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Late-type members of young stellar kinematic groups – I. Single stars
D. Montes,P J. Lopez-Santiago, M. C. Galvez, M. J. Fernandez-Figueroa, E. De Castro and
M. CornideDepartamento de Astrofısica, Facultad de Fısicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
Accepted 2001 June 28. Received 2001 May 31; in original form 2001 February 5
A B S T R A C T
This is the first paper of a series aimed at studying the properties of late-type members of
young stellar kinematic groups. We concentrate our study on classical young moving groups
such as the Local Association (Pleiades moving group, 20–150 MyrÞ, IC 2391 supercluster
(35 Myr), Ursa Major group (Sirius supercluster, 300 Myr), and Hyades supercluster
(600 Myr), as well as on recently identified groups such as the Castor moving group
(200 Myr). In this paper we compile a preliminary list of single late-type possible members of
some of these young stellar kinematic groups. Stars are selected from previously established
members of stellar kinematic groups based on photometric and kinematic properties as well
as from candidates based on other criteria such as their level of chromospheric activity,
rotation rate and lithium abundance. Precise measurements of proper motions and parallaxes
taken from the Hipparcos Catalogue, as well as from the Tycho-2 Catalogue, and published
radial velocity measurements are used to calculate the Galactic space motions (U, V, W ) and
to apply Eggen’s kinematic criteria in order to determine the membership of the selected stars
to the different groups. Additional criteria using age-dating methods for late-type stars will be
applied in forthcoming papers of this series. A further study of the list of stars compiled here
could lead to a better understanding of the chromospheric activity and their age evolution, as
well as of the star formation history in the solar neighbourhood. In addition, these stars are
also potential search targets for direct imaging detection of substellar companions.
Key words: catalogues – stars: activity – stars: chromospheres – stars: kinematics – stars:
late-type – open clusters and associations: general.
1 I N T R O D U C T I O N
Stellar kinematic groups (SKGs) are kinematically coherent groups
of stars that could share a common origin (the evaporation of an
open cluster, the remnants of a star formation region, or a
juxtaposition of several little star formation bursts at different
epochs in adjacent cells of the velocity field). Eggen (1994) defined
a ‘supercluster’ (SC) as a group of stars gravitationally unbound
that share the same kinematics and may occupy extended regions
in the Galaxy, and a ‘moving group’ (MG) as the part of the
supercluster that enters the solar neighbourhood and can be
observed all over the sky. It has long been known that in the solar
vicinity there are several groups of stars that share the same space
motions as well-known open clusters. The youngest and best
documented groups are the Hyades supercluster (Eggen 1958a,
1960a, 1984a, 1992b, 1996, 1998b) associated with the Hyades
cluster (600 Myr), and the Ursa Major group (Sirius supercluster)
(Eggen 1960b, 1983a, 1992a, 1998c; Soderblom & Mayor
1993a,b) associated with the UMa cluster of stars (300 Myr). A
younger kinematic group called the Local Association or Pleiades
moving group seems to consist of a reasonably coherent kinematic
stream of young stars with embedded clusters and associations
such as the Pleiades, a Per, NGC 2516, IC 2602, and Scorpius-
Centaurus (Eggen 1975, 1983b,c; 1992c, 1995a). The ages of the
stars of this association range from about 20 to 150 Myr. Evidence
has been found that X-ray- and EUV-selected active stars and
lithium-rich stars (Favata et al. 1993, 1995, 1998; Jeffries & Jewell
1993; Mullis & Bopp 1994; Jeffries 1995) are members of this
association. Other two young moving groups are the IC 2391
supercluster ð35–55 MyrÞ (Eggen 1991, 1995b) and the Castor
Moving Group (200 Myr) (Barrado y Navascues 1998).
Since Olin Eggen introduced the concept of MGs and the idea
that stars can maintain a kinematic signature over long periods of
time, their existence (mainly the old MGs) has been rather
controversial (see Griffin 1998; Taylor 2000). There are two factors
that act against the persistence of an MG: the Galactic differential
rotation (tends to spread the stars) and the disc heating (velocity
dispersion of disc stars increase with age). However, recent studiesPE-mail: [email protected]
Mon. Not. R. Astron. Soc. 328, 45–63 (2001)
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(Chereul, Creze & Bienayme 1998, 1999; Dehnen 1998; Asiain
et al. 1999; Skuljan, Hearnshaw & Cottrell 1999; Feltzing &
Holmberg 2000; Myllari, Flynn & Orlov 2000; Torra, Fernandez &
Figueras 2000) using astrometric data taken from Hipparcos and
different procedures to detect MGs not only confirm the existence
of classical young MGs (and some old MGs), but also detect finer
structures in space velocity and age that in several cases can be
related to kinematic properties of nearby open clusters or
associations. Skuljan, Cottrell & Hearnshaw (1997) have also
confirmed the Eggen’s hypothesis of MGs using Hipparcos
astrometric data. These authors found that the use of Hipparcos
data considerably reduces the velocity dispersions for all the Eggen
MGs. However, Eggen’s membership criterion of constant V is not
confirmed, and they conclude that both U and V velocity
components must be used to create more realistic membership
criteria. More complex structures characterized by several longer
branches (Sirius, middle, and Pleiades branches) running almost
parallel to each other across the UV-plane have been found by
Skuljan et al. (1999) in their study of the velocity distribution of
stars in the solar neighbourhood.
Well-known members of these moving groups are mainly early-
type stars, and few studies have concentrated on late-type stars.
However, evidence has been found that many young, late-type stars
can be members of some young MG [X-ray- and EUV-selected
active stars and lithium-rich stars (Jeffries 1995); the late-type
stellar population of the Gould belt (Guillout et al. 1998; Makarov
& Urban 2000)]. Identification of a significant number of late-type
members of these young moving groups would be extremely
important for a study of their chromospheric and coronal activity
and their age evolution. This is the aim of this series of papers.
