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Astronomy & Astrophysics manuscript no.
(will be inserted by hand later)
Speckle interferometry of nearby multiple stars. II. #
I. Balega 1 , Y.Y. Balega 1 , A.F. Maksimov 1 , E.A. Pluzhnik 1,3 , D. Schertl 2 , Z.U. Shkhagosheva 1,3 , and
G. Weigelt 2
1 Special Astrophysical Observatory, N.Arkhyz, Karachai­Cherkesia, 369167 Russia
2 Max­Planck­Institut f˜ur Radioastronomie, Auf dem H˜ugel 69, D­53121 Bonn, Germany
3 Isaac Newton Institute of Chile, SAO RAS Branch
Received date; accepted
Abstract. This paper is a continuation of di#raction­limited speckle interferometry of binary and multiple stars
carried out at the 6­m telescope of the Special Astrophysical Observatory in Zelenchuk. The program has con­
centrated on nearby (# > 10 mas) close binaries discovered or measured during the Hipparcos mission. Here, we
present 132 measurements of relative positions and magnitude di#erences for 99 pairs and 8 measurements for
6 triple systems. 54 entries in the paper are new Hipparcos binaries. New triple systems with late­type dwarf
components, discovered in the course of observations, are HIP 8533 and HIP 25354.
Key words. stars: binaries (including multiple) -- techniques: interferometry
1. Introduction
This paper continues presentations of the results of binary
and multiple star speckle interferometry based upon ob­
servations made at the 6­m BTA telescope of the Special
Astrophysical Observatory in Zelenchuk. Precise speckle
measurements of binary stars carried out over many years
remain the main e#ective source of orbital parameters.
Most of our program objects are nearby low­mass main­
sequence stars discovered or measured by Hipparcos. The
purposes of this study are: (1) to select new pairs exhibit­
ing relatively fast orbital motion; (2) to derive the orbital
elements of the newly discovered pairs; (3) to obtain accu­
rate magnitude di#erences for the components of binary
and mutiple systems. Together with the Hipparcos par­
allaxes and di#erential magnitudes, the orbits allow the
estimation of mass sums of the components, their lumi­
nosities, and spectral types. The mass ratios, period, and
eccentricity distributions can be studied for our sample
stars.
2. Observations and results
The observations presented here were obtained in October
1999 using the new speckle camera developed in 1998
(Maksimov et al. 2003). The first results from the speckle
Send o#print requests to: Y. Balega, e­mail: balega@sao.ru
# Based on data collected at the Special Astrophysical
Observatory, Russia
program with this new instrument were reported in Balega
et al. (2002 hereafter B02).
The image motion­compensated seeing (FWHM)
during the observations was 1. ## 0 - 1. ## 5. Filters with
the following center wavelength/bandwidth were used:
545 nm/30nm (centre of the V ­band), 610nm/20nm (G),
800 nm/60nm (centre of the R­band). In the following,
they are designated as V # , G # , and R # .
Relative positions and magnitude di#erences of each
binary were derived from the ensemble averaged power
spectrum of speckle interferograms without compensation
of the atmospheric transfer function. Magnitude di#erence
between the components of a binary was estimated from
the contrast of the fringes measured at di#erent circle radii
of the power spectrum (see B02). The 180 # ambiguity of
the position angle # o was overcome by the Walker method
(Walker1981).
A double­slit pupil mask was used for direct calibration
of the measurements. In addititon, an independent cali­
bration was performed by observations of standard speckle
interferometric binaries with slow orbital motion.
Table 1 contains 132 measurements of 99 binary stars.
The entries for each system are presented in the same con­
densed format used in B02. Columns 1 through 3 list the
designation of the system: the Hipparcos number (ESA
1997), the name of the star or its catalog number, and
the discovery designation. The next columns contain the
epoch­2000 coordinates, the epoch of observations given
as the fractional Basselian year. They are followed by the
measured position angles # o given in degrees, angular dis­
tances # in mas, and their errors. The # o values have not

2 I. Balega et al.: Speckle interferometry of nearby multiple stars. II
been corrected for precession and are thus based upon the
equinox for the epoch of observation. Magnitude di#er­
ences #m, together with their errors, are listed in Columns
10 and 11. The final column gives the filter indication (as
central wavelength/FWHM in nm). Note that in the dis­
covery designation column the HDS (Hipparcos Double
Stars) numbers are included, following the upgraded daily
Washington Double Star Catalog, maintained at the US
Naval Observatory (Mason et al. 2003). The table lists 53
HDS entries, from which 16 have been observed by speckle
interferometry for the first time.
