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ISSN 1990-3413, Astrophysical Bulletin, 2007, Vol. 62, No. 3, pp. 235­243. c Pleiades Publishing, Ltd., 2007. Original Russian Text c D.A. Rastegaev, Yu.Yu. Balega, E.V. Malogolovets, 2007, published in Astrofizicheskij Byulleten, 2007, Vol. 62, No. 3, pp. 251-259.

Speckle Interferometry of Metal-Poor Stars in the Solar Neighborhood. I
D. A. Rastegaev* , Yu. Yu. Balega, and E. V. Malogolovets
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, 369167 Russia
Received June 15, 2007; in final form, June 28, 2007

Abstract--We report the results of speckle-interferometric observations of 109 high proper-motion metalpoor stars made with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. We resolve eight objects--G102-20, G191-55, BD+19 1185A, G89-14, G87-45, G87-47, G111-38, and G114-25--into individual components and we are the first to astrometrically resolve seven of these stars. New resolved systems included two triple (G111-38, G87-47) and one quadruple (G89-14) star. The ratio of single-to-binary-to-triple-to-quadruple systems among the stars of our sample is equal to 71:28:6:1. PACS numbers : 97.20.Tr, 97.80.-d DOI: 10.1134/S1990341307030042

1. INTRODUCTION Stars of the halo and thick disk of our Galaxy are old metal-poor objects with large spatial velocities [1, 2]. The studies of these stars can be used to impose constraints on the physical conditions during the early stages of the formation of our Galaxy. Binary and multiple stars are the best candidate objects to be used for studying the process of star formation at the time of formation of our Galaxy, because they bear more information about this process compared to single stars. This information is coded both in the orbital parameters (eccentricity, semi-major axis) and physical parameters of the components (component luminosities and the mass function). The authors of early papers dedicated to the study of the multiplicity of the old population of the Galaxy [3, 4] concluded that the fraction of binary and multiple systems among these objects is very low compared to the corresponding fractions for younger stars of the Galactic disk, which are richer in heavy elements. However, the picture has changed in the last two decades. In series of papers opened by [5] is shown that the binary-to-single star ratio for halo and thick-disk stars is comparable to the corresponding ratio for the overwhelming majority of stars in the solar neighborhood. Such studies are based on the analysis of stellar spectra [6, 7] using the data on visual binaries and common proper motion pairs [8, 9]. We still have insufficient data about the multiple old stars in the solar neighborhood with orbital semimajor axes in the interval from 1 to 100 AU observable with adaptive optics and speckle-interfero*

metric facilities. We point out the paper by Zinnecker et al. [10] who report the results of observations of population II stars using the techniques of speckle interferometry, adaptive optics, and direct imaging. To expand the database on such objects and determine the properties of the components of multiple systems, we began speckle-interferometric observations of metal-poor objects with large proper motions located in the close vicinity of the Sun. In this paper we report the results of observations of 109 halo and thick-disk stars made during the period from April through December, 2006. The paper has the following layout: Section 2 describes the sample of stars studied; Section 3 analyzes the methods of observations and reduction of the data obtained; Sections 4 and 5 list the results of observations and additional information about the resolved stars, respectively; Section 6 discusses the multplicity of the stars studied, and the last section gives the conclusions. 2. THE SAMPLE We selected our program stars from the CLLA catalog [11]. This catalog is actually a sample of A- to early K-type dwarfs from the Lowell Proper Motion Catalog [12, 13], which contains mostly NorthernHemisphere stars brighter than 16 magnitude with proper motions exceeding 0.26 /year. We selected a total of 223 stars from the CLLA catalog based on the following three criteria: 1. [m/H] < -1; 2. > -10 ; 3. mV < 12.
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Fig. 1. Distribution of the stars of the sample by metallicity [m/H] and V component of spatial velocity. The dashed line separates stars moving in prograde and retrograde orbits.

Fig. 2. Distribution of heliocentric distances of the stars of the sample (we adopt the distances from the CLLA catalog).

