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The Astronomical Journal, 132:994 - 998, 2006 September
# 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A.

SPECKLE MEASUREMENTS AND DIFFERENTIAL PHOTOMETRY OF VISUAL BINARIES WITH THE 6 METER TELESCOPE OF THE SPECIAL ASTROPHYSICAL OBSERVATORY
? Jose A. Docobo,1 Vakhtang S. Tamazian,1 Yuri Y. Balega,2 and Norair D. Melikian
Received 2006 May 8; accepted 2006 May 17
3, 4

ABSTRACT Results of speckle measurements and differential photometry carried out with the 6 m telescope of the Special Astrophysical Observatory ( Russia) at the end of 2004 are presented. One new (COU 1569) and four improved orbits (ADS 440AC, ADS 1729, ADS 5726, and COU 1897), as well as their dynamical mass estimates, are reported. Key words: binaries: visual -- stars: fundamental parameters -- techniques: photometric

1. INTRODUCTION This paper is the next in a series dedicated to the speckle measurements of visual binaries carried out in the recent years ? ? at the Observatorio Astronomico RamonMar?a Aller (OARMA) i of the University of Santiago de Compostela ( Docobo et al. 2001c, 2004). The results of speckle measurements made with the 6 m telescope of the Special Astrophysical Observatory (SAO) ( Russia) are reported. The objective of these studies is to obtain orbital parameters and dynamical and individual masses for mostly ( but not only) late-type visual binaries. Yet a close follow-up of some flare- and UV Ceti - type variables is being made, with the aim of revealing the possible duplicity of these stars. Apart from this, in the known binary systems a possible relationship between components' activity and their position on the orbit is studied. 2. SPECKLE OBSERVATIONS The speckle interferometric observations were performed with the speckle camera and an intensified 1280 ; 1024 pixel CCD coupled with an S25 photocathode. Under good seeing conditions, this system allows us to observe binary components as faint as 15.0 mag in optical wavelengths with a dynamic range of about 5.0 mag. The diffraction-limited resolution is about 22 mas. The image motion-compensated seeing ( FWHM ) during the observations was 1B0-1B5. The relative position and magnitude difference Ám of each binary was derived from the ensemble averaged power spectrum. A double-slit pupil mask and interferometric binaries with slow orbital motion were used for calibration. More details regarding the observation and reduction procedure can be found in Balega et al. (2002) and remained essentially unchanged. In total, we have obtained 33 measurements for 32 systems, out of which 9 were unresolved. The observations are listed in Table 1, the columns of which list (1) the Washington Double Star Catalog ( WDS) number ( Mason et al. 2003), (2) the ADS number (Aitken & Doolittle 1932) or other designation, (3) the observation epoch ( in fraction of the Besselian year), (4) the position
1 ? ? Observatorio Astronomico Ramon Maria Aller, Universidade de Santiago ? de Compostela, Avenida das Ciencias s/n, 15782 Santiago de Compostela, Spain; oadoco@usc.es, oatamaz@usc.es. 2 Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai-Cherkesia 369167, Russia; balega@sao.ru. 3 Byurakan Astrophysical Observatory, Aragatsotn Region, 378433 Byurakan, Armenia; nmelikia@bao.sci.am. 4 Isaac Newton Institute of Chile, Armenian Branch, 378433 Byurakan, Armenia.