In this first paper we focus on the compilation of a preliminary
list of single late-type stars, previously established members, or
possible new candidates of the different young SKGs mentioned
above (see Table 1). We have examine the kinematic properties of
these stars using the more recent radial velocities and astrometric
data available, in order to determine their membership to the
different SKGs. In a companion paper (Montes et al. 2001c,
hereafter Paper II) we give the list of spectroscopic binaries, some
of them well-known chromospherically active binaries (for
preliminary results see Montes, Latorre & Fernandez-Figueroa
2000a and Montes et al. 2001a). The origin of these young SKGs
will be addressed in Paper III. With this aim we have taken the
most recent data available in the literature (including astrometric
data from the Hipparcos Catalogue and the new Tycho-2
Catalogue) of the nearby young open clusters, OB associations,
T associations, and other associations of young stars as TW Hya, in
order to calculate their Galactic space motions (U, V, W ) and space
coordinates (X, Y, Z ), and to study their possible association with
the different young SKGs as well as with the young flattened and
inclined Galactic structure known as the Gould Belt (for
preliminary results see Montes 2001a,b; for a review of the
evolution from OB associations and moving groups to the field
population see Brown 2001).
In addition to the kinematic properties we have also compiled
for each star the photometric, spectroscopic and physical
properties, as well as information about activity indicators and Li
abundance. For some of the candidate stars included in the list
analysed in this paper we have also taken high-resolution echelle
spectra in order to obtain a better determination of their radial
velocity, lithium abundance, rotational velocity and the level of
chromospheric activity (for preliminary results see Montes 2001b,
Montes, Lopez-Santiago & Galvez 2001b and Montes et al.
2001d). We will use all these data in forthcoming papers to analyse
in detail the membership to the different young SKGs and
identified possible age subgroups (see Barrado y Navascues 1998,
Barrado y Navascues et al. 1999, Song et al. 2000 and Lopez-
Santiago, Montes & Galvez 2001).
In Section 2 we describe the young SKGs we have considered in
this work. Details of the sample selection are given in Section 3. In
Section 4 we analyse the membership of this sample to the different
SKGs using as membership criteria the Galactic space-velocity
components (U, V, W ) and the Eggen’s kinematic criteria. Finally,
Section 5 gives the discussion and conclusions.
2 YO U N G S K G s
We focus our study here on the five youngest and best documented
SKGs: the Local Association (Pleiades moving group,
20–150 MyrÞ, IC 2391 supercluster (35 Myr), Castor moving
group (200 Myr), Ursa Major group (Sirius supercluster, 300 Myr),
and Hyades supercluster (600 Myr). The properties of these SKGs
are summarized in Table 1. We list the name, possible open clusters
associated to the group, range of age (Myr), the Galactic space-
velocity components (U, V, W ), total velocity (VT) and the
coordinates (A, D ) of the convergent point (C.P.). The velocity
vectors have been calculated by us using the spherical parameters
and VT assigned to each group in the literature (Eggen 1958b;
1984c, 1991, 1992c). For the recently identified Castor MG the
C.P. and VT have been derived by us from the space-velocity
components given by Barrado y Navascues (1998). In Fig. 1 we
Table 1. Young stellar kinematic groups.
Name Cluster(s) Age U, V, W VT C.P. (A, D )(Myr) (km s21) (km s21) (h, o)
Local Association Pleiades, a Per, M34 20–150 211.6, 221.0, 211.4 26.5 (5.98, 235.15)(Pleiades moving group) d Lyr, NGC 2516, IC2602,
IC 2391 supercluster IC 2391 35–55 220.6, 215.7, 29.1 27.4 (5.82, 212.44)
Castor moving group 200 210.7, 28.0, 29.7 16.5 (4.75, 218.44)
Ursa Major group Ursa Major 300 14.9,1.0, 210.7 18.4 (20.55, 238.10)(Sirius supercluster)
Hyades supercluster Hyades, Praesepe 600 239.7, 217.7, 22.4 43.5 (6.40, 6.50)
46 D. Montes et al.
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have plotted the position of these SKGs in the (U, V ) and (W, V )
planes. The velocity components of the substructures found in
these SKGs by Asiain et al. (1999) using statistical methods and
Chereul et al. (1999) using a 3D wavelet analysis both in the
density and velocity distributions are also plotted in Fig. 1. Orlov
et al. (1995), using a hierarchical clustering method, have found
several kinematic groups in the solar neighbourhood having
velocity components close to the five young SKGs considered here.
We have plotted the U, V, W components of these MGs in Fig. 1 for
comparison.
3 S E L E C T I O N O F T H E S A M P L E
The sample of late-type stars (spectral type later than F2) analysed
in this work has been selected from previously established
members of some of these SKGs, based on the photometric and
kinematic properties, as well as from new candidates based on
other criteria such as their level of chromospheric and coronal
activity, rotation rate, and lithium abundance, which are spectro-
scopic signatures of youth.
On the one hand, the rotation rate in late-type stars moderates the
dynamo mechanism which generates and amplifies the magnetic
fields in the convection zone, but there is a further relationship
between rotation and age. Rotation rates decline with age, because
stars lose angular momentum through the coupling of the magnetic
field and stellar mass loss, and thus there is an indirect trend of
decreasing magnetic activity with increasing age. On the other
hand, the resonance doublet of Li I at l6708 A is an important
diagnostic of age in late-type stars, since it is easy destroyed by
thermonuclear reactions in the stellar interiors. Therefore a high
level of magnetic activity, rapid rotation, and strong lithium
absorption are spectroscopic signatures of youth, and the stars
selected in this way are good candidates to be members of some of
the young SKGs we are analysing here.
The main sources from which we have selected this late-type star
sample are:
(1) the membership lists given by Eggen in his four decades of
research on SKGs (Eggen 1958a,b, 1960a,b, 1975, 1983a–c,
1984a–c, 1989, 1991, 1992a–c, 1994, 1995a,b, 1996, 1998a–c),
and additional lists given by Soderblom & Mayor (1993a);
(2) the study by Agekyan & Orlov (1984) and Orlov et al.
(1995), which searched for kinematic groups in the solar
neighbourhood (see also Popovic, Ninkovic & Pavlovic 1995);
(3) the study of ages of spotted late-type stars by Chugainov
(1991);
(4) X-ray- and EUV-selected active stars and lithium-rich stars
(Favata et al. 1993, 1995, 1998; Jeffries & Jewell 1993; Mullis &
Bopp 1994; Tagliaferri et al. 1994; Jeffries 1995; Schachter et al.
1996; Hunsch, Schmitt & Voges 1998a,b; Hunsch et al. 1999;
Cutispoto et al. 1999; 2000);
(5) single rapidly rotating stars such as AB Dor, PZ Tel, HD
197890, RE J18161541, BD1224409 (LO Peg), HK Aqr, V838
Cen, V343 Nor and LQ Hya, previously assigned membership of
the Local Association;
(6) chromospherically active late-type dwarfs in the solar
neighbourhood with studied kinematic properties (Soderblom &
Clements 1987; Young, Sadjadi & Harlan 1987; Upgren 1988;
Soderblom 1990; Ambruster et al. 1998);
(7) flare stars with studied kinematic properties (Poveda et al.
