Parameters of 20 newly detected eclipsing binaries from the $Kepler$ database
D. Dimitrov\inst{1}
D. Kjurkchieva\inst{2}
V. Radeva\inst{2}
The paper presents a sample of newly detected eclipsing binaries from the public $Kepler$ data. Orbits and fundamental parameters of 20 unknown eclipsing binaries were determined by modeling of their photometric data. Most of them are well-detached, high-eccentric binaries. We established that the target KID8552719 satisfied all widespread criteria for a planetary candidate. Fitting its light curve we obtained radius R$_{p}$=0.9 R$_{Nept}$, distance to the host star $a$=42.58 R$\sun$=0.198 AU and equilibrium temperatute T$_{p}$=489 K. These values imply a Neptune-size object out of the habitable zone of the host star.
KeplerEB-v22.tex
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\begin{document}

\title{Parameters of 20 newly detected eclipsing binaries from the $Kepler$ database}
\titlerunning{Parameters of 20 eclipsing binaries from the $Kepler$ database}
\author{D. Dimitrov\inst{1}, D. Kjurkchieva\inst{2}, V. Radeva\inst{2}}
\authorrunning{D. Dimitrov, D. Kjurkchieva, V. Radeva}
\tocauthor{D. Dimitrov} \institute{Institute of Astronomy, Bulgarian Academy of Sciences
    \and Department of astronomy, Shumen University\newline
    \email{dinko@astro.bas.bg};
    {d.kyurkchieva@shu-bg.net};
   {veselka.radeva@gmail.com} }
%% \papertype can be "research report", "review", "conference talk", "conference poster", %% \ "lecture at scientific

\papertype{conference talk}

\maketitle

\begin{abstract}
The paper presents a sample of newly detected eclipsing binaries from the public $Kepler$ data.
Orbits and fundamental parameters of 20 unknown eclipsing binaries were determined by
modeling of their photometric data. Most of them are well-detached, high-eccentric binaries. We established
that the target KID8552719 satisfied all widespread criteria for a planetary candidate.
Fitting its light curve we obtained radius
R$_{p}$=0.9 R$_{Nept}$, distance to the host star $a$=42.58 R$\sun$=0.198 AU
and equilibrium temperatute T$_{p}$=489 K. These values imply a Neptune-size object out of the
habitable zone of the host star.
\end{abstract}
\keywords{data analysis; eclipsing binaries; star fundamental parameters; planetary systems-stars: individual KID1995732, KID2307206, KID3102000, KID3428468, KID3851949, KID4247023, KID4659255, KID6182849, KID6233483, KID6312534, KID6525209, KID6933781, KID6947666, KID7021177, KID7132542, KID7620844, KID7866921, KID8044608, KID8491745, KID8552719}




\section*{Introduction}

The \emph{Kepler} Mission of NASA is specifically designed (Borucki et al. 2010; Koch et al. 2010; Batalha et al. 2010;
Caldwell et al. 2010; Gilliland et al. 2010) to survey a portion of our region of the Milky Way galaxy to discover
Earth-size planets in/near the habitable zone. The second research area of the \emph{Kepler} mission is
asteroseismology. Moreover some certain objects are observed by ordering of so called "guest-observers".

It was found that one-meter class Schmidt telescope with FoV of 105 square degrees would fulfill the goal of the
\emph{Kepler} mission. This photometer is equipped by 95-megapixel focal plane composed of 42 science CCDs and four
fine guidance sensor CCDs. The CCDs are read out every 6.54 s and
then summed into 29.4 min Long Cadence bins. In addition, up to 512 targets can be observed in Short Cadence mode, at a
59-sec sampling. The observed band spans 423-893 nm, i.e. the \emph{Kepler} magnitudes (Kp) are usually within 0.1 of an R magnitude. The dynamic range is from Kp=7 to Kp=17.

Preliminary counting stars brighter than V=14 from the USNO star catalog, the Cygnus region has been chosen as the
richest area. The Kepler Input Catalog (KIC) of the stars of the observed field (containing 13.2 million targets) was
made preliminary. The photometer sees roughly half million targets. But because it is telemetry-limited, not every
pixel is read out and stored. Only around 190000 pre-selected stars of interest are observed. The selection criteria were determined according to the primary goal of the mission (Batalha et al. 2010).

\emph{Kepler} mission was launched in March 2009. The observations are organized into three-month intervals called
quarters defined by the roll maneuvers the spacecraft executes about its boresight to keep the solar arrays pointed
toward the Sun (Haas et al. 2010). The data packages are processed and analyzed by a Science Pipeline.

2321 planet candidates have already been detected until June 2012, 61 of them are confirmed (Koch et al. 2010, Borucki et al. 2010, Dunham et al. 2010, Latham et al. 2010, etc.).

Another very important achievement of the {\emph{Kepler} mission is discovery of great numbers of variable stars which
light curves are with unprecedented precision. Many eclipsing binaries were discovered and classified automatically on
this rich data base.

Prsa et al. (2011, Paper I) catalogs 1879 eclipsing and ellipsoidal binary systems identified in the first Kepler data
release (Borucki et al. 2010). Slawson et al. (2011, Paper II) provide an updated catalog augmented with the second \emph{Kepler} data release which
increases the baseline nearly to 125 days. As a result 386 new systems have been added while 100 systems have been
removed from the previous catalog. With these changes, the total number of identified eclipsing binary systems in the
\emph{Kepler} field-of-view has increased to 2165, that is 1.4 $\%$ of the Kepler target stars.

The detection of the EBs presented in the foregoing catalogs are based primarily on the initial pipeline calibrated
light curves. Prsa et al. (2011) used automated approach to identify plausible EBs, which entails morphological classification of each light curve's power spectrum.
Blomme (2011) proposed improvement of the method for automate classification.

Answering to the appeal to use the available resources of the {\emph{Kepler} database for additional research we tried
to search for additional eclipsing binaries using the public data from \emph{Kepler} sets Q0, Q1 and Q2. This paper
presents the procedure and results from this work.



\section{Our searching method}

Our searching of eclipsing binaries began in 2011 on the basis of the public data of quarters Q0-Q2 of the {\emph{Kepler} mission. Initially we used the data from the web-based NASA Exoplanet Archive
http://exoplanetarchive.ipac.caltech.edu/\\
applications/ETSS/Kepler/
index.html. Further we used also the access to these data via
ftp://130.167.252.39/pub/kepler/lightcurves/. It should be noted that we considered
only the long cadence data because the short cadence ones were with bigger scatter

The photometric data for each quarter and KID are calibrated for bias (dark level) and converted to fluxes. They are available in two forms: "RAW" and "CORR".

Light curves for all observed stars (processed on a quarterly basis at NASA Ames Research Center) are placed in the
archive. Users of {\emph{Kepler} data might work with both versions of the light curves. Particularly, everyone may use
de-trended data or make de-trending himself.

During 2011 the web-based NASA Exoplanet Archive contained not only stellar parameters (magnitudes, temperatures, etc.) but also the statistical parameters of their light curvesl
"Light curve chi-squared", "Points in light curve beyond 5 $\sigma$" and "Fraction of points in light curve beyond 5 $\sigma$".
We used the values of these statistical parameters to search for eclipsing binaries and managed to pick around thousand EB candidates. Unfortunately, the web-based NASA Exoplanet Archive do not contain yet the foregoing statistical parameters and the considered method for selection of EB candidates is not applicable.

The next step was visual examination of our EB candidates. It revealed that most of them are false positives and only around hundred are true EB.

Besides the foregoing approach we made visual inspection of all light curves of one third of the Kepler data (until folder 0040 from the downloaded ftp data).

As a result of these two ways of searching we gathered candidates that were out of the published catalogs of $Kepler$ eclipsing binaries (Prsa' catalog version 2.0).

Further we checked if some of these candidates were known variables (to the middle of May 2012). For this aim we used:

(i) Lists of Planetary Candidates, False Positives and Eclipsing Binaries from the site
http://archive.stsci.edu/kepler/results.html;

(ii) The AAVSO database of variable stars (International Variable Star Index)

(iii) Databases SIMBAD and ADS.

Several candidates turned out known variables and were removed from our sample.
Thus we made the first version of our list of EB candidates.

In this paper we present part of the newly detected eclipsing stars satisfying the additional condition
to have at least 3 eclipses from different type.

During the visual inspection of the light curves of the \emph{Kepler} database we established that they need additional
preliminary "manual" treatment before detailed analysis because the maximum fluxes as well as the light amplitudes for
many stars differ from one quarter (even subset) to another. Moreover, the "CORR" data are not always properly
de-trended. That is why we decided to use the RAW data of our targets and to made own normalization and de-trending of
the data. For this aim the data from each subset were reproduced by spline function and normalized separately.

At the beginning of 2012 when the quarters Q3-Q6 became free-accessed we used the new data
for more precise determination of the ephemeres of our targets.

The last examination of our targets consisted in checking for possible mis-classified of variability of some target as a result of
contamination of nearby known binary with the same period. This effect is due to the high star density near the
galactic plane and to the fact that the \emph{Kepler} pixels projected onto 4 arcsec on the sky. Thus, for instance, we found that the unknown variable star KID3098197 (detected by us) and the known EB star KID3098194 (Paper I) at distance 4 arcsec have the same period and type of variability (Fig. 1). It is difficulty to say which of
these stars is the true variable because the contamination depends on the relative magnitude of the stars in question
and their separation on the sky. As a result of the examination for contamination effect (into area with radius 60
arcsec around our candidates) several candidates as KID3098197 were excluded from our list.