The measured angular separations in Table 1 range
from a minimum value of 16 mas for the close binary
HR 233 to 1859mas for the components of HIP 103767. In
speckle interferometry an accuracy of the measurements is
a function of many parameters: seeing, stellar magnitude,
magnitude di#erence, angular separation, etc. For most of
our data the typical value of the error is 0.5--2 mas in #
and 0.2--0.5 # in # o . This corresponds to the relative error
of the vector measurements in the range 0.1--2%; however,
in some cases of very close pairs, the error can reach 10%
(see e.g. HIP17932=CHR126 with # = 21 mas).
For 25 systems, indicated by an asterisk following their
# o values, the 180 # position angle ambiguity was not re­
solved.
111 magnitude di#erences for 92 binaries are given in
Table 1. The mean­square errors of #m measurements
vary widely from 0.01 m to 0.75 m , corresponding to dif­
ferent conditions of observation. In 12 cases, indicated by
colons, the #m measurements are uncertain, while for 7
pairs no #m value is given. In all these cases, except #
Aur, the binaries were too wide to fit the entrance window
of the detector.
Measurements of 6 triple systems are listed in Table 2.
For all the systems the angle # is given starting at the
position of the brighter component. To avoid possible
confusion in the components' identification, we desig­
nate them as A,B,C, according to their relative bright­
ness. Additional components to known binaries were dis­
covered in HIP 8533 and HIP 25354. The reconstructed
geometry and di#erential magnitudes of HIP 8533 are
shown in Fig.1. A third companion close to the primary
star is also suspected in the M2­type binary HIP 39402.
However, this result needs confirmation. No estimation
of the magnitude di#erence was made for this system.
Specific notes concerning the measured triple systems are
given in Subsection 2.1. The close spectroscopic subsys­
tem BAG 15 (B02) in the triple system HIP 111805 was
not resolved during the 1999 run; therefore, it is given
as a Table 1 entry. Three triples, ADS 14749, ADS 16214,
and ADS 16904, with early spectral type components were
included in the program as speckle interferometry calibra­
tion targets.
For 32 Hipparcos pairs absolute magnitudes and spec­
tral types of the components were estimated using our
#m measurements, Hipparcos parallaxes, and Hipparcos
median magnitudes Hp. Spectral types for the luminos­
ity class V were taken from (Lang 1992). The results are
=0.21
Dm
=0.21
Dm
=0.42
Dm
A
C
B
N
E
0.05
Fig. 1. Geometry of the triple system HIP 8533. The size of the
circles corresponds to relative brightness of the components.
presented in Table 3. For three pairs (HIP: 93119, 94960,
and 103067) the absolute magnitudes do not correspond
to (B -V ) and (V - I) colors of main sequence stars. The
increased luminosity of these binaries can be caused by
the presence of a third companion or by the evolved sta­
tus of the companions. The values in Table 3, combined
with 63 values from the first paper of the program, give a
total of 95 absolute magnitudes and spectral types of the
components.
2.1. Notes to triple systems
HIP 8533. The system was included in the observ­
ing list as a component solution binaty of the Hipparcos
Catalogue (ESA 1997). Until then, there was only one
measurement of the star, by Muller (Worley & Douglass
1997), who resolved it as a binary (MLR 297) with #=300
mas and #m=0.8. We found the star to be a triple sys­
tem with a low level of hierarchy: the ratio between the
short and the long vector is 0.26. Based on the Hipparcos
parallax of the system, we define absolute magnitudes of
the three components: 5.8, 6.0, and 6.2, corresponding to
spectral types G8 and K0.
HIP 25354. A new triple star with high hierarchy. The
main component is a K8 star, while the secondary is a dou­
ble with M­type components. Because of large separation
between the A­star and the BC, the magnitude di#erences
for A­B or A­C cannot be measured with our camera.
HIP 39402. An additional component at a distance of
40 mas from the secondary is suspected in the system.
Magnitude di#erence is between 1.5 and 2 magnitudes.
HIP 101955. This observation confirms the fast or­
bital motion of the spectroscopic subsystem BAG 14.
Di#erential magnitudes and estimated absolute magni­
tudes coincide with the observations of the previous year.
