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{\bf Individual notes (Tables 1 to 6)}
\vspace{5mm}

  {\bf 1.  [33 Psc]}    (282)  listed  it as  a  binary  system  with  ``strong'' 
Ca\,{\sc ii}
emission.   (77) lists  spectral type K1III, (288) used $P_{\rm orb} = 78.93$ days and
suggested that  33 Psc  may not be an RS CVn type system.  (286) and (44) give
$M_V =  +2.4$ mag  ($\approx$27 pc),  but (306) lists Dist. = 84 pc.  Note the eccentric
orbit.   (193) determined  $M_V =  -0.6$ mag, (307) found a $V$-amplitude of 0.006
mag due to ellipticity effect, whereas (44) reported $\Delta V$ of about 0.05 mag.
The  time  of  conjunction  in  the  catalog  is  actually  derived  from  the
ellipticity effect.  (44) found similar (U,V,W) motions.

  {\bf 2.  [HD 38]}   The separation of the visual components A--B is only 3".

  {\bf 3.  [5 Cet]}   Ca\,{\sc ii} S Index = 0.767 (285). Photometry  from  
(437) showed a W
UMa type  light curve;  they found  $\Delta V =  0.2$ mag.   The full amplitude of
$\Delta V = 0.2$ mag is attributable to the ellipticity effect (459,437) with the
two minima  unequal by 0.055 mag in $V$ (582).  (459) and (582) suggest that the
K-star nearly  fills its  Roche  lobe.    (459)  also  gives  the  mass  ratio
(hot/cool) $\leq 0.82\pm0.16$.  $M_V = -1.5$ mag in reference (556).
(597) lists $L_X = 0.03 \cdot 10^{31}$ erg\,s$^{-1}$.

  {\bf 4.  [BD Cet]}     H and K emission a bit  weaker  than that seen in V711 Tau,
$F(K) = 3.1\cdot 10^6$ and  $F(H) = 3.3\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$  
(146).    Sometimes  no  $V$-variability  
(146),  (283) gives  $<(V-I)>_{KC} =  1.19$ mag  and $<(V-R)>_{KC} = 0.62$
mag, photometric  minimum at  JD 244\,4949.5 (206). (193) gives $V(max) = 8.2$ mag.

  {\bf 5.  [13 Cet A]}   Triple system!  The active system is the A-component of the
visual binary ADS 490 and belongs to the Hyades moving group (77), the visusal
component B  was seen  at blue wavelengths by (492) [B: G4V, $P_{\rm orb} = 6.92$ yr].
(77) mentions  ``$\delta$ Sct?'' type but not confirmed so far.  (282) listed it as
a binary  system with ``strong'' Ca\,{\sc ii}  emission.   (144) gave K = 38.4 km\,s$^{-1}$ and
(139) derived  e =  0.11!   Best orbit  is given.   (456) derived the relative
space motions (U,V,W) = $(-27,-14,-11)$ km\,s$^{-1}$.  (139) reports ``weak, 
I(K)$\approx$3'' Ca\,{\sc ii}
H and  K emission,  but (615)  obtained $\log F'(H) = 6.5$ 
erg\,cm$^{-2}$s$^{-1}$ with $V-R = 0.48$.

  {\bf 6.   [FF And]}     (395) gives $R$-brightness of 8.97 mag.   (818) lists $R-I =
0.65$ mag.  (380) listed (U,V,W) with $\gamma = +10$ km\,s$^{-1}$!
(862) lists $L_X = 0.03\cdot 10^{31}$ erg\,s$^{-1}$.

  {\bf 7.   [$\zeta$ And]}     (18), (77),  and (259)  give  K1II, (44) K0III and (348)
K1III.    (348)  derived  $\log  F_X  =  5.385$
erg\,cm$^{-2}$s$^{-1}$.   IR excess  $(J,H,K) =  (0.20,--,0.25)$ mag (349).  
$F(K) = 8.7\cdot 10^5$
and $F(H) = 1.1\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ (309).  (306) gives $M_V = 
-2.2$ mag and Dist. =
48 pc.   (259)  listed a  rotational period  of 38.9 days and (75) reported an
amplitude of  0.14 mag  due to  the ellipsoidal  shape of the primary with the
period of  the orbital  motion.  Probably ``contact'' configuration.  (44) found
similar (U,V,W)  motions.   Photometry from  1983-84 through  1985-86 has been
reported in  (579).   Recent discussion  of the  ellipticity effect  in (582).
(325) lists  $v\sin i \approx  45$  km\,s$^{-1}$.  
Other $v\sin i$ measures range between 36 and 40 km\,s$^{-1}$ (448,491).

  {\bf 8.   [CF Tuc]}     (34)  listed  a  F0V/G2--5V  spectral  type.   (283) gives 
$<(V-I)>_{KC} = 0.89$ mag.   An older orbit can be found in  (34).   Further $UBVRI$
photometry in  (580) and  references therein.  (658) reports an IR excess from
IRAS fluxes and broad-band IR photometry.  $T_{\rm conj}$ in Table 4 has been computed
from the orbit in (727).

  {\bf 9.   [HD 6286]}    (614) analyzed four groups of photometric $V$ data and found
two possible  periods of $6.21\pm0.15$ and $35.3\pm0.1$ days, respectively.  There
are several  possible spectroscopic  periods between 90 and 180 days, best one
is given in Table 4.

 {\bf 10.   [AY  Cet]}   White dwarf as hot component!  (170) classified the  
cool component  as G5IIIe. (259) lists $\log L_X = 31.18$ erg\,s$^{-1}$ and   
(856) lists $L_X = 2.086\cdot 10^{31}$ erg\,s$^{-1}$. Flare activity (146), 
$F(K) = 2.7\cdot 10^6$ and
$F(H) =  2.1\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$  (171), (253)  gives a time of light minimum at JD
244\,4636.0, (310) reports changes in the mean $(U-B)$ color of up to 0.1 mag and
0.07 mag in $(B-V)$.  (306) gives $M_V = 0.3$ mag and Dist. = 110 pc, (439) listed
59 pc.   Eccentric  orbit.   (262) derived  $R(G5) \geq 9$ R$_\odot$;  most  of  the
photometric characteristics  were taken  from (310)  but also  from (253).   A
preliminary orbit  can be found in (254).  (579) found a photometric period of
$75.12\pm0.03$ days,  substantially shorter  than the  one given  in the  table.
They derive $R\sin i = 9\pm 3$ R$_\odot$ for the G5III primary.  With a revised $v\sin i$,
$f(m)$, and  mean photometric period (655) derive $R = 15\pm 1$ R$_\odot$.  (254) found
$R = 6.8$ R$_\odot$ from flux relations.

 {\bf 11.   [UV  Psc]}   (308) gives G2V/K0IV, and (62) G2V--IV/K0IV.  Orbital period
is variable  according to  (62) and  (252), but (816) found no clear evidence.
(116) gives  $<B-V> =  0.81$ mag,  and (308)  $(B-V)_{\rm hot} =  0.72$ mag.   G-star is
variable (160).   (116) gives G2V--IV/K0IV, and (160) listed radii of 1.24/0.93
R$_\odot$  for  the  hot/cool  component  respectively  while  (116)  quoted
1.219/0.929 R$_\odot$.  (458) classified it as G2V/K0IV, (448) measured one
component in  their spectra  and listed  $v\sin i =  45$ km\,s$^{-1}$.   (815) lists $B-V =
0.69\pm0.02$ for  the hot  component and $0.91\pm0.06$ mag for the cool component
in agreement  with (160).   Properties  derived  from  light  curve  fits  are
summarized in (632), recent time of minima in (671).

 {\bf 12.  [HD 8435]}   (173) classified it as G8IV--III. $T_{\rm conj}$ in Table 4 has been
computed from the orbit in (727).

 {\bf 13.   [HD  8358]}   Asymmetric light variations (212), a time of light minimum
is JD  244\,5214.7  (212).  (335) showed that 0.52 days is the correct rotation
period.   (382) determined Ca\,{\sc ii} H \& K emission surface fluxes $F(K) = 
7.9-9.8 \cdot 
10^6$ and  $F(H) =  0.89-1.3 \cdot 10^7$ erg\,cm$^{-2}$s$^{-1}$,  they also  found a photometric
period of  0.515503 days.   Note  that this  star has an unusual broad H$\alpha$
emission line.   Further  $UBVRI$ photometry  in (580).  (382) reported 
$V(max) = 8.15$ mag.

 {\bf 14.  [AR Psc]}   (167) measured X-ray flux at 0.5--20 keV.  (349) reports X-ray
flares up  to $4.0\pm0.2 \cdot 10^{32}$ erg\,s$^{-1}$  during  1978.    (54)  mentioned  no
variability of  the Ca\,{\sc ii}  K-emission core during a one month interval.  $F(K) =
2.9\cdot10^6$ and  $F(H) = 2.9\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ (171).  
H$\epsilon$ in emission, $F(H\epsilon) =
5.1\cdot 10^5$ erg\,cm$^{-2}$s$^{-1}$  (171).   (147) gives G5 spectral type, (171) listed it as
G5III, (262)  reports that  the H$\alpha$  line of  the more  massive star is in
emission [as  the Ca\,{\sc ii}  K line]  while the  line of the less massive star is a
very weak  absorption feature.   Note the eccentric orbit!  Space motions also
in  (382).  (579) derived photometric periods of 12.11 and 12.38 in 1985
and 1986,  respectively.   (629)   obtained incorrect orbital elements!  $V\sin i$
measure of  (262) has  been updated  and a  better value  is given in Table 3.
Rotation is pseudosynchronous (826).

 {\bf 15.   [HD  10909]}    (283) found another photometric period of 63.83 days and
$<(V-I)>_{KC} = 1.04$ mag.  Note the eccentric orbit!  (614) verified that 
the 30-day  
photometric period is the  correct one.   With e = 0.39 and $P_{\rm orb} 
= 15$ days, the
predicted pseudosynchronous  rotation period would be $1/2 P_{\rm orb}$ but 
$P_{\rm phtm} = 2 \cdot P_{\rm orb}$ is observed!

 {\bf 16.   [HD 12545]}   This star showed the largest photometric wave amplitude of
any spotted  star known  to date  (701)!   Li\,{\sc i}6707 is a strong 
absorption line
(809).   $UBVRI$ photometry  of (809) gave $\Delta T_{\rm (phot-spot)} =  
1100\pm35$ K, $i =
50\pm17\deg$,  and $P_{\rm phtm}  = 24.30\pm0.02$  days. (806) report a 23.68  day
photometric period from four years of $uvby$ photometry at Lowell which would be
in excellent  agreement with the pseudosynchronous rotation period.  The space
motions in  (809), given  in Table  6, suggest an old disk star.  $V\sin i = 18.3$
km\,s$^{-1}$ (860).

 {\bf 17.  [6 Tri]}   Component $\iota$ Tri A of the visual binary ADS 1697, $\iota$ Tri B
is another  SB2 and only 4" distant.  (723) gives spectral types for HR 642 of
F5V/G5III (these  classifications belong  to the  visual B  and A  components,
respectively, not  to the  spectroscopic  binary  components  of  A).      For
component B:  F6V ($P  =  2.236$  days)  and  mentioned  ``$\Delta V  =  
0.075$  mag
pulsating?''.   (348) measured  $\log F_X = 6.074$ erg\,cm$^{-2}$s$^{-1}$.  (306) gives Dist. =
85 pc,  (245): 500  pc, (77):  250 pc.   (139)  derived $M_V = +1.6$ mag from an
assumed absolute  magnitude for  the visual comparison HD 13480B, which itself
is a  spectroscopic binary.   (436)  found some  evidences  for  a  systematic
secular variation  in light  on a  time scale  of $\approx$\,100 days.  
$V\sin i$ measure of
(448) has been updated and a better value is given in Table 3.

 {\bf 18.   [HD 14643]}   Another  possibility  for  $P_{\rm phtm}$  is  18.67  days  (283).
$<(V-I)>_{KC} = 0.96$ mag (283) in disagreement with the listed spectral type.

 {\bf 19.   [CC  Eri]}    See  also reference  (270).   IRAS fluxes are discussed in
(757).   (756) found  evidence  for  long-term  variations  of  the  mean  $JHK$
magnitudes from 1977 through 1990. (422) lists $L_X = 0.047\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 20.   [HD 17084]}   (283) lists $<(V-I)>_{KC} = 0.87$ mag.  (173) classifies it as
G5IV.  $T_{\rm conj}$ in Table 4 has been computed from the orbit in (727).
(856) lists $L_X = 4.365\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 21.   [RS  Ari]}    (703) estimates a spectral type of F8 from visual spectra.
The spectral  classification in  Table 3  is mostly  based upon  the eclipsing
light curve (702) [EA/DS = detached system with a subgiant].

 {\bf 22.   [VY  Ari]}    Correct photometric period is given in the table.  Earlier
determinations can  be found  in (171),  (297), (350),  and  (524).    $F(K)  =
6.8\cdot 10^6$ and  $F(H) =  6.8\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$  (171), (306)  gives K0III.    (297)
obtained $(V-R)_c  = 0.55$  mag, $(V-I)_c  = 1.08$  mag and $(B-V)_c = 0.97$ 
mag and
expect a K3--K4 dwarf.  (524) measured a magnetic field strength of $\vec{B} 
= 2000\pm
200$ G  with a  filling factor  of $0.66\pm0.14$  (see also 427).  A very 
similar
orbit with $e = 0.074\pm0.004$ is given by (635).  (818) lists $R-I = 0.35$ mag.

 {\bf 23.   [HD  19485]}    (366)  classified it  as a G5 dwarf.  $P_{\rm phtm} 
= 6.45$ days
(614).  Strong Ca\,{\sc ii} H and K emission from both components of $\log F'_{\rm hot}(K,H) =
(6.72,6.65)$ and $\log F'_{\rm cool}(K,H) = (6.61,6.53)$ erg\,cm$^{-2}$s$^{-1}$ (588).

 {\bf 24.  [HD 19754]}   (283) lists mean $<(V-R)>_{KC}$ and $<(V-I)>_{KC}$ of 0.61 mag and 1.16
mag, respectively.   See also (262).  (614) determined a photometric period of
$48.01\pm0.04$ days which fits their data combined with photometry of (283).

 {\bf 25.   [LX  Per]}    (24) and (51) classified it as G5IV/G5IV.  (108) gives for
the secondary $B-V = +0.93$ mag.   (65) postulated $dM/dt = 1.1\cdot 10^{-7} 
- 3.0\cdot 10^{-6}$ M$_\odot$yr$^{-1}$,  no $\vec{B}$,  and $d\ln P/dt = +1.13\pm1.05 
\cdot 10^{-6}$ yr$^{-1}$,  $F(K) = 1.3\cdot 10^6$  and
$F(H) =  8.6\cdot 10^5$ erg\,cm$^{-2}$s$^{-1}$ (309).  (203) gives masses 
$M_{\rm hot}/M_{\rm cool} = 1.33/1.39$ M$_\odot$ and
radii $R_{\rm hot}/R_{\rm cool}  = 1.60/3.16$ R$_\odot$.  (51) $<B-V> = 0.72$ mag.  (109) listed it with
spectral type  G0/K0.   (133) obtained  $P_{\rm orb} =  8.038044$ days.    For  period
variations see  also (103).   Distortion wave migration period is given as 460
days by (126) and as 475 days by (144).  A more recent value for the migration
wave period  is $479\pm5$  days (477), we used this value to derive 
$P_{\rm phtm}$ which
is given  in the catalog.  The eclipse is probably partial (DSH).  (44) listed
(U,V,W) =  (-40,-17,-21) with  a distance of 79 pc.  (103) lists 
$V(max) = 8.20$
mag.   $V\sin i$ measure  of (448) has been updated and a better value is given in
Table 3.

 {\bf 26.   [HD  19942]}   (614) additionally report a photometric wave amplitude of
$0.22\pm0.019$ mag  [Note that  the rms  error in (614) is a misprint].  $V\sin i =
13.9$ km\,s$^{-1}$ (860).

 {\bf 27.   [HR  1023]}    A-component  of the close visual pair ADS 2509 [B is less
than 1"  away].  New spectral classification is given in Table 3. (77) lists  
G5III and Harlan, 1974 (=738) classified it as G2Ib. 
(543) reported radial velocity variations of $\approx$17 km\,s$^{-1}$.  Weak
or no G-band in the spectrum (173).  The observed $v\sin i$ is more than ten times
greater than the upper limit for synchronous rotation (733).  IUE observations
by (732) show only two emission lines.  H$\alpha$ observations in (262), $v\sin i =
20$ km\,s$^{-1}$ (262).  (585) found no clear evidence for photometric variability from
4 years  of APT  data ($\sigma_{\rm int} = 0.0087$ mag), nor did (476).  (734) noted a
weak G-band  and EW(Li\,{\sc i}6707) = 221 m\AA \ ($\log n(Li) = 2.93$) and found $v\sin i = 17\pm5$
km\,s$^{-1}$.   (735) derived  an eccentric  orbit with $e = 0.037\pm0.009$, $\omega = 50$,
but otherwise  in agreement  with the orbit by (733) given in Table 4.  Ca\,{\sc ii} H
and K  spectra  show  weak  emission  with  a  sharp  central  absorption  but
moderately high surface fluxes of $\log F'_{\rm (K,H)} = (6.28,6.23)$ 
erg\,cm$^{-2}$s$^{-1}$ (588).

 {\bf 28.  [UX Ari]}   Activity parameter $\log R = 0.54$ (318), (307) gives Dist. = 55
pc, (259)  lists $\log L_X = 31.32$ erg\,s$^{-1}$.  IR excess $(J,H,K) = (0.44,0.72,0.83)$
mag (349).   Radio flux 200 mJy var.\ (33), $F(K) = 4.3\cdot 10^6$ and $F(H) 
= 3.4\cdot 10^6$
erg\,cm$^{-2}$s$^{-1}$ (309).   (306)  listed system  radial  velocity  $\gamma  =  +16$  km\,s$^{-1}$.
Variable microwave  radiation (119,157), UV-emission  (119,135), H$\alpha$ is
strongly correlated with phase (18), (251) also reports IR colors $(K-L) = 0.05$
mag, $(K-M)  = 0.0$  mag and  $(K-N) =  0.0$ mag.   Distortion  wave migration was
accelerating in early years (87) but wave was migrating hardly at all in later
years (563).   (44)  found  somewhat  different space motions, (U,V,W) = 
$(-26,-20,-17)$ km\,s$^{-1}$ with a  distance of  56 pc.   Weak  lines from  a third star are
visible at  red wavelengths.  This third star appears to have been detected by
(663) with  speckle interferometry.   Differential rotation from a sequence of
Doppler images is --2\% (Sun: +20\%) (710).