angle ( in degrees) with its corresponding error, (5) the separation (in arcseconds) with its corresponding error, (6) the magnitude difference between components and the corresponding error of photometry, (7, 8) and the central wavelength and bandwidth of the filter used (in nanometers). 3. NEW AND IMPROVED ORBITS AND DYNAMICAL MASSES The first orbit for COU 1569 and improved orbits for ADS 440AC, ADS 1729, ADS 5726, and COU 1897 are presented. They are calculated using the method of Docobo (1985), the essence of which is briefly summarized in Docobo et al. (2000) and Tamazian et al. (2002). The apparent orbits of these binaries are shown in Figure 1. Except for ADS 440AC, none of the systems are included in the Multiple Star Catalog ( Tokovinin 1997) and /or the Ninth Catalogue of Spectroscopic Binary Orbits ( Pourbaix et al. 2004). At the same time, since all components of these binaries are mainsequence stars, a well-known Baize-Romani algorithm ( Baize & Romani 1946; Heintz 1978, p. 62) can be applied in order to obtain their dynamical parallaxes. In Table 1 the measurements previously used by the authors for orbit calculation are marked with an asterisk. These orbits were announced in IAU Commission 26 Information Circulars ( ICs) 156, 157, and 158, and some of them have already been published by Tamazian et al. (2005) and Tamazian & Docobo (2006). The new orbit for ADS 440AC was submitted for publication to IC 159. The measurements used to calculate the new orbits reported in this work are marked with two asterisks. Table 2 gives the residuals of our observations with those orbits that do not need to be recalculated or are still in the process of calculation, and Table 3 contains orbital elements, total masses, and the Hipparcos ( Perryman et al. 1997) and dynamical parallaxes of the newly calculated binaries. We report in Table 4 the weighted rms of the observational residuals (O À C ) for our newly calculated orbits, as well as for previously known orbits taken from the USNO ( Hartkopf & Mason 2006) and OARMA ( Docobo et al. 2001b) catalogs, using the observation-weighting rules described in Docobo & Ling (2003). Finally, Table 5 contains the ephemerides for the newly calculated orbits. In the following, comments on individual systems are given. ADS 440AC (=MCY 1): This system consists of the M-type dwarf components A and C of Gl 22 (ADS 440). It was first resolved in 1989 by near-infrared speckle interferometry with 994


MEASUREMENTS OF VISUAL BINARIES WITH SAO

995

Fig. 1.--Apparent orbits of the newly calculated binaries (the scale on both axes is in arcseconds). Each measurement is connected to its predicted position by an O À C line. The dashed line passing through the primary star represents the line of nodes. The circles and stars represent visual and speckle measurements, respectively, and the arrow shows the direction of the orbital motion.

the 2.3 m telescope of the Steward Observatory located on Kitt Peak ( McCarthy et al. 1991). An astrometric orbit with a period of 15.95 yr was first calculated by Hershey (1973) and then improved by Heintz (1993) on the basis of a larger set of astrometric plates obtained with the Sproul 24 inch (0.6 m) refractor. Using the infrared speckle interferometry data obtained by J. Woitas with the 3.5 m telescope of Calar Alto and covering an orbital arc of more than 300 , Docobo et al. (2002) computed an improved solution with a period of 16.12 yr. Our latest observation with the 6 m telescope indicates that the period is somewhat lower, and it would be reasonable to recalculate the orbit. We obtain a new 15.64 yr solution (see Table 3), which, however, does not affect the previous value of its total mass, 0.59 M ( Woitas et al. 2003). If a seemingly erroneous one-dimensional measurement of this pair at the epoch 1991.7201 ( Woitas et al. 2003) is removed,

the rms of residuals in position angle and separation is clearly improved (see Table 4). ADS 1729 (=A2013): This binary star was discovered in 1909 by Aitken (1909b) with the 36 inch (0.9 m) telescope of the Lick Observatory. Since then, various orbits have been calculated for this star, all with a period close to 35 yr. An exception is the orbit of Costa & Docobo (1983) with a period of 73 yr based on the possibility of rotating some measurements 180 . Our measurement has been performed exactly at the time of minimal separation, thus allowing us to improve (especially in position angle) the previous orbit of Heintz (1994), whose predicted position was deviating by 17N5 with regard to the latest speckle datum. As is seen from Table 3, the Hipparcos parallax coincides with the dynamical parallax to within a 1 margin. The total mass of the system (1.8 M ) is close to that expected for a pair of K5 dwarfs.


