\documentstyle[adc,11pt]{article}
\newcommand{\dmv}{Documentation for the Computer-Readable Version}
\newcommand{\cat}{A Catalog of Chromospherically Active Binary Stars}
\newcommand{\abbr}{CABS}
\newcommand{\catref} {Strassmeier et. al. (1992)}
\newcommand{\pcatref}{Strassmeier, K. G., Hall, D. S., Fekel, F. C., and Scheck,
M.}
\parindent 0pt
\parskip 11pt

\begin{document}

{\bf Abstract.}

The catalog contains 206 spectroscopic binary systems with at least one
late-type component that shows Ca II H and K emission in its spectrum. These
systems include the classical RS CVn binaries and BY Dra binaries. The catalog
summarizes information on the photometric, spectroscopic, orbital, and physical
properties of the systems as well as space motions and positions. Up to 42
``parameters'' for each stellar system are listed followed by the appropriate
reference to direct interested colleagues to the original papers. A
comprehensive selection of further information for each star is given in the
individual notes. In addition, the catalog contains a candidate list of 138
stars that have similar characteristics but are not definitely known binaries or
have not had Ca\,{\sc ii} H and K emission observed. This version updates and
replaces the 1988 catalog of similar information. (Strassmeier et al., 1988).

\section{Introduction}

Stars always appear in order of increasing right-ascension for the epoch 2000.0.
For the current version of the catalog, the literature was searched through
December 31, 1991 although a few later references are included. Additionally,
some entries are cited with ``private communication'', which make this catalog
also a first-hand source. A number in parentheses behind an entry always
corresponds to a reference given in the bibliography. See the 1988 publication
for specific requirements and restrictions in compiling these catalogs. See the
source reference for more details about this catalog.

The following binary systems, which were listed in the first edition of the
catalog, were not included in the present edition due to insufficient evidence
for chromospheric activity:   \\
$\eta$ And \\
26 Aql       \\
4 UMi        \\
$\nu^2$ Sgr  \\
$\tau$ Sgr

the following stars are chromospherically active but are components in a
``wide'' binary and were not included.

HD 25893 \\
HD 79211 \\

Forty three new binary systems have been included in the present
edition.

\section{Source Reference}

Strassmeier, K. G., Hall, D. S., Fekel, F. C., and Scheck, M., 1992,
A\&AS, 100, 173

\section{File Summary}

The catalog has a total of nine files with individual notes for the main
entries in Files 1 through 6 and a bibliography for all files. File 7 contains
the candidate list. File 8 contains the notes for the catalog and file 9, the
references. The nine files and their overall contents are:

\begin{definition}{8em}
\item[File 1.] Catalog cross reference
\item[File 2.] Photometric properties
\item[File 3.] Spectroscopic properties
\item[File 4.] Orbital elements
\item[File 5.] Stellar properties and general information
\item[File 6.] Positions and space motions
\item[File 7.] Candidate list
\item[File 8.] Notes (In LaTeX)
\item[File 9.] References

\end{definition}
\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit   & Format  & Item                   \\ \hline
 1 -  3   &        & I3      & Number                 \\
 6 - 15   &        & A10     & Variable name          \\
18 - 23   &        & I6      & HD/HDE number          \\
26 - 29   &        & I4      & HR number              \\
32 - 42   &        & A11     & Bayer name             \\
45 - 50   &        & A6      & Flamsteed name         \\
53 - 63   &        & A11     & DM number              \\
66 - 68   &        & A3      & SAO                    \\
70 - 75   &        & I6      & SAO number             \\
78 -104   &        & A27     & Other designation      \\
\hline
\end{tabular}
\caption{Format File 1 - Catalog Cross Reference}
\end{table}

\pagebreak[4]

