
\documentclass[journal]{rmaa}

\usepackage{paralist}
\usepackage{psfrag,color}
\usepackage[latin1]{inputenc}


\title{Speckle Interferometry at the Observatorio\\ Astron\'omico Nacional. II}


\author{
V.~G. Orlov,
V.~V. Voitsekhovich,
J.~L. Rivera,
C.~A. Guerrero,
and F. Ortiz
\affil{Instituto de Astronom\'ia, Universidad Nacional Aut\'onoma de M\'exico, Mexico}}


\shortauthor{Orlov et al.}

\shorttitle{Speckle Interferometry at the Observatorio Astron\'omico Nacional. II}


\fulladdresses{
\item C.~A. Guerrero, V.~G. Orlov,  F. Ortiz,  J.~L. Rivera,  and V.~V. Voitsekhovich: Instituto de Astronom\'ia, Universidad Nacional Aut\'onoma de M\'exico, 
Apdo. Postal 70-264, Cd. Universitaria, 04510 M\'exico D. F., Mexico (cguerrero,~orlov,~fortiz,~jrivera,~voisteko@astroscu.unam.mx).}


\listofauthors{V.~G.~Orlov, V.~V.~Voitsekhovich, J.~L.~Rivera, C.~A.~Guerrero, \& F.~Ortiz}

\indexauthor{Orlov, V.~G.}
\indexauthor{Voitsekhovich, V.~V.}
\indexauthor{Rivera, J.~L.}
\indexauthor{Guerrero, C.~A.}
\indexauthor{Ortiz, F.}


\SetYear{2010}
\SetVolume{46}
\ReceivedDate{2010 March 27} 
\AcceptedDate{2010 May 27} 


\resumen{Presentamos mediciones interferom\'etricas de motas para estrellas binarias, obtenidas en junio de 2009 en el telescopio de 
1.5 m del Observatorio Astron\'omico Nacional en San Pedro M\'artir (M\'exico). Nuestros datos comprenden 189 mediciones de \'angulos 
de posici\'on y separaciones de 144 sistemas. Las separaciones angulares medidas abarcan desde $0\arcsec.16$ hasta $3\arcsec.64$. La 
magnitud m\'axima de la componente m\'as brillante es de 10.96. El error medio en las separaciones es de $0\arcsec.02$ y en los 
\'angulos de posición de $1.5\arcdeg$. Algunos \'angulos de posici\'on se determinaron con la ambig\"uedad usual de $180\arcdeg$.\medskip}


\abstract{We present speckle interferometric measurements of binary stars made during June of 2009 with the 1.5~m telescope of 
the Observatorio Astron\'omico Nacional at SPM (Mexico). The data contain 189 position angle and separation measures of 144 systems. 
The measured angular separations range from $0\arcsec.16$ to $3\arcsec.64$. The maximum magnitude of the brighter component is 
10.96. The mean error in separation is $0\arcsec.02$ and in the position angles $1.5\arcdeg$. Some of the position angles were 
determined with the usual $180\arcdeg$ ambiguity.\medskip}


\addkeyword{binaries: visual}
\addkeyword{stars: fundamental parameters}
\addkeyword{techniques: high angular resolution}
\addkeyword{techniques: interferometric}


\begin{document}

\maketitle


\section{Introduction}

In our previous paper (Orlov et al. 2009) we reported results of speckle observations of binary stars obtained at the 
1~m telescope of Observatorio Astron\'omico Nacional at Tonanzintla (OAN-Tonanzintla), Mexico. The telescope is located 
at a site with moderate seeing. As it is well known the resolution of speckle interferometry (SI) does not depend on seeing. 
However, the limiting magnitude of stars which can be resolved by SI does depend on seeing. The Instituto de Astronom\'ia 
has a total of four telescopes. Three of them are situated at Observatorio Astron\'omico Nacional at San Pedro M\'artir, 
Mexico (OAN-SPM).  The OAN-SPM is located in one of the best astronomical sites (\'Avila, Cruz-Gonz\'alez, \& Tapia 2003). Included at the 
SPM site are 3 telescopes: 84~cm, 1.5~m and 2.1~m.

In this paper we present results from four observing nights in June 2009. The observations were performed at the 1.5~m 
telescope of the OAN-SPM.


