1 AN And. Photometric and absolute elements are not reliable. The both
  1  components have considerable excess radii for their masses.
  3 V805 Aql. The both components (especially primary) have considerable
  3  excess radii for their masses.
  4 Sig Aql. Obtained elements aren't very reliable.
  5 V539 Ara. System has a gaseous streams; the depth of Min I changes with time
  7 AR Aur. According to Nordstrom, Johansen (1994A&A...282..787N) a secondary 
  7  component is stay that is before ZAMS. The system belong to Aur OB I 
  7  association.
  8 EO Aur. Photometric elements and mass ratio of components have been found
  8  roughly.
  9 HS Aur. Elements are very reliable.
 11 ZZ Boo. Both components have considerable excess radii for their masses.
 13 SZ Cam. The third light (L3=30%) is the binary system. Evolutional status of
 13  system is not very evident. Photometric elements aren't reliable. Light 
 13  curve is very variable from season to season; perhaps, the system has 
 13  gaseous streams. There is a near visual satellite, B0 star which has 
 13  approximately the same brightness as the eclipsing system at a distance 
 13  18". Visual satellite (ADS 2984A) is likely to be the binary system that is
 13  why it is a sextuple system. Accrording to Kholopov, 1958, Kraft, Landolt, 
 13  1959ApJ...129..287K, this system is the member of the very young open 
 13  cluster NGC 1502 near the center of which that system is. Budding 
 13  (1975Ap&SS..36..329B) notes the existence of absorbing substance around the
 13  system.
 14 TU Cam. Eclipses are very small; gaseous streams distort light curves;
 14  photometric elements and mass ratio of components have been found roughly,
 14  primary component has considerable excess of radius for its mass.
 15 AN Cam. Photometric elements are very unreliable.
 16 AS Cam. Light curves are asymmetric out of eclipses; there are evident form
 16  changes of light curve in time. Probably, there is a gaseous substance in
 16  the system. Mass ratio of components is evaluated unreliably.
 19 EM Car. Elements are very reliably.
 21 YZ Cas. Elements are very reliably.
 22 AR Cas. Eclipses are very small. Photometric elements and mass ratio of
 22  components has been found roughly. There is a near visual satelite
 22  (at a distance 1").
 23 CC Cas. It is likely to be the member of Cam OB I association.
 26 SZ Cen. Both components have considerable excess of radii for their masses.
 27 V346 Cen. The primary component has considerable excess of radii for
 27  its mass.
 28 WX Cep. The primary component has considerable excess of radius for its
 28  mass and the secondary component has the excess of radius, too. Probably,
 28  there are gaseous streams in the system.
 29 ZZ Cep. Photometric elements weren't estimated reliably. Secondary
 29  component has considerable excess of radius for its mass. Probably,
 29  there are gaseous streams in the system.
 30 AH Cep. Probably, there is the third body in a system. There is a gaseous 
 30  substance in the system.
 31 CW Cep. Photometric elements aren't reliable. According to Botzula R.A.
 31  (1978, Izv. Astron. Obs. Engel. 44, 70), the primary component is 
 31  surrounded by rare gaseous envelope. It is a young system; It is a member 
 31  of Cep 0B III association.
 32 EI Cep. Both components have considerable excess radii for there masses.
 33 EK Cep. According to Popper (1987AJ.....93..672P) the secondary component is
 33  the star on pre-main sequence stage.
 34 NY Cep. Photometric elements aren't very reliable. Secondary minimum
 34  lacks because of the big eccentricity of the orbit.
 36 XY Cet. Both components have considerable excess of radii for their masses.
 37 RS Cha. At least, one of system components is a physical variable
 37  (perhaps, Del Set type). Both components have considerable excess of radii
 37  for their masses.
