\documentstyle[twoside, ibvs2, epsf]{article}
\input ibvse.sty

\begin{document}

\IBVShead{5364}{9 January 2003}

\IBVStitletl{The First Eclipsing Binary Observations}{ at the Ulupinar Astrophysics Observatory}

\IBVSauth{Dem\.{i}rcan, O.$^1$; Erdem, A.$^1$; \"{O}zdem\.{i}r, S.$^1$; \c{C}\.{i}\c{c}ek, C.$^1$; Bulut, \.{I}.$^1$; Soydugan, F.$^1$; Soydugan, E.$^1$; Baki\c{s}, V.$^1$; Kaba\c{s}, A.$^1$; Bulut, A.$^1$; T\"{u}ys\"{u}z, M.$^1$; Zejda, M.$^2$; Budding, E.$^1$}

\IBVSinst{Ulupinar Astrophysics Observatory, \c{C}anakkale Onsekiz Mart University, TR-17100, \c{C}anakkale, Turkey}

\IBVSinst{N. Copernicus Observatory and Planetarium, Kravi hora 2, Brno, Czech Republic}

\SIMBADobj{AB And} 
\SIMBADobj{AD And} 
\SIMBADobj{BX And}
\SIMBADobj{OO Aql} 
\SIMBADobj{XZ Aql} 
\SIMBADobj{V417 Aql}
\SIMBADobj{TZ Boo} 
\SIMBADobj{AC Boo} 
\SIMBADobj{TY Cap}
\SIMBADobj{RZ Cas} 
\SIMBADobj{AB Cas} 
\SIMBADobj{IR Cas}
\SIMBADobj{IV Cas} 
\SIMBADobj{DK Cep} 
\SIMBADobj{EG Cep}
\SIMBADobj{XX Cep} 
\SIMBADobj{YY CrB} 
\SIMBADobj{ZZ Cyg}
\SIMBADobj{V836 Cyg} 
\SIMBADobj{V859 Cyg} 
\SIMBADobj{RZ Dra}
\SIMBADobj{AI Dra} 
\SIMBADobj{RZ Equ} 
\SIMBADobj{EW Lyr}
\SIMBADobj{PY Lyr} 
\SIMBADobj{V508 Oph} 
\SIMBADobj{AT Peg}
\SIMBADobj{BB Peg} 
\SIMBADobj{FG Sct} 
\SIMBADobj{V Sge}
\SIMBADobj{V Tri} 
\SIMBADobj{RT UMi} 
\SIMBADobj{AH Vir}


\begintext


\IBVSEobs{The \c{C}anakkale Onsekiz Mart University (\c{C}OMU)
Ulupinar Astrophysics Observatory was built in 2001, close by the
slopes of Mt. Ida, overlooking ancient Troy. The location
(longitude: 01\hr 45\mm 54\sec\ E, latitude: 40\deg 06\arcm 01\arcs\ N, 
altitude: 410 m) has about 200 clear nights
in a year. It is only ten km from \c{C}anakkale, but it is
sheltered by a low ridge from most of scattered night glow. The
observatory owns two (30 cm (T30) and 40 cm (T40)) Meade
Schmidt-Cassegrain telescopes with an SBIG ST-237 CCD camera and a
SSP-5A photometer, containing a Hamamatsu, R 4040 photomultiplier
tube(PMT). Further details about the observatory and its equipment
were given by Demircan (2003).}

\IBVSEred{Reduction of the CCD frames was made with
MUNIDOS\footnotemark\ software, and reduction of photoelectric
observations was made by ATMEX\footnotemark\ software.}

\footnotetext[1]{Hroch, F., Nov\'ak, R., 1997, MUNIDOS, {\tt http://munipack.astronomy.cz/}}

\footnotetext[2]{Keskin, V., 2001, ATMEX, {\tt http://astronomy.sci.ege.edu.tr/\~{}keskinv/}}

\IBVSEmethod{Kwee -- van Woerden method (Kwee \& van Voerden,
1952), and in some cases, depending on the nature of the data set,
several procedures written by A. Gaspani (1995) based on
artificial neural networks were used.}