 {\bf 29.   [V711  Tau]}    A-component  of the  visual  binary  ADS  2644.    (135)
classifies it  as G5V/K0IV, (322) gives G2V/K1IV, (351) used G0V/K1IV and (77)
lists G9V.   (312)  measured $\Delta V_{\rm wave}  = 0.03$  mag in 1981 and 0.22 mag in
1979.   (347) gives  $L_X =  12\pm1.5\cdot 10^{30}$ erg\,s$^{-1}$,  (259) lists $\log L_X = 31.41$
erg\,s$^{-1}$ and  (250) gives $\log L_X = 31.29$ erg\,s$^{-1}$.  Activity parameter $\log R = 0.90$
(318).   IR excess  $(J,H,K) = (0.50,0.58,0.87)$ mag (349).  Radio flux 1200 mJy
(100), $F(K)  = 2.9\cdot 10^6$ and $F(H) = 2.6\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ (309).  UV-emission (8,
135), H$\alpha$  variable (16)  and line-shape  correlated with phase (18, 135),
EW(H$\alpha$) =  +685 m\AA \ (323), H$\alpha$ is also related to radio flux (246).  IR
colors $(K-L)  = 0.06$  mag, $(K-M)  =  0.0$  mag  and  $(K-N)  =  0.0$  mag  (251).
Distortion wave  migration period  is 13  yr (87).  Further radio observations
are also  given by (135), (49), (88) and (157).  (44) found somewhat different
space motions,  (U,V,W) = $(+23,-10,-2)$ km\,s$^{-1}$ using $(m-M) = 1.2$ mag.  Additional
$UBVRI$ photometry  in (579) and (580).  (642) derive a spot migration period of
$7.4\pm0.8$ yrs.   Optical  flares of  up to  0.6 mag  in $U$  and 0.18  mag in  $V$
reported by  (690) and  (691) and  another twice  as strong  later in the same
night seen by (874).

 {\bf 30.  [HD 22403]}   (262) calls it an early-type BY Dra system.  (804) report a
big X-ray  flare from  ROSAT observations.   $V\sin i$  measure of  (262) has been
updated and a better value is given in Table 3.  Earlier orbit by (176).

 {\bf 31.  [HR 1176]}   (201) listed it as a binary with Ca\,{\sc ii} 
emission (intensity
4 on  their scale  which is  very weak!).   H  and K emission already noted by
(201).   (559) finds intermittent H and K emission, most of their observations
showing no  emission.   High-resolution spectra  of (588) reveal weak emission
lines blueshifted  with respect  to the  Ca\,{\sc ii} absorption  resonance lines with
large V/R  emission ratio  [$\log F'($K,H$) = (6.22,6.14)$ erg\,cm$^{-2}$s$^{-1}$ (588)].  (306)
lists it  with Dist. = 14 pc which is inconsistent with the ``giant'' luminosity
classification.   Eggen (=44)  lists $B-V  = 0.70$  and $V = 5.80$ mag.  (725) and
(724)  found   no  clear   evidence  for   photometric  variability,  however,
microvariability and/or long-term variations possible [see note by D. Hoffleit
in IBVS  2695].   The F2:V  classifiation of  the secondary component has been
deduced from  the composite  spectrum (559).   $V\sin i$ measure of (588) has been
updated and a better value is given in Table 3.

 {\bf 32.  [V471 Tau]}   Although (44) claims V471 Tau is an outlying Hyades cluster
member, (696) claims it is not. Activity parameter $\log R = 1.53$ (318), $<(U-B)>
= +0.59$ mag,  $<(B-V)> = 0.92$ mag  (44),  eclipsing  Algol-type  (62),  primary
minimum (eclipse  of the  white dwarf)  at JD 244\,0612.6708 (742), $f(m) = 0.172$
(304).  H$\alpha$ is in absorption (222).  $M_V = +6.35$ mag in (44) and +5.6 mag
in (222).   $\gamma  = +36.8$ km\,s$^{-1}$ (44), with that (222) derived $(U,V,W) = 
(-43.3,-18.0,-2.2)$ km\,s$^{-1}$.   (304)  gave  $\gamma = +40$ km\,s$^{-1}$.   (340) gives  for  the  cool
component spectral  type K2V, (222) suggests K0V.  For period and $T_0$ see also
(338).   (342) gives  a trigonometric parallax of 0.0099" and $M_V = +4.5\pm0.7$
mag.   (696) measured  an absolute parallax of 0.006" and $\mu(\alpha,\delta) = (+115,-2)$.  
Distortion wave migration period is $247\pm4$ days, [from Guinan E.~F. \& 
Sion E.~M.: 1982,  (in prep.) as referenced in (141)].  From that (141) found
$P_{\rm phtm} = 0.520086$ days.  But (480) found retrograde migration with a period of
$182.17\pm0.73$ days.  (337) reports $uvby$-photometry, (480) also found evidences
for a  spot-cycle of  about 18  years.   (141) computed  a mass  loss rate  of
$1.6\cdot 10^{-6}$ M$_\odot$yr$^{-1}$.   The  photometric period  given in  the catalog has been
calculated using  the migration period given in (480) and their orbital period
of 0.52118301  days.  (337) gives individual $V$-magnitudes of 13.9/9.52 mag for
the   hot/cool component  respectively.   $(O-C)$ eclipse  residuals shown to be
consistent with the motion of a short period system about a 3rd component [see
Beavers, Herczeg \& Liu:  1986,  ApJ  300,  785].    Time  resolved  H$\alpha$
observations in (662);  recent times of minima in (671), spot ``wave'' photometry
in (742),  white-dwarf pulsation photometry in (743).  Ca\,{\sc ii} H and K monitoring
a.o. in the extensive study of (742).  (807) obtained further H$\alpha$ profiles
and conclude that the observed transient-emission components arise from plasma
surrounding the  K dwarf  and not  from plages  on the  surface as  thought in
(662).   V471 Tau  is also  listed in  the catalog  of Ritter (1990) [A\&AS 85,
1179]. (856) lists $L_X = 0.148\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 33.  [CF Tau]}   (702) lists it as G0 and as detached EA type.

 {\bf 34.   [HD 26354]}   (283) lists $<(V-I)>_{KC} = 1.07$ mag.  (173) classifies it as
K2IV.  See also references (501) and (134).

 {\bf 35.   [EI Eri]}   Correct orbital period is given!  The 2.044 day period is
an alias (262).  First orbit by (302) is practically identical with the one of
(583).   (146) suggests  $i \approx 30\deg$ and radius of the primary 
component $R \approx 3$ 
R$_\odot$.   Sporadic H$\alpha$  emission (18).   (146) gives spectral type G0IV--III
and $v\sin i  = 35-40$ km\,s$^{-1}$ and  a photometric  period of 2.049 days, (439) lists
Dist. =  60 pc  [note that  the 2  pc distance is a misprint in (439)].  (302)
showed that  the primary  nearly fills  its Roche  lobe.  EW(Li\,{\sc i}6707) = 
36 m\AA \ 
(302).  $P_{\rm phtm} = 1.935$ days (283), $\Delta V_{\rm wave} = 0.19$ mag (48).  Light curves
for the  1979/80, 1980/81,  and 1982/83  seasons can  be found  in (207).   An
improved orbit is given by (583).  
Nine  years of  $V$ photometry  has been  analyzed in  (583).   (584)
obtained $UBVRI$ photometry in 1988.

 {\bf 36.   [BD +23$^\circ$635]}    Hyades  triple system  (453).  Confirmed by (289) to be
chromospherically active,  but no  Ca\,{\sc ii} H \& K observation has been obtained so
far.    Note  that  two  stars  are  seen  in  the  spectrum  (284),  but  the
spectroscopic binary in this triple system is single lined.

 {\bf 37.   [HD  27130]}   (44) lists it as an Hyades-member and gives $(R-I) = +0.29$
mag.   (222) mentioned  it as  an eclipsing  binary with $\Delta V = 0.15$ mag but
without a secondary minimum.  (304) lists $e = 0.04$ and $T_0$ at JD 242\,3102.193.
(352) reports  large X-ray  flaring of $>10^{31}$ erg\,s$^{-1}$.   (409)  [= SAO catalog]
lists $\mu_\alpha  = +0.116"$ and $\mu_\delta = -0.017"$.  (U,V,W) also in (222).  The
system is  a SB2  with very  weak lines from the secondary component (301).  A
CORAVEL orbit is listed in (492).

 {\bf 38.   [HD  27149]}    (44) lists it as an Hyades-member and gives G2V spectral
type.   (304) lists  $e = 0.23$ and $T_0$ at JD 243\,6843.3.  (387) reports 
$P_{\rm orb} =
75.664$ days.  Note the eccentric orbit!  (U,V,W) also in (222).

 {\bf 39.  [HD 27691]}   Member of the Hyades.  Brighter component (A) of ADS 3169AB
[$P_{\rm orb} =  255.5$ yr,  B only 0.7" away with $V = 9.3$ mag].  Spectroscopic pair first
noted by  Adams  \&  Joy  1919.    Orbit  by  (544)  very  poor.    Alleged
eccentricity is likely to be spurious (Griffin R., priv. comm.).  SAO catalog
lists $m_V  = 8.1$ mag from AGK1.  (585) point out the possibility that the star
is a low-amplitude variable ($\Delta V < 0.01$ mag)  and  found  two  uncertain
photometric periods  of 3.5  and 4.9  days.   Although no obvious Ca\,{\sc ii} H and K
emission lines are visible in the spectrum (588), the flux level is moderately
high: $\log F'(K,H) =  (6.41,6.27)$ erg\,cm$^{-2}$s$^{-1}$ (588).  This is somewhat puzzling
since $v\sin i = 8$ km\,s$^{-1}$.  X-ray flares (290).

 {\bf 40.   [HD 28291]}   Very eccentric orbit! $P_{\rm orb} = 41.66$ days,$\gamma = +39.81$,
$K =  7.28$, $e  = 0.66$,  $\omega =  327$, $a_1 \sin i = 3.12\cdot 10^6$ km, $f(m) = 0.0007$,
$T(HJD) =  244\,3650.67$  (521).   Spectral type K0V [Woolley et al., see (521)].
(774) found  the star  to be  variable in  light with  $P_{\rm phtm} =  
11.5$ days and
assumed  it   to  be   the  rotation   period  [note  that  the  corresponding
pseudosynchronous rotation  period would be 8.3 days (Hut 1981, A\&A 99, 126)].
Ca\,{\sc ii} H \& K  $S$-index varies between 0.32 and 0.52 (775) [compared to, e.g., SV
Cam ($S = 0.47$), and HD 27130 ($S = 0.3\pm0.62$)].

 {\bf 41.   [HD  28591]}    (306)  listed a  G5IV classification.   (579)  derived a
photometric period  of $21.45\pm0.25$  days.  Seven radial velocities from (745)
confirm the orbit in the catalog.  $V\sin i = 25.8$ km\,s$^{-1}$ (745).

 {\bf 42.   [V833  Tau]}    A fainter star 2' distant is a white dwarf (575).  (379)
derived no photometric period but reported a $\approx$\,60 yr cycle with an amplitude of
0.5 mag.   The  system is  seen nearly pole-on, $i < 35 \deg$ (379).  (222) found
(U,V,W) = (-41.7,-18.2,-0.4) km\,s$^{-1}$ with $\gamma = +38$ km\,s$^{-1}$.  (222) measured $R-I =
0.510$ mag.  (818) also lists $R-I = 0.51$.  (618) observed a $V$-amplitude of 0.04
mag in  1983 and  flares in  $UBV$.  (619) found the first photometric period of
1.85 days.   Further  discussion in (574) and (747).  A new circular orbit has
been given  by (805): $P = 1.787979\pm0.000003$ days, $T_0 = 2447900.752\pm0.004$,
$K_1 = 10.3\pm0.1$ km\,s$^{-1}$, $\gamma = 35.19\pm0.1$ km\,s$^{-1}$.  Their measured $v\sin i$ (Table 3)
is $6.3\pm0.4$  km\,s$^{-1}$ as  compared to $8\pm2$  km\,s$^{-1}$  measured  by  (588).    (860)
determined $9.3\pm0.6$ km\,s$^{-1}$ and report several radial velocity measurements.

 {\bf 43.  [3 Cam]} (597) lists $L_X = 0.12\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 44.   [RZ  Eri]}   (65) postulated $dM/dt = 1.1\cdot 10^{-7} - 2.0\cdot 
 10^{-6}$ M$_\odot$yr$^{-1}$, no $\vec{B}$,
and $d\ln P/dt  = 4.48\pm4.01 \cdot 10^{-7}$ yr$^{-1}$.  (306) gives Dist. $\geq 16$ pc.  (259)
listed Dist. = 275  pc, (61)  [and (470)] gave Dist. = 105 pc.  (44): $<B-V> =
0.65$ mag.  Eccentric orbit!  (110) listed preliminary masses of 1.7/1.7 
M$_\odot$ for the
hot/cool component, respectively.   The  orbital period  in (304) is a misprint!  (528) [and
referenced in (61)] classified the star as A5--F5V/G8IV.  (U,V,W) space motions
can be  found in (44).  The radii listed in (558) are too large by a factor 2.
(411) found  $P_{\rm phtm} = 21.6$ days and (474) report a $V$-amplitude of 0.068 mag.
The photometry of (579) and a redetermination of the orbital elements by (586)
showed RZ Eri to be another asynchronous rotator.  $V\sin i$ measure of (448) has
been updated and a better value is given in Table 3.

 {\bf 45.  [V808 Tau]}   Hyades member.  (378) also mentioned $V_{\rm prim} = 10.28$ mag and
$V_{\rm sec} =  10.59$ mag.   Note  the highly  eccentric orbit!   See  also (276) and
(376).   (U,V,W) also  in  (222).    (645)  question  the  active-chromosphere
character of V808 Tau.

 {\bf 46.   [HD  30957]}   (376) noted the Ca\,{\sc ii} H and K emission and considered it a
probable spectroscopic  binary.   Asymmetries in  the H  and K  emission lines
suggest emission from both components (588).  (745) confirmed the existence of
doubled lines in the spectrum.

 {\bf 47.   [HD  31738]}    (727)  listed it  as a single star with $\gamma = +6.6$ km\,s$^{-1}$.
(262) found asymmetric absorption lines and suggested that they were due to an
unresolved secondary  component.  (588) identified it as a recently discovered
SB2.   Ca\,{\sc ii} H  and K  emission confirmed  by  (262).    (407)  discovered  the
photometric variability  but concluded  that their  comparison  star  was  the
likely variable.   (579) re-examined these data and found that HD 31738 is the
variable not  the comparison  star!   The star  is not listed in (298).  (283)
report a  $V$-variability of  0.04 mag.   H$\alpha$  is  a  weak,  almost  absent,
absorption feature  (262).   $V\sin i$ measure  of (262)  has been  updated and  a
better value is given in Table 3.

 {\bf 48.   [12  Cam]}    (77) lists $\gamma = -8$ km\,s$^{-1}$, which is wrong.  (745) lists six
new velocities and determined $v\sin i = 11$ km\,s$^{-1}$.  (712) [and (351)] listed Abt's
$e = 0.35$ orbit.  This orbit (=2), listed in the first version of the CABS
catalog, is wrong.  New orbit is listed, which has a somewhat different period
and zero  eccentricity (FCF).  IR excess $(J,H,K) = (0.17,0.28,0.15)$ mag (349).
(206) found  $M_V =  -1.5$ mag  from the  width of  the  Ca\,{\sc ii}  K  line.    (259)
calculated Dist. = 180  pc.   (412) found  $P_{\rm phtm} =  80.94$ days.   The large
minimum radius  of 16 R$_\odot$ comes from the observed photometric period and the
measured $v\sin i$.   (658)  reports large  IR excess at 12 and 25 
$\mu$m.  $V\sin i$
measure of (448) has been updated and a better value is given in Table 3.

 {\bf 50.   [HD  34802]}    (283)  lists $<(V-I)>_{KC}  = 1.14$ mag.  (306) lists 
G5IV.   A high-resolution echelle spectrum of the H \& K region in (538) shows
``strong'' emission  lines reaching  the continuum.   $T_{\rm conj}$ in Table 4 has been
computed from the orbit  in (727).

 {\bf 51.   [$\alpha$  Aur]}    Multiple  system.   (77), (62), a.o. gave spectral type
G0III/G5III. (881) and (590) revised the spectral types to G0-1III/G8-K0III. See  
also Griffin \& Griffin: 1986 [JAp\&A 7, 45] who found the hotter star to be  
the brighter star in $V$.
(663) obtained a new orbit  from speckle  observations and  found spectral  
types of  G0III and G9III. (881) give $b-y$ colors of 0.586 and 0.451 mag 
for the hot and cool component, respectively, which are better than the $B-V$  
colors listed in Table 2. 
Not a typical RS CVn system because the hotter component (G0III)
is the  active component,  UV-flux variations  $< 5\%$,  and 
$L_X(hot)/L_X(cool) =
0.1$, no  flaring (314).   IR  excess $(J,H,K)  = (-0.14,-0.21,-0.19)$ mag (349).
(136) reports  masses $M_{\rm hot}/M_{\rm cool}  = 2.91/3.03$ M$_\odot$ and 
radii $R_{\rm hot}/R_{\rm cool} = 8.9/14.1$ R$_\odot$.
(306) Dist. = 13 pc.  EW(H$\alpha$) = $-1445$ m\AA \ (323), strong Li\,{\sc i}6707 
line from
the ``F''-star  (345).   EW(He\,{\sc i}10830)  = 500$\pm$50 m\AA \ (435) [and 700 m\AA \ in (354)].
The rotational  period of  the ``G''-star  is uncertain!   The $V$-amplitude seen by
(315) and  listed in  the earlier version of this catalog with a question mark
is very  doubtful.   (315) also  found from  the same undersampled light curve
$P_{\rm phtm} =  366$  days;  recently  (426)  found  $P_{\rm rot}$(G0/K0) 
=  (10/67:)  days,
respectively.   (305) measured $v\sin i \,(hot/cool) = 35/9$ km\,s$^{-1}$.  (687) found their
comparison star  (9 Aur)  to be  variable with  a period  of 36--39 days and an
amplitude of  0.08 mag.   For another orbit determination see Batten A.~H. 
\& Erceg  V.: 1975,  MNRAS 171, 47P.    Speckle  observations  and  a
re-determination of the evolutionary status were made by Bagnuolo and coworkers
[AJ 96, 1056; AJ 98, 2275].   (653)  found phase dependent He\,{\sc i}10830 equivalent
width variations correlated with the 104-day orbital period.  