 38 RZ Cha. Both components have considerable excess of radii for their masses.
 39 TY CrA. Eclipsing pair is a member of the triple system 
 39  (M3~(2.4+/-0.5)M_{sun}_).  The second component (satellite) is likely to be
 39  on pre-main sequence stage (Casey et al., 1995AJ....109.2156C). According 
 39  to data of Vitrichenko E. A. and Shevchenko (1995PAZh...21..434V), the 
 39  secondary component in eclipsing pair is surrounded by dust envelope it 
 39  leads to excess of its radius. The system TY CrA and reflective nebula 
 39  illuminated by it are members of CrA 1 association.
 40 alf CrB. Eclipses are very small. Photometric elements have been computed
 40  not very reliably. The system is likely to belong to the moving cluster UMa
 42 MR Cyg. Components mass ratio was estimated from spectroscopic observations
 42  not very reliably. System is very cramped, although it is detached.
 42  Early values of the spectrum of system primary component were estimated
 42  approximately as AO, however R. H. Hardie (private information mentioned in
 42  the paper of Batten, 1967PDAO...13..119B) noticed that really this spectrum
 42  is much more early: B3V; all later determinations (spectral and 
 42  colorimetric) confirm this evaluation.
 43 MY Cyg. Both components have some excess of radii for their masses.
 43  According to Popper, 1971ApJ...169..549P, both components are Am-stars.
 44 V380 Cyg. Depths of minimums are very small; obtained photometric elements
 44  are very unreliable. More massive component has considerable excess of
 44  radius for its mass. Probably, it is surrounded by extended gaseous
 44  envelope (Batten, 1962PDAO...12...91B; Leushin, Snezhko, 
 44  1981Ap.....17..315L), as a result its dimensions, estimated from 
 44  photometric observations, can be exceeded, and its spectrum can belong to 
 44  brightness class III.
 45 V442 Cyg. Elements are very reliable.
 46 V453 Cyg. The system likes V447 Cyg, V448 Cyg. It is in the region of the
 46  young open cluster NGC 6871; the system can be cosidered as the physical
 46  member of this cluster. The both components are on G-R diagramm near the
 46  turn point of the cluster.
 48 V478 Cyg. The system is bright component of visual-binary system APS 13711;
 48  visual satellite is at a distance 3.3". The system is likely to belong
 48  to Cyg II.
 50 V1765 Cyg. The radial velocities curve of secondary componentt and the
 50  masses ratio of components aren't very reliable.
 52 BH Dra. Photometric and spectral elements aren't very reliable. The mass
 52  ratio of components is estimated approximately. The system is bright
 52  component of visual-binary system ADS 18919. Visual satellite is at
 52  a distance 10".
 54 CM Dra. It is eclipsing variable system with the least known masses of
 54  components. Because of spots activity it is obtained a sinusoidal
 54  vibrations of brightness ~0.01", rarely in the system happens a 
 54  considerable outbursts. It is proposed, that CM Dra is a member of type II
 54  of stellar population. CM Dra is the one of the nearest to us eclipsing
 54  stars.
 55 DE Dra. The secondary minimum isn't discovered in light curve, because
 55  brightness and sizes of the secondary are very small. A phorometric
 55  element hasn't been found surely. There is no spectoscopic and photometric
 55  data about the secondary star. But, from computed values of mass and radius
 55  of secondary component we can expect that the secondary is the late
 55  F- or G-star.
 56 CW Eri. Phorometric elements aren't very reliable.
 57 YY Gem. It is one of the most active dMe-stars with large x-ray emmision.
 57  Changes of light curves out of eclipses are explained by spots activity.
 57  It has a photometric and spectroscopic evidences of present a gaseous
 57  matter (possibly a gaseous stream) in the system. Brightness of system
 57  feels a short-time outbursts, which amount to 1" in filter U. YY Gem is
 57  the member of a multiply Castor system (ADS 6165) Castor C. A brighter
 57  component Castor A is at a distance 77", components A and B also are
 57  the binary.