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KICneihbour3.eps, width=0.95\textwidth}}
    \caption[]{Illustration of contamination effect by the stars KID3098194 and KID3098197}
    \label{1}
  \end{center}
\end{figure}



\section{Light curve modeling}

As a result of our searching method we found around 150 newly detected EB from the \emph{Kepler} database
Q0-Q2. This paper presents 20 of them (Sample 1) which periods and light curves are well determined and allow detailed
analysis. Table 1 presents information for their coordinates and ephemeres while Figure 2 shows fields around them with sizes 1 arcmin.

\begin{table}
\begin{center}
\caption{Coordinates and ephemeres of the targets from Sample 1}
\begin{tabular}{ccccr}
\hline
\\
KID     & RA[2000]       & DEC[2000]      &  BJD0           &   Period  \\
\\
\hline
\\
1995732 & 19h 04m 51.84s & 37d 25m 30.86s & 2455049.45692971 & 77.363032  \\
2307206 & 19h 29m 30.28s & 37d 39m 26.86s & 2455086.53717057 &204.030667  \\
3102000 & 19h 09m 23.87s & 38d 17m 09.74s & 2454997.25556938 & 57.059216  \\
3428468 & 19h 06m 53.61s & 38d 35m 44.38s & 2455032.44996961 &114.908636  \\
3851949 & 19h 27m 36.80s & 38d 55m 33.10s & 2454976.78185172 & 54.776991  \\
4247023 & 19h 07m 23.64s & 39d 18m 17.78s & 2455061.78039575 & 47.189567  \\
4659255 & 19h 32m 11.61s & 39d 43m 31.26s & 2455067.15120620 &198.014033  \\
6182849 & 18h 52m 17.77s & 41d 32m 27.17s & 2454967.70080728 &  6.399107  \\
6233483 & 19h 56m 12.01s & 41d 32m 14.82s & 2454976.85610603 & 15.873552  \\
6312534 & 19h 55m 32.15s & 41d 39m 43.49s & 2454965.94158660 &  3.015550  \\
6525209 & 19h 30m 53.13s & 41d 54m 17.71s & 2455017.42871952 & 75.131944  \\
6933781 & 19h 06m 47.36s & 42d 27m 04.18s & 2455062.75755611 &130.419512  \\
6947666 & 19h 26m 01.46s & 42d 26m 53.20s & 2455071.15247452 & 56.687032  \\
7021177 & 19h 10m 32.89s & 42d 31m 50.95s & 2455017.49723690 & 18.645334  \\
7132542 & 19h 43m 32.45s & 42d 37m 18.77s & 2455067.74039272 & 66.360950  \\
7620844 & 19h 42m 26.49s & 43d 15m 37.51s & 2455070.18823707 & 58.621582  \\
7866921 & 18h 39m 25.46s & 43d 40m 04.44s & 2455107.26924060 & 91.500871  \\
8044608 & 19h 47m 36.97s & 43d 49m 26.00s & 2455067.64037980 &106.175893  \\
8491745 & 19h 22m 02.79s & 44d 33m 21.67s & 2455059.64770915 &111.320439  \\
8552719 & 19h 15m 53.20s & 44d 37m 28.31s & 2455009.27199064 & 88.407500  \\
\end{tabular}
\end{center}
\end{table}

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KICtotalmaps4.eps, width=0.7\textwidth}}
    \caption[]{Fields around the targets (at the centers) with size 1 arcmin}
    \label{2}
  \end{center}
\end{figure}

Figures 3-6 exhibit the parts of the phased light curves around the eclipses (the longer out-of-eclipse parts are almost flat).

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=fig01.eps, width=0.99\textwidth}}
    \caption[]{Eclipses of KID1995732, KID2307206, KID3102000, KID3428468, KID3851949, KID4247023 and their fits}
    \label{3}
  \end{center}
\end{figure}

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=fig02.eps, width=0.99\textwidth}}
    \caption[]{Eclipses of KID4659255, KID6182849, KID6233483, KID6312534, KID6525209, KID6933781 and their fits}
    \label{4}
  \end{center}
\end{figure}

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=fig03.eps, width=0.99\textwidth}}
    \caption[]{Eclipses of KID6947666, KID7021177, KID7132542, KID7620844, KID7866921, KID8044608 and their fits}
    \label{5}
  \end{center}
\end{figure}

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=fig04.eps, width=0.99\textwidth}}
    \caption[]{Eclipses of KID8491745, KID8552719 and their fits}
    \label{6}
  \end{center}
\end{figure}

Table 2 summarizes the parameters of the eclipses (phase of the secondary eclipse $\varphi_{2}$, durations $d_{i}$ and
amplitudes $A_{i}$ of the two minima) as well as the orbit parameters $e$ and $\omega$ determined by modeling.

\begin{table}
\begin{center}
\caption{Parameters of the eclipses and the orbit of the targets}
\begin{tabular}{crcrcccr}
\hline
\\
KID & $\varphi_{2}$ & $d_{1}$&$ d_{2}$& $A_{1}$& $A_{2}$ & $e$          & $\omega$        \\
        &        & days   & days   & mag    & mag    &                  & 			\\
\hline
\\
1995732 & 0.4165 & 0.4951 & 0.5415 & 0.1430 & 0.1040 &	0.14252	&	157.08	\\
2307206 & 0.5071 & 0.7141 & 0.4897 & 0.7600 & 0.3410 &	0.17664	&	273.55	\\
3102000 & 0.0790 & 0.3081 & 0.2970 & 0.0950 & 0.0045 &	0.73492	&	181.77	\\
3428468 & 0.0787 & 0.3103 & 0.1724 & 0.3100 & 0.1800 &	0.77405	&	207.65	\\
3851949 & 0.6425 & 1.5007 & 1.0187 & 0.0080 & 0.0020 &	0.29014	&	319.65	\\
4247023 & 0.2891 & 0.4719 & 0.3303 & 0.6570 & 0.4920 &	0.37693	&	151.88	\\
4659255 & 0.4599 & 0.4040 & 0.3723 & 0.1900 & 0.0450 &	0.07572	&	213.66	\\
6182849 & 0.5000 & 0.2240 & 0.2150 & 0.5240 & 0.1388 &	0.01178	&	269.91	\\
6233483 & 0.4813 & 0.3492 & 0.3175 & 0.0132 & 0.0047 &	0.05569	&	238.72	\\
6312534 & 0.5000 & 0.1206 & 0.1206 & 0.0203 & 0.0087 &	0.00115	&	 15.42	\\
6525209 & 0.2176 & 0.8565 & 0.3757 & 0.1480 & 0.0399 &	0.58949	&	224.72	\\
6933781 & 0.8044 & 0.1826 & 0.3391 & 0.0033 & 0.0014 &	0.56295	&	 32.14	\\
6947666 & 0.1260 & 0.2834 & 0.2834 & 0.0628 & 0.0019 &	0.63304	&	175.39	\\
7021177 & 0.5543 & 0.1604 & 0.5482 & 0.7088 & 0.3385 &	0.57877	&	 83.09	\\
7132542 & 0.2632 & 0.8361 & 0.7831 & 0.6767 & 0.6277 &	0.38159	&	182.84	\\
7620844 & 0.5416 & 0.3517 & 0.2579 & 0.3500 & 0.0892 &	0.18617	&	290.21	\\
7866921 & 0.3814 & 0.7869 & 0.6497 & 0.0760 & 0.0430 &	0.22484	&	214.15	\\
8044608 & 0.8510 & 0.4247 & 0.3716 & 0.2019 & 0.0283 &	0.58766	&	356.54	\\
8491745 & 0.5973 & 0.9574 & 0.9462 & 0.0712 & 0.0158 &	0.15338	&	  0.33	\\
8552719 & 0.5000 & 0.7073 & 0.7073 & 0.0020 & 0.0000 &	0.00000	&	180.00	\\
\end{tabular}
\end{center}
\end{table}

The qualitative analysis of the light curves led to the following notes.

(1) The secondary eclipses of KID3102000 and KID6947666 are around 10 times shallower than the primary minimum.

(2) The flat bottoms of the secondary eclipses of KID3851949, KID6182849, KID6233483, KID6525209, KID7866921, KID8491745 imply
occultations.

(3) The light curve of the most targets exhibits different duration of the two eclipse minima and/or the secondary
minimum is shifted from phase 0.5 that are sure evidences of eccentric orbits (Table 2). The selection effect could explain
partially such a result because the eccentric systems can be identified more surely. Another reason for the relative
big number eccentric orbits is the relative large orbital periods of the targets from our Sample 1. It is known
that eccentric orbits are not too infrequent among well-separated systems of long periods.

The quantitative analysis of the targets was made by modeling of their light curves using the software $PHOEBE$ (Prsa $\&$ Zwitter
2005), the values of the mean temperatures $T_{m}$ from the Kepler Input Catalog (Batalha et al. 2010) and the
limb-darkening coefficients derived by Sing (2009) especially to the \emph{Kepler} wide, nonstandard response function
and avoiding the major deficiency present at the limbs of the 1D stellar models.

It is known that the modeling of eccentric binaries requires much time and sometimes is very difficult without any guessed input values
of the fitted parameters. That is why we calculated preliminary values of the eccentricity $e$ and periastron
angle $\omega$ by the analytical formulae of Kopal (1959). Their using as input parameters shortened considerably the
modeling time. Another trick in this direction was the averaging the huge number of data points out of the eclipses
into phase bins.