1996);
(8) the study of field M dwarfs with high-resolution spectra by
Delfosse et al. (1998), including the recently identified M9V star
DENIS 1048 2 39, which is the closest star later than M7V
(Delfosse et al. 2001);
(9) other chromospherically active stars (Henry, Fekel & Hall
1995; Henry et al. 1996; Soderblom et al. 1998);
(10) late-type stars included in the list of the nearest 100 stellar
systems given by the Research Consortium on Nearby Stars
(RECONS1);
(11) the study of nearby young solar analogues by Gaidos (1998)
and Gaidos, Henry & Henry (2000);
(12) the sample of nearby, single, solar-type stars selected as
proxies for the Sun at different stages in the project the ‘Sun in
Time’ by Bochanski et al. (2000);
(13) the study of nearby young X-ray-active low-mass stars with
well-measured parallaxes by Wichmann & Schmitt (2001), and
(14) the active stars included in the Vienna-KPNO search for
Doppler-imaging candidate stars (Strassmeier et al. 2000).
1 RECONS: http://joy.chara.gsu.edu/RECONS/
Figure 1. (U, V ) and (W, V ) planes (Boettlinger diagram) in the region of the young disc stars. Large crosses are centred at the five young SKGs analysed in this
work, as given in Table 1. Different symbols are used to plot the position of other SKGs and substructures found by other authors. The dotted line represents the
boundaries that determine the young disc population as defined by Eggen (1984b, 1989).
Late-type members of young stellar kinematic groups 47
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For this selected sample we analysed here only single stars or
effective single stars (wide visual binaries). The spectroscopic
binaries are analysed in Paper II. We have considered only isolated
stars, that is, we have excluded from the sample known members of
open clusters and OB associations. However, we have included
some members of other associations of young stars, such as TW
Hya and the recently identified b Pic moving group (Barrado et al.
1999), Tucanae association (Zuckerman & Webb 2000),
Horologium association (Torres et al. 2000), and HD 199143
stellar group (van den Ancker et al. 2000; van den Ancker, Perez &
de Winter 2001), which could be stream stars related with the Local
Association (see Lopez-Santiago et al. 2001 and Montes 2001a,b).
Some pre-main-sequence late-type stars [weak T Tauri stars
(WTTSs), and post-T Tauri stars (PTTSs) are also included in our
sample as possible members of the youngest SKG, the Local
Association. Oppenheimer et al. (1997) have identified two very
young M dwarfs which also could be members of the Local
Association. In the last few years many WTTSs, PTTSs and young
zero-age main-sequence stars have been identified (using Li as an
age criterion) with optical follow-up spectroscopy of ROSAT X-ray
sources in and around nearby star-forming regions and OB
associations. Some of these stars could be members of the Local
Association, as has been suggested by Martın & Magazzu (1999)
and Frink (2001), or may represent a population of Gould Belt low-
mass stars (Wichmann et al. 1999, 2000). We have not included
these newly identified young stars in our sample, because only a
few have enough data (astrometric data and radial velocities) to
analyse their kinematics, but they will be included in future work.
Our sample also includes some of the host stars of extrasolar
planets discovered in the past few years by measuring their
Keplerian Doppler shifts (to date more than 60; see Marcy,
Cochran & Mayor 2000 and Marcy & Butler 2000). These stars are
nearby late-type stars with high-precision radial velocity
measurements. Although many of them have ages greater than
3 Gyr, derived using evolutionary tracks (Fuhrmann, Pfeiffer &
Bernkopf 1998; Ford, Rasio & Sills 1999) or Ca II H and K fluxes
(Henry et al. 2000), others are known to be younger and could
therefore be possible members of some of the young SKGs
analysed here.
4 M E M B E R S H I P O F T H E M OV I N G G R O U P S
4.1 Galactic space-velocity components
In order to determine the membership of this sample to the
different SKGs, we have studied the distribution of stars in velocity
space by calculating the GALACTIC SPACE-VELOCITY COMPONENTS
(U, V, W ) in a right-handed coordinated system (positive in the
directions of the Galactic Centre, Galactic rotation, and the North
Galactic Pole, respectively). We have modified the procedures in
Johnson & Soderblom (1987) to calculate U, V, W, and their
associated errors. The original algorithm (which requires epoch
1950 coordinates) is adapted here to epoch J2000 coordinates in
the International Celestial Reference System (ICRS) as described
in the Introduction and Guide to the Data (section 1.5) of the ‘The
Hipparcos and Tycho Catalogues’ (ESA 1997). The uncertainties
of the velocity components have been obtained using the full
covariance matrix in order to take into account the possible
correlation between the astrometric parameters. We have used the
correlation coefficients provided by Hipparcos. It should be noted
that the differences between the errors calculated in this way and
those obtained by considering the covariances to be zero (as in
Johnson & Soderblom 1987) are very small. These differences are
generally less than 0.1 km s21; only for a small number of stars
(eight) are the differences between 0.2 and 0.5 km s21, and in only
one case the difference is 1.2 km s21. The largest differences are
for stars with the largest errors in the input data.
PARALLAXES and PROPER MOTIONS have been taken mainly from
‘The Hipparcos and Tycho Catalogues’ (ESA 1997) and ‘The
Tycho-2 Catalogue’ (Høg et al. 2000), which supersedes the PPM
(Positions and Proper Motions) Catalogue (Roser & Bastian 1991;
Bastian et al. 1993; Roser, Bastian & Kuzmin 1994); ACT
Reference Catalog (Urban, Corbin & Wycoff 1997), and TRC
(Tycho Reference Catalogue) (Høg et al. 1998).
RADIAL VELOCITIES are taken primarily from the compilation
WEB (Wilson Evans Batten) Catalogue (Duflot, Figon &
Meyssonnier 1995), the mean radial velocities catalogue of
galactic stars (Barbier-Brossat & Figon 2000) which supplements
the WEB Catalogue, the Catalogue of Radial Velocities of Nearby
Stars (Tokovinin 1992), the Vienna-KPNO search for Doppler-
imaging candidate stars, and from other references given in
SIMBAD, and in the CNS3, Catalogue of Nearby Stars,
Preliminary 3rd Version (Gliese & Jahreiß 1991) or the CNS3R
(CNS3 Revised Version).2 For the stars for which we have taken
high-resolution echelle spectra (see Montes et al. 2001b,d) we have
used the radial velocities (marked with ‘*’ in Tables 2 to 7)
obtained by us by cross-correlation with radial velocity standard
stars of similar spectral types.
