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% -------------- Title and affiliation
%                (please edit accordingly)

\title{The science case of the PEPSI
high-resolution echelle spectrograph and polarimeter for the LBT}

\author{K. G. Strassmeier\inst{1,}\inst{2}\fnmsep\thanks{kstrassmeier@aip.de,
www.aip.de/pepsi/}, R.
Pallavicini\inst{3}\fnmsep\thanks{pallavic@oapa.astropa.unipa.it},
J. B. Rice\inst{4,}\inst{1}\fnmsep\thanks{rice@BrandonU.ca}, M. I.
Andersen\inst{1}\fnmsep\thanks{mandersen@aip.de}, \and F. M.
Zerbi\inst{5}\fnmsep\thanks{zerbi@merate.mi.astro.it}\\}

\institute{Astrophysical Institute Potsdam (AIP), An
der Sternwarte 16, D-14482 Potsdam, Germany
\and
Universit\"at Potsdam, Am Neuen Palais 10, D-14469 Potsdam, Germany
\and
INAF - Osservatorio Astronomico di Palermo,
Piazza del Parlamento 1, I-90134 Palermo, Italy
\and
Department of Physics, Brandon University, Brandon, Manitoba R7A
6A9, Canada
\and
INAF - Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate
(LC), Italy }

\date{Received; accepted; published online}



% -------------- Abstract

\abstract{ T e x t. \keywords{follow A\&A style} }




\maketitle





% -----------------------------------------------------------------

\section{Introduction}

\subsection{Stellar magnetic fields: a paradigm}

\subsubsection{Rotational velocities of very low-mass stars and
brown dwarfs}

The advent of large and high quantum-efficiency CCD detectors,
combined with high-resolution spectrographs and abundant computing
power, has ushered stellar astronomy into an era when we can
produce images of the surfaces of other stars (called Doppler
imaging or Doppler tomography, see Fig.~\ref{F1} and
Fig.~\ref{F2}). From these images we can study both the spatial
pattern of surface phenomena and their temporal behavior. There
are several well-proven techniques to map the surface temperature
distribution of cool stars from integral light (see  Piskunov \&
Rice \cite{pis:ric}) but the next goal is to apply these
techniques to the circularly {\em and} linearly polarized light
components (e.g. Piskunov \& Kochukhov \cite{zdi-review}).

%------------- single-column figure
\begin{figure}[t]
   \centering
   \includegraphics[angle=0,width=8.5cm]{sunekdra.eps}
   \caption{A comparison of a Doppler image of the G2V-star EK~Dra
   and a photospheric white-light image of the Sun. }
   \label{F1}
\end{figure}


%------------- double-column figure
\begin{figure*}[t]
   \centering
   \includegraphics[angle=0,width=17cm]{sunekdra.eps}
   \caption{A comparison of a Doppler image of the G2V-star EK~Dra
   and a photospheric white-light image of the Sun. }
   \label{F2}
\end{figure*}






% -------------- Acknowledgements

\acknowledgements KGS acknowledges support from ...




% -------------- References

\begin{thebibliography}{}

\bibitem[2002]{zdi-review}
Piskunov N. E., Kochukhov, O.: 2002, A\&A 381, 736

\bibitem[1993]{pis:ric}
Piskunov N. E., Rice J. B.: 1993, PASP 105, 1415

\end{thebibliography}




\end{document}