 {\bf 53.  [HR 1908]}   (372) lists 14 radial velocities which show the star to be a
binary system.   Three velocities by (860) show no variations.  $V\sin i = 
9.6\pm2.2$ km\,s$^{-1}$ (860) is quite different from the value of 
$<3$ km\,s$^{-1}$ listed in (588).

 {\bf 54.   [TW  Lep]}   $V\sin i$ of the F-star is $<20$ km\,s$^{-1}$ (171). $F(K)  = 5.0\cdot 
10^6$ and
$F(H) =  4.4\cdot 10^6$ erg\,cm$^2$s$^{-1}$  (171).   (306) gives  spectral type G4III for the
cooler star.  (283) found $P_{\rm phtm}$ = 28.57 or 28.34 days, (35) estimated Dist. =
50:  pc,   (439)  used   28.2  pc   which  is   inconsistent  with  the  giant
classification.  (283) also reports $<(V-I)>_{KC} = 1.16$ mag.  (306) listed 
$\gamma = +36$ km\,s$^{-1}$, which is wrong.

 {\bf 55.   [HD  37824]}    (262)  reported that  a UV  spectrum  shows  the  F-type
secondary suggested  by (173).   (727)  gives a  similar orbit.   Ca\,{\sc ii}  $F(K) =
1.3\cdot 10^6$ and  $F(H) =  1.3\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ (171).  (306) lists G5IV, Dist. = 63
pc and  $M_V =  +3.2$ mag  which are incorrect since the star is a giant.  (171)
gives $<(V-R)>  = 0.81$  mag and  $v\sin i$ of  the K-star of $<20$ km\,s$^{-1}$.  (283) found
$P_{\rm phtm} =  54.88$ or  53.48 days,  (214) found  $P_{\rm phtm} = 52.6$ days.  (262) found
$P_{\rm orb} =  53.5$ days.   (821) found six spots existing between 1978 and 1990 and
estimated the  differential rotation  coefficient  from  the  range  of  their
rotation periods.

 {\bf 56.   [HD  39576]}    $\gamma$  and  $K$  are  estimated  from  the  four  individual
measurements given  in (484).  EW(Ca\,{\sc ii} K) $\approx 0.2$ \AA \ (484), 
$E(B-V) \leq 0.03$ (484),
$F_{H1}+ F_{K1} =  2.62\cdot 10^7$ erg\,cm$^{-2}$s$^{-1}$,  and activity parameter $\log R_{HK} = -3.42$
(484). $V\sin i$ of $65\pm10$ km\,s$^{-1}$ measured by (484) seems too high, 
correct value given in Table 3.

 {\bf 57.   [HD  39937]}    Called  ``38 G  Pic'' in  (546).   Three  radial  velocity
measurements by (546) showed a range of $\approx$38 km\,s$^{-1}$ at 36 \AA/mm.  (123) found from
three observations,  +13.7, +15.3, and +4.5 km\,s$^{-1}$ at 40 \AA/mm, and 
from the Ca\,{\sc ii}
K emission  line +89, +8, and --11 km\,s$^{-1}$ at 2.5 \AA/mm and concluded 
that this may
be a  new RS  CVn type binary.  They also noted the displacement of the Ca\,{\sc ii} H
and K  emission lines  blueward from the absorption centroid.  Radial velocity
variability also  detected by  (768) from  four  observations  [+40.1,  +17.7,
+46.7, and  +2.9 km\,s$^{-1}$].   Microwave-flux density at 5 GHz of 3.3 mJy 
(758) is
rather small  when compared  to, e.g.,  V711 Tau.   (546)  lists the star 
with $m_V = 5.87$ mag.

 {\bf 58.   [SZ  Pic]}   Both components are seen in 20 \AA/mm spectra and are clearly
of different  brightness, line  ratio 0.7--0.8.  Measured radial velocities for
the brighter/fainter components  are $+16.2\pm1.2 / -63.1\pm4.5$  km\,s$^{-1}$.   See
reference (5).   (700)  points out that the photometric period of 2.4 days (9)
is wrong.   The  true rotation  period is  exactly twice  this value  and  was
entered into Table 2.

 {\bf 59.   [HD  39743]}    The information on this star is rather sparse and its entry
into the catalog is primarely based upon unpublished observations of one of us
(FCF).

 {\bf 60.   [CQ  Aur]}    (258) listed it as G0III(:), (65) gives $d\ln P/dt = +2.45\pm
0.42\cdot 10^{-6}$ yr$^{-1}$.   (353)  found a  differential rotation  rate  of  
$1.0\cdot 10^{-9}$
rad\,s$^{-1}$deg$^{-1}$, and  a cycle period of 4--5 yr.  Distortion wave migration period is
5.5 yr  retrograde (12),  from that  we have computed $P_{\rm phtm}$ which is given in
Table 2.   $V\sin i$ measure of (448) has been updated and a better value is given
in Table 3.

 {\bf 61.   [HD  42504]}   Another possibility for $P_{\rm phtm}$ is 50.59 days (283), (283)
also lists $<(V-I)>_{KC} = 1.08$ mag.  Note the eccentric orbit!

 {\bf 62.   [HD  45088]}    The  H \& K emission was first noted by Bopp, B. W.: 1980
[PASP 92,  218].   The primary orbit is from (419) whereas the secondary orbit
is from  (418), the  orbit is  eccentric!  (427) measured a magnetic field for
both stars:  $\vec{B}(K3) =  2400$ G  and $\vec{B}(K5) = 3000$ G.  (624) measured Ca\,{\sc ii} H and K
line-core flux  density of $2.7\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$.  (786) reports a non-detection
of long-term  photometric variability  using the  Sternberg  plate  collection
since 1900.

 {\bf 63.   [HD  46697]}   Another possibility for $P_{\rm phtm}$ is 13.95  
days (283). (306) lists Dist. = 240 pc.  (283) reports $(V-I)_{KC} = 1.14$ mag.

 {\bf 64.   [W92  in NGC2264]}     It is  not absolutely  clear if W92 is an NGC2264
cluster member or not (256).  (256) also gives the photometric period to 0.745
days or  1.490 days  and suggests  it as  a spotted W UMa-binary.  (256) gives
further $M_{\rm bol}  = +1.7$  mag and  $E(B-V) =  0.08$.   The $v\sin i$ value given in the
catalog is  that from  Herbig 1962,  (256) found  100--150 km\,s$^{-1}$.  (363) gives
relative 100-year proper motions.

 {\bf 65.   [SV Cam]}   (308) classified it as G0--5V/K4V, (258) lists G3V/G5V.  (65)
postulated $dM/dt = 1.3-3.1 \cdot 10^{-8}$ M$_\odot$yr$^{-1}$, no $\vec{B}$, 
and $d\ln P/dt = +1.58\pm0.64 \cdot 
10^{-8}$ yr$^{-1}$.    (293)  gives  a  differential  rotation  rate  of  $2.60\cdot10^{-10}$
rad\,s$^{-1}\deg^{-1}$ for  the active component, and a cycle period of 10 yr.  
$dP/dt$ due
to a  third body (76).  (293) reports a change of the migration direction from
direct to retrograde motion around 1975--76, and back to direct motion in 1983--84, 
thus  the photometric  period  is  variable  around  the  orbital  period.
(U,V,W) also  in (44).  Small change of systemic velocity over 40 years (630).
(76) found $i = 80\deg$.  (630) estimates masses of 1.0/0.7 M$_\odot$.  (810)
report light-curve  modeling with  a bright spot on the primary with radius of
$70\deg$  and temperature difference of 110 K.  Further spot modeling results in
(817).

 {\bf 66.   [VV  Mon]}    (258)  classified it  as G2/K0IV.  (65) postulated $dM/dt =
4.8\cdot 10^{-9} - 1.3\cdot 10^{-8}$ M$_\odot$yr$^{-1}$,  $\vec{B}(dipol) = 
156$ G, and $d\ln P/dt = -2.23\pm0.54 \cdot
10^-6$ yr$^{-1}$.  (293) gives a differential rotation rate of $5.6\cdot 
10^{-10}$ rad\,s$^{-1}$deg$^{-1}$ 
for the K0 star, and a cycle-period of 7--8 yr.  (109) gives G2V--III/K0III, and
masses of  1.45/1.35 M$_\odot$.   (293)  classified it  as G2V/K0III.  (110) listed
minimum masses of 1.4/1.5 M$_\odot$ for the hot/cool component respectively.  (257)
listed Dist.  = 260 pc.  The orbital period derived from the radial velocities
is 6.05056  days (507).   $V\sin i$ measure of (448) has been updated and a better
value is given in Table 3.

 {\bf 67.  [Gl 268]}   Other name: ``Ross 986''.  Flare activity reported by (534) and
(535).  Space motions also in (431).  (818) lists $R-I = 1.37$ mag.

 {\bf 68.   [SS  Cam]}    (258)  classified it  as F5V/G1III.  (259) gives $\log L_X =
30.89$ erg\,s$^{-1}$.   (65) postulated $dM/dt = 4.1\cdot 10^{-7} - 4.5\cdot 
10^{-6}$ M$_\odot$yr$^{-1}$, no $\vec{B}$, and
$d\ln P/dt =  +2.07\pm1.72 \cdot 10^{-7}$ yr$^{-1}$.  Cool star fills 95\% of its Roche lobe.
Distortion wave  migration period is 78 yr (61) [and references therein], from
that we  have computed $P_{\rm phtm}$ which is listed in Table 2.  $\Delta 
V_{\rm wave} = 0.11$ mag in (61), $<V> = 10.0$ mag in (258).

 {\bf 69.   [HD  57853]}    Binary with HR 2813 (77).  Orbit for the A - Bab pair is
given.   (697) conclude  that the  system is  at least  triple  and  that  the
observed ``secondary'' lines belong to the brighter component of a close binary:
``primary'' lines  are designated A, ``secondary'' lines Ba, and the unseen binary
component as  Bb [Bab:  $P_{\rm orb} =  10$ days  (697)].   Orbit in  Table 4 might be
eccentric (697)  but more  observations are needed.  EW(He\,{\sc i} D3) = 40 
m\AA \ (697).
(615) report  $\log F'$(Ca\,{\sc ii} H) =  6.24 erg\,cm$^{-2}$s$^{-1}$,  and 
noted  $v\sin i = 25$ km\,s$^{-1}$.
Strong Lithium 6707 line has been observed by (827).

 {\bf 70.   [AR  Mon]}    (259) gives spectral type F--G/K0III, (62) listed G8III/K2--3III.  
(258) classified the cooler component as K0III.  (65) postulated $dM/dt
= 1.0\cdot 10^{-10} - 5.2\cdot 10^{-9}$ M$_\odot$yr$^{-1}$, $\vec{B}(dipol) 
= 44$ G and $d\ln P/dt = -1.98\pm1.49 \cdot 
10^{-6}$ yr$^{-1}$. Semidetached  configuration (875). (159) gives Dist. = 495(:)
pc.

 {\bf 71.   [YY  Gem]}    Other  name: ``Castor C''.  C-component of the bright visual
multiple system  ADS 6175  is the eclipsing binary YY Gem [A-component = $\alpha$
Gem, B-component  = HD  60178].   Circumstellar matter (391), the masses given
are times  $\sin^3 i$,  but $i$  is near $90\deg$ (390).  (380) lists $M_V = +8.26$ mag
and parallax  of 0.064".  (461) reviewed the period determinations, (380) also
lists $(B-V)  = 1.49$ mag and $(R-I) = 0.78$ mag.  EXOSAT and IUE observations in
(652). (423) lists $L_X = 0.04\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 72.   [HD  61245]}   Another possibility for $P_{\rm phtm}$ is 11.57 days (283), (283)
also lists $<(V-I)>_{KC} = 1.06$ mag.

 {\bf 73.   [$\sigma$ Gem]}   (129) gives $L_X = 2.04\cdot 10^{31}$ erg\,s$^{-1}$,  
(471) reports it as a
fast-transient X-ray  source and  detected an  outburst in  1977.   IR  excess
$(J,H,K) =  (0.20,0.14,0.12)$ mag  (349).   Transition-region line strengths are
correlated with  orbital phase  (314).   $F(K) =  7.0\cdot 10^5$ and  $F(H) 
= 5.7\cdot 10^5$
erg\,cm$^{-2}$s$^{-1}$ (309).   (306)  gives Dist. = 40 pc.  Cycle period is 5.8 yr (311),
cycle period  from spot modeling is 2.7 yr (564).  EW(H$\alpha$) = --1000 m\AA, and
EW(Li\,{\sc i}6707) $\approx$ 31$\pm$10 m\AA \ (323),  EW(He\,{\sc i}10830) = 1000 m\AA \ (354), (356) also
gives $M_V  = -1.6$  mag from H \& K width.  (139) listed it with $M_V = +0.4$ mag.
EXOSAT and  IUE observations  in (660).  Ca\,{\sc ii} H and K and H$\alpha$ observations
in (588)  and (649).   $V\sin i$  measure of  (689) has  been updated and a better
value is given in Table 3.

 {\bf 74.   [HD  65195]}    Binary  system containing a giant star with a relatively
short orbital period.  $V = 9.12$ mag is an estimate in (550).  PPM star catalog
(=737) lists  Mag =  10.0.  Ca\,{\sc ii} H and K spectra show weak emission lines with
$\log F'(K,H) = (6.06,6.01)$ erg\,cm$^{-2}$s$^{-1}$ (588).

 {\bf 75.   [54  Cam]}   Spectrum consists of an F9IV and a G5IV composite (590) and
not of  two F9  stars as  listed in  the first  version of  the CABS  catalog.
Activity parameter  $\log R  = -0.16$  and $P_{\rm phtm}  = 10.90$ days (318).  IR excess
$(J,H,K) =  (0.13,0.05,0.15)$ mag (349).  Eccentric orbit!  (139) suggested that
the Ca\,{\sc ii}  H \&  K emission  is probably not chromospheric, 
(439) reports a non-detection  
with  the VLA  at 4.8  GHz.   (139) listed it as F8V.  (U,V,W) space
motions also in (44).  Emissions are only seen for the cooler component (590).
(411) shows that the rotation, defined by the starspots, is pseudosynchronous.

 {\bf 76.   [HD  71071]}   (283) determined two possibilities for $P_{\rm phtm} = 20.83$ and
32.92 days,  and $<(V-I)>_{KC}  = 0.96$  mag.   Note the  eccentric orbit!   (614)
performed a  period analysis on several $V$-band data groups and found a variety
of periods  consistent with  their data  (9.5, 21,  34, and 65 days).  We have
entered the most likely period in Table 2 (i.e., 21 days).

 {\bf 77.   [GK  Hya]}    (258)  classified it  as  G5V  and  noted  a  semidetached
configuration.   (259)  gives  $\log L_X = 30.90$  erg\,s$^{-1}$.   (65) gives  $d\ln P/dt =
-2.28\pm1.27 \cdot 10^{-7}$ yr$^{-1}$.   (109) gives F8/G8 spectral type,  (62) listed it
as G0/G7IV.   $V\sin i$ measure of (448) has been updated and a  better  value  is
given in Table 3.

 {\bf 78.   [HR  3385]}    Our  spectra show  now evidence  of the  F-type companion
suggested by (173).  (283) lists $<(V-I)>_{KC} = 0.93$ mag.  $T_{\rm conj}$ in Table 4 has
been computed  from the  orbit in  (727).   (829) reports  $\log n\,(Li)  = 
1.1$ and 
equivalent width  $\approx 50\pm10$ m\AA \  [see also  (827)],   and  
$v\sin i  =  10-15$  km\,s$^{-1}$.
Spectral types were originally given by (173) of K0III+F, and G8III by Houk.

 {\bf 79.   [RU  Cnc]}    (109) assigned F5/K1 spectral type, (62) listed F9V:/G9V:.
(65) postulated  $dM/dt = 4.8\cdot 10^{-11} - 2.4\cdot 10^{-10}$ 
M$_\odot$yr$^{-1}$, $\vec{B}(dipol) = 111$ G, and
$d\ln P/dt =  -2.09\pm0.80 \cdot 10^{-7}$ yr$^{-1}$.   (353)  gives a differential rotation
rate of $5.5 \cdot 10^{-10}$ rad\,s$^{-1}$deg$^{-1}$ for the active component, and a cycle period of
4--5 yr.   (12) listed a distortion wave period of 7.5 yr retrograde, from that
we have  computed $P_{\rm phtm}$ listed in Table 2.  (112) lists $V = 10.1$ mag.  (813)
obtained fundamental photometric parameters from $uvby$ and H$\beta$ photometry.

 {\bf 80.   [RZ Cnc]}   (258) and GCVS [edition 1970] give K2III/K4III.  (259) lists
K1III/K4III.   (304) $i = 87.5\deg$, (65)  postulated  $dM/dt  =  3.2\cdot  
10^{-13}  -
6.0\cdot 10^{-11}$ M$_\odot$yr$^{-1}$,  $\vec{B}(dipol) =  8$ G  and $d\ln P/dt = 
-2.39\pm2.06 \cdot 10^{-7}$ yr$^{-1}$.
Semidetached configuration  (875).   (159) derived  $M_V =  1.4/2.3$ mag  and  a
distance of 310 pc.