\begin{center}

Notes to File 1
\end{center}

\begin{definition}{8em}
\item[No.]             Catalog sequence number.
\item[Variable]        ``General Catalog of Variable Stars'' identification. \\
                  NSV = ``New Catalog of Suspected Variable Stars'' number.
\item[Other names]     Identifications given by other sources.                \\
                  ADS = Aitken Double Star.   (The angle brackets,$ < >,$
indicate which of the visual components  is  the  active  binary.
                        The parentheses, ( ), indicate the visual  component  or
                        components that are included in the  V-magnitude  listed
                        in File 2).           \\
                  GC  = General Catalog,       \\
                  Gl  = Gliese Catalog,        \\
                  BV  = Bamberg Variable,      \\
                  CZ  = Cape Zone Star number, \\
                  FK4 = Fundamental Katalog No. 4, \\
                  AGK2= Zweiter Katalog der Astronomischen Gesellschaft,  \\
                  AGK3= Dritter Katalog der Astronomischen Gesellschaft,  \\
                  LDS = Luyten Double Star,                               \\
                  OS  = Otto Struve Variable,                             \\
                  P   = Prager Variable,                                  \\
                  S   = Sonneberg Variable,                               \\
                  vB  = van Buren number,                                 \\
                  SVS = Soviet Variable Star,                             \\
                  HV  = Harvard Variable,                                 \\
                  Lal = Lallande Star,                                    \\
                  Boss= Boss number,                                      \\
                  BPM = Bruce Proper Motion survey number,                \\
                  PPM = Proper Motion catalog,                            \\
                  1E..= First EINSTEIN catalog of x-ray sources,          \\
                  Ynn = Yale Catalog Volume nn number,                    \\
                  Cnn = Cape Photographic Catalog Volume nn number.       \\

\end{definition}

\clearpage

\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit   & Format  & Item                   \\ \hline
 1 -  3   &        & I3      & Number                 \\
 5 - 18   &        & A14     & Name                   \\
19 - 24   &        & I6      & HD/HDE number          \\
25 -      &        & A1      & HD/HDE component       \\
26 -      &        & A1      & Magnitude type         \\
27 - 32   & mag    & F6.3    & V$_{max}$                \\
34 - 38   &        & A5      & Reference for V$_{max}$  \\
39 - 46   & mag    & A8      & Delta wave             \\
47 - 51   &        & A5      & Delta wave reference   \\
52 - 60   & days   & A9      & Photometric period     \\
61 - 69   &        & A9      & Reference for P$_{phtm}$ \\
71 - 82   & mag    & A12     & $<U-B>$ hot/cool         \\
83 - 87   &        & A5      & Reference for $<U-B>$   \\
88 - 98   & mag    & A11     & $<B-V>$ hot/cool         \\
99 -103   &        & A5      & Reference for $<B-V>$    \\
105-119   & mag    & A15     & $<V-R>$ hot/cool         \\
120-124   &        & A5      & Reference for $<V-R>$    \\
125-139   & mag    & A15     & $<R-I>$ hot/cool         \\
140-144   &        & A5      & Reference for $<R-I>$    \\
\hline
\end{tabular}
\caption{Format File 2 - Photometric Properties}
\end{table}

\begin{center}
Notes to File 2
\end{center}

\begin{definition}{16em}
\item[V$_{max}$]        Maximum brightness in V bandpass.  ``pg'' means that
only an old photographic magnitude was available.

\item[DeltaV$_{wave}$]  Maximum amplitude of the ``wave'' in V passband, due to
spots,
                  not ellipticity or reflection.   CONST means that  photometry  has
                  been obtained but no wave has been observed.

\item [P$_{phtm}$]      Photometric (= rotation) period, in days, derived from
the light curve.   Rotation periods from (v sin i) measurements are  not
                  included.   If ``(orb)'' is given, then the photometric period
                  is nearly the same as the orbital period  in  File 4.
                  Sometimes we have computed P$_{phtm}$ from the wave  migration
period using the  relation  1/P$_{migr}$ = 1/P$_{phtm}$ -
                  1/P$_{orb}$; if so, we
                  have mentioned that in  the  individual  notes.   Due  to  the
                  inherently irregular behaviour of large starspot  groups,  the
                  photometric period  in  all  spotted  stars  is  intrinsically
                  variable!

\item [$<U-B>,<B-V>,<V-R>,<R-I>$]        Mean colors in the standard Johnson
UBVRI system for the hot/cool component respectively.   If no slash,
/, is given, then the combined color (outside eclipse)  is  listed.   Values  in
             brackets, [ ], are assumed from the spectral type versus color
             relations of Johnson (1966) [ARA\&A 4, 193],  FitzGerald (1970)
                  [A\&A 4, 234], or Schmidt-Kaler (1982)
                  [in: Landolt-Boernstein,Vol. 2b, p.1].
                  An asterisk, *,  means  that  this  entry  is
                  measured in the Kron-Cousins UBV(RI)$_{KC}$  system.   For
                  transformation to the standard Johnson system, see,  e.g.,
                  Bessell (1979) [PASP 91, 589].