HIP 116726. In B02 the measurement for CHR 149 was
erroneously given as for the AC component. The correct
entry is: CHR149=BC, # = 43.1 # ± 2.0 # .

I. Balega et al.: Speckle interferometry of nearby multiple stars. II 3
3. Summary
We continue the speckle study of binaries discovered by
Hipparcos and other nearby low­mass systems. The aim
is to select binaries with fast relative motion in order to
determine new orbits and to combine the Hipparcos paral­
laxes with the speckle interferometric #m measurements
to derive absolute magnitudes and spectral types of the
components.
The presented sample of stars includes 54 new
Hipparcos doubles with parallaxes above 10 mas and sep­
arations of less than # 1 ## . From these, 17 entries have
been observed in 1999 by speckle interferometry for the
first time. Two new triple systems were discovered among
the objects of the program: HIP 8533 and HIP 25354. For
32 new Hipparcos pairs, absolute magnitudes and spec­
tral types of components were derived from our #m mea­
surements and Hipparcos parallaxes under the assumption
that the components are the main­sequence stars.
Acknowledgements. This research has made use of the
SIMBAD database, operated at CDS, Strasbourg, France,
and the Washington Double Star Catalog of the US Naval
Observatory. The speckle interferometry program at the 6­m
telescope has been supported by the Russian Foundation for
Basic Research through grant No. 01­02­16563a. Additional
support for this work was provided by the Russian Federal
Program Astronomia through contract No. 40.022.1.1.1101.
References
Balega, I.I., Balega, Y.Y., Hofmann, K.­H., et al. 2002, A&A,
385, 87
ESA 1997, The Hipparcos and Tycho Catalogues, ESA SP­1200
Lang, K.R. 1992, Astrophysical Data: Planet and Stars.
(Springer­Verlag, NY)
Maksimov, A.F., Balega, Y.Y., Beckmann, U., Weigelt, G.,
Pluzhnik, E.A. 2003, Bull. SAO, 56, 25
Mason, B.D., Wyco#, G.L., Hartkopf, W.I. 2003,
http://ad.usno.navy.mil/wds
Walker, J.G. 1981, Opt. Acta, 28, 735
Worley, C.E., Douglass, G.G. 1997, A&AS, 125, 523

4 I. Balega et al.: Speckle interferometry of nearby multiple stars. II
Table 1. Binary star measurements
HIP Name/ Discoverer Coord. Epoch # # # # # ## #m ##m Filter
Catalog No. designation 2000 1999.0+ mas mas
823 HDS 23 00101+3825 .8155 295.4* 0.3 172.7 0.8 0.22 0.14 R #
1055 BD +19 # 020 HDS 29 00132+2023 .8156 172.4 0.2 578.7 0.7 1.15 0.03 R #
1233 ADS 197 A 1256 00153+4412 .8212 222.8* 0.9 37.7 0.6 0.28 0.12 G #
1987 HD 2057 HDS 56 00251+4803 .8211 76.0 1.0 117.5 2.0 2.39 0.09 R #
3361 BD +12 # 081 HDS 93 00428+1249 .8156 98.6 0.3 220.3 0.8 1.16 0.03 R #
