# Calibrating the metallicity of M dwarfs in wide physical binaries with F-,
G-, and K- primaries – I: High-resolution spectroscopy with HERMES: stellar
parameters, abundances, and kinematics††thanks: Based on observations obtained
with the HERMES spectrograph mounted on the 1.2 m Mercator Telescope at the
Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofísica de Canarias

D. Montes1, R. González-Peinado1, H. M. Tabernero2,1, J. A. Caballero3, E.
Marfil1, F. J. Alonso-Floriano4,1, M. Cortés-Contreras3, J. I. González
Hernández5,6, A. Klutsch7,1, and C. Moreno-Jódar8,1
1Departamento de Física de la Tierra y Astrofísica & UPARCOS-UCM (Unidad de
Física de Partículas y del Cosmos de la UCM), Facultad de
Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
2Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal,
Universidad de Alicante, Apdo. 99 E-03080, Alicante, Spain
3Centro de Astrobiología (INTA–CSIC), ESAC campus, Camino Bajo del Castillo
s/n, E-28691 Villanueva de la Cañada, Madrid, Spain
4Leiden Observatory, Leiden University, 2300 RA Leiden, Netherlands
5Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, E-38200 La
Laguna, Tenerife, Spain
6Departamento Astrofísica, Universidad de La Laguna, E-38206 La Laguna,
Tenerife, Spain
7INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania,
Italy
8Escuela Técnica Superior de Ingeniería Aeronáutica y del Espacio, Plaza de
Cardenal Cisneros 3, E-28040, Madrid, Spain
E-mail<EMAIL_ADDRESS>
(Accepted 2018 May 09. Received 2018 May 09; in original form 2018 March 02)

###### Abstract

We investigated almost 500 stars distributed among 193 binary or multiple
systems made of late-F, G-, or early-K primaries and late-K or M dwarf
companion candidates. For all of them, we compiled or measured coordinates,
$J$-band magnitudes, spectral types, distances, and proper motions. With these
data, we established a sample of 192 physically bound systems. In parallel, we
carried out observations with HERMES/Mercator and obtained high-resolution
spectra for the 192 primaries and five secondaries. We used these spectra and
the automatic StePar code for deriving precise stellar atmospheric parameters:
$T_{\rm eff}$, $\log{g}$, $\xi$, and chemical abundances for 13 atomic
species, including [Fe/H]. After computing Galactocentric space velocities for
all the primary stars, we performed a kinematic analysis and classified them
in different Galactic populations and stellar kinematic groups of very
different ages, which match our own metallicity determinations and isochronal
age estimations. In particular, we identified three systems in the halo and 33
systems in the young Local Association, Ursa Major and Castor moving groups,
and IC 2391 and Hyades Superclusters. We finally studied the exoplanet-
metallicity relation in our 193 primaries and made a list 13 M-dwarf
companions with very high metallicity that can be the targets of new dedicated
exoplanet surveys. All in all, our dataset will be of great help for future
works on the accurate determination of metallicity of M dwarfs.

###### keywords:

proper motions – stars: abundances – binaries: visual – stars: fundamental
parameters – stars: late-type – stars: solar-type

††pubyear: 2018††pagerange: Calibrating the metallicity of M dwarfs in wide
physical binaries with F-, G-, and K- primaries – I: High-resolution
spectroscopy with HERMES: stellar parameters, abundances, and
kinematics††thanks: Based on observations obtained with the HERMES
spectrograph mounted on the 1.2 m Mercator Telescope at the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de
Canarias–B

##  1 Introduction

Cool, low-mass dwarfs of M spectral type are, by far, the most numerous
stellar constituents of the Milky Way. Having main-sequence lifetimes that
exceed the current age of the Universe (Baraffe et al., 1998; Henry et al.,
2006), M dwarfs stand as excellent objects in order to probe the structure and
evolution of the Milky Way’s thin and thick discs. Because of their ubiquity,
M dwarfs may also be the largest population of planet-hosting stars. As a
result, a large fraction of low-mass planets are expected to orbit an M-type
star within its habitable zone, which is considerably closer than for solar-
like ones.

Figure 1: Left panel: distribution of spectral types for the stars of our
sample. Blue and red bars represent primaries and secondary candidates,
respectively, while open and filled bars represent physical and optical
components, respectively. Note the tail of optical secondaries in the
background with spectral types much earlier than primaries. The late T dwarf
is GJ 570 D (Burgasser et al., 2000). Right panel: angular separation between
stars in pairs and their uncertainties, colour-coded with the difference in
$J$ magnitude.

More importantly, the detectability of any such planet via the transit and
radial-velocity techniques is enhanced by the lower masses and smaller radii
of M dwarfs (Clanton & Gaudi, 2014; Reiners et al., 2018). Therefore, M dwarfs
have become key targets for planet hunting (e.g. MEarth – Charbonneau et al.,
2009; Berta-Thompson et al., 2015; Dittmann et al., 2017). This is also
illsutrated by new spectrographs optimised for exoplanet searches around M
dwarfs (e.g. CARMENES – Alonso-Floriano et al., 2015a; Quirrenbach et al.,
2016; Reiners et al., 2018).

The observational efficiency of exoplanet searches around M dwarfs could be
vastly increased with prior knowledge of stellar metallicity. In this sense,
previous studies have already pointed out that planets are more likely to be
found orbiting metal-rich, solar-like stars (Santos et al. 2001, 2004; Fischer
& Valenti 2005 – but see below). However, the metallicity of low-mass dwarfs
has been an elusive fundamental property due to the complexity of modeling
their atmospheres. Fortunately, the advent of new observational techniques, as
well as independent theoretical improvements in atmospheric models, now seem
to link the metallicity of M dwarfs to both their photospheric and
spectroscopic features (Bonfils et al., 2005; Bean et al., 2006b; Woolf &
Wallerstein, 2006; Johnson & Apps, 2009; Hauschildt & Baron, 2010; Rojas-Ayala
et al., 2010, 2012; Önehag et al., 2012; Neves et al., 2014; Maldonado et al.,
2015; Passegger et al., 2018). Not only do these metallicity studies have deep
implications in the realm of stellar astrophysics, but they also play a
crucial role in the analysis of the Galactic evolution (West et al., 2011;
Woolf & West, 2012).

There were preliminary indications that the M dwarfs with known planets have
sub-solar metallicities (Bonfils et al., 2005; Bean et al., 2006b), in
contrast to their earlier counterparts. Actually, while giant planets
preferentially form around metal-rich stars, Neptunes and super-Earths are not
necessarily more abundant in metal-rich stars but they are abundant at solar
metallicity (Sousa et al., 2008; Adibekyan et al., 2012; Buchhave et al.,
2012). However, more recent results showed instead that planet-hosting M
dwarfs appear to be metal-rich (Johnson & Apps, 2009; Rojas-Ayala et al.,
2010; Terrien et al., 2012). We refer the reader to Hobson et al. (2018) for a
recent review on the planet-metallicty relation in M dwarfs.

A few studies have estimated M-dwarf metallicities using wide multiple systems
that consist of at least an M dwarf and a higher-mass star, typically of late
F-, G-, or early-K spectral type. Since binaries are assumed to be born in a
common parental cloud and be coeval, the composition of the FGK star, which
can be accurately derived from a careful comparison with theoretical models
and current tools, can be extrapolated to its companion M dwarf. However, in
some cases small differences in composition between components (often at a
level of $\approx$0.05 dex) may arise if they are comoving but not coeval,
there originally was chemical heterogeneity within the birth cloud, or some of
the components underwent accretion of planetary material after birth (see
Desidera et al., 2004; Teske et al., 2015; Brewer et al., 2016; Andrews et
al., 2018; Oh et al., 2018, and references therein). Some of these studies
have used optical and infrared spectroscopy to tie spectroscopic features to a
metallicity scale (Valenti et al., 1998; Woolf & Wallerstein, 2005, 2006; Bean
et al., 2006a; Bean et al., 2006b; Woolf et al., 2009; Rojas-Ayala et al.,
2010, 2012; Terrien et al., 2012; Mann et al., 2013, 2014, 2015; Gaidos &
Mann, 2014; Newton et al., 2014; Souto et al., 2017). Other studies have used
photometric calibrations. For example, Bonfils et al. (2005) and Johnson &
Apps (2009) used M dwarfs in wide binaries to derive a relation between
metallicity, absolute $K$-band magnitude, and the $V-K$ colour index (higher
metallicity M dwarfs are slightly brighter at a given colour – see also
Casagrande et al., 2008; Schlaufman & Laughlin, 2010; Johnson et al., 2012;
Neves et al., 2012).

To date, different authors with different methods have analysed only slightly
over one hundred wide FGK+M benchmark systems, which results in a lack of
homogeneity in the literature. A larger and homogeneous sample of wide visual
binaries and multiple systems covering a large range in metallicity and
spectral type is needed to reduce the scatter of the current calibrations and
to get a good calibration relationship that would be valid throughout the
parameter space. Here we start a series of papers devoted to improve the
spectroscopic calibration of the M-dwarf metallicity. In this first article,
we present our sample with a total of nearly 500 stars, study the common
proper motion of the multiple systems, and derive stellar atmospheric
parameters of the FGK “primaries” ($T_{\rm eff}$, $\log{g}$, $\xi$, and
chemical abundances for 13 atomic species).

##  2 Analysis

Figure 2: Left panel: $\Delta{\rm PA}$ vs. $\mu~{}{\rm ratio}$ diagram.
Physical (red filled circles), doubtful physical (red open circles) and
optical (blue crosses) attending to our criteria. Dashed vertical and
horizontal lines mark the 0.15 and 0.25 $\mu$ ratio and 15 deg $\Delta$PA.
Right panel: heliocentric distances for primary (1) and companion (2) stars
colour-coded with metallicity. Dashed lines indicate 1.5:1, 1:1, and 0.5:1 $d$
relationships, respectively. Black crosses represent optical pairs. Low-
metallicity stars tend to lie in the upper part of the 1:1 distance relation.

First of all, we collected from the literature 193 binary or multiple system
candidates formed by late-F, G-, or early K-type primaries and late-K or
M-type secondaries observable from Calar Alto, in Southern Spain ($\delta$
$\textgreater$ –23 deg). The main sources used to gather our initial sample
were searches for common proper motion companions (Gliese & Jahreiß, 1991;
Poveda et al., 1994; Poveda et al., 2009; Simons et al., 1996; Tokovinin,
1997; Gould & Chanamé, 2004; Zapatero Osorio & Martín, 2004; Caballero, 2007,
2009; Lépine & Bongiorno, 2007; Raghavan et al., 2010), as well as previous
metallicity calibrations of M dwarfs based on photometric and/or spectroscopic
data (see Section 1). The sample consists on 489 stars distributed in 193
binary or multiple candidate systems, from which 193 are late-F, G-, or early
K-type primaries, and 296 are companion candidates.

Table 6 lists the surveyed systems studied in this paper. For each of the 296
pairs of primaries and companion candidates, we tabulate its number and
discoverer code as provided by the Washington Double Star Catalog (WDS – Mason
et al., 2001). To avoid including too many spurious sources in the analysis,
we tabulate all components with designation A to D regardless of their WDS
notes (such as “Proper motion or other technique indicates that this pair is
non-physical”), and all the physical pair candidates regardless of their
designation (e.g. GJ 570 D is component G in WDS, HD 211472 B is component T
in WDS). We were not able to identify faint optical companions found in deep
adaptive optics surveys (e.g. Lafrenière et al. 2007; Ehrenreich et al. 2010;
Janson et al. 2013; Ammler-von Eiff et al. 2016) and the LDS 585 “D” companion
of the system WDS 17050–0504 (according to WDS, LDS 585 “D” is a dubious
double111“A dubious double (or Bogus binary) may represent a positional typo
in the original publication […], an optical double dissappearing due to
radically different proper motions, a plate flaw, or simply a pair not at a
magnitude, separation, etc., sufficiently similar to those noted when the
first measure was added” (Mason et al., 2001).). Three pairs have no WDS
entry, and are marked with “…” in the ‘Discoverer code’ field.

In Table 6 we also provide angular separation $\rho$ and position angle
$\theta$ measured by us with the Virtual Observatory tool TOPCAT (Taylor,
2005) from Two-Micron All Sky Survey (2MASS – Skrutskie et al., 2006) data,
Simbad’s star name, equatorial coordinates, $J$-band magnitude, and spectral
type from the literature. Fig. 1 shows the distribution of spectral types of
primaries and companions. Most spectral types of primaries range from F4 V to
K5 V, and of physical companions from K7 V to M7 V, while angular separations
range from 4 to about 4000 arcsec, with uncertainties lower than 0.4 arcsec.

The close companion candidates in four systems with very bright primaries,
namely WDS 04359+1631 (Aldebaran B), WDS 16147+3352 ($\sigma$ CrB “C”), WDS
19553+0624 ($\beta$ Aql B), and WDS 20462+3358 ($\epsilon$ Cyg B and C), were
not tabulated by 2MASS in spite of being visible in their images. Besides, the
88-arcsec wide companion candidate BD–13 5608B in system WDS 20124-1237 was
not tabulated by 2MASS due to a nearby speckle from the primary ($\xi$ Cap).
In these five cases, we computed $\rho$ and $\theta$ with the raw 2MASS
$H$-band images and Aladin Sky Atlas (Bonnarel et al., 2000).

In Table 15 we list heliocentric distances and proper motions of all the
investigated stars, which we used for discarding optical (non-physical) pairs.
First, we compiled parallactic distances in the following order from the
Tycho-Gaia Astrometric Solution (TGAS – Gaia Collaboration et al., 2016), the
new (HIP2 – van Leeuwen, 2007) and old (HIP1 – Perryman et al., 1997)
Hipparcos reductions, van Altena et al. (1995), and Prieur et al. (2014; only
for $\mu^{02}$ Her BC). All 193 primaries have parallactic distances, while
only 52 companions do. Of the remaining 244 companion candidates, we derived
our own spectro-photometric distances for 165 late K, and early and
intermediate M dwarfs resolved by 2MASS, using the spectral type–$M_{J}$
relation of Cortés-Contreras et al. (2017). As discussed in Section 4.2, this
relationship is applicable only to main-sequence late-type dwarfs of solar
metallicity, and the tabulated spectro-photometric distances of low-
metallicity dwarfs must be handled with care. For two secondaries with $J$
magnitude and reliable spectral type ($\eta$ Cas B in WDS 00491+5749, and
BD+48 3952B in WDS 23104+4901) we did not derive any distance because their
2MASS quality flags indicate a poor photometry. Besides, there are two
physical companions, a white dwarf and a brown dwarf, with both spectral type
and near-infrared magnitudes without a distance derived by us, namely $o^{02}$
Eri B (DA2.3) in WDS J04153-0739, and GJ 570 D (T8) in WDS 14575-2125.
Atogether, there are only 74 companion candidates without any heliocentric
distance determination.

Next, we compiled proper motions for the 193 primaries and 293 (all but three)
companions from the following catalogues and works: TGAS, Hot Stuff for One
Year (HSOY – Altmann et al., 2017), HIP2, UCAC5 (Zacharias et al., 2017),
Tycho-2 (Høg et al., 2000), PPMXL (Roeser et al., 2010), UCAC4 (Zacharias et
al., 2012), Caballero (2009), Faherty et al. (2009, for GJ 570 D), and Ivanov
(2008, for Aldebaran B), in this order. For 37 stars (36 secondaries and the
primary 39 Leo A in WDS 10172+2306) with probably wrong proper motions or no
proper motions whatsoever, we improved or measured their values for the first
time. To do so, we used the method used by Caballero (2009) and the
astrometric epochs from DENIS (Epchtein et al., 1997), USNO-A2 (Monet, 1998),
2MASS, GSC2.3 (Lasker et al., 2008), AllWISE (Cutri & et al., 2014), CMC15
(Muiños & Evans, 2014), Gaia DR1 (Gaia Collaboration et al., 2016), and, in
the most difficult cases, the SuperCOSMOS digitalization of the Digital Sky
Survey photographic plates (Hambly et al., 2001). The time baseline varied
between 4.5 and 119.3 years, with a median of seven astrometric epochs per
star. As for the distances, we did not assign proper motions of primaries to
companions. We were not able to compile or measure by ourselves any proper
motions of the secondaries in the systems WDS 00491+5749 ($\eta$ Cas AB; first
measured in 1779), WDS 11378+4150 (BD+42 2230 AC; first detected in 1998) and
WDS J21546–0318 (HD 208177 AB; first observed in 1829).

With the distances and proper motions in Table 15, we set a uniform criterion
to distinguish between physical (bound) and optical (unbound) systems (Fig. 2,
left panel). First, we computed two parameters for each pair of stars: the
$\mu~{}{\rm ratio}$, defined as:

$\left(\mu\,\rm
ratio\right)^{2}\,$=$\,\dfrac{\left(\mu_{\alpha}\cos{\delta}\,_{1}-\mu_{\alpha}\cos{\delta}\,_{2}\right)^{2}\,\text{+}\,\left(\mu_{\delta\,1}-\mu_{\delta\,2}\right)^{2}}{\left(\mu_{\alpha}\cos{\delta}\,_{1}\right)^{2}\text{+}\,\left(\mu_{\delta\,1}\right)^{2}},$
(1)

and the proper motion position angle difference:

$\Delta{PA}\,$=$\,\left|{PA_{1}-PA_{2}}\right|,$ (2)

where $PA_{i}$ is the angle between $\mu_{\alpha}\cos{\delta}_{i}$ and
$\mu_{\delta,i}$, being $i$ = 1 for the primary star and $i$ = 2 for the
companion candidate.

