CN And CWA_CB According to lc from Jassur & Khodadadi [352] it is a CBV system because of asymmetry (primary maximum is greater than secondary) and large dA, but according to lc solution it is CWA overcontact system with components in poor termal contact. But according to van Hamme et al. [319] and their lc solution (with two spots) it is semidetached system with components in marginal contact, the decreasing period is consistent with this suggestion (and in this case mass transfer from more massive primary to less massive and smaller secondary exists). EE Aqr CBV___: According to Wronka et al. [320] it is semi-detached system with more massive primary almost filling its critical lobe and less massive secondary filling Roche lobe. there is no any asymmetry on lc, but minima of different depth. So it may be CB or CBF, not CBV. V802 Aql CWA Classified as CWW by Samec et al. [105], secondary spectra is later than usual. V1713 Aql System will belong to CB or CW if subdwarf are components of these classes. There is no individual investigations. Confirmation of spectra is needed. V883 Ara Period is not suitable for any of the classes, there is no individual investigations, system is chemically peculiar and on eccentric orbit. TU Boo CWW_CWA The primary minimum of lc is a transit so system may be classified as A-subtype, but Niarchos et al. [485] have solved the lc with WD method and have stressed that some physical characteristics are typical for W-subtype systems. Moreover, their solution with spots have given secondary (less massive and smaller) is being some hotter than primary. This is typical for W-subtype too. According to Coughlin et al. [354] is a marginal contact system with both components almost fill their critical lobes, light curve asymmetric, so authors use hot spot on the primary to solve light curves. They supposed the mass transfer from secondary to primary which is supported by increasing period. The shape of the lc corresponds to A-subtype, but q is greater than 0.4 and components are only in marginal contact like the typical W-subtype system. So it rather CB of V subclass? DU Boo CWA___: According to Pribulla et al. [276] to explain both photometric and spectroscopic observations several phenomena are required: (i) large heated areas, most probably on the secondary component and very likely resulting from the mass and energy flow heating the hemisphere facing the observer around phase 0.25, (ii) additional matter close to the neck connecting the component producing “bumps” in the BFs observed around the first quadrature, (iii) streams of matter most probably approaching the observer before the primary minimum (making the profile of the primary being wider before the primary minimum), or (iv) deviations from the Roche model. But the mass transfer from the more to the less massive component would result in period decrease in the system which is not observed. Fill-out factor is large so system is in deep contact. Their analysis clearly showed that the complications in DU Boo cannot be explained by dark/hot surface areas only. In fact, without BFs, photometry does not require any additional phenomena. Additional source of light seen in BFs in DU Boo is visible only around first quadrature (phase 0.25) and its RV corresponds to the neck area connecting the components. In other quadrature the systems look more like detached or semidetached. So It may be the CW system. To determine subclass more investigation are needed. IQ Cam DW The spectral type of secondary is earlier than for for other DW. IQ Cam is one of the best SN Ia progenitor candidates known today. Eclipsing nature is not known exactly. AD Cap SC There is no enough data to classify this system properly. Pojmanski [93] gives magnitude range 9.65 (0.33) in V band and minII=minI (ASAS-3 light curve). This values are smaller than for other SC systems, and period is smaller as compared with other SC. Also in Antonopoulou [397] spectral type is equals to K4V+K5V.AD Cap is chromospheric active system of RS CVn type. More observations and investigations are needed. AO Cas CE Too large P for CE systems, possible it is a CG system, but too small A1 in this case. Ell configuration is possible. In most studies the system is found to be a semidetached and the primary while less massive is more luminous than secondary. According to Gies & Wiggs [321] and Bagnuolo & Gies [199] the system is semidetached, less massive secondary is subgiant which fills its Roche lobe and more massive primary is a MS star and doesn't fill its Roche lobe. Then SH type is more suitable? But too early Sp2 for typical SH type. V570 Cas A1 is large, may belong to SA, but all SA have EA or EB light curves, not E:. Period is given according to Alfonso-Garzon et