\vspace*{2cm}

{\small \IBVSEstars{
AB And & EB & 23 11 32 & +36 53 36 & GSC\,2763:0683 & 45502.1040 & 0.33188902 & 1\\
AD And & EB & 23 36 45 & +48 40 15 & GSC\,3641:0419 & 39002.4445 & 0.98619443 & 1\\
BX And & EW & 02 09 03 & +40 47 39 & GSC\,2833:0053 & 48237.4893 & 0.61011419 & 1\\
XZ Aql & EA & 20 22 13 & -07 21 03 & GSC\,5174:0186 & 47743.4700 & 2.13918369 & 1\\
OO Aql & EW & 19 48 13 & +09 18 32 & GSC\,1058:0409 & 39322.6916 & 0.50679190 & 1\\
V417 Aql & EW & 19 35 24 & +05 50 18 & GSC\,0490:2611 & 43016.2099 & 0.37031370 & 1\\
TZ Boo & EW & 15 08 09 & +39 58 12 & GSC\,3044:0740 & 52390.3886 & 0.29716474 & present paper \\
AC Boo & EW & 14 56 28 & +46 21 44 & GSC\,3474:0880 & 52407.4388 & 0.35244147 & present paper \\
TY Cap & EA & 20 24 30 & $-$12 57 55 & GSC\,5749:1055 & 44793.4527 & 1.42345612 & 1\\
RZ Cas & EA & 02 48 56 & +69 38 03 & GSC\,4312:1101 & 48960.2260 & 1.19524980 & 1\\
AB Cas & EA & 02 37 32 & +71 18 16 & GSC\,4320:0403 & 46849.2820 & 1.36687530 & 1\\
IR Cas & EB & 23 06 52 & +54 04 52 & GSC\,3998:1901 & 28750.2740 & 0.68068890 & 1\\
IV Cas & EA & 23 49 31 & +53 08 05 & GSC\,4001:1392 & 40854.6480 & 0.99851747 & 1\\
XX Cep & EA & 23 38 20 & +64 20 03 & GSC\,4288:0241 & 41539.5307 & 2.33732600 & 1\\
DK Cep & EA & 21 58 33 & +60 56 54 & GSC\,4262:2154 & 33590.5578 & 0.98590874 & 1\\
EG Cep & EA & 20 15 57 & +76 48 36 & GSC\,4585:0413 & 40050.4491 & 0.54462274 & present paper \\
YY CrB & EW & 15 50 32 & +37 50 07 & GSC\,3054:1278 & 51674.3541 & 0.37656417 & present paper\\
ZZ Cyg & EA & 20 23 53 & +46 55 18 & GSC\,3576:1596 & 45000.3501 & 0.62861631 & 1\\
V836 Cyg & EB & 21 21 24 & +35 44 11 & GSC\,2715:0264 & 44853.4914 & 0.65341148 & 1\\
V859 Cyg & EW & 19 27 13 & +28 56 50 & GSC\,2137:2999 & 34629.4119 & 0.40499999 & 1\\
RZ Dra & EA & 18 23 06 & +58 54 13 & GSC\,3916:1962 & 44177.5609 & 0.55087616 & 1\\
AI Dra & EA & 16 56 18 & +52 41 54 & GSC\,3886:0105  & 37544.5092 & 1.19881489 & 1 \\
RZ Equ & EA & 21 17 52 & +09 50 06 & GSC\,1109:2135 & 37161.3730 & 1.96143000 & 2\\
EW Lyr & EA & 18 33 16 & +37 45 13 & GSC\,3105:1934  & 26499.6842 & 1.94874423 & 1\\
PY Lyr & EW & 19 20 26 & +28 56 44 & GSC\,2136:3105 & 34980.4372 & 0.38576273 & 1\\
V508 Oph & EW & 17 58 49 & +13 29 47 & GSC\,1019:1849 & 44785.3350 & 0.34479220 & 1\\
AT Peg & EA & 22 13 24 & +08 25 31 & GSC\,1136:1084 & 45640.4590 & 1.14609013 & 1\\
BB Peg & EW & 22 22 57 & +16 19 28 & GSC\,1682:1530 & 43764.3416 & 0.36150147 & 1\\
FG Sct & EW & 18 44 57 & $-$06 08 30 & GSC\,5126:4019 & 29017.5579 & 0.27057207 & 1\\
V Sge & E/NL & 20 20 15 & +21 06 09 & GSC\,1643:1423 & 50169.4910 & 0.51419534 & 1\\
V Tri  & EB & 01 31 47 & +30 22 02 & GSC\,2293:1382 & 48573.6604 & 0.58520570 & 1\\
RT UMi & EA & 17 04 06 & +80 19 45 & GSC\,4576:0151 & 26631.3010 & 1.84197580 & 1\\
AH Vir & EW & 12 14 21 & +11 49 10 & GSC\,0869:0551 & 47569.6110 & 0.40752300 & 1\\
} }