We discarded 84 pairs of stars that have: ($i$) $\mu~{}{\rm ratio}>$ 0.15,
and/or ($ii$) proper motion position angle difference $\Delta{\rm PA}>$ 15 deg
(compare with the selection criteria in e.g. Lépine & Bongiorno 2007, Dhital
et al. 2010, and Alonso-Floriano et al. 2015b). Besides, we investigated in
detail the three pairs with $\Delta{\rm PA}<$ 15 deg and 0.15 $<\mu~{}{\rm
ratio}<$ 0.25. Two of them, namely WDS 15282-0921 AC and WDS 23026+2948 AC,
are very wide pairs ($\rho$ > 1000 arcsec) that are affected by high proper
motion projection effect (as between $\alpha$ Cen AB and Proxima). The third
pair, WDS 23536+1207 AB (VYS 11), is a close binary of $\rho$ = 5.7 arcsec
already investigated by Tokovinin & Kiyaeva (2016). We also classified these
three systems as physical despite they did not pass our $\mu$ ratio criterion.
We must wait for $Gaia$ DR2 to confirm them. Overall, we have 209 physical
pairs distributed in 192 systems. We only discarded the source WDS 10585-1046
(LDS 4041).

As a double check, we compared the compiled and derived heliocentric distances
of primaries and companions (Fig. 2, right panel). For systems with
parallactic distances only, they vary less than 15 %, while for systems with
spectro-photometric distances, they vary less than 50 %, except for three
pairs with low metallicities (Section 4.2). To assure that we did not reject
any physical pair because of abnormal metallicity, we did not discard any pair
based on different heliocentric distances. New parallax-based distances, such
as the ones provided by Gaia DR2 (Gaia Collaboration et al., 2018), are
invaluable since they are independent of metallicity and stellar parameter
analyses.

Figure 3: Histogram of signal-to-noise ratios measured in our HERMES spectra.

##  3 Spectroscopy and kinematics

###  3.1 Observations and reduction

Figure 4: High-resolution spectra of three representative primaries from our
sample (from top to botom): $\theta$ Per, HD 129290 A, and V452 Vul (HD
189733). Top: Full investigated wavelenght range. Bottom: zoomed range, 10 nm
wide, near H$\alpha$ $\lambda$ 656.3 nm.

FGK-type stars of the multiple systems described above are relatively bright,
$J<$ 9.0 mag ($V<$ 11.0 mag), which allowed us to obtain high signal-to-noise
ratio, high-resolution, optical spectra with reasonable exposure times
($t_{\rm exp}\leq$ 20 min), and to derive reliable stellar parameters and
abundances. We took high-resolution echelle spectra of 192 primaries and 5
secondaries with HERMES (High Efficiency and Resolution Mercator Echelle
Spectrograph – Raskin et al., 2011) at the 1.2 m Mercator Telescope at the
Observatorio del Roque de los Muchachos (La Palma, Spain) between January 2010
and December 2017. We used the high resolution mode, which provides with a
spectral resolution of 86,000 in the approximate wavelength range from
$\lambda$ 380 nm to $\lambda$ 875 nm. Most of the spectra have a signal-to-
noise ratio (SNR) between 60 and 140 in the $V$ band, as shown in the third
column of Table 24 and Fig. 3. Additionally, we took several spectra of the
asteroid Vesta with the same spectrograph configuration. All the obtained
spectra were reduced with the automatic pipeline for HERMES (Raskin et al.,
2011). Next, we used several standard tasks within the IRAF environment for
normalising the spectra, using a low-order polynomial fit to the observed
continuum, and for applying the corresponding Doppler correction. To do so, we
computed the observed radial velocity ($V_{r}$), which is the sum of the
spectrum relative velocity (measured with the IRAF function fxcor) and
barycentric correction (obtained from the FITS header). When several exposures
were available for the same star, we combined all the individual spectra and
obtained a unique spectrum with higher SNR. For our analysis we used only the
wavelength range from 450 nm to 700 nm (Fig. 4). The 197 stars observed with
HERMES are marked with “H” in the last column of Table 6.

We also observed many M-dwarf companions with the low-resolution optical
spectrograph CAFOS at the 2.2 m Calar Alto telescope. They are marked with “C”
(Alonso-Floriano et al., 2015a) and “C*” (unpublished) in the last column of
Table 6. We are using these spectra for calibrating spectral indices and
abundance determinations with features analysed at high spectral resolution,
and will appear in forthcoming publications. In particular, seven of our
M-dwarf companions (namely BX Cet, $o^{02}$ Eri C, HD 233153, BD–02 2198,
$\rho^{01}$ Cnc B, $\theta$ Boo B, and HD 154363 B) have also been observed
with the CARMENES spectrograph with very high SNR and spectral resolution
(Quirrenbach et al., 2016; Reiners et al., 2018).

###  3.2 Stellar parameters

Figure 5: Upper panel: Effective temperature as a function of spectral type. Middle panel: Error in effective temperature as a function of the effective temperature. Down panel: Microturbulence velocity ($\xi$) against effective temperature. All the symbols are colour-coded with SNR. Black-ensquared stars represent low-gravity stars (Section 4.4). Table 1: Solar parameters and element abundances. Parameter |
---|---
$T_{\rm eff}$ [K] | 5777$\pm$18
$\log{g}$ | 4.41$\pm$0.05
$\xi$ [km s-1] | 0.91$\pm$0.03
Element |  $\log{\epsilon}$ (X)
Fe | 7.48$\pm$0.01
Na | 6.44$\pm$0.03
Mg | 7.69$\pm$0.05
Al | 6.51$\pm$0.01
Si | 7.59$\pm$0.07
Ca | 6.44$\pm$0.05
Sc | 3.15$\pm$0.03
Ti | 5.02$\pm$0.05
V | 4.03$\pm$0.03
Cr | 5.70$\pm$0.05
Mn | 5.51$\pm$0.03
Co | 4.95$\pm$0.03
Ni | 6.30$\pm$0.07

Stellar atmospheric parameters (effective temperature $T_{\rm eff}$, surface
gravity $\log{g}$, microturbulence velocity $\xi$, and iron abundance [Fe/H],
Section 4.2) were computed using the automatic StePar code (Tabernero, Montes
& González Hernández, 2012), which relies on the equivalent width ($EW$)
method. We employed the 2014 version of the MOOG code (Sneden, 1973) and a
grid of Kurucz ATLAS9 plane-parallel model atmospheres (Kurucz, 1993). As the
damping prescription, we used the Unsöld approximation multiplied by a factor
recommended by the Blackwell group (“option 2” within MOOG). We employed the
line list of $\sim$300 solar-calibrated Fe i and Fe ii lines from Sousa et al.
(2008). We measured their $EW$s using ARESv2 (Sousa et al., 2015). ARES input
parameters were set to those recommended in its
manual222https://github.com/sousasag/ARES,
http://www.astro.up.pt/~sousasag/ares/. The StePar code iterates within the
parameter space until the slopes of $\chi$ vs. $\log{\epsilon}$(Fe i) and
$\log{(EW/\lambda)}$ vs. $\log{\epsilon}$(Fe i) are zero (i.e. the iron atoms
are in excitation equilibrium). In addition, it imposes the ionisation
equilibrium, such that $\log{\epsilon}$(Fe i)=$\log{\epsilon}$(Fe ii). We also
imposed that the [Fe/H] average of the MOOG output is equal to the iron
abundance of the atmospheric model.

Table 24 shows the stellar atmospheric parameters of 198 F-, G-, and K- stars
in our sample (193 primaries and 5 secondaries). The StePar code is based on
an $EW$ method that is meant to work for a limited range of $T_{\rm eff}$. We
were not able to determine with StePar the stellar atmospheric parameters of
21 stars:

  * •

Hot. Stars with spectral types earlier than F6 ($T_{\rm eff}\approx$ 6700 K)
do not have enough iron lines for our analysis. The triple system 9 Aur
Aa,Ab,B comprises three stars of spectral types F2 V and early M, and the
effective temperature reported in the literature is $\sim$7000 K (Allende
Prieto & Lambert, 1999; Le Borgne et al., 2003). The star HD 27887 A, with an
F5 V spectral type and $T_{\rm eff}\approx$ 6500 K (Allende Prieto & Lambert,
1999; Katz et al., 2011) is at the boundary of our grid, and StePar did not
converge either.

  * •

Cool. Stars with spectral types later than K4 ($T_{\rm eff}\approx$ 4500 K),
on the contrary to hot stars, have too many overlapping iron lines. We were
not able to derive parameters for Aldebaran (K5 III, 3900 K; Soubiran et al.
1998; Prugniel et al. 2011) and SZ Crt (K7 V, 4200 K; Wright et al. 2011; Luck
2017).

  * •

Fast. At high rotational velocities, iron lines become so broad that overlap,
too. Six stars rotate too fast for StePar, i.e. have $v\sin{i}\gtrsim$ 10 km
s-1. Published $v\sin{i}$ values for the six of them range from 16.2 km s-1
for V368 Cep (Mishenina et al., 2012) to 84.8 km s-1 for $\eta$ UMi A
(Schröder et al., 2009).

  * •

SB2. We discarded double-line spectroscopic binaries with blended or partially
blended lines. We found double peaks in spectral lines of eight primary stars;
as discussed in Section 4.1, four are reported here for the first time. We
were able to derive stellar atmospheric parameters for HD 200077 Aa1, the
primary of a known SB2 (see Section 4.1). There is a ninth SB2 in our sample,
namely $\sigma$ CrB Aa,Ab (Bakos, 1984).

  * •

No obs. We could not observe only one primary, the SB2 $\sigma$ CrB Aa,Ab.

To sum up, we derived reliable spectroscopic stellar parameters for 175
primaries and 5 companions. Only $\sigma$ CrB Aa,Ab (the “193rd” primary star)
lacks our homogeneous spectroscopy. Stellar parameters derived with StePar are
given in Table 24, together with [Fe/H] from the literature, when available.
Fig. 5 shows the effective temperature and other parameters derived by us. In
addition, as can be seen in the top part of Table 1, we have successfully
derived the atmospheric parameters of the Sun ($T_{\rm eff}$, $\log{g}$,
$\xi$) by means of a solar spectrum (Vesta) taken with the HERMES
spectrograph.

###  3.3 Abundances

In order to calculate the individual chemical abundances of the 180 stars, we
assumed the stellar parameters derived with StePar. We obtained abundances for
13 different chemical species: Fe, the $\alpha$-elements (Mg, Si, Ca, and Ti),
the Fe-peak elements (Cr, Mn, Co, and Ni), and the odd-Z elements (Na, Al, Sc,
and V). We calculated chemical abundances using the $EW$ method, Kurucz ATLAS9
plane-parallel model atmospheres (Kurucz, 1993), and the MOOG code (Sneden,
1973), as in Tabernero et al. (2012); Tabernero et al. (2017). The $EW$s were
determined using the ARES code (Sousa et al., 2015), following the approach
described in Section 3.2. We also re-measured manually the EWs with the task
splot within the IRAF environment when any individual abundance determination
of particular lines was separated from the general trend. We computed final
abundances in a differential manner (i.e., in a line-by-line basis) with
respect to our solar spectrum (Vesta) observed with HERMES. See the resulting
solar element abundances ($\log{\epsilon}$ (X)) in the bottom part of Table 1.
Table 28 reports these differential abundances ([X/H]) thus derived for our
star sample.

###  3.4 Kinematics

Stellar kinematic groups (SKGs), superclusters (SCs), and moving groups (MGs)
are kinematic coherent groups of stars that may share a common origin and,
therefore, age and chemical composition (Boesgaard & Friel, 1990; Eggen, 1994;
De Silva et al., 2007; Famaey et al., 2008; Antoja et al., 2009). Among them,
the youngest SKGs are: the Hyades SC ($\sim$600 Myr), Ursa Major MG (Sirius SC
– $\sim$400 Myr), Castor MG ($\sim$300 Myr), Local Association (Pleiades MG –
20 to 150 Myr), and IC 2391 SC (35–55 Myr), We refer the reader to Montes et
al. (2001), López-Santiago et al. (2006), Klutsch et al. (2014), Riedel et al.
(2017) and references therein for more details.

Other very young SKGs, such as the $\epsilon$ Chamaeleontis, TW Hydrae,
$\beta$ Pictoris, Tucana-Horologium, AB Doradus, Columba, Carina, and
Hercules-Lyra moving groups, have kinematics close to the Local Association,
as well as Argus’ to IC 2391, and Octans and Octans-Near’s to Castor
(Zuckerman & Song, 2004; Torres et al., 2008; Montes, 2010, 2015; Bell et al.,
2015). Even new associations are identified, such as the All Sky Young
Association (ASYA – Torres et al. 2016).

With the coordinates in Table 6, parallactic distances and proper motions in
Table 15, and radial velocities measured in Section 3.1, we computed
Galactocentric space velocities as in Montes et al. (2001) with the procedure
established by Johnson & Soderblom (1987). For the single- and double-lined
spectroscopic binaries (Section 4.1) and the unobserved star $\sigma$ CrB
Aa,Ab, we adopted their systemic radial-velocity values $\gamma$ from the
literature. Table 32 lists the used radial velocities $V_{r}$ along with the
computed space velocities $U$, $V$, and $W$ of our 198 F-, G-, and K- stars.

##  4 Results and discussion

We investigated 489 stars distributed in 193 systems, formed by 193 primary
F-, G-, and K- stars and 296 common proper-motion companions and candidates
(Table 6). For these systems, we studied their proper motions and distances,
as explained in Section 2. We got a final sample of 192 physical systems, of
which 135 are double and 57 are multiple (43 triple, 9 quadruple, and 5
quintuple). In Table 15 we marked the 84 discarded stars, along with other
useful remarks for the remaining stars.

###  4.1 Spectroscopic binaries

Table 2: Primary spectroscopic binaries. WDS | Name | Type | Referencea
---|---|---|---
00452+0015 | HD 4271 Aa,Ab | SB1 | Gri01
00491+5749 | Archid Aa,Ab | SB1 | A&L76
02291+2252 | BD+22 353Aa,Ab | SB1 | Hal12
02482+2704 | BC Ari Aa,Ab | SB1 | Lat02
03206+0902 | HD 20727 Aa,Ab | SB1 | D&M91
03396+1823 | V1082 Tau Aa,Ab | SB2 | Lat92
03398+3328b | HD 278874 Aa,Ab | SB2 | This work
03566+5042 | 43 Per Aa,Ab | SB2 | Wal73
05067+5136 | 9 Aur Aa,Ab | SB1 | Abt65
05289+1233 | HD 35956 Aa,Ab | SB1 | Kat13
06173+0506c | HD 43587 | SB1 | Kat13
09245+0621b | HD 81212 AB | SB2 | This work
09393+1319 | HD 83509 Aa,Ab | SB2 | Gri03
15282-0921c | HD 137763 | SB1 | D&M92
16147+3352d |  $\sigma$ CrB Aa,Ab | SB2 | Bak84
16329+0315c | HD 149162 | SB1 | Lat02
16348-0412 | HD 149414 Aa,Ab | SB1 | Lat02
20169+5017 | HD 193216 Aa,Ab | SB1 | Gri02
20462+3358 |  $\epsilon$ Cyg Aa,Ab | SB1 | Gra15
20599+4016c | HD 200077 Aa1,Aa2,Ab | SB2 | Gol02
23026+2948b | BD+29 4841Aa,Ab | SB2 | This work
23581+2420b | HD 224459 Aa,Ab | SB2 | This work
a Reference – Abt65: Abt (1965); A&L76: Abt & Levy (1976);
Bak84: Bakos (1984); D&M91: Duquennoy & Mayor (1991);
D&M92: Duquennoy et al. (1992); Gol02: Goldberg et al. (2002);
Gra15: Gray (2015); Gri01: Griffin (2001); Gri02: Griffin (2002);
Gri03: Griffin (2003); Hal12: Halbwachs et al. (2012);
Kat13: Katoh et al. (2013); Lat92 Latham et al. (1992);
Lat02: Latham et al. (2002); Wal73: Wallerstein (1973).
b New SB2, discovered in this work.
c Resolved close multiple system described in text.
d Not observed by us.

As discussed in Section 3.2, we were not able to determine stellar parameters
for seven double-peak spectroscopic binaries (SB2s). They are listed in Table
2, together with the other SB2s $\sigma$ CrB Aa,Ab (not observed) and HD
200077 Aa,Ab (with stellar parameters). We report for the first time four
SB2s, namely HD 278874 Aa,Ab, HD 81212 AB, BD+29 4841 Aa,Ab, and HD 224459
Aa,Ab. Only for the later, we have two HERMES spectra separated by one day but
we could not see any significant difference between them, so the orbital
period must be $P_{\rm orb}\gg$ 1 d. Interestingly, HD 81212 AB was found to
be an astrometric binary by F. G. W. Struve in 1831. The pair is separated by
$\rho$ = 1.1–1.9 arcsec and, thus, unresolved by us. The very small magnitude
difference between A and B, $\Delta m\approx$ 0.12 mag, indicates a mass ratio
close to unity. We estimate an orbital period of 200–300 yr for the
astrometric pair, and a radial-velocity difference of about 6 km s-1, which is
consistent with what we observe in the double-line spectroscopic binary.
Therefore, the spectroscopic binary can actually be the astrometric binary.
This fact could also explain the apparently wrong parallax tabulated by TGAS.
The other three new SB2 stars are not known close astrometric binaries.