\end{definition}


\hspace{9em}  Colors in brackets, ``[ ]'', are assumed from the spectral
classification.

\hspace{9em}        A slash, ``/'', always separates values for the
hot/cool component,
        respectively. If no slash is given, then the combined value is listed.

\hspace{9em}        Braces, ``( )'', denote the close binary in a
spectroscopic triple
        system.

\hspace{9em}        A color with an asterisk, ``*'', in front is
measured in the
        Kron-Cousins RI system. All other values are in the Johnson
        UBVRI system.

\hspace{9em}        ``const'' in the ``Delta V$_{wave''}$ column means
that photometry has been \linebreak[4] obtained but no spot wave has been
observed.

\clearpage

\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit         & Format  & Item                   \\ \hline
  1-  3   &              & I3      & Number                 \\
  5- 18   &              & A14     & Name                   \\
 19- 24   &              & I6      & HD/HDE                 \\
   - 25   &              & A1      & HD/HDE component       \\
 26- 42   &              & A17     & Spectral type hot/cool \\
 43- 51   &              & A9      & Spectral type reference\\
   - 53   &              & I1      & Binary nature          \\
 55- 59   &              & A5      & Binary reference       \\
 61- 69   & km/sec       & A9      & V sin(i) hot/cool      \\
 71- 79   &              & A9      & V sin(i) reference     \\
 80- 94   &              & A15     & CaII H\&K emission      \\
 95-103   &              & A9      & CaII emission reference\\
105-118   &              & A14     & H$\alpha$ behavior     \\
120-128   &              & A9      & H$\alpha$ reference    \\
129-137   &$10^{31}$ erg/s & A9      & X-ray luminosity       \\
138-146   &              & A9      & X-ray reference        \\
147-155   & mJy          & A9      & Radio flux density     \\
156-164   &              & A9      & Radio flux reference   \\
\hline
\end{tabular}
\caption{Format File 3 - Spectroscopic properties}
\end{table}

\begin{center}
Notes to File 3
\end{center}

\begin{definition}{15em}

\item[No]              Catalog sequence number.
\item[Name]            The more commonly used of the names in File 1.
\item[Spectral type]   Spectral type and luminosity class of  the  hot/cool
                       component, always in that order.

\item[SB]              Binary nature.  \\
\hspace{9em} SB1 = single-line spectrum,\\
\hspace{9em} SB2 = double-line spectrum,  \\
\hspace{9em} SB3 = three components are seen in  the  spectrum
(spectroscopic triple system),   \\
\hspace{9em} Y = yes, spectroscopic binary, but not yet known
if the spectrum is single- or double-lined.\\
\item[v sin i]         Projected rotational velocity  for  the  hot/cool
component in km/s.                                 
\item[CaII H \& K emission]     Singly ionized calcium H and K  emission.   This
column contains information on the strength of the emission  as  well
                  as to which component the emission belongs. Absolute
                  emission-line surface fluxes are given, if available, in  the
                  ``Notes''.\\
\hspace{14em} cool  =  the cooler component is the emitter,  \\
\hspace{14em} hot   = the hotter component is the emitter,    \\
\hspace{14em} both  =  both components show H and K emission.

class A, B, C, D, (E) =  emission strength after Hearnshaw's
scale, see Figure 1 in A\&AS 72, 291.                      \\

I$_{K}$ = 5, 4, 3, (2)=  strength of the K-emission line in terms of
Wilson's eye-estimated intensities on a scale from 0 (no) to 5 (``strong'')
emission. \\
\end{definition}

\begin{definition}{17em}

\item[H$\alpha$ behavior] Balmer H$\alpha$ line behaviour         \\

\end{definition}

\hspace*{12em}      abs. =   ``normal'' absorption,      \\
\hspace*{12em}      em.  =   emission above the continuum, \\
\hspace*{12em}      fld-in abs. =   absorption  profile
``filled-in'' with (presumably) \linebreak[4] chromospheric emission,\\
\hspace*{12em}      strong abs. =   strong absorption profile, \\
\hspace*{12em}      mod. abs.   =   moderate  absorption  (this
terminology is taken whenever an author used it but is equivalent to
``filled-in abs.''),           \\
\hspace*{12em} wk abs. = weakly filled-in absorption profile (in
these cases the degree of ``filling-in'' is not obviously visible by visual
inspection but significant when a standard star spectrum is subtracted).  \\
\hspace*{12em}       flares  =   H$\alpha$ flare has been observed. For further
explanation, the original reference should be examined.

\begin{definition}{10em}
\item [X-ray luminosity]        X-ray luminosity in $10^{31}$ erg/s. ``f$_{x}$''
means that only a flux measure in erg/cm$^{2}$/s is available.\\

\item [Radio flux density]      Radio flux densities in mJy.