Our initial sample of more than 1000 stars was reduced to 638
stars with accurate parallaxes, proper motions and radial velocities
available in the literature to calculate the Galactic space-velocity
components (U, V, W ). As we are interested only in young MGs,
we restrict this sample to the stars for which the U, V and W
components follow the criterion from Leggett (1992) for young
disc stars ð250 , U , 20; 230 , V , 0; 225 , W , 10Þ, or
more exactly to the stars with U and V velocity components inside
or near the boundaries (dotted lines in Figs 1 and 2) that determine
the young disc population as defined by Eggen (1984b, 1989,
1998a). We have found 535 stars that satisfied this restriction.
In Tables 2 to 7 we list the stellar and astrometric data we have
compiled for the stars in each SKG. We give the name (HD, Henry
Draper number; variable star name or other name; HIP, Hipparcos
identifier; GJ, Gliese Catalogue number), spectral type, coordinates
(ICRS J2000.0), radial velocity (Vr) and the error in km s21,
parallax (p) and the error in milliarcseconds (mas), proper motions
ma cos d and md and their errors in mas per year (mas yr21). The
calculated U, V, and W velocity components with their associated
errors in km s21 are also given in these tables.
In Fig. 2 we represent the (U, V ) and (W, V ) planes for this
restricted star sample. The distribution of the stars in this figure
shows concentrations around the central (U, V, W ) position
corresponding to the five MGs listed in Table 1. To begin the
classification, following Eggen’s membership criterion of constant
V, we have considered as members only stars with small V
dispersions. However, taking into account the results found by
other authors (Skuljan et al. 1997, 1999), we have considered a
large dispersion in the U, V components (<8 km s21) with respect
to the central position of the MG in the (U, V ) plane to classify a
star as a possible member. In addition, we have taken into account
the information provided by the W component, in the sense
that stars considered as possible members for their position in
2 CNS3R available only at ARI (Astronomisches Rechen-Institut Heidel-
berg) Database for Nearby Stars at http://www.ari.uni-heidelberg.de/aricns/
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the (U, V ) plane are excluded if their W component deviates
considerably (<8 km s21) with respect to the W component of the
MG. Following these we have classified the stars from our sample
as members of one of the MGs or as other young disc stars if their
classification is not clear but is inside or near the boundaries that
determine the young disc population (see Tables 2 to 7). In Fig. 2
we plot with different symbols the stars belonging to the different
SKGs, and the other young disc stars. Filled symbols represent
stars that, in addition, satisfied Eggen’s criteria described in the
next two subsections.
4.2 Convergent point
The members of a moving group can be established by the degree
to which their motions define a common convergent point in the
sky. However, this is not a sufficient membership criterion (there
might be some stars moving in the same direction, but with a
significantly different speed). Eggen’s criteria of membership
(described in the next subsection) also take into account the
magnitude of the velocity vector.
We can apply the convergent point criterion to a moving group
by plotting the great circles defined by the proper motions and
positions of individual stars and test whether their poles are close to
the convergent point given in the literature for that moving group.
We have applied this analysis to our sample of candidate members
to the five MGs studied in this paper (see Fig. 3 for the case of the
Hyades). We have obtained, in general, a good agreement between
the position of the poles and the convergent point. However, there
are some stars with clear discrepancies, which are probably not
members. These deviations with respect to the convergent point
will be analysed in a more quantitative way by applying Eggen’s
criteria, as described in next subsection.
In this convergent point analysis (following other authors) we
have not corrected for the Sun’s motion. It is possible that the Sun’s
motion induces this effect, so we need to prove that the MGs really
converge towards a point independently of this effect. In fact,
nearly all the convergent points of the MGs are situated close to the
apex or antiapex. If we make this correction with each moving
group, we obtain that in the cases of the Hyades, Ursa Major, IC
2391 and Castor MGs the trend of the candidate star members to
have a common convergent point is maintained. However, in the
case of the Local Association the dispersion increases somewhat. It
seems that the proper motion great circles tend to converge towards
several points that are close together. This could indicate that the
Local Association has several substructures, or that is a
concentration of different MGs with similar space motions.
4.3 Eggen’s criteria
Eggen has developed several criteria during many years studying
stars in MGs (see Eggen 1958a, 1995b). These criteria are based on
one supposition: it is possible to treat MGs, whose stars are
extended in space, like moving clusters, whose stars are
concentrated in space. As in the moving cluster method, it is
assumed that the total space velocities of stars in a moving group
are parallel and move towards a common convergent point.
Eggen’s criteria try to quantify how the space motion of the stars
deviates from the convergent point, and use the following
parameters and relations:
(1) The components of the absolute proper motion (m ) in the
direction of the convergent point (y ) and perpendicular to it (t ).
(2) The angular distance between the star and the convergent
point (l ).
(3) The trigonometric parallax (p)
(4) The relations between the tangential (Vtan), radial (Vr) and
total (VTotal) velocities in the moving cluster method:
V tan ¼ 4:74mp21;
V tan ¼ VTotal sin l; V r ¼ VTotal cos l;
VTotal ¼ 4:74mp21 sin21l
The total velocity can also be calculated from the U, V, W
components as
VTotal ¼ ðU2 1 V 2 1 W 2Þ1=2:
The two main Eggen criteria are as follows.
(1) PECULIAR VELOCITY CRITERION
In the first papers Eggen used the ratio ðt/yÞ as a measure of how
the star turns away from the convergent point, but later he defined a
Figure 2. (U, V ) and (W, V ) planes as in Fig. 1 for our star sample. We plot with different symbols the stars belonging to the different stellar kinematic groups,
and the other young disc stars. Filled symbols are stars that satisfied both of Eggen’s criteria (peculiar velocity, PV, and radial velocity, rc), and open symbols
are other possible members.
Late-type members of young stellar kinematic groups 49
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Ta
ble
2.
Lo
cal
Ass
oci
atio
n.
