%\documentstyle{laamt} \documentstyle{article} \def\vec#1{{\bf#1}} \begin{document} {\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 $ = 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) $ = 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): $ = 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), $ = 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 $ = 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 $$ = 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 $$ = 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 $$ = 8.5 mag, (91) reports a wave amplitude $\Delta V_{\rm wave}$ = 0.04 mag. (44) $ = 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}