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DOCOBO ET AL.
TABLE 1 Spec kle Measurements Filter (nm) WDS (1)
a

ADS or Other Designation (2) HEI 299 ADS 328 ADS 440AC ADS 701 COU 750 ADS 1729 ADS 1865 WOR 2 ADS 2028 COU 1511 ADS 2271 ADS 2406 COU 1688 ADS 2799 COU 567 ADS 3323 COU 2031 ADS 5726 AR Mon AR Mon ADS 6828 ST 8AB COU 1897 ADS 7158 R Leo KUI 44AB COU 1569 COU 169 AD Leo COU 292 SZ Uma COU 1905 R Vir

Epoch 2004.0+ (3) 0.99015 0.99019 0.99022 0.99026 0.99030 0.99042 0.99044 0.99033 0.99048 0.99051 0.99053 0.99056 0.99058 0.99060 0.99062 0.99067 0.99070 0.99106 0.99103 0.99107 0.99109 0.99111 0.99114 0.99116 0.99122 0.99124 0.99126 0.99131 0.99130 0.99134 0.99138 0.99141 0.99144

Æ (deg) (4) 2.7 Æ 1.8 87.4 Æ 0.4 28.8 Æ 0.5 197.3 Æ 0.3 24.8 Æ 0.4 148.6 Æ 1.1 207.5 Æ 0.5 100.0 Æ 0.4 270.9 Æ 0.5 64.1 Æ 0.5 163.1 Æ 0.4 Unres.b Unres. 164.5 Æ 0.8 176.0 Æ 0.8 77.7 Æ 1.2 221.1 Æ 3.5 162.6 Æ 0.4 Unres. Unres. 290.7 Æ 1.1 68.2 Æ 0.4 55.1 Æ 0.8 303.8 Æ 0.7 Unres. 254.3 Æ 0.6 69.8 Æ 0.6 343.3 Æ 0.3 Unres. 280.0 Æ 0.5 334.0 Æ 1.4 Unres. Unres.

Æ (arcsec) (5) 0.218 0.115 0.470 0.182 0.257 0.065 0.182 0.399 0.145 0.135 0.243 Æ Æ Æ Æ Æ Æ Æ Æ Æ Æ Æ .. . .. . Æ Æ Æ Æ Æ .. . .. . Æ Æ Æ Æ .. . Æ Æ Æ .. . Æ Æ .. . .. . 0.007 0.001 0.003 0.001 0.002 0.002 0.002 0.002 0.001 0.001 0.002

Ám Æ (mag) (6) Æ 0.30 Æ 0.10 Æ 0.20 Æ 0.13 Æ 0.07 Æ 0.10 Æ 0.09 Æ 0.10 Æ 0.05 Æ 0.04 Æ 0.03 . .. . .. 0.81 Æ 0.05 0.91 Æ 0.05 0.33 Æ 0.23 0.92 Æ 0.06 0.24 Æ 0.12 . .. . .. 0.0c 3.90 Æ 0.50 1.70 Æ 0.03 0.37 Æ 0.03 . .. 0.70 Æ 0.10 0.45 Æ 0.04 0.00 Æ 0.21 . .. 0.40 Æ 0.02 3.70 Æ 0.70 . .. . .. 1.80 0.83 2.40 0.0 0.40 0.17 0.11 0.55 1.20 0.75 1.53

kc (7) 800 545 800 545 800 800 800 800 545 545 545 545 545 545 545 545 545 800 800 545 545 800 545 545 545 545 545 800 800 545 800 800 800

Ák (8) 110 30 110 30 110 110 110 110 30 30 30 30 30 30 30 30 30 110 110 30 30 110 30 30 30 30 30 110 110 30 110 110 110

00155À1608 ................. 00243+5201Ã ................. 00321+6715ÃÃ ............... 00516+2237Ã ................. 01450+2703Ã ................. 02159+0638ÃÃ ............... 02278+0426 .................. 02288+3215Ã ................. 02399+0009 .................. 02415+4053 .................. 03006+4753Ã ................. 03128À0112.................. 03321+4340 .................. 03503+2535Ã ................. 04298+1741 .................. 04364+3413Ã ................. 04464+4221Ã ................. 07036+3941ÃÃ ............... 07208À0516 ................. 07208À0516 ................. 08285À0231Ã ................ 08427+0935 .................. 08585+3548ÃÃ ............... 09036+4709 .................. 09476+1126 .................. 09498+2111Ã ................. 10059+3412ÃÃ ............... 10140+2227 .................. 10200+1950 .................. 10269+1931 .................. 11200+6551 .................. 11294+4205 .................. 12385+0659 ..................
a b c