%%%%% FIGURA 1

\begin{figure}[!t]
\centering
\includegraphics[width=0.99\columnwidth]{vorlovfig1.eps}
\caption{The centered image of the binary star COU 1581. It was obtained by averaging 700 
previously centered speckle interferograms. The window is $6\arcsec.3 \times 6''.3$.}
\label{fig:linea1}
\vspace{0.3cm}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


\section{OBSERVATIONS}

The observations were performed at the 1.5~m telescope of the Observatorio Astron\'omico Nacional which is located at the 
San Pedro M\'artir (Mexico). For these observations we used the DRAGON equipment (Voitsekhovich et al. 2005), which was 
slightly modified to be able to record speckle interferograms (Orlov et al. 2007). During the observations we had good seeing 
conditions. We estimated that the seeing was between 0.7 to 1 arcsec. Unfortunately, aberrations introduced by the telescope had 
a larger effect. It can be clearly seen on a centered image of one of the stars (Figure~1). Aberrations of the 1.5~m mirror 
cannot be corrected because the telescope is not equipped with an active optics system.


%%%%% TABLA 1

\begin{table}[!b]
\vspace{0.25cm}
\centering
%\setlength{\tabnotewidth}{0.99\columnwidth}
\tablecols{5}
\setlength{\tabcolsep}{0.95\tabcolsep}
\caption{Distribution of pairs by their separations} 
\label{tab:Data1}
\footnotesize
\begin{tabular}{ccccc}
\toprule
$>1\arcsec.5$  & $1\arcsec.5-1\arcsec$  & $1\arcsec-0\arcsec.5$ & $0\arcsec.5-0\arcsec.25$ & $< 0\arcsec.25$ \\
\midrule
18             & 23                     & 38                    & 57                       & 12 \\
\bottomrule
\end{tabular}
%\vspace{0.4cm}
\end{table}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

\vspace{0.3cm}

After calibration we determine the Pixel Scale $=0.024\arcsec$/px and detector orientation. For calibration we used 40 wide 
pairs with very slow orbital motions and some of them with known orbital parameters.

During four nights of observations we made 189 measurements of 144 pairs. Most of observed binaries have separations less than 
$1\arcsec$. Table~1 shows how these 144 pairs are distributed  according to their separations.


%%%%%% FIGURA 2

\begin{figure}[!t]
\centering
\includegraphics[width=0.99\columnwidth]{vorlovfig2.eps}
\caption{Reconstructed ACF of the binary star COU 1581. Separation $= 0\arcsec.305$.}
\label{fig:linea2}
\vspace{0.4cm}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%%%%% FIGURA 3

\begin{figure}[!t]
\centering
\includegraphics[width=0.99\columnwidth]{vorlovfig3.eps}
\caption{Result of self-calibrating shift-and-add technique for the binary star COU 1581.}
\label{fig:linea3}
\vspace{0.3cm}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


\section{DATA PROCESSING and Results}

For each binary star, a typical observing procedure involved the accumulation of one set of 700 short exposure images 
on hard disk. One short exposure image consists of a two-dimensional $582 \times 584$ array of 8-bit numbers. The volume 
of one set on the hard disk is 226 MB. The data were processed by the algorithm which was explained in detail by Tokovinin, 
Mason, \& Hartkopf (2010). This algorithm permits derivation of the binary star parameters without using the reference star. 
The resulting autocorrelation function (ACF) of one binary star COU 1581 calculated by this algorithm is shown in Figure~2. 
The position of the secondary is calculated as the center of weight of values of the ACF in a region around the maximum value.