 {\bf 81.   [TY Pyx]}   (108)  gives  $(B-V)_{\rm secondary} = +0.69$ mag.   
(44)  mentioned
$<B-V> =  0.685$ mag and $\Delta V = 0.05-0.1$ mag over a few hours. (351) 
gave $v\sin i =
30^{+10}_{-5}$ km\,s$^{-1}$.   $V\sin i$  measure of (326) has been updated and a better value
is given  in Table 3.  (7) reports a $V$-amplitude of 0.14 mag.  (65) postulated
$dM/dt =  0-3.2 \cdot 10^{-7}$ M$_\odot$yr$^{-1}$, no $\vec{B}$, and $d\ln P/dt = +1.71\pm3.00 \cdot 10^{-7}$ yr$^{-1}$.
IR excess  $(J,H,K) = (-0.10,0.09,0.11)$ mag (349).  $F(K) = 1.2\cdot10^6$ and $F(H) =
3.1\cdot10^6$ erg\,cm$^{-2}$s$^{-1}$  (309),  both  G5-stars  are  active  
(171).  (306)  gives
$\mu_\alpha =  -0.066"$, Dist. = 20  pc and $M_V = +4.4$ mag.  (282) listed it with
$M_V = +0.22$ mag.  (113) gave G4--5V/G5--7V.  (U,V,W) space motions also in (44).

 {\bf 82.   [WY  Cnc]}    (65)  estimated $dM/dt  = 0-1.7 \cdot 10^{-8}$ M$_\odot$yr$^{-1}$, no $\vec{B}$, and
$d\ln P/dt = -1.74\pm2.50\cdot 10^{-8}$ yr$^{-1}$.   Sarma M.~B.~K.: 1976  
[Bull. Astron.  
Inst. Czech. 2, 335]  derived a cycle period of 10 yr.  Migration wave period
is 5.5(:)  yr [see (61) and references therein], yielding a photometric period
of 0.8290(:)  days.   (24) obtained  $V(max) =  9.49$ mag.   (659)  report an IR
excess of  the primary  star.   Secondary is  probably no later than M0 (632).
(632) also  derive masses and radii from a light curve solution.  (665) report
$V$ and  $K$-band photometry.   $BV$ photometry for the years 1988 and 1989 
has been reported by (694).

 {\bf 83.   [XY  UMa]}    (258)  and (329)  mentioned it  to be semidetached.  (308)
derived $B-V=0.85$  mag, (329)  gives $i = 83.5\deg$ and found no secondary
component on  blue spectrograms  with 86 \AA/mm and 136 \AA/mm.  (65) postulated
$dM/dt  =  1.3-2.6 \cdot 10^{-7}$ M$_\odot$yr$^{-1}$,  no $\vec{B}$,  and  
$d\ln P/dt = +8.82\pm3.09 \cdot 10^{-8}$ 
yr$^{-1}$.  The average system brightness varies on a time  scale of 25 yr (329).
Flares in  $UBVR$ (154,  155); XY  UMa is not the radio source detected by (55),
see Cohen  A.~M. et al.:  1977 [Mem. R. Astr. Soc. 84, 1].  (460) presents 
a soft X-ray light curve. (329) noted a 3.5--4 yr spot cycle. Secondary mass 
is estimated of 0.6 M$_\odot$ by (630). First orbit determination also by (630).  
(659) report an IR excess of the primary component.  Recent times of minima in
(669). Further photometry  in (679)  and (685). Long-term variations of the
orbital period with 25 or 40 years (755).

 {\bf 84.   [HD  80715]}    Strong  Ca\,{\sc ii} IRT  emission reversals   
(279).  ``Possible
microvariability'' noted  by Rufener \& Bartholdi,  1982  [A\&AS
48,  503].   (279) suggested  the dK3/dK3  spectral type.   (510) noted
moderate Ca\,{\sc ii}  HK emission.  Strong emission found from both components (577).
Balmer  H$\epsilon$ also  in  emission  (577).    (681)  confirm  the  photometric
variability.

 {\bf 85.   [IL Hya]}   (44) mentioned filled-in H$\alpha$.  $F(K) = 2.0\cdot 
10^6$, and $F(H) = 3.0\cdot 10^6$  erg\,cm$^{-2}$s$^{-1}$ (309). 
$(R-I)  = +0.45$  mag  given  by  (44).    $UBVRI$ photometry also  in (368).   
(35)  estimated Dist. = 38 pc which is certainly 
incorrect.   (439) listed  Dist. =  263 pc  which has  been  adopted  for  the
catalog.   If IL Hya is indeed a giant then this distance is the 
best estimate, 
not the  value of 138 pc ($M_V = +3$ mag) suggested by (368).  (114) found 
$P_{\rm orb}
= 12.868$  days from  eight $v_r$  measurements.   (368) [and in (44)] incorrectly
assumed a double period light curve and $P_{\rm phtm} = 25.4$ days, (114) has seen two
unequal maxima  per cycle  with two  possible photometric  periods, 12.89  and
12.75 days,  which is  in accordance  with the  results of  (283).  (114) also
reports a  wave amplitude  of $\Delta V = 0.15$ mag in 1981. (44) used 
$\gamma = 0(:)$ km\,s$^{-1}$ and obtained  (U,V,W) =  (-3,-9,-28) km\,s$^{-1}$.   
(114)  classified it  as  F5V/K0III.
(686) report  a $V$-amplitude of  0.16 mag in 1988.  (368) discovered the light
variability of  this star in 1971 with a visual amplitude of 0.45 mag which is
the third largest spot amplitude ever seen from a CA binary system.

 {\bf 86.   [HD  83442]}    (373) gives $P_{\rm phtm} = 65.7$ days, (283) lists $<(V-I)>_{KC} =
1.22$ mag.   Eccentric  orbit!   See also (134).  High velocity star, see space
motions in Table 6!

 {\bf 87.   [DH  Leo]}    Triple  system consisting  of a  K0V primary with variable
H$\alpha$ activity,  a late K or M0 dwarf secondary with H$\alpha$ emission, and a
distant inactive  third component  of late  K or  early M dwarf classification
(153). The 3$^{rd}$ component has been detected by speckle interferometry (880).   
$f(m)$ for  the close  pair =  1.21 (153),  $i = 70\deg$ (14).  (14) also
gives $a\sin i  = 1.38\cdot 10^6$ km, the listed $a\sin i$ is for the primary and secondary
SB system.   [(222) a.o. suggested that the third component is a white dwarf,
which turned out to be wrong.]  Activity parameter $\log R = 1.31$ (318).  
$F(K) =
1.1\cdot 10^7$ and $F(H) = 7.5\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ (309).  (18) reports sporadic H$\alpha$
emission.   (153) mentioned possible partial [grazing] eclipses with 
$i \approx 70-75\deg$, but are not confirmed by reference (425).  Note also
that $T_{\rm conj}$  is taken  from the  preprint of  (425). (U,V,W) also  
in (222). 
(590) arrived  at slightly  different spectral  classifications for  the close
pair of K2V+K5V and $v\sin i = 47$ and $33$ km\,s$^{-1}$, respectively.
(856) lists $L_X = 0.209\cdot 10^{31}$ erg\,s$^{-1}$.

 {\bf 88.   [XY  Leo B]}    The primary component  (=XY Leo A: two early K dwarfs) is
the well-known  W UMa  binary XY Leo.  The Ca\,{\sc ii} H and K emission of component B
was also  seen by  (835) but  thought to  be associated  with the A-component.
H$\alpha$ appears  to be  slightly stronger  for the  tertiary (Ba) than for the
quarternary (Bb) (830).  Strong Mg\,{\sc ii} h and k emission from the combined system
were seen  by (833).   Orbital  period A-B  is 7274  days (834).   Inclination
between the  two orbits  $\approx 66\deg$ (830).  (832) observed X-ray 
luminosity of
$5.8-6.1\cdot 10^{29}$  erg\,s$^{-1}$ for XY Leo A+B but (830) noted that 
approximately half of 
it must be due to B (this is listed in Table 3).

 {\bf 90.   [HD  91816]}   The photometric period of (365) is likely 1/2 the orbital
period!  See also (579).  (578) found some evidence for a slow decrease of the
mean $V$  brightness from  1984 through  1988.  This trend is confirmed by (580)
who finds $V(max) = 8.021$ mag.

 {\bf 91.  [DM UMa]}   (813) noted that a main-sequence luminosity classification is
in better agreement with their $uvby$ and H$\beta$ photometry.  (36) presented the
first orbit  and reports a variable H \& K emission, H$\alpha$ is correlated with
flare activity.   (36)  gives K2IV--III, and reports a soft X-ray detection and
(132) gives  $L_X = 7\cdot 10^{31}$ erg\,s$^{-1}$.  (259) measured 
$\log L_X = 31.24$ erg\,s$^{-1}$.  Note
that the  given photometric period is the mean derived from two-spot 
modelling
-- the individual values are $P_{\rm phtm} = 7.471$ and $7.481$ days (475).
(683)  report $V$  amplitudes   between  0.04  and  0.18  in  1987  and  1986,
respectively.   Further photometry  in (693).   $V\sin i$  measure of  (448) is in
agreement with values from KPNO spectra. (FCF) reports line-profile variability.  

 {\bf 92.  [$\xi$ UMa B]}   B-component of the visual binary ADS 8119.  See also (330).
Activity parameter $\log R = +0.28$ (318).  (375) derived an age of 
$> 3.0\cdot 10^9$ yr
from a  two temperature  fit.  (77) notes ``VAR: ampl. 0.03 mag''.  (U,V,W) also
in (375).   The  given time  of conjunction is derived by visual inspection of
the velocity  curve in  Berman, L.:  1931 [Lick  Obs. Bull. 15, 109].   (579)
report a  possible long-term  periodicity with  $P \approx 800$ days and $\Delta V \approx 0.05$
mag from  2 1/2  years of  data.  The two visual components of the system have
similar spectral types (G0V), but quite different Lithium contents [see, e.g.,
(827)]. The revised spectral classifications by (506) appear to solve the Li problem.  


 {\bf 93.  [HR 4430]}   Ca\,{\sc ii} H and K emission not detected by (139) and (726); (741)
lists a  very weak  H and  K line-core  flux density.   The major cause of the
light variability of $\Delta V \approx 0.1$ mag is the ellipticity effect (229, 579).  First
orbit of  (230) was  judged circular  by Lucy \& Sweeney  1971 [AJ 76, 544].
H$\alpha$  shows   no  line-profile   variability  (670).    The  newly  derived
eccentricity ($0.024\pm0.011$)  might not  be significant (670).  (588) measured
$v\sin i = 16\pm2$ km\,s$^{-1}$.

 {\bf 94.   [DF  UMa]}   A-component of the close visual binary ADS 8242 (separation
2--3").   ADS 8242B  is also  a dM star with weak H \& K emission [see (393) and
(394)].   (270) suggests  the secondary  to be  $\approx$\,dM5.   (638)  
present EXOSAT observations and found $L_X = 0.027\cdot 10^{31}$ erg\,s$^{-1}$   
and evidence for a X-ray flare. 

 {\bf 95.   [HD 101309]}   Another possibility for $P_{\rm phtm}$ is 11.71 days (283), (283)
also gives $<(V-I)>_{KC} = 1.07$ mag.

 {\bf 96.  [HR 4492]}   (306) lists Dist. = 33 pc, (77) lists it as A0V/G2III, (283)
reports  mean  $(V-R)_{KC}$  and  $(V-I)_{KC}$  colors  of  0.53  mag  and  1.06  mag,
respectively.   (483)  listed  $P_{\rm orb}  =  53.85$  days.    (123)  also  reported
moderately strong  H \&  K emission.   $T_{\rm conj}$ in Table 4 has been computed from
the orbit in (727).  $\log L_X = 31.63$ erg\,s$^{-1}$ (856).

 {\bf 97.  [RW UMa]}   (259) gives $\log L_X = 30.64$ erg\,s$^{-1}$, (347) reports  
$L_X = 435\pm
31\cdot 10^{30}$ erg\,s$^{-1}$  due to  flare activity.   (130) reports an 
X-ray emission of $9.6\cdot 10^{32}$ erg\,s$^{-1}$.   
(65) postulated $dM/dt = 4.4\cdot 10^{-10} 
- 1.4\cdot 10^{-9}$ M$_\odot$yr$^{-1}$,
$\vec{B}(dipol) =  245$ G,  and $d\ln P/dt = -2.65\pm0.75 \cdot 10^{-7}$ yr$^{-1}$.  (61) listed it
with F9V/K1IV  spectral type.   Masses  and radii  also can be found in (110),
(565) and  (109).  (334) gave an inclination of $i = 81\deg$.  (611) adopted $i =
88\deg$  and observed  a photometric  ``wave'' amplitude of 0.07 in $B$ in 1973 and
report a  possible detection  of an optical flare.  (813) obtained fundamental
photometric parameters from $uvby$ and H$\beta$ photometry.

 {\bf 98.   [93 Leo]}   (145) claims emission at Ca\,{\sc ii} H and K may not be present at
all but  an artifact  of the composite nature of the spectrum of 93 Leo.  (77)
lists spectral  type A7V/G5III--IVe.   (288)  used individual  $V$-magnitudes  of
$V(A6) =  5.52$ mag and $V(G5) = 5.09$ mag.  (145) gives $(B-V)_{\rm hot} = +0.15$ mag and
$(B-V)_{\rm cool} =  +0.96$ mag.   (77)  lists $v\sin i = 
119/\leq 50$ km\,s$^{-1}$ for the hot/cool
component, respectively.   (145)  obtained $i \approx 52\deg$.   IR excess  
$(J,H,K) =
(0.09,0.22,0.23)$ mag  (349).   (306) lists Dist. = 22 pc.  EW(H$\alpha$) = 
-1249 
m\AA, EW(Li\,{\sc i}6707) =  74$\pm$10 m\AA \ (323), (139)  listed it  with 
$M_V = +1.8$ mag.
(579) present  strong evidence  that the  late-type star  is  an  asynchronous
rotator.  (145) gave $v\sin i$ = 15 km\,s$^{-1}$ for the G-component.

 {\bf 99.   [HD  106225]}   (212) suggested two possible photometric periods 
of 0.91 and 10.6 days, 
and two  possible spectroscopic  periods of 6.851 and 10.389 days. The 10-day  
period is the correct one.
New orbital  elements are  given in the catalog and succeed the ones from the 
first edition!  The velocities show
relatively large  residuals due to starspots (KGS).  (262) lists
$P_{\rm phtm} =  10.8$ days, and derived a giant classification. $UBVRI$
photometry has  been reported  by (580) who finds a visual ``wave'' amplitude of
0.15 mag in 1987 and significant variability of the $V-R$ and $V-I$ colors.  
(848) reports line-profile variability.

{\bf 100.   [HR 4665]}   (18) and (149) give a (single-line) K0III--IV spectral type,
but both  stars are  active (171).  (259) lists $\log L_X = 31.41$ 
erg\,s$^{-1}$.  $F(K) =
2.7\cdot 10^6$ and  $F(H) =  2.3\cdot10^6$ erg\,cm$^{-2}$s$^{-1}$  (309).  (306) gives Dist. = 140 pc
and $M_V  = 0.2$  mag, (44)  gave $M_V = +3.0$. (470) calculated Dist. = 95 pc.
(149) derived K0III/K2IIIab.  Distortion wave migration period is 16 yr (243),
$P_{\rm phtm} =  63.15$ days  (258), $<(V-R)>  = 0.77$  mag (309),  (59) reports further
H$\alpha$ and  H \& K observations.  (21) noted ``strong'' H \& K emission, and gave
K0III/K0III spectral  type and  radii  of 20(:)/20(:)  R$_\odot$  and
masses of  $\geq 1.31/\geq 1.29$ M$_\odot$.   For (U,V,W) see also (44).  
(579) determine a
mean photometric  period of  $63.8\pm0.6$ days  from 3  years of  $V$ data.  (658)
report large IR excess at 12 and 25 $\mu$m.

{\bf 101.  [AS Dra]}   (282) gives a combined absolute magnitude of +4.9 mag.  (444)
measured Ca\,{\sc ii}  H \&  K fluxes  for both components to $F(K) = 5.3/7.4 
\cdot 10^5$ and
$F(H) =  8.2/3.6 \cdot 10^5$ erg\,cm$^{-2}$s$^{-1}$  for the  hot/cool component,  respectively
(mean values  are given).   Eccentric  orbit by  Greenstein, J. L. et al. 
1957
(=531) in  Batten's 8th  Catalog has  been  revised  by  (492)  with  circular
elements.

{\bf 102.  [HD 108102]}   Member of the Coma Berenices cluster (44), (44) also gives
$(U-B)$= 0.0 mag, $(B-V)$= 0.50 mag and $(R-I)$= 0.19 mag.  (444) measured Ca\,{\sc ii} H
\& K  fluxes for both components in the range of $F(K) = 2.9-3.3 \cdot 10^6$ 
and $F(H) 
= 1.9-2.7  \cdot 10^6$  erg\,cm$^{-2}$s$^{-1}$, not  knowing which component is responsible for
the different  peaks!  The given time of conjunction has been derived from the
velocity curve  in reference  (85), but Kraft's [=(85)] zero phase appears not
to fall  at conjunction.   Note  also that the masses given have been computed
from the  orbit given  in (85).   Another  possibility for  $P_{\rm phtm}$ is 1.3 days
(572).   (526) derived  $V(max) =  8.16$ mag.  The star is also in the sample of
(604).

{\bf 103.   [BD+25$^\circ$2511]} (44) mentioned a possible visual amplitude of over 0.1 mag.
H \&  K emission  noted by  (182).  (225) classified it as G8.  For (U,V,W) see
also (44).   (745)  listed twenty  velocities for both components and in (860)
derived a preliminary orbit from altogether 36 observations which is listed in
Table 4.   Errors of the elements are  as  follows:  $e \pm$0.006, $\omega 
\pm$19, $\gamma \pm$ 0.24, $K_1 \pm$0.47, $K_2 \pm$0.53, $a\sin i \pm$0.03, 
and $P_{\rm orb} \pm$0.000054 days.

{\bf 104.   [HD 111487]}     Mg b  absorption lines at 5180 \AA \ appear to show central
emission (608)  [termed ``splitting'' in (608)].  No Ca\,{\sc ii} H and K region spectra
available so  far, but  strong evidence  that the  star  is  chromospherically
active.     X-ray  emission  originally  detected  by  Helfand \& Caillault
[incorrectly referenced  in (608)!].   Preliminary light-curve modeling of the
eclipse gave $k = 0.76$, $r(G) = 0.144$, and $L(G) = 0.89$ (711).

