XZ And SA DI!=DII, without confirmation CD And System can belong to DGlate only because of its large period, but A2 is not suitable for DG. According to Kreiner [1] period = 34.4434. And then it is not DG, but DM or SA. Only old photographic data are available. So confirmation of value of the period and new observations are necessary. V374 And To classify as DM new value of A1 is necessary. Semi-regular pulsating star in Simbad. Is system really eclipsing? V395 And C May belong to CE only but spectra is somewhat later than needed V413 And Period is large to classify as SA, period is short to classify as DGlate. There is no individual investigations. AP Aps Only photographic data are known, value of A2 is large. EB light curve with two equal minima. Period may be twice shorter? More observations and investigation are needed. BQ Aqr System may belong to SA class, but secondary spectra must be measured. KV Aqr System will belong to D2S or SA if curve type (EA or EB) is given. MU Aqr CB____: Is designated as CB? in Pribulla et al. [91], only one light curve is published by Dvorak [465] with large dA, while on ASAS-3 light curve dA almost equals to 0. So investigation are needed. Y Aql System can be classified, if luminosity class will be determined properly. V413 Aql System may be classified as DGlate or D2S, if spectra will be determined properly. V719 Aql Value of A1 is large, old photographic data only. V885 Aql New photometry is required to classify this system as DM or SH. V1251 Aql Old photographic data only, period =1d is not suitable for ASAS-3 light curve. V1345 Aql There is no secondary minimum on ASAS-3 light curve, but GCVS gives MinII-MinI=0.46 (apsidal motion?). More observations and investigations are needed. System class is unknown, but system was included in Budding catalogue [62] of Algol type binaries. V1436 Aql To classify as DM new value of A1 is necessary. V1464 Aql C ELL+DSCT in VSX, RR in Simbad, confirmation is needed ER Ara Value of A2 is large, old photographic data only. IR Ara System is denoted as SRB variable in VSX, has very long period. Not eclipsing? Eclipsing nature must be confirmed or rejected. IZ Ara System is denoted as SRB variable in VSX, has very long period. Not eclipsing? Eclipsing nature must be confirmed or rejected. KO Ara Pojmanski [45] gives RPC type of variability, value of A2 is large to classify system as DW. Also system can belong to CB or CWW, but in this case curve type must be determined properly. KU Ara Value of A2 is large, investigation is necessary. LT Ara Old photographic data only, large value of A1 does not permit to classify system as DW or D2S, according to ASAS-3 light curve A1 is about 2.5 mag. In this case system may belong to SA. V781 Ara CW Only photographic data, confirmation of curve type is needed. V851 Ara Both depth are small, confirmation of photometric data is necessary. RX Ari CB_S There is no individual investigations. EP Aur CB____: Light curves were published by Zhang et al.[466], but analysis of their data was not published. HR Aur Morphological type of light curve and spectral class must be determined properly to classify this system as DR. V523 Aur Value of A2 is large for DW and S2C, curve type is not appropriate to CB and CWW, new photometry is necessary. AQ Cam Value of A1 is large, old photographic data only. RU Cnc DR According to Scaltriti et al. [468] the durations of the eclipse (0d894+-0.020) and of the totality (0.314d+-0.016), i.e. DI=0.088P, dI=0.031P, MinII-MinI=0.5. ASAS-3 light curve gives DII=DI. So confirmation of GCVS data is needed. HQ Cnc Morphological type of light curve must be determined properly to classify as CB. RV CVn CW_CB According to lc of Hoffmann [467] it is rather CB system, but there is no investigations. EF CMa Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. EQ CMa With such late spectra may belong to DM class only, but both components are giants! There is no investigations! According to Parihar et al. [406] spectra is K2III+F0V. If it is right value then system will be classified SA class. KV CMa Period is close to limit for DGlate class, but A2 is not suitable, spectra must be determined properly to classify system. Long period given by Otero & Dubovsky [36] is not appropriate for ASAS light curve. There is period value in GCVS. Eccentric system [36]. There is no individual investigations. CW CMi CB____: Light curves were published by Merchan-Benitez & Jurado-Vargas [365], but there is no individual investigation AW Car Value of A1 is large, old photographic data only. V338 Car Period as for DGlate only, but spectra is needed to classify system. Photographic data are known only. Be star in Simbad, there is no individual investigations. V712 Car DGE class is only possible because of WN spectra for primary but A2 value is larger than typical secondary minima for other DGE. New