 58 RX Her. It is possible presence of diffuse gaseous matter in the system.
 59 TX Her. There are irregular vibrations of brightness out of eclipses.
 59  In a primary munimum a light curve is asymmeric; to all appearance the
 59  system has a gaseous matter.
 61 HS Her. The light curve is strongly distorted at phases 0.5-0.7, to all
 61  appearance because the system has gaseous matter (Botzula, 1984, 
 61  Izv, Astron. Obs. Engel. 48, 15; Hall & Hubbard, 1971PASP...83..459H). 
 61  Mass ratio has been estimated rougly.
 62 V642 Her. Primary component has considerable excess radius for its mass.
 62  The system is the considerable evolved from initial point of main sequence.
 62  According to (Zissel, 1972AJ.....77..610Z) the both components are Am-stars
 63 V819 Her. The eclipses are very small. The system is the spectral triple.
 63  The third component is brighter than eclipsing pair. Spectrum of the third
 63  component is the G8 IV-III with emission in H and K of CaII.
 66 AI Hya. The both components have considerable excess radii for their masses.
 66  Bigger, more massive and less hot component is the variable 6 Set type.
 68 KW Hya. Primary component have considerable excess radius for its mass.
 69 chi2 Hya. Primary component have considerable excess radius for its mass.
 71 CO Lac. According to Botzula (1981, Izv. Astron. Obs. Engel. 47, 19; 1984, 
 71  Izv. Astron. Obs. Engel. 48, 15), it is possible, there is diffuse gaseous 
 71  matter in the system.
 72 EN Lac. The depth of the secondary minimum is very small; therefore a 
 72  spectrum of the secondary star has been estimated very indefinitely. 
 72  Primary component is the physical variable {beta} Cep type. The mass ratio 
 72  of components has been estimates roughly.
 73 TX Leo. The eclipses are very fine; obtained photometric elements aren't
 73  very reliable. The both components have considerable excess radii for their
 73  masses. The mass ratio and elements founded from they aren't very reliable.
 73  The system is the bright component of visual binary ADS 7837; visual
 73  satellite is at a distance 2.4".
 75 RR Lyn. Both components have considerable excess radii for its masses.
 75  Main component is Am-star.
 76 FL Lyr. It is possible, this system has gas matter that causes distortion
 76  light curves.
 77 V478 Lyr. Main minimum has small depth, secondary minimum isn't discovered
 77  on brightness curve. Satellite spectrum was evaluated approximately.
 77  Primary component has spot activity.
 78 TZ Men. Elements are very reliable.
 79 UX Men. Elements are very reliable.
 80 RU Mon. There is the third body in the system that has mass 2.2M_{sun}_ and 
 80  period 67.6 years.
 82 IM Mon. The eclipses are very small. Photometric elements are not reliable.
 82  The system is very cramped.
 83 U Oph. The system is likely to have gas streams that are responsible for
 83  peculiarity on light curve (Popper, 1978ApJ...220L..11P).
 84 WZ Oph. Minima are almost equal in depth and shape. The eclipses are almost 
 84  tangent.
 85 VV Ori. It is very cramped massive DMS-system. There are streams of gas in
 85  the system according to photometric and spectroscopy data (Duerbeck, 
 85  1975A&AS...22...19D). W Ori is spectral-triple system that has very short
 85  period of rotation around gravity centre of triple system: according to
 85  (Duerbeck, 1975A&AS...22...19D) P=199 days. The third component is 
 85  invisible photometrically. Budding, Najim, (1980Ap&SS..72..369B) shows that
 85  the system is connected with "Belt-subgroup" of association Ori I.
 88 V1031 Ori. The system is triple. P1=3500-3700 years. More massive and
 88  larger component is a bit colder than satellite. The third component at
 88  a distance 0.164".
 89 del Ori A. The evoluation of photometric elements presents a large
 89  difficulty since the eclipses are very small, curve light is distorted and
 89  asymmetrical; at least one component is physical variable. Del Ori A is a 
 89  very cramped parted system with both components that greatly were evolved
 89  from FMS. Del Ori A is a bright component of visual triple system ADS 3144.