{\bf 105.   [IN Com]}     Central star  in the planetary nebula LT-5.  Triple system
(836).   It is  not clear  whether the system is a SB1 or SB2!  (839) proposed
the system  to be  SB1 with  a low-mass  component and the hot subdwarf as the
third body or, a SB1 with the hot subdwarf as the companion; they pointed out
that their  data do  not confirm  the 1.99-day orbital period of (836) but are
best fitted  with a period of 1.7545$\pm$0.0001 days.  In our Tables 3, 4, and 5
we adopted  the CORAVEL  orbit of  (836) but  state that the situation remains
unclear.  Extensive photometry is presented in (839) for the years 1985-89 and
by (838)  for 1983 [see also Noskova, R. I.: 1989, SvAL 15, 149].  (836) point
out that both components should fill their Roche lobes. Note that the photometric 
period is significantly different from either orbital period!

{\bf 106.   [HD 112859]} We caution that the orbit of  
(882) might be incorrect (P$_{\rm orb}$=1.3086 days, $\gamma$=+12.3, K=92.0, 
e=0.0, asini=1.65). Six recent radial velocity measures by one of us (FCF) 
indicate an inconsistency with the period of 1.3 days. 

{\bf 107.   [UX Com]}    (258) lists only G5III, (62) gave G2/K2IV.  (259) gives 
$\log
L_X =  31.51$ erg\,s$^{-1}$.   (65)  postulated $dM/dt  = 1.4\cdot 10^{-8}  
- 1.1\cdot 10^{-7}$ M$_\odot$yr$^{-1}$,
\vec{B}(dipol) =  579 G,  and $d\ln P/dt  = -2.06\pm0.96  \cdot 10^{-6}$  
yr$^{-1}$.   (110) gives
masses of  1/1.1 M$_\odot$ for the hot/cool component respectively.  (444) measured
Ca\,{\sc ii} H  \& K  fluxes: $F(K)  = 0.96-1.32  \cdot 10^7$  and  $F(H)  =  
1.0-1.2  \cdot  10^7$ erg\,cm$^{-2}$s$^{-1}$.

{\bf 108.  [HD 113816]}   $\gamma$ and $K$ are estimated from 15 individual radial velocity
measurements given in (484).   $E(B-V) \leq$  0.03 (484),  $F_{H1}+F_{K1} =  
1.39\cdot 10^7$ erg\,cm$^{-2}$s$^{-1}$, activity parameter $\log R_{HK}$ = 
-3.17 (484).
The $v\sin i$ of 30 km\,s$^{-1}$ of (484) seems to be too large, (FCF) measured 
6$\pm$2 km\,s$^{-1}$ which is listed. 

{\bf 109.   [RS CVn]}     Prototype of  RS CVn  systems!   (259) gives spectral type
F4III/K0IV and $\log L_X = 31.27$ erg\,s$^{-1}$, (347) gives $L_X = 62\pm30 
\cdot 10^{30}$ erg\,s$^{-1}$.
(108) derived  radii R$_{\rm hot} = 1.7:$, and R$_{\rm cool} = 4.0:$ R$_\odot$.  (257) lists
Dist. =  145 pc,  (259) 150  pc, and  (245) Dist.  =  22  pc.    (65)
postulated  $dM/dt = 4.3-7.8 \cdot 10^{-10}$ M$_\odot$yr$^{-1}$,  
\vec{B}(dipol) = 156 G,  and $d\ln P/dt = 
-3.17\pm0.48 \cdot 10^{-7}$ yr$^{-1}$.  (38) gives $i = 87.0\pm0.2 \deg$.   
$F(K) = 1.2\cdot 10^6$,
and $F(H)  = 9.7 \cdot 10^5$ erg\,cm$^{-2}$s$^{-1}$ (309), (444) derived 
$F(K) = 1.4-2.25 \cdot 10^6$,
and $F(H)  = 1.4-2.5  \cdot 10^6$  erg\,cm$^{-2}$s$^{-1}$.  Frequent 
non-periodic period changes 
(36,356) a.o.. Strong H \& K maximum at wave minimum (96), IR-colors 
$(K-L) = 0.0$ mag,  $(K-M) =  0.0$ mag,  and $(K-N) > 0.1$ mag (251).  
Mean $(B-V)$= 0.59 mag
(44).  (28) gives a distortion wave migration period of 10.2 yr, see also 
(60), (355) and (356) and references therein.  The photometric period given in
the catalog has been computed with the migration period of 9.48 yr obtained by
(355), (642)  obtained 9.4 yr in close agreement with (355).  Polarization has
been measured  by (104).   (590)  derived spectral  types  of  F6IV+G8IV  from
spectrum synthesis of red and blue spectra.

{\bf 110.   [HR 4980]}     The BSC (=77) notes a companion 3.2 mag fainter and 25.3"
distant.   (697) estimate  an age  of 2  Gyr from  the Li-age  calibration  of
Soderblom.   Both spectroscopic components show moderately strong 
Li\,{\sc i}6707, and
the strongest yet measured He\,{\sc i}D3 absorption for any dwarf star (697).  Shallow
NaD line  cores is  further evidence  for chromospheric emissions (697) yet no
Ca\,{\sc ii} H  and K observations are available to date.  Possible eclipses (697) but
not confirmed so far.

 {\bf 111.   [BL CVn]}   (551) obtained $P_{\rm phtm} = 9.31\pm0.06$ days and attributed the
light variations  to the  ellipticity effect ($P_{\rm orb} = 18.69$) but not sure (see
496).   IUE observations in (496).  $V\sin i = 7/35$ km\,s$^{-1}$, which 
suggests that the 
cooler component  is chromospherically  active (262).  The light variations of
$\approx$\,0.16 mag  are mostly  due to  the ellipticity  effect (551,582).  (588) noted
that their Ca\,{\sc ii} H and K spectra for the cool component are likely contaminated
by the continuum of the hotter component.

{\bf 112.  [HD 116204]}   Quasi-sinusoidal light curve with P = 21.7 days and 
$\Delta V 
= 0.06$  mag (229).   (262)  estimates KIII spectral type from the $(B-V)$ color.
(595)  report  $BV$  photometry  from  1983-84  through  1986-87  and  derive  a
photometric period of 21.9$\pm$0.2 days from their 1987.14 light curve.

{\bf 113.  [HD 116378]}   Faint companion [= AGK3 +36$^\circ$1200, also G5? 
(see 729)] about 
35" away  from the spectroscopic pair (729, 712), 1.5 mag fainter.  The Ca\,{\sc ii} H
and K  emission lines  are very  weak but  the  absolute  surface  fluxes  are
moderately high [$\log F'(K,H) = (6.32,6.28)$ erg\,cm$^{-2}$s$^{-1}$ (588)].

{\bf 114.  [HR 5110]}   $\Delta V = 0.010$ mag due to reflection effect (77, 66, 19), no
wave amplitude  is seen.   (37) gives $i = 13 \deg$.  (259) lists $\log L_X 
= 31.11$ 
erg\,s$^{-1}$.   IR excess  $(J,H,K) = (0.01,0.08,0.07)$ mag (349).  (306) lists Dist. =
39  pc  and  $M_V  =  1.9$  mag.    Secondary  fills  Roche  lobe,  semidetached
configuration.   $<(U-B)>$ =  0.06 mag  (77), $<(B-V)>$ = 0.39 mag (37), $<(R-I)>$ =
0.30 mag  (77), (37)  gives individual colors for the hot/cool star of $(V-I)$=
1.36/1.91 mag  and $(B-V)$ = 0.34/1.36  mag, respectively.   (149) listed it as
SB1, (37) noted also SB1 but assumed that the Ca\,{\sc ii} emission is from the second
component.   For (U,V,W)  see also  (44).   (37) derived  $V(max) =  4.95$  mag,
another measure  by (643)  gave 4.91  mag.   SB1 orbit  with CORAVEL in (492).
(804) report  a possible  modulation of  the  X-ray  light  curve  from  ROSAT
observations.

{\bf 115.   [HD 118238]}     Another possibility is $P_{\rm phtm}$ = 22.94 days (283), (283)
also gives  $<(V-I)>_{KC}$ =  1.32 mag.   (173) classifies it as K2III.  
$T_{\rm conj}$ in Table 4 has been computed from the orbit in (727).
(856) lists $L_X = 6.166\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 116.   [HD 119285]}     Another possibility is $P_{\rm phtm} = 12.35$ days (283), (283)
also gives  $<(V-I)>_{KC}$ =  1.24 mag.  (79) classifies it as K1Vp.  (697) report
$uvby$ photometry  and found  $P_{\rm phtm} = 12.12\pm0.18$ days and 
$\Delta y = 0.06$ mag,
and gives a time of maximum light at HJD 2444767.71.  (697) also noted a flare
in $u$  and $v$.   Radial-tangential  macroturbulence was  determined to 3.0$\pm$0.5
km\,s$^{-1}$ (697).  EW(He\,{\sc i} D3) = 29$\pm$8 m\AA \, EW(Li\,{\sc i} 6707) = 63$\pm$4 
m\AA \ (697).  From TiO
bandhead depression  (697) estimate a spot coverage of 18-37 \% of the stellar
surface.  Earlier orbit by (727) is very similar to that given in Table 4.

{\bf 117.   [BH Vir]}   (148) derived masses and radii of 0.9/0.9 M$_\odot$ and 1.12/1.16
R$_\odot$,  respectively.  Earlier work by Wilson \& Rafert [1980, A\&AS 42,
195] gave  masses of  1.10/0.95  and  radii  of  1.25/1.05  for  the  hot/cool
component, respectively.  The adopted masses in Table 5 are a weighted mean of
the masses  listed in (634) which are in agreement with the mass ratio of 
1.02
from (1).   See  also (636)  for absolute dimensions.  Extensive photometry is
reported by (78).  1989-$UBV$ photometry in (695).

{\bf 118.   [HD 127535]}   (384) reports a filled-in H$\alpha$ line.  (483) reported a
wave amplitude  of 0.06 mag in 1980-81.  H$\beta$, H$\gamma$, H$\delta$ are reported
to be  also ``filled-in'' (79).   (164) were  the first to determine the rotation
period of  5.97 days.   See  also (625).   (580)  report $UBVRI$ photometry from
February 1987  showing a  $V$ amplitude  of 0.10 mag and significant $V-R$ 
and $V-I$ color variations in phase with $V$.

{\bf 119.   [RV Lib]}    (257) also gives Dist. = 270 pc, (259) Dist. = 276 pc.  For
(U,V,W) see  also (44).   High-resolution Ca\,{\sc ii} H and K observations (620) show
both stars  to be  emission-line objects.   (620)  concluded that the hot star
(G5) is the more active.  $V\sin i$ measure of (628) has been updated and a better
value is given in Table 3.  Semidetached according to (875).

{\bf 120.   [HR 5553]}    Orbit of (731) agrees well with the one listed in Table 4.
(740) list the star as K1V.  Ca\,{\sc ii} emission also noted by (747).  Member of the
Hyades moving group (77), noted as ``VAR?'' in (77).  (739) obtained $V$ = 6.00 mag.
(841) found no lines of the secondary at red wavelengths.

{\bf 121.   [SS Boo]}    (258) classified it as G8Ve/G8Ve.  (259) and (247) give 
$\log L_X =  30.80$ erg\,s$^{-1}$.   (65) postulated $dM/dt = 8.2\cdot 10^{-8} - 
3.7\cdot 10^{-7}$ M$_\odot$yr$^{-1}$, no
\vec{B}, and  $d\ln P/dt =  +2.16\pm1.38\cdot 10^{-7}$ yr$^{-1}$.   (252)  gives  time  of  primary
eclipse JD 2420707.369.   (293)  obtained a  differential rotation  rate  of
$1.5\cdot 10^{-9}$ rad\,s$^{-1}$\,$\deg^{-1}$  for the  K1-star and a cycle period of 7-8 yr.  Migration
wave periods  derived are:  7.5, 9.3,  and 6.4  yr [see  (61)  and  references
therein, see  also (293)].   A  detailed spectroscopic  study is  presented by
(627) who  also found  double H$\beta$  emission.   Note that  the chromospheric
emission of  the G  dwarf component is fairly weak at H\&K but well established
in the  IR-triplet (627).   However,  (620) found  only one emission component
from 0.1  \AA/px spectra.   (627)  also observed  an   excess Balmer  absorption
feature near  primary eclipse  (but  not  at  secondary  eclipse)  which  they
interpret arising  from some  obscuring material  associated with the subgiant
component.   

{\bf 122.   [HD 136901]}     (229) estimated a G5 spectral type.  (366) give a K1III
classification.   See also (262).  The earlier photometric period of 9.63 days
and $\Delta V$  = 0.16 mag by (229) was actually due to the ellipticity effect and
thus 1/2  the true period, see (579).  Primary component is very close to 
filling 
its Roche  lobe and  the two  minima of  the ellipticity effect are unequal by
0.08 mag  in $V$  (582).   (581) found no evidence for a hot secondary component
from IUE  spectra and  estimate the  mass of the giant primary in the range of
2.5 -  4 M$_\odot$.  (582) determined the orbital period independently from
the ellipticity effect: 18.6685$\pm$0.0015 days.

{\bf 123.   [GX Lib]}   (25) gives spectral type K0III-IV.  (255) lists $e = 
0.017\pm 
0.010$, $(V-R)= 0.75$ mag and an only weakly active, ``strong'' absorption H$\alpha$
profile with  EW =  1.38 \AA.   (255)  also mentioned  that the  K1-star fills a
substantial fraction  of its  Roche lobe.   (306)  lists Dist. = 120 pc.  (25)
noted two  possible orbital  periods; a  more likely one with 11.12 days which
turned out to be the correct one.  (146) found  5.586 days for the photometric
period but  (262) confirmed the orbital period to be 11.133 days, so the light
curve should  be double  ``humped''.   (727) gives  an orbit with $e = 
0.06\pm0.03$.
Note the  high space  velocity.  (579) arrive at the conclusion that both, the
ellipticity effect  and a  spot wave, cause the light variations.  The star is
in the X-ray sample of (604).

{\bf 124.   [HD 137164]}     Another possibility is $P_{\rm phtm}$ = 44.18 days (283), (283)
also gives $<(V-I)>_{KC}$ = 1.11  mag.  Note that the orbit given in the tables of
(727) seems  to be  wrong, although the radial velocity plot in (727) includes
the correct  orbit!   The elements given in the catalog are provided by one of
the authors of (283).  Very eccentric orbit!

{\bf 125.   [UZ Lib]}     Not an FK Com star as originally suggested by (450) 
but an RS CVn system, see (269).  Mass-ratio of  4:1 (269),  $v\sin i$ = 90 
km\,s$^{-1}$ (450), (455) reports IR excess ``which is
attributable to  a  third  light''  and  gives  $J-K= 0.78$  mag.    (269)
tentatively suggested a dM companion but (613) showed that 
$T_{\rm sec} \approx 8000$ K from IUE observations.  
(597) lists $L_X = 10.7\cdot 10^{31}$ erg\,s$^{-1}$.  
$UBV$ photometry by (759) had a maximum wave amplitude
of  0.25 mag in 1989 and 0.15 mag in 1988.

{\bf 126.   [RT CrB]}     (259) gives $\log L_X = 30.74$ erg\,s$^{-1}$.  
(112) lists $<V>$ = 10.2
mag and  (109) estimated G0/G8 spectral type.  (202) found no photometric spot
wave in  1979 and  1981, nor  did (111)  in 1973.   (620)  found Ca\,{\sc ii}  H and K
emission lines  from both  components with  the stronger emission belonging to
the cool component.

{\bf 127.   [HD 141690]}    (614) found no photometric period from a total magnitude
range of  0.082 mag in $V$.  No orbit is published to date but (366) observed
a range of velocities of $\approx$\,40 km\,s$^{-1}$ which proves it is a binary.

{\bf 128.   [1E1548.7+1125]}    No H$\alpha$ emission observed, ratio 
$(F_{\rm em}/F_{\rm abs})$ for
Ca\,{\sc ii} H \& K  = 0.44,  $\log (F_X/F_V)  = 1.3$  where 
$F_X = 9.04\cdot 10^{-13}$ erg\,cm$^{-2}$s$^{-1}$ (267).  See also (344).

{\bf 129.  [RS UMi]}   (259) gives $\log L_X = 30.95$ erg\,s$^{-1}$.  (65) 
postulated $d\ln P/dt = +1.46\pm2.96 \cdot 10^{-6}$ yr$^{-1}$.

{\bf 130.   [HD 143313]}    See (271) and (146).  (417) pointed out that this may be
an eclipsing  binary and  gave predicted times of minimum light. Photometry by
(271), however,  reveals no  clear signs  of eclipses,  so  we  adopted  ``non-
eclipsing'' in the catalog.

{\bf 131.  [HD 144515a]}   The star is a quadruple system (two SB's designated A and
B) plus  a possible  additional component  (492) [B:  also SB1 with 
$P_{\rm orb} = 11$
days].   Old orbit  from Sanford  (=713) is  listed in  Batten's  8th  catalog
(=712).   Ca\,{\sc ii} emission  found by  (624).   Time of  light  curve  minimum  at
2446272.64 (614).   (614)  present photometry made between 1985 and 1988.  
$\log F'(H,K) = (6.3,6.4)$ erg\,cm$^{-2}$s$^{-1}$ (KGS).

{\bf 132.   [$\sigma^2$ CrB]}    Is the brighter component of the visual binary ADS 9979
[sep. 6.6"].   (120)  suggests that  one component  of the SB2 system may have
$\delta$ Scuti  type variability  with $P  = 0.1$  days  and  $\Delta V$  =  0.05  mag.
However, the  spectral types  are too  late for  such variability  and  it  is
unconfirmed.   From (120), (77) noted one component to be a $\delta$ Scuti star
(?), and  (258) mentions the same amplitude and P $\approx$ 0.1 days. (Obviously  
an error promulgated through the literature). (194) gives for
TZ CrB  $i \approx 28 \deg$.  Activity parameter $\log R$ = +0.77 (318).  
$F(K) = 1.0\cdot 10^7$,
and $F(H)  = 1.0\cdot 10^7$  erg\,cm$^{-2}$s$^{-1}$ (171).   (444) also 
measured Ca\,{\sc ii} H \& K fluxes for 
both components.   (3)  and (32)  report a detection at soft X-rays, and (177)
noted ``coronal  line-emission'', EXOSAT observations in (661).  (122) 
mentioned it as 
a ``variable  radio source''; (62) listed a spectral type F6-8V/?, (125) gives a
similar orbit,  and derived  masses and radii of 1.064/0.94 and 0.8/0.76 solar
units, for the hot/cool component, respectively.  Note that the given spectral
type for the hotter component is from (458).  (194) found evidence of a 3.5 yr
periodicity of  the mean  $V$ magnitude, (579) found a 2.0 yr period.  The given
photometric period differs by 2.5 \% from the orbital period.

