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\documentclass{aa}
%\documentclass[referee]{aa}
\usepackage{graphicx}
\usepackage{subfig}
\usepackage{txfonts}
\usepackage{amstext}
\usepackage{color}
\usepackage{longtable}
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\usepackage{hyperref}
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\hypersetup{
 colorlinks   = true, %Colours links instead of ugly boxes
 urlcolor     = blue, %Colour for external hyperlinks
 linkcolor    = blue, %Colour of internal
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 }

\begin{document}

\newcommand{\bu}{$\bullet$ }
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\newcommand{\ksi}{\xi}
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\newcommand{\ub}{\hbox{$U\!-\!B$}}
\newcommand{\hp}{$H_{\rm p}$}

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\newcommand{\hip}{$Hipparcos$}
\newcommand{\ond}{Ond\v{r}ejov}


\title{Half a century of \ubv\ photometry at Hvar\\
I. Overview and emission-line stars and binaries
\thanks{Based on photometric observations from
the Hvar Observatory and ESA Hipparcos Satellite.
 } }
\author{
H.~Bo\v{z}i\'c\inst{1}\and
P. Harmanec\inst{2}\and
J.~Horn\thanks{Ji\v{r}\'\i\ Horn passed away on Dec. 13, 1994}\inst{3}\and
K.~Juza\thanks{Karel Juza passed away on March 13, 1994}\inst{3}\and
P.~Koubsk\'y\inst{3}\and
S.~K\v{r}\'\i\v{z}\thanks{Svatopluk K\v{r}\'\i\v{z} passed away on Feb. 23, 2018}\inst{3}\and
P.~Mayer\thanks{Pavel Mayer passed away on Nov. 7, 2018}\inst{2}\and
P.~Hadrava\inst{4}\and
D.~Ru\v{z}djak\inst{1}\and
D.~Sudar\inst{1}\and
S.~\v{S}tefl\thanks{Stanislav \v{S}tefl passed away on June 11, 2014}\inst{3}\and
M.~Wolf\inst{2}\and
P.~Zasche\inst{2}\and
M.~Bro\v{z}\inst{2}\and
J.~Havelka\thanks{Josef Havelka passed away on June 19, 2009}\inst{3}\and
J.~Honsa\inst{3}\and
V.~Kocourek\inst{3}\and
M.~Tlamicha\inst{3}\and
F.~\v{Z}\v{d}\'arsk\'y\inst{3}\and
A.~Harmanec\inst{5}\and
J.~Jon\'ak\inst{2}\and
A.~Opli\v{s}tilov\'a\inst{2}\and
I.~Piantschitsch\inst{6,7,8}\and
I.~Skoki\'c\inst{1}\and
J.~\v{S}vr\v{c}kov\'a\inst{2}\and
K.~Vitovsk\'y\inst{2}\and
D.~Vr\v{s}nak\inst{9}\and
M.~Zummer\inst{5}
}
\institute{
Hvar Observatory, Faculty of Geodesy, Zagreb University,
Ka\v ci\'ceva~26, HR-10000 Zagreb, Croatia
  \and
Astronomical Institute, Faculty of Mathematics and Physics,
Charles University, V~Hole\v{s}ovi\v{c}k\'ach~2,\\
CZ-180~00~Praha~8, Czech Republic
  \and
Astronomical Institute of the Czech Academy of Sciences, Fri\v{c}ova~298,
CZ-251~65~Ond\v{r}ejov, Czech Republic
  \and
Astronomical Institute of the Czech Academy of Sciences, Bo\v{c}n\'\i~II~1401/1,
CZ-141~00 Praha~4, Czech Republic
 \and
Faculty of Mathematics and Physics, Charles University, Prague, Czech Republic
 \and
Institute of Physics, University of Graz, Universit\"atsplatz 5, A-8010 Graz,
Austria
 \and
Departament de F\'\i sica, Universitat de les Illes Balears (UIB), E-07122, Spain
 \and
Institute of Applied Computing \& Community Code (IAC3), UIB, Spain
 \and
Faculty of Electrical Engineering and Computing, University of Zagreb,
 Unska~3, HR-10000 Zagreb, Croatia
}
\date{Received \today}

\abstract {We present a summary report on 52 years of systematic photoelectric
\ubv\ observations of early-type emission-line stars {\bf and binaries of all
luminosity classes} secured by a~number of mainly
Croatian and Czech observers at the Hvar Observatory.
All these observations were {\bf carefully re-reduced} to the standard \ubv\ system
defined by the Johnson standard stars through the nonlinear transformation formul\ae.
{\bf These observations represent a very unique set of homogeneous observations,
covering also the near ultraviolet parts of the electromagnetic spectrum, where
the hot stars emit the maximum of their flux. This is extremely important addition to
the modelling of emission-line envelopes since the existing models are usually only
based on $V$ magnitude observations and/or very broad-band space photometries.
Our observations indicate that all emission-line stars of all luminosity classes}
are light and colour variables, but there is great individuality in the behaviour
of each star and often different variability patterns are found in the individual
passbands. We tried to classify various types of variability only on the basis of Hvar
photometry, complemented by the Hipparcos \hp\ photometry transformed
to Johnson $V$ passband, since these observations conveniently fill
the gap in Hvar observations. {\bf We also provide simple statistics of the recognized
types of variations and a~list of known binaries and multiple systems.
Observations of various other types of variables, including accidental discoveries,
will be reported in a~follow-up paper II.}
}

\keywords{stars: early-type --
  stars: emission-line (Be) --
  binaries: eclipsing --
  binaries: ellipsoidal}