%%%%% TABLA 2

\begin{table*}[!t]
\vspace{0.1cm}
\centering
%\setlength{\tabnotewidth}{\columnwidth}
\tablecols{8}
%\setlength{\tabcolsep}{1.\tabcolsep}
\caption{Speckle measurements on the 1.5~m telescope} 
\label{tab:Data2}
\footnotesize
\begin{tabular}{clcccccl}
\toprule
WDS                         & \multicolumn{1}{c}{Disc.} & Date      & P.A   & Sep.     & P.A. Orb. & Sep. Orb. & \multicolumn{1}{c}{Reference} \\
$ (\alpha,\delta J2000.0) $ & \multicolumn{1}{c}{Name}  & Besselian & (deg) & (arcsec) & (deg)     & (arcsec)  &  \\
\midrule
12154+4008 & A  1999      & 2009.4326 & ~62.2 & 0.29 & ~40.9 & 0.53 & Seymour et al. 2002 \\
12182+2718 & HDS1733      & 2009.4410 & 241.9 & 0.32 &       &      &  \\
12244+4305 & STT 250      & 2009.4327 & 351.2 & 0.33 &       &      &  \\
12306+3431 & HDS1759      & 2009.4327 & 203.3 & 0.27 &       &      &  \\
12328+2301 & AG  179      & 2009.4327 & 142.0 & 0.99 &       &      &  \\
12510+3129 & HDS1804      & 2009.4300 & 256.8 & 0.75 &       &      &  \\
12510+3129 & HDS1804      & 2009.4327 & 257.2 & 0.75 &       &      &  \\
12575+2457 & COU 397      & 2009.4300 & ~60.6 & 0.68 &       &      &  \\
12575+2457 & COU 397      & 2009.4410 & ~60.6 & 0.68 &       &      &  \\
12575+2457 & COU 397      & 2009.4327 & ~61.1 & 0.69 &       &      &  \\
13004+3545 & HU 1141      & 2009.4327 & 343.5 & 0.49 &       &      &  \\
13037+2339 & STF1714      & 2009.4410 & 307.2 & 3.12 &       &      &  \\
13037+2339 & STF1714      & 2009.4327 & 307.2 & 3.13 &       &      &  \\
13063+2044 & HU  739      & 2009.4327 & 204.1 & 1.37 & 207.3 & 1.39 & Seymour et al. 2002 \\
13063+2044 & HU  739      & 2009.4410 & 204.1 & 1.37 &       &      &  \\
13091+2127 & HU  572      & 2009.4411 & 344.6 & 0.46 & ~10.1 & 0.35 & Zulevic 1969 \\
           &              &           &       &      & 105.5 & 0.52 & Baize 1981 \\
           &              &           &       &      & ~50.7 & 0.35 & Baize 1986 \\
13128+4030 & A  1606      & 2009.4328 & 195.9 & 1.29 &       &      &  \\
13128+4030 & A  1606      & 2009.4411 & 196.5 & 1.30 &       &      &  \\
13221+3952 & HDS1876      & 2009.4300 & ~88.9 & 0.26 &       &      &  \\
13225+4242 & COU1581      & 2009.4411 & 157.5 & 0.33 &       &      &  \\
13266+3235 & COU 787      & 2009.4300 & 147.4 & 0.34 &       &      &  \\
13280+3235 & A  1856      & 2009.4411 & 343.5 & 1.08 &       &      &  \\
13280+3235 & A  1856      & 2009.4328 & 343.7 & 1.07 &       &      &  \\
13305+3430 & A  1857      & 2009.4301 & 340.9 & 0.48 &       &      &  \\
13305+3430 & A  1857      & 2009.4328 & 341.4 & 0.47 &       &      &  \\
13348+4242 & HDS1908      & 2009.4411 & ~24.1 & 0.48 &       &      &  \\
13387+3823 & COU1429AB    & 2009.4411 & ~64.0 & 0.66 &       &      &  \\
13387+3823 & COU1429AB    & 2009.4301 & ~64.4 & 0.66 &       &      &  \\
13465+1545 & A  2063      & 2009.4411 & 136.9 & 0.23 &       &      &  \\
13465+1545 & A  2063      & 2009.4328 & 136.9 & 0.19 &       &      &  \\
13465+1545 & A  2063      & 2009.4301 & 137.4 & 0.25 &       &      &  \\
13509+3555 & COU1132      & 2009.4301 & 147.5 & 0.79 &       &      &  \\
13509+4422 & A  1613AB    & 2009.4328 & 259.9 & 3.08 &       &      &  \\
13571+3426 & BU  937      & 2009.4301 & 135.0 & 1.04 &       &      &  \\
14082+3645 & STT 276AB    & 2009.4301 & 206.9 & 0.44 &       &      &  \\
14087+3341 & HU  742      & 2009.4329 & 354.0 & 0.24 & ~67.0 & 0.29 & Popovic 1972 \\
14087+3341 & HU  742      & 2009.4412 & 355.6 & 0.25 &       &      &  \\
14109+1513 & HDS1989Aa,Ab & 2009.4412 & 358.7 & 0.43 &       &      &  \\
14109+2412 & HDS1988      & 2009.4329 & 150.2 & 3.29 &       &      &  \\
14113+3013 & COU 605      & 2009.4412 & 163.5 & 0.26 &       &      &  \\
14113+3013 & COU 605      & 2009.4329 & 164.4 & 0.27 &       &      &  \\
14124+2843 & STT 277AB    & 2009.4301 & ~64.3 & 0.19 &       &      &  \\
14164+2539 & HDS2006      & 2009.4412 & 249.2 & 0.70 &       &      &  \\
14184+3412 & HU  901      & 2009.4301 & ~32.6 & 0.61 &       &      &  \\
14276+2037 & HO  542      & 2009.4329 & 213.6 & 0.98 &       &      &  \\
14278+3257 & STF1848      & 2009.4302 & 356.2 & 3.09 &       &      &  \\
14278+3257 & STF1848      & 2009.4412 & 356.3 & 3.08 &       &      &  \\
14295+3612 & HU 1268      & 2009.4412 & 345.2 & 0.30 & 313.0 & 0.38 & Erceg 1975 \\
14436+3745 & STF1875      & 2009.4329 & 128.5 & 3.06 &       &      &  \\
14485+2445 & COU 304      & 2009.4329 & 300.8 & 0.46 &       &      &  \\
\bottomrule
\end{tabular}
\end{table*}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%%%%% TABLA 2 CONTINUA

