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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.