The fitting parameters of our procedure and their values derived as a result of the light curve solutions are shown in
Table 3 which columns are: mean temperature T$_{m}$; the ratio of the temperatures of the components
$T_{2}/T_{1}$; orbital inclination $i$; photometric mass ratio $q$; relative radii $r_{1}$ and $r_{2}$; third light L3.
The values of the rest fitting parameters (initial epoch BJD0, period $P$; eccentricity $e$ and periastron angle
$\omega$) are given in Tables 1-2. The fits of the minima of some targets are not perfect and may be considered as preliminary ones. The next public data will be used for improving of these models.

\begin{table}
\begin{center}
\caption{Fundamental parameters of the binaries from Sample 1}
\begin{tabular}{ccrcrrrc}
\hline
\\
KID		& T$_{m}$ & $T_{2}/T_{1}$ &	$i$		&	$q$	&	$r_{1}$	&	$r_{2}$	&	L3	\\
\hline
\\
1995732	&	5163	&	0.959	&	89.1715	&	0.450	&	0.01902	&	0.00689	&	0.1264\\
2307206	&	5342	&	0.897	&	89.8847	&	0.787	&	0.00536	&	0.00514	&	0.0037\\
3102000	&	5718	&	0.683	&	89.9889	&	0.218	&	0.02003	&	0.00472	&	0.0000\\
3428468	&	4279	&	0.860	&	89.3941	&	1.830	&	0.00597	&	0.00506	&	0.0000\\
3851949	&	4981	&	0.840	&	88.8893	&	0.102	&	0.07074	&	0.00549	&	0.0000\\
4247023	&	5424	&	0.987	&	89.6098	&	1.003	&	0.01492	&	0.01459	&	0.0000\\
4659255	&	5153	&	0.784	&	89.6561	&	0.992	&	0.00425	&	0.00444	&	0.0000\\
6182849	&	5893	&	0.816	&	89.2096	&	1.254	&	0.06713	&	0.04041	&	0.0003\\
6233483	&	5942	&	0.808	&	86.8016	&	1.000	&	0.06943	&	0.00991	&	0.0000\\
6312534	&	4897	&	0.894	&	77.3068	&	0.300	&	0.01480	&	0.09830	&	0.1307\\
6525209	&	5207	&	0.851	&	89.5055	&	0.450	&	0.02113	&	0.00690	&	0.0000\\
6933781	&	5502	&	1.045	&	89.6300	&	1.000	&	0.00362	&	0.00579	&	0.9850\\
6947666	&	5777	&	0.629	&	88.8576	&	0.080	&	0.02041	&	0.00456	&	0.0000\\
7021177	&	5684	&	0.985	&	89.2692	&	1.000	&	0.02896	&	0.02442	&	0.0000\\
7132542	&	5389	&	0.989	&	89.5995	&	1.260	&	0.01929	&	0.02335	&	0.0000\\
7620844	&	5056	&	0.741	&	89.1450	&	1.000	&	0.01070	&	0.01265	&	0.0000\\
7866921	&	5019	&	0.904	&	89.0497	&	0.202	&	0.02444	&	0.00629	&	0.0000\\
8044608	&	5788	&	0.718	&	89.1088	&	0.350	&	0.01207	&	0.00666	&	0.0000\\
8491745	&	4839	&	0.837	&	89.4061	&	0.236	&	0.02405	&	0.00564	&	0.0000\\
8552719	&	5114	&	0.196	&	89.4149	&	0.038	&	0.02009	&	0.00080	&	0.0000\\
\end{tabular}
\end{center}
\end{table}



\section{Analysis and comments on the results}

The analysis of the obtained parameters led to several important conclusions.

(1) Almost all orbital inclinations, excluding the shortest-period target KID6312534, are near 90$^{0}$ that is normal
for long-period eclipsing binaries.

(2) The relative stellar radii are less 0.07 that means that the systems are well-detached.

(3) The temperatures of stellar components are in the range 3500-6000 K. The primaries are the hotter components. The temperatures of the secondaries are smaller with less 1500 K than those of the primaries. The only exclusion is the target KID8552719 which secondary' temperature is of planetary' order.

(4) The values of the photometric mass ratio $q$ are in the range 0.20-1.83. It shoult be noted that the $q$ values are precisely determined only for the targets with total eclipses.

(5) Although the presence of eccentric systems in our sample was expected (Table 2) it was surprising to find 7 of the
20 targets to have $e > $0.5 (the biggest value is $e$=0.77). It should be noted that the final values of the
eccentricity and periastron angle differ from the preliminary ones by only several $\%$.

The examination of the Eclipsing Binary with Eccentric Orbits Catalog (Bulut $\&$ Demircan 2007) revealed that 22 targets have $e >$ 0.3 and only 2 of them are with $e >$ 0.5. In fact, this catalog
containing information for 124 systems with eccentric orbits, at present is the largest catalogue of eccentric binaries compiled from the literature including three large sources Hipparcos catalogue, the atlas of Kreiner, Kim $\&$ Nha (2001) and the ninth catalogue of spectroscopic binary orbits (Pourbaix et al. 2004).

The examination of the catalogs from PaperI and PaperII revealed that 1376 are eccentric systems: 7 with $e >$ 0.6; 34 with $e >$0.5; 184 with $e >$ 0.3; 799 with $e >$ 0.1 (the biggest value is $e$=0.64).

It should be noted that the most eccentric binary 41 Dra has a period of 1247 d and $e$=0.97. The last value is
determined by radial velocity curve (Tokovinin et al. 2003).

The presented statistics exhibit the relative big frequency of high-eccentric targets in our Sample 1. We attributed
this result mainly to the huge duration of uninterrupted observations made by Kepler.

(6) Besides the eclipses with orbital period of P$_{orb}$=3.0156 d the target KID6312534 exhibits a variability with
amplitudes around 4.5 times smaller than the depths of the primary eclipses and
a period of around P$_{2}$=3.005 days which values slightly change from one subset to another.
It is reasonable to attribute the second variability to spots and the period P$_{2}$ to the stellar rotation.
This means that KID6312534 is synchroneous that is normal for a such orbital period. The small
changes of P$_{2}$ may due to the differential rotation of the spotted star. It should be noted that there were several subsets in which the spot variability lacks at all. This fact may due to some artificial effect. 

After the submission of our manuscript we were informed that KID6312534 is known eclipsing binary which light curve has been 
investigated by Coughlin et al. (2011). The reason of this discrepancy is that this target presents in the Prsa' catalog version
1.0 but misses in the newer version 2.0 we checked.  

(7) The modeling of KID6933781 was possible only with huge value L3=0.98. This result implies that the modeled light
variability does not belong to the observed star but rather to a nearby star which light enters into the aperture around
the observed target. The map of KID6933781 (Fig. 3) revealed central bright star and faint star at distance of 10
arcsec or 2.5 pix. Taking into account that the aperture of the $Kepler$ photometry is with radius 5-6 pix it is
reasonable to suppose that the eclipsing star in this case is the faint star.

(8) Besides the binary period of 18.6 days the system KID7021177 exhibits light changes with a period of P=6.355932
days (Fig. 8) which light curve means possible rotational variability (caused by spots, etc.).

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KIC7021177spot.eps, width=0.9\textwidth}}
    \caption[]{The additional (rotation) variability of KID7021177 and its folded curve}
    \label{8}
  \end{center}
\end{figure}

(9) The depth of the primary eclipse of KID8552719 is only 0.002 mag and there
is not any indication of a secondary eclipse (Fig. 6). Hence, this target reveals
behavior of an exoplanet candidate. The shape of the light minimum also
resembles transit event (not V-shape).



\section{The exoplanet candidate KID8552719}

The planet detection passes through data validation (DV)
and follow-up observations (FOP). DV performs false-positive
elimination from diagnostics that can be pulled out of the \emph{Kepler}
data itself (Batalha et al. 2010), while the FOP relies on additional observations such
as moderate and high-precision spectroscopic radial velocities.

If the modeled light curve of given exoplanet candidate
leads to radius $<$ 2R$_{J}$ it is assigned a Kepler Object of Interest (KOI) number.
But only those candidates that pass the DV tests are submitted to
the follow-up observers for spectroscopic vetting, confirmation,
and characterization. Candidates with a companion radius larger than 2R$_{J}$ are likely associated
with late M dwarfs and are not considered as high-priority planetary candidates.

The goal of the DV tests is to eliminate the false positives caused by either
grazing or diluted eclipsing binaries.

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KIC8552719_model.eps, width=0.7\textwidth}}
    \caption[]{Model of KID8552719 by our code}
    \label{9}
  \end{center}
\end{figure}

We used own code (Kjurkchieva $\&$ Dimitrov, 2012)
to model the light curve of KID8552719.
For this aim we retrieved the star parameters from the Kepler Input Catalog:
T$_{s}$=5114 K (Sp K0 V); R$_{s}$=0.822 R$\sun$; $\lg g_{s}$=4.56.
We calculated the stellar mass M$_{s}$=0.94 M$\sun$. With these
initial values a transit fit was computed (Fig. 9).
In fact, the fitted parameters were R$_{s}$/a, R$_{p}$/R$_{s}$, orbital inclination $i$,
limb-darkening coefficient $u$, initial epoch T0 and period $P$.

As a result of modeling we obtained: orbital inclination $i$=89$^{0}$.53;
orbital radius $a$=42.58 R$\sun$=0.19757 AU; R$_{p}$=0.0321 R$\sun$=0.315 R$_{J}$=0.9 R$_{Nept}$.
Thus, KID8852719 turned out almost Neptune-sized object and passed
the first criterion for exoplanet candidate.