\vspace*{2cm}

\IBVSEsource{
1. Kreiner et al., 2000 \\
2. Khopolov et al., 1985
}


\vfill

{\normalsize \IBVSEmin{
AB~And       & 52510.3486  & 3     & I    & $ - $  &  $0.0761$    & 149, c \\
AD~And       & 52505.4228  & 9     & I    & $ - $  &  $0.0042$    & 47, c \\
BX~And       & 52514.3830  & 5     & I    & $ - $  &  $-0.0068$   & 21, c \\
XZ~Aql       & 52492.5279  & 6     & I    & $ - $  &  $0.1740$    & 126, c \\
OO~Aql       & 52505.3277  & 7     & I    & $ - $  &  $-0.0348$   & 104, c \\
             & 52508.3695  & 16    & I    & $ - $  &  $-0.0338$   & 120, c \\
V417~Aql     & 52498.4486  & 16    & II   & $ - $  &  $-0.0550$    & 77, c \\
             & 52511.4103  & 2     & II   & $ - $  &  $-0.0551$    & 25, c \\
TZ~Boo       & 52367.3542  & 7     & II   & $B,V,R$&  $-0.0041$   & 37, p \\
             & 52387.4136  & 11    & I    & $B,V,R$&  $-0.0034$   & 33, p \\
             & 52388.3060  & 10    & I    & $B,V,R$&  $-0.0024$   & 39, p \\
             & 52390.3827  & 8     & I    & $B,V,R$&  $-0.0059$   & 43, p \\
AC~Boo       & 52407.4402  & 7     & I    & $B,V,R$&  $0.0014$    & 37, p \\
             & 52409.3785  & 7     & II   & $B,V,R$&  $0.0013$    & 32, p \\
TY~Cap       & 52521.4056  & 3     & I    & $ - $  &  $0.0096$    & 49, c \\
RZ~Cas       & 52537.6186  & 3     & I    & $ B,V $&  $0.0099$    & 38, p \\
AB~Cas       & 52490.4170  & 5     & I    & $ - $  &  $0.0406$    & 236, c \\
IR~Cas       & 52512.4113  & 1     & I    & $ - $  &  $-0.0315$   & 29, c \\
             & 52527.3849  & 3     & I    & $ - $  &  $-0.0330$   & 37, c \\
IV~Cas       & 52497.3579  & 5     & I    & $ - $  &  $-0.0038$   & 194, c \\
XX~Cep       & 52515.5559  & 3     & I    & $ - $  &  $-0.0574$   & 55, c \\
DK~Cep       & 52495.3570  & 10    & I    & $ - $  &  $-0.0009$   & 413, c \\
EG~Cep       & 52577.3173  & 10    & I    & $ - $  &  $0.0006$   & 180, c \\
YY~CrB       & 52469.4692  & 4     & II   & $B,V,R$&  $-0.0001$   & 35, p \\
             & 52473.4240  & 4     & I    & $B,V,R$&  $0.0007$    & 39, p \\
ZZ~Cyg       & 52493.4256  & 5     & I    & $ - $  &  $-0.0310$   & 308, c \\
V836~Cyg     & 52528.4862  & 3     & I    & $ - $  &  $0.0236$    & 31, c \\
V859~Cyg     & 52524.3749  & 9     & I    & $ - $  &  $0.0384$    & 43, c \\
RZ~Dra       & 52496.3363  & 7     & I    & $ - $  &  $-0.0055$   & 89, c \\
AI Dra       & 52458.3834  & 5     & II   & V      &  $0.0175$    & 46, p \\
RZ~Equ       & 52468.4761  & 11    & I    & $ - $  &  $0.1034$    & 318, c \\
EW~Lyr       & 52515.3885  & 1     & I    & $ - $  &  $-0.0312$   & 63, c \\
PY~Lyr       & 52469.4388  & 2     & I    & $ - $  &  $0.0625$    & 265, c \\
             & 52470.4020  & 1     & II   & $ - $  &  $0.0613$    & 237, c \\
V508~Oph     & 52486.4355  & 7     & II   & $ - $  &  $-0.0057$   & 19, c \\
             & 52513.3314  & 1     & II   & $ - $  &  $-0.0036$   & 23, c \\
AT~Peg       & 52512.3486  & 8     & I    & $B,V,R$&  $-0.0668 $  & 36, p \\
BB~Peg       & 52513.4118  & 2     & I    & $ - $  &  $0.0116$    & 108, c \\
FG~Sct       & 52472.3579  & 7     & I    & $ - $  &  $-0.0104$   & 179, c \\
             & 52472.4943  & 3     & II   & $ - $  &  $-0.0093$   & 194, c \\
V~Sge        & 52523.3653  & 21    & I    & $ - $  &  $-0.0240$   & 81, c \\
V~Tri        & 52497.4679  & 3     & I    & $ - $  &  $0.0033$    & 79, c \\
RT~UMi       & 52529.4791  & 16    & I    & $ - $  &  $-0.0016$   & 59, c \\
AH~Vir       & 52397.4148  & 2     & II   & $B,V,R$&  $0.0826$    & 41, p \\
             & 52398.4328  & 2     & I    & $B,V,R$&  $0.0818$    & 32, p \\
} 
}


