\section{Atmospheric parameters of BD-002862}

Determination of atmospheric parameters requires high-resolution spectra with good signal-to-noise ratio (the best value is more than S/N$\sim$100). Spectra obtained with PST 1 in Borowiec for the BD-002862 have low S/N values, in range from 10 to 25. This high-resolution spectra from echelle spectrograph (mounted on the PST 1) have also distorted line profile due to merging curved orders in reduction process. All these factors influenced the uncertainty of the obtained parameters. The component BD-00 2862 is a eclipsing binary object whether its spectrum is dominated by the lines of the main component. As the S/N of our spectra are not sufficient for spectrum analysis we decided to investigate the average spectrum.  
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To estimate atmospheric parameters (effective temperature, $T_{\rm eff}$, surface gravity, $\log g$, metallicity [M/H], and projected rotational velocity, $v\sin i$) was used the iSpec code (Blanco-Cuaresma et al., 2014) adapting the same method as described in Dimitrow et al. 2017. The microturbulence and macroturbulence velocities were assumed to 1 km\,s$^{-1}$ and 0 km\,s$^{-1}$, respectively. The values of the microturbulence were chosen as typical for those types of stars temperatures (Gray 2005). The macroturbulence velocities are related to $v\sin i$ and it is difficult to distinguish the two, especially from data with low S/N. Atmospheric parameters were calculated with synthetic spectral fitting technique using ATLAS9 grids of atmospheric models (Kurucz, 2005), the VALD database for atomic data (Kupka et al., 2011) and solar abundances were taken from publication Asplund et al., 2009.  

For the twelve selected spectra, with S/N higher than 15 and different phases of orbital rotation, were calculated cross-correlation radial velocities and aligned relative to the synthetic spectrum with the iSpec code. The synthetic spectrum was generated for $T_{\rm eff}$, $\log g$ and $v\sin i$ values, which were obtained from modeling of the system for the component 1 (see Tab. 5), micro- and macroturbulence velocities were set to 1 and 0 km\,s$^{-1}$ and [M/H] = 0.0 dex. In the next step, the spectra were combined by using the median flux values. The signal-to-noise ratio for the received average spectrum was around 50. Comparison of combined spectrum and spectrum obtained on April 2. 2009 is shown in Fig. \ref{fig:f1}. Additionally, the continuum of spectra regions containing lines taken to determining atmospheric parameters was normalized and corrected to minimize the effect of the bad normalization. 

To estimated the effective temperature was used sensitivity of Balmer lines to this parameter. The received spectra cover the range 4500--9000 \AA, hence only two Balmer lines $H_{\alpha}$ and $H_{\beta}$ were used. During calculation parameter $\log g$ was set to 4.0\,dex, while it does not affect Balmer line profile for stars cooler than $T_{\rm eff} < 8000$\,K (Smalley, 2005). To evaluate uncertainties of $T_{\rm eff}$ we took in to account difference in temperature calculated separately from the lines. Obtained value effective temperature was 5600 $\pm$ 400 K.

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* To estimate all uncertainties were taking in to account 

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Should we write here comparison of obtained parameters from modeling? 

\begin{center}
\begin{table}[!ht]
\centering
%\caption{My caption}
\label{tab:Ta}
%\small
\scalebox{0.85}{
\begin{tabular}{cccc}
\hline
\vspace{0.1cm}
 $T_{\rm eff} [K] $ & $\log g $ [dex]  & [M/H] [dex] & $v\sin i$ [km s$^{-1}$]\\
\hline
 5600$\pm$400 &  3.8$\pm$0.5 & -0.30$\pm$0.20 & 30$\pm$4\\
\hline
\end{tabular}
}
\caption{The atmospheric parameters obtained from spectrum synthesis for the analyzed stars BD-00 2862.}
\end{table}
\end{center}

%See the code for Figure \ref{fig:frog} in this section for an example.


\section{REFERENCES}

\begin{itemize}
\item Asplund M., Grevesse N., Sauval A.J., Scott P., 2009, ARA \& A, 47, 481
\item Blanco-Cuaresma, S., Soubiran, C., Heiter, U., and Jofré, P. 2014, A\&A, 569, A111
\item Gray D.F., 2005, The Observation an analysis of Stellar Photospheres, Cambridge University Press
\item Kupka, F., Dubernet, M.-L., and VAMDC Collaboration. 2011, Baltic Astronomy, 20, 503
\item Kurucz R. L., 2005, ATLAS12, SYNTHE, ATLAS9, WIDTH9, et cetera. Memorie della Societa Astronomica Italiana Supplementi, 8:14
\item Smalley B., 2005, MSAIS, 8, 130


\end{itemize}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{Fig1.eps}
\caption{\label{fig:f1} The combined average spectrum obtained from 12 spectra (red colour) and for comparison on of the observed spectrum (black colour).}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{BD002862_Hb_fit_v2.eps}
\caption{\label{fig:f2a} The comparison of the combined spectrum (gray colour) and synthetic (with different colours) of the $H_{\beta}$ region. The different colours of syncorrespond to synthetic spectra calculated for various effective temperatures within the limits of error.}
\end{figure}

\vspace{0.5cm}

%\begin{figure}
%\centering
%\includegraphics[width=1.0\textwidth]{BD002862_Hb_fit_v1.eps}
%\caption{\label{fig:f2} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the $H_{\beta}$ region.}
%\end{figure}

%\begin{figure}
%\centering
%\includegraphics[width=1.0\textwidth]{BD002862_Hb_fit_v3.eps}
%\caption{\label{fig:f2b} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the $H_{\beta}$ region.}
%\end{figure}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{BD002862_NaI_fit.eps}
\caption{\label{fig:f3} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the Na D region.}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{BD002862_MgbI_fit.eps}
\caption{\label{fig:f4} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the Mg b I region.}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{BD002862_CaI_fit.eps}
\caption{\label{fig:f5} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the Ca I region.}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=1.0\textwidth]{BD002862_FeI_fit.eps}
\caption{\label{fig:f6} The comparison of the combined spectrum (black colour) and synthetic (red colour) of the Fe I region.}
\end{figure}


\begin{figure}[!h]
\centering
\includegraphics[width=0.5\textwidth]{frog.jpg}
\caption{\label{fig:frog}Hello :)}
\end{figure}