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V/46        Classical (Evolved) Algol-Type Binary Candidates (Budding 1984)

A Catalogue of Classical (Evolved) Algol-Type Binary Candidate Stars Budding E. <CDS Bull. No. 27, p. 91 (1984)> =1984BICDS..27...91B
ADC_Keywords: Binaries, eclipsing Description: A catalogue of some 414 classical Algol-type binary candidates is presented. Apart from the entries on numerous well-known and studied Algols, the catalogue draws attention to a large number of probably similar but generally less well-known stars, as well as others which may have been cited as possible Algols, though for which the overall evidence appears weaker. Acronyms used: BD = Brancewicz and Dworak (1980) (catalog II/150) GM = Giuricin and Mardirossian (1981a) GCVS = General Catalog of Variable Stars II/139 File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 86 528 The Catalogue remarks.dat 80 568 Remarks
See also: II/139 : General Catalog of Variable Stars (GCVS), 4th Ed. (Kholopov+ 1988) II/150 : Parameters for eclipsing binaries (Brancewicz+, 1980) J/A+A/417/263 : Catalogue of Algol type binary stars (Budding+, 2004) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID [1/414]+= Serial number of entry. 4 A1 --- Cont [+] indicates a continuation of NEXT star 5- 13 A9 --- name *Name of star 16- 24 F9.4 d Per ? Period 27- 31 F5.2 solMass mass *? Mass of the primary star 32 A1 --- u_mass [?] Uncertainty remark on mass 35- 46 A12 --- Sp *Spectral Type 49- 52 F4.2 --- q *? Mass ratio quoted by BD 55- 57 I3 % subVol *? Subgiant volume / Roche volume 58 A1 --- u_subVol [?] Uncertainty remark on subVol 60 A1 --- l_qsd [<≳?] Limit or approximate flag on qsd 61- 64 F4.2 --- qsd *]0/1]? Calculated mass ratio 65- 67 A3 --- n_qsd Remark on qsd 69 A1 --- l_Depth1 [>] Limit flag on Depth1 70- 73 F4.2 mag Depth1 *? The importance of depth of primary minimum 74- 75 A2 --- n_Depth1 [pvVB?] Passband (as in GCVS). 78- 82 F5.3 --- r1 *[0/1[? Relative radius of primary 84- 86 F3.1 --- sd *]0/1[? sd status
Note on name: Arranged in alphabetical order of constellation listing (as in the General Catalogue (GCVS) of Kukarkin et al., 1969, 1970, 1971,1974) Note on mass: The mass as given in the catalogue of Brancewicz and Dworak (1980) (hereafter BD), to two decimals. Sometimes an additional entry (above the BD mass) refers to some other recent estimates. This will usually be for the more well known Algol systems, the mass being that quoted by Giuricin and Mardirossian (1981a) (hereafter GM). Note on Sp: The MK spectral type(s) (when available) are almost always those of BD. A colon indicates uncertainty, while brackets refer to types which have been indirectly inferred by certain other light curve analysts (see BD for details).A few of the candidate stars are not listed by BD, in which case the types are probably those quoted by Kukarkin et al., (GCVS - op. cit.) or Wood et al.,(1980). Note on q: For many systems this comes from an initial trial value which is subsequently iteratively improved on, in order to make the system parameters (especially those of the primary star) fit in the prescribed correlations (see section 2 of the publication) to within some permitted tolerance. Note on subVol: subVol (r(L2)) indicates BD's assessment of the volumetric percentage proportion of its limiting (Roche) lobe occupied by the subgiant component. In a majority of cases of candidate EA2 systems BD find this quantity to be less than 100 (i.e. an "undersize" implication). This could, however, reflect systematic errors of some adopted constant values in some of the formulae put together in order to effect solutions (Budding, 1983). In any case, the proximity of r(L2) to 100 is a good clue to the likelihood of an SD (semi-detached) system designation. Note on qsd: The quantity q(SD) would usually denote the mass ratio calculated using BD's relative radius of the secondary component (R(2)/Sep), a quantity already determined in the light curve analysis as r(2), and Kopal's (1959) Table (3-2), which relates the mean relative radius of the component in an sd system, i.e. one which is in contact with its surrounding (inner) Roche critical surface (passing through the inner Lagrangian point), to the corresponding mass ratio. Again, as with the entries in mass, additional recently published values are sometimes also included above the main entry for more well known systems. Other possible entries for q(SD) will be referred to in the next section. Note on Depth1: For certain eclipsing binary systems, that this is a salient observational parameter, by means of which likely sd candidates may be identified, was already stressed in Shapiro's (1973) thesis. This quantity was utilized by Budding (1981) to select light curves of EA2 type. It will indeed become clear on