0.050 0.056 0.100 0.022 0.245

0.002 0.002 0.003 0.003 0.001

0.025 1.236 0.108 0.164 0.041 0.134 0.550 0.081 0.132

0.003 0.005 0.002 0.002 0.002 0.002 0.002 0.002 0.004

Double asterisks (ÃÃ ) denote orbits revised in this work, and single asterisks (Ã ) denote orbits revised in other papers. Pair unresolved. Bad power spectrum.

ADS 5726 (=A1959): This is a pair of red dwarfs discovered by Aitken (1909a), the orbit of which has completed various revolutions since its discovery; there are, sensibly, a lower number of observations in comparison with the pair A2013. The orbit of Seymour & Mason (2000) gives small but systematic residuals since 1991. The rms in position angle, at least, can be improved with a practically circular orbit.

Both Hipparcos and dynamical parallaxes coincide to within a 1 margin, while the total mass is slightly larger than that expected for a pair of M dwarfs. COU 1897: Both this and the following binary were discovered by P. Couteau with the 50 cm refractor of the Nice Observatory. Only one provisional orbit with a period of 104 yr has been obtained for this system (Couteau 1999), but our latest

TABLE 2 Observational Re siduals w ith No R ec alculated Orbits Á (deg) À2.2 0.0 +0.7 À2.5 +0.8 +1.1 À2.4 +51.8a Á (arcsec) +0.008 À0.006 +0.004 À0.010 +0.002 À0.007 À0.004 +0.011

WDS 00155À1608 .............. 02278+0426 ............... 02399+0009 ............... 02415+4053 ............... 09036+4709 ............... 09036+4709 ............... 10140+2227 ............... 10269+1931 ...............
a

Reference Hershey & Taff (1998) Andrade (2001) Docobo & Ling (2001a) Hartkopf & Mason (2001) Barnaby et al. (2000) Hartkopf et al. (2000) Couteau (1999) Couteau (1997)

Orbit under revision (B. Mason 2006, private communication).


TABLE 3 Or bi ta l Ele me nt s Element P ( yr) ............................... T ....................................... e ........................................ a (arcsec) .......................... i (deg) ............................... (deg) ............................. ! (deg) ............................. ADS 440AC 15.64 2000.76 0.174 0.511 44.6 175.1 106.8 Æ Æ Æ Æ Æ Æ Æ 0.20 0.20 0.003 0.005 1.5 1.0 5.0 ADS 1729 34.66 2005.69 0.593 0.346 112.3 91.8 137.6 Æ Æ Æ Æ Æ Æ Æ 0.15 0.2 0.01 0.002 2.0 2.0 3.0 ADS 5726 31.85 1988.36 0.008 0.259 63.3 172.3 147.7 Æ Æ Æ Æ Æ Æ Æ 0.25 4.6 0.008 0.003 2.5 3.5 35 COU 1897 165.0 1985.8 0.334 0.255 61.1 168.1 2.3 Æ Æ Æ Æ Æ Æ Æ 10 2 0.02 0.009 2 5 15 COU 1569 117.0 1997.78 0.494 0.237 69.3 60.7 140.1 Æ Æ Æ Æ Æ Æ Æ 15 0.5 0.06 0.02 2 2 3

Hipparcos Parallax
Hip

(mas)......................... Total mass (M )...........

98.74 Æ 3.37 0.57 Æ 0.06

26.37 Æ 3.69 1.86 Æ 0.78 Dynamical Parallax

21.30 Æ 2.80 1.77 Æ 0.70

4.11 Æ 0.84 8.77 Æ 5.58

5.92 Æ 1.13 4.69 Æ 3.17



dyn

(mas)......................... Total mass (M )...........