 89  Very close satellite of almost the same brightness as eclipse system is
 89  discovered at a distance 0.15" from Del Ori A (Heintze, 
 89  1980ApJS...44..111H). Del Ori A belongs to "Belt-subgroup" of 
 89  association Ori I.
 90 eta Ori. The eclipses are very small. Eta Ori is a multiple system, 
 90  brightness component of which is spectral-triple (Waelkens & Lampens, 
 90  1988Ap&SS.142...99W).
 91 BK Peg. The both components have considerable excess of radii for their 
 91  mass. The less massive component is a bit hotter than more massive 
 91  component.
 92 EE Peg. Absolute elements are very reliable. EE Peg is spectral-third system
 92  0.3M_{sun}_<M_{star}_<0.7M_{sun}_, P1 = 1464 days. Primary component is
 92  Am star.
 93 AG Peg. The system isn't stationary and it has signs of diffusive substance 
 93  existence (Botzula P.A., 1984, Izv. Astron. Obs. Engel. 48, 15). AG Peg is 
 93  a bright component of visual triple system ADS 2990. The nearest visual 
 93  secondary component is at a distance 0.96". The system belongs to 
 93  OB-association Per II (Blaauw (1952BAN....11..405B) and Seyfen et al.
 93  (1960ApJ...132...58S)).
 95 V467 Per. The eclipses are very small, the system is really ellipsoidal
 95  variable. Photometric and absolute elements aren't very reliable.
 96 zet Phe. Zeta Phe is a bright component of visual triple system;
 96  visual secondary component is at a distance 0.6" and 6.4".
 97 PV Pup. The system has variable brightness starting with P~1.92 days,
 97  different from orbital. The cause of this variable brightness isn't
 97  evident. The light curve form in the maximum and in the secondary minimum
 97  changes. The visual double ADS 6348, in which PV Pup is feeble part makes
 97  visual and not physical pair.
 98 TY Pyx. The both components are almost equal in size and surface
 98  brightness and they have outstanding excess of radii for their masses.
 98  Popper, 1969BAAS....1..257P, discovered emission lines H and K CaII in the 
 98  system spectrum that belong to both components. Both components are likely 
 98  to be near the point of leaving the main sequence.
 99 VV Pyx. More feeble visual secondary component is observed at a distance
 99  0.3" of eclipsing pair.
100 V1647 Sgr. The system is likely to have feebler visual secondary component.
102 V906 Sco. Both components have considerable excess of radii for their
102  masses. V906 Sco is a physical part of open clump NGC 6475 and it belongs
102  to the brightest stars of this clump.
103 AL Scl. Primary component has outstanding excess of radius for its mass.
104 EG Scr. Photometric elements and radii of components aren't evaluated very
104  reliably. Ratio of component masses is evaluated sufficiently exactly.
104  Both components are likely to have considerable excess of radii for their
104  masses.
105 CD Tau. The both components have considerable excess of radii for their
105  masses. CD Tau is a bright component of visual double system ADS 3866.
105  Visual secondary component is at a distance 10.2".
106 V818 Tau. The depth of secondary minimum is very small. The system is
106  a component of multiple system ADS 8347 L3=0.3. Both components have
106  considerable excess of radii for their masses.
108 CV Vel. The both components have considerable excess of radii for their 
108  masses.
109 DM Vir. The both components have considerable excess of radii for their 
109  masses.
110 alf Vir. The depths of minimums are very small. Evaluation of photometric
110  elements by brightness curve is difficult because of a very small depth of
110  eclipses and physical variability of primary component (which is likely to
110  be a variable of type {beta} Cep). There are data that the system has gas
110  substance (Struve O. et al., 1958ApJ...128..310S).
111 HD 84207. Photometric components and radii aren't evaluated very reliably.
113 V3903 Sgr. This system is denoted as '100a' in the original article.