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\centerline{\bf Notes to Table 1 (Hartkopf et al., 1993, AJ, 106, 352}
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\bpar {\bf 00283$-$2020 = B 1909:} This has long been a difficult
visual system, with the two components remaining within 0$''$\llap.2 of
each other throughout the orbit.  With this observation we have
completed a full revolution using speckle data alone, and have derived
new orbital elements which will be published shortly.

\bpar {\bf 00479$-$2921 = I 261:} Having had only one other measure in
the last 35 years, this pair needs further observation, especially
since we appear to be near periastron at this epoch.

\bpar {\bf 01243$-$0655 = Bu 1163:} A new interferometric orbit of this
very eccentric (e = 0.94) system is in preparation.

\bpar {\bf 02396$-$1153 = Fin 312:} Residuals from the orbit of
Hartkopf et al. (1989, AJ, 98, 1014) are (0$^{\circ}$\llap.2,
-0$''$\llap.003).

\bpar {\bf 02398$+$0009 = A 1928:} Periastron passage for this very
close visual pair has thus far been well covered by speckle.

\bpar {\bf 02518$-$2117 = See 21:} This very close visual system was
discovered at a separation of 0$''$\llap.36 and has closed steadily for
over 90 years.  It is unknown at this point whether the system is still
approaching periastron or has begun to widen.

\bpar {\bf 03544$-$4021 = Fin 344 AB:} This is the first observation of
this system since those of Finsen in the 1960's, and is considerably
closer than any of his results.  It is known that in some instances
Finsen's $\rho$ values appeared systematically larger than those of
speckle; further observations of this system will determine whether
such is again the case.

\bpar {\bf 04037$-$1545 = A 2913:}  This system closed steadily from
its discovery at 0$''$\llap.45 in 1915 to 0$''$\llap.22 in 1959; this
is the first observation in 30 years so it is unknown whether the pair
has passed through periastron.

\bpar {\bf 04256$+$1557 = Fin 342 Aa:} Residuals from the orbit of
McAlister et al. (1988, AJ, 96, 1431) are (-2$^{\circ}$\llap.3,
0$''$\llap.008).

\bpar {\bf 05248$-$5219 = I 345 AB:} This system has also decreased in
separation steadily since the 1920's, and was last resolved visually in
1983.

\bpar {\bf 05565$-$2631 = B 94:} This system was last resolved visually
in 1978, and appears to be continuing to approach periastron.

\bpar {\bf 07003$-$2207 = Fin 334 Aa:} The system has opened slightly
since the last speckle observation in 1989.3; unfortunately it was last
observed in 1966 so it may be difficult to pin down the time of
periastron passage.

\bpar {\bf 08125$-$4616 = CHARA 143 Aa:} These measurements confirm the
discovery observation of this close companion to See 96, made in the
spring of 1989.

\bpar {\bf 08285$-$0230 = A 551 AB:} Speckle observations are in poor
agreement with the orbit of van den Bos (1953, Union Obs. Circ., 6,
211). A new orbit is in preparation.

\bpar {\bf 09123$+$1459 = Fin 347 Aa:} Residuals from the orbit of
Hartkopf et al. (1989, AJ, 98, 1014) are (-0$^{\circ}$\llap.3,
-0$''$\llap.003) and (-3$^{\circ}$\llap.2, 0$''$\llap.003).

\bpar {\bf 10120$-$2836 = B 194:} Periastron passage apparently
occurred about the time of or shortly before our first speckle
observation in 1989.3.

\bpar {\bf 12597$-$0348 = CHARA 39 Aa:} This interferometric system has
now completed nearly 180$^{\circ}$\thinspace of revolution since its
discovery in 1984.  A preliminary determination of orbital elements
yields a low--eccentricity orbit with a period of 15.7 years.  Absolute
quadrant determinations based on reanalysis of earlier speckle data
have ruled out a possible short--period high--eccentricity orbit. A
more complete orbital analysis is in progress.

\bpar {\bf 14373$+$0217 = CHARA 42 Aa:} This system apparently is
continuing to close toward periastron.

\bpar {\bf 16057$-$0617 = Fin 384 Aa:} Residuals from the orbit of
Baize (1992, A\&AS, 92, 31) are (-4$^{\circ}$\llap.5, 0$''$\llap.003).

\bpar {\bf 16245$-$3734 = B 868:}  This system may have made a very
close periastron passage between the times of our 1989.3 observation
($\rho$ = 0$''$\llap.039) and this one, although unfortunately the
system was not observed in 1990.

\bpar {\bf 16391$-$3713 = Fin 340 AB:} From its discovery in 1954
through the mid-1960's, this system closed from 0$''$\llap.14 to
0$''$\llap.10 and increased in $\theta$ from 147$^{\circ}$\thinspace to
172$^{\circ}$\llap.~  It is impossible to determine from this single
speckle measure whether the pair has gone through periastron and
flipped quadrant, but this should become obvious within the next couple
of observations.

\bpar {\bf 16438$-$5330 = Fin 251 AB:} The close third component CHARA
147 Aa discovered in 1989.3 was unfortunately not confirmed in these
observations.

\bpar {\bf 17207$-$5625 = Fin 255 AB:} This observation finally
confirms the discovery of this system by Finsen, made in 1931!

\bpar {\bf 19253$-$2431 = Fin 327:} With 15 years of speckle data on
this system we are finally able to attempt to improve upon Finsen's
(1965, Republic Obc. Circ., 7, 85) orbital elements.  We apparently
view the pair at a nearly 90$^{\circ}$\thinspace inclination and since
the $\Delta$m for the components is near zero there is considerable
ambiguity between a high--eccentricity short--period orbit and a
low--eccentricity long-period one.  A new orbital analysis is now in
preparation, including reanalysis of earlier speckle data in order to
derive absolute quadrants and possibly resolve this ambiguity.

\vfill\eject\end