\setcounter{table}{1}
\begin{table*}[!t]
\vspace{0.1cm}
\centering
\centerline{TABLE~2 (CONTINUED)\smallskip}
\tablecols{8}
\footnotesize
\begin{tabular}{clcccccl}
\toprule
WDS                         & \multicolumn{1}{c}{Disc.} & Date      & P.A   & Sep.     & P.A. Orb. & Sep. Orb. & \multicolumn{1}{c}{Reference} \\
$ (\alpha,\delta J2000.0) $ & \multicolumn{1}{c}{Name}  & Besselian & (deg) & (arcsec) & (deg)     & (arcsec)  &  \\
\midrule
15002+2129 & HU  907   & 2009.4413 & 277.3 & 0.24 &       &      &  \\
15002+2129 & HU  907   & 2009.4329 & 278.0 & 0.21 &       &      &  \\
15049+3428 & STF1908AB & 2009.4413 & 151.4 & 1.33 &       &      &  \\
15075+1541 & A  2228   & 2009.4330 & ~12.2 & 3.29 &       &      &  \\
15136+3453 & HO   60   & 2009.4413 & ~68.1 & 0.18 & ~72.7 & 0.16 & Baize 1993a \\
15136+3453 & HO   60   & 2009.4330 & ~73.5 & 0.16 & ~72.7 & 0.16 & Baize 1994 \\
15151+3650 & STT 295   & 2009.4413 & 150.3 & 0.30 &       &      &  \\
15192+4329 & A  1630   & 2009.4330 & 244.8 & 0.78 &       &      &  \\
15208+4242 & A   573   & 2009.4413 & 171.9 & 0.71 &       &      &  \\
15257+2638 & STF1941   & 2009.4330 & 212.6 & 1.38 &       &      &  \\
15271+2355 & A    82   & 2009.4330 & 351.0 & 0.83 &       &      &  \\
15272+4133 & COU1443   & 2009.4413 & 172.8 & 0.49 &       &      &  \\
15307+3810 & HU 1163   & 2009.4413 & 168.1 & 0.22 & 189.1 & 0.17 & Couteau 1990 \\
15307+3810 & HU 1163   & 2009.4330 & 169.3 & 0.21 & 191.9 & 0.21 & Zulevic 1995 \\
           &           &           &       &      & 191.9 & 0.21 & Zulevic 1996 \\
           &           &           &       &      & 169.4 & 0.21 & Hartkopf  et al. 2000 \\
15390+2545 & COU 612   & 2009.4413 & 177.5 & 0.29 & 326.6 & 0.15 & Baize 1992a \\
           &           &           &       &      & 326.6 & 0.15 & Baize 1993b \\
           &           &           &       &      & 176.2 & 0.26 & Docobo  \& Ling 1998a \\
           &           &           &       &      & 173.2 & 0.30 & Aristidi et al. 1999 \\
15404+2123 & HU  579   & 2009.4414 & 136.5 & 0.70 &       &      &  \\
15498+4431 & BU  621   & 2009.4302 & ~26.4 & 0.67 &       &      &  \\
15554+2932 & HO  399   & 2009.4302 & 117.3 & 3.59 &       &      &  \\
15574+4140 & STF1991AB & 2009.4331 & 195.5 & 3.02 &       &      &  \\
15574+4140 & STF1991AB & 2009.4414 & 195.8 & 3.01 &       &      &  \\
15574+4140 & STF1991AB & 2009.4302 & 196.4 & 2.99 &       &      &  \\
16115+1507 & A  1799   & 2009.4414 & 117.6 & 0.76 &       &      &  \\
16128+3922 & STF2028   & 2009.4302 & 144.7 & 0.39 & 140.8 & 0.33 & Alzner 2001 \\
16156+1944 & HU  480   & 2009.4331 & 261.9 & 1.61 &       &      &  \\
16161+2936 & A   348   & 2009.4302 & 149.2 & 1.04 &       &      &  \\
16192+4140 & STT 309   & 2009.4302 & 307.4 & 0.28 & 306.6 & 0.28 & Seymour et al. 2002 \\
16199+2341 & COU 108   & 2009.4414 & 255.1 & 0.63 &       &      &  \\
16199+2341 & COU 108   & 2009.4331 & 255.9 & 0.62 &       &      &  \\
16248+3925 & HU 1276   & 2009.4302 & 270.3 & 0.39 &       &      &  \\
16248+3925 & HU 1276   & 2009.4414 & 270.4 & 0.42 &       &      &  \\
16273+2653 & A   226   & 2009.4331 & ~94.1 & 1.01 &       &      &  \\
16273+2653 & A   226   & 2009.4415 & ~94.3 & 1.02 &       &      &  \\
16309+3804 & STF2059   & 2009.4303 & 186.3 & 0.36 &       &      &  \\
16326+2314 & BU  817   & 2009.4303 & 327.9 & 0.94 &       &      &  \\
16326+2314 & BU  817   & 2009.4331 & 328.1 & 0.94 &       &      &  \\
16384+3514 & COU 985   & 2009.4415 & ~69.4 & 0.30 & ~79.4 & 0.20 & Baize 1993c \\
16384+3514 & COU 985   & 2009.4331 & ~70.1 & 0.30 & ~82.8 & 0.21 & Docobo  \& Ling 1998b \\
           &           &           &       &      & ~82.8 & 0.20 & Docobo  et al. 2000 \\
16412+1714 & HDS2366   & 2009.4331 & ~95.8 & 0.53 &       &      &  \\
16422+3753 & HDS2372   & 2009.4303 & 252.1 & 0.18 &       &      &  \\
16422+4112 & STF2091   & 2009.4303 & 325.9 & 0.40 &       &      &  \\
16476+4255 & COU1452   & 2009.4415 & 103.5 & 0.26 &       &      &  \\
16476+4255 & COU1452   & 2009.4332 & 108.6 & 0.29 &       &      &  \\
16539+2547 & COU 492   & 2009.4332 & ~91.9 & 0.52 &       &      &  \\
16539+2547 & COU 492   & 2009.4415 & ~91.9 & 0.52 &       &      &  \\
17063+2631 & A   228   & 2009.4388 & 185.7 & 0.46 &       &      &  \\
17075+3810 & COU1291   & 2009.4303 & 301.1 & 0.28 & ~~0.6 & 0.15 & Baize 1993c \\
           &           &           &       &      & 356.3 & 0.07 & Docobo  \& Ling 1998a \\
           &           &           &       &      & 348.0 & 0.07 & Docobo  \& Ling 2002 \\
\bottomrule
\end{tabular}
\end{table*}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%%%%% TABLA 2 CONTINUA