inspection of the candidate list that most of the more well known classical Algol systems have light curves of this type. The value of the depth is given in magnitudes. Note on r1: The tenth column gives the relative radius of the primary component r(1), which is simply derived from (R(1)/Sep) as listed by BD. Like the previously mentioned r(2), this is a quantity which would normally be calculated from analysis of the photometric data, and though published results of such analyses often quote its value to three or more significant decimal digits, a two digit value is already an optimistic assessment of the likely information content for the majority of less well-known candidate stars. The extent of disagreement between different sources on such parameters for even the more well-known examples suggests that a two figure number is a realistic datum to insert here. This quantity can, of course, be combined with the mass, mass ratio and the period to allow absolute sizes of the system components to be derived. Note on sd: The sd status could be regarded as a crude probability assessment of the semi-detached nature of the system. It takes the five values from 0.1 up to 0.9 in steps of 0.2. 0.9 will normally be placed alongside the well-known cases (such as most of those in the GM list), for which comparison information columns (4) and (8) is presented. A value 0.7 is associated with binaries of apparently similar superficial properties to the 0.9 cases, but such binaries appear to be relatively neglected. 0.5 goes with the binaries for which an EA2 or EA1 designation might be about equally likely, whereas the balance of probability would seem to be against a normal sd classification for the 0.3 systems. Those binaries with sd status 0.1 are regarded as definitely unlikely to represent classical evolved Algol systems.
Byte-by-byte Description of file: remarks.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID [1/414]+= Serial number of entry. 5- 13 A9 --- name *Name of star 17- 18 A2 --- ref *Reference to most recent well-known catalog 22 A1 --- l_Q [<] Less than sign 23- 25 F3.1 --- Q *? Quality description 32- 80 A49 --- rem *Remarks
Note on name: The name is blank for continuation lines Note on ref: K Koch et al., (1970) S Svechnikov, (1969) T Tchudovichev, (1952) G Gaposchkin, (1940) Note on Q: The above sources usually refer to the quality of the original photometric data, or give some (numerical) indication as to their feelings of the overall reliability of their solutions. This has been put together here under the general quality descriptor Q, which may be interpreted in a similar way to the sd status measure, except that (since Svechnikov's `weights' are in a scale of 1-10) the values 0.2, 0.4 etc. might also appear. Note on rem: The remarks column offers a few words of additional information. In order to appreciate these, however, it will be necessary to understand the following abbreviations: BD The catalogue of Brancewicz and Dworak (see(4) above). C Cester et al. (1978b). EA Algol type light curve as defined by Kukarkin et al., (1969). EA1, Subdivisions of the EA type designation introduced EA2 by Budding (1981). EA1 refers to a pair of eclipsing unevolved Main Sequence dwarfs, giving rise to a light curve sometimes described as being of `Algol type'; though often with distinctive differences from that of an EA2 type system, which refers to evolved Algols forming the main subject of this article. G Gaposchkin's(1940) catalogue (see(12) and(13) above). GM Giuricin and Mardirossian (1981) (see(4) above). HN Hall and Neff (1979). k Ratio of relative radii (usually r(2)/r(1)). lc Light curve. mf Mass function. min Photometric minimum (Min II refers to the depth of the secondary minimum.). oc Occultation, i.e. eclipse formed by the larger star obscuring the smaller one. q Ratio of masses (i.e. M lesser/M greater = M(2)/M(1)). RS A system containing an "undersize" subgiant. Special attention was called to these systems by Kopal (1959) and also (using the same designation, though with a slightly more restricted meaning, by Svechnikov (1969). Many systems of this type have since been found to conform to a special RS CVn-type designation (Hall, 1976); Morgan and Eggleton, 1979). Svechnikov (1969) described these as AR systems. The issue will be discussed further in the next section. Sz Szafraniec (see (12) and (13) above.) Her gathered information on photometry is often of interest in connection with less well-known candidates. sd Semi-detached, in the sense of Kopal (1955). sec Secondary. tr Transit, i.e. eclipse formed by the smaller star obscuring the larger one.
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(End) Julie Anne Watko [SSDOO/ADC], Francois Ochsenbein [CDS] 11-Jun-1996
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