observations are needed to confirm A2 and spectra AL Cas CE____: Investigations and observations are needed. IR Cas CB Photographic values for A1 and A2 in GCVS are too large. We use in CEV NSVS photometric data. More observations are needed. KL Cas Old photographic data only. V442 Cas Value of A1 is large, old photographic data only. V554 Cas Because of its spectra may belong to DGlate only, but A1 is smaller than typical values for DGlate systems. Spectra must be determined properly. Only photographic data are known. AB Cen There is no observations, period is longer than for SA class. V388 Cen Old photographic data only. V495 Cen May be classified as DM or SA, if spectra will be determined properly. V619 Cen Value of A1 is large and does not permit to classify system as DGearly, DM or SC, old photographic data only. If curve type is determined, then system will belong to SA or DR class. V797 Cen Because of its long period system may belong to DGlate class only, but VSX gives L type of variability, so confirmation of eclipsing nature is necessary. V983 Cen Value of A1 is small, He-weak CP star. New photometry is necessary. Is system really eclipsing? V1054 Cen Value of A2 is large for CB, both A1 and A2 are large for CWW, period is longer than for CE class. VSX gives good EW light curve. Investigation is necessary. TV Cep New photometry is necesary to classify system as DM or DR. If secondary spectra is given then system will belong to SA or even SC. According to Halbedel [5] spectra is F2II/III. Only photographic data are known. DL Cep Old photographic data only. GS Cep CB____: Investigations and observations are needed. KL Cep Period is suitable for DGlate only, but secondary spectra is unknown. V445 Cep CWA Ell in GCVS, there is no confirmation of the eclipsing nature. zet Cep Is system really eclipsing? TU Cet SA There is no confirmation of MinII-MinI!=0.5. CL Cet C Discovered by Hipparcos, see ASAS light curve, EW in VSX, RR in Simbad, confirmation is needed DO Cha C Is discovered by Hipparcos, EW in the VSX, but ell variable in Simbad, there is no individual investigation TW Cir Value of A1 is large, old photographic data only. AQ Cir May be classified as DM, if spectra will be determined properly. EQ Com System will be classified as contact if new photometric data is available. KW Com System will belong to DM, if new photometric data is obtained. Photographic A1 is large. Has E+UV type of variability in VSX, Is system a candidate to BY Dra variables? KY Com Large value of A1 does not permit to classify system as DM. Only old photographic data are known. Has E+UV type of variability, Is system a candidate to BY Dra variables? SX Cru CW Too large A1, only photographic data are known. TX Cru Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. UZ Cru Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. WX Cru Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. DT Cru CE There is no individual investigations, confirmation of the eclipsing nature is needed. VV Cyg S There is no confirmation of MinII-MinI!=0.5, only photographic data are given. CV Cyg CWW The system class in not known properly, it may belong to CWA subclass, because depth of minima varies (see Vinko et al. [469]), there are no radial velocity curves. OV Cyg Value of A1 is large, old photographic data only. PV Cyg Value of A1 is large, old photographic data only. QR Cyg Old photographic data are given only. QU Cyg CW Only photographic data, confirmation of curve type is needed V371 Cyg Only old photographic data are available, system can be classified as SA, if secondary spectra will be determined. V445 Cyg Large value of A2 is not appropriate for DM, DW and SA, old photographic data is only known, according to Halbedel [5] spectra is mid FIII. Also secondary spectra is necessary for the classification. V546 Cyg Period is shorter than for DGlate and longer than typical SA. Spectra and new photometric data are necessary to classify this system. V628 Cyg CE____: Agerer et al. [470] have published new observations and given the new value of period (which was large, confirmed by Kreiner [1]), but inversigations are needed. V680 Cyg CB____: System class was not determided properly. CB according to Shaw [330] V698 Cyg System may belong to DR or SA, but has longer period, spectra is not suitable for DGlate. Spectra is given by Halbedel [176], but according to Zakirov & Eshankulova [471] spectra equals to A7II and K4III? Only photographic old photometry. V703 Cyg The value of period given by Hoogeveen [44] is twice shorter than GCVS gives. Confirmation is needed. V706 Cyg Values of A1 and A2 are large, old photographic data only. V779 Cyg Period is shorter than for CG class, but longer, than for CE. There is no investigations. Only old photographic data are known. V788 Cyg According to Nakada et al. [472] is a carbon star. Period is not appropriate for any of the classes, only photographic photometry is given. Also to classify this system spectra is necessary. V797 Cyg System can belong to DM or SH, but value of A2 is large. Confirmation of photometric data in V is needed. V825 Cyg System can belong to DM or SA, but values of A2 and dA are not suitable for both classes. Only old photographic data are available. V959 Cyg SA There is no confirmation of MinII-MinI!