89.33 Æ 1.5 0.77 Æ 0.05

29.41 Æ 0.9 1.34 Æ 0.14

22.13 Æ 1.1 1.58 Æ 0.24

4.92 Æ 0.5 5.11 Æ 1.76

6.69 Æ 0.5 3.25 Æ 1.38

TABLE 4 rms of (O À C ) R esidua ls rms (O À C ) (deg) 1.3 1.6 3.9 5.8 3.5 4.1 1.9 3.4 3.2 (O À C ) (arcsec) 0.011 0.024 0.031 0.036 0.020 0.020 0.005 0.008 0.008

Star ADS 440AC ............... ADS 1729 .................. ADS 5726 .................. COU 1897 .................. COU 1569 ..................
a

Orbit's Source This papera Woitas et al. (2003)a This paper Heintz (1994) This paper Seymour & Mason (2000) This paper Couteau (1999) This paper

Without the 1991.7201 measurement.

TABLE 5 Ephemerides ADS 440AC (deg) 71.8 95.2 116.8 135.2 151.1 165.8 181.2 200.1 228.0 270.1 (arcsec) 0.424 0.429 0.459 0.498 0.529 0.536 0.505 0.436 0.347 0.302 ADS 1729 (deg) 265.8 252.3 237.4 219.5 199.1 179.3 162.9 150.5 141.4 134.5 (arcsec) 0.165 0.166 0.153 0.140 0.135 0.144 0.163 0.190 0.219 0.251 ADS 5726 (deg) 181.7 187.7 194.8 204.0 216.6 234.4 257.9 282.6 302.6 316.9 (arcsec) 0.247 0.230 0.206 0.179 0.151 0.128 0.116 0.122 0.142 0.169 COU 1897 (deg) 247.2 252.9 258.5 263.9 269.1 274.0 278.6 282.9 286.9 290.6 (arcsec) 0.107 0.107 0.109 0.111 0.113 0.117 0.121 0.125 0.130 0.136 COU 1569 (deg) 255.9 259.0 262.2 265.7 269.3 273.3 277.6 282.2 287.3 292.7 (arcsec) 0.133 0.130 0.126 0.122 0.118 0.114 0.109 0.105 0.101 0.097

Epoch 2007.0......................... 2008.0......................... 2009.0......................... 2010.0......................... 2011.0 ......................... 2012.0......................... 2013.0......................... 2014.0......................... 2015.0......................... 2016.0.........................


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DOCOBO ET AL. 1997.271 (Couteau 1999) measurement is incompatible with our orbital solution. The dynamical mass of the system suffers strongly from the low relative accuracy of the Hipparcos parallax, so the comments regarding COU 1897 are completely valid in this case, too. Adopting a 1.9 M mass forthis systemoftwo G5 dwarfs, the corresponding parallax should be close to 8 mas. Further observations of this pair are welcome in order to adjust its preliminary orbit.

observation reveals that period should be larger. Apart from this, the provisional orbit demonstrates systematic (O À C ) residuals with observations since 1991. Due to a less than 10 mas parallax, its value measured by Hipparcos (4:11 Æ 0:84 mas) has a large uncertainty, although it coincides well with the obtained dynamical parallax of 4.9 mas. Such a large uncertainty is translated to the total mass of the system. A parallax of 4.8 mas would provide a total mass of 5.5 M , expected for a pair of A1 V components. COU 1569: We present the first orbit for this pair. While the number of observations is still small, three successful speckle measurements at the 1980s epochs 1984.0527 ( McAlister et al. 1987), 1984.3832 ( Hartkopf et al. 2000), and 1987.2637 ( McAlister et al. 1989) demonstrate that the star had at that time just passed the separation minimum. It was not resolved by Couteau at the epoch 1988.306 nor by Hipparcos in 1991.25. Currently, when the covered orbital arc surpasses 180 the components are at the relative maximum in separation. Couteau's

This paper was financed by the research project AYA 2004? 07003 of the Spanish Ministerio de Educacion y Ciencia. This research made use of the Washington Double Star Catalogs maintained at the US Naval Observatory and the SIDONIe ^ Database maintained at the Nice - Cote d'Azur Observatory (France).

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