The next criterion (Batalha et al. 2010) required modeling of the odd
and even numbered transits independently.
A significant difference in the companion radii (10 $\sigma$ difference) for the odd and even transit
implies that this system is likely a diluted EB at twice the orbital period.
Our candidate did not reveal considerable difference of the odd and even transits
and passed this criterion.

A false positive can be identified by presence of secondary events at phase 0.5
with depth greater than 2$\sigma$. Our examination for phase 0.5 did not reveal
such a event. In any case, in order to escape cases as KID310200 and KID694766 (see Figs. 3 and 4)
with shallow secondary events far away from phase 0.5, we examined the whole
light curve of KID8552719 but did not find such a secondary event.
Hence, our candidate passed this test as well.

Assuming the star and companion behave as black bodies
we estimated the equilibrium temperature T$_{eq}$ of the secondary component
of KID8552719 by the formula (Batalha et al. 2012)
\begin{equation}
T_{eq} = T_{s}(R_{s}/2a)^{1/2}[f (1 - A_{B})]^{1/4}
\end{equation}
where $A_{B}$ is a Bond albedo and $f$ is a a proxy for atmospheric thermal circulation.
Using the values $A_{B}$=0.1 (for highly irradiated planets, Rowe
et al. 2006) and $f$=1 for efficient heat distribution to the
nightside of planet we obtained a rough estimate for the dayside
temperature of the secondary T$_{eq}$=489 K. This value is nearly that of dayside Mercury
and is suitable to a planet. It should be noted that it is higher than the temperature limit
of the habitable zone of the host star.

% hot Jupiter planet candidates (Jupiter-size candidates with orbital periods near 3 days)
% warm Jupiters (with slightly larger orbits) and hot Neptune-size candidates

The next test for false positives is checking of possible shift of the photocenter
just at the transit (Batalha et al. 2010).
If there are transit-like features in both the row and column centroid residuals and they
are highly correlated with the transit features in the flux time series this is evidence of
a diluted EB, i.e. false positive. In our case there were not any shifts of the photocenter of KID8552719
during the transits.

Another diagnostics to confirm the identity of the transiting
(or eclipsing) object is to examine the spatial flux distributions and
to find if the out-of-transit photocenter is centered on the target star.
For this test one should compare the out-of-transit image with
the difference image. If their brightest pixels are different then the event is
possible a false positive. The last step is to make a time series analysis
of the brightest pixels that confirms which is the source of the transit
variability.

The planetary candidate KID8552719 passed also all photocenter motion diagnostics
(the centroid time series, the difference image, and the pixel flux time series) and
it may be included in the next version of the planetary candidate catalog.
We estimated that if the planet mass is near that of Neptune (as its radius)
then the mass ratio of the system should be around 10000 and the effect on the radial
velocity of the host star would be around 1 m/s.

During the final stage of preparation of this manuscript we found a paper of
Huang, Bakos and Hartman appeared in the astro-ph.EP on May 29 2012 (Paper III).
These authors reported new 16 planetary candidates based on searching for in the Q1-Q6 public data.
One of them is KID8552719.

Huang, Bakos $\&$ Hartman (2012) used the formalism of Mandel $\&$ Agol (2002) and
fitted the parameters R$_{p}$/R$_{s}$, the square of the impact parameter  $b$=$a \cos i$/ R$_{s}$
and the inverse of half duration $\zeta$/R$_{s}$ = 2/T$_{dur}$ that is related to a/R$_{s}$ and the impact parameter $b$.
	 	
The comparison of our results with those in Paper III revealed that the values of the planetary radius coincide within 1 $\%$ while the values of the rest geometric parameters
(orbital inclination and semi-major axis) differ by 2 $\%$. We attributed the last differences  to the different methods of normalization of the $Kepler$ data.

There is not estimation of the planet temperature in Paper III.


\section{Conclusion}

Applying own searching method for eclipsing binaries to the public
$Kepler$ database Q0-Q2 we detected candidates that were out of the published catalogs of the  $Kepler$ eclipsing stars.

This paper presents the results of our light curve solutions of 20 newly detected eclipsing binaries and the values of their orbital and fundamental parameters. Most of them turned out binaries
with high-eccentric orbits and consequently present appropriate targets for study of apsidal motion and the internal structure of the component stars.

Some of our discoveries have interesting peculiarities. We confirmed the conclusion of Huang, Bakos $\&$ Hartman (2012) that KID8552719 satisfied the criteria for a planetary candidate. The estimations for its physical parameters revealed the Neptune-size object out of the habitable zone of the host star.

Hence, the softwares do are indispensable for an automatic processing and analysis of a huge data-sets of the space missions as \emph{Kepler} but the obtained results in this
paper revealed that it is deserved to examine such data-sets "manually/visually" in order to compensate the omission of
some interesting objects and events, available in the database but not registered by the software. At first glance this
time-consuming work seems boring and requires patience and attention. But it is a true pleasure to see the wonderful
light curves of the \emph{Kepler} mission!

	
\section*{Acknowledgements}
This study is supported by funds of the project DO 02-362 of the Bulgarian Ministry of education and science. is
partially supported by projects DO 02-362, DO 02-85 and DDVU 02/40-2010 of the Bulgarian National Science Fund.

This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology,
under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program, the SIMBAD 
database, operated at CDS, Strasbourg, France, and NASA's Astrophysics
Data System Abstract Service.


\begin{thebibliography}{}

Batalha N. et al., 2010, ApJ 713L, 109 \\

Batalha N. et al., 2012,arXiv:1202.5852 \\

Blomme J. et al., 2011, MNRAS 418, 96 \\

Borucki W. et al., 2010, Sci 327, 977 \\

Bulut, I., Demircan O., 2007, MNRAS 378, 179 \\

Caldwell D. et al., 2010, SPIE 7731E, 30 \\

Coughlin J., Lopez-Morales M.,  Harrison T.,  Ule N.,  Hoffman D. , 2011, AJ 141, 78

Dunham E. et al., 2010, ApJ 713L, 136D\\

Gilliland R. et al., 2010, ApJ 713L, 60 \\

Haas M. et al. 2010, ApJ 713L, 115 \\

Howarth D., 2010, MNRAS 413, arXiv: 1011.2631\\

Huang X., Bakos G., Hartman J, 2012, arXiv:1205.6492\\

Kjurkchieva D., Dimitrov D., 2012, IAUS 282, 474\\

Koch D. et al. 2010, ApJ 713L, 131\\

Kopal Z., 1959, Close Binary stars, The Iternational Astrophysical Series v.5 \\

Kreiner J., Kim C., Nha I., 2001, aocd.book \\

Latham D. et al. 2010, ApJ 713L, 140L\\

Pourbaix D. et al., 2004, 2004, A $\&$ A 424, 727 \\

Prsa A., Zwitter T., 2005, ApJ, 628, 426\\

Prsa A. et al., 2011, AJ 141, 83 \\

Rowe J. et al., 2006, ApJ 646,1241\\

Sing K., 2009, $A \& A$ 510, 21\\

Slawson R. et al., 2011, AJ 142, 160\\

Tokovinin A. et al., 2003, A $\&$ A 409, 245 \\

\end{thebibliography}

\end{document}





The examination of the \emph{Eclipsing Binary with Eccentric Orbits Catalog} (Bulut $\&$ Demircan 2007) revealed that
22 targets among 124 eccentric binaries have $e > 0.3$ and only 2 of them are with $e > 0.5$. In fact this catalog
containing information for 124 systems with eccentric orbits at present is the largest catalogue of eccentric binaries
compiled from the literature including three large sources Hipparcos catalogue, the atlas of Kreiner, Kim $\&$ Nha
(2001) and the ninth catalogue of spectroscopic binary orbits (Pourbaix et al. 2004). This catalog presents also
information about 150 candidate eclipsing binaries with eccentric orbits (with incomplete photometric observations) but
their eccentricities are still undetermined.

The examination of the catalog of Prsa et al. (2011, Paper I) containing 1879 eclipsing and ellipsoidal stars revealed
that 1376 are eccentric systems: 7 with $e > 0.6$; 34 with $e > 0.5$; 184 with $e > 0.3$; 799 with $e > 0.1$ (the
biggest value is $e=0.64$). The orbital periods are in the range [2d, 100 d] with exception of 2 targets with $P > 100
d$ (37 have $P > 50 d$).

It should be noted that the most eccentric binary 41 Dra has a period of 1247 d and $e$=0.97. The last value is
determined by radial velocity curve (Tokovinin et al. 2003).

The presented statistics exhibits the relative big frequency of high-eccentric targets in our Sample 1. We attributed
this result mainly to the huge duration of uninterrupted observations made by \emph{Kepler}.

(6) Besides the eclipses with orbital period of $P_{orb}$=3.0156 d the target KID6312534 exhibits a variability with
smaller amplitudes compared with the eclipses and a period of $P_{2}$=3.005 days (Fig. 13) which values slightly change
from one subset to another. It is reasonable to attribute the second variability to spots and the second period to the
stellar rotation (although the light curve shape of this variability resembles also pulsation type). This means that
the eclipsing system is synchroneous that is normal for a such small orbital period. In fact, KID6312534 is the target
with the shortest orbital period in our sample. The slight changes of $P_{2}$ may be explained by differential rotation
of the spotted star.

We noted that the light amplitudes of the spot variability increases/decreases from one sub-run to another
simultaneously with the increasing/decreasing of the eclipse depths. This means that the two variabilities belong to
one star. The very deep light analysis of the area around KID6312534 with several close stars revealed that the
detected variabilities originate rather from neighbor star. Moreover, there are several subsets in which the second
variability lacks at all. It may due to some artificial effect.