al. [413], but as can be seen, their light curve is very strange and does not resemble ones for eclipsing variables. So eclipsing nature must be confirmed firstly. V731 Cas S2C P is larger than for other S2C systems (<=0.25d for others except V Sge which has period bout 0.5d). According to Downes et al. [90] cataclysmic status is uncertain. More investigations are needed. V741 Cas May belong to SA class, but primary spectra is some early, for SC both spectra is not appropriate. According to Duemmler et al. [322] system is detached, but primary is close to contact. So is this system in intermediate state? SV Cen CE It is a CE type system rather because of period, Sp types, masses and luminosity of both stars. But A1 is large. Magnitudes in CEV agree with values which are given in GCVS, different investigations and light curves from VSX. V748 Cen According to van Genderen et al. [323] secondary is M4III star, filling its Roche lobe, primary is a hot small star. Probably system is symbiotic and may belong to D2S class, but to know it exactly primary spectra should be determined properly. Also Large A1, is included to list of symbiotic stars of Belczynski et al.[167]. V1133 Cen May be classified as CB only, but luminosity class for secondaries of CB is IV-V, not III. There is no publications, so system is needed to be investigated. ZZ Cep DM Too large A1, far from line M for DM systems (see Fig.1 in Malkov et al. [324]). The binary is the brigther star of the triple system ADS 16252. Spectral class of the system were derived by Herbig [258]. Analysys of the V light curve was firstly performed by Kandpal & Srivastava [259] and by Cester et al. [142]. The system is detached. Derived absolute dimensions of the secondary component contradicts to spectral type of Herbig. The secondary component lies far above the MS band as would a subgiant star. The nature of the system remains unclear. BE Cep CWW System was studied recently by Dai et al. [488] who supposed system to be marginal contact W-type W UMa binary, while Samec et al. [489] have predicted near-contact configuration. The dA value (i.e. A1-A2) is larger than for other CWW systems and spectral type is unknown. DY Cet CWA System was classified as A-subtype of U UMa class by Rucinski et al. [454] based on RV curve, later this class was confirmed by Deb & Singh [343] (according to solution of ASAS light curve). But our algorithm recognizes it as near-contact system because of late type secondary. Secondary spectra is not appropriates to CWA configuration but we used data of Pourbaix et al. [11]. Primary spectra was determined by [454] based on color indexes and seem to be right while secondary spectra may be uncorrect. So data of Pourbaix must be proven. GO Cyg CB Sp2 is earlier than for other CB systems. Near-contact system according to Ulas et al. [325], in which the primary (massive and hotter) component is slightly greater than its Roche lobe, while the cool component is slightly smaller than it. GO Cyg is an unevolved system with both its components very close to the ZAMS. GO Cyg has the most massive components among the known CB systems. Light curves are symmetric, so it is not CBV system. V729 Cyg CG Was denoted as CB system in old version of CEV and in Csizmadia & Klagyivik [120], but period is greater and spectral type is earlier than for other CB systems. We changed ev. class to CG and spectral type according to Rauw et al.[198]. The masses of the components equal to (38-55)M and (10-15)M for primary and secondary respectively [198]. V1329 Cyg D2S A1 in GCVS and therefore in CEV for B band is around 6 mag. According to Chochol et al. [326] magnitude range is around 11.7-14.2, so A1=2.5. And mean brightness slowly decreases (see their lc). AV Del SA According to Mader et al. [272] it is semidetached system and may belong to SC ev. class. Sp class for secondary is unknown, Sp type for primary equals to F8 and is too early for SC. Also period value, A2 value and mass of the primary (more massive and hotter) are smaller than for other SC systems. There is no chromospherical activity (see [272]) on both light curves and spectra. So SC status is not proofed properly. BI Del DG System is included to the Catalogue of Chromospherically Active Binaries of Eker et al. [50] but without type designation. Spectral type not known exactly, lies with DR systems on the Sp1-logP and A1-A2 planes, differs from other DG systems. May be DR? Need more investigations for confirmation. A1 is larger than 0.75. BV Eri CBF Period is smaller than for other CBF systems. According to Gu et al. [327] value of period is valid. It is CB according to Gu [328], light curves resembles the CBF ones. So system may be the CBF with the smallest period. SV Gem SH Large A1 according