\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 & $$ hot/cool \\ 83 - 87 & & A5 & Reference for $$ \\ 88 - 98 & mag & A11 & $$ hot/cool \\ 99 -103 & & A5 & Reference for $$ \\ 105-119 & mag & A15 & $$ hot/cool \\ 120-124 & & A5 & Reference for $$ \\ 125-139 & mag & A15 & $$ hot/cool \\ 140-144 & & A5 & Reference for $$ \\ \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 [$,,,$] 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 \end{document}