranged in 11 columns. A brief explanation of the items follows: Column 1 line 1 The Right Ascension for 1900. 2 The name(s) of the star, and the components involved. 2 1 The Declination for 1900. An asterisk following this value indicates a Note. 2 (Continuation of the name, or components, if necessary). 3 1 The ADS number. 2 (Continuation of the name, or components, if necessary). 4 1 The magnitude of component A. 2 The spectral type of component A. 5 1 The magnitude of component B. 2 The spectral type of component B. An asterisk following this value indicates that the spectral types have been inferred from a combined spectrum and a known magnitude difference, as previously discussed. 6 1 The period in years, P. 2 The time of periastron passage, T. 7 1 The semi-major axis, a, in seconds of arc. 2 The eccentricity, e. 8 1 The inclination, i. 2 The longitude of periastron (omega) reckoned from the node as listed. 9 1 The node (OMEGA). An identified ascending node is indicated by an asterisk following the value. 2 The equinox (if any) to which the node refers. 10 1 The grade, as previously discussed, followed by the date of the last observation used in the computation, when known. 2 Inclusive dates for which an ephemeris is given by the author. 11 1 The computer of the orbit. 2 The reference. The notes following the catalog are mainly concerned with multiplicity, variability, and spectroscopic motions or sub-motions. The closing date for this catalog is 1 July, 1982. It contains 928 or- orbits of 847 systems (counting triples as two systems). There are 23 orbits of unresolved systems. Of the non-ambiguous orbits, 62 are grade 1, 118 grade 2, 263 grade 3, 266 grade 4, and 131 grade 5. ACKNOWLEDGMENTS We are particularly indebted to G.G. Douglass and J. Woodbury for their important programming help on this project. We also owe a debt of gratitude to Dr. Wayne H. Warren Jr. of the National Space Science Data Center, who inter- rogated his extensive data files to provide us with many magnitudes and spectral types. The second author acknowledges support by the National Science Foundation REFERENCES Christy, J.W., Walker, R.L. 1969 Pub. Ast. Soc. Pacific 81, 643. Finsen, W.S. 1934 Union Obs. Circ. 4, 23. 1938 Ibid. 4, 466. Finsen, W.S., Worley, C.E. 1970 Republic Obs. Circ. 7, 203. Heintz, W.D. 1978 Double Stars. D. Reidel Co., Dordrecht. Worley, C.E. 1963 Pub. U.S. Naval Obs., 18, pt.3.