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)
HD
67
SA
O248115
HIP
459
G5
V0
528.4
52
61
13
33.0
67.0
2.0
18.5
70.9
583.9
01.3
02
77.8
01.3
02
10.0
21.0
72
28.2
91.6
21.2
91.7
030.0
430.7
92
12.5
N15.9
N
HD
105
1E
0003.3
-4201
HIP
490
G0
V0
552.5
52
41
45
11.0
43.2
2.0
24.8
50.9
298.5
01.0
02
75.8
01.1
02
9.5
70.7
02
21.7
40.9
22
2.8
81.9
123.9
325.4
42
4.4
Y10.2
N
HD
166
HR
8H
IP544
GJ
5K
0V
06
36.7
829
117.4
12
6.9
0.2
72.9
80.7
5380.5
00.9
02
177.9
00.9
02
15.0
00.2
02
21.6
00.2
42
10.0
40.1
928.1
527.9
93.4
Y2
7.1
Y
HD
1405
PW
And
K2
V0
18
20.9
030
57
22.0
32
11.0
0.1
32.6
81.0
0143.7
01.2
02
171.5
01.1
02
5.4
20.3
32
28.6
90.6
32
17.9
40.7
434.2
731.9
42
9.5
N2
7.6
Y
HD
1466
SA
O248159
HIP
1481
F8
V0
18
26.1
22
63
28
38.9
77.0
2.0
24.4
20.6
889.8
01.3
02
58.0
01.3
02
8.7
70.8
62
20.0
31.0
82
1.2
51.6
221.9
023.3
62
6.9
N12.8
Y
BP
M1699
HIP
1910
M0
V0
24
8.9
82
62
11
4.4
14.0
2.0
21.5
92.2
284.1
06.9
02
55.3
06.4
02
10.1
82.1
82
19.9
52.6
01.6
91.9
122.4
624.8
52
7.6
N13.7
N
CT
Tuc
HIP
1993
K7
V0
25
14.6
62
61
30
48.3
37.0
2.0
26.6
924.0
084.5
919.3
02
63.4
023.9
02
6.3
98.9
12
18.9
714.8
92
0.9
85.2
420.0
420.6
22
7.5
N11.4
Y
HD
3221
HIP
2729
K4
V0
34
51.2
02
61
54
58.1
02
1.0
2.0
21.7
81.0
188.0
01.8
02
50.5
01.7
02
12.4
00.9
92
17.3
41.3
25.8
41.6
722.1
025.4
12
7.1
N2
14.4
N
HD
5996
BD
+68
67
HIP
4907
G5
V1
257.2
269
13
37.4
12
20.0
0.5
38.7
30.7
8225.3
01.1
02
149.1
01.2
02
13.4
80.5
92
30.7
70.5
12
19.1
10.3
838.6
537.0
22
3.2
Y2
17.0
Y
HD
9540
HIP
7235
GJ
59A
K0
V1
33
15.8
12
24
10
40.6
73.0
1.0
51.2
70.8
8272.7
01.4
02
159.4
01.4
02
11.2
70.3
02
27.1
10.5
10.2
70.9
929.3
634.5
22
1.4
Y18.5
N
BD
+17
232
K3
Ve
137
39.4
218
35
32.9
13.2
1.0
15.8
05.0
069.9
01.5
02
47.5
01.5
02
13.2
83.7
12
20.0
96.8
82
8.5
62.1
625.5
625.4
13.2
Y3.6
Y
HD
10008
BD
207
268
HIP
7576
G5
V1
37
35.4
72
645
37.5
211.6
0.6
42.3
50.9
6171.9
01.4
02
97.7
01.4
02
13.1
60.3
52
18.1
30.5
22
11.0
70.5
624.9
924.1
02.3
Y9.8
Y
HD
10360
GJ
66B
K5
V1
39
47.7
02
56
11
34.0
020.9
0.9
148.0
07.0
0302.6
01.4
02
14.1
01.3
02
3.6
30.3
72
16.1
60.5
22
16.0
20.7
823.0
413.1
12
0.1
Y8.8
N
HD
10361
HIP
7751
GJ
66A
K5
V1
39
47.5
62
56
11
47.3
419.5
1.0
122.7
51.4
1286.1
01.0
116.6
61.4
12
5.5
90.2
12
15.6
30.4
82
15.0
70.8
622.4
214.8
81.1
Y10.0
N
V596
Cas
HIP
9291
GJ
82
dM
4e
-1
59
23.5
158
31
16.0
22
9.8
0.5
83.2
03.6
8322.5
03.2
02
193.7
03.2
02
8.6
60.7
92
21.2
70.7
62
5.3
20.3
423.5
721.8
44.3
Y2
6.0
Y
HD
12230
47
Cas
HIP
9727
F0
V2
57.3
877
16
52.7
32
26.0
5.0
29.8
00.5
6122.7
02.0
02
60.2
02.1
02
2.5
32.9
62
32.2
63.8
72
10.0
91.3
633.9
024.0
64.5
Y2
11.2
N
HD
15013
BD
+33
429
HIP
11352
G5
V2
26
9.5
934
28
10.0
42
2.5
0.5
23.1
91.2
1115.4
00.9
02
49.9
01.0
02
13.1
20.8
82
22.2
21.1
90.9
30.2
825.8
223.2
511.1
N2
1.8
Y
HD
16765
84
Cet
HIP
12530
F7
IV2
41
14.0
00
41
44.3
67.8
1.0
46.2
41.3
1222.4
00.9
02
127.1
00.9
02
12.6
60.6
62
24.1
40.7
62
2.6
70.8
127.3
930.4
15.8
Y16.4
N
HD
17925
EP
Eri
HIP
13402
GJ
117
K1
V2
52
32.1
32
12
46
10.9
717.5
0.1
96.3
30.7
7397.3
01.2
02
189.9
01.3
02
15.0
10.1
02
21.8
00.1
82
8.6
80.1
127.8
528.8
64.1
Y19.5
Y
HD
19668
BD
210
626
HIP
14684
G0
V3
942.2
92
934
46.5
914.6
0.7
24.9
01.2
888.0
01.2
02
113.3
01.1
02
5.1
10.5
12
28.7
71.4
82
10.2
70.5
830.9
737.0
52
5.6
Y25.6
N
1E
0318.5
-19.4
K7
V3
20
49.5
02
19
16
10.0
020.8
1.0
37.0
05.0
090.8
01.8
02
43.8
04.9
02
12.6
90.7
42
17.2
71.6
62
11.8
51.0