=0.5 and DI!=DII, only photographic data are given. V1034 Cyg SA____: System class was not determided properly. SA according to Shaw [330] V1068 Cyg System can belong to SA class, but value of A2 is larger than typical A2 for other SA, only photographic data are known. V1362 Cyg Value of period was determined inaccurately. System will belong to SA if curve type is given. V1374 Cyg A2 is too large. Only photographic magnitudes are known. Observations are needed. V1433 Cyg Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. V2082 Cyg CWA Possible Ell variable (GCVS, VSX), confirmation is needed. V2136 Cyg VSX gives spectra as B4V (based on ESA [412]). In this case may be classified as DM or SA. Be star. So spectra need to be determined properly. V2483 Cyg Has very long orbital period which suitables only for DGL class, while A2 value is larger than for other DGL systems. Unstudied. TZ Dra SA____: Investigations are needed to determine system class properly. SA according to Shaw [330] BR Dra Old photographic data only. AN Eri Old photographic data only. HL Eri VSX gives the value of period (based on data from ESA [412]), but this value is not suitable for ASAS-3 light curve. May be classified as SA, but A1 is smaller. Period and photometry are needed. RY For System will be classified as DW, SA or CB if secondary spectra is determined. UW Gem Will be classified as SA if shape of the light curve will be determined (EA,EB). EL Gem Value of A2 is large for DM, SA and CB classes, but if period is twice shorter than system will be classified. EU Gem Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. IP Gem Old photographic data only. OR Gem Period is given by Pojmanski [45], but it is shorter than for DGlate, but longer, than for SA. VSX (based on superWASP lc) gives p=2.0294. Value of period must be determined properly. BF Gru In the VSX p=75 and type of variability SR (based on data of Dvorak [427]), but Pojmanski [45] gives period=76.536469 and type of variability=MISC. So period and type of variability are undetermined. V691 Her Period and depth A1 are given by Pojmanski [45], but in [45] type of variability is MISC. Confirmation of eclipsing nature is needed. V707 Her Period is shorter than for CG class, but longer, than for CE. There is no investigations. Only old photographic data are known. V740 Her System may belong to CB, but spectra is later than typical value for other CB, only old photographic data. V1055 Her CB____: Evolutionary class is given according to Pribulla et al.[91], but there is no lc solution. WY Hor C Denoted as DSCT in Pojmanski, his period given in CEV, but according to Kiraga [473] it is EW with twice longer period. Confirmation is needed. SS Hya According to Lloyd & West [87] star may be constant, period is unknown, confirmation of variability is needed. VW Hya SA According to Pojmanski [45] period may be twice longer and magnitude range is 10.72 (A1=1.47) V. In this case A2=A1. But in CEV we use data of Burki et al. [67]. CH Hya CW There is no confirmation of MinII-MinI!=0.5, only photographic data are given. BZ Hyi System can belong to DGlate or SA, but secondary spectra and period are necessary. CE Hyi C EW in VSX, DSCT in GCVS, confirmation of the eclipsing nature is needed. XX Lac Value of A1 is large, only old photographic data. CN Lac CB_S Detached in the Brancewicz & Dworak catalogue [339], included also in the catalogue of RS CVn systems by Dryomova et al. [474]. There is no individual investigations. V407 Lac C EW in VSX (based on ESA data), Ell in GCVS, confirmation in needed. V Lep CB____: CB is according to Shaw [330]. Individual investigation is needed. WX Lep VSX gives the value of period (based on data from ESA [412]), but this value is not suitable for ASAS-3 light curve. VSX also gives spectra as B3Vn based on data from [412]. DGearly, but spectra is some later. DGlate, but A1 is some smaller. SA but spectra is some earlier. SH but A1 is some smaller. If spectra from VSX is used then system will be classified as DM. So properly determination of spectra, period and photometry is necessary. EY Lib Value of period is not determined properly, A1 is large. Only old photographic data. Shape of the curve is needed to be known. IV Lib System may be classified as SA if secondary spectra will be determined. KQ Lib CB____: Pribulla et al. [91] have denoted if as CB?, lc was published by Bernhard & Lloyd [475] but there is no