Figure 6: Left panel: iron abundance published in the literature against that
obtained in this work, colour-coded with SNR. Black dashed line represents 1:1
relation. Right panel: iron abundance as a function of effective temperature
for our primary stars, colour-coded with $\log{g}$. Black-ensquared stars
represent low-gravity stars.

There are full orbital parameters ($P$, $e$, $\gamma$, $K_{1}$, $K_{2}$)
available in the literature for the other five stars, including $\sigma$ CrB
Aa,Ab and HD 200077 (S${}_{{\rm B}^{9}}$ – Pourbaix et al., 2004). The later
is part of a quintuple system containing a close SB2 (F8 V + G6–9:, $P$ =
112.5 d) first resolved by Horch et al. 2012 (LSC 1, $\rho\approx$ 0.022
arcsec), a close companion resolved by Hipparcos (late K; COU 2431, $\rho$ =
2.2 arcsec), and the wide cool companion G 210–44 (K7 V + M0–1:), which is in
turn another close binary (Latham et al., 1988; Goldberg et al., 2002; Mazeh
et al., 2003; Caballero, 2009). In our HERMES spectra of HD 200077, the Aa1
component (late F) dominates over Aa2 (late G) and Ab (late K, not visible),
and its lines were well separated from those of the other components.

Besides, there are 13 known single-line spectroscopic binaries (SB1) in our
sample. We did not discard them in our analysis because the determined stellar
parameters correspond to the primary in the system and were not significantly
affected by the companion. Four of the SB1s were also resolved
astrometrically:

  * •

HD 43587 (CAT 1, $\rho\approx$ 0.90 arcsec). The orbital period of $P$ = 34.2
yr determined by Katoh et al. (2013) from radial-velocity monitorisation
matches reasonably well the adaptive optics observations by Catalá et al.
(2006). The system deserves a new analysis given the low mass of the
companion, several magnitudes fainter than the primary.

  * •

HD 137763 (BAG 25, $\rho\approx$ 0.10 arcsec). The orbital period of $P$ =
2.44 yr determined by Duquennoy et al. (1992) also matches the measured
projected physical separations measured astrometrically (Jancart et al., 2005;
Balega et al., 2006; Horch et al., 2015), and, therefore, the dynamical masses
of the two stars can be determined precisely.

  * •

HD 149162 (DSG 7, $\rho\approx$ 0.0148 arcsec and $\rho\approx$ 0.284 arcsec).
Again, the astrometric measurements of Horch et al. (2015) agree with the
spectroscopic measurements of Latham et al. (2002), who determined an orbital
period of 0.620 yr. This is a hierarchical triple system, and the seven-month
period of the SB1 corresponds to the closest pair. The effect of the component
at $\sim$0.3 arcsec is not discernible spectroscopically. The wide common
proper motion companion, at 4.2 arcmin to the south east, is in turn a binary
made of an M3.0 V star and a white dwarf, which makes HD 149162 a quintuple
system.

  * •

$\epsilon$ Cyg (CHR 100, $\rho$ = 0.041 arcsec). This well-studied, binary
giant star has been the subject of numerous radial-velocity surveys (e.g.
Griffin 1994; Gray 2015) and has also been resolved with optical
interferometry (Hartkopf et al., 1994).

###  4.2 [Fe/H]

Table 3: Estimated ages for the seven low-gravity stars ($\log{g}$ < 4.1) with stellar parameters in our sample. WDS | Simbad | $\log{g}$ | [Fe/H] | Estimated | Published | Referencea
---|---|---|---|---|---|---
|  |  |  | age [Gyr] | age [Gyr] |
01572-1015 | HD 11964 A | 3.85$\pm$0.06 | 0.06$\pm$0.02 |  $\sim$5–10 | 9.77$\pm$0.52 | Tsa13
05466+0110 | HD 38529 A | 3.75$\pm$0.07 | 0.32$\pm$0.02 |  $\sim$2–5 | 3.77$\pm$0.36 | Ram12
08110+7955 | BD+80 245 | 3.63$\pm$0.20 | –1.58$\pm$0.07 |  $\sim$13–14 | … | …
11523+0957 | HD 103112 | 3.75$\pm$0.19 | 0.22$\pm$0.06 |  $\sim$10 | … | …
17465+2743 |  $\mu^{01}$ Her A | 4.03$\pm$0.04 | 0.27$\pm$0.02 |  $\sim$10 | 7.88$\pm$0.24 | Ram12
19553+0624 |  $\beta$ Aql A | 3.64$\pm$0.06 | –0.16$\pm$0.01 |  $\sim$2–5 | 4.08$\pm$3.95 | Ram13
20462+3358 |  $\epsilon$ Cyg A | 2.74$\pm$0.11 | –0.11$\pm$0.03 |  $\sim$1 | 0.90$\pm$0.20 | daS15
aReference – Ram12: Ramírez et al. (2012); Ram13: Ramírez et al. (2013);
Tsa13: Tsantaki et al. (2013);
daS15: da Silva et al. (2015).

We derived stellar atmospheric parameters of 175 primaries and five
secondaries (Section 3.2 and Table 24), from which 50 are presented here for
the first time. One of the parameters is the iron abundance [Fe/H], which is
the most used proxy for metallicity. In the left panel of Fig. 6, we depict
spectroscopic [Fe/H] collected from the literature against the ones derived by
us. For a fair comparison, we only collected spectroscopic [Fe/H] from the
literature (e.g., Valenti & Fischer, 2005; Sousa et al., 2011; Ramírez et al.,
2013; Santos et al., 2013), and did not take into account the ones derived
photometrically (e.g., Bonfils et al., 2005; Johnson & Apps, 2009; Schlaufman
& Laughlin, 2010). We compiled and selected spectroscopic [Fe/H] with the
PASTEL Catalogue (Soubiran et al., 2016), giving priority to the most recent
works. According to the diagram, our values agree very well with the published
ones, mainly in the range of –1.0 < [Fe/H] < 0.5 and no significant offset is
detected. The iron abundance determined by us does not display any trend as a
function of $T_{\rm eff}$ or $\log{g}$, as shown in the right panel of Fig. 6,

The least metallic star in our sample is the red giant branch star BD+80 245
(G0 IV). We measured [Fe/H] = –1.58$\pm$0.07, a value slightly higher than
those provided by Fulbright (2000, [Fe/H] = –2.05), Stephens & Boesgaard
(2002, [Fe/H] = –1.76), and Roederer et al. (2014, [Fe/H] = –2.04). BD+80 245
was also studied by Ivans et al. (2003), who classified it as a halo star
based on its chemical composition (we also classified it as a halo star in
Section 4.5 based on kinematics), and explained a possible formation from
material polluted by the earliest supernovae Ia events that occurred in the
Milky Way. BD+80 245 is the only star that stays away from the general trend
in the left panel of Fig. 6.

In general, [Fe/H] has an effect on the derivation of spectro-photometric
distances (Section 2). As illustrated in Fig. 2, stars with [Fe/H] < –0.4 tend
to lie in the upper part of the 1:1 relation between primary and “secondary”
distances. This effect may be due to an intrinsic offset in the spectral
type–$M_{J}$ relation used to derive spectro-photometric distances to our
late-K and M dwarfs, as Cortés-Contreras et al. (2017) assumed solar
metallicity (all 192 physical primaries have parallactic distances but 160
companions have spectro-photometric distances). The two low-metallicity
systems that suffer more from this offset are WDS 03150+0101 (BD+00 549A, with
[Fe/H] = –0.88, and BD+00 549B), and WDS 22090-1754 (HD 210190, with [Fe/H] =
–0.42, and LP 819-37, with $\zeta$ = 0.856, where $\zeta$ is a metallicity
spectral index defined by Lépine et al. 2007 and measured by Alonso-Floriano
et al. 2015a). For these systems, the spectro-photometric distances for the
secondary component are about twice as large as the parallactic distance of
the primary.

Besides, for WDS 16348-0412 (HD 149414 Aa,Ab, with [Fe/H] = –1.16, and GJ
629.2B, with $\zeta$ = 0.664) we did not derive a spectro-photometric distance
for the secondary because it is a sub-dwarf candidate (sdM0:, Alonso-Floriano
et al. 2015a)333Note the wrong spectral type of GJ 629.2B in Simbad.. Instead,
we adopted the spectro-photometric distance of 48${}^{\text{+}12}_{-9}$ pc
from the $M_{J}$-SpT relationship for subdwarfs in Zhang et al. (2013), which
agrees with the distance to its very low metallicity primary tabulated by TGAS
of 46.3$\pm$0.9 pc. We concluded that the metallicity affects the derivation
of our spectro-photometric distances, but heterogeneously and in extreme
cases.

###  4.3 Abundances

Apart from iron, we measured chemical abundances of 12 different elements for
the 180 F-, G-, and K- stars in our sample (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr,
Mn, Co, and Ni – see Section 3.3 and Table 28). Galactic trends are depicted
in Figs. 11 and 12 where we plot the abundance ratios of [X/Fe] versus [Fe/H]
for each element X. We compared them to the FGK stellar sample from Adibekyan
et al. (2012). Our sample covers a wide range of [Fe/H] and includes a few
low-metallicity stars ([Fe/H] $<$ –1.0) that fall well below the range studied
by Adibekyan et al. (2012) and, as expected, have enhanced content in $\alpha$
elements (Bensby et al., 2014; Jofré et al., 2015).

Using our line-by-line differential analysis we reproduced the expected
behaviour of the different chemical species, with manganese being a remarkable
exception. Useful Mn lines are scarce and difficult to measure in our HERMES
spectra either by hand (with IRAF splot) or with a semiautomatic method (using
the ARES code), and thus our results present an offset that reflects this
fact. Interestingly, we also reproduced the scatter found by Adibekyan et al.
(2012) for vanadium and scandium, which is a known issue for stars cooler than
5000 K (see Neves et al. 2009 and Tabernero et al. 2012 for further details).
Giants and subgiants tend to deviate from the general trends. Although this
effect appears to be entirely real (Smiljanic, 2012; Tabernero et al., 2012),
it is not observed in these cases, and, therefore, may be an effect only on
very low gravity stars ($\log{g}\leq$ 2.5).

###  4.4 Giants and subgiants

Figure 7: Surface gravity as a function of effective temperature for our
primary stars, colour-coded with metallicity. Red dashed lines correspond to
isochrones of [Fe/H] = 0.0 and ages of 1, 2, 5, and 10 Gyr, from top to
bottom. Blue dashed lines correspond to isochrones of [Fe/H] = –1.5 and ages
of 13 and 14 Gyr. All isochrones are from YaPSI (Spada et al., 2017). The
grey, horizontal, dashed line correspond to $\log{g}$ = 4.1.

Among our list of 192 physical primaries there are eight stars with surface
gravities lower than $\log{g}$ = 4.1 (see Fig. 7). They are Aldebaran
($\log{g}$ = 1.66; Prugniel et al. 2011), for which we were not able to
determine stellar parameters with StePar, the giant star $\epsilon$ Cyg A
($\log{g}$ = 2.74), BD+80 245 ($\log{g}$ = 3.63), which is the red giant
branch star with the lowest metallicity in our sample, and five subgiant stars
with $\log{g}$ = 3.64–4.03. Of them, HD 103112 had not been reported before to
display any subgiant class or low-gravity feature in its spectra (but see
McDonald et al. 2017 and their photometric analysis). The remaining four
subgiants are quite well investigated, either because of their brightness
($\beta$ Aql A and $\mu^{01}$ Her A) or presence of exoplanets (HD 11964 A and
HD 38529 A; Section 4.6).

For the seven low-gravity stars with derived stellar parameters, we estimated
their ages using the Yale-Potsdam Stellar Isochrones (YaPSI – Spada et al.,
2017) with two different iron abundances ([Fe/H] = 0.0 and [Fe/H] = –1.5) and
fixed solar helium abundance (Y = 0.28; see again Fig. 7). Estimated ages
agree within uncertainties with published values in five cases (Table 3). We
determined ages for the first time for the two remaining stars: the poorly-
investigated subgiant HD 103112 and the very low-metallicity star BD+80 245.
For the later, we infer an age similar to that of the Universe (limited by the
accuracy of the YaPSI models), which is consistent with the hypothesis of
Ivans et al. (2003) of it being a halo star polluted by the earliest supernova
explosions.

###  4.5 Kinematics

Figure 8: Toomre diagram of our F-, G-, and K- stars. Black stars: halo; black
filled circles: thick disc; grey semi-filled circles: thick-to-thin transition
disc; grey open circles: thin disc. Blue: Hyades SC; red: Local Association;
green: Ursa Major MG; magenta: IC 2391 SC; cyan: Castor MG; orange: other
young stars. Dashed grey lines represent constant values of the total space
velocity $v_{tot}$=($U^{2}\text{+}V^{2}\text{+}W^{2}$)1/2 in steps of 50 km
s-1. The Galactocentric space velocities $U$, $V$, and $W$ are referred to the
local standard of rest. Figure 9: Same as Fig 8, but for the Böttlinger
diagrams. Crosses mark the centres of each young SKG. Upper panels represent
zoomed areas of lower panels. In the top left panel, the dashed grey line
confines the young disc population as defined by Eggen (1984, 1989).

As illustrated by the Toomre diagram (Fig. 8), we classified each star in the
different Galactic populations, halo (H), thick disc (TD), thick-to-thin
transition disc (TD-D), and thin disc (D), as in Bensby et al. (2003, 2005).
For that, we assumed Gaussian distributions of space velocities $U$, $V$, and
$W$. We found 165 stars in the thin disc, 23 in the thick disc, 7 in the
thick-to-thin transition disc, and 3 in the halo, as it is shown in Table 32
and Fig. 8. The three stars in the halo are:

  * •

Ross 413. It is a halo star catalogued by Allen & Monroy-Rodríguez (2014) in
the context of MACHO studies. The iron abundance derived by us, [Fe/H] =
–0.58, is again slightly higher than the published value ([Fe/H] = –0.77;
Woolf & Wallerstein 2005).

  * •

BD+80 245. It is the old, low-metallicity, subgiant star discussed above. Our
classification as an halo star agrees with the one published in Ivans et al.
(2003; see Section 4.2).

  * •

HD 149414. It is a well-studied halo star (e.g. Sandage 1969; Tomkin & Lambert
1999; Gratton et al. 2003; Allen & Monroy-Rodríguez 2014), and the star with
the second lowest iron abundance in our sample ([Fe/H] = –1.16). Besides, it
is also a single-lined spectroscopic binary (Table 4.1).

In general, thick-disc (and also thick-to-thin-transition-disc) stars have
subsolar metallicities. However, there are some remarkable outliers, such as
HD 102326 ([Fe/H] = +0.15$\pm$0.02), HD 103112 ([Fe/H] = +0.22$\pm$0.06), and
HD 190360 ([Fe/H] = +0.21$\pm$0.02), which may represent the tail of the
distribution towards high metallicities or, conversely, a kinematic
classification at the boundary with the thin disc.

Next, for the stars in the thin disc, we separated between young disc stars
and non-young disc stars (designated with the symbol ’$\times$’ in Table 32)
as defined by Eggen (1984, 1989) and depicted in the Böttlinger diagram (Fig
9). Thick disc, thick-to-thin transition disc, and halo stars are also non-
young disc stars. Besides, for each young disc star, we studied its membership
in known SKGs, also as in Montes et al. (2001). In particular, we identified
33 star candidates in SKGs: 12 stars in the Local Association, 10 in the
Hyades SC, eight in the Ursa Major MG, two in the IC 2391 SC, and one in the
Castor MG, whereas 20 are young disc star with no apparent SKG membership
(designated with ’YD’ in Table 32). Also, we checked the membership of our 33
young Galactic disc stars with the LACEwING (Riedel et al., 2017) and BANYAN
$\Sigma$ (Gagné et al.,
2018)444http://www.exoplanetes.umontreal.ca/banyan/banyansigma.php algorithms.
As summarised in Table 32, of the 33 stars candidates in known SKGs, 17 had
been already proposed to belong to some of them.

  * •

Local Association. Seven of our 12 LA candidates were already classified as
probable LA members by Montes et al. (2001). All of them except HD 98736 had
been later assigned to SKGs linked to the LA, which supports our
classification: Hercules-Lyra (V538 Aur and V382 Ser, by Fuhrmann 2004; DX Leo
and HH Leo, by Eisenbeiss et al. 2013), AB Doradus (V577 Per, by Riedel et al.
2017), and Columba (V368 Cep, with BANYAN $\Sigma$). The eighth known LA star
candidate is HD 82939, which proper-motion companion MCC 549 has been subject
of debate: Schlieder et al. (2012) proposed it to be a member in the $\beta$
Pictoris moving group, also linked to the LA, but this statement was later
denied by Malo et al. (2014) and Shkolnik et al. (2017). There is no trail of
lithium in our HERMES spectrum of HD 82939 (G5 V), which supports the Malo et
al. (2014) conclusion.

  * •

Hyades super-cluster. We recovered two stars previously considered as members
of the Hyades SC using different methods: the multi-planet host $\rho^{01}$
Cnc A (aka Copernicus, 55 Cnc), with chemical tagging (Tabernero et al.,
2012), and HD 51067 A, with LACEwING (Riedel et al., 2017). Besides, HD 116963
could be a Carina-Near star according to BANYAN $\Sigma$.

  * •

Ursa Major moving group. Four stars were confirmed as UMa MG members by
chemical tagging in Tabernero et al. (2017): the pair WDS J05445-2227
($\gamma$ Lep and AK Lep), V869 Mon, and HD 167389. Another two stars, HD
24961 and SZ Crt, were also classified as UMa MG members by Montes et al.
(2001), King et al. (2003), and López-Santiago et al. (2010).

