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V/46 Classical (Evolved) Algol-Type Binary Candidates (Budding 1984)
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A Catalogue of Classical (Evolved) Algol-Type Binary Candidate Stars
Budding E.
<CDS Bull. No. 27, p. 91 (1984)>
=1984BICDS..27...91B
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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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 86 528 The Catalogue
remarks.dat 80 568 Remarks
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See also:
II/139 : General Catalog of Variable Stars (GCVS), 4th Ed. (Kholopov+ 1988)
II/150 : Parameters for eclipsing binaries (Brancewicz+, 1980)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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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
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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.
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Byte-by-byte Description of file: remarks.dat
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Bytes Format Units Label Explanations
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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
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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