solution. V401 Lyr Old photographic data only. V417 Lyr CW Too large A1. Only photographic magnitudes are known for this star and therefore more observations are needed. V428 Lyr System will be classified as DM or SA if new photometric data is obtained. V482 Lyr Long period LPV variable according to Pigulski et al. [476]. Not eclipsing? Eclipsing nature must be confirmed. V574 Lyr CB____: Denoted as CB? by Pribulla et al. [91]. ROTSE-1 lc was published by Blattler & Diethelm [293]. Solution is needed. V582 Lyr CB Lies higher and to the right from other CB on A1-A2 plane. More investigations are needed. TV Mic Large value of A2 does not allow to classify system as DM or SA, confirmation of photometric data is necessary. CD Mic System will be classified as D2S or SA if secondary spectra is determined. TU Mon SH A1>1. New observations and investigation are needed? AQ Mon SA DI!=DII, according to Brancewicz & Dworak [339] is a detached system, we can't find confirmation of DI!=DII BM Mon Large value of A1 does not allow to classify system as DM or SH, confirmation of photometric data is necessary. HY Mon Value of the period is not known exactly, Kreiner [1] gives p=1.565725, but VSX gives p=7.28243! V752 Mon C EW in VSX, DSCT in GCVS, confirmation is needed. V788 Mon Long period is given by Pojmanski [45], type of variability in [45] is MISC, if system is eclipsing with EW light curve, then such a long period is impossible! There is no investigations V853 Mon System can be classified as CWW, but value of A2 is smaller than needed. Investigation is necessary. V883 Mon Period is some shorter than typical value for DGlate type class, there is no observations and investigation of this system. V884 Mon Because of its long period may belong to DGlate only, but luminosity class given in CEV (V) is not appropriate to DGlate class. So spectral investigation is needed. UV Mus SA A2>0.6. But Why? Detached in Brancewicz & Dworak [339] AY Mus DM There is no confirmation of MinII-MinI!=0.5, there is no secondary minima on the light curves of Soderhjelm [477]. BH Nor We use new photometric data from Pojmanski [45] but period may be twice shorter than GCVS and Kreiner [1] give. More investigations are needed. GX Nor CW Both A1 and A2 are large for any of the contact classes, old photographic data only. HX Nor Period is shorter than for DGlate, and A2 is larger, there is no investigations. OT Nor Old photographic data only. V389 Nor Old photographic data only. DE Oct C EW in VSX, denoted as RRc in GCVS, confirmation is needed. alf Oct May belong to SA class, but A1 is lower than low limit for SA systems, so confirmation of A1 is needed. RV Oph SA DI!=DII, without confirmation. CY Oph The value of period given by Hoogeveen [44] is twice shorter than GCVS gives. Confirmation is needed. LL Oph System will belong to SA if secondary spectra is given. QR Oph Only old photographic data. V920 Oph Old photographic data only. V1510 Oph A1 is large to classify as DM or DR or DGearly. To classify as SA curve type is needed (EA or EB). Only old photographic data. V1892 Oph For CB period is short, for CWW A1 is large. Old photographic data only. V2060 Oph Period may be twice longer, only photographic data are known, more observations are needed. A1 is large to classify system as CWW. V2382 Oph CE BE type in GCVS, denoted as E+BE in VSX, curve type is complicated PX Ori Too large A1, only photographic magnitudes are given, period is not known, more investigations are needed. V643 Ori Period is close to typical values of DGlate systems, but secondary spectra is necessary. V1375 Ori System will be classified as DGlate if spectra is determined. V1537 Ori System is denoted as TTS/ROT variable in VSX according to Herbst et al. [478]. Not eclipsing? Eclipsing nature must be confirmed. V1824 Ori May belong to SA class but A2 value is large! Unstudied. CM Pav Too large A1, only photographic magnitudes are given, period is not known, more investigations are needed. HZ Peg Old photographic data only. V355 Peg CWA System was observed spectroscopically by Pych et al. [486] who have determined its primary spectra and supposed CWA: or possible semi-detached configuration. According to [486] curve type is EW while VSX gives EB type. Photometric observations are needed because only detached class is possible for this system DG Per Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. HP Per Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. KR Per System can belong to several classes simultaneously until new photometry and spectra are not known exactly. LX Per DR We can't find any confirmation of DII!