\setcounter{table}{1}
\begin{table*}[!t]
\vspace{0.1cm}
\centering
\centerline{TABLE~2 (CONTINUED)\smallskip}
\tablecols{8}
\footnotesize
\begin{tabular}{clcccccl}
\toprule
WDS                         & \multicolumn{1}{c}{Disc.} & Date      & P.A   & Sep.     & P.A. Orb. & Sep. Orb. & \multicolumn{1}{c}{Reference} \\
$ (\alpha,\delta J2000.0) $ & \multicolumn{1}{c}{Name}  & Besselian & (deg) & (arcsec) & (deg)     & (arcsec)  &  \\
\midrule
17094+1901  & A  2086     & 2009.4332 & 204.3 & 3.14 &       &      &  \\
17116+3916  & HU 1178AB   & 2009.4332 & ~~9.5 & 0.36 &       &      &  \\
17116+3916  & HU 1178AB   & 2009.4303 & ~10.4 & 0.36 &       &      &  \\
17116+3916  & HU 1178AB   & 2009.4303 & ~10.7 & 0.36 &       &      &  \\
17184+3240  & BU  628     & 2009.4303 & 267.1 & 0.52 & 255.4 & 0.39 & Zulevic 1986 \\
17215+2845  & KUI  80AB   & 2009.4388 & 169.9 & 0.62 &       &      &  \\
17221+2310  & COU 415     & 2009.4388 & 249.3 & 0.24 & 174.5 & 0.27 & Baize 1992a \\
            &             &           &       &      & 174.5 & 0.27 & Baize 1993b \\
17239+3627  & STF2162     & 2009.4304 & 284.5 & 1.35 &       &      &  \\
17250+4306  & COU1454     & 2009.4304 & 148.0 & 0.98 &       &      &  \\
17251+3444  & HU  922     & 2009.4304 & 225.4 & 0.21 & ~~6.8 & 0.31 & Heintz 1982 \\
17275+1627  & A  2184     & 2009.4388 & ~30.4 & 1.87 &       &      &  \\
17377+4250  & HDS2489     & 2009.4304 & 346.7 & 0.55 &       &      &  \\
17377+4250  & HDS2489     & 2009.4332 & 347.1 & 0.55 &       &      &  \\
17412+4139  & STF2203     & 2009.4416 & 293.7 & 0.73 &       &      &  \\
17434+3357  & HO  560     & 2009.4304 & 263.3 & 1.32 &       &      &  \\
17434+3357  & HO  560     & 2009.4416 & 263.3 & 1.33 &       &      &  \\
17434+3357  & HO  560     & 2009.4388 & 265.2 & 1.37 &       &      &  \\
17486+2339  & BAR   8     & 2009.4416 & 237.8 & 1.16 &       &      &  \\
17504+3526* & STF2236     & 2009.4389 & ~18.9 & 0.31 &       &      &  \\
17504+3526* & STF2236     & 2009.4304 & ~22.6 & 0.32 &       &      &  \\
17504+3526  & STF2236     & 2009.4389 & ~97.0 & 3.39 &       &      &  \\
17504+3526  & STF2236     & 2009.4304 & ~97.1 & 3.37 &       &      &  \\
17506+3932  & COU1301     & 2009.4389 & ~84.3 & 1.74 &       &      &  \\
17506+3932  & COU1301     & 2009.4416 & ~85.0 & 1.74 &       &      &  \\
17541+2949  & AC    9     & 2009.4389 & 240.6 & 1.09 &       &      &  \\