Hence, additional ground-base observations may provide information which is the variable star.

(7) Besides the binary period of 18.6 days the system KID7021177 exhibits light changes with a period of P=6.355932
days (Fig. 14) which light curve means possible rotational variability (caused by spots, ellipsoidal stars, etc.).

(8) The depth of the primary eclipse of KID8552719 is only 0.002 mag and there is not indication of a secondary
eclipse. That is why this binary was suspected as a planetary system. We plan to carry out spectral observations in
order to confirm or reject this assumption.

(9) About half targets of our sample revealed deviations of the light center during the eclipses from the common trend
of the shift of the light center during the quarter (increasing, decreasing or parabolic). We established that the
values of these deviations are different for the two eclipses, bigger for the deeper eclipse. They do not depend on the
coordinates, period, eccentricity, eclipse depth, $\varphi_{2}$, $\omega$ of the targets. We did not find correlation
between the direction of the deviations (up or down) during the eclipses and the foregoing parameters as well as the
common trend of the shift of the light center during the quarter (increasing, decreasing or parabolic). The values of
the x-deviations and y-deviations during the eclipses do not exceed 0.1 pixel and change between the quarters Q1 and Q6
by a factor up to 6-7. The target KID 2307206 exhibits even change of the direction of the y-deviations during the
eclipses between the quarters Q1 and Q6.

Initially, we thought that the considered effect is caused by contamination of nearby stars. But their presence should
be appeared as L$_{3}$ while our modeling did not reveal such a result. Pure physical and geometric considerations also
reject the assumption that contamination of nearby stars may cause the established deviation of the light center during
the eclipses for some binaries. This effect requires separate study in order to derive additional information about the
binaries.


%The position of the light center of the target changes between the quarters Q1 and Q6 by up to 5-6 pixels.

%The light position of the targets shift on pixel frame nonsynchonous during the quarters (every star separately).







\section{Conclusion}

Applying own selection procedure and criteria for searching for eclipsing binaries in the public $Kepler$ database Q0,
Q1, Q2 we detected candidates that have been missed by the automatic discovery of the pipe-line.

This paper presents the results of the determination of the orbits and fundamental parameters of 20 newly-detected
eclipsing binaries entering our Sample 1 and obtained by modelling of their photometric data. Most of them are binary
with high-eccentric orbits and present appropriate targets for study of apsidal motion and hence the internal structure
of the component stars.

Some of our discoveries have interesting peculiarities. Hence, the softwares do are indispensable for an automatic
processing and analyzing of a huge data-sets of the space missions as \emph{Kepler} but the obtained results in this
paper revealed that it is deserved to examine such data-sets "manually/visually" in order to compensate the omission of
some interesting objects and events, available in the database but not registered by the software. At first glance this
time-consuming work seems boring and requires patience and attention. But it is a true pleasure to see the wonderful
light curves of the \emph{Kepler} mission!






KID	e	w		d Phase	BJD	Period	Tmean	T2/T1	incl.	q	om1	om2	R1	R2	L3 1995732	0.14252	157.08	2.74156	
-0.04003	2455049.45692971	77.363032	5163	0.959	89.1715	0.450	53.090	66.749	0.1902	0.0689	0.1264
2307206	0.17664	273.55	4.77430	0.00396	2455086.53717057	204.030667	5342	0.897	89.8847	0.787	187.483	191.214	 
0.0536	0.0514	0.0037 3102000	0.73492	181.77	3.17243	-0.21400	2454997.25556938	57.059216	5718	0.683	
89.9889	0.218	50.779	50.490	0.2003	0.0472	0.0000 3428468	0.77405	207.65	3.62410	-0.26500	2455032.44996961	 
114.908636	4279	0.860	89.3941	1.830	175.705	365.442	0.0597	0.0506	0.0000 3851949	0.29014	319.65	5.57896	
0.08000	2454976.78185172	54.776991	4981	0.840	88.8893	0.102	14.282	20.444	0.7074	0.0549	0.0000 4247023	 
0.37693	151.88	2.65076	-0.09150	2455061.78039575	47.189567	5424	0.987	89.6098	1.003	68.747	70.456	
0.1492	0.1459	0.0000 4659255	0.07572	213.66	3.72915	-0.02070	2455067.15120620	198.014033	5153	0.784	
89.6561	0.992	236.145	224.879	0.0425	0.0444	0.0000 6182849	0.01178	269.91	4.71082	0.00000	2454967.70080728	
6.399107	5893	0.816	89.2096	1.254	16.168	31.917	0.6713	0.4041	0.0003 6233483	0.05569	238.72	4.16648	
-0.00950	2454976.85610603	15.873552	5942	0.808	86.8016	1.000	15.466	101.985	0.6943	0.0991	0.0000
6312534	0.00115	15.42	0.26919	0.00000	2454965.94158660	3.015550	4897	0.894	77.3068	0.300	7.067	4.407	 
1.4800	0.9830	0.1307 6525209	0.58949	224.72	3.92209	-0.18500	2455017.42871952	75.131944	5207	0.851	
89.5055	0.450	48.422	67.949	0.2113	0.0690	0.0000 6933781	0.56295	32.14	0.56100	0.11850	2455062.75755611	
130.419512	5502	1.045	89.6300	1.000	278.599	175.000	0.0362	0.0579	0.9850 6947666	0.63304	175.39	3.06111	
-0.18000	2455071.15247452	56.687032	5777	0.629	88.8576	0.080	49.220	20.724	0.2041	0.0456	0.0000
7021177	0.57877	83.09	1.45025	0.01500	2455017.49723690	18.645334	5684	0.985	89.2692	1.000	36.909	43.333	 
0.2896	0.2442	0.0000 7132542	0.38159	182.84	3.19109	-0.12000	2455067.74039272	66.360950	5389	0.989	
89.5995	1.260	53.867	55.455	0.1929	0.2335	0.0000 7620844	0.18617	290.21	5.06507	0.02350	2455070.18823707	
58.621582	5056	0.741	89.1450	1.000	94.670	80.265	0.1070	0.1265	0.0000 7866921	0.22484	214.15	3.73760	
-0.06500	2455107.26924060	91.5008708	5019	0.904	89.0497	0.202	41.182	33.851	0.2444	0.0629	0.0000
8044608	0.58766	356.54	6.22271	0.18000	2455067.64037980	106.175893	5788	0.718	89.1088	0.350	83.692	55.295	 
0.1207	0.0666	0.0000 8491745	0.15338	0.33	0.00584	0.04860	2455059.64770915	111.320439	4839	0.837	89.4061	 
0.236	41.861	43.424	0.2405	0.0564	0.0000 8552719	0.00000	180.00	3.14159	0.00000	2455009.26190964	88.414031	 
5114	0.196	89.4149	0.038	49.827	49.022	0.2009	0.0080	0.0000



KID  & RA[2000]    & DEC[2000]  &  BJD0  &   Period & m \\
\\
\hline
\\
1995732 & 19h 04m 51.84s & 37d 25m 30.86s & 2455126.8186591 & 77.36284 & \\ 2307206 & 19h 29m 30.28s & 37d 39m 26.86s &
2455086.5350501 & 204.03401 & \\ 3102000 & 19h 09m 23.87s & 38d 17m 09.74s & 2454997.2595449 & 57.05953 & \\ 3428468 &
19h 06m 53.61s & 38d 35m 44.38s & 2455492.0800000 & 114.90820 & \\ 3851949 & 19h 27m 36.80s & 38d 55m 33.10s &
2455360.1522500 & 54.78906 & \\ 4247023 & 19h 07m 23.64s & 39d 18m 17.78s & 2455061.7750000 & 47.18950 & \\ 4659255 &
19h 32m 11.61s & 39d 43m 31.26s & 2455463.1820000 & 198.01500 &\\ 6182849 & 18h 52m 17.77s & 41d 32m 27.17s &
2454980.4990000 & 6.39910 &\\ 6233483 & 19h 56m 12.01s & 41d 32m 14.82s & 2454992.7350000 & 15.87350 & \\ 6312534 & 19h
55m 32.15s & 41d 39m 43.49s & 2455005.1400000 & 3.01560 & \\ 6525209 & 19h 30m 53.13s & 41d 54m 17.71s &
2455092.5650000 & 75.13180 & \\ 6933781 & 19h 06m 47.36s & 42d 27m 04.18s & 2455062.7570000 & 130.42000 & \\ 6947666 &
19h 26m 01.46s & 42d 26m 53.20s & 2455014.4600000 & 56.69000 & \\ 7021177 & 19h 10m 32.89s & 42d 31m 50.95s &
2455036.1425000 & 18.64540 & \\ 7132542 & 19h 43m 32.45s & 42d 37m 18.77s & 2455067.7450000 & 66.361000 & \\ 7620844 &
19h 42m 26.49s & 43d 15m 37.51s & 2455011.5650000 & 58.622000 & \\ 7866921 & 18h 39m 25.46s & 43d 40m 04.44s &
2455198.7700000 & 91.500500 & \\ 8044608 & 19h 47m 36.97s & 43d 49m 26.00s & 2455067.6400000 & 106.176000 &\\ 8491745 &
19h 22m 02.79s & 44d 33m 21.67s & 2455059.6480000 & 111.320000 & \\ 8552719 & 19h 15m 53.20s & 44d 37m 28.31s &
2455097.7000000 & 88.409000 & \\