=DI. NP Per Value of A2 is large, old photographic data only. V364 Per CW Only photographic data, A1 and A2 are large. V382 Per System will belong to SA if curve shape is determined properly and secondary spectra is given. V481 Per Only old photographic data. V579 Per C EW in VSX, RR variable in the Simbad data base, confirmation is needed. BQ Phe C EW in VSX, SX Phe type variable in Simbad, confirmation is needed RT Pic Only photographic magnitudes are given, period is not determined. A1 is large. More observations are needed. UZ Pic Long period is not appropriate for any of the classes, system is not eclipsing in VSX. Eclipsing nature needs to be confirmed or rejected. EE Psc CB____: Denoted as CB? by Pribulla [91], but there is no investigations X PsA CW Too large A1 and A2. Only photographic magnitudes are known for this star and therefore more observations are needed. VY Pup SA___: Denoted as SA by Shaw [330] There is no individual investigations and observations. AU Pup CWA A1>0.75 and A2>0.6. EH Pup Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. KK Pup According to Hoogeveen [44], who find the period, value of period may be twice longer, so need for more observations. KY Pup System may belong to CE class only, but luminosity class (III) is not suitable. There is no individual investigations for this system. So spectral investigations are needed. LW Pup System may belong to DGlate class only, but period is some shorter than for other DGlate systems. There is investigations and observations of this system. V401 Pup System is the perfect candidate to SC class except its A1 value (in CEV HIP photometry is given, SC low limit for A1 is 0.48). From the ASAS-3 light curve depth of primary minima is about 0.4. New observations are desirable. V409 Pup Denoted as eclipsing variable according to Koen & Eyer [479], there is no confirmation. V617 Pup Spectral type is needed to classify system exactly. V634 Pup All parameters except spectra are appropriate for DGlate. Spectra is close to limit. There is no individual spectral investigations. AR Pyx Because of its long period may belong to DGlate only, VSX gives for this system mag range 8.68-9.21(V), logP=1.6797 and SRB type of variability. Period in CEV is given according to Pojmanski [45], he also gives mag range 8.7-9.04 (V) and type of variability as 'MISC'. Not eclipsing? Eclipsing nature must be confirmed or rejected. QT Sge System is the perfect candidate to DGearly, but to classify this system the spectra of secondary is needed to be determine properly! V356 Sgr SH There is no confirmation of MinII-MinI!=0.5 and DII!=DI. V497 Sgr Values of A1 and A2 are large, old photographic data only. V525 Sgr CBV___: Denoted as CBV by Shaw [330]. There is no investigations V765 Sgr Too large A1, only photographic magnitudes are known, more investigations are needed. V766 Sgr Because of its period may belong to DGlate only, but A2 is large. There is no individual investigation, only ASAS-3 light curve, confirmation of photometric data is necessary. V777 Sgr System may belong to DGlate, but spectra are needed to be determined properly, because secondaries of DGlate systems have luminosity class II-III, but the V777 Sgr secondary has luminosity class I. V1108 Sgr Period is shorter than for DGlate and some longer than for SA. Investigations and confirmations of period is needed. V1276 Sgr Spectra of the secondary is necessary to classify this system as CB. V1282 Sgr Too large A1(>4), only photographic data are known. V1315 Sgr Value of A1 is large, old photographic data only. V1357 Sgr Value of A2 is large for DW, curve type is not suitable for CB, new observations are required. V1428 Sgr Only old photographic data is given, system will belong to DW is secondary spectra is known. V1712 Sgr Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. Only old photographic data are known. V2876 Sgr Old photographic data only. V3501 Sgr CW Only photographic data, confirmation of curve type is needed. V4066 Sgr Only old photographic data is given, system will belong to DW is secondary spectra is known. V4118 Sgr Because of very short period in CEV can belong to S2C only, but curve type is not suitable for S2C. VSX gives p=0.27835. So value of period must to be proved. V4153 Sgr Period is shorter than for DGlate class, but longer, than for SA. There is no investigations. V4374 Sgr To classify this system spectral class of the secondary must be determined. V4408 Sgr CE EW in VSX, long period variable in Simbad, confirmation is needed. V5566 Sgr System can belong to DM or SA, if spectra will be determined properly. IM Sco Only photographic magnitudes are given, period is not determined. A1 is large. More observations are needed. V381 Sco DG A1>2. Classified as DG, but has A1>2. Only photographic data are known. V383 Sco Period and spectra are suitable for DGlate only, but A1 is large! Old photographic data only. On ASAS-3 light curve mag range is about 10.61-13.40, so A1 is large anyway! Confirmation of the value of A1 is necessary. V412 Sco CW Only photographic data, A1 and A2 are large. V472 Sco Long period