3951 HR 233 MCA 2 00507+6415 .8210 273.0* 1.5 16.0 0.4 1.08 0.08 G #
4267 ADS 746 STT 20 00546+1911 .8129 193.7 0.2 518.0 0.4 1.03 0.03 G #
4809 HD 6009 HDS 134 01017+2518 .8128 49.5* 0.3 88.5 0.3 0.19 0.04 G #
4849 GJ 3071 HDS 135 01024+0504 .8129 6.6 0.3 305.4 0.8 1.66 0.05 G #
4990 ADS 873 HO 213 01040+3528 .8129 109.0 0.2 299.6 0.5 0.65 0.07 G #
.8129 109.2 0.2 298.6 0.5 0.71 0.05 R #
.8129 108.8 0.2 298.6 0.4 0.58 0.06 V #
.8129 108.9 0.2 299.0 0.4 0.57 0.06 G #
.8155 109.3 0.2 299.1 0.6 0.65 0.04 R #
.8155 109.1 0.2 297.8 0.4 0.53 0.02 V #
.8155 109.3 0.2 298.4 0.3 0.53 0.02 G #
5531 HD 6840 HDS 155 01108+6747 .8211 180.4 0.3 121.2 0.4 0.75 0.03 G #
6060 ADS 1040 STF 102 01178+4901 .8209 275.0 0.2 476.9 0.6 0.89 0.04 V #
.8209 274.7 0.4 478.0 3.0 0.82 0.05 G #
.8212 275.5 0.2 476.0 0.8 0.90 0.03 R #
6694 BD+12 # 0176 HEI 305 01260+1315 .8156 115.8* 0.2 476.1 0.5 0.14 0.09 R #
6730 HDS 188 01267+1123 .8156 183.1* 0.2 704.0 1.0 0.15 0.19 R #
7338 HDS 211 01345+7804 .8179 288.1 0.6 136.0 2.0 2.28 0.04 R #
7397 HDS 213 01354+1126 .8157 39.9* 1.7 25.1 0.8 0.00 0.72 R #
10438 HR 640 MCA 6 02145+6631 .8210 78.4 0.3 94.6 0.3 1.27 0.02 G #
11253 HD 14874 HDS 314 02249+3039 .8130 283.9 0.3 351.0 2.0 2.57 0.06 G #
11352 HD 15013 HDS 318 02262+3428 .8130 228.3 0.3 96.5 0.4 0.16 0.05 G #
12153 HR 763 MCA 7 02366+1227 .8130 43.0* 0.4 29.7 0.2 0.08 0.09 G #
12640 HR 793 BLA 1 02424+2001 .8130 281.2 0.3 44.7 0.2 0.46 0.02 V #
13117 HDS 366 02487+0002 .8212 38.6 0.4 1553.0 8.0 R #
14075 HD 18774 HDS 385 03014+0615 .8184 86.0* 0.5 55.0 0.5 0.17 0.16 V #
14230 HD 18940 HDS 389 03035+2304 .8131 335.6 1.1 44.9 0.9 1.74 0.03 V #
14524 GJ 3202 HDS 396 03076­0358 .8185 162.5* 0.2 363.8 0.9 0.14 0.12 R #
14669 GJ 125 HDS 404 03095+4544 .8186 8.6 0.2 509.4 0.7 1.72 0.02 R #
15368 HDS 414 03181+0803 .8185 308.4 0.2 910.0 2.0 1.06: 0.14 R #
15597 HD 20716 HDS 418 03209+2031 .8212 340.1 0.3 589.9 3.0 3.70: 0.20 G #
15737 HD 20893 HDS 423 03228+2045 .8131 291.9 0.3 464.0 2.0 G #
16042 HD 21242 CHR 9 03266+2843 .8185 41.0* 3.8 42.0 3.0 2.77 0.13 V #
17932 HR 1176 CHR 126 03501+4458 .8214 72.3* 0.5 21.0 2.0 1.37 0.08 V #
18089 HR 1199 Kui 15 03520+0632 .8186 207.5 0.2 737.5 0.4 0.48: 0.02 R #
.8186 207.5 0.2 738.3 0.4 G #
.8187 207.4 0.2 738.9 0.4 V #
.8213 207.6 0.2 738.9 0.4 G #
.8213 207.5 0.2 739.2 0.4 V #
HD 25811 BAG 4 04063+1952 .8185 259.4* 0.4 68.1 0.5 0.18 0.12 G #
.8213 258.9* 0.4 68.3 0.4 0.23 0.27 V #
19472 HD 285465 HEI 35 04102+1722 .8185 205.6 0.7 60.4 0.8 1.29 0.04 G #
19591 HD 284163 CHR 14 04119+2338 .8186 178.3 0.2 266.7 0.6 1.32 0.01 R #