924.4
920.7
21.6
Y16.3
Y
HD
21845
V577
Per
HIP
16563
K2
-3
33
13.4
946
15
26.5
42
2.0
1.0
29.6
11.4
067.0
01.1
02
176.0
01.1
02
8.9
11.0
12
23.9
01.2
22
16.2
00.8
330.2
229.8
62
4.3
Y2
1.2
Y
HD
25457
BD
200
632
HIP
18859
GJ
159
F6
V4
236.7
40
16
8.1
318.1
0.9
52.0
00.7
5150.7
00.9
02
252.0
00.9
02
8.2
50.7
22
28.7
60.4
42
12.2
10.5
532.3
238.3
42
1.8
Y27.5
N
HD
25665
BD
+69
238
HIP
19422
GJ
161
G5
-4
935.0
469
32
29.0
12
13.7
0.2
54.1
70.7
973.6
01.0
02
298.8
01.1
02
7.4
20.3
12
23.8
20.2
72
17.0
40.2
430.2
127.7
32
4.3
Y2
7.9
Y
HD
29883
BD
+27
688
HIP
21988
GJ
176.2
K5
V4
43
35.4
427
41
14.6
517.4
0.6
44.7
40.9
954.6
00.8
02
264.9
00.8
02
17.2
30.5
82
23.4
30.5
92
16.6
80.3
433.5
331.4
12
2.6
Y13.1
Y
HD
36705A
AB
Dor
HIP
25647
K0
V5
28
44.8
52
65
26
54.9
728.0
1.0
66.9
20.5
448.9
01.3
0137.6
01.2
02
7.7
50.1
52
25.5
60.8
42
13.3
20.5
529.8
520.1
32
1.3
Y17.3
N
HD
36869
BD
215
1082
G3
V5
34
9.1
62
15
17
3.1
824.1
2.0
28.6
07.1
025.6
01.3
02
22.3
01.2
02
14.8
61.5
62
18.3
11.6
22
7.5
21.0
024.7
513.1
73.2
N12.3
N
HD
37572
UY
Pic
HIP
26373
K0
V5
36
56.8
52
47
57
52.8
732.4
1.7
41.9
01.7
424.6
01.1
01.2
01.1
02
7.5
50.4
02
27.9
71.3
92
14.7
80.9
132.5
24.5
62
2.6
N4.4
N
HD
37394
HIP
26779
GJ
211
K1
V5
41
20.3
453
28
51.8
10.3
0.2
81.6
90.8
33.5
01.1
02
523.6
01.1
02
12.8
90.2
32
23.3
50.2
72
14.5
50.1
830.3
830.3
42
1.7
Y0.7
Y
HD
233153
HIP
26801
GJ
212
M0.5
-5
41
30.7
353
29
23.2
81.9
1.0
80.1
31.6
73.1
61.6
12
517.2
61.0
42
14.4
40.9
52
22.9
40.6
32
14.3
20.3
930.6
630.5
62
1.7
Y0.7
Y
HD
43989
V1358
Ori
HIP
30030
F9
V6
19
8.0
62
326
20.3
819.1
2.4
20.1
00.9
910.6
00.9
02
43.7
01.0
02
10.1
22.0
32
18.6
21.3
72
5.3
20.4
621.8
518.5
92
3.9
N15.8
Y
HD
45081
AO
Men
HIP
29964
K5
-6
18
28.2
12
72
241.4
316.2
1.0
25.9
91.0
22
8.5
01.5
075.7
01.4
52
10.5
00.6
62
16.3
80.8
82
8.7
60.5
321.3
423.0
90.1
Y18.4
Y
V577
Mon
HIP
30920
GJ
234A
M4
-6
29
23.4
02
248
50.3
215.0
0.5
242.8
82.6
4694.6
63.0
02
618.5
52.4
82
3.9
20.4
32
22.6
90.3
24.9
50.1
223.5
516.7
12
15.7
N14.0
Y
HD
261557
BD
+03
1342
HIP
31849
K3
V6
39
31.3
63
19
10.6
511.3
0.3
16.6
01.7
52
30.7
01.3
02
64.4
01.3
02
3.7
30.7
32
16.0
81.2
02
16.4
41.7
823.3
031.1
94.4
Y24.0
N
HD
48189
HIP
31711
GJ
3400A
G1.5
V6
38
0.3
92
61
32
0.2
032.3
1.0
46.1
50.6
42
26.0
03.8
072.4
03.4
02
7.2
00.4
02
28.8
70.9
22
14.8
50.5
633.2
517.3
32
0.3
Y15.4
N
BD
+20
1790
K5
Ve
723
44.0
020
25
6.0
09.3
1.0
31.6
05.0
02
55.0
05.0
02
238.0
05.0
02
5.2
31.0
92
32.6
14.7
92
18.4
03.4
137.8
142.3
62
4.6
Y21.7
N
BD
+02
1729
HIP
37288
GJ
281
K7
-7
39
23.0
42
11
1.1
818.5
5.0
67.2
71.5
12
147.6
01.6
02
247.3
01.5
02
10.9
93.9
42
21.4
72.9
22
13.1
31.0
927.4
629.1
40.3
Y20.9
Y
YZ
CM
iH
IP37766
GJ
285
M4.5
-7
44
40.1
73
33
8.9
626.0
0.5
168.5
92.6
72
348.5
01.8
02
446.9
01.9
02
19.2
70.4
02
22.2
40.3
12
8.0
00.2
730.5
021.9
72.1
Y15.3
N
HD
64725
BD
+37
1804
HIP
38825
K0
III
756
44.7
636
53
47.1
417.2
0.2
4.6
61.0
62
7.7
01.1
02
27.3
01.1
02
20.3
51.4
12
26.3
56.1
82
4.5
03.2
533.6
029.2
72
4.3
Y6.5
N
FP
Cnc
HIP
39896
GJ
1108A
K7
-8
856.3
932
49
11.4
111.3
1.0
48.2
63.1
62
30.0
03.7
72
217.2
02.5
02
10.7
40.8
82
21.7
61.3
82
1.6
40.7
924.3
221.0
92
7.1
N5.6
Y
BD
+07
1919
HIP
39721
GJ
9251A
K8
-8
79.0
97
23
0.1
320.3
5.0
24.8
53.9
22
1.3
03.3
02
138.0
03.1
02
5.5
34.1
92
32.5
24.3
82
4.1
32.5
533.2
428.0
02
14.3
N17.2
Y
BD
+07
1919B
GJ
9251B
K5
-8
78.7
87
22
58.3
920.3
5.0
35.4
06.0
02
3.0
03.3