to GCVS, but ASAS gives 10.55-10.62 in V band, and Guilbault et al. [329] and remarks in VSX (by Otero): it stopped eclipsing around 1940. Reflection variability with the orbital period is seen in survey data between 1989 and 2009. Also small amplitude ellipsoidal variations superposed causing a small secondary minimum at phase 0.5. Period constant over the last 102 years. Is system Ell or not eclipsing? MT Her CB_S__: Denoted as SA in Shaw [330] but Budding & Murad [331] have given detached solution of their lc. Why system is CB? V772 Her DM Triple system, see Boyd et al. [332] for details. RS Ind CBF___: Denoted as possible CBF by Shaw [330]. Marton et al. [212] have solved lc for the several possible configurations, their results partly support CB configuration. RY Ind SA_CB CB type is according to Shaw [330], while Lapasset & Claria [333] have found the system is semidetached algol-like binary (via Russell & Merrill method) RT Lac SA Too large A2. RT Lac is among the most peculiar stars of RS CVn type systems. While most of this type binary has equal-mass components, the RT Lac components have unequal masses. Ibanoglu et al. [262] has reported that brightness of the system at three phases, i.e., mid-primary and quadratures, shows quasi-periodic changes. The brightness at the primary eclipse (phase 0.0) shows the largest variation with a maximum amplitude of about 0.3 mag in the B and V filter. The light variations at second maximum (phase 0.75) resemble those at primary eclipse but with a maximum amplitude of about 0.2 mag, while the variations at first maximum (phase 0.25) are generally in the opposite sense, but with a lower amplitude (about 0.1 mag). In addition, although not strictly periodic, the average cycle of the light variations is almost the same for both second maximum and primary eclipse. Such a significant out-of-eclipse variations may be lead to large A2 value. In CEV we use photometric data from [262] obtained in 1992 because of the smallest difference Max1-Max2 in that observational period. According to [262] more massive, smaller and hotter component is mostly responsible for the change in the light curve because of its chromospheric activity. More over Ibanoglu et al. [195] have shown that The less massive, larger star fills its own lobe. Therefore, a gas stream from the larger, less massive star to the more massive one will be expected. It may also belongs to SC ev. class, but its period is smaller than for other SC systems. It spectral type is later than for SA. VY Lac SA_CB According to Semeniuk & Kaluzny [299] system is semidetached, but Shaw [330] have included it in his list of CB systems UV Leo CB_DM Giuricin et al. [334] have solved lc and confirmed the earlier hypotesis about detached status, but have stressed that the less massive component looks like more evolved star. Solution of Frederik & Etzel [335] confirms of detached status with possible magnetic activity for one of the components, so system may be the DR? But period is much longer compared to other DR systems. Looks like typical CB. RT LMi CWW_CWA Niarchos et al. [336] have classified it as CWW based on lc solution. Rucinski et al. [301] have derived RV curve and classified system as CWA. Later Qian et al. [337] have shown than lc of binary is variable and primary minimum was an occultation in 1994 while it is a transit in 2003. Based on their lc system is CWA, but solution of these lc have given CWW type! Qian et al. have concluded that RT LMi could not be uniquely assigned a subtype based on Binnendijk’s classification. RR Lep SA_CB Vyas & Abhyankar [338] have supposed system to be semi-detached algol-like, but Shaw [330] has included it in the list of CB systems. TT Lyr SH A1 is larger than 2, secondary spectra is K0 (Liao & Qian [213]), but why it is SH? V361 Lyr CBV According to Hilditch et al. [114] this star is a typical CBV system with asymetrical light curve. More massive and hotter primary fills its Roche lobe, while cooler and smaller secondary is detached. However Hilditch stressed out that this system is a rare because of its small period and significant difference in eclipse depth as compared with other CBV binaries. In CEV we use magnitude in secondary maximum (around 0.75P). IT Nor C Had a CG type in old CEV version, but too low period and late Sp as compared with other CG systems. Value of P is not known exactly. According to VSX P equals to P=1.754145, but in GCVS, [1] and in CEV now P=0.6357943. According to Shaw [330] P=0.3509, Sp=A0. According to Brancewicz & Dworak [339] system is semidetached, both components close to fill their Roche lobe. CB? V2610 Oph Tas & Evren [340] have investigated this system based on light curves and classified it as CWA, but later Pribulla et al.