1995732 & 0.14252 & 157.1 & 5163 & 0.959 & 89.172 & 0.0190 & 0.0069 & 0.450 & 0.126 &	\\ 2307206 & 0.17664 & 273.5 &
5342 & 0.897 & 89.885 & 0.0054 & 0.0051 & 0.787 & 0.004 &	 \\ 3102000 & 0.73492 & 181.8 & 5718 & 0.683 & 89.989 &
0.0200 & 0.0047 & 0.218 & 0.0   &	\\ 3428468 & 0.77405 & 207.6 & 4279 & 0.860 & 89.394 & 0.0060 & 0.0051 & 1.830 &
0.0   &	\\ 3851949 & 0.29440 & 319.5 &      &       &        &        &        &       &	      &	\\ 4647023 &
0.37693 & 151.9 & 5424 & 0.987 & 89.610 & 0.0149 & 0.0146 & 1.003 & 0.0   &	\\ 4659255 & 0.07572 & 213.7 & 5153 & 0.784
& 89.656 & 0.0043 & 0.0044 & 0.992 & 0.0   &	\\ 6182849 & 0.01178 & 269.9 & 5893 & 0.816 & 89.210 & 0.0671 & 0.0404
& 1.254 & 0.0   &	\\ 6233483 & 0.0559 & 238.3 &      &       &        &  	    &  	 &       &	     &       \\ 6312534
& 0.0000 &   0.0 &      &       &        &        &        &       &       &$P_{rot}$=3.003042  \\ 6525209 & 0.5908 &
221.3 &      &       &        &        &        &       &       &         \\ 6933781 & 0.5645 &  32.1 &      &       &
&        &        &       &       &        \\ 6947666 & 0.5875 & 180.0 &      &       &        &        &        & &
&        \\ 7021177 & 0.5539 &  88.1 &      &       &        &        &  	 &  	   & 	     & $P_{rot}$=6.355932\\
7132542 & 0.3734 & 185.0 &      &       &        &   	    &        &       &       &	 \\ 7620844 & 0.1672 & 293.0 &
&       &        &        &        &       &       &      \\ 7866921 & 0.2094 & 207.1 &      & &        &   	    &  	 
&  	   &	     &		\\ 8044608 & 0.5554 & 353.1 &      &       &        &        & &       &       &        \\
8491745 & 0.1529 & 357.8 &      &       &        &        &        &       &       &
\\ 8552719 &        &       &      &       &        &        &        &       &       & exoplanet? \\



KID  & Period & $\varphi_{2}$ & $d_{1}$&$ d_{2}$& $A_{1}$& $A_{2}$ & x-shift & y-shift \\
        & days     &        & days   & days   & mag    & mag\\
\hline
\\
1995732 & 77.36284 & 0.4165 (0.43)& 0.4951 & 0.5415 & 0.1430 & 0.1040 & 0.01  up & 0.015 dn  \\ 2307206 &204.03401 &
0.5071 (0.50)& 0.7141 & 0.4897 & 0.7600 & 0.3410 & 0.08  dn & 0.04  up  \\ 3102000 & 57.05953 & 0.0790 (0.11)& 0.3081 &
0.2970 & 0.0950 & 0.0045 & 0.00     & 0.00      \\ 3428468 &114.90820 & 0.0787 (0.10)& 0.3103 & 0.1724 & 0.3100 &
0.1800 & 0.00     & 0.00      \\ 3851949 & 54.78906 & 0.6425 (0.64)& 1.5007 & 1.0187 & 0.0080 & 0.0020 & 0.00     &
0.00      \\ 4247023 & 47.18950 & 0.2891 (0.29)& 0.4719 & 0.3303 & 0.6570 & 0.4920 & 0.005 dn & 0.00      \\ 4659255
&198.01500 & 0.4599 (0.46)& 0.4040 & 0.3723 & 0.1900 & 0.0450 & 0.005 dn & 0.00 	   \\ 6182849 &  6.39910 & 0.5000
(0.50)& 0.2240 & 0.2150 & 0.5240 & 0.1388 & 0.08  up & 0.10  dn  \\ 6233483 & 15.87350 & 0.4813 (0.46)& 0.3492 & 0.3175
& 0.0132 & 0.0047 & 0.065 dn & 0.045 up  \\ 6312534 &  3.01560 & 0.5000 (0.50)& 0.1206 & 0.1206 & 0.0203 & 0.0087 &
0.075 dn & 0.025 up  \\ 6525209 & 75.13180 & 0.2176 (0.21)& 0.8565 & 0.3757 & 0.1480 & 0.0399 & 0.003 up & 0.005 up  \\
6933781 &130.42000 & 0.8044 (0.80)& 0.1826 & 0.3391 & 0.0033 & 0.0014 & 0.00     & 0.00	   \\ 6947666 & 56.69000 &
0.1260 (0.14)& 0.2834 & 0.2834 & 0.0628 & 0.0019 & 0.00     & 0.00	   \\ 7021177 & 18.64540 & 0.5543 (0.53)& 0.1604 &
0.5482 & 0.7088 & 0.3385 & 0.00     & 0.00	   \\ 7132542 & 66.36100 & 0.2632 (0.27)& 0.8361 & 0.7831 & 0.6767 & 0.6277
& 0.005 dn & 0.015 up  \\ 7620844 & 58.62200 & 0.5416 (0.55)& 0.3517 & 0.2579 & 0.3500 & 0.0892 & 0.015 dn & 0.007 dn
\\ 7866921 & 91.50050 & 0.3814 (0.38)& 0.7869 & 0.6497 & 0.0760 & 0.0430 & 0.006 up & 0.007 dn  \\ 8044608 &106.17600
&
0.8510 (0.84)& 0.4247 & 0.3716 & 0.2019 & 0.0283 & 0.00     & 0.00	   \\ 8491745 &111.32000 & 0.5973 (0.60)& 0.9574 &
0.9462 & 0.0712 & 0.0158 & 0.00     & 0.00	   \\ 8552719 & 88.40900 & 0.5000 (....)& 0.7073 & 0.7073 & 0.0020 & 0.0000
& 0.00     & 0.00	   \\
































The values of the deviations of the light center during the eclipses are different for the two eclipses, bigger for the
deeper eclipse. They do not depend on the coordinates, period, eccentricity, eclipse depth, $\varphi_{2}$, $\omega$ of
the targets. There is not correlation between the deviation directions (up or down) during the eclipses and the
foregoing parameters. These directions during the eclipses do not depend on the common trend of the shift of the light
center during the quarter (increasing, decreasing or parabolic).

The position of the light center of the target changes between the quarters Q1 and Q6 by up to 5-6 pixels. The values
of the x-deviations and y-deviations during the eclipses may change by a factor 6-7 between the quarters Q1 and Q6. The
directions (up or down) of the x-deviations and y-deviations during the eclipses may change between the quarters Q1 and
Q6 (see 2307206).

The light position of the targets shift on pixel frame nonsynchonous during the quarters (every star separately).

The pixel positions of the stars from Q2 and Q6 are the same.





Every 93 days the spacecraft rotates 90 degrees, referred to as a quarterly roll, which changes which stars are on
which CCDs. Every quarter the pixel selection process is repeated with a new collection of targets.

Kepler�s lack of a shutter means that pixels are exposed to the sky during readout, which causes image smear along
columns. The leading 20 masked and 26 trailing virtual columns measure this smear data. The black level and smear data
are called collateral data and are used to calibrate the pixel data during ground processing.6

Kepler on-board flight system software does not allow specification of arbitrary collections of pixels for each target.
A table of 1024 aperture masks is loaded onto the spacecraft, and the pixels associated with a target are fit into one
of these masks. Efficient design of these masks is required to gather the desired pixels without too many excess
pixels.

Stellar targets are point-like sources whose pixels are selected to maximize the signal to noise ratio (SNR). Stellar
targets are specified by a Kepler ID, which is used to look up pertinent data in the Kepler Input Catalog (KID).
Stellar targets may be either LC or SC.

Long cadence: There may be no more than 170,000 target definitions, with no more than 10,000 per output channel, and no
more than 5.44 million pixels across the FOV. This implies an average of # 32 pixels per target definition to attain
170,000 target definitions.

Basic Kepler mission requirements specify the capability to observe stars with magnitudes between 9 and 15.
Simultaneously meeting the above constraints yet providing efficient mask assignment for a wide range of stellar
magnitudes is a significant challenge. Observation of stars brighter than magnitude 9 is allowed with the understanding
that pixel efficiency will be significantly degraded, so these observations can use a very large number of pixels.


It is deserved to explore the effect of considerable temporal binning, especially the long-cadence photometry, on the
light curves and on the retrieval system parameters. Kipping (2010) has made similar investigation mainly for CoRoT
which binning is 8.5 minutes while that of Kepler is even 30 minutes. These effects are particularly crucial in light
of the long-cadence photometry often used for discovering new exoplanets by for example CoRoT and the Kepler Mission
(8.5 and 30 minutes). One of the dominant effects of long integration times is a systematic underestimation of the
lightcurve derived stellar density, which has significant ramifications for transit surveys. Kipping (2010) present a
discussion of numerical integration techniques to compensate for the effects and produce expres- sions to quickly
estimate the errors of such techniques, as a function of integration time and numerical resolution. This allows for an
economic choice of resolution before attempting fits of long-cadence lightcurves.


For transit observations at visible wavelengths, limb darkening is quite pronounced producing a well-known curvature in
the flat-bottom part of the lightcurve. For large integration times, the curvature is smeared out, producing a flatter
transit trough morphology. If we were trying to fit such a transit lightcurve, and the limb darkening parameters are
exactly known, our hypothetical fitting algorithm would move towards a case where limb-darkening is least effective.
This occurs for near-equatorial transits. This is because as the transit impact parameter becomes larger and larger, we
move closer and closer to the limb of the star where limb darkening accentuates. Therefore, LC data pushes b' towards a
more equatorial value due to limb darkening i.e. b' < b.