\end{definition}

Spectral types and luminosity classes in brackets, ``[ ]'', are
assumed.

A slash, ``/'', always separates values for the hot/cool component,
respectively.

Braces, ``{ }'', denote the close binary in a spectroscopic triple system.

\clearpage

\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit        & Format  & Item                            \\ \hline
  1-  3   &             & I3      & Number                          \\
  6- 18   &             & A13     & Name                            \\
 19- 24   &             & I6      & HD/HDE                          \\
   - 25   &             & A1      & HD/HDE component               \\
 26- 34   & day         & F12.8   & Orbital period                  \\
 36- 40   &             & A5      & P$_{orb}$ reference               \\
 42- 46   &             & A2      & Orbital period variability      \\
 47- 55   &             & A5      & Period variability reference    \\
   - 58   &             & A1      & Component behind at conjunction \\
 59- 69   &HJD-2400000  & F11.3   & Heliocentric date - conjunction \\
 70- 74   &             & A5      & Conjuntion date reference       \\
 76- 82   & km/s        & A7      & V$_{0}$                         \\
 83- 88   &             & A6      & V$_{0}$ reference               \\
 90-100   & km/s        & A11     & K hot/cool                      \\
101-109   &             & A9      & K reference                     \\
111-114   &             & F4.1    & Eccentricity                    \\
116-120   &             & A5      & Eccentricity reference          \\
122-126   & $^\circ$    & F5.1    & Omega                           \\
128-132   &             & A5      & Omega reference                 \\
134-144   &$10^{6}$km   & A11     & a sin(i) hot/cool               \\
146-154   &             & A9      & a sin(i) reference              \\
\hline
\end{tabular}
\caption{Format File 4 - Orbital elements}
\end{table}
\begin{center}
Notes to File 4
\end{center}

\begin{definition}{10em}

\item[P$_{orb}$]            Orbital period in days. \\

\item[dP$_{orb}$/dt] Orbital period variability. More quantitative results in
terms of (dlnP/dt) are given in the individual notes. \\
\hspace{6em} y = yes  \hspace{10em}  n = no \\

\item[T$_{conj}$] Heliocentric Julian date of conjunction with the (presumed)
hotter star behind. If the star is not an eclipsing binary, then we have
computed T$_{conj}$ either from the time of periastron passage or, if e = 0,
from the time of quadrature in order to simulate primary eclipse.
\item [V$_{0}$] System's center-of-mass radial velocity in km/s.
\item [K] Semiamplitude of the hot/cool component in km/s. If
both stars have the same spectral class, then the more massive star is listed
first. If both stars have the same mass, then the larger star is listed first.
\item [e] Eccentricity.
\item [omega] Longitude of periastron in degrees.
\item [a sin i] Separation in
$10^6$ km. It means: (a sin i) = total semimajor axis if no slash, /, is given,
and (a$_{1}$sin i)/(a$_{2}$ sin i) = semimajor axis for the orbit of the
hot/cool component respectively. If both stars have the same spectral class,
then the more massive star is listed first. If both stars have the same mass,
then the larger star is listed first.

 \end{definition}


A slash, ``/'', always separates values for the hot/cool component,
respectively. If no slash is given, then the combined value is listed. In cases
where it is not clear which component is the hotter or cooler one, the times of
conjunction correspond to:             \\
\hspace*{9em} ``s'' = secondary behind, \\
\hspace*{9em} ``p'' = primary behind     \\
\hspace*{9em} ``t'' = tertiary behind.   \\

Braces, ``{ }'', denote the close binary in a
spectroscopic triple system.

``a ='' in the (a sin i) column means, that the sum of
the orbital semimajor axes is listed.