  * •

IC 2391 super-cluster. V447 Lac was classified as a doubtful member in
Hercules-Lyra by Eisenbeiss et al. (2013), but a more recent analysis by
Riedel et al. (2017) located it in the Argus moving group, which is
kinematically linked to the IC 2391 super-cluster.

We computed the mean iron abundance for each SKG and compared them with the
ones published in the literature (Boesgaard & Friel, 1990; Randich et al.,
2001; Paulson et al., 2003; Vauclair et al., 2008; Pompéia et al., 2011;
Tabernero et al., 2012; De Silva et al., 2013; Tabernero et al., 2017), and
found a good agreement between them. Although this is not an exhaustive
chemical tagging analysis, it supports our kinematic classification.

###  4.6 Planetary systems with late-type dwarfs

Figure 10: Normalised cumulative iron abundance histogram of the stars in our sample with (red, shaded) and without planets (blue), and of the Sousa et al. (2011) sample with (yellow) and without planets (cyan). Table 4: F, G, K- stars with confirmed exoplanets in our sample. WDS | Primary | [Fe/H] | Planet(s) | Referencea | Secondary | $s$
---|---|---|---|---|---|---
|  |  |  |  |  | [au]
01572-1015 | HD 11964 A | 0.06$\pm$0.02 | b, c | Wri09 | HD 11964 B | 974$\pm$23
03480+4032 | HD 23596 | 0.28$\pm$0.02 | b | Per03 | J03480588+4032226 | 3693$\pm$52
04359+1631 | Aldebaran | –0.27$\pm$0.05b | b | Hat15 | Aldebaran B | 573$\pm$11
05466+0100 | HD 38529 A | 0.32$\pm$0.02 | b, c | Ben10 | HD 38529 B | 11148$\pm$175
06332+0528 | HD 46375 A | 0.23$\pm$0.06 | b | WF11 | HD 46375 B | 363$\pm$12
08526+2820 |  $\rho^{01}$ Cnc A | 0.29$\pm$0.04 | b, c, d, e, f | Nel14 |  $\rho^{01}$ Cnc B | 1044$\pm$10
09152+2323 | HD 79498 | 0.21$\pm$0.02 | b | Rob12 | BD+23 2063B | 2768$\pm$80
13018+6337 | HD 113337 A | 0.17$\pm$0.03 | b | Bor14 | LSPM J1301+6337 | 4419$\pm$48
18006+2943 | HD 164595 A | –0.08$\pm$0.01 | b | Cou15 | HD 164595 B | 2509$\pm$27
18292+1142 | HD 170469 | 0.28$\pm$0.02 | b | Fis07 | J18291369+1141271 | 2617$\pm$37
20007+2243 | V452 Vul | –0.10$\pm$0.03 | b | Sou10 | J20004297+2242342 | 224$\pm$2
20036+2954 | HD 190360 A | 0.21$\pm$0.02 | b, c | Vog05 | HD 190360 B | 2854$\pm$27
21324-2058 | HD 204941 | –0.19$\pm$0.03 | b | Dum11 | LP 873-74 | 1610$\pm$12
23419-0559 | HD 222582 A | 0.00$\pm$0.02 | b | But06 | HD 222582 B | 4637$\pm$59
a Reference – Ben10: Benedict et al. (2010); Bor14: Borgniet et al. (2014);
But06: Butler et al. (2006);
Cou15: Courcol et al. (2015); Dum11: Dumusque et al. (2011); Fis07: Fischer et
al. (2007); Hat15: Hatzes et al. (2015);
Nel14: Nelson et al. (2014); Per03: Perrier et al. (2003); Rob12: Robertson et
al. (2012); Sou10: Southworth (2010);
Vog05: Vogt et al. (2005); WF11: Wang & Ford (2011); Wri09: Wright et al.
(2009).
b: Iron abundance from Hatzes et al. (2015).

As González (1997), Santos et al. (2001) and Fischer & Valenti (2005) reported
for the first time, the probability of hosting a giant exoplanet tends to
increase with the iron abundance (metallicity) of F-, G-, and K- dwarf stars.
This relationship has been investigated and confirmed in detail afterwards by
many other authors (González, 2006; Guillot et al., 2006; Pasquini et al.,
2007; Ghezzi et al., 2010; Johnson et al., 2010; Sousa et al., 2011; Buchhave
et al., 2018). However, this relationship has not been found to hold for M
dwarfs (Laughlin et al., 2004; Johnson & Apps, 2009; Hobson et al., 2018).

We searched for confirmed exoplanet discoveries around our 193 primaries using
The Extrasolar Planet Encyclopaedia555http://exoplanet.eu/. The identified
planetary systems are listed in Table 4, along with our derived iron abundance
and the projected physical separation $s$ between primary and companion. The
separations between stars in a system is much larger than between star and
planet (e.g. $\sim$7000 times in the case of V452 Vul, also known as HD
189733; Martin 2018).

We found that 14 of our FGK primaries have, at least, one confirmed exoplanet.
Of them, ten have a derived iron abundance [Fe/H] $\geq$ 0.0, and of these
ten, eight have [Fe/H] $\geq$ 0.15, including the five-planet host $\rho^{01}$
Cnc A. This new proof of the planet-metallicity relation is illustrated by
Fig. 10. As depicted, the detection probability of exoplanets in both Sousa et
al. (2011) sample and ours tends to be higher when the iron abundance
increases.

We performed a Kolmogorov-Smirnoff test to assess the difference between the
stars with and without planets in our sample. At the 2$\sigma$ level, we can
safely say that they are significantly different. We also repeated the test
for the Sousa et al. (2011) sample and found the same result at the same
confidence level. In addition, we compared our subsamples with Sousa et al.
(2011)’s and found no difference between them (with and without planets) at
the 2$\sigma$ level confidence, in spite of the iron abundance range of stars
with exoplanets in the Sousa et al. (2011) sample (–0.50 $\leq$ [Fe/H] $\leq$
+0.40) being slightly wider than ours (–0.20 $\leq$ [Fe/H] $\leq$ +0.40).

In order to prove the planet-metallicity relation in M dwarfs, we have
prepared Table 5. It tabulates the 13 most metallic ([Fe/H] $\geq$ 0.16),
late-K- and M-dwarf companions of our sample brighter than $J$ = 10.5 mag and
without companion at $\rho$ < 5 arcsec (exactly as in the CARMENES radial-
velocity survey – Caballero et al. 2016). They should be high-priority targets
of exoplanet searches, as they have the same iron abundance as their primaries
if they were born in the same molecular cloud. Six late-type dwarfs in Table 5
are already common proper-motion companions to FGK-type stars with known
exoplanets (Table 4). Interestingly, of the 13 M dwarfs, only one is being
monitored in radial velocity by CARMENES, which sample is unbiased by
metallicity or activity (Reiners et al., 2018).

Table 5: Single late-K and M dwarf companions with [Fe/H] $>$ 0.16. WDS | Late-type | SpType | [Fe/H]
---|---|---|---
| companion |  |
02556+2652 | HD 18143 B | K7 V | 0.18$\pm$0.05
| HD 18143 C | M4.0 V | 0.18$\pm$0.05
03480+4032a | J03480588+4032226 | M1.5 V | 0.28$\pm$0.02
04429+1843 | HD 285970 | K5 V | 0.24$\pm$0.02
05466+0100a | HD 38529 B | M2.5 V | 0.32$\pm$0.02
06332+0528a | HD 46375 B | M2.0 V | 0.23$\pm$0.06
07191+6644 | HD 55745 B | M0.0 V | 0.23$\pm$0.02
08526+2820a,b |  $\rho^{01}$ Cnc B | M4.5 V | 0.29$\pm$0.04
09152+2323a | BD+23 2063B | M0.0 V | 0.21$\pm$0.02
10010+3155 | 20 LMi B | M6.0 V | 0.21$\pm$0.01
11218+1811 | HD 98736 | M0.0 V | 0.30$\pm$0.06
20036+2954a | HD 190360 B | M4.5 V | 0.21$\pm$0.02
23104+4901 | HD 218790 | K5 V | 0.29$\pm$0.01
a: FGK-type primary with confirmed exoplanet. See Table 4.
b: M dwarf being monitored by CARMENES.

##  5 Conclusions

This is the first item of a series of papers devoted to improve the
metallicity calibration and to investigate the abundances of M dwarfs. For
that, we investigate wide binary and multiple benchmark systems containing
solar-like primaries and M-dwarf companions. Here we present the sample and
our first results on physical companionship, stellar parameters, abundances,
and kinematics of the primaries.

Here we characterised a sample of 489 stars distributed in 193 binary and
multiple candidate systems formed by a late-F-, G-, or early-K primaries and
at least late-K- or M-dwarf companion candidate. For each of them, we compiled
or derived coordinates, spectral types, $J$-band magnitudes, proper motions,
and heliocentric distances. After a common proper-motion analysis, we ended up
with a sample of 192 binary and multiple physical FGK+M systems. With HERMES
at the 1.2 m Mercator Telescope, we obtained high-resolution optical spectra
of 197 stars and, after excluding spectroscopic binaries, fast rotators, and
hot and cool stars, we derived stellar atmospheric parameters for 175
primaries and five companions with the the StePar code. We measured effective
temperature $T_{\rm eff}$, surface gravity $\log{g}$, microturbulence velocity
$\xi$, and photospheric chemical abundances for 13 atomic species, including
iron. For 50 stars we tabulated the first measure of [Fe/H]. We estimated ages
for the seven stars with the lowest surface gravity using isochrones for
different iron abundances. We computed Galactocentric space velocities $U$,
$V$, and $W$ for the 198 FGK stars, and compared them with the ones published
in the literature. We identified three systems in the Galactic halo, 23
systems in the thick disc, and 33 systems in young stellar kinematic groups
(of which 16 are new candidates). Finally, we studied the presence of
exoplanets around our F-, G- and K-type primaries, and provided a list of
late-type dwarf companions useful to test the planet-metallicity relation in M
dwarfs under the assumption that companions have the same metallicity as
primary stars.

Forthcoming papers of this series will focus on the calibration of spectral
indices from optical to infrared low-resolution spectra and photometry of
M-dwarf companions with the metallicity of their primaries. We will also
derive stellar atmospheric parameters and abundances of the M-dwarf companions
with spectral synthesis on high-resolution spectra, and compare the results
with the values presented here, which will be very useful for other groups
worldwide.

## Acknowledgements

This research made use of the SIMBAD database and VizieR catalogue access
tool, operated at Centre de Données astronomiques de Strasbourg, France, the
Spanish Virtual Observatory, the NASA’s Astrophysics Data System, and the
Washington Double Star Catalog maintained at the U.S. Naval Observatory.
Financial support was provided by the Universidad Complutense de Madrid, the
Comunidad Autónoma de Madrid, the Spanish Ministerio de Economía y
Competitividad (MINECO) and the Fondo Europeo de Desarrollo Regional
(FEDER/ERF) under grants AYA2016-79425-C3-1/2-P, AYA2015-68012-C2-2-P,
AYA2014-56359-P, RYC-2013-14875, and FJCI-2014-23001, the Conserjería de
Educación, Juventud y Deporte de la Comunidad de Madrid, and the Fondo Social
Europeo y la Iniciativa de Empleo Juvenil (YEI) under grant
PEJD-2016/TIC-2347, and the Spanish Ministerio de Educación, Cultura y
Deporte, programa de Formación de Profesorado Universitario under fellowship
FPU15/01476. Finally, we would like to thank the anonymous referee for helpful
comments and corrections.

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##  Appendix A Additional graphs

Figure 11: Abundance ratios of [X/Fe] versus [Fe/H], where X = Na, Mg, Al, Si,
Ca, and Sc. Red circles: our stars; black-ensquared circles: low-gravity
stars; small grey circles: stars from Adibekyan et al. (2012).

Figure 12: Same as Fig. A1, but for X = Ti, V, Cr, Mn, Co, and Ni.