20227 HD 27323 HDS 555 04201+3108 .8187 29.1 0.5 324.0 3.0 3.60 0.10 G #
20553 HD 27836 HDS 564 04242+1445 .8187 261.2 0.4 189.0 2.0 2.65 0.06 G #
20605 HDS 566 04248+1552 .8159 1.2 0.2 449.0 1.0 0.31 0.14 R #
20679 HD 27990 COU 2682 04258+1800 .8188 270.2 0.3 137.7 0.5 0.83 0.02 R #
20745 HD 286798 WOR 15 04268+1240 .8160 42.6 0.3 209.3 0.7 0.22 0.08 R #
20777 DF Tau THB 1 04271+2542 .8188 91.9 0.6 100.0 1.0 0.23 0.11 R #
20895 HDS 576 04287+2613 .8160 125.4 0.4 167.7 0.9 0.17 0.09 R #
21092 HDS 585 04312+0157 .8187 272.8 0.4 304.0 2.0 0.89 0.04 R #

I. Balega et al.: Speckle interferometry of nearby multiple stars. II 5
Table 1. (continued)
HIP Name/ Discoverer Coord. Epoch # # # # # ## #m ##m Filter
Catalog No. designation 2000 1999.0+ mas mas
21280 HD 285931 CHR 17 04340+1510 .8188 216.6 0.3 140.6 0.4 1.22 0.02 G #
.8188 216.4 0.3 140.7 0.5 1.23 0.02 G #
.8214 216.6 0.4 141.2 0.7 1.38 0.05 V #
22550 ADS 3475 BU 883 04512+1104 .8159 79.1* 0.2 230.2 0.4 0.33 0.09 R #
23317 HDS 650 05009+6107 .8160 339.2 0.2 347.3 0.8 1.50 0.03 R #
23418 HDS 654 05020+0959 .8160 162.0 0.2 1077.3 0.9 0.90: 0.07 R #
23699 HD 32641 STT 97 05056+2304 .8161 150.3 0.2 360.1 0.4 1.09 0.02 R #
24608 # Aur ANG 1 05167+4600 .8182 50.1 0.4 55.5 0.4 V #
26220 # Ori A PTR 1 05353­0523 .8189 175.1* 0.9 212.0 4.0 3.23 0.75 V #
26221 # Ori C WGT 1 05353­0523 .8189 33.5* 1.9 42.0 2.0 1.03 0.11 G #
28832 ADS 4660 A 1951 06052+0708 .8135 42.8 0.3 448.0 2.0 R #
.8135 42.6 0.3 449.0 2.0 G #
.8135 42.6 0.3 449.0 2.0 V #
29269 HD 39861 HDS 841 06102+8131 .8161 196.4 0.2 647.8 0.6 1.40 0.03 V #
30272 ADS 4950 STF 881 06221+5922 .8216 140.7 0.2 673.7 0.6 1.29: 0.02 V #
34524 HD 54322 CHR 216 07092+1903 .8161 325.3 0.4 145.3 0.9 1.89 0.03 V #
39402 HDS 1149 08033+5251 8217 284.1 0.8 133.0 2.0 0.27 0.19 R #
40167 ADS 6650 STF 1196 08122+1739 .8162 86.6 0.2 821.9 0.5 V #
40818 HR 3269 FIN 346 08198+0357 .8190 63.6 0.2 255.8 0.3 0.47 0.04 V #
.8190 63.7 0.2 256.3 0.2 0.37 0.02 G #
.8190 63.7 0.2 257.0 0.5 R #
43861 HD 76261 HDS 1291 08561+3626 .8216 328.6* 0.3 765.0 3.0 3.11: 0.19 V #
43948 GJ 330 HDS 1296 08571+1139 .8162 222.4 0.2 523.7 0.7 1.41 0.03 R #
44471 ADS 7158 A 1585 09036+4709 .8217 27.6* 0.5 43.0 0.4 0.28 0.31 V #
44955 GJ 336 COU 1561 09095+3250 .8162 206.2 0.2 822.6 0.8 1.16: 0.04 R #
46199 HD 81105 HDS 1353 09252+4606 .8216 326.9 0.6 264.0 3.0 2.45 0.11 V #
60444 GJ 3722 HDS 1745 12236+6711 .8217 171.4* 1.4 88.0 3.0 0.25 0.26 R #
93119 WOR 26 18582+7519 .8178 151.7* 0.3 167.3 0.5 0.17 0.08 R #
94076 HR 7272 A CHR 84 19091+3436 .8205 165.9 0.5 89.8 0.7 2.01 0.05 V #
94679 ADS 12239 STT 371 19159+2727 .8204 159.9 0.2 884.4 0.5 0.56: 0.02 R #