{\bf 133.  [GU Her]}   (702) lists it as a detached F8 main-sequence star.

{\bf 134.   [CM Dra]}     Other names: ``LP101-15'' and ``G225-67''.  For wave-amplitude
see Fig.  4 in  (395).   Depth of  the eclipse in $V$ is $\approx$0.03-0.05 mag with 1.5
hour duration  (395).  Note that (395) derived $P_{\rm orb}$ = 0.63430 days 
and a time
of primary eclipse at JD 244 1855.75425.  (654) verifies the orbital period of
1.268 days.  $U$-band flares of up to 1.1 mag (654). (856) also lists $L_X = 
0.003\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 135.   [HD 149414]}    Not a short-period binary!  Note the high systemic velocity and
large orbital eccentricity (717).  Metallicity $[M/H] = -1.4$ (717) from CORAVEL
dips, $\log T_{\rm eff} = 3.708-3.737$ K.

{\bf 136.   [WW Dra]}   A-component of the visual binary ADS 10152 (357).  
$(B-V)_{\rm hot}$
= 0.65 mag and $(B-V)_{\rm cool}$ = 0.97 mag  (44). (108) gives 
$(B-V)_{\rm secondary}$ [=
$(B-V)_{\rm cool}$] = +1.0 mag.   (259)  gives $\log L_X = 30.84$ erg\,s$^{-1}$.  (65) postulated
$dM/dt =  9.2 \cdot  10^{-11} -  3.6\cdot 10^{-10}$ M$_\odot$yr$^{-1}$,  
\vec{B}(dipol) = 106 G, and  $d\ln P/dt =
-1.70\pm0.55 \cdot 10^{-7}$ yr$^{-1}$.   $F(K) = 2.2\cdot 10^6$ and $F(H) = 
1.6\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$
(309).   (109) gives  G2/K0, (149) G2IV/G8IV.  (282) listed it with $M_V$ = +2.6
mag.  For (U,V,W) see also (44).

{\bf 137.   [$\epsilon$ UMi]}    A-component of the visual binary ADS 10242 (357).  The
$V(max)$ value  in Table 2 is the combined magnitude from both components!  (77)
gives $\pi$ = 0.010".  (328) gives radial-tangential macroturbulence of 9.2$\pm$1.6
km\,s$^{-1}$ and  concluded that  $\epsilon$ UMi  is undergoing rapid rotational braking.
(291) found that the eclipse is grazing-total, eclipse duration is less than 2
days with  $V$-depth (primary  eclipse) = 0.04 mag and (secondary eclipse) = 
0.02 mag, respectively.

{\bf 138.  [HD 152178]}   Note the significant difference between the orbital period
and the  photometric period.  Ca\,{\sc ii} emission already noted by (465).  A time of
light minimum  would be  2446605.5 (614).  (465) gives G8-K0 Vp but a spectrum
by one  of us (FCF) of the 6430 \AA \ region indicates that the star is definitely
a giant.

{\bf 139.   [V792 Her]}    (13) obtained $V(max) = 8.50$ mag and also derives radii of
2.8/9.5 R$_\odot$ for the hot/cool component, respectively [see also (210)],
(264) mentioned  variable H  \& K emission and a missing H$\alpha$ line in July
1980.   (262) listed  it as  F/KIII and  reported moderate H$\alpha$ absorption,
(210) found  F/G8IV.  (262) also derived minimum radii of 3/11 R$_\odot$ for
the F  and the  K-star, respectively.  (264) obtained Ca\,{\sc ii} H \& K 
fluxes of  $\approx 7\cdot 10^7$ erg\,cm$^{-2}$s$^{-1}$.  (13) measured 
$\Delta V_{\rm wave}$ in 1982 of 0.09 mag.
(500)  gives  individual  $V$-magnitudes  of  9.73/8.48  mag  for  the  hot/cool
component, respectively.

{\bf 140.   [HD 155989]}   (614) found three (different) photometric periods 
for three different
data sets  all significantly  different from  the orbital  period of  122 days
[$P_{\rm phtm}$ =  39, 37, and 30 days, respectively]!  None of them, however, appears
convincing.   Ca\,{\sc ii} observations  give $\log  F'(H,K) =  (5.92, 6.02)$   
erg\,cm$^{-2}$s$^{-1}$ (KGS).

{\bf 141.   [HD 155555]}     (163) found  $P_{\rm phtm}$ = 1.66 days (accurate to 
7\%), (384)
derived $<(B-V)>$  = 0.767  mag and  (283) lists  $<(V-I)>_{KC}$ =  0.89 mag.    For
(U,V,W) see also (44).  Further $UBV$ photometry has been reported by (580) with
$\Delta V$ = 0.075 mag in 1987.  (645) questions the active-chromosphere character
of HD  155555 but Fig. 2 of (844) shows strong Ca\,{\sc ii} H and K emission.  Earlier
orbit by (10) is in agreement with the improved orbit in Table 4.

{\bf 142.   [HR 6469]}   Is a spectroscopic triple system [resolved by McAlister, H.
A. et  al.: 1984,  ApJS 54, 251].  The active component in HR 6469 is
the third  [G5IV] star, and not one of the components of the closer pair as is
usually the case.  The close pair is the eclipsing system, but the G5IV and F-
stars are  non-eclipsing, see (205).  The orbital period for the close pair is
2.23 days  (205).   The listed  photometric period is most likely the rotation
period of  the active  G5IV star.   (205) also derived $P_{\rm orb}$ = 2.2299 days for
the close  pair and  a time  of primary  minimum at JD 244 5839.813.  The long
orbit is  given in  the catalog.    $F(K)  =  4.2\cdot 10^6$  and  $F(H)  =  
3.4\cdot 10^6$ 
erg\,cm$^{-2}$s$^{-1}$ (171).   (306)  estimates a  distance of  22 pc  which is certainly
wrong.   EW(H$\alpha$) = -1360 m\AA \, EW(Li\,{\sc i} 6707) = 60$\pm$15 m\AA \ (323).  (205) noted
F7V spectral type for the hotter star.  (643) obtained $V(max) = 5.55$ mag.  The
depth of  primary and  secondary eclipse  are 0.12  mag and  0.08  mag in  $V$,
respectively (579) [see also front cover of IAPPP Comm. 29].

{\bf 143.   [HD 158393]}    Another possibility is $P_{\rm phtm}$ = 30.77 
days (283).  $JHKL$ 
photometry is  reported by (406).  (406) also suggest $E(B-V)$= 0.15 mag, (283)
gives $<(V-I)>_{KC}$  = 1.23  mag.  K-star nearly fills its Roche lobe (406).  See
also (614).

{\bf 144.   [29 Dra]}    (No HR number!)  White dwarf as hot component (185).  H \& K
emission similar  to that  of II  Peg.   H$\alpha$ line is variable (185).  
(306) listed
Dist. =  180 pc.   (262)  gives a  K2III classification  for the cool star and
noted a  weak H$\alpha$  absorption line.   A  time of  minimum light  is JD 244
4445.0 (184).  (579) present several years of $UBV$ photometry and derive 
$P_{\rm phtm}$
= 28.8  days and  $\Delta V$ = 0.105 mag in 1985.  There is a significant increase
of the mean light level from 1984 through 1987 of 0.2 mag.

{\bf 145.   [HR 6626]}     Primary (=A) of ADS 10782ABC [B: F7V, $V$ = 9.70 mag, 
$B-V$ =
0.75 (722), $v\sin i$ = 11.7 km\,s$^{-1}$ (721), 8" away; C: 70" away from 
A (77)].  (721)
noted a physical connection between the spectroscopic pair and the B component
which would  make HR 6626 a triple system.  The Ca\,{\sc ii} emission is just 
somewhat stronger as  compared to  an inactive  K3 giant, but HR 6626 
might have an (unseen) early-type spectroscopic 
companion which dilutes  the emission.   Fluxes for the A pair are $\log
F'(H,K) =  (5.42,5.53)$ erg\,cm$^{-2}$s$^{-1}$  (KGS).   (407) discovered  the  photometric
variability of  0.03 mag in $V$ and found $P_{\rm phtm}$ = 53.5$\pm$2.4 days.  
(579) found
$P_{\rm phtm}$ =  49.66$\pm$0.04 days,  i.e., 1/2 the orbital period, and concluded that
the star  is an  ellipsoidal variable  with a  small reflection  effect 
($\Delta V$  = 0.011$\pm$0.003 mag).   However, (582) argue that there is no 
reflection effect.
Abnormal scatter in the $V$ light curve suggest weak starspot activity (579).

{\bf 146.   [HD 163621]}   SAO catalog (=409) lists $V$ = 7.3 mag.  (590) found a mass
ratio of 1.47 (cool/hot) from radial velocity amplitudes.  They also concluded
that the  star is  either slightly  metal poor  or metal  rich and  earlier in
spectral type.   But  (793) examined  his spectra and classified it as K0V and
found no  evidence for  the G6V  star at  blue wavelengths suggesting that the
weaker lined  star is  cooler rather than hotter.  The wave amplitude given by
(DSH) is the largest one produced by five spots found to exist during a 3-year
interval, whose rotation periods were within 2\% of the orbital period.
(856) lists $L_X = 1.445\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 147.   [Z Her]}    Is a Hyades member (44, 222).  (61) [and (470)] gave Dist. =
85 pc.   (149)  gives G0IV/G5IV.  (62) lists for the wave amplitude 
$\Delta V$ =
0.02-0.03 mag.   The  H$\alpha$ emission  occurs only during flares (222).  (65)
postulated $dM/dt = 2.3\cdot 10^{-12}  - 3.0\cdot 10^{-11}$ M$_\odot$yr$^{-1}$, \vec{B}(dipol)  =  71  G,  and
$d\ln P/dt =  -2.84\pm1.59 \cdot  10^{-8}$ yr$^{-1}$.   Strongest  H$\alpha$ 
emission  at wave
minimum (133).   Masses  and radii  also in (168).  IR colors $(K-L) = 0.0$ mag,
$(K-M) = -0.1$ mag, and $(K-N) = 0.0$ mag (251).  Distortion wave migration period
is 1.4  yr retrograde  (46) and  this  value  has  been  used  to  derive  the
photometric period  given in  the catalog.   Not  detected at X-rays by (130),
(444) observed  Ca\,{\sc ii} H  \& K  fluxes: $F(K)  = 3.6-5 \cdot 10^5$ and 
$F(H) = 2.9-5.4 \cdot
10^5$ erg\,cm$^{-2}$s$^{-1}$.   For  (U,V,W) see also (222).  (579) found $P_{\rm phtm}$ = 3.970$\pm$
0.007 days  and $\Delta V = 0.035\pm0.003$  mag in  1985.  (609) found no orbital
period variations.

{\bf 148.  [MM Her]}   (44) adopted G8IV/G8IV.  (259) gives $\log L_X = 30.76$ erg\,s$^{-1}$ in
accordance with  (129).   (249) reports  X-ray emission  of $0.36\cdot 
10^{31}$  erg\,s$^{-1}$.
(258) lists $<V>$ = 9.45 mag.  (121) gives $V$ amplitude (eclipse) = 0.94-0.99 mag
and $i = 86.35\pm0.09 \deg$.  (65) postulated $dM/dt = 0-5.9 \cdot 10^{-9}$ 
M$_\odot$yr$^{-1}$, no \vec{B},
and $d\ln P/dt  = -1.40\pm2.03\cdot 10^{-7}$  yr$^{-1}$.   IR color  $(K-L) 
=  0.0$ mag  (251).
Distortion wave  period is  7.5 yr  accelerating (121).   For (U,V,W) see also
(44).    (610)  derived  slightly  different  radial  velocity  amplitudes  
of (hot/cool) $74.0/70.5$ km\,s$^{-1}$ and a systemic velocity of $-51.5$ 
km\,s$^{-1}$.

{\bf 149.   [V772 Her]}     Triple system.   Visual  binary ADS 11060AB!  ``A'' is the
short-period eclipsing  binary [B-comp.:  G5V, $v\sin i$  =  18 km\,s$^{-1}$].    
The  B-component is  seen in  the spectrum  [$P_{\rm orb}(A,B) =  
20.25$ yr, see (532)].  The
spectroscopic binary  is single lined.  (873) show that eclipse timings of the
A-component trace  the light  travel time effect expected by the 20.25-year AB
orbit.   All three components lie on or near the  main sequence (266).   
$\gamma$ =
-19.9 km\,s$^{-1}$, $e$ =  0.045, $T_0$  at JD  244 1032.24 $\pm$ 0.04  
days (336).  (42) 
obtained $V(max)  = 7.02$  mag.   (479,873) presented  further photometry:  they
derived a  time of  conjunction and  found that  the light  variations outside
eclipse are partially due to the ellipticity effect.  (457) and (873) observed
no secondary  eclipses, depth of primary eclipse is $\approx$\,0.05 mag in $V$.  Flares in
the $U$-bandpass  [see also  (457) and  references therein].   The  maximum wave
amplitudes in  Table 4  in (579)  are misprints  and should  read 0.038 mag in
1984, 0.027  mag in  1985, and  0.04 in 1986.  The visual amplitude due to the
ellipticity effect  is around 0.02 mag (579,873).  (197) list a minimum radius
for the  G0 component  of 0.93 R$_\odot$.  (620) obtained a series of Ca\,{\sc ii} H
and K  spectra with  variable emission  strengths.   (591) and (812) [see also
Stern, R. A.: 1992, in ``Frontiers of X-ray Astronomy'', 28th Yamada Conf.] report
the detection  of significant  X-ray light-curve variability and (804) noted 
three 
X-ray flares  within two  days detected  by ROSAT.  Stroemgren $uvby$ and H$\beta$
photometry in (811).  Ca\,{\sc ii} H and K line monitoring by (811) show varying H and
K emission line strengths.

{\bf 150.   [HD 165590C]}     C-component of  the multiple system ADS 11060.  
The A 
component is  the well  known ``active''  binary V772  Her.   Separation A-C  is
28.2".   $m-M$ =  2.5 mag  [$\approx$ 32  pc].   The given  proper motions and space
motions are adopted as the same as for the close pair ADS 11060AB.

{\bf 151.   [HD 165141]} The  chromospherically  active  star  HD  165141   
is classified as  a G8III  and marginal  Barium star  (173) and is listed as 
having a
constant velocity  by Balona, 1987 (=727).   A  recent  spectroscopic
observation of this star with the IUE-satellite by one of us (FCF) shows a hot
white-dwarf  companion.   An examination  of the  radial velocities  listed by
Balona suggests  a low-amplitude  long-term variation  consistent  with  other
Barium stars  which is  confirmed by  recent observations of one of us 
(FCF).  The listed   
period of $\approx$ 5200 days is a rough estimate and has an uncertainty of 
about 500 days. Another
possibility for  $P_{\rm phtm}$ is 33.64 days (283).  (501) classifies it as G8-K0III-
IIp and reports H \& K emission.  $V\sin i$ measure of (727) has been updated and a
better value is given in Table 3.

{\bf 152.   [V815 Her]}     (262) called  it an  early-type BY Dra binary.  Activity
parameter $\log R$ = +0.87 (318).  $F(K) = 5.8\cdot 10^6$ and $F(H) = 
6.2\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$
(171), (444)  measured $F(K)  = 4.1-4.6  \cdot 10^6$  and  $F(H)  =  3.8-4.6  
\cdot  10^6$ 
erg\,cm$^{-2}$s$^{-1}$.    (624)  obtained  Ca\,{\sc ii}  H  and  K  
line-core  flux  of  $6.1\cdot 10^6$
erg\,cm$^{-2}$s$^{-1}$.   (262) gives  minimum radius  for the  G5 star  of 
1 $R_\odot$.  For
(U,V,W) see also (44).  (369) derived $P_{\rm phtm}$ = 1.8 days and (62) 
listed $\Delta V$ 
= 0.10  mag.   (804) report  possible rotational modulation of the X-ray light
curve from ROSAT observations.

{\bf 153.   [PW Her]}     (108)   classified it  as G0/?, (258) lists K0V-IV.  (259)
gives $\log L_X = 31.01$ erg\,s$^{-1}$.  (65) lists $d\ln P/dt = 
-4.92\pm6.70 \cdot 10^{-7}$ yr$^{-1}$.
(110)  listed  minimum  masses  of  1.4/1.6  M$_\odot$  for  the  hot/cool
component, respectively.   Light  curve in  (111).  (611) found differences of
epochs determined from radial velocities and photometry.

{\bf 154.  [HDE 319139]}   Intermediate object between the pre-main sequence 
T Tauri
stars and  the main-sequence flare  and spotted stars (281).  Flares in the 
$U$ 
band (449), (458).  EW(H$\alpha$) = 100 \AA (!) and is correlated with photometric
phase (281).   Most  luminous flare  star for  which there  is  an  individual
measure of  flare incidence  (449).   $V$ =  10.2 mag  in the  Cape Photographic
Durchmusterung.

{\bf 155.   [AW Her]}   (258) lists it as G0/K2.  (109): G0/K1.  (259) gives 
$\log L_X  
= 30.94$  erg\,s$^{-1}$.   (65) lists  $d\ln P/dt =  -0.70\pm1.27 \cdot  
10^{-6}$ yr$^{-1}$.    (813)
obtained fundamental photometric parameters from $uvby$ and H$\beta$ photometry.