17577+2815  & HO  424     & 2009.4389 & 203.0 & 1.42 &       &      &  \\
17584+3524  & COU1000     & 2009.4416 & 153.3 & 0.89 &       &      &  \\
17591+3228  & HU 1185     & 2009.4416 & 138.5 & 0.36 & 148.4 & 0.27 & Heintz 1975 \\
18017+4011  & STF2267     & 2009.4304 & 271.1 & 0.55 &       &      &  \\
18017+4011  & STF2267     & 2009.4389 & 271.7 & 0.56 &       &      &  \\
18025+4414  & BU 1127AB   & 2009.4332 & ~52.9 & 0.73 & ~65.4 & 1.15 & Popovic 1970 \\
            &             &           &       &      & ~62.6 & 1.02 & Popovic  \& Pavlovic 1995a \\
            &             &           &       &      & ~62.6 & 1.02 & Popovic  \& Pavlovic 1995b \\
18033+3921  & STF2275     & 2009.4416 & 297.2 & 0.27 & 300.0 & 0.26 & Popovic 1998 \\
            &             &           &       &      & 299.9 & 0.26 & Popovic et al. 2000 \\
18063+3824  & HU 1186     & 2009.4304 & 115.6 & 0.25 & 141.3 & 0.09 & Heintz 1965 \\
18063+3824  & HU 1186     & 2009.4416 & 123.3 & 0.30 & 119.0 & 0.22 & Baize 1992b \\
            &             &           &       &      & 121.1 & 0.20 & Heintz 1995 \\
18126+3836  & BU 1091     & 2009.4305 & 320.7 & 0.72 &       &      &  \\
18126+3836  & BU 1091     & 2009.4416 & 320.7 & 0.72 &       &      &  \\
18178+4351  & A 578 AB    & 2009.4332 & 157.2 & 1.75 &       &      &  \\
18178+4351  & A 578 Aa,Ab & 2009.4332 & 247.0 & 0.31 &       &      &  \\
18264+4326  & HDS2606     & 2009.4417 & ~49.3 & 1.02 &       &      &  \\
18432+3822  & HDS2651     & 2009.4305 & ~50.8 & 0.44 &       &      &  \\
18450+4239  & HDS2657     & 2009.4305 & ~37.1 & 0.21 &       &      &  \\
19018+3448  & COU1612     & 2009.4305 & 318.7 & 0.82 &       &      &  \\
19072+4451  & A   703     & 2009.4305 & 188.4 & 0.54 &       &      &  \\
19072+4451  & A   703     & 2009.4390 & 189.3 & 0.56 &       &      &  \\
19089+3404  & COU1462     & 2009.4306 & 204.7 & 0.19 & 225.1 & 0.62 & Mante 1994 \\
            &             &           &       &      & 203.0 & 0.20 & Mante 1997 \\
            &             &           &       &      & 203.0 & 0.20 & Mante 1999 \\
19122+3215  & HU  941     & 2009.4333 & 146.1 & 1.08 &       &      &  \\
19131+2154  & A   153     & 2009.4306 & 267.7 & 0.71 &       &      &  \\
\bottomrule
\end{tabular}
\end{table*}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%%%%% TABLA 2 CONTINUA