.8204 160.0 0.2 885.2 0.4 0.65: 0.02 G #
.8204 160.1 0.2 883.3 0.6 0.72: 0.02 V #
94720 ADS 12248 CHR 85 19164+1433 .8205 217.7 0.6 51.5 0.6 1.42 0.05 V #
94960 HD 181148 HDS 2734 Aa 19194­0136 .8178 193.9 0.2 478.7 0.6 0.36 0.04 R #
95178 HD 183678 HDS 2740 19218+7708 .8181 355.7 0.3 442.0 3.0 3.18 0.09 G #
95299 HD 182085 HDS 2745 19233­0635 .8205 27.2 0.3 1069.0 4.0 3.09: 0.22 R #
95995 GJ 762.1 MCA 56 19311+5835 .8179 204.1 0.2 85.8 0.2 0.27 0.04 G #
96656 GJ 765.2 MLR 224 19391+7625 .8128 348.3 2.3 46.0 2.0 0.76 0.08 G #
97496 # Sge AGC 11 19490+1909 .8150 140.9 0.2 136.3 0.2 V #
.8150 140.7 0.2 136.5 0.3 G #
.8150 140.5 0.2 136.4 0.3 0.39 0.35 R #
103067 BD+42 # 3895 COU 2542 20530+4258 .8151 94.2 0.2 246.9 0.5 0.81 0.03 R #
103502 HDS 2989 20582+4011 .8151 149.5 0.2 279.2 0.6 0.96 0.02 R #
103767 HD 200406 HDS 2997 21016+4730 .8180 234.0 0.2 1859.0 3.0 G #
103810 ADS 14575 STF 2751 21021+5640 .8179 354.3 0.2 1624.5 0.9 V #
.8179 354.5 0.2 1624.8 0.9 G #
.8179 354.7 0.2 1625.4 0.8 R #
104075 HD 200746 HDS 3004 21051+0757 .8207 340.5 0.5 323.0 3.0 3.25 0.16 G #
104383 BD­05 # 5480 HDS 3013 21088­0426 .8178 287.5 0.2 302.2 0.5 1.67 0.04 R #
104581 BD+16 # 4472 HEI 187 21111+1704 .8151 257.0 0.2 1114.0 1.0 0.98: 0.04 R #

6 I. Balega et al.: Speckle interferometry of nearby multiple stars. II
Table 1. (continued)
HIP Name/ Discoverer Coord. Epoch # # # # # ## #m ##m Filter
Catalog No. designation 2000 1999.0+ mas mas
105187 BD+65 # 1572 HDS 3032 21185+6613 .8180 143.8 0.2 752.1 0.7 0.93 0.03 R #
105371 HD 203220 HDS 3038 21206+1310 .8207 305.8 0.3 215.0 1.0 2.45 0.06 G #
106394 HD 205142 HDS 3065 21330+2408 .8208 244.8 0.2 531.0 2.0 2.45 0.05 G #
106972 GJ 4210 HDS 3083 21399+2737 .8152 77.9 0.6 105.0 2.0 1.23 0.03 R #
107181 HDS 3092 21426+0233 .8152 57.4 0.3 254.0 1.0 1.05 0.05 R #
108917 # Cep MCA 69 22038+6438 .8127 78.4 0.5 66.7 0.5 1.47 0.03 V #
109281 HD 210211 HDS 3145 22083+2409 .8208 354.4 0.3 92.9 0.3 0.57 0.04 G #
109951 HD 211276 HDS 3158 22161­0705 .8152 70.5 0.3 297.1 0.8 1.87 0.04 V #
111685 GJ 4287 HDS 3211 22375+3923 .8153 17.5 0.2 272.1 0.5 1.43 0.03 R #
111805 ADS 16138 HO 295 22388+4419 .8208 150.2 0.2 190.6 0.3 0.31 0.04 G #
112422 BD +32 # 4510 HDS 3233 Aa 22463+3319 .8154 102.1 0.3 232.0 2.0 1.12 0.03 R #
112695 HD 216027 HDS 3241 22493+1517 .8208 16.9* 0.7 92.9 0.3 2.29 0.08 V #
113852 HD 217944 HDS 3285 23034+5834 .8210 117.2* 0.6 380.0 4.0 3.02 0.15 G #
114576 ADS 16591 A 2298 23126+0241 .8209 116.2 0.2 222.4 0.4 0.42 0.07 V #
114922 GJ 893.4 HDS 3316 23167+1937 .8153 46.2 0.4 106.8 0.6 0.16 0.09 R #