\IBVSfig{9cm}{5364-f1.eps}{(a) Photoelectric light and
color curves of AH Vir and (b) Unfiltered CCD light curve of PY
Lyr}
%\IBVSfigKey{5364-f1.eps}{AH Vir ; PY Lyr}{light curve}

\IBVSfig{9cm}{5364-f2.eps}{Unfiltered CCD minima of (a) ZZ Cyg and
(b) EW Lyr}
%\IBVSfigKey{5364-f2.eps}{ZZ Cyg ; EW Lyr}{light curve}


\IBVSErem{The 33 stars, whose details are listed in Table 1, were
observed using either conventional filtered Johnson standard ($BVR$)
photoelectric photometry with the SSP-5A or unfiltered with the
ST-237. 45 times of minima, primary and some secondary, are listed
in Table 2, together with $O-C$ values corresponding to the Table~1
ephemerides. The remarks column of Table 2, e.g. 147,c, gives
first the number of data points used in the calculation of each
minimum time followed by an identification of which system was
used; thus ``c'' refers to the 30 cm + ccd combination and ``p'' means
the single channel photometer on the 40 cm telescope. We show, in
Figures 1, \& 2, selected light curves corresponding
to these reported results.\\
\\
Figure 1a shows a typical light curve (AH Vir) obtained with the
single channel photometer on the 40 cm telescope. In Fig 1b, the
moderate low amplitude $\sim $12.5-13 mag W UMa binary PY Lyr light
curve reflects a reasonable level of scatter for 20 sec
integrations. The measured standard error on a run of 300 points
is 0.018 mag, for example, as compared with 0.015 mag,
corresponding to purely Poissonian counting statistics.  Similar
calculations for other binaries at comparable magnitudes show
similar ($\sim $2\%) individual datum accuracies and point to
essentially high steadiness of attainable conditions at the site.
Light curves of such variables will be presented
in more detail in subsequent IBVS articles.\\
\\
Asymmetry around the outer tangencies
of the short period system ZZ Cyg and the distinct totality
observed for EW Lyr (Fig 2a,b) present interesting challenges for
further study of these deep-minimum classical Algols.}
\IBVSEdata{Upon request}

\IBVSEack{For the development of the Ulupinar Observatory,
technical support has come from Varol Keskin, financial support
has come from the \c{C}anakkale Onsekiz Mart University Research
Foundation.}


\references

Demircan, O., 2003, \emph{Sky \& Telescope, (submitted)}

Gaspani, A., 1995, 3rd GEOS workshop on variable star data
acquisition and processing techniques, 13-14 May 1995, S.
Pellegrino Terme, Italy

Kholopov, P. N. (ed.), et al., 1985, \emph{General Catalogue of
Variable Stars, Moscow Nauka Publishing House}

Kreiner, M. J., Kim, C.-H. and Nha, I.-S., 2000,
{\emph{An Atlas of $O-C$ Diagrams of Eclipsing
Binaries, Krak\'{o}w}}

Kwee, K. K., \& van Woerden, H., 1956, {\it Bull.\ Astron.\ Inst.\
Neth.}, {\bf 12}, 327

\endreferences

\end{document}