\setcounter{table}{1}
\begin{table*}[!t]
\vspace{0.1cm}
\centering
\centerline{TABLE~2 (CONTINUED)\smallskip}
\tablecols{8}
\footnotesize
\begin{tabular}{clcccccl}
\toprule
WDS                         & \multicolumn{1}{c}{Disc.} & Date      & P.A   & Sep.     & P.A. Orb. & Sep. Orb. & \multicolumn{1}{c}{Reference} \\
$ (\alpha,\delta J2000.0) $ & \multicolumn{1}{c}{Name}  & Besselian & (deg) & (arcsec) & (deg)     & (arcsec)  &  \\
\midrule
19214+1948  & HO  637      & 2009.4333 & ~27.6 & 1.20 &       &      &  \\
19251+2213  & COU 513      & 2009.4333 & ~~2.6 & 0.25 &       &      &  \\
19266+3120  & HDS2762      & 2009.4306 & 214.6 & 0.35 &       &      &  \\
19272+1626  & HDS2765      & 2009.4333 & 177.5 & 0.36 &       &      &  \\
19331+3254  & HU  948AB    & 2009.4306 & 149.9 & 0.26 &       &      &  \\
19331+3254  & HU  948AB    & 2009.4333 & 152.2 & 0.27 &       &      &  \\
19350+2947  & A   368      & 2009.4306 & 153.4 & 0.50 &       &      &  \\
19356+4002  & A  1400      & 2009.4390 & 122.5 & 0.35 & 134.3 & 0.24 & Seymour et al. 2002 \\
19358+2316  & A   163      & 2009.4333 & ~20.8 & 0.23 & ~~1.7 & 0.18 & Baize 1981 \\
19466+4346  & HDS2810      & 2009.4390 & ~49.5 & 0.34 &       &      &  \\
19532+4238  & COU2635      & 2009.4390 & 157.5 & 0.54 &       &      &  \\
19538+2237  & COU 825AB    & 2009.4334 & ~32.0 & 1.23 &       &      &  \\
19575+2018  & BU  425AB    & 2009.4334 & 239.7 & 1.35 &       &      &  \\
19583+2208  & AG  244AB    & 2009.4334 & 273.2 & 1.51 &       &      &  \\
20016+3435  & COU1947      & 2009.4307 & ~88.4 & 0.27 &       &      &  \\
20082+2105  & J  1168      & 2009.4334 & 192.6 & 0.88 &       &      &  \\
20109+2237  & HDS2877      & 2009.4334 & 201.4 & 0.45 &       &      &  \\
20157+4339  & A 2095AB    & 2009.4390 & 155.9 & 0.26 & 146.7 & 0.21 & Zulevic 1997 \\
            &              &           &       &      & 146.8 & 0.24 & Ling 1999 \\
20157+4339  & STF2659AC    & 2009.4390 & 314.0 & 3.03 &       &      &  \\
20172+2415  & HDS2893      & 2009.4334 & 168.4 & 0.31 &       &      &  \\
20177+4030  & HDS2897      & 2009.4390 & 269.0 & 0.33 &       &      &  \\
20302+2651  & WOR   9AB    & 2009.4334 & 256.4 & 0.51 &       &      &  \\
20333+2727  & HDS2935      & 2009.4334 & 114.1 & 0.48 &       &      &  \\
20477+4204  & BU  268      & 2009.4391 & 199.3 & 0.39 &       &      &  \\
20506+3024  & STT 415      & 2009.4280 & 232.2 & 3.68 &       &      &  \\
20531+2909  & STT 417AB    & 2009.4280 & ~27.7 & 0.90 &       &      &  \\
20564+4308  & COU2544      & 2009.4391 & 160.4 & 0.32 &       &      &  \\
20564+4308  & COU2544      & 2009.4280 & 160.5 & 0.33 &       &      &  \\
20582+3510  & COU1813      & 2009.4335 & 308.9 & 1.16 &       &      &  \\
21000+4004  & KUI 103AB    & 2009.4335 & 356.2 & 0.42 & 182.6 & 0.64 & Lippincott 1975 \\
21000+4004  & KUI 103AB    & 2009.4280 & 357.1 & 0.43 & ~44.0 & 0.54 & Baize 1989 \\
            &              &           &       &      & ~44.0 & 0.54 & Baize 1991 \\
            &              &           &       &      & ~40.5 & 0.60 & Heintz 1994 \\
            &              &           &       &      & ~32.8 & 0.31 & Docobo  \& Ling 1994 \\
            &              &           &       &      & 336.9 & 0.23 & Soderhjelm 1999 \\
            &              &           &       &      & ~12.4 & 0.35 & Mante 2000 \\
            &              &           &       &      & ~12.4 & 0.43 & Pourbaix 2000 \\
21018+3916  & STF2746      & 2009.4391 & 321.1 & 1.19 &       &      &  \\
21089+1748  & HU  365      & 2009.4335 & ~19.9 & 1.03 &       &      &  \\
21111+1704  & HEI 187      & 2009.4335 & 255.7 & 1.13 &       &      &  \\
21115+4115  & STT 431AB    & 2009.4391 & 125.2 & 2.62 &       &      &  \\
21115+4115  & STT 431AB    & 2009.4281 & 125.3 & 2.61 &       &      &  \\
21143+4109  & STT 432      & 2009.4391 & 114.8 & 1.33 &       &      &  \\
21161+4101  & COU2229      & 2009.4281 & 272.1 & 0.78 &       &      &  \\
21171+4312  & A   401      & 2009.4391 & 219.7 & 0.41 &       &      &  \\
21328+3904  & A  1443      & 2009.4391 & 240.4 & 0.27 &       &      &  \\
21328+3904  & A  1443      & 2009.4281 & 240.7 & 0.25 &       &      &  \\
21334+3058  & COU 732Aa,Ab & 2009.4336 & 264.8 & 0.49 &       &      &  \\
21356+3446  & COU1481      & 2009.4281 & 171.7 & 0.64 &       &      &  \\
21363+1627  & HDS3076      & 2009.4336 & 262.5 & 0.34 &       &      &  \\
21380+4153  & A   402      & 2009.4281 & ~45.9 & 0.85 &       &      &  \\
21421+4414  & A   403      & 2009.4281 & ~77.7 & 0.48 &       &      &  \\
\bottomrule
\end{tabular}
\end{table*}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