{\bf 156.   [BY  Dra]}      Prototype  of  BY  Dra  systems!    Linear  polarization
observations can  be found  in (397).   Zeeman-observations  are  reported  in
(398), Ca\,{\sc ii}  emission is variable (346), $F(H) = F(K) = 3.8\cdot 
10^5$ and $F(H\epsilon) = 
7.8\cdot 10^4$ erg\,cm$^{-2}$s$^{-1}$  (171).   Long term variations in $V$ 
with a period of 50-60 
yr (402).  First orbit  by (400),  another orbit determination can be found in
(401).   The listed mass for the secondary is taken from (400).  Note the high
eccentricity!   Most of  the observers  use spectral  type dM0e/dMe [see e.g. 
(401)] but  the given  classification is  better.   H$\alpha$ emission is 
variable
(651).   EINSTEIN source  with $\log L_X =  29.5$ (593).  (422) lists $L_X = 
0.051\cdot 10^{31}$ erg\,s$^{-1}$.  
(818) lists 
$R-I$ = 0.55 mag. (411)  showed  that  the  rotation,  defined  by  the  
starspots,  is pseudosynchronous.

{\bf 157.   [1E1848+3305]}    No  Ca\,{\sc ii} H and K observations but emission at the Ca\,{\sc ii}
infrared triplet (IRT) and at H$\alpha$ suggest H and K emission.

{\bf 158.   [1E1848+3325]}    No  Ca\,{\sc ii} H and K observations but emission at the Ca\,{\sc ii}
infrared triplet (IRT) and at H$\alpha$ suggest H and K emission.

{\bf 159.   [o Dra]}     A-component of  the visual  binary ADS  11799. 
[ADS
11799B: K3IIIp,  $v\sin i \leq$ 54 km\,s$^{-1}$.]  The $V(max)$ value in 
Table 2 includes both 
visual components.   (306)  gives $M_V$  = -0.9  mag.   (77) lists spectral type
G9III and  parallax of 0.006".  (245) lists a parallax of 0.003$\pm$0.005" [$\approx$ 333
pc].   Eccentric orbit!  The given minimum radius has been computed from $v\sin i$
and $P_{\rm phtm}$  = 143  days (579).   (658)  report large  IR excess  at 
12  and 25
$\mu$m.   $V\sin i$ measure of (448) has been updated and a better value is given
in Table 3.

{\bf 160.  [V1285 Aql]}   Other name ``AC +08$^\circ$142-393''.  
The photometric period of 12
days of  (709) is  highly uncertain.   The  listed photometric  period is  the
rotation period  from Mg\,{\sc ii}  flux variations  [$P_{\rm rot} =  2.9\pm0.7$ 
days  (705)].
Note the large difference from the orbital period (10.3 days).  (696) lists an
absolute parallax  of 0.089".  Flare monitoring by (819).  (804)
reports a X-ray flare from ROSAT data. (862) lists $L_X = 0.008\cdot 
10^{31}$ erg\,s$^{-1}$.  

{\bf 161.   [V775 Her]}     See (271) and (146).  (262) gives dK1 classification and
derived a  minimum radius  for the K1 dwarf of 0.9 R$_\odot$, (81) suggested 
that it
may undergo  partial eclipses.  (73) called it ``a new RS CVn variable'' but the
spectral type  is that  of a BY Dra binary.  For (U,V,W) see also (44).  (650)
obtained several  years of  photometry and  found $V(max)  = 7.80$  mag in 1985,
i.e., 0.2  mag brighter than the years before and after.  (624)  measured Ca\,{\sc ii}
H and  K line-core  flux density of $4.1\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$.  
No eclipses detected by (621). (856) lists $L_X = 0.17\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 162.   [V478 Lyr]}    Early-type BY Dra binary (262).  (74) called it ``a new RS
CVn variable''.   (258)  lists a  time of photometric minimum at JD 244 4506.76
and $\Delta V$  = 0.033 mag.  (306) gives $\gamma$ = +9 km\,s$^{-1}$.  
(74) gives spectral type 
G6V and  notes ``strong''  H \&  K emission from the hot component.  (44) derived
(U,V,W) components with $\gamma$ = 0: km\,s$^{-1}$!  (845) derived a secondary mass of $\approx$0.3
M$_\odot$  with an  assumed mass  for the  primary of 0.9 M$_\odot$.  (74) found
$P_{\rm phtm}$ =  2.185 days  and $\Delta V$  = 0.033  mag but  no evidence  for eclipses.
(579) derived  different  photometric  periods  within  one  observing  season
indicating rapid  spot evolution  and (587) found seven spots existing between
1980 and  1988 with  lifetimes between  several months  and  a  year.    (587)
detected a  shallow partial  eclipse but no secondary eclipse. (262) reported
$V(max) = 7.72$ mag.

{\bf 163.   [HR 7275]}     (259) gives  $\log L_X = 30.56$ erg\,s$^{-1}$.  IR wave 
amplitude at
$(J,H,K,L) =  (0.11,0.09,0.09,0.06)$ mag  (321).   $F(K) =  3.0\cdot 10^6$ 
and  $F(H)  = 
2.5\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$  (171).   (306) list Dist. $\geq$ 33 
pc.  (259) and (439) give
Dist. =  48 pc,  which is  incompatible with  the measured  $M_V$.  (77) lists a
parallax of  0.002" [$\approx$  500 pc]  and (245)  lists a  trigonometric parallax of
0.004$\pm$0.006" [$\approx$  250  pc]  which  would  be  consistent  with  a  III-IV
classification.   (139) found  $M_V$ = -1.2 mag from the width of the Ca\,{\sc ii} H \& K
lines (Dist. = 250 pc).  Distortion wave migration period is 2.7 yr (52), (52)
also gives  $\Delta V_{\rm wave}$ =  0.22 mag and $P_{\rm phtm}$ = 27.8 
days.  (132) reports X-ray 
emission  of $6.3\cdot 10^{31}$  erg\,s$^{-1}$, (325)  derived  
$v\sin i <  15$  km\,s$^{-1}$.    (77)
classified it  as K1IV.   For  (U,V,W) see also (44).  (579) report dramatic 
$V$-amplitude 
changes  from one  season to the other.  H$\alpha$ monitoring by (672)
and (673) [see also (588)] shows large equivalent-width variations. 

{\bf 164.   [1E1919+0427]}    No  Ca\,{\sc ii} H and K observations but emission at the Ca\,{\sc ii}
infrared triplet (IRT) and at H$\alpha$ suggest also H and K emission.

{\bf 165.   [HD 181809]}     (35) reports  K1IV.   A light curve can be found on the
front page  of IAPPP No. 26 [from Pazzi L., 1986, in Nigel, South
Africa].   From this  D. S. Hall derived the listed values of $P_{\rm phtm}$ = 61.0$\pm$
0.3 days  and $\Delta V_{\rm wave}  \approx$ 0.35 mag, which is unusually 
large for an RS CVn 
binary.   Other $P_{\rm phtm}$  determinations are  given by  (283), namely  58.33 and
57.34 days,  about 4.5  times longer  than the orbital period!  Their observed
amplitude of  0.27 mag  is somewhat smaller than the listed value appearing in
the catalog.   (614)  analyzed 11  years of  $V$ photometry and found amplitudes
ranging from 0.12 to 0.31 mag.

{\bf 166.   [HD 182776]}     Another possibility is $P_{\rm phtm}$ = 46.05 days (283), (283)
also gives $<(V-I)>_{KC}$ = 1.27 mag.

{\bf 167.   [HR 7428]}     (306) lists  Dist. =  320 pc,  and $M_V$ = -1.1 mag.  (190)
derived $f(m)$ = 0.1222.  (191) reports a visual amplitude of 0.015 mag possibly
due to spots and also evidence for an ellipticity and a reflection effect, but
the 0.033  mag amplitude found by (656) for the ellipticity effect is a better
value.  (643) found $V(max) = 6.38$ mag.  (579) report a small difference in the
heights of  light maxima  and minima  and estimated a spot ``wave'' amplitude of
0.02 mag.   (656)  found evidence  for differential  rotation from photometric
periods of  four individual  spots.   HR 7428  has the largest IR excess at 
60 $\mu$m in the sample of (658).

{\bf 168.   [HD 185151]}     (22) reports  a blueshifted H$\alpha$ emission wing and a
double-sine light  curve.   $F(K) =  3.3\cdot 10^5$ and  $F(H) =  2.4\cdot 
10^5$  erg\,cm$^{-2}$s$^{-1}$
(171).    (262)  listed  $P_{\rm phtm}$  =  40.1  days,  which  is  the  same  as  the
spectroscopic period.   (22)  also gives  $v\sin i$ =  25 km\,s$^{-1}$  and 
a single-lined 
spectrum of  a K2III  star and  found following preliminary orbit: $\gamma$ = -22.7
km\,s$^{-1}$, K  = 44.2  km\,s$^{-1}$, $e$  = 0.10,  $\omega$ = 87.5 $\deg$ 
and $a\sin i = 24\cdot 10^6$ km.  (122)
reports ``strong''  H \&  K emission,  (262) mentioned  a weak H$\alpha$ line, (22)
estimated a  radius of  17-22 R$_\odot$.   (443) found light variations with
$\Delta V$ =  0.125 mag  and a period of 40.133 days due to the ellipticity effect
[see also  (442)].   (22) mentioned  ``possible eclipses''  which have  not been
confirmed by  (443).   (FCF) found  a more recent time of conjunction with the
primary star behind at JD 244 5967.536.  (579) report a wave amplitude of only
0.04 mag  and $P_{\rm phtm}$  = 40.4  days in  1985, and  40.2 days in 1986.  From the
observed mass  function and assumed secondary mass, (655) estimate $i = 
62\pm12 \deg$ and suggest an early F star as secondary component. Evidence of 
the F-type secondary is seen in IUE spectra (FCF). 

{\bf 169.   [1E1919+0427]}    No  Ca\,{\sc ii} H and K observations but emission at the Ca\,{\sc ii}
infrared triplet  (IRT) and  at H$\alpha$  suggest  H  and  K  emission. 
$BVRI$ 
photometry by (716) indicate the presence of a spot wave but no eclipses.

{\bf 170.   [HD 185510]}     The hot companion is most likely a B1-2 subdwarf (185).
Photometry by Moffett, T. J., 1980 [priv. comm. to (185)] is consistent with a
K1III spectral  type for  the cooler  component.   (173) gives K0IV-III.  Weak
H$\alpha$ absorption feature and ``strong'' H \& K emission (185).  (262) 
also report a
weak H$\alpha$  absorption line and  give the minimum radius for the cool
star as  6 R$_\odot$.  (186) obtained $P_{\rm phtm} \approx$ 25 days, (283) 
found another 
possibility for  $P_{\rm phtm}$, namely  26.02 days,  and gave  a  slightly  different
orbit.  (614) analyzed seven photometric data sets and found periods of around
25 days.   Light  curve appears  sometimes double  humped and sometimes single
humped (614).   (658)  report large  IR excess at 12 and 25 $\mu$m.  
(597) lists $L_X = 14\cdot 10^{31}$ erg\,s$^{-1}$.  Subdwarf
IUE spectrum in (744) as well as $UB$ photometry.

{\bf 171.  [HD 188088]}   Super-metal-rich star with strong CN and sodium (416), the
colors are  from Moffett,  T., 1979  [priv. comm.  to (416)].  Note the highly
eccentric orbit!   (416)  also derived  the age  of the  system to $5\cdot 
10^8 - 2\cdot 10^9$ yr  and reported a lack of lithium.   (416) derived a rotational period
of 6.5  days from  $v\sin i$ measurements.  (614) report a significantly different
photometric period of 16 days which has been entered into Table 2.  Thus, with
$e$ =  0.692, HD  188088 rotates  more slowly  than the pseudosynchronous value.
For (U,V,W) see also (380).

{\bf 172.   [HD 190540]}   (173) noted H \& K emission and gave F/K0IV spectral type.
The photometric  period from  (208), $\approx$\,8.3  days, is half of the orbital period
(262), doubling it results in the photometric period given in the catalog [see
also (262)].

{\bf 173.   [HD 191262]}     (614) observed  a large  range of differential $V$ values
($\sigma_{\rm ext}$ =  0.048 mag)  but found  no convincing  period.   The  photometric
period given  by one of us (DSH) is the mean of values found from two-spot model fits of
six light  curves during  a 2.5-year  interval, and the amplitude given is the
maximum in $V$.  Ca\,{\sc ii} H and K spectra show double emission components with equal
fluxes of $\log F'(K,H) = 6.4$ erg\,cm$^{-2}$s$^{-1}$ (588).

{\bf 174.   [HD 193891]}    The star is
not listed  in the  Abt \& Biggs catalog.  Ca\,{\sc ii} observations give 
$\log F'(H,K) = (6.25,6.35)$ erg\,cm$^{-2}$s$^{-1}$ (KGS).  ``Weak'' 
emission was first noted by (531). 

{\bf 175.  [BI Del]}   (702) lists it as G0 and semidetached EA.

{\bf 176.   [HD 195040]}   H$\alpha$ core absorption (35), (38) also gives $V$ = 8.4 mag
and a  K3IV-III classification.   (371)  reports $P_{\rm phtm}$ = 23 days, (283) found
another possibility of 25.15 days.  See also (614).

{\bf 177.  [CG Cyg]}   (308) classified it as G1V/G9V or G9V/K0V and gave masses for
both classifications.   (258):  G2III/K2IV, (308)  gives $<(B-V)>$  = 0.78  mag.
(65) postulated $dM/dt = 1.4-3.7\cdot 10^{-9}$ M$_\odot$yr$^{-1}$, 
\vec{B}(dipol) = 1118 G, and $d\ln P/dt =
-6.53\pm1.49 \cdot  10^{-8}$ yr$^{-1}$.   IR  excess $(J,H,K)  = 
(-,-,\approx 0.15)$  mag (349).
Possibly circumstellar  matter  (244)!    (93)  reports  IR  excess  in  
$JHKL$.
Distortion wave migration period is 10 yr (61), (432) found 
$dP/dt = 4.8\cdot 10^{-11}$
days/day.   It  is  not  known  which star shows the Ca\,{\sc ii} H \& K emission (61).
(632) obtain  $i =  82.8 \deg$,  component masses  of  0.72/0.72 M$_\odot$,  
and  radii  of
0.84/0.79 R$_\odot$ from light curve analysis and suggest spectral types of
G9V/K0V.  (664) notes small-scale ``bumps'' on the shoulders of the light curve.
Further photometry  has been  reported by  (666), (676),  (678), a.o..
(826) found  the mean brightness (outside eclipse) to vary with the same cycle
length as  the orbital period, i.e. $\approx$\,50 years, predicted by the magnetic cycle
theory of (872).

{\bf 178.   [V1396 Cyg]}   A-component of the close visual binary 
AC+39$^\circ$1214-608 [B-component is  a  
M3.5  dwarf (647)].   The  $V(max)$ value  in Table 2 is the
combined AB brightness.  (405)  lists  IR-colors $(J-H) = 0.603$ mag and 
$(H-K) =
0.204$  mag,  EW(H$\alpha$)  =  +1.28  m\AA \  (405),  see  also  (818)  for  H$\alpha$
variability.   For (U,V,W)  see also  (381).   The listed spectral type is the
combined classification,  see reference  (381).  Individual magnitudes for the
primary/secondary are  10.7/11.3 mag, respectively (381).  A new CORAVEL orbit
for Aa  - Ab  and A - B from (647) is given in Table 4 ($e$ = 0 assumed).  (647)
also noted  that the inner and outer orbits are not coplanar.  (818) lists 
$R-I= 0.91$ mag for the combined color.

{\bf 179.   [ER Vul]}    Orbit of (762) is in agreement with the newly derived orbit
of (814)  which is  listed in  Table 4 except that the eccentricity of 0.02 by
(762) is likely spurious.  Activity parameter $\log R$ = 1.04 (318).  (308) notes
for the  masses (hot/cool)  = 1.23/1.13  M$_\odot$, respectively.   (65) postulated
$dM/dt = 3.6\cdot 10^{-9} - 1.8\cdot 10^{-8}$ M$_\odot$yr$^{-1}$, 
\vec{B}(dipol) = 723 G, and $d\ln P/dt = -2.47\pm
0.92 \cdot  10^{-7}$ yr$^{-1}$.   (306)  lists $\mu_\alpha$ = 0.080", 
$\mu_\delta$ = 0.01", gives 
Dist. =  200 pc and classified it as G0III with $M_V$ = +0.6 mag which is highly
unlikely for  a 0.6-day  binary!   (458) listed  $v\sin i$ (hot/cool) = 85/85 km\,s$^{-1}$,
masses (hot/cool) =  0.90/0.88 M$_\odot$ with equal radii of 1.23 R$_\odot$, 
(467)
derived a  somewhat different  epoch for the primary minimum of 244 0182.3212 +
0.698082$\cdot$E,  and found  the orbital semimajor axis to be $a$ = 4.25 
R$_\odot$.
For (U,V,W)  see also  (44, 98).  (62) listed $\Delta V$ = 0.04 mag.
(596) suggest  that both  stars are ``active'' and not only the G0V component as
suggested by  (467).   (632) derived  slightly different masses and radii than
spectroscopic values  of (762).   (159)  gives a  distance of  45 pc and $M_V$ =
4.8/4.6 mag.

{\bf 180.   [HD 202134]}     Another possibility is $P_{\rm phtm}$ = 60.24 days (283), (283)
also gives $<(V-I)>_{KC}$ = 1.16 mag.  Note the high eccentricity, and the 
high U 
velocity!   (384) observed a brightening in $V$ by 0.07 mag over 8 nights, 
thus 
$\Delta V_{\rm wave}$ could  be larger  than 0.14  mag.   (173) classifies it as K1III.
See also (614).

{\bf 181.   [HD 202908]}     Triple system  [see (278)].  All three stars show H \& K
emission (278).   (278)  also found a large lithium abundance, which indicates
that HD  202908 is a young solar type star.  (306) lists Dist. = 36 pc.  A few
additional velocities and comments in (747).

{\bf 182.   [HR 8170]}   The eccentricity of the orbit of (714) would be judged zero
by the  precepts of Lucy \& Sweeney.  (492) present an updated circular orbit
for the  hot component.  The system is a SB2.  Member of the Sirius group (77)
and UMa stream (77).  The absolute Ca surface flux is computed from the 
flux value $F$(Ca\,{\sc ii}) = 5.83 in (624, 741) by multiplying with 
$1.29\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$.