We use the data of the CLLA catalog to make several figures illustrating some of the main characteristics of our sample. Figure 1 shows the distribution of our selected stars on the "metallicity ­ V-component of the spatial velocity" plane, which demonstrates that our stars belong to different components of the Galaxy. The left-hand part of the diagram is occupied by halo objects -- metal-poor stars with high velocity dispersion. The upper right corner is populated by stars belonging to the metal-weak tail of the thick disk. About 20% of all stars (45 objects) move in retrograde orbits. Figure 2 shows the distribution of the heliocentric distances of the stars of our sample. We used the photometric distances from the CLLA catalog. Arifyanto et al. [14] compared the photometric parallaxes with the corresponding trigonometric parallaxes measured by Hipparcos [15] for stars of the catalog considered and showed that there is a small discrepancy between the heliocentric distances determined using different methods. However, we did not correct the photometric distances in any way. Fig. 3 shows the distribution of the metallicities of the stars studied. The [m/H] < -3 metallicity interval is represented by only one star, G64-12, with [m/H] = -3.52. Half of the stars studied have metallicities in the interval [m/H] = [-1.58; -1). As is evident from the distribution of stellar temperatures (Fig. 4), these are F-, G-, and K-type stars. 3. OBSERVATIONS AND DATA REDUCTION We performed speckle-interferometry of 109 stars of the sample with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS): in April (one star), May (five objects), June (six objects), and December, 2006

Fig. 3. Distribution of the metallicities of the stars of the sample (we adopt the metallicities from the CLLA catalog).

(97 objects). Before December 2006 observations were made using a facility described by Maksimov et al. [16]. Its detector consists of a fast 1280â1024 Sony ICX085 CCD combined with a three-stage image intensifier with electrostatic focusing. In December we used a new facility based on an EMCCD (a CCD with internal electron gain) with higher quantum efficiency and better linearity. Both facilities are capable of detecting objects with component magnitude differences up to 4m . We recorded speckle interferograms in filters with the parameters of 545/30 nm (the first and the second numbers give the central wavelength and half bandwidth of the filter, respectively), 550/20, 800/110,and 800/100 nm with exposures ranging from five to 20 milliseconds. In December 2006 we obtained 500
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Table 2 gives some data on resolved systems. The last column of this table summarizes the results of all available astrometric and spectroscopic observations of the objects studied including the speckleinterferometric observations performed with the 6-m telescope of SAO RAS. 5. ADDITIONAL DATA ON RESOLVED STARS In this section we summarize additional data on the resolved stars. For some objects we list two distances determined from photometric [11] and trigonometric [15] parallaxes. It is evident that the distance determined using the former method is underestimated, because it does not take into account the luminosity of the additional component. On the other hand, the additional component also introduces certain error in the measured trigonometric parallaxes, especially for short-period systems. G102-20 (05h 40m 09s 7 +12 10 41 ; HIP 26676). . This known SB1-type spectroscopic binary with a 26-year period [7] and a heliocentric distance of 70 pc [15] was resolved speckle-interferometrically for the first time. . G191-55 (05h 57m 28s 6+58 40 49 ;BD+58 876; TYC 3762-1904-1). It is an F8-type binary [18] located at a heliocentric distance of 93 pc [11]. . +19 21 39 ; BD+19 1185A (06h 03m 14s 9 HIP 28671). It is a G0V-type object [18]. The binary nature of this star with = 223 mas was discovered by Hipparcos. Its heliocentric distance is estimated at d 42 [11] and d 66 pc [15]. This is a triple system given the presence of a distant companion ( 7 )BD+19 1185B. . G89-14 (07h 22m 31s 5 +08 49 13 ; HIP 35756; WDS 07224+0854) is a new quadruple system. We resolved it as a pair with a separation of 0.99 . Allen et al. [8] provide evidence suggesting that the system may contain a physically bound component at a distance of 34 . At the same time, G89-14 is an SB1type spectroscopic binary with a period of 190 days [7]. The star is at a heliocentric distance of 94 pc [15]. . G87-45 (07h 32m 58s 7 +31 07 00 ; TYC 2453763-1). It is a G2-type star [18] known as an SB2type spectroscopic binary with a period of 51 days [19]. The spectrum of this star exhibits signs of a third component [7], which we must have resolved. The distance to the star is d 123 pc [11]. . G87-47 (07h 35m 34s 1 +35 57 11 ; HIP 36936). A new triple system whose distance is estimated at

Fig. 4. Distribution of the temperatures of the stars of the sample (we adopt the temperatures from the CLLA catalog ).