02
131.2
03.2
02
9.0
14.0
22
25.2
93.6
42
0.6
32.1
926.8
518.8
52
9.3
N11.6
N
HD
70146
BD
+22
1914
HIP
40920
G5
III
821
4.9
122
154.1
54.5
0.2
3.9
21.0
82
10.6
00.9
02
17.4
00.9
02
6.6
41.2
62
19.2
55.3
12
14.5
85.0
925.0
426.8
90.0
Y10.8
N
HD
70573
BD
+02
1951
G6
V8
22
49.9
51
51
33.5
519.5
1.0
21.9
05.0
02
50.5
01.3
02
49.0
01.3
02
14.6
70.7
72
18.7
81.6
42
6.6
63.1
524.7
419.7
21.9
Y12.7
N
HD
77407
BD
+38
1993
HIP
44458
G0
-9
327.0
937
50
27.5
24.4
0.2
33.2
40.9
12
80.2
01.2
02
168.0
01.3
02
10.1
00.3
02
23.9
10.7
02
7.1
20.3
826.9
126.1
92
5.0
Y2.5
Y
HD
82443
DX
Leo
HIP
46843
GJ
354.1
K0
V9
32
43.7
626
59
18.7
18.1
0.1
56.3
50.8
92
147.8
01.4
02
246.7
01.3
02
9.9
10.1
52
22.8
30.3
62
5.6
10.2
325.5
124.1
12
4.6
Y4.2
Y
HD
82939
BD
+38
2052
HIP
47110
G5
V9
36
4.2
837
33
10.3
62
1.0
0.3
26.2
91.1
42
99.1
01.1
02
90.8
01.1
02
10.9
40.6
12
17.4
70.8
02
12.7
90.6
224.2
624.1
22.5
Y2
0.7
Y
BD
221
2961
K-
959
8.4
22
22
39
34.6
127.7
1.0
27.5
05.0
02
65.0
04.3
02
22.0
03.7
02
11.3
61.3
82
27.7
91.1
02.4
01.8
630.1
214.5
71.9
Y8.7
N
DK
Leo
HIP
50156
GJ
2079
K7
-10
14
19.1
821
429.4
510.0
1.0
48.9
51.7
12
137.7
01.4
02
167.1
01.4
02
10.3
30.5
52
20.6
80.7
32
2.3
20.8
923.2
320.9
22
3.0
Y2.7
N
HD
89744
BD
+41
2076
HIP
50786
GJ
9326
F7
V10
22
10.5
641
13
46.3
12
6.5
1.3
25.6
50.7
02
119.5
00.9
02
138.6
01.0
02
10.4
10.8
42
29.6
20.8
52
14.1
61.1
234.4
433.7
62
4.7
Y2
4.3
Y
BD
+01
2447
HIP
51317
GJ
393
M2
-10
28
55.5
50
50
27.5
88.3
0.5
138.2
92.1
32
602.3
01.9
12
731.8
52.1
02
7.4
80.1
92
28.6
10.5
02
15.8
20.5
133.5
433.2
22
7.3
N10.1
Y
HD
92945
SA
O179168
HIP
52462
GJ
3615
K1
V10
43
28.2
72
29
351.4
323.2
0.6
46.3
60.8
42
212.5
01.5
02
50.0
01.2
02
14.8
80.3
52
28.2
70.5
62
3.9
90.4
032.2
025.3
34.9
Y12.9
N
EE
Leo
HIP
53020
GJ
402
M4
-10
50
52.0
66
48
29.3
42
2.0
0.1
177.4
623.0
02
804.3
936.5
02
809.5
916.5
02
7.8
91.5
72
22.5
43.1
82
19.0
62.4
230.5
530.6
52
4.1
Y2
5.2
Y
HD
96064
BD
203
3040A
HIP
54155
G8
V11
441.4
72
413
15.9
118.3
0.8
40.5
71.4
02
178.6
01.2
02
102.9
01.2
02
14.2
20.4
62
26.6
90.7
42
0.6
10.8
030.2
524.6
62.2
Y5.7
N
HD
97334B
HR
4345
HIP
54745
GJ
417
G0
V11
12
32.3
535
48
50.6
92
3.6
1.0
46.0
40.9
02
248.6
01.4
02
151.9
01.4
02
15.8
00.5
42
23.1
70.5
02
11.2
30.9
430.2
130.5
81.9
Y2
6.2
Y
HD
98736
BD
+19
2443
HIP
55486
GJ
426A
G5
-11
21
49.3
418
11
24.0
12
4.1
2.0
31.6
81.5
52
148.2
01.0
02
93.6
01.1
02
12.2
90.8
42
19.0
71.2
12
13.7
81.9
226.5
426.2
11.7
Y2
1.4
Y
HD
99303
BD
+20
2601
HIP
55772
G5
V11
25
39.9
520
07.6
64.5
0.4
32.7
91.1
92
202.1
00.8
02
91.0
00.8
02
20.9
00.7
62
23.6
30.8
52
7.2
10.5
732.3
631.5
26.4
N2.7
Y
HD
102195
BD
+03
2549
HIP
57370
K0
V11
45
42.2
92
49
17.3
42.1
0.6
34.5
11.1
62
190.0
01.0
02
112.6
01.1
02
15.4
20.5
82
23.7
40.8
72
11.1
30.7
030.4
230.2
42.4
Y0.6
Y
HD
102392
BD
211
3178A
BH
IP57494
GJ
444A
BK
2+
?-
11
47
3.8
42
11
49
26.6
319.7
2.0
40.5
72.6
62
191.0
01.5
02
64.8
01.4
02
13.8
91.1
02
27.0
31.6
24.4
41.6
430.7
123.0
06.3
N3.7
N
BD
+08
2599
HIP
60661
GJ
466
M0
V12
25
58.5
88
344.0
32
5.0
2.0
25.0
81.8
52
129.7
02.4
02
110.8
02.3
02
11.0
61.0
22
27.3
32.3
52
13.9
72.0
132.6
332.5
72
3.4
Y2
5.7
Y
HD
108767B
del
Crv
BK
0V
12
29
50.9
12
16
31
14.9
97.0
5.0
37.1
10.6
92
209.9
70.6
22
139.3
00.4
62
13.5
41.5
22
28.4
93.1
72
9.4
73.6
132.9
332.2
11.2
Y1.9
Y
HD
109157
SA
O82366
HIP
61198
G7
V12
32
27.4
328
54.6
27.1
0.4
22.8
01.2
12
82.0
01.3
02
121.3
01.2
02