As is well known, the ACF has no information about the Fourier phase of the image; therefore, the position angle is determined 
only modulo $180\arcdeg$. To avoid this inconvenience we also used Christou's self-calibrating shift-and-add technique 
(Christou et al. 1986). Figure~3 shows an image which was calculated using this technique. We have to admit that the technique 
doesn't work for weak objects when single photon events are strongly dominant in the speckle image.

Table~2 contains 189 measurements pertaining to 144 binary or multiple stars. The format for presentation of these measurements 
is not the same as in our previous publication (Orlov et al. 2009). We include three new columns for ephemerides of binaries 
with known orbital elements. Column~1 contains the epoch-2000 coordinates in the format used in the Washington Double Star (WDS) 
Catalog (Worley \& Douglass 1997). The second column gives the name of the star or discoverer designation. The third column gives 
the epoch of the observation in fractional Besselian year. The two following columns  contain the measured position angles 
$\theta$ given in degrees and angular distances $\rho$ in arcseconds. The last three columns show ephemerides calculated for the 
date of observation and references to publications in which orbital elements can be found. As one can see, some orbits give very 
discrepant position of the secondary.


\section{CONCLUSION}

A program of speckle observations has been started at the Observatorio Astron\'omico Nacional telescopes, with the goal of 
obtaining astrometric data of double stars. This study started with well-known binaries from the WDS catalogue.  One hundred 
seventy five position angle and separation measures for one hundred sixty three binaries have been presented, a subset of 
which has been used to determine measurement precision. We only present here the cases where the binary was clearly resolved. 
The results on binaries which demand more detailed analysis will be reported in subsequent publications.

%\vspace{0.1cm}

\acknowledgements

The speckle interferometry program at the OAN telescopes is supported by the Direccion General de Asuntos del Personal Acad\'emico 
(Universidad Nacional Aut\'onoma de M\'exico, Mexico) under projects IN104910 and IN113308 (PAPIIT).


%\vspace{0.15cm}

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\end{document}