114927 BD+33 # 4679 HDS 3315 23167+3441 .8154 222.9* 0.5 96.5 0.8 0.37 0.07 R #
.8154 222.8* 0.5 96.3 0.8 0.26 0.09 R #
115666 ADS 16748 HO 489 23260+2742 .8153 224.2 0.2 526.0 1.0 0.33 0.06 V #
.8206 224.1 0.2 525.4 0.4 0.36 0.07 G #
.8206 224.6 0.2 526.4 0.4 0.88 0.04 R #
.8207 224.0 0.2 524.7 0.7 0.29 0.06 V #
118287 ADS 17151 A 1498 23595+5441 .8127 87.2 0.4 380.0 3.0 V #
.8127 86.5 0.3 379.0 2.0 G #
.8181 86.5 0.2 377.1 0.5 0.34 0.03 V #
.8181 86.5 0.2 377.8 0.6 0.58 0.03 G #
.8181 86.3 0.2 377.9 0.6 R #
Table 2. Triple star measurements
HIP Name/ Discoverer Coord. Epoch # # # # # ## #m ##m Filter
Catalog No. designation 2000 1999.0+ mas mas
8533 AB 01500+7456 .8128 290.6 3.5 57.2 3.6 0.21 0.06 R #
AC MLR 297 175.0 1.2 181.9 3.6 0.42 0.06
BC 161.0 1.2 212.9 4.2 0.21 0.05
25354 AB HDS 711 05253+6511 .8160 232.7 1.0 1441.9 23.7 R #
AC 235.6 0.8 1289.5 17.9
BC 29.6 3.3 167.6 9.6 0.47 0.30 R #
101955 AB KUI 99 20396+0458 .8206 131.3 0.2 299.3 0.8 0.94 0.03 G #
AC BAG 14 105.7 0.3 164.2 0.7 1.14 0.03
BC 336.5 0.4 167.1 1.1 0.20 0.02
104642 AB ADS 14749 21118+5959 .8125 213.3 0.2 1033.9 1.0 G #
AC MCA 67 148.6* 5.5 25.0 2.5 0.56 0.05
BC 34.5 0.3 1023.4 2.8
AB .8126 213.4 0.2 1030.3 1.4 V #
AC 146.8* 4.1 28.4 2.1 0.60 0.04
BC 34.8 0.2 1019.3 2.5
AB .8126 213.1 0.2 1032.9 1.2 R #
AC 145.6* 6.3 24.3 2.7 0.42 0.07
BC 34.3 0.3 1023.8 3.6
112170 AB ADS 16214 22431+4710 .8209 301.0 0.2 493 .1 0.5 0.65 0.04 G #
AC 311.1 0.2 498.6 1.2 1.49 0.04
BC HU 91 32.4 0.8 87.7 1.2 0.84 0.02 G #
116726 AB ADS 16904 23393+4543 .8212 150.8 0.3 242.2 1.2 0.13 0.06 V #
AC 145.0 0.8 227.6 3.2 1.00 0.05
BC CHR 149 26.2 6.7 27.7 3.3 0.86 0.04

I. Balega et al.: Speckle interferometry of nearby multiple stars. II 7
Table 3. Absolute magnitudes and spectral types of binary star components
HIP MA MB Filter SpA SpB HIP MA MB Filter SpA SpB
1987 4.6 7.0 R # G2 K4 43948 9.8 11.2 R # M2 M4
6694 7.6 7.7 R # K6 K6 44955 8.7 9.9 R # M0 M2
7397 7.8 7.8 R # K6 K6 46199 7.3 9.7 V # K5 M2
15368 7.7 8.7 R # K6 M0 60444 11.4 11.6 R # M4 M4
19472 6.9 8.2 G # K4 K7 93119 7.7 7.9 R # K6 K6
19591 7.0 8.3 R # K4 K8 94960 7.1 7.4 R # K4 K5
20227 5.2 8.8 G # G5 M0 95178 6.2 9.4 G # K1 M1
20553 4.5 7.2 G # G1 K4 95299 7.3 10.4 R # K5 M3
20605 9.3 9.6 R # M1 M1 103067 5.5 6.3 R # G8 K2
20679 6.2 7.0 R # K1 K4 103502 8.3 9.2 R # K7 M1
20745 8.5 8.7 R # K8 M0 104075 4.9 8.2 G # G4 K7
21092 9.4 10.3 R # M1 M3 104383 7.6 9.3 R # K6 M1
29269 4.6 6.0 V # G1 K0 104581 5.7 6.7 R # G9 K3
34524 4.8 6.7 V # G3 K3 105187 6.4 7.3 R # K2 K5
39402 9.6 9.8 R # M1 M2 109951 4.9 6.8 V # G4 K3
43861 5.0 8.2 V # G5 K7 112422 6.6 7.7 R # K3 K6