Any eccentricity can be considered as the sign of apsidal motion of the orbit in space. In order to find the apsidal
motion period which is used in obtaining the internal structure constants of component stars, the photometric light
curves of the eclipses and/or the radial velocity curves should be obtained at different times. The shift of the
secondary minimum with respect to primary minimum in time or the change of (?) obtained from either light or radial
velocity curve analysis reveals the apsidal motion period. It must also be noted that the (O�C) diagrams formed by the
primary and secondary eclipse minima times exhibit tilted sinusoidal variations of the same period, but phase shift of
180?. Such period is the apsidal motion period of the system.








































\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KID_uncorrected.eps, width=0.2\textwidth}}
    \caption[]{Uncorrected and corrected data}
    \label{1}
  \end{center}
\end{figure}

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KID_neighbour.eps, width=0.2\textwidth}}
    \caption[]{Illustration of contamination effect by the stars KID 309819794 and KID 309819797}
    \label{2}
  \end{center}
\end{figure}


\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KID1995732n.eps, width=0.2\textwidth}}
    \caption[]{Eclipses of KID 1995732 and its fits}
    \label{3}
  \end{center}
\end{figure}



\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=KID7021177.eps, width=0.2\textwidth}}
    \caption[]{Additional variability of KID 7021177}
    \label{13}
  \end{center}
\end{figure}





The effects of orbital eccentricity upon light curves of eclipsing binaries are manifest at a glance. First, according
to the laws of areas, the times of the light minima will generally not be separated by exactly half the orbital period,
but will be displaced by a relative amount depending on both the eccentricity and orientation of the apsidal line with
respect to the line of sight. The same law will also render both minima to be asymmetric and of unequal durations. Only
when i=90$^{0}$ the light minima coincide with the conjunctions.`

\begin{figure}[!htb]
  \begin{center}
    \centering{\epsfig{file=Fig3.eps, width=0.7\textwidth}}
    \caption[]{Eclipses of KID 1995732 and their fits}
    \label{3}
  \end{center}
\end{figure}

\begin{figure}[!htb]
  \begin{center}
    \centering{\epsfig{file=Fig4.eps, width=0.7\textwidth}}
    \caption[]{Eclipses of KID 1995732 and their fits}
    \label{4}
  \end{center}
\end{figure}

\begin{figure}[!htb]
  \begin{center}
    \centering{\epsfig{file=Fig5.eps, width=0.7\textwidth}}
    \caption[]{Eclipses of KID 1995732 and their fits}
    \label{5}
  \end{center}
\end{figure}

Probably some \emph{Kepler} variables (especially with very small amplitudes) are false positives due to this
artificial effect.

For distances greater than a few kpc, stars in this field are above the galactic disk, thus minimizing the number of
background giant stars.


: to measure the fraction of stars that have terrestrial planets near their habitable zones


(3) It turned out that: (i) the values of the limb-darkening coefficients for the reproduction of the light curve are
considerably smaller than those corresponding to the respective temperature: (ii) the contribution of these
coefficients to the fit is essential, especially for the low-amplitude curves.

The latest version of the light curve program for binary stars (Wilson-Devinney, PHOEBE, etc.) use the limb-darkening
coefficients of Van Hamme (1993) for a linear,logarithmic and square root limb-darkening laws. These coefficients are
calculated on the ATLAS stellar atmosphere models for solar chemical composition stars with a wide range of effective
temperatures and surface gravities.

%For binary star light curve modeling purposes, Van Hamme (1993) proposed the %use of a logarithmic or a square root
law.

Howarth (2010) provides new limb-darkening coefficients for model-atmosphere grids at Galactic, LMC, and SMC
abundances. The grids cover T(eff) = 3.5-50 kK, from log(g) = 5.0 to the effective Eddington limit. Limb-darkening
coefficients and synthetic photometry are presented in the UBVRIJHKLM, uvby, ugriz, WFCAM, \emph{Hipparcos/Tycho), and
\emph{Kepler} passbands for these models.

Sing (2009) provides stellar Limb-Darkening Coefficients for \emph{CoRot} and \emph{Kepler} which contain wide,
nonstandard response functions, and are producing a large inventory of high-quality transiting lightcurves, sensitive
to stellar limb darkening. These coefficients are calculated with ATLAS stellar atmospheric model grids and span a wide
range of T$_{eff}$, log g, and metallically M/H. Comparing the stellar model limb darkening to results from the first
seven \emph{CoRot} planets, Sing (2009) got better fits when two model intensities at the limb are excluded in the
coefficient calculations. This calculation method can help to avoid a major deficiency present at the limbs of the 1D
stellar models. \emph{Kepler} operate at optical wavelengths, where the effects of limb-darkening are strong,

Sing et al. (2008) found that for the widely used Kurucz 1D ATLAS stellar models, the largest differences between
existing limb-darkening data and the 1D stellar models was at the limb, where ATLAS models predict a dramatic increase
in the strength of limb darkening. For the sun, the ATLAS models over-predict the strength of limb darkening by
>20 $\%$ at $\mu$ = cos($\theta$) values below 0.05, though seemed
to perform well otherwise, over-predicting the strength by only a few percent. While there remain few other
observational constraints, theoretical atmospheric models have also been unable to provide a satisfactory fits to the
observations of eclipsing binary stars (Claret 2008).

Sing supposed that linear laws will likely fit transit light curves quite well for both CoRot and Kepler in cooler K
type stars, or for earlier types at low S/N. Higher order terms will likely be needed in F and G type stars at high
S/N, where multiple LDCs can be fit at good precision.

%Estimation of parameter errors in inverse problems. Determining %limb-darkening coefficients in classical eclipsing
systems by M K %Abubekerov, N Yu Gostev, A M Cherepashchuk Astronomy Reports %(2009) Volume: 53, Issue: 8, Pages:
722-749

%
http://exoplanetarchive.ipac.caltech.edu/cgi-bin/bgServices/nph-bgExec?bgApp=%2FETSS%2Fnph-etss&etss_dataset=Kepler&etssdetail=2307206&etssfind=View

Claret (2008) The LDCs should also be corrected for the irradiation effect

Figures 3-12 show parts of the phased light curves of our targets around the eclipses while Table 2 presents the main
parameters of these eclipses: phase of the secondary eclipse $\varphi_{2}$; durations $d_{i}$ and amplitudes $A_{i}$ of
the two minima.

\begin{table}
\begin{center}
\caption{Parameters of the eclipses of the targets from Sample 1}
\begin{tabular}{crcrccccc}
\hline
\\
KID  & Period & $\varphi_{2}$ & $d_{1}$&$ d_{2}$& $A_{1}$& $A_{2}$ & x-shift & y-shift \\
        & days     &        & days   & days   & mag    & mag\\
\hline
\\
1995732 & 77.36284 & 0.4165 (0.43)& 0.4951 & 0.5415 & 0.1430 & 0.1040 & 0.01  up & 0.015 dn  \\ 2307206 &204.03401 &
0.5071 (0.50)& 0.7141 & 0.4897 & 0.7600 & 0.3410 & 0.08  dn & 0.04  up  \\ 3102000 & 57.05953 & 0.0790 (0.11)& 0.3081 &
0.2970 & 0.0950 & 0.0045 & 0.00     & 0.00      \\ 3428468 &114.90820 & 0.0787 (0.10)& 0.3103 & 0.1724 & 0.3100 &
0.1800 & 0.00     & 0.00      \\ 3851949 & 54.78906 & 0.6425 (0.64)& 1.5007 & 1.0187 & 0.0080 & 0.0020 & 0.00     &
0.00      \\ 4247023 & 47.18950 & 0.2891 (0.29)& 0.4719 & 0.3303 & 0.6570 & 0.4920 & 0.005 dn & 0.00      \\ 4659255
&198.01500 & 0.4599 (0.46)& 0.4040 & 0.3723 & 0.1900 & 0.0450 & 0.005 dn & 0.00 	   \\ 6182849 &  6.39910 & 0.5000
(0.50)& 0.2240 & 0.2150 & 0.5240 & 0.1388 & 0.08  up & 0.10  dn  \\ 6233483 & 15.87350 & 0.4813 (0.46)& 0.3492 & 0.3175
& 0.0132 & 0.0047 & 0.065 dn & 0.045 up  \\ 6312534 &  3.01560 & 0.5000 (0.50)& 0.1206 & 0.1206 & 0.0203 & 0.0087 &
0.075 dn & 0.025 up  \\ 6525209 & 75.13180 & 0.2176 (0.21)& 0.8565 & 0.3757 & 0.1480 & 0.0399 & 0.003 up & 0.005 up  \\
6933781 &130.42000 & 0.8044 (0.80)& 0.1826 & 0.3391 & 0.0033 & 0.0014 & 0.00     & 0.00	   \\ 6947666 & 56.69000 &
0.1260 (0.14)& 0.2834 & 0.2834 & 0.0628 & 0.0019 & 0.00     & 0.00	   \\ 7021177 & 18.64540 & 0.5543 (0.53)& 0.1604 &
0.5482 & 0.7088 & 0.3385 & 0.00     & 0.00	   \\ 7132542 & 66.36100 & 0.2632 (0.27)& 0.8361 & 0.7831 & 0.6767 & 0.6277
& 0.005 dn & 0.015 up  \\ 7620844 & 58.62200 & 0.5416 (0.55)& 0.3517 & 0.2579 & 0.3500 & 0.0892 & 0.015 dn & 0.007 dn
\\ 7866921 & 91.50050 & 0.3814 (0.38)& 0.7869 & 0.6497 & 0.0760 & 0.0430 & 0.006 up & 0.007 dn  \\ 8044608 &106.17600
&
0.8510 (0.84)& 0.4247 & 0.3716 & 0.2019 & 0.0283 & 0.00     & 0.00	   \\ 8491745 &111.32000 & 0.5973 (0.60)& 0.9574 &
0.9462 & 0.0712 & 0.0158 & 0.00     & 0.00	   \\ 8552719 & 88.40900 & 0.5000 (....)& 0.7073 & 0.7073 & 0.0020 & 0.0000
& 0.00     & 0.00	   \\