\maketitle


%{\onecolumn
%\longtab{
%\begin{flushleft}
\begin{table*}
	\tiny
\caption{A list of early-type emission-line stars, more frequently observed 
at Hvar Observatory, number of their observations, and the types of their 
variability (as defined in Sect.~3) found.}\label{types}
	\begin{tabular}{rrrcccccccc}
	\hline\hline
	Star   &HD/BD &    No. &LTEM&LTCV&MTBIN&VLTV&RAV\\
\hline
	$\omicron$ Cas&   4180& 895&  p& ? & EL&  no&yes\\
	$\gamma$ Cas  &   5394& 137&  p&yes& ? & inc&yes\\
	V442 And      &   6226& 964&  p& no& no&dec?&yes\\
	$\varphi$ And &   6811& 504& no&no?& no& dec&?\\
	$\varphi$ Per &  10516& 678&  p&yes&yes& dec&yes\\
	V554 Per      &  14818& 146& no&yes& no&  no&yes\\
	HR 894        &  18552& 118& no& no& no&  no&yes?\\
	RX Cas        &+67 244& 361& no& no& EB&  no&no?\\
	13 Tau        &  23016& 114& no& no& no&  no&no?\\
	17 Tau        &  23302& 367& no&yes& no&  no& no\\
	V971 Tau      &  23480& 265& no&yes& no&  no&yes\\
	$\eta$ Tau    &  23630& 205& no&yes& no& no?& no\\
	BU Tau        &  23862& 469&  i& no& no&  no& no\\
	V960 Tau      &  36576& 392&  p&yes& no&  no&yes\\
	$\zeta$ Tau   &  37202&1100&p+i&yes&yes&  no&yes\\
	$\omega$ Ori  &  37490&  90&  p& no& no&  no&yes\\
	V731 Tau      &  37967& 107& no& no& no&  no&yes\\
	V696 Mon      &  41335& 318& no& no& no& dec&no?\\
	HR 2418       &  47054&  63& no& no& no&dec?&yes\\
	OT Gem        &  58050& 437&  p& no& no&  no&yes\\
	$\beta$ CMi   &  58715& 168& no& no& no&  no&yes\\
	BR CMi        &  61273& 103& no& no& EL&  no& no\\
	UX Mon        &  65607& 152& no& no& EB&  no&yes\\
	HD 81357      &  81357&  93& no& no& EL&  no& no\\
	$\kappa$ Dra  & 109387& 429&  p& no& no&  no&yes\\
	$\vartheta$ CrB&138749& 158& no& no& no&  no&yes\\
	V839 Her      & 142926& 685&  i& no&yes&  no& no\\
	$\delta$ Sco  & 143275&  98&  p& no& no&inc?&no?\\
	$\zeta$ Oph   & 149757& 168&  p& no& no&  no&yes\\
	V744 Her      & 162732&1449&  i& no& no& dec& no\\
	V2048 Oph     & 164284& 164&  p& no& no& dec&yes\\
	V974 Her      & 164447& 183&  p& no& no&  no&no?\\
	$\omicron$ Her& 166014& 182& no& no& no&  no&yes\\
	NW Ser        & 168797& 327& no& no& no&  no&yes\\
	CX Dra        & 174237&1167&  p& no&yes&  no&yes\\
	$\beta$ Lyr   & 174638& 544& no&yes& EB&  no&yes\\
	7 Vul         & 183537& 131&  p& no& no&  no&yes\\
	V923 Aql      & 183656&1620&  i&yes& no&  no&yes\\
	V1294 Aql     & 184279&1709&p+i&yes&yes& dec&yes\\
	V1507 Cyg     & 187399& 193& no& no&yes&  no& no\\
	V1746 Cyg     & 189687& 209& i?& no& no&  no&yes\\
	V1624 Cyg     & 191610& 510&  p& no&  ?&  no&yes\\
	20 Vul        & 192044& 130& no& no& no&  no&yes?\\
	QR Vul        & 192685& 191&  p& no& no&  no&yes\\
	P Cyg         & 193237& 122& no& no& no&  no&yes\\
	25 Vul        & 193911& 124&  ?& no& no&  no&yes\\
       V2119 Cyg      & 194335& 140&  ?& no& no&  no&yes\\
          HR 7843     & 195554& 161& i?& no& no&  no&yes\\
        V1661 Cyg     & 198478& 288& no& no& no&  no&yes\\
         V832 Cyg     & 200120& 849&  p&yes&yes& inc&no?\\
        V1931 Cyg     & 200310& 889&  p& no& no&  no&yes\\
          8 Lac A     & 214168& 151& no& no& no&  no&yes\\
         V360 Lac     & 216200& 424& no&yes& EL&  no&yes\\
           EW Lac     & 217050&1281&  p& no& no& inc&yes\\
         V378 And     & 217543& 267&  p& no& no&  no&yes\\
   $\omicron$ And     & 217675&1636& no&yes& no&  no&yes\\
	   KX And     & 218393&1210& no& no&yes&  no&yes\\
	   KY And     & 218674& 970& no& no& no&  no&yes\\
	   LQ And     & 224559& 590& no& no& no&  no&yes\\
	   \hline
	   \end{tabular}
\tablefoot{Column LTEM: p = positive correlation between the brightness and
emission-line strength, i = inverse correlation between the brightness and
emission-line strength; column MTBIN: EB = eclipsing binary, EL = ellipsoidal
variations, yes denotes either mild sinusoidal variation with the known orbital
period or some peculiar orbital changes; column VLTV: dec = slow secular decrease
of brightness during phases of quiescence, inc = slow secular increase of
brightness during phases of quiescence.}
\end{table*}
%}
%\end{flushleft}
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\bibliographystyle{aa}
\bibliography{hvar6}
\end{document}