##  Appendix B Long tables

Table 6: Basic properties of investigated systems and stars. WDS | Comp. | Discoverer | $\rho$ | $\theta$ | Namea | $\alpha$ | $\delta$ | $J^{b}$ | Spectral | Obs.c
---|---|---|---|---|---|---|---|---|---|---
|  | code | [arcsec] | [deg] |  | (J2000) | (J2000) | [mag] | type |
00153+5304 | A |  |  |  | G 217-41 | 00:15:14.8 | +53:04:27 | 8.84$\pm$0.02 | K3 V | H
| B | GIC 5 | 18.90$\pm$0.08 | 354.43$\pm$0.23 | G 217-40 | 00:15:14.6 | +53:04:46 | 10.82$\pm$0.02 | M2.5 V | C
00385+4300 | A |  |  |  | BD+42 126 | 00:38:29.2 | +43:00:00 | 8.41$\pm$0.02 | G5 V | H
| B | LDS 5176 | 53.09$\pm$0.08 | 124.45$\pm$0.02 | LP 193-345 | 00:38:33.2 | +42:59:30 | 10.49$\pm$0.02 | M0.5 V | C*
00452+0015 | A |  |  |  | HD 4271 Aa,Ab | 00:45:11.0 | +00:15:12 | 5.98$\pm$0.02 | F8 V | H
| BC | LDS 836 | 55.35$\pm$0.17 | 44.90$\pm$0.24 | HD 4271 B | 00:45:13.6 | +00:15:51 | 10.11$\pm$0.02 | M4.0 V+ | C
00467-0426d | Aa,Ab |  |  |  | HD 4449 | 00:46:40.5 | –04:25:37 | 6.09$\pm$0.02 | G5 V | H
| B | LDS 9100 | 66.80$\pm$0.10 | 39.41$\pm$0.12 | LP 646-9 | 00:46:43.4 | –04:24:46 | 11.12$\pm$0.03 | M4.0 V | C
00491+5749 | A |  |  |  | Achird Aa,Ab | 00:49:06.2 | +57:48:55 | 2.11$\pm$0.57 | G0 V | H
| B | STF 60 | 12.49$\pm$0.34 | 317.53$\pm$0.09 |  $\eta$ Cas B | 00:49:05.2 | +57:49:04 | 7.17 | K7 V | C
| C | STF 60 | 225.06$\pm$0.30 | 259.50$\pm$0.09 | Zkh 17 | 00:48:38.5 | +57:48:14 | 9.55$\pm$0.02 | … | …
01055+1523 | A |  |  |  | HD 6440 A | 01:05:29.9 | +15:23:24 | 7.12$\pm$0.02 | K3.5 V | H
| B | STF 87 | 6.15$\pm$0.23 | 202.66$\pm$2.81 | HD 6440 B | 01:05:29.8 | +15:23:18 | 7.15$\pm$0.02 | K7 V | C
01076+2257 | A |  |  |  | HD 6660 A | 01:07:37.9 | +22:57:19 | 6.42$\pm$0.02 | K4 V | H
| B | LDS 9112 | 9.54$\pm$0.10 | 72.54$\pm$0.75 | HD 6660 B | 01:07:38.5 | +22:57:22 | 9.53$\pm$0.04 | M3.5 V | C
01187-0052 | Aa,Ab |  |  |  | HD 7895 | 01:18:41.1 | –00:52:03 | 6.54$\pm$0.02 | K0 V+ | H
| B | HJ 5453 | 27.93$\pm$0.18 | 208.46$\pm$0.51 | HD 7895 B | 01:18:40.2 | –00:52:28 | 8.01$\pm$0.02 | K7 V | C
| C | HJ 5453 | 251.54$\pm$0.18 | 17.35$\pm$0.05 | J01184607-0048029 | 01:18:46.1 | –00:48:03 | 12.39$\pm$0.02 | … | …
01215+3120 | A |  |  |  | EN Psc | 01:21:28.2 | +31:20:29 | 6.81$\pm$0.02 | K2 V | H
| B | LDS 1096 | 10.42$\pm$0.08 | 290.88$\pm$0.27 | BD+30 206B | 01:21:27.4 | +31:20:33 | 9.98$\pm$0.02 | M3.5 V | C
01226+1245 | A |  |  |  | BD+12 168A | 01:22:36.6 | +12:45:04 | 7.86$\pm$0.03 | K3 V | H
| B | BU 1360 | 5.71$\pm$0.11 | 24.41$\pm$1.49 | BD+12 168B | 01:22:36.7 | +12:45:09 | 8.68$\pm$0.03 | K7 V | C*
01230-1258 | A |  |  |  | HD 8389 A | 01:23:02.6 | –12:57:58 | 6.40$\pm$0.02 | K0 V | H
| BC | GAL 307 | 40.79$\pm$0.08 | 313.17$\pm$0.01 | HD 8389 B | 01:23:00.6 | –12:57:30 | 8.75$\pm$0.02 | M0.0 V+ | C*
01340-0141 | A |  |  |  | BD-02 247 | 01:34:02.1 | –01:41:10 | 8.65$\pm$0.02 | G5 V | H
| B | SKF 296 | 431.96$\pm$0.11 | 20.82$\pm$0.02 | LP 588-9 | 01:34:12.4 | –01:34:26 | 11.72$\pm$0.02 | M1.0 V | C
01450-0104 | A |  |  |  | BD-01 237 | 01:44:59.1 | –01:03:31 | 8.29$\pm$0.03 | K0 V | H
| B | LDS 9123 | 41.57$\pm$0.13 | 310.54$\pm$0.02 | LP 588-44 | 01:44:57.0 | –01:03:04 | 11.03$\pm$0.02 | M2.0 | C*
01572-1015 | A |  |  |  | HD 11964 A | 01:57:09.6 | –10:14:33 | 5.02$\pm$0.03 | G8 IV | H
| B | GAL 315 | 29.65$\pm$0.36 | 133.74$\pm$0.02 | HD 11964 B | 01:57:11.0 | –10:14:53 | 8.41$\pm$0.02 | M0.0 V | C
02290-1959 | Aa,Ab |  |  |  | HD 15468 | 02:29:01.7 | –19:58:45 | 6.59$\pm$0.02 | K4 V+ | H
| B | UC 744 | 474.31$\pm$0.11 | 242.16$\pm$0.02 | HD 15468 C | 02:28:31.9 | –20:02:27 | 9.18$\pm$0.03 | M2.5 V | C
02291+2252 | A |  |  |  | BD+22 353Aa,Ab | 02:29:07.3 | +22:52:05 | 7.84$\pm$0.02 | K0 V | H
| B | HU 603 | 5.85$\pm$0.08 | 231.41$\pm$1.16 | BD+22 353B | 02:29:07.0 | +22:52:01 | 8.73$\pm$0.03 | K7 V | C
| C | HU 603 | 78.98$\pm$0.09 | 272.15$\pm$0.06 | J02290160+2252084 | 02:29:01.6 | +22:52:08 | 10.26$\pm$0.02 | … | …
| D | FOX 9043 | 46.55$\pm$0.08 | 259.94$\pm$0.12 | J02290400+2251573 | 02:29:04.0 | +22:51:57 | 12.94$\pm$0.02 | … | …
02361+0653e | AB |  |  |  | HD 16160 A | 02:36:04.9 | +06:53:13 | 4.15$\pm$0.26 | K0 V+ | H
| C | PLQ 32 | 163.95$\pm$0.33 | 109.55$\pm$0.07 | BX Cet | 02:36:15.4 | +06:52:19 | 7.33$\pm$0.02 | M4.0 V | C
02442+4914 | A |  |  |  |  $\theta$ Per A | 02:44:12.0 | +49:13:42 | 3.03$\pm$0.24 | F7 V | H
| B | STF 296 | 20.52$\pm$0.30 | 304.76$\pm$0.20 |  $\theta$ Per B | 02:44:10.3 | +49:13:54 | 6.69$\pm$0.02 | M1.5 V | C
| C | STF 296 | 94.35$\pm$0.30 | 242.67$\pm$0.24 | J02440341+4912590 | 02:44:03.4 | +49:12:59 | 10.61$\pm$0.02 | … | …
02482+2704 | A |  |  |  | BC Ari Aa,Ab | 02:48:09.1 | +27:04:07 | 6.06$\pm$0.03 | K1 V | H
| B | LDS 1138 | 20.33$\pm$0.08 | 22.48$\pm$0.31 | LP 354-414 | 02:48:09.7 | +27:04:26 | 10.73$\pm$0.02 | M5 V | C*
02556+2652 | A |  |  |  | HD 18143 A | 02:55:39.1 | +26:52:24 | 6.90$\pm$0.04 | K2 IV | H
| B | STF326 | 5.27$\pm$0.11 | 220.98$\pm$1.74 | HD 18143 B | 02:55:38.8 | +26:52:20 | 6.89$\pm$0.04 | K7 V | …
| C | LDS 883 | 43.95$\pm$0.11 | 265.70$\pm$0.16 | HD 18143 C | 02:55:35.8 | +26:52:21 | 9.56$\pm$0.02 | M4.0 V | C
03042+6142 | A |  |  |  | HD 18757 | 03:04:09.6 | +61:42:21 | 5.39$\pm$0.02 | G4 V | H
| B | KUI 11 | 55.54$\pm$0.09 | 313.65$\pm$0.01 | J03040397+6142596 | 03:04:04.0 | +61:43:00 | 10.87$\pm$0.02 | … | …
| C | LDS 9142 | 263.08$\pm$0.08 | 65.67$\pm$0.02 | vMa 2-4 | 03:04:43.4 | +61:44:10 | 8.88$\pm$0.02 | M3.0 V | C
03078+2533 | A |  |  |  | HD 19381 A | 03:07:50.5 | +25:33:07 | 7.23$\pm$0.02 | F8 V | H
| B | TOK 234 | 124.12$\pm$0.08 | 122.09$\pm$0.01 | HD 19381 B | 03:07:58.3 | +25:32:02 | 11.25$\pm$0.02 | M3.5 V | C*
03150+0101 | A |  |  |  | BD+00 549A | 03:15:04.8 | +01:02:15 | 8.91$\pm$0.02 | G5 V | H
| B | GIC 39 | 78.18$\pm$0.10 | 312.69$\pm$0.01 | BD+00 549B | 03:15:00.9 | +01:03:08 | 11.62$\pm$0.03 | M0.5 V | C*
03206+0902 | A |  |  |  | HD 20727 Aa,Ab | 03:20:37.0 | +09:02:01 | 7.11$\pm$0.02 | G0 V | H
| B | GIC 40 | 81.65$\pm$0.11 | 83.53$\pm$0.08 | HD 20727 B | 03:20:42.5 | +09:02:10 | 11.08$\pm$0.02 | M4.0 V | C*
Table 7: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 03321+4340 A HD 21727 A 03:32:05.1 +43:40:12
7.34$\pm$0.02 G5 V H B LDS 9155 14.50$\pm$0.08 136.91$\pm$0.02 HD 21727 B
03:32:05.9 +43:40:01 9.24$\pm$0.02 K7 V C 03332+4615 A V577 Per 03:33:13.5
+46:15:27 6.84$\pm$0.02 G5 V H B ES 560 9.46$\pm$0.08 142.28$\pm$0.09 HD 21845
B 03:33:14.0 +46:15:19 8.38$\pm$0.03 M0.0 V C 03356+4253 A HD 22122 03:35:35.8
+42:53:15 6.30$\pm$0.02 F8 V H B BUP 45 46.02$\pm$0.08 212.36$\pm$0.15
J03353356+4252364 03:35:33.6 +42:52:36 12.38$\pm$0.02 … … C BUP 45
180.33$\pm$0.09 90.95$\pm$0.03 HD 22157 03:35:52.2 +42:53:12 5.91$\pm$0.02 K0
… D LDS 9156 82.39$\pm$0.08 283.78$\pm$0.04 Wolf 191 03:35:28.5 +42:53:35
10.83$\pm$0.02 M0.5 V C 03396+1823 A V1082 Tau Aa,Ab 03:39:33.6 +18:23:06
6.65$\pm$0.02 G5+ H B TOK 14 9.89$\pm$0.18 245.35$\pm$1.35 J03393295+1823017
03:39:33.0 +18:23:02 11.86$\pm$0.06 … … Ca,Cb LDS 9159 254.74$\pm$0.18
175.73$\pm$0.03 Wolf 209 03:39:34.9 +18:18:52 9.33$\pm$0.02 M1.5 V C*
03398+3328 A HD 278874 Aa,Ab 03:39:49.0 +33:28:24 7.12$\pm$0.02 K2 H B ES 327
15.43$\pm$0.10 294.46$\pm$0.18 HD 278874 B 03:39:47.9 +33:28:30 8.97$\pm$0.03
M3.0 V C* 03480+4032 A HD 23596 03:48:00.4 +40:31:50 6.17$\pm$0.02 F8 V H B
TOK 240 70.79$\pm$0.08 62.81$\pm$0.09 J03480588+4032226 03:48:05.9 +40:32:23
9.35$\pm$0.02 M1.5 V C 03520+3947 A HD 275867 03:52:00.3 +39:47:44
7.55$\pm$0.02 K2 V H B GRV 197 53.82$\pm$0.08 207.48$\pm$0.12 TYC 2868-639-1
03:51:58.1 +39:46:57 8.28$\pm$0.02 M0.0 V C 03556+5214 A HD 24421 03:55:37.1
+52:13:37 5.77$\pm$0.03 F8 V H B LEP 16 52.39$\pm$0.08 358.12$\pm$0.08 LSPM
J0355+5214 03:55:36.9 +52:14:29 10.89$\pm$0.03 M2.5 V C C LEP 16
236.57$\pm$0.09 191.39$\pm$0.03 LSPM J0355+5209 03:55:32.0 +52:09:45
11.18$\pm$0.02 … … 03566+5042 A 43 Per Aa,Ab 03:56:36.5 +50:41:43
4.23$\pm$0.21 F5 V H B S 440 75.52$\pm$0.10 30.77$\pm$0.10 BD+50 860B
03:56:40.6 +50:42:48 8.15$\pm$0.02 K7 V C C S 440 88.49$\pm$0.10
132.16$\pm$0.01 J03564340+5040438f 03:56:43.4 +50:40:44 11.35$\pm$0.02 … … D S
440 65.69$\pm$0.10 289.77$\pm$0.05 J03562999+5042055 03:56:30.0 +50:42:06
12.00$\pm$0.02 … … 03575-0110 A HD 24916 A 03:57:28.7 –01:09:34 6.06$\pm$0.02
K4 V H B BU 543 11.04$\pm$0.11 16.32$\pm$0.72 HD 24916 B 03:57:28.9 –01:09:23
7.77$\pm$0.02 M2.5 V C 04153-0739 A $o^{02}$ Eri A 04:15:16.3 –07:39:10
3.01$\pm$0.24 K0.5 V H B STF 518 83.22$\pm$0.39 102.93$\pm$0.20 $o^{02}$ Eri B
04:15:22.0 –07:39:25 9.85$\pm$0.03 DA2.9 … C STF 518 78.34$\pm$0.39
97.71$\pm$0.25 $o^{02}$ Eri C 04:15:21.7 –07:39:17 6.747$\pm$0.02 M4.5 V C
04252+2545 A HD 27887 A 04:25:10.8 +25:44:57 6.93$\pm$0.02 F5 H B TOK 247
42.93$\pm$0.08 271.24$\pm$0.11 HD 27887 B 04:25:07.6 +25:44:58 11.51$\pm$0.02
M2.0 V C* 04359+1631 A Aldebaran 04:35:55.2 +16:30:33 –2.10$\pm$0.19 K5 III H
Bg BU 550 28.05$\pm$0.32 115.64$\pm$0.31 Aldebaran B 04:35:57.2 +16:30:21 …
M3.0 V C* C STB 2 133.16$\pm$0.32 31.36$\pm$0.19 BD+16 630 04:36:00.1
+16:32:27 8.36$\pm$0.06 K4 … 04397+0952 Aa,Ab HD 286955 04:39:42.6 +09:52:19
7.15$\pm$0.02 K2 V+ H B GIC 51 34.07$\pm$0.10 163.35$\pm$0.11 BD+09 621B
04:39:43.3 +09:51:47 10.26$\pm$0.02 M3.0 V C* 04429+1843 A HD 29836 04:42:51.7
+18:43:14 5.90$\pm$0.02 G2 V H B LDS 2266 141.76$\pm$0.08 102.94$\pm$0.02 HD
285970 04:43:01.4 +18:42:42 7.75$\pm$0.04 K5 V C C LDS 2266 301.65$\pm$0.08
119.43$\pm$0.01 LP 415-358 04:43:10.2 +18:40:46 12.35$\pm$0.03 … … 04559+0440
Aa,Ab HD 31412 04:55:55.9 +04:40:14 5.97$\pm$0.02 F9.5 V+ H B LDS 9181
21.61$\pm$0.08 277.59$\pm$0.19 HD 31412 B 04:55:54.5 +04:40:16 8.50$\pm$0.02
M2.0 V C 05003+2508 A HD 31867 A 05:00:17.5 +25:08:11 6.81$\pm$0.03 G2 V H B
TOK 253 33.96$\pm$0.10 126.52$\pm$0.04 HD 31867 B 05:00:19.5 +25:07:51
9.41$\pm$0.03 M1.0 V C 05067+5136h AB 9 Aur Aa,Ab 05:06:40.6 +51:35:52
3.99$\pm$0.21 F2 V+M2 H C H 6 35 90.13$\pm$0.17 61.59$\pm$0.15 9 Aur C
05:06:49.2 +51:36:35 7.34$\pm$0.03 K5 V C D BU 1046 143.57$\pm$0.17
350.79$\pm$0.06 J05063820+5138136 05:06:38.2 +51:38:14 10.58$\pm$0.02 … …
05189-2124 A HD 34751 A 05:18:47.2 –21:23:38 6.94$\pm$0.03 K6 V H B DON 101
4.91$\pm$0.08 76.38$\pm$1.21 HD 34751 B 05:18:47.5 –21:23:36 7.85$\pm$0.16
M3.5 V C 05264+0351 A HD 35638 05:26:23.1 +03:51:24 6.78$\pm$0.02 F5 V H B TOK
254 43.24$\pm$0.08 253.08$\pm$0.14 J05262029+0351111 05:26:20.3 +03:51:11
10.93$\pm$0.02 M1.5 V C* 05289+1233 A HD 35956 Aa,Ab 05:28:51.6 +12:33:03
5.61$\pm$0.02 G0 V H B TOK 94 5.56$\pm$0.08 71.04$\pm$1.12 J05285199+1233049
05:28:52.0 +12:33:05 7.59$\pm$0.08 … … C TOK 94 8.55$\pm$0.08 3.04$\pm$0.59
J05285166+1233117 05:28:51.7 +12:33:12 10.35$\pm$0.08 … … D TOK 94
16.86$\pm$0.08 245.12$\pm$0.38 J05285058+1232560 05:28:50.6 +12:32:56
9.18$\pm$0.02 … … E LDS 6186 99.39$\pm$0.10 134.17$\pm$0.01 G 102-4 05:28:56.5
+12:31:54 9.65$\pm$0.02 M4.0 V C