\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes         & Unit       & Format  & Item                   \\ \hline
  1-  3       &            & I3      & Number                 \\
  6- 18       &            & A13     & Name                   \\
 19- 24       &            & I6      & HD/HDE                 \\
   - 25       &            & A1      & Component              \\
 27- 33       & pc         & A7      & Distance               \\
 34- 38       &            & A5      & Distance refernce      \\
 40- 53       & mag.       & A14     & M$_{V}$ hot/cool       \\
 55- 59       &            & A5      & M$_{V}$ reference      \\
 60- 74       &solar mass  & A15     & Masses hot/cool        \\
 76- 80       &            & A5      & Masses reference       \\
 82- 91       &solar radius& A10     & Radii hot/cool         \\
 92-100       &            & A9      & Radii reference        \\
102-105       &            & A4      & Eclipse                \\
107-111       &            & A5      & Eclipse reference      \\
113-117       &$\circ$     & A5      & Inclination            \\
119-123       &            & A5      & Inclination reference  \\
125-127       &            & A3      & IUE archive            \\
129-131       &            & A3      & IAU Comm. 27 archive   \\
\hline
\end{tabular}
\caption{Format File 5 - Stellar properties and general information}
\end{table}
\clearpage

\begin{center}
Notes to File 5
\end{center}
\begin{definition}{9em}

\item [Distance] Distance in parsecs. If no reference is given, then the value
has been computed from the absolute visual magnitude already given in the
catalog. No interstellar absorption was taken into account. A value in brackets,
[ ], has been computed from an M$_{V}$ value itself in brackets, as explained
below.
\item [M$_{V}$] Absolute visual brightness. If no reference is given, then the
value has been computed from the distance already given in the catalog. A value
in brackets, [ ], is an assumption from the spectral type.
\item [Masses] Mass in solar units of the hot/cool component respectively. A
``$\geq$'' indicates that (m sin$^3$ i) is listed, and ``f(m)'' indicates that
the mass-function is given. If both stars have the same spectral class, then the
more massive star is listed first. If both stars have the same mass, then the
larger star is listed first. (Note that all entries in the ``MASSES'' bytes
followed by the reference ``(727)'' can't be found in that paper, but we have
used their orbital elements to determine these entries.)
\item [Radii] Radius in solar units of the hot/cool component respectively. A
``$\geq$'' indicates that (R sin i) is listed. Same convention as above for
cases of identical spectral class or equal mass.


\item [Eclipse]         Type of eclipse.  It means:                     \\
\hspace{12em} NONE  = Not eclipsing,                                    \\
\hspace{12em} TOT   = complete (total/annular) eclipses,                \\
\hspace{12em} PRTL  = partial eclipses,                                 \\
\hspace{12em} YES   = an eclipse has been observed, but it is not
known if partial or total                                               \\
\hspace{12em} PSBL = it is possible that eclipses take place but
further observations are necessary to confirm it.
\item [i] Inclination of the pole of the orbital plane or of the rotation axis,
in degrees.
\item [IUE]             Observed with IUE (through March 31, 1990)?
\item [IAU Comm. 27]    File in  the  IAU  Commission  No. 27  ``Archive  of
                Unpublished Observations  of  Variable  Stars''  (Breger 1985,
                PASP 97, 85; Breger, Jaschek, Dubois 1990, IBVS 3422).
\end{definition}

Values in brackets, ``[ ]'', are assumed.   \\
        ``f(m)'' denotes the mass-function.  \\
        Dashes, ``-'', in a reference column mean that this entry has been
        computed by the authors.               \\
        A slash, ``/'', always separates values for the hot/cool component,
        respectively.  If no slash is given, then the combined value is listed.
                                               \\
        Braces, ``( )'', denote the close binary in a spectroscopic triple
        system.                                \\

\clearpage

\begin{table} [h]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit         & Format  & Item                     \\ \hline
  1-  3   &              & I3      & Number                   \\
  6- 18   &              & A13     & Name                     \\
 19- 24   &              & I6      & HD/HDE                   \\
   - 25   &              & A1      & HD component		\\
 27- 28   & hr           & I2      & Right Ascension (2000.0) \\
 30- 31   & min          & I2      & Right Ascension (2000.0) \\
 33- 36   & sec          & F4.1    & Right Ascension (2000.0) \\
 39- 41   & $\circ$      & I3      & Declination (2000.0)     \\
 43- 44   & $'$          & I2      & Declination (2000.0)     \\
 46- 47   & $''$         & I2      & Declination (2000.0)     \\
 50- 56   & $\circ$      & F6.2    & Galactic longitude       \\
 58- 63   & $\circ$      & F6.2    & Galactic latitude        \\
 66- 68   & pc           & I3      & Distance                 \\
 71- 76   & km/sec       & F6.1    & Systemic Velocity        \\
 79- 83   &              & A5      & Sys. velocity reference  \\
 86- 89   &$0.001''$/yr  & I4      & Proper motion in RA      \\
 91- 95   &$0.001''$/yr  & I5      & Proper motion in Dec.    \\
 98-101   & pc           & I4      & X                        \\
103-106   & pc           & I4      & Y                        \\
108-111   & pc           & I4      & Z                        \\
113-119   & km/sec       & I4      & U                        \\
121-126   & km/sec       & I4      & V                        \\
128-133   & km/sec       & I4      & W                        \\
\hline
\end{tabular}
\caption{Format File 6 - Positions and space motions}
\end{table}