points to DGlate class, but secondary spectra is needed for classification. V486 Sco Has large period! Pre-MS Herbig Ae star? Not eclipsing? Eclipsing nature must be proved. V591 Sco Value of A2 is large. If period is twice shorter, than system will be classified as DM. V1090 Sco System can belong to CE class only, but spectra is not appropriate. V1225 Sco To classify this system the confirmation of spectra is needed, small values of A1 and A2 is needed. V1288 Sco System may belong to several classes: DGearly (but secondary spectra is not appropriate and period is shorter), SA (but spectra is earlier) and SH (but period is shorter). There is no individual observations and investigations. V1291 Sco Period is shorter than for DGlate class and some longer than for SA class. Confirmation of the period is needed. VX Sct System will belong to SA or DM if secondary spectra is given. Old photographic data are only known. BH Sct Large value of A2 does not permit to classify system as DM or SA, only old photographic data are available. ER Sct DM There is no confirmation of MinII-MinI!=0.5, only photographic data are given. FN Sct Large value of A1 is not suitable to classify system as DM or SH. New photometric observations are needed. GM Sct Large value of A2 does not permit to classify system as DM or SA, confirmations of the photometric data is needed. IN Sct Large value of A1 does not permit to classify system. Only old photographic data are known. V372 Sct Large value of A1 does not permit to classify system. Only old photographic data are known. RS Ser CB____: Incomptele lc was published by Walas et al. [480], Pribulla et al. [91] have denoted its as CB? LC solution is needed. CQ Ser CB____: CB is according to Shaw [330]. There is no investigation DG Ser CW Too large A1. Only photographic magnitudes are known for this star and therefore more observations are needed. AV Tel A2 is large for CB, A1 is large to classify system as CWW, confirmation of photometric data is needed. V Tri SA____: As SA was denoted by Shaw [330]. Investigations are needed. HV TrA Period may be twice longer, only photographic data are known, more observations are needed. RW UMa DR We can't find any confirmation of DII!=DI. Has large A1. DN UMa DM There is no confirmation of MinII-MinI!=0 and e!=0. According to Abt [481] e=0. AS Vel DM There is no confirmation of MinII-MinI!=0 and e!=0. According to Garcia et al. [482] e=0. BT Vel CW According to Lucy [483] BT Vel is a CW, but A1 and A2 are too large for CW. More observations and investigations are needed. BW Vel According to Lucy [483] BW Vel is rather of beta Lyr type because of dA value. But his conclusion was based on old photographic observations with dA being equal to 1. So more observations and investigations are needed to determine system class. CK Vel The value of period given by Hoogeveen [44] is twice shorter than GCVS gives. Confirmation is needed. DU Vel A2 is large to classify system as DM or SA. If period is twice shorter as Pojmanski [45] gives, then system will be classified. NO Vel System will belong to DGearly class, if sec spectra is given. Additionally VSX given the value of period, but it is not suitable for ASAS light curve. OQ Vel C EW in VSX, RR in Simbad, confirmation is needed. QY Vel Period is some longer than for SA and spectra is some later. Secondary spectra is needed. V353 Vel C EW in VSX, DCST in Simbad, confirmation is needed. KZ Vir CWA_CB Was classified as CWA by Rucinski et al. [484] but they have noted that system may be close, but detached binary. Later Pribulla et al. [91] have denoted system as CB. There is no individual investigations LM Vir Curve shape (EW) is suitable for contact classes, but A1 is too small VSX gives the value of period, but it is not appropriate for ASAS light curve. LN Vir Spectra is appropriate for SC and DGlate classes, but A1 is small for both. there is no another data except from Hipparcos. MW Vir System can belong to CB or CWA because of its spectra, but A1 is small for both classes, VSX gives the value of period, but it is not suitable for ASAS light curve. V349 Vir Is a possible gamma Dor variable [84]? W Vol To classify this system spectra of both components must be determined properly. UZ Vol System will belong to DGlate, if secondary spectra is determined. VX Vol Such a long period and late spectra point to DGlate class, but low limit of log of periods of DGlate is 1.849. SRB variable in VSX, so confirmation of the eclipsing nature is needed. WZ Vol Because of its period may belong to DGlate only, but spectra is not suitable for this class. CD Vul SA_CB_: Denoted as CB? by Shaw [330], while Brancewicz & Dworak [339] have classified as semi-detached. There is no individual investigation MN Vul Large value of A2 does not permit to classify system as DM, DR or SA, only old photographic data are available.