short-exposure images for each of most of the objects. For each of the remaining objects 2000 exposures are accumulated. A description of the technique used to determine the relative positions and component magnitude differences from the power spectra of speckle interferograms averaged over the set can be found in [17]. The diffraction limit of the resolution is equal to 0.022 in the 545/30 and 550/20 nm filters and 0.033 in the 800/110 and 800/100 filters. The measured position angles and angular separations are accurate to 0.3­2.8 and 1 to 5 mas, respectively. The errors of measured and depend on a number of parameters: component separation, magnitude difference, and seeing . The accuracy of the component magnitude difference determined from the power spectrum is also a function of the same parameters. It usually varies from 0.05m to 0.2m for mV = 8 ­ 10 objects. 4. RESULTS OF OBSERVATIONS The main results of this work are listed in Tables 1 and 4. We resolved into components the following eight objects: G102-20, G191-55, BD+19 1185A, G8914, G87-45, G87-47, G111-38, and G114-25. We astrometrically resolved seven among these eight objects for the first time and found new components in five objects: G191-55, G89-14, G87-47, G111-38, and G114-25. We were the first to astrometrically resolve the well-known spectroscopic binary G102-20 [7]. We are also the first to establish the astrometric binarity of the G87-45 system whose spectrum exhibits signatures of three components [7]. The astrometric binarity of the resolved object BD+19 1185A was earlier discovered by Hipparcos [15].
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d 62 [11] and d 100 pc [15]. The system is known as an SB1-type spectroscopic binary with a period of 13 days. The Hipparcos catalog lists it as an object with stochastic astrometric solution. We found a third component. For this object we could determine the position of the secondary only with an uncertainty of ±180 . . G111-38 (07h 49m 32s 0 +41 28 08 ; HIP 38195; WDS 07495+4128). A new triple system. Hipparcos resolved it as a binary with = 2.154 . We resolved one of the components. The distance to the system is estimated at d 50 pc [11] or d 200 pc [15]. The spectral type of the system is G5 [18]. . G114-25 (08h 59m 03s 4 -06 23 46 ; HIP 44111). A new binary of spectral type F7 [18]. Its heliocentric distance is d 131 pc [11]. 6. MULTIPLICITY OF STARS

the WDS catalog. To this end, we analyzed the component magnitude difference and the change of the component separations over thetimeperiods covered by observations. As a result, we left only 12 objects among the initial 43 WDS components and used them to compute the ratios of the number of systems of different degree of multiplicity.

6.2. Ratio of the Systems of Different Degree of Multiplicity
To compute the ratio of the number of systems of different degree of multiplicity among the stars studied, we use all the data that we gathered on the observations of these systems using different methods. Of the 109 stars considered 24 are spectral binaries [6, 7]; one star (G87-45) is a spectral triple [7]; seven stars are speckle-interferometric binaries, and one star (G111-38) is a speckle-interferometric triple. Twelve stars have companions listed in the WDS catalog. It goes without saying that there are components detected using different methods. For example, the G102-20 binary with a period of 26 years [7] was found both spectroscopically and using speckle interferometry. Similarly, the outer pair in the triple system G111-38 ( 2 ) can be detected both using speckle interferometry and visually. The resulting ratio of the number of single, binary, triple, and quadruple systems discovered using all methods among the stars of our sample is equal to 71:28:6:1. The corresponding estimate for F7- to G9type disk stars uncorrected for unresolved binaries [21] is equal to 51:40:7:2. We point out an important difference between the two samples compared. Whereas our sample consists of stars selected by magnitude and spatial velocities, the sample used in [21] is only distance limited (all its stars are located within 22 pc of the Sun).

6.1. Distant Components
For 109 of the objects considered we used additional data on the spectroscopic multiplicity of these stars [6, 7] and the data on distant components from the WDS [20] catalog. Whereas spectroscopic and interferometric components appear to be undoubtedly physically bound, one must treat wide visual companions more carefully. We found a total of 43 WDS components (in some cases several components for one object), most of which we rejected as accidental optical projections. Table 3 lists the data on the all found wide components. The first column gives the names of the stars studied and the second column, all the WDS components found. For the components found to be physically bound to the corresponding stars columns 3 and 4 give the component separation and magnitude difference, respectively. We adopt the latter from the WDS catalog and they may differ slightly from the quantities given in the corresponding references. The `+'and `-' signs in column 5 (Status) mark the components, which we consider to be possibly physically bound to the main star and physically unbound optical pairs, respectively. A question mark in this column indicates that we are not sure about our decision. The last column gives the references to the papers, which contain data on the corresponding pair and confirm or disprove its physical relationship. In all cases these are two papers [8, 9] dedicated to wide pairs of population II stars and the Hipparcos catalog [15]. Additional symbol in this column indicates that our observations confirm the presence of the given component. If no references are given, it means that we made our own decision about the physical association based on the data provided by

7. CONCLUSIONS We selected for observations with high angular resolution a total of 223 high proper motion metal-poor objects from the CLLA catalog [11]. Our speckle-interferometric observations of 109 stars made with the 6-m telescope of SAO RAS allowed us to resolve eight stars into components and we were the first to astrometrically resolve seven objects. Additional data on spectral and astrometric multiplicity allowed us to estimate the ratio of the number of single, binary, triple, and quadruple systems to be 71:28:6:1. In the next paper of this series we will continue to publish the results of our speckle-interferometric observations of the star sample presented.
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Table 1. Speckle-interferometric measurements of resolved objects