\begin{center}
Notes to File 6
\end{center}
\begin{definition}{10em}

\item [X, Y, Z]         Rectangular space coordinates relative to the sun in
parsecs.                                                                  \\
\hspace{17em} X is in the direction toward the galactic center,    \\
\hspace{17em} Y is in the direction of the galactic rotation, and  \\
\hspace{17em} Z is the distance from the  galactic  plane  and  is  positive
toward the galactic north pole.                      \\
\item [U, V, W]         Space velocities relative to the Sun in km/s.      \\
 U directs toward the galactic center (= right-hand system),  \\
 V is in the direction of the galactic rotation, and          \\
 W points in the direction of the galactic north pole.
For the computations we followed the  procedure  described  in
Johnson  and  Soderblom  (1987)  [AJ 93, 864].   We  used  the
distances (`Dist') and center-of-mass velocities (`V$_{0}'$)
from our Files 5 and 4 which are reproduced in this file for
convenience.
\end{definition}

\clearpage

\begin{table} [ht]
\centering
\begin{tabular}{ l l l l }
\hline
Bytes     & Unit         & Format  & Item                     \\ \hline
  1-  3   &              & I3      & Number                   \\
  6- 25   &              & A20     & Identification           \\
 27- 31   & mag          & F5.2    & V magnitude              \\
 33- 48   &              & A16     & Active Chromosphere?     \\
 51- 53   &              & I3      & Activity reference       \\
 57- 66   &              & A10     & Binary?                  \\
 69- 71   &              & I3      & Binary reference         \\
 75 132   &              & A58     & Notes                    \\
\hline
\end{tabular}
\caption{Format File 7 - Candidate list}
\end{table}

\begin{center}
Notes to File 7
\end{center}

\begin{definition} {14em}

\item [V magnitude]           Mean brightness in the V passband.
\item [ACT. CHROMOSPH.?] Active chromosphere? This column lists whether there is
observational evidence for the existence of an active chromosphere or not. It
means:         \\
\hspace{16em} HK emission  =  CaII H and K emission lines were observed,  \\
\hspace{16em} x-ray source = the star has been detected as an x-ray
source,                                                                   \\
\hspace{16em} H$_{a em.}$    =  H$_{\alpha}$ line is in emission,         \\
\hspace{16em} H$_{a fld-in}$ = H$_{\alpha}$ line is in absorption but
``filled in'' by (presumably) chromospheric emission,                     \\
\hspace{16em} ?            =  no observations available.                  \\
\item [BINARY?]            = Spectroscopic binary system?                 \\
\hspace{16em} SB1          =  single-lined spectrum,                      \\
\hspace{16em} SB2          =  double-lined spectrum,                      \\
\hspace{16em} yes          =  yes,   the  star  is  a  binary  but more
                 observations are needed,                                 \\
\hspace{19em} v$_{r}$ const? =  constancy of measured radial velocities  is
 questioned,                                 \\
\hspace{19em} eclipsing    =  the system is an eclipsing binary,          \\
\hspace{19em} ?            =  no observations available.                  \\

\end{definition}

File 8 is in LaTeX and can be read with the article style.
\\
\\
\\
\begin{table} [ht]
\centering
\begin{tabular}{ l l l }
\hline
Bytes     & Format  & Item                     \\ \hline
  4-  6   & I3      & Reference Number         \\
  9-210   & A202    & Reference                \\
\hline
\end{tabular}
\caption{Format File 9 - References}
\end{table}

\section{References}
Strassmeier K. G., Hall D. S., Zeilik M., Nelson E., Eker Z., Fekel
F. C., 1988, A\&AS 72, 192   \\

Strassmeier, K. G., Hall, D. S., Fekel, F. C., and Scheck, M., 1992,
A\&AS, 100, 173
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