Table 8: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 05413+5329 A V538 Aur 05:41:20.3 +53:28:52
4.30$\pm$0.26 K1 V H B ENG 22 98.04$\pm$0.13 71.24$\pm$0.09 HD 233153
05:41:30.7 +53:29:23 6.59$\pm$0.02 M1.0 V C C BUP 82 115.14$\pm$0.13
322.68$\pm$0.01 J05411251+5330239 05:41:12.5 +53:30:24 13.25$\pm$0.02 … … D
BUP 82 697.49$\pm$0.13 282.57$\pm$0.01 HD 37229 05:40:04.0 +53:31:24
8.40$\pm$0.03 F5 … 05427+0241 A HD 38014 05:42:45.8 +02:40:45 6.97$\pm$0.02 K1
V H B LDS 6192 57.07$\pm$0.14 354.91$\pm$0.13 G 99-27 05:42:45.5 +02:41:42
9.45$\pm$0.03 M3.0 V C 05445-2227 A $\gamma$ Lep 05:44:27.8 –22:26:54
2.80$\pm$0.27 F6 V H B H 6 40 96.90$\pm$0.41 349.66$\pm$0.19 AK Lep 05:44:26.5
–22:25:19 4.85$\pm$0.19 K2 V H C H 5 50 206.60$\pm$0.30 0.42$\pm$0.08
J05442769-2223272 05:44:27.7 –22:23:27 10.35$\pm$0.03 … … "D" …i
1123.54$\pm$0.30 68.57$\pm$0.02 vB 1 05:45:43.2 –22:20:04 11.13$\pm$0.03 M3.5
V C 05466+0110 A HD 38529 A 05:46:34.9 +01:10:05 4.91$\pm$0.23 G4 IV H B RAG 1
283.82$\pm$0.14 304.77$\pm$0.01 HD 38529 B 05:46:19.4 +01:12:47 9.72$\pm$0.02
M2.5 V C 05584-0439 AB HD 40397 A 05:58:21.5 –04:39:02 5.66$\pm$0.02 G7 V H C
A 322 194.46$\pm$0.08 302.67$\pm$0.01 HD 40374 05:58:10.6 –04:37:17
8.26$\pm$0.03 G5V … D LDS 3684 89.29$\pm$0.08 313.03$\pm$0.01 LP 659-4
05:58:17.2 –04:38:01 11.11$\pm$0.02 M4.5 V C 06066+0431 A Ross 413 06:06:30.0
+04:30:41 8.94$\pm$0.02 K4 V H B VBS 12 12.22$\pm$0.08 135.11$\pm$0.01 vB 2
06:06:30.6 +04:30:33 11.16$\pm$0.02 M3.0 V C 06173+0506 Aa,Ab HD 43587
06:17:16.1 +05:06:00 4.96$\pm$0.27 F9 V H B ENG 26 179.97$\pm$0.14
240.48$\pm$0.06 HD 254595 06:17:05.7 +05:04:31 9.45$\pm$0.02 … … C BUP 87
44.13$\pm$0.14 245.60$\pm$0.25 J06171345+0505419 06:17:13.4 +05:05:42
10.38$\pm$0.03 … … D BUP 87 67.62$\pm$0.14 212.41$\pm$0.17 J06171372+0505030
06:17:13.7 +05:05:03 11.95$\pm$0.03 … … Ea,Eb LEP 24 103.10$\pm$0.14
307.16$\pm$0.02 G 106-36 06:17:10.6 +05:07:02 9.09$\pm$0.02 M3.5 V+ C
06314-0134 A HD 291763 06:31:23.1 –01:34:14 8.42$\pm$0.03 K2 V H B SKF 289
434.25$\pm$0.08 169.27$\pm$0.01 LHS 6107 06:31:28.5 –01:41:20 10.55$\pm$0.03
M1.5 V C 06319+0039 A HD 291725 06:31:51.4 +00:38:59 8.16$\pm$0.03 G7 V H B
GIC 62 436.48$\pm$0.08 251.99$\pm$0.01 NLTT 16628 06:31:23.7 +00:36:45
11.08$\pm$0.02 M1.5 V C 06332+0528 A HD 46375 A 06:33:12.6 +05:27:47
6.45$\pm$0.02 K1 V H B SLE 299 10.43$\pm$0.08 310.09$\pm$0.03 HD 46375 B
06:33:12.1 +05:27:53 8.70$\pm$0.03 M2.0 V C 06368+3751 A BD+37 1545 06:36:46.4
+37:51:07 8.07$\pm$0.02 G5 V H B LEP 25 45.23$\pm$0.08 303.92$\pm$0.03 LSPM
J0636+3751W 06:36:43.2 +37:51:32 11.44$\pm$0.03 M3.5 V C 06461+3233 A HD
263175 A 06:46:05.1 +32:33:20 7.02$\pm$0.02 K3 V H B LDS 6201 30.93$\pm$0.08
100.31$\pm$0.13 HD 263175 B 06:46:07.5 +32:33:15 8.99$\pm$0.02 M1.0 V C
06523-0510 A HD 50281 A 06:52:18.1 –05:10:25 5.01$\pm$0.25 K3.5 V H Ba,Bb WNO
17 58.84$\pm$0.17 180.22$\pm$0.16 HD 50281 B 06:52:18.1 –05:11:24
6.58$\pm$0.03 M2.0 V+ C C TNN 6 51.18$\pm$0.35 188.98$\pm$0.45
J06521752-0511158 06:52:17.5 –05:11:16 13.97$\pm$0.36 … … 07041+7514 A HD
51067 A 07:04:03.9 +75:13:39 6.14$\pm$0.02 G0 V H B STF 973 12.58$\pm$0.08
31.83$\pm$0.53 HD 51067 B 07:04:05.7 +75:13:50 7.00$\pm$0.02 G5 H C LDS 1642
61.01$\pm$0.08 17.30$\pm$0.12 LP 16-395 07:04:09.5 +75:14:37 11.18$\pm$0.02
M4.0 V C* 07058+8337 A HD 48974 07:05:49.9 +83:36:44 7.51$\pm$0.03 G5 V H B
LDS 1640 296.70$\pm$0.09 296.99$\pm$0.01 LP 4-248 07:03:11.0 +83:38:59
11.11$\pm$0.02 M3.5 C 07191+6644 A HD 55745 A 07:19:08.3 +66:44:23
6.72$\pm$0.02 F8 V H B HZG 4 8.47$\pm$0.11 35.16$\pm$1.06 HD 55745 B
07:19:09.2 +66:44:30 8.88$\pm$0.03 M0.0 V C 07321-0853 A HD 59984 07:32:05.8
–08:52:53 5.09$\pm$0.27 G0 V H B STF 1112 23.80$\pm$0.11 112.98$\pm$0.13 BD-08
1964B 07:32:07.3 –08:53:02 8.84$\pm$0.02 K5 V C 07400-0336 A V869 Mon
07:39:59.3 –03:35:51 5.49$\pm$0.03 K2 V H B BGH 3 57.96$\pm$010
112.68$\pm$0.05 HD 61606 B 07:40:02.9 –03:36:13 6.38$\pm$0.02 K7 V … "C" …j
3894.11$\pm$0.09 296.75$\pm$0.01 BD-02 2198 07:36:07.1 –03:06:39 6.79$\pm$0.03
M1.0 V C 08082+2106 A BD+21 1764A 08:08:13.2 +21:06:18 6.86$\pm$0.02 K7 V H B
COU 91 10.62$\pm$0.10 146.49$\pm$0.15 BD+21 1764Ba, Bb 08:08:13.5 +21:06:08
7.34$\pm$0.02 M3.0V C 08082+7155 A HD 66171 08:08:10.5 +71:55:28 6.98$\pm$0.02
G2 V H B LDS 1667 49.33$\pm$0.11 256.48$\pm$0.15 LP 35-148 08:08:00.3
+71:55:17 10.88$\pm$0.02 M2.0 V C* 08107-1348 A 18 Pup A 08:10:39.8 –13:47:57
4.14$\pm$0.23 F6.5 V H Ba,Bb LDS 204 97.23$\pm$0.11 239.30$\pm$2.90 18 Pup B
08:10:34.3 –13:48:51 8.28$\pm$0.02 M3.0 V+ C C WFC 287 79.14$\pm$0.11
204.33$\pm$0.11 J08103760-1349096 08:10:37.6 –13:49:10 10.65$\pm$0.02 … …
08110+7955 A BD+80 245 08:11:06.2 +79:54:30 8.71$\pm$0.03 G0 IV H B LDS 1668
110.54$\pm$0.08 208.34$\pm$0.06 LP 17-109 08:10:46.2 +79:52:52 12.54$\pm$0.03
K5 V C* C PWS 3 121.10$\pm$0.08 325.24$\pm$0.01 J08103991+7956089 08:10:39.9
+79:56:09 11.37$\pm$0.03 … … D OSO 21 15.83$\pm$0.08 289.35$\pm$0.19
J08110051+7954346 08:11:00.5 +79:54:35 14.65$\pm$0.06 … …

Table 9: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 08138+6306 A HD 67850 08:13:45.8 +63:06:14
7.17$\pm$0.02 G0 V H B LDS 2564 244.54$\pm$0.10 112.74$\pm$0.01 NLTT 19115
08:14:19.0 +63:04:40 9.91$\pm$0.02 M1.5 V C C RAO 60 249.36$\pm$0.10
109.32$\pm$0.01 J08142041+6304518 08:14:20.4 +63:04:52 14.38$\pm$0.03 … …
08161+5706 A HD 68638 08:16:06.3 +57:05:39 6.07$\pm$0.02 G8 V H B ENG 34
127.21$\pm$0.11 145.96$\pm$0.01 HD 237688 08:16:15.1 +57:03:54 8.34$\pm$0.02
F8 … C BUP 113 226.89$\pm$0.11 150.14$\pm$0.01 J08162022+5702224k 08:16:20.2
+57:02:23 10.34$\pm$0.03 … … D GIC 79 60.03$\pm$0.11 148.08$\pm$0.03 G 194-18
08:16:10.3 +57:04:48 10.56$\pm$0.02 M2.5 V C* 08484+2042 A HD 75076 08:48:24.0
+20:41:47 7.54$\pm$0.02 F8 V H B TOK 266 34.18$\pm$0.10 22.55$\pm$0.21
J08482492+2042188 08:48:24.9 +20:42:18 11.33$\pm$0.02 M1.5 V C* 08492+0329 A
HD 75302 08:49:12.5 +03:29:05 6.24$\pm$0.02 G5 V H B LEP 33 159.38$\pm$0.13
285.20$\pm$0.03 LSPM J0849+0329W 08:49:02.3 +03:29:47 10.76$\pm$0.02 M4 …
08526+2820 A $\rho^{01}$ Cnc A 08:52:35.8 +28:19:51 4.77$\pm$0.24 G8 V H B LDS
6219 84.61$\pm$0.17 127.96$\pm$0.02 $\rho^{01}$ Cnc B 08:52:40.8 +28:18:59
8.56$\pm$0.03 M4.5 V C 09008+2347 A HD 77052 09:00:49.3 +23:46:48
7.65$\pm$0.02 G2 V H B TOK 268 55.50$\pm$0.18 79.094$\pm$0.22
J09005322+2346586 09:00:53.2 +23:46:59 11.40$\pm$0.02 M2.5 C 09029+0600 A
BD+06 2091 09:02:51.3 +06:00:28 8.67$\pm$0.03 G0 V H B GWP 1132
105.48$\pm$0.11 15.86$\pm$0.08 LSPM J0902+0602 09:02:53.2 +06:02:10
11.26$\pm$0.02 M1.5 V C 09058+5532 A HD 77599 09:05:45.9 +55:31:44
6.84$\pm$0.03 G0 V H B LDS 3852 56.35$\pm$0.23 53.044$\pm$0.32 NLTT 20915
09:05:51.2 +55:32:18 11.49$\pm$0.02 M3.5 V C 09152+2323 A HD 79498 09:15:09.4
+23:22:32 6.85$\pm$0.02 G5 V H B BUP 127 60.03$\pm$0.08 170.74$\pm$0.07 BD+23
2063B 09:15:10.1 +23:21:33 9.14$\pm$0.02 M0.0 V C C STT 570 74.03$\pm$0.09
78.10$\pm$0.08 BD+23 2065 09:15:14.7 +23:22:48 8.51$\pm$0.03 G0 … 09211+6024 A
BD+61 1116 09:21:06.8 +60:24:11 7.36$\pm$0.02 K0 V H B LDS 1227
164.97$\pm$0.10 150.97$\pm$0.01 LP 91-22 09:21:17.7 +60:21:47 9.13$\pm$0.02
M1.5 V C 09245+0621 AB HD 81212 AB 09:24:28.6 +06:21:00 5.81$\pm$0.03 F5 H C
LDS 3888 122.33$\pm$0.17 325.24$\pm$0.02 LP 547-41 09:24:23.9 +06:22:42
10.60$\pm$0.03 M4.0 V C 09327+2659 A DX Leo 09:32:43.8 +26:59:19 5.58$\pm$0.02
G9 V H B LDS 3903 65.04$\pm$0.20 67.28$\pm$0.22 HD 82443 B 09:32:48.3
+26:59:44 10.36$\pm$0.02 M5.5 V C 09353-1019 A HD 83008 09:35:17.9 –10:18:51
8.04$\pm$0.03 K0 V H B LDS 6229 91.64$\pm$0.10 280.848$\pm$0.05 BD-09 2878
09:35:11.8 –10:18:34 9.08$\pm$0.04 K5 V C 09361+3733 A HD 82939 09:36:04.3
+37:33:10 6.88$\pm$0.02 G5 V H B SKF 254 162.28$\pm$0.16 121.49$\pm$0.02 MCC
549 Ba,Bb 09:36:15.9 +37:31:46 8.09$\pm$0.02 M0.0 V C 09393+1319 A HD 83509
Aa,Ab 09:39:17.2 +13:18:45 6.01$\pm$0.02 F7 V H B TOK 270 50.56$\pm$0.13
131.55$\pm$0.01 J09391981+1318118 09:39:19.8 +13:18:12 11.56$\pm$0.02 m1 …
10010+3155 A 20 LMi A 10:01:00.7 +31:55:25 4.27$\pm$0.33 G3 V H B RAG 7
134.11$\pm$0.17 278.46$\pm$0.06 20 LMi B 10:00:50.3 +31:55:46 10.26$\pm$0.02
M6.0 V C 10172+2306 A 39 Leo A 10:17:14.6 +23:06:23 4.99$\pm$0.26 F8 V H B STT
523 7.75$\pm$0.14 298.75$\pm$0.41 39 Leo B 10:17:14.1 +23:06:27 8.36$\pm$0.03
M1 … 10306+5559 A 36 UMa A 10:30:37.6 +55:58:50 4.03$\pm$0.22 F8 V H B LDS
2863 122.85$\pm$0.32 302.92$\pm$0.04 36 UMa B 10:30:25.3 +55:59:57
6.12$\pm$0.02 K7 V C C ARN 4 241.05$\pm$0.32 291.16$\pm$0.04 TYC 3819-1188-1
10:30:10.8 +56:00:17 10.50$\pm$0.02 … … 10504-1326 A BD-12 3277 10:50:22.4
–13:26:07 8.40$\pm$0.03 G3 V H B LDS 4023 8.55$\pm$0.08 21.40$\pm$0.73 LP
731-61 10:50:22.7 –13:26:00 11.65$\pm$0.05 m: … C LDS4023 150.80$\pm$0.08
92.20$\pm$0.03 LP 731-65 10:50:32.8 –13:26:13 11.09$\pm$0.02 M4 … D ARN 73
118.78$\pm$0.08 82.03$\pm$0.05 BD-12 3278 10:50:30.5 –13:25:51 7.502$\pm$0.02
… … 10507+5148 A LZ UMa 10:50:40.3 +51:47:59 6.62$\pm$0.02 G5 V H B LDS 3019
178.24$\pm$0.10 186.17$\pm$0.04 GJ 3628 10:50:38.3 +51:45:02 9.83$\pm$0.02
M3.5 V … 10585-1046 A BD-10 3166 10:58:28.8 –10:46:13 8.61$\pm$0.03 K0 V H B
LDS 4041 20.75$\pm$0.10 214.47$\pm$0.38 LP 731-76 10:58:28.0 –10:46:31
9.51$\pm$0.02 M5.0 V C 11047-0413 A HH Leo 11:04:41.5 –04:13:16 6.30$\pm$0.03
G8 V H BC STF 1506 11.55$\pm$0.11 221.35$\pm$0.79 HD 96064 BC 11:04:41.0
–04:13:25 7.27$\pm$0.02 M0.5 V+ C 11152+7329 A HD 97584 A 11:15:11.9 +73:28:31
5.78$\pm$0.02 K4 V H B STF 1516 60.40$\pm$0.14 103.49$\pm$0.10 BD+74 456a
11:15:25.8 +73:28:17 5.26$\pm$0.28 M2 … C STT 539 6.52$\pm$0.10
322.74$\pm$0.16 HD 97584 B 11:15:11.1 +73:28:36 7.88$\pm$0.02 M2.5 V C
11214-2027 A SZ Crt 11:21:26.6 –20:27:13 6.10$\pm$0.02 K7 V H B STN 22
4.06$\pm$0.10 344.44$\pm$0.94 HD 98712 B 11:21:26.6 –20:27:09 6.64$\pm$0.07
M2.5 V C