Name of the system/ subsystem G102-20 G191-55 BD+19 1185A G89-14 G87-45 G87-45 G87-47 G111-38AB G111-38AB G111-38AC G111-38AC G111-38BC G111-38BC G114-25


( )

( )

m

Filter

0.120±0.006 0.814±0.002 0.115±0.001 0.989±0.005 0.285±0.002 0.285±0.002 0.078±0.003 0.084±0.001 0.084±0.001 2.133±0.005 2.133±0.005 2.216±0.005 2.216±0.005 0.781±0.005

308.0±2.8 125.1±0.3 183.6±0.7 0.8±0.4 271.3±0.5 270.7±0.4 54.0 ±2.1 7.9±0.7 7.8±1.3 200.0±0.3 200.0±0.3 199.5±0.3 199.5±0.3 323.7±0.5


3.24±0.11 2.00±0.01 1.77±0.02 4.14±0.06 2.01±0.04 1.76±0.02 1.74±0.03 0.78±0.01 0.75±0.01 1.34±0.01 1.10±0.01 0.57±0.02 0.36±0.03 3.83±0.16

550/20 800/100 550/20 800/100 550/20 800/100 800/100 550/20 800/100 550/20 800/100 550/20 800/100 800/100

The position of the secondary component is known with an uncertainty of ±180.

Table 2. Additional data on resolved stars [m/H]

Name of the system/ subsystem G102-20 G191-55 BD+19 1185A G89-14 G87-45 G87-47 G111-38 G114-25
h h h

Coordinates (2000.0) 05h 40m 09s 7+12 10 41 . 05 57 28.6+58 40 49 06 03 14.9+19 21 39 07 22 31.5+08 49 13 07h 32m 58s 7+31 07 00 . 07 35 34.1+35 57 11 07 49 32.0+41 28 08 08 59 03.4 -06 23 46
h m s h m s h m s m s m s m s

m

V

Total multiplicity of the system 2 2 3 4 3 3 3 2

10.22 10.47 9.32 10.40 11.44 10.34 8.7 11.92

-1.17 -1.94 -1.47 -1.90 -1.49 -1.34 -1.04 -2.28

Metallicities adopted from the CLLA catalog [11].

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RASTEGAEV et al. Table 3. WDS components for stars of the sample Name G172-16 G2-38 G172-61 G71-33 G74-5 WDS companion 00386+4738OSO 7 01270+1200LDS3282 01344+4844ES 2587 01452+0331LDS3306 02104+2948BUP 29AB 02104+2948BUP 29AC 02104+2948BUP 29AD G37-26 G246-38 G95-57A/G95-57B 03084+2620OSO 14 03313+6644OSO 15 03470+4126STF 443AB 03470+4126STF 443AC 03470+4126FOX 135CD HD 25329 G99-31W BD+19 1185A 04033+3516OSO 16 05449+0915HDS 769 06032+1922HDS 823Aa 06032+1922LDS6195AB G88-10 G89-14 07104+2421OSO 19 07224+0854GIC 72AB 07224+0854ALC 2BC G112-43/G112-44 G111-38 07437-0004HJ 2413 07495+4128A 2468AB 07495+4128LDS 900AB-C G90-25 G251-54 07536+3036BUP 108 08110+7955LDS1668AB 110.5 5.4 08110+7955PWS 3AC 08110+7955OSO 21AD G40-14 G113-22 G9-36 08161+1942LDS3781 08170+0001LDS3782 08580+2428OSO 23AB 08580+2428OSO 23AC G115-49 G120-15 09053+3848OSO 24 11063+3113TDS7665AB 11063+3113OSO 36AC G10-4 11110+0625OSO 37 7.6 0.68 98.0 7.6 34.0 6.3 11.8 1.58 2.2 1.27 0.2 2.12 6.9 4.06 7.4 0.62 ( ) m Status References + + - - - - - - - + - - - - + + - - + + + - - + -? - + - - - - +? - - [9] [9]
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8.4 5.85 24.6 5.5

[9] [8] [9]

[9] [9] [8]

[9] [9] [15] [15], [8] [9] [8] [8] [8] [15],

[9] [9]

[9] [8]

[9] [9] [9]