{\bf 183.   [HD 204128]}  (283) lists  $<($V-I$)>_{KC}$ = 1.26 mag and $V$  = 9.58 mag.
Eccentric orbit!

{\bf 184.   [BD-00$^\circ$4234]}  ``Intermediate case  of an  RS CVn  and a  BY Dra  type
binary?'' (272).  H$\epsilon$ is also in emission (272).  For (U,V,W) see also (272).
Note the  high U-velocity!  (828) reported possible orbital period changes and
found $P_{\rm orb}$ =  3.7584 days and $T_0$ = 2444063.908.  
Lithium abundance $\log n(Li)$ 
= 0.65 presumably for the primary star (828).  Chemically an old star 
$[Fe/H]$ = -0.7 (828).

{\bf 185.   [HD 205249]}     (306) lists  it as G5IV.  (173) reports H \& K emission,
(209) found  the photometric  period to  be $\approx$\,58  days, (283)  lists  a  second
possibility of 57.31 days, (283) also gives $<(V-I)>_{KC}$ = 1.01 mag.

{\bf 186.  [AD Cap]}   Activity parameter $\log R$ = 0.65 (318).  (259) gives 
$\log L_X = 
31.28$ erg\,s$^{-1}$.   (108)  and (258) note ``semidetached'' character, (318) listed it
as ``detached''.   GCVS  1969 and  (252) as well as Wood, F. B. et al.: 
1980 [``A finding list  for observers  of interacting  binary stars'',  
5th edition]  give
$P_{\rm orb}$ =  6.11826 days  [Tsesevich 1954,  Izv. Astr. Obs. Odesskii 
4, 165], but
2.96 days is the correct orbital period according to (628).

{\bf 187.   [42 Cap]}   (77) gives the spectral type G1V/G0V and notes a single line
spectrum.   Eccentric orbit!   (139)  listed it with $M_V$ = +2.5 mag, 
IR excess 
(93).  For (U,V,W) see also (44).  $V\sin i$ measure of (494) has been updated and
a better value is given in Table 3.

{\bf 188.   [FF Aqr]}    (217) derived masses and radii of 0.6/2.5 M$_\odot$ and 0.15/6.0
R$_\odot$  for the  hot/cool component,  respectively.  The light variations
outside eclipse  are asymmetric  and maximum  light occured at phase 0.66 [see
the light  curve in  (216), their Fig. 2], nevertheless (216) attributed these
variations to a ``very strong'' reflection effect.

{\bf 189.   [RT Lac]}   (245) listed a trigonometric parallax of 0.023$\pm$0.008" 
[$\approx$ 43 pc] but
(61), (307)  and others,  used Dist.  = 205  pc, (259)  gives 210  pc, and from
Eggen's [=(44)] $M_V$ one may find Dist. $\approx$ 150 pc.  
(258), (259) and (244) noted it as ``semidetached''.  (93) derived
an orbital  semimajor axis  of $a = 11.1\cdot 10^6$ km.  (65) postulated 
$dM/dt = 5.9-
7.3 \cdot 10^{-7}$ M$_\odot$yr$^{-1}$, no \vec{B}, and $d\ln P/dt = 
+2.89\pm0.32 \cdot 10^{-7}$ yr$^{-1}$.  IR excess
$(J,H,K) =  (0.41,0.51,0.61)$ mag  (349).  G-star fills its Roche lobe (84,875).
(309) lists  $F(K) = 4.2\cdot 10^6$ and $F(H) = 3.9\cdot 
10^6$ erg\,cm$^{-2}$s$^{-1}$.  Cycle period 
30-35 yr   
[Haslag,  K.:  1977,  M.Sc.  Thesis,  Vanderbilt  U.,  Nashville,  TN].
Sporadic  excess   of  emission   and  absorption   in  H$\alpha$   core  (180),
circumstellar matter  (244), (150) also reports IR excess at $JHKL$.  Distortion
wave migration  period is  given as  10 yr by (92) and as 4.5 yr by (150), but
the wave periods also range from 5-40 yr in (61) [and references therein].  We
listed it  as a  ``total'' eclipsing  binary, but it could be possibly ``partial''
due to  radius changes  of up to 20\% reported by the same source, namely (38).
(110) derived  minimum masses  of 0.6/1.5 M$_\odot$.   Recent times  of minima  in
(671).  $V\sin i$ measure of (421) has been updated and a better value is given in
Table 3.

{\bf 190.  [HK Lac]}   (259) gives $\log L_X = 31.14$ erg\,s$^{-1}$.  (306) lists 
$M_V$ = 0.2 mag 
and Dist.  = 170  pc, (139)  derived $M_V$ = -1.0(:) mag from H \& K width.  
(11)
gives $P_{\rm phtm}$  = 25.3  days, whereas (62) gives 24.0026 days which is 
closer to
the orbital  period.   Distortion wave  migration period is given as 85 yr and
270 yr  by (178).   (50)  found $<(B-V)>$  = 1.11  mag  and  classified  it  as
FIV/K0III, (139)  listed $<(B-V)>$ = 1.01 mag, (434) found a possible spot cycle
of $\approx$\,7 yr, (287)  notes ``strong'' H$\alpha$ absorption.  HK Lac is also listed in
(298).   (178) estimated  an  inclination  of  $i \approx  60  \deg$.    (579)  report
photometric  periods   of  24.53  and  24.21  days  in  1983-84  and  1984-86,
respectively.  13 years of photometry are analyzed in (824).

{\bf 191.  [AR Lac]}   (358) a.o. note flare activity.  (259) and (359) give Dist. =
40 pc,  (159): Dist.  = 50  pc, (259)  also lists $\log L_X = 31.18$ 
erg\,s$^{-1}$.  (18) 
gives G2IV/K0V,  (77) lists  it as G2IV/K0III.  (166) notes short-time H$\alpha$
emission variability.   (65)  postulated $dM/dt =  7.0-9.9 \cdot 10^{-10}$ 
M$_\odot$yr$^{-1}$,
\vec{B}(dipol) =  165 G [(359) estimated 5-80 G], and $d\ln P/dt = 
2.158\pm0.22 \cdot 10^{-7}$
yr$^{-1}$.   IR excess $(J,H,K) =  (0.17,0.25,0.25)$ mag (349).  (181) gives 
$i = 87 \deg$.   
(108) derived  preliminary radii  of 1.8/3.1 R$_\odot$, respectively.
$F(K) = 1.4\cdot 10^6$ and $F(H) = 1.2\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ 
(309).   (77) lists $\mu_\alpha$ = 
-0.029" and $\mu_\delta$ = 0.035".  Short term variability ($\approx$\,3 min) 
in H \& K (61), 
H$\alpha$ is filled-in (18), and has a presumably randomly variable 
absorption profile (19,
181).   (133) derived  masses of  1.31/1.32 M$_\odot$,  and (195)  gives  radii  of
1.1/2.19 R$_\odot$ for the hot/cool component, respectively.  See also (31).
Orbital semimajor  axis $a = 6.51\cdot 10^6$ km (195).  IR colors $(K-M) = 
0.0$ mag and
$(K-N) =  0.0$ mag  (251), $<(B-V)>$  = 0.81 mag and $\Delta V_{\rm wave}$ = 0.04 mag (31).
Distortion wave  migration period  is given  by (86) to 2.5 yr and by (131) to
12.5$\pm$0.3 yr.   Examination  of 18 light curves by (569) revealed a migration
between 10  to 15  yr/cycle and 50 to 60 yr/cycle.  X-ray observations also by
(132) and  (249) a.o.. High-resolution  line profiles  are reported by (322).
(642) report the finding of a 10 yr spot cycle period.  $V\sin i$ measure of (181)
has been updated and a better value is given in Table 3.

{\bf 192.   [WW Cep]}    Narrow lines are seen in the red with a line-depth ratio of
$\approx\,$6:1 and  equal widths  (692).  (692) also notes that the ephemeris in the new
GCVS (=702) are inconsistent with his spectra.  (702) lists it as G3, EA/SD:.

{\bf 193.   [HD 212280]}     (366) gave a G0IV ``composite'' classification, and found
double lines  on one  plate, with  radial velocities  of -39.4 and +40.3 
km\,s$^{-1}$, respectively.

{\bf 194.   [V350 Lac]}   Ca\,{\sc ii} $F(K) = 1.1\cdot 10^6$ and $F(H) = 1.2\cdot 
10^6$ erg\,cm$^{-2}$s$^{-1}$ (171).
(306) gives  Dist. =  200 pc  with $M_V$ = -0.1 mag and lists $\mu_\alpha$ = -0.029"
and $\mu_\delta$  = -0.04".   (304):  $a_1 \sin  i =  9.81\cdot 10^6$ km,  
(258)  lists  a
photometric (?)  period of 17.748 days.  The $V$-amplitude of 0.13 mag is due to
the ellipticity effect (75,582).  (309) also noted H \& K emission, (262) gives
a K2III  classification and  doubled the  photometric period  to be consistent
with the  orbital period.   [See also (75) and (579).]  The radio flux density
of 20  mJy listed  in the first edition of the catalog is from Feldman, P. A.:
1983 [priv. comm. to (439)].  For (U,V,W) see also (44).

{\bf 195.  [FK Aqr]}   A-component of the visual pair ADS 11854.  The B-component is
also a  dMe flare  star [=  Gl 867B = FL Aqr, see IBVS 1407] with $V$(B-comp.) =
11.5 mag,  25" away [but is excluded in the measurements of (273)].  The light
from this  component varies by 0.15 mag in $V$ with a period of 1.95 days (424).
(403) reported  a dM1e star with double H$\alpha$ and Ca\,{\sc ii} H \& K emission lines.
Optical flares  (541)!   See also (404).  (818) also lists $R-I$ = 0.94 mag.  X-
ray observations  are summarized by (862) and (861).  It is not clear which of
the two  components, Gl 867 A or B, is the more luminuous at X-ray wavelengths
(861). (861) lists $L_X = 0.02\cdot 10^{31}$ erg\,s$^{-1}$ from the combined 
count rate.  

{\bf 196.   [IM Peg]}     Also known  as the optical counterpart of the X-ray source
4U225218.   (77) lists it as K1-2II-IIIe.  The strong H \& K emission was noted
by (75).   (170)  noticed ``moderate'' emission strength.  (259) gives 
$\log L_X = 
30.64$ erg\,s$^{-1}$.   $F(K)  = 7.2\cdot 10^6$  and $F(H)  = 6.0\cdot 10^6$ 
erg\,cm$^{-2}$s$^{-1}$ (309).  (306) 
gives $M_V$ = 0.0 mag.  (259) used 51 pc.  (306) listed 130 pc.  Distortion wave
migration period  is 6.5  yr (41).   For  (U,V,W) see also (44).  (579) report
``wave'' amplitudes  in the  range of 0.17 through 0.22 mag from 1983-84 through
1987.

{\bf 197.   [HD 217188]}     It is not sure whether the $V$ amplitudes of 0.18 mag and
0.16 mag  reported by  (579) and  (232), respectively,  are due to complex spot
activity or  a combination  of ellipticity effect, reflection effect, and weak
spot activity.  The formal value for $P_{\rm phtm}$ from (579) is given in Table 2 but
is almost exactly a factor two larger than the orbital period.

{\bf 198.  [HD 217344]}   (283) gives $<(V-I)>_{KC}$ = 0.82 mag.  (173) classifies it as
G5IV.  $T_{\rm conj}$ in Table 4 has been computed from the orbit in (727).
(856) lists $L_X = 1.318\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 199.   [KU Peg]}     (850) report no detection of a hot, luminuous companion in
IUE spectra.   The  primary has very strong UV lines (850).  (852) pointed out
that, if  the photometric  period is  the rotation  period of the star, the MK
class II  radius would  result in a very small inclination making it difficult
to explain the 0.07 mag photometric amplitude.  A ``giant'' (III) classification
and $i \approx 60 \deg$ would be a better guess.

{\bf 200.   [KZ And]}     B-component is  a spectroscopic binary in the close visual
pair ADS 16557 [component A is only 15" away, $V \approx$ 7.2 mag] (273, 258).
(592) lists $L_X = 0.05\cdot 10^{31}$ erg\,s$^{-1}$.  

{\bf 201.   [RT And]}     (65) postulated $dM/dt = 2.1-2.6 \cdot 10^{-9}$  
M$_\odot$yr$^{-1}$, \vec{B}(dipol) =
526 G,  and $d\ln P/dt  = 1.17\pm0.06\cdot 10^{-7}$  yr$^{-1}$.   
(258) listed $<V>$ = 8.5 mag,
(91) reports a wave amplitude $\Delta V_{\rm wave}$ = 0.04 mag.  (44) $<B-V> = 
0.56$ mag.
Detached system!   (90)  gave a  spectral type  similar to  that listed in the
catalog.   The secondary  component seems  to be a K0V [see summary in (633)].
(633) also  discuss previous  light curve  solutions.   Orbital inclination is
uncertain but  the small  eccentricity is  confirmed from light curve analysis
(633).  Ca\,{\sc ii} H and K emission not detected with CCD + echelle (703).  A recent
time of  minimum in  (671).   Further photometry  in (680),  (684), (688), and
others.

{\bf 202.   [SZ Psc]}     (108) gives preliminary radii for the hot/cool component 
as 1.6:/4.0: R$_\odot$ 
and the  masses as  1.33/1.65 M$_\odot$,  respectively.  (38) noted $i = 
77.75\pm1.0 
\deg$ and  (181) $i  = 75.8  \deg$.   (259) gives  $\log L_X  = 31.40$  
erg\,s$^{-1}$.    (65) 
postulated $dM/dt  = 6.1-7.8  \cdot 10^{-8}$ M$_\odot$yr$^{-1}$,  
\vec{B}(dipol) = 252 G,  and $d\ln P/dt =
-5.25\pm0.33 \cdot 10^{-6}$ yr$^{-1}$.   $F(K)  = 3.3\cdot 10^6$  and $F(H) 
= 3.6\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$
(309).   H$\alpha$ ``outbursts''  (243).   (181) also gives radii of 
1.38/5.08 R$_\odot$, and noted variable IR.  But no IR-excess (248).  
Distortion wave migration period 
is 4.2  yr (103).   (82) reports $(B-V) = 0.81-0.99$ mag and 
$\Delta V_{\rm wave}$ = 0.14
mag; orbital semimajor axis $a = 10.9\cdot 10^6$ km (82).  (282) listed it 
with $M_V =
-1.43$ mag,  (243) also  reported H$\alpha$  outbursts in  1979.  For (U,V,W) see
also  (44).    (804)  report  a  massive  X-ray  flare  ($>1$  day)  from  ROSAT
observations.   $V\sin i$ measure  of (181) has been updated and a better value is
given in Table 3.

{\bf 203.   [EZ Peg]}   (265) and (428) report KPNO data and estimated a preliminary
orbital period.   They  also showed  that EZ Peg is an RS CVn system with both
stars in  synchronous rotation.  The primary is the active component.  The hot
B spectrum  reported by  Vyssotsky in  1943 seems to be an artifact of the low
spectral resolution he used.  EZ Peg is therefore not a U Geminorum system.

{\bf 204.   [$\lambda$ And]}     (286) mentioned  variable line widths and found 
$M_V$ 
ranges from +1.9 to -0.3 mag derived from Ca\,{\sc ii} K width.  (139) listed it with
$M_V$ =  +2.0 mag.   (44)  gives $(R-I)$= +0.40 mag.  (300) estimates 
$i \approx 30 \deg$. 
(259) gives  $\log L_X  = 30.56$  erg\,s$^{-1}$.   IR excess $(J,H,K) = 
(0.61,-,0.87)$ mag
(349).   $F(K) = 1.7\cdot 10^6$ and $F(H) = 1.7\cdot 10^6$ erg\,cm$^{-2}$s$^{-1}$ 
(309).  EW(He\,{\sc i} 10830) 
= 1000  m\AA \ (354).  For H \& K see also (45).  (579) derive seasonal photometric
periods of 55.8, 51.6, and 55.2 days, evidence for sinusoidal variation of the
mean brightness  is also presented.  (870) find an 11-year cycle.  (871) found
nine spots  between 1976  and 1991  with lifetimes  between 1.4 and 6.5 years.
$V\sin i$ measure  of (448)  has been updated and a better value is given in Table
3.  Further H$\alpha$ and Ca\,{\sc ii} H and K spectroscopy in (649) and (588).

{\bf 205.   [HD 222317]}   Listed in (298).  Photometry by (579) showed very small 
$V$
amplitudes of  0.01 mag in 1985 and 0.005 mag in 1986.  Ca\,{\sc ii} H and K 
line-core
flux density  of $4.77\cdot 10^6$  erg\,cm$^{-2}$s$^{-1}$ measured  by (624).   Earlier  orbit by
(408) must be judged circular by the precepts of Lucy \& Sweeney.

{\bf 206.   [II Peg]}     (44) listed it as K0V, (128) and (307) gave K2V-IV.  (128)
also gives $(V-R)$= 0.86-0.92 mag.  (259) measured $\log L_X = 30.30$ 
erg\,s$^{-1}$, (347) 
gives $L_X = 40\pm12 \cdot 10^{30}$ erg\,s$^{-1}$.  (300) estimated 
$i \approx 60 \deg$, (128) and (68)
derived $e$  = 0.033$\pm$0.035,  so we  have adopted  an $e$  = 0 solution for the
catalog.   Cycle period  8-10 yr (360) and long term variations of the mean B-
magnitude with  $\approx$\,40 yr  (361).   (306) gives  Dist. = 21 pc and 
$M_V$ = 5.9 mag. 
H$\alpha$ emission is well correlated with spot activity (127).  (118) mentioned
X-ray flares.   For  (U,V,W) see  also (44).   (579) report photometry for the
years 1985  and 1986.   (127)  found a $V$ amplitude of 0.43 mag in 1977.  (640)
detected TiO  band variations  in phase  with $BV$  photometry.   (641) detected
variable He\,{\sc i} D3 emission.   Further  photometry has  been reported  by (667),
(675), (682).   (588)  measured absolute  Ca\,{\sc ii} surface  fluxes  of  
$\log  F'(K,H)  =
(6.46,6.46)$ erg\,cm$^{-2}$s$^{-1}$.   Flaring  and quite  X-ray and  UV light  curves were
reported by (864).

\end{document}