Table 10: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 11218+1811 A HD 98736 11:21:49.3 +18:11:24
6.49$\pm$0.02 K0 V H B STF 1534 5.15$\pm$0.14 316.36$\pm$0.05 BD+19 2443B
11:21:49.1 +18:11:28 7.65$\pm$0.08 M0.0 V C 11378+4150 A BD+42 2230A
11:37:50.8 +41:49:32 8.38$\pm$0.03 G6 V H B LDS 5735 28.49$\pm$0.18
340.37$\pm$0.22 BD+42 2230B 11:37:49.9 +41:50:00 11.04$\pm$0.02 M2.0 V C C DAL
24 5.68$\pm$0.21 172.32$\pm$1.86 J11375084+4149269 11:37:50.8 +41:49:27 10.57
… … 11403+0931 A BD+10 2321 11:40:16.6 +09:30:44 8.05$\pm$0.02 K0 V H B LDS
4131 62.38$\pm$0.16 88.32$\pm$0.15 LP 493-31 11:40:20.8 +09:30:45
10.12$\pm$0.02 M1.5 V C 11455+4740l A HD 102158 11:45:30.5 +47:40:01
6.86$\pm$0.03 G2 V H B LEP 45 1176.09$\pm$0.16 72.42$\pm$0.01 G 122-46
11:47:21.7 +47:45:57 10.59$\pm$0.02 m2.5 … 11475+7702 A HD 102326 11:47:30.3
+77:02:24 7.43$\pm$0.03 G8 IV H B LDS 1739 60.91$\pm$0.11 281.65$\pm$0.08 LP
20-89 11:47:12.7 +77:02:36 9.20$\pm$0.02 K7 V C 11523+0957 A HD 103112
11:52:20.9 +09:56:53 5.87$\pm$0.02 K0 IV H B LDS 4152 230.10$\pm$0.17
349.05$\pm$0.03 LP 493-64 11:52:17.9 +10:00:39 11.42$\pm$0.03 M4.0 V C
12049+1729 A HD 104923 12:04:57.0 +17:28:36 7.21$\pm$0.02 K0 V H B LEP 49
27.26$\pm$0.10 206.62$\pm$0.28 RX J1204.9+1728 12:04:56.1 +17:28:12
9.79$\pm$0.02 M3.5 V C 12051+1933 A BD+20 2678A 12:05:07.0 +19:33:16
8.31$\pm$0.02 G5 V H B GIC 103 117.20$\pm$0.17 144.07$\pm$0.02 BD+20 2678B
12:05:11.9 +19:31:41 11.19$\pm$0.02 m2: … 12069+0548 A HD 105219 12:06:56.5
+05:48:12 7.18$\pm$0.02 K0 V H B HJ 1210 6.98$\pm$0.40 115.73$\pm$1.64 BD+06
2551B 12:06:56.9 +05:48:09 8.58$\pm$0.04 K5 V C 12089+2147 Aa,Ab BD+22 2442
12:08:54.7 +21:47:19 8.14$\pm$0.02 G2 V+ H B LDS 930 15.716$\pm$0.11
39.30$\pm$0.58 BD+22 2442B 12:08:55.4 +21:47:32 11.15$\pm$0.02 M0.5 V C
12372+3545 A BD+36 2288 12:37:13.7 +35:44:46 8.47$\pm$0.02 G5 V H B LEP 58
273.10$\pm$0.11 4.49$\pm$0.03 LSPM J1237+3549 12:37:15.5 +35:49:18
11.35$\pm$0.02 M1.5 V C 12406+4017 A HD 110279 12:40:37.4 +40:17:17
7.38$\pm$0.02 F8 :V H B HJ 2617 5.69$\pm$0.16 2.21$\pm$1.58 BD+41 2317B
12:40:37.4 +40:17:23 8.28$\pm$0.06 G:V … C HJ 2617 170.20$\pm$0.16
175.3$\pm$0.05 TYC 3021-982-1 12:40:38.5 +40:14:27 9.99$\pm$0.03 F:V … D BKO
114 43.44$\pm$0.16 343.70$\pm$0.14 J12403633+4017586 12:40:36.3 +40:17:59
10.61$\pm$0.02 M: … 12482-2448 A HD 111261 A 12:48:10.7 –24:48:24
6.80$\pm$0.02 K4 V H B HJ 4551 12.04$\pm$0.10 306.12$\pm$0.10 HD 111261 B
12:48:10.0 –24:48:16 7.32$\pm$0.03 K7 V … 12489+1206 A HD 111398 12:48:52.4
+12:05:47 5.90$\pm$0.02 G5 V H B ENG 49 173.43$\pm$0.13 349.15$\pm$0.03 TYC
885-572-1 12:48:50.2 +12:08:37 9.55$\pm$0.02 … … C ENG 49 300.30$\pm$0.13
340.17$\pm$0.01 BD+12 2516 12:48:45.4 +12:10:29 10.18$\pm$0.02 A0 … D SLE 903
202.20$\pm$0.11 178.79$\pm$0.03 TYC 885-920-1 12:48:52.1 +12:02:25
10.10$\pm$0.02 … … E LEP 59 75.77$\pm$0.11 168.57$\pm$0.07 LSPM J1248+1204
12:48:53.5 +12:04:33 11.40$\pm$0.02 M4.5 V C 12549-0620 A BD-05 3596
12:54:56.0 –06:20:19 8.28$\pm$0.02 K5 V H B LDS 4294 20.14$\pm$0.23
318.56$\pm$0.06 GJ 488.2 B 12:54:55.1 –06:20:04 11.38$\pm$0.02 M4.5 V C
13018+6337 A HD 113337 A 13:01:46.9 +63:36:37 5.19$\pm$0.02 F5 V H Ba,Bb LDS
2662 119.79$\pm$0.14 307.44$\pm$0.012 LSPM J1301+6337 13:01:32.7 +63:37:50
10.31$\pm$0.02 M3.5+ … 13077-1411 A HD 114001 13:07:39.2 –14:11:17
6.89$\pm$0.03 F5 V H B TOK 286 63.26$\pm$0.08 207.58$\pm$0.10
J13073714-1412130 13:07:37.1 –14:12:13 11.60$\pm$0.02 m3: … C TOK 286
1665.72$\pm$0.09 10.57$\pm$0.01 J13080016-1343595 13:08:00.2 –13:43:59
12.66$\pm$0.03 … … D GWP 1910 59.42$\pm$0.09 252.87$\pm$0.10 J13073525-1411344
13:07:35.3 –14:11:34 15.33$\pm$0.04 … … 13114+0938 A HD 114606 A 13:11:21.4
+09:37:34 7.53$\pm$0.02 G1 V H B LDS 5771 81.83$\pm$0.22 169.16$\pm$0.52 HD
114606 B 13:11:22.4 +09:36:13 9.68$\pm$0.02 M0.0 V C 13169+1701 A HD 115404 A
13:16:51.0 +17:01:02 4.90$\pm$0.04 K2 V H B BU 800 7.39$\pm$0.11
105.97$\pm$0.62 HD 115404 B 13:16:51.5 +17:01:00 6.53$\pm$0.03 M0.5 V C C BU
800 120.55$\pm$0.11 338.62$\pm$0.03 J13164800+1702543 13:16:48.0 +17:02:54
11.36$\pm$0.02 … … D BU 800 43.99$\pm$0.11 82.97$\pm$0.17 J13165410+1701074
13:16:54.1 +17:01:07 11.74$\pm$0.02 … … 13253+4242 A BD+43 2328 13:25:17.4
+42:41:58 7.87$\pm$0.02 K1 V H B TOK 288 72.77$\pm$0.16 112.81$\pm$0.06 StKM
1-1067 13:25:23.5 +42:41:30 9.08$\pm$0.02 K7 V C 13274-2138 A HD 116963
13:27:24.9 –21:39:19 7.94$\pm$0.02 K4 V H B LDS 6278 138.46$\pm$0.08
105.97$\pm$0.05 LP 797-105 13:27:34.5 –21:39:57 9.66$\pm$0.02 M2.5 …
13315-0800 A HD 117579 A 13:31:28.7 –08:00:26 7.528$\pm$0.02 G5 V H B LDS 4371
31.51$\pm$0.10 31.00$\pm$0.24 HD 117579 B 13:31:29.8 –07:59:59 9.60$\pm$0.03
M0.0 V C 13316+5857 A HD 117845 13:31:33.8 +58:57:10 6.90$\pm$0.02 G2 V H B
JNN 151 11.39$\pm$0.11 52.76$\pm$0.81 J13313493+5857171 13:31:34.9 +58:57:17
9.63$\pm$0.03 M1 … C TOK 290 164.65$\pm$0.13 273.07$\pm$0.04 J13311250+5857191
13:31:12.5 +58:57:19 10.95$\pm$0.02 M2.5 C

Table 11: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 13321-1115 Aa,Ab HD 117676 13:32:04.7
–11:15:23 7.55$\pm$0.03 G8 V+ H B TOK 291 83.98$\pm$0.13 157.60$\pm$0.05 TYC
5548-829-1 13:32:06.9 –11:16:41 9.45$\pm$0.03 M0.0 V C 13470+0621 A HD 120066
13:46:57.1 +06:21:01 5.21$\pm$0.02 G0 V H B LDS 3101 488.44$\pm$0.15
104.82$\pm$0.22 BD+07 2692 13:47:28.8 +06:18:56 7.76$\pm$0.04 K7 V C
14050+0157 A HD 122972 14:04:58.7 +01:56:59 7.51$\pm$0.03 G6 V H B LDS 5807
49.15$\pm$0.16 299.34$\pm$0.07 Ross 799 14:04:55.8 +01:57:23 10.13$\pm$0.02 M2
… 14196-0509 A HD 125455 A 14:19:34.9 –05:09:04 6.09$\pm$0.03 K1 V H B KUI 67
15.08$\pm$0.21 105.17$\pm$0.58 HD 125455 B 14:19:35.9 –05:09:08 10.49$\pm$0.03
M4.0 V C 14245+6015 A BD+60 1536 14:24:26.9 +60:15:25 7.65$\pm$0.02 K5 V H B
LDS 2710 8.79$\pm$0.13 153.91$\pm$0.39 LP 97-826 14:24:27.4 +60:15:17
9.73$\pm$0.02 M2.0 V C 14252+5151 A $\theta$ Boo A 14:25:11.8 +51:51:03
3.18$\pm$0.24 F7 V H B STT 580 69.46$\pm$0.30 181.62$\pm$0.25 $\theta$ Boo B
14:25:11.6 +51:49:54 7.88$\pm$0.02 M2.5 V C 14255+2035 A HD 126512 14:25:30.1
+20:35:25 6.08$\pm$0.04 F9 V H B LEP 67 63.11$\pm$0.09 289.67$\pm$0.05 LSPM
J1425+203W 14:25:25.9 +20:35:46 12.46$\pm$0.03 … … 14260+3422 A BD+35 2558
14:25:59.9 +34:22:15 8.55$\pm$0.02 K0 V H B GIC 118 559.67$\pm$0.12
357.76$\pm$0.01 G 178-25 14:25:58.2 +34:31:34 10.38$\pm$0.02 K7 V … C PWS 7
31.01$\pm$0.13 286.28$\pm$0.16 J14255753+3422239m 14:25:57.6 +34:22:24
13.06$\pm$0.03 … … D PWS 7 69.30$\pm$0.13 217.94$\pm$0.15 J14255649+3421205
14:25:56.5 +34:21:21 14.71$\pm$0.03 … … 14336+0920 A HD 127871 A 14:33:34.9
+09:20:04 7.16$\pm$0.02 K2 V H B LDS 962 73.49$\pm$0.21 85.501$\pm$0.17 HD
127871 B 14:33:39.9 +09:20:10 10.23$\pm$0.02 M3.5 V C 14415+1336 A HD 129290 A
14:41:28.7 +13:36:05 7.18$\pm$0.02 G2 V H B LDS 967 93.43$\pm$0.15
13.20$\pm$0.11 HD 129290 B 14:41:30.3 +13:37:36 10.35$\pm$0.02 M1.0 V C
14446-2215 A HD 129715 14:44:35.5 –22:15:11 7.23$\pm$0.02 K2 V H B LDS 4498
68.53$\pm$0.08 68.60$\pm$0.09 LP 858-23 14:44:40.1 –22:14:46 10.57$\pm$0.02
M4.5 V C 14493+4950 AB HD 130986 A 14:49:18.1 +49:50:16 6.94$\pm$0.02 F8 V+ H
C TOK 298 48.76$\pm$0.11 220.99$\pm$0.19 J14491476+4949390 14:49:14.8
+49:49:39 10.24$\pm$0.02 M1.5 V C 14575-2125 A HD 131977 14:57:28.0 –21:24:56
3.66$\pm$0.26 K4 V H Ba,Bb H N 28 24.68$\pm$0.41 305.15$\pm$0.23 HD 131976
14:57:26.5 –21:24:42 4.55$\pm$0.26 M1.5 V+ … C H N 28 195.09$\pm$0.41
323.33$\pm$0.02 J14571953-2122161 14:57:19.5 –21:22:16 12.68$\pm$0.02 g: … D H
N 28 259.75$\pm$0.30 343.74$\pm$0.04 J14572267-2120432 14:57:22.7 –21:20:43
12.61$\pm$0.02 … … G BUG 4 258.34$\pm$0.30 314.29$\pm$0.01 GJ 570 D 14:57:15.0
-21:21:48 15.32$\pm$0.05 T8 … 14595+4528 A HD 132830 14:59:32.9 +45:27:51
7.09$\pm$0.02 K0 V H B DAM 30 63.11$\pm$0.11 202.93$\pm$0.14 MCC 56 14:59:30.6
+45:26:53 8.10$\pm$0.03 K7 V C 15123+3939 A HD 135144 15:12:17.8 +39:39:21
6.98$\pm$0.02 K3 V H B LEP 73 485.77$\pm$0.11 218.74$\pm$0.02 LP 222-50
15:11:51.5 +39:33:02 9.87$\pm$0.02 M2.5 V C 15131+1808 A BD+18 2985 15:13:06.9
+18:08:09 8.64$\pm$0.02 K0 V H B TOK 299 34.50$\pm$0.10 353.79$\pm$0.14
J15130664+1808438 15:13:06.6 +18:08:44 11.02$\pm$0.02 M2.0 V C 15164+1648 A HD
135792 A 15:16:25.6 +16:47:39 6.53$\pm$0.04 G0 V H Ba,Bb HO 547 5.32$\pm$0.10
292.50$\pm$0.56 HD 135792 B 15:16:25.3 +16:47:42 7.82$\pm$0.19 K5 V+ C
15204+0015 A HD 136378 15:20:26.1 +00:14:41 7.77$\pm$0.03 K1 V H B GIC 126
196.55$\pm$0.11 170.51$\pm$0.03 Ross 1050 15:20:28.3 +00:11:27 9.45$\pm$0.03
M0.0 V C 15211+2534 A HD 136655 15:21:09.3 +25:34:02 7.31$\pm$0.04 K2 V H B
GRV 903 69.05$\pm$0.08 243.04$\pm$0.09 MCC 739 15:21:04.8 +25:33:30
8.46$\pm$0.03 K7 V C 15282-0921 Aa,Ab HD 137763 15:28:09.6 –09:20:53
5.44$\pm$0.02 G9 V H B SHJ 202 52.25$\pm$0.11 132.64$\pm$0.01 HD 137778
15:28:12.2 –09:21:28 5.99$\pm$0.03 K2 V H "C" …n 1216.24$\pm$0.10
342.62$\pm$0.01 GJ 586 C 15:27:45.1 –09:01:32 10.55$\pm$0.03 M4.5 C 15289+5727
A HD 138367 15:28:51.9 +57:26:43 5.93$\pm$0.03 F7 V H B BU 945 35.50$\pm$0.11
97.02$\pm$0.16 J15285631+5726381 15:28:56.3 +57:26:38 11.38$\pm$0.02 … … C FOX
189 65.46$\pm$0.11 17.71$\pm$0.12 J15285442+5727448 15:28:54.4 +57:27:45
11.33$\pm$0.02 … … D GIC 128 185.26$\pm$0.11 130.64$\pm$0.01 G 224-69
15:29:09.4 +57:24:42 8.83$\pm$0.02 M1.0 V C 15353+6005 A HD 139477 15:35:20.0
+60:05:13 6.46$\pm$0.02 K3 V H B LDS 2723 42.33$\pm$0.24 97.27$\pm$0.28 LP
99-392 15:35:25.7 +60:05:08 9.27$\pm$0.02 M3.5 V C* 15431-1303 A HD 140269
15:43:08.7 –13:03:23 5.62$\pm$0.02 G1 V H B TOK 303 53.11$\pm$0.08
304.52$\pm$0.02 J15430573-1302525 15:43:05.7 –13:02:53 10.24$\pm$0.02 M1.5 V C
15482+0134 A V382 Ser 15:48:09.5 +01:34:18 5.99$\pm$0.02 G8 V H B EIS 1
17.83$\pm$0.11 352.42$\pm$0.29 HD 141272 B 15:48:09.3 +01:34:36 9.30$\pm$0.02
M2.5 V C

Table 12: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 16024+0339 Aa,Ab HD 143809 16:02:22.4
+03:39:07 7.74$\pm$0.02 G0 V+ H B CAB 4 86.40$\pm$0.11 252.57$\pm$0.09 BD+04
3100s 16:02:16.9 +03:38:41 10.35$\pm$0.03 M1.5 V C 16048+3910 A HD 144579 A
16:04:56.8 +39:09:23 5.18$\pm$0.02 G8 V H B WNO 47 70.40$\pm$0.11
280.22$\pm$0.07 HD 144579 B 16:04:50.9 +39:09:36 9.90$\pm$0.02 M4.0 V C
16147+3352 A $\sigma$ CrB Aa,Ab 16:14:40.9 +33:51:31 3.95$\pm$0.98 F6 V+ … B
STF 2032 6.25$\pm$0.19 236.40$\pm$2.29 $\sigma$ CrB B 16:14:40.4 +33:51:27
6.83 G1 V H Cg STF 2032 21.89$\pm$0.19 94.07$\pm$0.46 UCAC4 620-052945
16:14:42.2 +33:51:29 … … … D STF 2032 89.35$\pm$0.17 82.27$\pm$0.12 TYC
2583-1900-1 16:14:48.0 +33:51:43 8.96$\pm$0.03 … … Ea,Eb STF 2032
633.97$\pm$0.13 241.14$\pm$0.02 $\sigma$ CrB C 16:13:56.3 +33:46:24
8.60$\pm$0.02 M2.5 V+ C 16150+6040 A HD 146868 16:14:57.1 +60:40:11
6.38$\pm$0.02 G5 V H Ba,Ba LDS 1434 107.49$\pm$0.28 196.38$\pm$0.19 LP 100-134
16:14:53.0 +60:38:28 9.82$\pm$0.02 M3.0 V+ C 16175+7545 A $\eta$ UMi A
16:17:30.3 +75:45:19 4.37$\pm$0.26 F5 V H B LDS 1844 228.28$\pm$0.30
125.04$\pm$0.02 $\eta$ UMi B 16:18:21.0 +75:43:08 10.84$\pm$0.02 M4.0 V C
16329+0315 Aa,Ab,Ac HD 149162 16:32:51.6 +03:14:46 7.16$\pm$0.02 K1 V+ H B LEP
79 251.99$\pm$0.08 138.39$\pm$0.01 G 17-23 16:33:02.8 +03:11:37 10.63$\pm$0.02
M3.0 V C C DAM 649 258.26$\pm$0.37 138.40$\pm$0.01 LSPM J1633+0311S 16:33:03.1
+03:11:33 16.31$\pm$0.28 D: … 16348-0412 A HD 149414 Aa,Ab 16:34:42.4
–04:13:45 8.06$\pm$0.02 G8 V H B GIC 144 1176.48$\pm$0.14 36.40$\pm$0.01 GJ
629.2B 16:35:29.0 –03:57:57 11.09$\pm$0.02 sdM0 C C LMP 14 92.84$\pm$0.17
320.80$\pm$0.01 J16343843-0412321 16:34:38.4 –04:12:32 11.21$\pm$0.02 … …
17050-0504 A HD 154363 A 17:05:03.4 –05:03:59 5.52$\pm$0.02 K5 V H B LDS 585
184.57$\pm$0.08 122.83$\pm$0.01 HD 154363 B 17:05:13.8 –05:05:39 6.78$\pm$0.03
M1.5 V C C ABT 13 372.35$\pm$0.08 73.90$\pm$0.02 J17052739-0502152 17:05:27.4
–05:02:15 9.63$\pm$0.02 … … 17178+5227 A HD 156985 17:17:50.4 +52:26:50
6.13$\pm$0.02 K2 V H B LEP 81 182.69$\pm$0.08 216.31$\pm$0.04 LP 138-36
17:17:38.6 +52:24:22 9.77$\pm$0.02 M3.5 V C 17272+4213 A HD 158415 17:27:13.9
+42:13:05 7.12$\pm$0.02 G5 V H B TOK 313 135.80$\pm$0.11 297.61$\pm$0.02 TYC
3094-1728-1 17:27:03.1 +42:14:08 8.50$\pm$0.02 K5 V C 17411+7225 A HD 161897
17:41:06.7 +72:25:13 6.28$\pm$0.02 G6 V H B GIC 148 89.57$\pm$0.09
28.40$\pm$0.08 G 258-17 17:41:16.1 +72:26:32 10.28$\pm$0.02 M4.0 V C
17428+1646 A BD+16 3263 17:42:50.5 +16:45:54 7.54$\pm$0.02 K0 V H B BPMA 51
128.52$\pm$0.08 169.93$\pm$0.03 LSPM J1742+1643 17:42:52.0 +16:43:48
10.40$\pm$0.02 M1.5 V C 17465+2743 Aa,Ab $\mu^{01}$ Her A 17:46:27.5 +27:43:14
1.87$\pm$0.21 G5 IV+ H BC STF 2220 34.91$\pm$0.30 248.52$\pm$0.62 $\mu^{02}$
Her BC 17:46:25.1 +27:43:01 5.77$\pm$0.02 M3.5 V+ C D ABT 14 318.28$\pm$0.30
4.49$\pm$0.06 J17462940+2748315 17:46:29.4 +27:48:32 11.03$\pm$0.02 M5 V …
17477+2748 A BD+27 2891 17:47:39.2 +27:47:40 8.28$\pm$0.03 G0 V H B GIC 149
75.81$\pm$0.08 115.91$\pm$0.03 G 182-27 17:47:44.3 +27:47:07 11.42$\pm$0.03
M1.5 V C 18006+2934 A HD 164595 A 18:00:38.9 +29:34:19 5.86$\pm$0.02 G2 V H B
LDS 6413 88.08$\pm$0.08 104.58$\pm$0.04 HD 164595 B 18:00:45.4 +29:33:57
9.06$\pm$0.02 M2.0 V C 18006+6833 A BD+68 971 18:00:36.1 +68:33:24
8.19$\pm$0.02 K2 V H B LDS 1460 30.66$\pm$0.10 171.18$\pm$0.16
J18003695+6832539 18:00:37.0 +68:32:54 9.67$\pm$0.02 K7 V C 18090+2409 A HD
166301 18:08:58.7 +24:09:30 6.18$\pm$0.03 G0 V H B TOK 318 51.41$\pm$0.10
119.77$\pm$0.04 PM J18090+2409 18:09:01.9 +24:09:04 9.30$\pm$0.03 M1.0 V C
18131+4129 A HD 167389 18:13:07.2 +41:28:31 6.22$\pm$0.03 F8 V H B TOK 319
94.19$\pm$0.08 300.83$\pm$0.02 J18130001+4129198 18:13:00.0 +41:29:20
10.21$\pm$0.02 M3.5 V C 18161+6839 A BD+68 986 18:16:04.0 +68:38:55
8.77$\pm$0.03 G8 V H B LDS 1464 110.40$\pm$0.21 32.25$\pm$0.15 LP 71-256
18:16:14.8 +68:40:28 11.53$\pm$0.02 M1.5 V C 18292+1142 A HD 170469 18:29:11.0
+11:41:44 7.05$\pm$0.02 G5 V H B TOK 321 43.21$\pm$0.10 112.55$\pm$0.07
J18291369+1141271 18:29:13.7 +11:41:27 10.50$\pm$0.02 K5 V C* C TOK 321
166.96$\pm$0.34 257.47$\pm$0.14 J18285988+1141075 18:28:59.9 +11:41:08
16.55$\pm$0.14 … … 18333+2219 A HD 171314 A 18:33:17.8 +22:18:51 6.82$\pm$0.03
K4 V H B LEP 89 49.05$\pm$0.08 302.26$\pm$0.03 HD 171314 B 18:33:14.8
+22:19:18 11.12$\pm$0.03 M4.5 V C* 18409+3132 A BD+31 3330A 18:40:54.9
+31:31:59 6.80$\pm$0.02 K2.5 V H B HJ 1337 9.30$\pm$0.08 154.16$\pm$0.25 BD+31
3330B 18:40:55.2 +31:31:52 8.21$\pm$0.02 M1.0 V C* 19321-1116 A HD 183870 A
19:32:06.7 –11:16:30 5.91$\pm$0.02 K2 V H B TOK 333 208.49$\pm$0.08
174.33$\pm$0.02 HD 183870 B 19:32:08.1 –11:19:57 9.60$\pm$0.02 M3.5 V C*