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SPECKLE INTERFEROMETRY OF METAL-POOR STARS... Table 3. (Contd.) Name G66-22 G23-14 G143-33 WDS companion 14433+0550OSO 58 19518+0537OSO 112 20084+1503OSO 117AB 20084+1503OSO 117AC 20084+1503OSO 117AD 20084+1503OSO 117AE 20084+1503LDS1033AF G125-64 20090+4252OSO 118AB 20090+4252OSO 118AC Table 4. Unresolved stars Name G172-16 G33-30 G2-38 G172-58 G172-61 G173-10 G2-50 G71-33 G245-32 G133-45 G71-55 G72-60 G74-5 G74-30 G36-47 G37-26 G5-19 G221-7 G5-35 G246-38 G79-42 G79-43 Filter (/, nm) 800/100 800/100 800/100 800/100 Epoch 2006.9463 2006.9437 2006.9438 2006.9462 Name G79-56 G95-57A G95-57B HD 25329 G82-18 G84-29 G191-23 G86-39 G86-40 G96-48 G99-31W G102-27 G99-48 G101-34 G192-28 G105-50 G192-43 G87-13 G108-48 G107-50 G87-27 G88-10 ( ) m Status References + - - - - - - - - [9] [9] [9], [9] [9] [9] [9] [9]

241

3.2 3.19

Table 4. (Contd.) Filter (/, nm) 800/100 550/20 550/20 550/20 800/100 550/20 800/100 800/100 Epoch 2006.9468 2006.9414 2006.9414 2006.9414 2006.9415 2006.9415 2006.9448 2006.9415

550/20; 800/100 2006.9462 550/20; 800/100 2006.9463 800/100 800/100 550/20 800/100 800/100 800/100 550/20 800/100 800/100 550/20 550/20 550/20 800/100 800/100 800/100 800/100 2006.9438 2006.9438 2006.9443 2006.9467 2006.9438 2006.9468 2006.9468 2006.9467 2006.9468 2006.9468 2006.9468 2006.9442 2006.9468 2006.9442 2006.9468 2006.9468
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550/20; 800/100 2006.9416 800/100 2006.9417

550/20; 800/100 2006.9417 550/20 800/100 800/100 800/100 800/100 800/100 800/100 800/100 800/100 2006.9471 2006.9471 2006.9471 2006.9448 2006.9471 2006.9448 2006.9417 2006.9445 2006.9475

550/20; 800/100 2006.9472 800/100 2006.9472

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242 Table 4. (Contd.) Name G108-58 G88-27 G90-3 G88-32 BD-1 1792 G112-43 G112-44 G90-25 G251-54 G234-24 G40-8 G234-28 G40-14 G113-22 G194-22


RASTEGAEV et al. Table 4. (Contd.) Epoch 2006.9445 2006.9472 2006.9472 2006.9418 2006.9446 2006.9446 2006.9446 Name G253-41 G120-15 G10-4 BD+36 2165 HD 97916* G56-30 G254-24 G147-62 G121-12 G176-53 G122-51 G66-22 G166-45 G16-13 G16-20 G153-21 G170-47 G23-14 G23-20 G24-3 G143-33 G125-64 G171-15 Filter (/, nm) Epoch

Filter (/, nm) 800/100 800/100 800/100 800/100 800/100 800/100 800/100

550/20; 800/100 2006.9422 800/100 800/100 800/100 550/20 800/100 800/100 800/100 800/100 800/100 550/20 2006.9449 2006.9449 2006.9449 2006.945 2006.9449 2006.9423 2006.945 2006.9477 2006.9423 2006.945

550/20; 800/100 2006.9473 800/100 800/100 800/100 800/100 800/100 800/100 800/100 2006.9475 2006.9475 2006.9446 2006.9448 2006.9446 2006.9446 2006.9448

545/30; 800/110 2006.3747 545/30 545/30 545/30 545/30 545/30 800/110 800/110 800/110 800/110 800/110 800/100 2006.3747 2006.3748 2006.3749 2006.3749 2006.4488 2006.4517 2006.4517 2006.4518 2006.4518 2006.4518 2006.9463

BD+25 1981 550/20; 800/100 2006.9473 G46-5 G115-34 G9-36 G114-26 G115-49 G46-31 G41-41 G195-34 G48-29 G116-45 G161-73 G43-3 G53-41 G44-30 G58-23 G196-48 G58-25 G146-76 800/100 800/100 800/100 550/20 800/100 800/100 800/100 800/100 800/100 800/100 800/100 545/30 800/100 800/100 800/100 800/100 550/20 800/100 2006.9474 2006.9473 2006.9473 2006.942 2006.9473 2006.9476 2006.9476 2006.9422 2006.9476 2006.9473 2006.9476 2006.2759 2006.9421 2006.9422 2006.9422 2006.9422 2006.9422 2006.9477

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