\end{tabular}
\end{center}
\end{table}

\begin{table}
\begin{center}
\caption{Coordinates and ephemeres of the targets from Sample 1}
\begin{tabular}{ccccrc}
\hline
\\

KID		&	e		&	w		&			&	d Phase		&	BJD			&	Period	       \\ 1995732	&	0.14252	 
&	157.08	&	2.74156	&	-0.04003	&	2455049.45692971	&	77.363032	\\ 2307206	&	0.17664	&	273.55	&	 
4.77430	&	 0.00396	&	2455086.53717057	&	204.030667	\\ 3102000	&	0.73492	&	181.77	&	3.17243	&	
-0.21400	&	2454997.25556938	&	57.059216	\\ 3428468	&	0.77405	&	207.65	&	3.62410	&	-0.26500	&	 
2455032.44996961	&	114.908636	\\ 3851949	&	0.29014	&	319.65	&	5.57896	&	 0.08000	&	
2454976.78185172	&	54.776991	\\ 4247023	&	0.37693	&	151.88	&	2.65076	&	-0.09150	&	
2455061.78039575	&	47.189567	\\ 4659255	&	0.07572	&	213.66	&	3.72915	&	-0.02070	&	
2455067.15120620	&	198.014033	\\ 6182849	&	0.01178	&	269.91	&	4.71082	&	 0.00000	&	
2454967.70080728	&	6.399107	\\ 6233483	&	0.05569	&	238.72	&	4.16648	&	-0.00950	&	
2454976.85610603	&	15.873552	\\ 6312534	&	0.00115	&	15.42		&	0.26919	&	 0.00000	&	
2454965.94158660	&	3.015550	\\ 6525209	&	0.58949	&	224.72	&	3.92209	&	-0.18500	&	
2455017.42871952	&	75.131944	\\ 6933781	&	0.56295	&	32.14		&	0.56100	&	 0.11850	&	
2455062.75755611	&	130.419512	\\ 6947666	&	0.63304	&	175.39	&	3.06111	&	-0.18000	&	
2455071.15247452	&	56.687032	\\ 7021177	&	0.57877	&	83.09		&	1.45025	&	 0.01500	&	
2455017.49723690	&	18.645334	\\ 7132542	&	0.38159	&	182.84	&	3.19109	&	-0.12000	&	
2455067.74039272	&	66.360950	\\ 7620844	&	0.18617	&	290.21	&	5.06507	&	 0.02350	&	
2455070.18823707	&	58.621582	\\ 7866921	&	0.22484	&	214.15	&	3.73760	&	-0.06500	&	
2455107.26924060	&	91.5008708	\\ 8044608	&	0.58766	&	356.54	&	6.22271	&	 0.18000	&	
2455067.64037980	&	106.175893	\\ 8491745	&	0.15338	&	0.33		&	0.00584	&	 0.04860	&	
2455059.64770915	&	111.320439	\\ 8552719	&	0.00000	&	180.00	&	3.14159	&	 0.00000	&	
2455009.26190964	&	88.414031	\\

1995732 & 0.4165 & 0.4951 & 0.5415 & 0.1430 & 0.1040  &	0.14252	&	157.08	\\ 2307206 & 0.5071 & 0.7141 & 0.4897 &
0.7600 & 0.3410  &	0.17664	&	273.55	\\ 3102000 & 0.0790 & 0.3081 & 0.2970 & 0.0950 & 0.0045  &	0.73492	&	181.77	 
\\ 3428468 & 0.0787 & 0.3103 & 0.1724 & 0.3100 & 0.1800  &	0.77405	&	207.65	\\ 3851949 & 0.6425 & 1.5007 & 1.0187 &
0.0080 & 0.0020  &	0.29014	&	319.65	\\ 4247023 & 0.2891 & 0.4719 & 0.3303 & 0.6570 & 0.4920  &	0.37693	&	151.88	 
\\ 4659255 & 0.4599 & 0.4040 & 0.3723 & 0.1900 & 0.0450  &	0.07572	&	213.66	\\ 6182849 & 0.5000 & 0.2240 & 0.2150 &
0.5240 & 0.1388  &	0.01178	&	269.91	\\ 6233483 & 0.4813 & 0.3492 & 0.3175 & 0.0132 & 0.0047  &	0.05569	&	238.72	 
\\ 6312534 & 0.5000 & 0.1206 & 0.1206 & 0.0203 & 0.0087  &	0.00115	&	 15.42	\\ 6525209 & 0.2176 & 0.8565 & 0.3757 &
0.1480 & 0.0399  &	0.58949	&	224.72	\\ 6933781 & 0.8044 & 0.1826 & 0.3391 & 0.0033 & 0.0014  &	0.56295	&	 32.14	 
\\ 6947666 & 0.1260 & 0.2834 & 0.2834 & 0.0628 & 0.0019  &	0.63304	&	175.39	\\ 7021177 & 0.5543 & 0.1604 & 0.5482 &
0.7088 & 0.3385  &	0.57877	&	 83.09	\\ 7132542 & 0.2632 & 0.8361 & 0.7831 & 0.6767 & 0.6277  &	0.38159	&	182.84	 
\\ 7620844 & 0.5416 & 0.3517 & 0.2579 & 0.3500 & 0.0892  &	0.18617	&	290.21	\\ 7866921 & 0.3814 & 0.7869 & 0.6497 &
0.0760 & 0.0430  &	0.22484	&	214.15	\\ 8044608 & 0.8510 & 0.4247 & 0.3716 & 0.2019 & 0.0283  &	0.58766	&	356.54	 
\\ 8491745 & 0.5973 & 0.9574 & 0.9462 & 0.0712 & 0.0158  &	0.15338	&	  0.33	\\ 8552719 & 0.5000 & 0.7073 & 0.7073 &
0.0020 & 0.0000  &	0.00000	&	180.00	\\

%We followed also Sing (2009) that linear laws fit light curves quite well in cooler K type stars, or for earlier types
at low S/N while higher order terms %are needed in F and G type stars at high S/N.

\begin{figure}[!htb]
\begin{center}
    \centering{\epsfig{file=detrending1.eps, width=0.8\textwidth}}
    \caption[]{The light curves of KID3098197 from "CORR" data (top) and after our de-trending (bottom)}
    \label{1}
  \end{center}
\end{figure}


The data from every new quarter of $Kepler$ mission led to increasing of the list of the planet candidates:
the first version of the catalog, released in June 2010, contained 312 candidates (Borucki et al. 2011a);
the second version, released in February 2011, contained 1235 candidates (Quarters 1 through 5)
(Borucki et al. 2011b); Batalha et al. (2012) added 1091 viable new planet candidates, bringing the total count
up to over 2300. Additionally to the efforts of the $Kepler$ team outer researches
also discovered exoplanets. Thus the list of planetary systems discovered on
the $Kepler$ data increases continuously and our knowledge about the planetary worlds enriches.

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\begin{thebibliography}{}

Batalha N. et al., 2010, ApJ 713L, 109 \\

Batalha N. et al., 2012,arXiv:1202.5852 \\

Blomme J. et al., 2011, MNRAS 418, 96 \\

Borucki W. et al., 2010, Sci 327, 977 \\

Bulut, I., Demircan O., 2007, MNRAS 378, 179 \\

Caldwell D. et al., 2010, SPIE 7731E, 30 \\

Coughlin J., Lopez-Morales M.,  Harrison T.,  Ule N.,  Hoffman D. , 2011, AJ 141, 78

Dunham E. et al., 2010, ApJ 713L, 136D\\

Gilliland R. et al., 2010, ApJ 713L, 60 \\

Haas M. et al. 2010, ApJ 713L, 115 \\

Howarth D., 2010, MNRAS 413, arXiv: 1011.2631\\

Huang X., Bakos G., Hartman J, 2012, arXiv:1205.6492\\

Kjurkchieva D., Dimitrov D., 2012, IAUS 282, 474\\

Koch D. et al. 2010, ApJ 713L, 131\\

Kopal Z., 1959, Close Binary stars, The Iternational Astrophysical Series v.5 \\

Kreiner J., Kim C., Nha I., 2001, aocd.book \\

Latham D. et al. 2010, ApJ 713L, 140L\\

Pourbaix D. et al., 2004, 2004, A $\&$ A 424, 727 \\

Prsa A., Zwitter T., 2005, ApJ, 628, 426\\

Prsa A. et al., 2011, AJ 141, 83 \\

Rowe J. et al., 2006, ApJ 646,1241\\

Sing K., 2009, $A \& A$ 510, 21\\

Slawson R. et al., 2011, AJ 142, 160\\

Tokovinin A. et al., 2003, A $\&$ A 409, 245 \\

\end{thebibliography}