Table 13: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 19510+1025o A $o$ Aql A 19:51:01.6 +10:24:57
4.23$\pm$0.32 F8 V H B J 124 17.65$\pm$0.31 243.55$\pm$1.35 “$o$ Aql B”
19:51:00.6 +10:24:48 10.31$\pm$0.04 M0.0 V C* C J 124 22.02$\pm$0.31
220.89$\pm$1.15 $o$ Aql C 19:51:00.7 +10:24:40 8.89$\pm$0.03 M3.5 V C* D POP
1228 52.92$\pm$0.31 121.13$\pm$0.11 J19510473+1024293 19:51:04.7 +10:24:29
8.38$\pm$0.02 … … E POP 1228 84.75$\pm$0.31 146.99$\pm$0.06 J19510479+1023456
19:51:04.8 +10:23:46 9.78$\pm$0.02 … … 19553+0624 A $\beta$ Aql A 19:55:18.8
+06:24:24 2.29$\pm$0.25 G9.5 IV H Bg STT 532 13.19$\pm$0.31 356.80$\pm$1.37
$\beta$ Aql B 19:55:18.8 +06:24:37 … M2.5 V C* C STT 532 211.22$\pm$0.30
349.24$\pm$0.06 J19551614+0627513 19:55:16.1 +06:27:51 10.20$\pm$0.02 … …
20007+2243 A V452 Vul 20:00:43.7 +22:42:39 6.07$\pm$0.03 K0 V H B BAK 1
11.29$\pm$0.08 244.30$\pm$0.60 J20004297+2242342 20:00:43.0 +22:42:34
10.12$\pm$0.04 M3.5 … 20036+2954 A HD 190360 A 20:03:37.4 +29:53:48
4.55$\pm$0.23 G7 V H B LDS 6339 178.06$\pm$0.13 232.14$\pm$0.06 HD 190360 B
20:03:26.5 +29:52:00 9.55$\pm$0.02 M4.5 V C 20111+1611 A HD 191785 20:11:06.1
+16:11:17 5.83$\pm$0.03 K0 V H B ENG 71 203.04$\pm$0.08 147.74$\pm$0.01 HD
355082 20:11:13.6 +16:08:25 7.62$\pm$0.02 K0 … C BUP 205 175.78$\pm$0.08
164.55$\pm$0.02 J20110934+1608267 20:11:09.3 +16:08:27 12.34$\pm$0.02 … … D
HZG 15 40.78$\pm$0.08 266.57$\pm$0.13 J20110326+1611137 20:11:03.3 +16:11:14
10.11$\pm$0.02 … .. E GIC 163 104.09$\pm$0.08 94.80$\pm$0.04 GJ 783.2 B
20:11:13.3 +16:11:07 9.63$\pm$0.02 M4.0 V C 20124-1237 A $\xi$ Cap 20:12:25.9
-12:37:03 4.97$\pm$0.02 F7 V H Bg BUP 206 85.86$\pm$0.13 270.36$\pm$0.08 BD-13
5608B 20:12:19.9 -12:37:02 … K5 V C* C TDT 2085 1021.22$\pm$0.10
193.62$\pm$0.01 LP 754-50 20:12:09.4 –12:53:35 8.49$\pm$0.02 M0 V … 20169+5017
A HD 193216 Aa,Ab 20:16:54.5 +50:16:43 6.80$\pm$0.02 G5 V H B ENG 73
77.75$\pm$0.08 75.69$\pm$0.08 BD+49 3245B 20:17:02.4 +50:17:03 8.96$\pm$0.03 …
… C ENG 73 92.89$\pm$0.08 158.94$\pm$0.03 BD+49 3245C 20:16:58.0 +50:15:17
7.99$\pm$0.02 … … F GIC 155 105.85$\pm$0.08 286.85$\pm$0.03 BD+49 3245G
20:16:43.9 +50:17:14 9.41$\pm$0.02 M2.5 V C* 20408+1956 A HD 197076 A
20:40:45.1 +19:56:08 5.25$\pm$0.02 G1 V H B BUP 215 69.43$\pm$0.10
24.92$\pm$0.11 J20404719+1957100 20:40:47.2 +19:57:10 10.96$\pm$0.02 … … Ca,Cb
LDS 1045 125.09$\pm$0.10 184.04$\pm$0.05 J20404449+1954023 20:40:44.5
+19:54:03 8.16$\pm$0.02 M2.5 V+ C D RAO 23 111.11$\pm$0.10 192.41$\pm$0.06
J20404342+1954186 20:40:43.4 +19:54:19 12.93$\pm$0.02 … … E RAO 23
97.71$\pm$0.10 193.48$\pm$0.07 J20404350+1954321 20:40:43.5 +19:54:32
13.86$\pm$0.02 … … 20462+3358p Aa,Ab $\epsilon$ Cyg A 20:46:12.7 +33:58:13
0.64$\pm$0.22 K0 III+ H Bg STT 594 71.33$\pm$0.31 261.27$\pm$0.28 UCAC4
620-107894 20:46:07.0 +33:58:02 … … … Cg BU 676 78.27$\pm$0.31 264.99$\pm$0.25
$\epsilon$ Cyg C 20:46:06.4 +33:58:06 … M4 V+ C* 20473+1052 A BD+10 4379
20:47:16.8 +10:51:37 7.72$\pm$0.02 K2 V H B LEP 97 14.66$\pm$0.10
351.42$\pm$0.32 LSPM J2047+1051N 20:47:16.7 +10:51:51 11.96$\pm$0.03 M4.5 V C*
20599+4016 Aa1,Aa2,Ab HD 200077 20:59:55.3 +40:15:32 5.45$\pm$0.02 F8 V+ H B
ENG 79 163.46$\pm$0.08 218.56$\pm$0.04 TYC 3171-1426-1 20:59:46.3 +40:13:24
9.12$\pm$0.02 … … C BUP 221 210.54$\pm$0.08 153.44$\pm$0.01 TYC 3172-2041-1
21:00:03.4 +40:12:23 8.36$\pm$0.02 … … Da,Db LEP 98 1212.80$\pm$0.08
258.466$\pm$0.04 G 210-44 20:58:11.5 +40:11:29 8.14$\pm$0.03 K7 V+ C R SEI
1363 206.70$\pm$0.08 151.34$\pm$0.01 TYC 3172-2041-2 21:00:03.9 +40:12:30
9.27$\pm$0.02 … … 21324-2058 A HD 204941 21:32:23.5 –20:57:27 6.90$\pm$0.02 K2
V H B LDS 6354 56.01$\pm$0.08 218.94$\pm$0.12 LP 873-74 21:32:21.0 –20:58:10
8.47$\pm$0.02 M0.5 V C* 21519+4221 A HD 207966 A 21:51:52.9 +42:20:38
6.45$\pm$0.02 G8 V H B HO 172 10.66$\pm$0.10 82.37$\pm$0.60 HD 207966 B
21:51:53.9 +42:20:39 8.51$\pm$0.04 M0.5 V C* C HO 172 85.38$\pm$0.09
42.37$\pm$0.09 J21515810+4221407 21:51:58.1 +42:21:41 12.08$\pm$0.03 … … D HO
172 480.26$\pm$0.09 62.60$\pm$0.01 HD 208056 21:52:31.4 +42:24:19
7.89$\pm$0.03 F0 … 21546-0318 A HD 208177 21:54:35.9 –03:18:05 5.39$\pm$0.02
F6 V H B STF 2838 16.42$\pm$0.08 183.39$\pm$0.32 BD-03 5329B 21:54:35.6
–03:18:21 8.98$\pm$0.03 m0: … C TOK 349 143.76$\pm$0.08 101.99$\pm$0.03
J21544530-0318343 21:54:45.3 –03:18:34 11.51$\pm$0.02 M3.5 V C* 21575+2856 A
BD+28 4248 21:57:30.8 +28:56:13 7.65$\pm$0.02 G5 V H B LEP 104 84.97$\pm$0.10
189.27$\pm$0.08 LSPM J2157+2854 21:57:29.7 +28:54:50 10.53$\pm$0.02 M1.5 V C*
22066+4323 A BD+42 4301 22:06:36.6 +43:22:33 7.24$\pm$0.02 G3 V H B BVD 273
21.33$\pm$0.08 296.21$\pm$0.10 LSPM J2206+4322W 22:06:34.8 +43:22:42
10.78$\pm$0.02 M3.5 V C* 22090-1754 A HD 210190 22:08:58.7 –17:53:40
8.17$\pm$0.02 K0 V H B LDS 6379 354.19$\pm$0.14 349.45$\pm$0.02 LP 819-37
22:08:54.2 –17:47:52 11.97$\pm$0.02 M2.5 V C 22159+5440 A V447 Lac 22:15:54.1
+54:40:22 6.04$\pm$0.02 K1 V H B BU 377 39.42$\pm$0.08 61.95$\pm$0.17 TYC
3986-2670-1 22:15:58.1 +54:40:41 10.76$\pm$0.03 B5 … C BU 377 36.68$\pm$0.09
52.75$\pm$0.19 J22155749+5440446 22:15:57.5 +54:40:44 11.05$\pm$0.03 … … D BU
377 22.53$\pm$0.08 154.70$\pm$0.10 J22155524+5440020 22:15:55.2 +54:40:02
10.85$\pm$0.03 … … T GIC 177 76.84$\pm$0.08 107.39$\pm$0.04 HD 211472 B
22:16:02.6 +54:40:00 9.72$\pm$0.02 M4.0 V C

Table 14: continued

Basic properties of investigated systems and stars.  WDS Comp. Discoverer
$\rho$ $\theta$ Namea $\alpha$ $\delta$ $J^{b}$ Spectral Obs.c code [arcsec]
[deg] (J2000) (J2000) [mag] type 22311+4509 A HD 213519 A 22:31:05.7 +45:08:42
6.47$\pm$0.02 G5 H BC LEP 108 62.24$\pm$0.08 7.62$\pm$0.08 HD 213519 B
22:31:06.5 +45:09:44 10.34$\pm$0.02 M3+ … D RAO 29 61.58$\pm$0.09
354.10$\pm$0.08 J22310515+4509435 22:31:05.2 +45:09:44 14.97$\pm$0.04 … …
22467+1210 A $\xi$ Peg A 22:46:41.6 +12:10:22 3.36$\pm$0.25 F6 V H B HJ 301
11.19$\pm$0.30 97.08$\pm$1.38 $\xi$ Peg B 22:46:42.3 +12:10:21 7.94$\pm$0.02
M1.5 C* C HJ 301 176.99$\pm$0.30 5.98$\pm$0.11 BPS CS 30332-0037 22:46:42.8
+12:13:19 11.73$\pm$0.02 … 22524+0950 A $\sigma$ Peg A 22:52:24.1 +09:50:08
4.23$\pm$0.29 F6 V H Da,Db LDS 6388 250.20$\pm$0.17 19.55$\pm$0.05 $\sigma$
Peg B 22:52:29.8 +09:54:04 9.66$\pm$0.02 M3.0 V+ C 22589+6902 A BD+68 1345A
22:58:53.8 +69:01:50 7.33$\pm$0.02 K0 V H B GIC 186 21.57$\pm$0.08
233.34$\pm$0.31 BD+68 1345B 22:58:50.6 +69:01:37 10.59$\pm$0.02 M3.0 V C
23026+2948 A BD+29 4841Aa,Ab 23:02:34.6 +29:48:18 7.24$\pm$0.02 K0 V H B TOK
352 45.34$\pm$0.10 248.51$\pm$0.16 J23023133+2948016 23:02:31.3 +29:48:02
11.12$\pm$0.02 M3.0 V C* C TOK 352 1294.97$\pm$0.09 144.190$\pm$0.001
J23033276+2930486 23:03:32.8 +29:30:49 11.92$\pm$0.02 … .. 23104+4901 A HD
218790 23:10:21.3 +49:01:06 6.17$\pm$0.02 G0 V H B STF 2987 3.81$\pm$0.09
151.11$\pm$0.56 BD+48 3952B 23:10:21.5 +49:01:03 6.61$\pm$0.09 K5 V C*
23194+7900 A V368 Cep 23:19:26.6 +79:00:13 5.90$\pm$0.02 G9 V H B LDS 2035
10.85$\pm$0.11 215.14$\pm$0.78 HD 220140 B 23:19:24.5 +79:00:04 8.04$\pm$0.02
M3.5 V C C MKR 1 962.53$\pm$0.11 141.82$\pm$0.01 LP 12-90 23:22:53.9 +78:47:39
10.42$\pm$0.02 M5.0 V C 23235+4548 A HD 220445 23:23:28.8 +45:47:36
6.85$\pm$0.02 K0 V H B STF 3010 25.94$\pm$0.08 131.28$\pm$0.02 BD+44 4400
23:23:30.7 +45:47:19 7.38$\pm$0.02 K5 V C C STF 3010 38.69$\pm$0.08
129.06$\pm$0.02 J23233168+4547116 23:23:31.7 +45:47:12 11.10$\pm$0.02 … …
23266+4520 Aa,Ab HD 220821 23:26:40.6 +45:20:17 6.10$\pm$0.02 G0 V+ H B GIC
192 54.30$\pm$0.10 332.99$\pm$0.05 J23263798+4521054 23:26:37.9 +45:21:05
5.93$\pm$0.02 MIII C C GIC 192 57.57$\pm$0.08 352.65$\pm$0.07 BD+44 4419B
23:26:39.6 +45:21:14 8.20$\pm$0.03 M4.5 … 23355+3101 A HD 221830 A 23:35:28.9