[286] have pointed out that system is quadruple and also noted that lc solution of Tas & Evren is completely inapplicable because of multiplicity of V2610 Oph. When they have corrected the observed photometric amplitude for the contribution of secondary pair, they have obtained the full amplitude of the binary as 0.41, indicating a high orbital inclination angle. So new light curve analysis is needed to classify this system. FR Ori SA_CB Shaw [330] included it in his list of CB systems, while detached in Brancewicz & Dworak catalogue [339]. Zakirov [341] has suggested that system is SA with MS primary and pre-MS secondary filling its critical obe. One of these hypotesis must be proven. V357 Peg CWA System was classified as CWA by Rucinski et al. [284] who have given also primary spectra, this result was confirmed by Deb & Singh [343] and by Ekmekci et al. [289] but secondary spectra (G5V) which is given by Pourbaix et al. [11] is not suitable for CWA class but for CB only. On the other side Ekmekci et al. [289] have supposed F3IV spectral type for secondary. So secondary spectra must be determined properly to classify V357 Peg. AI Phe DR Period is long for DR class. Don't belong to long-period RS CVn systems, but active according to Karatas et al. [125]. VZ Psc CB_CWA P is smaller than for other CB systems. According to Hrivnak et al. [203] it is an old disk population star, displays exceptionally strong CaII H and K emission lines. Light curve has changed from that of W UMa with minima of equal depths to beta Lyr type with unequal depth. Analysis of light curves shows greatly overcontact configuration with very large temperature difference between components. Therefore components are in geometrical but not in physical contact like other CB systems. Also Hrivnak et al. [203] has shown that it is possible to solve light curves with hot spot on the secondary component. In this case system is in marginal contact. They have investigated the light curves assymetry and have shown than light curves asymmetric. So system is rather CB system. May belong to CBV class such as V361 Lyr. PW Pup Because of its period may belong to DGlate only, but A2 is larger than usual and secondary spectra is too early (G-M is typical values). Interacting with Halpha emission (Bopp et al. [455]), and close to contact (Eggen [456]). QR Sge DW Period is larger than for other DW systems, there is no period value in GCVS and VSX. The fastest runaway WR star in Galaxy. V5569 Sgr Large A1, it is "iron star" (only two such stars are known), consisting of Be with red supergiant component. Light curve is strongly variable e.g., see Howell et al. [390]: A1 varies from 0.7 to 2 mag) V1236 Tau According to Bayless & Orosz [185] is a double-lines eclipsing binary with two low mass and near identical components, secondary (less massive) is slightly enlarged. May belong to DM or DR class? BL Tel DG Too large A1. Out-of-eclipse light variations. The variability of bright F primary is around 0.2 mag. A1 changes from year to year. To explain the variability of color indexes van Genderen [457] supposed a cold asymmetric gas stream but we didn't find any confirmation of semidetached configuration. BD Tuc According to West et al. [458] A1 is about 1.4, A2 is about 0.5, spectra is B0.5V+B4III, system is semidetached. But their data must be confirmed. May belongs to SH, but spectra is needed. See also Loudon & Budding [459]. eps UMi For DGearly period is long and spectra is late, for DGlate period is short, A1 is large, for SA A1 is large. Marginal? LX Vel Is included in list of X-ray massive binaries of Liu et al. [460]. Is S2H system? VV Vir CBV Has been variously classified as a nearcontact system by Shaw [330], as a contact binary by Giuricin et al. [461], as a Beta Lyra (EB) semidetached binary (GCVS) and an RR Lyrae by Sandage, [95] variable. According to Samec et al. [266] system is semidetached with hot stream spot on a secondary (less massive, more cooler) component, their light curve is asymmetric with MaxI is being little greater than MaxII. So they classify this system as CBV. AG Vir CWA MinII-MinI>0.5 may be the result of mistaken moments of minima due to asymmentic light curves (e.g. see Michaels [462].) According to Pribulla et al. [276] it is rather CWA than CB system despite of light curve asymmetry. According to Pribulla the secondary minima are systematically delayed after phase 0.5. AW Vir CWA_CWW Lapasset et al. [463] based on lc analysys (unspotted model) have concluded that subtype (A or W) is undetermined because of nearly equal temperatures of both components and other reasons, but their best-fit solution formally corresponds to A-subtype. While Niarchos et al. [464] have founded (based on spotted solution) the W-subtype.