2.2
40.3
22
30.5
51.6
96.2
10.4
031.2
629.3
42
13.7
N11.0
Y
HD
110010
BD
+80
389
HIP
61597
GJ
479.1
G0
-12
37
19.2
379
12
55.7
12
19.0
1.0
27.9
40.5
82
124.7
01.0
011.2
01.2
02
10.2
50.6
22
22.4
10.7
12
14.3
20.6
428.5
026.2
91.2
Y2
15.5
Y
HD
111395
HR
4864
HIP
62523
GJ
486.1
G5
V12
48
47.0
524
50
24.8
12
8.6
1.0
58.2
30.9
92
335.0
01.2
02
106.0
01.1
02
18.4
30.3
62
21.6
30.4
32
9.2
21.0
029.8
830.5
95.8
Y2
12.3
Y
HD
113449
BD
204
3408
HIP
63742
G5
V13
349.6
62
59
42.5
72
6.3
0.6
45.2
01.2
72
189.6
00.7
02
223.2
00.8
02
7.8
50.2
82
25.2
40.8
52
16.8
60.6
131.3
530.4
62
6.7
N2
5.4
Y
Ross
1007
HIP
65016
GJ
507.1
M1.5
-13
19
40.1
333
20
47.5
22
11.7
1.0
57.5
22.3
02
296.3
03.8
02
144.2
04.2
02
12.8
10.6
32
25.5
31.0
52
7.6
51.0
029.5
732.5
42
1.4
Y2
18.0
N
HD
116956
BD
+57
1438
HIP
65515
G9
V13
25
45.5
356
58
13.7
72
13.1
0.3
45.7
60.7
22
218.3
00.9
010.7
01.1
02
15.9
00.3
32
18.8
00.2
72
8.8
30.2
726.1
629.4
72.9
Y2
19.1
Y
BD
203
3527
HIP
67092
GJ
524.1
K5
-13
45
5.3
32
437
13.2
54.6
0.5
38.9
71.8
02
166.9
01.9
02
96.4
02.0
02
7.9
90.6
22
22.4
41.0
81.8
40.4
623.8
924.3
93.9
Y7.8
Y
HD
124106
BD
211
3684
HIP
69357
GJ
3827
K1
V14
11
46.1
72
12
36
42.3
73.0
0.5
43.3
51.4
02
256.2
01.1
02
180.4
01.1
02
10.7
90.5
52
32.6
21.1
02
1.6
70.4
034.4
035.6
35.3
Y11.1
N
HD
125874
BD
+38
2549
HIP
70142
K2
V14
21
8.8
637
24
3.6
92
16.0
0.4
23.6
51.1
42
130.0
01.6
02
23.3
01.6
02
16.6
80.8
12
25.4
81.0
62
5.4
00.6
130.9
338.4
91.9
Y2
28.0
N
HD
129333
EK
Dra
HIP
71631
GJ
559.1
AG
1.5
V14
39
0.2
264
17
29.8
42
20.6
0.3
29.4
60.6
12
135.9
01.1
02
25.3
01.2
02
7.2
50.3
22
29.0
70.4
22
4.6
50.3
530.3
228.8
92
11.2
N2
21.6
Y
SA
O252852
GJ
560B
K5
V14
42
28.1
22
64
58
43.0
07.0
4.0
60.9
70.5
82
192.6
40.3
92
234.0
60.4
92
10.8
62.7
92
19.2
12.8
62
10.8
50.3
424.5
924.6
62
0.3
Y7.3
Y
HD
130004
BD
+14
2779
HIP
72146
K0
V14
45
24.1
813
50
46.7
22
10.0
0.6
51.2
00.9
82
230.8
01.0
02
226.7
01.0
02
5.1
20.3
12
30.7
60.6
02
4.9
80.5
331.5
839.5
82
4.9
Y2
26.3
N
HD
130322
BD
+00
3243
HIP
72339
K0
V14
47
32.7
20
16
53.3
22
12.5
0.0
33.6
01.5
12
132.7
01.0
02
140.9
01.1
02
9.7
60.1
82
26.2
91.3
12
10.7
50.1
330.0
332.5
52
1.4
Y2
17.8
Y
HD
134353
BD
+19
2929
HIP
74118
K0
V15
851.9
719
219.0
62
24.3
0.3
26.6
51.1
62
153.8
00.9
02
36.0
00.9
02
22.5
30.5
22
28.4
41.0
12
7.9
80.6
137.1
540.7
19.2
N2
30.9
N
HD
139084
V343
Nor
HIP
76629
K0
V15
38
57.5
52
57
42
27.2
75.1
0.5
25.1
51.0
92
46.2
01.5
02
97.9
01.5
02
6.7
30.6
52
17.3
40.7
42
9.8
20.5
321.0
320.5
52
1.0
Y2.6
Y
HD
139664
gL
up
HIP
76829
GJ
594
F5
V15
41
11.3
82
44
39
40.3
42
5.4
2.0
57.0
90.7
22
168.7
00.7
22
265.6
90.6
02
15.0
81.7
52
19.7
60.9
82
9.7
20.3
226.6
926.1
12.2
Y2
2.0
Y
50 D. Montes et al.
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Tab
le2.
–co
nti
nued
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)
HD
140901
HR
5864
HIP
77358
GJ
599A
G6
V15
47
29.1
02
37
54
58.7
12
5.2
2.0
65.6
00.7
72
414.9
01.2
02
213.7
01.4
02
18.9
41.8
02
27.8
00.8
45.7
40.4
734.1
227.8
119.8
N2
5.2
Y
HD
141272
BD
+02
3001
HIP
77408
GJ
3917
G8
V15
48
9.4
61
34
18.2
62
27.2
0.3
46.8
41.0
52
176.5
01.1
02
165.8
01.0
02
19.5
80.2
42
27.6
10.5
72
13.9
70.2
436.6
234.1
33.6
Y2
24.0
Y
HD
141714
del
CrB
HIP
77512
G3.5
III
15
49
35.6
526
46.2
12
19.1
0.9
19.7
10.7
32
78.1
00.9
02
64.3
00.9
02
5.1
20.5
02
30.0
90.9
42
5.0
10.8
030.9
348.6
62
5.6
Y2
42.5
N
HD
142361
1E
1552.0
-2338
G3
IV15
54
59.8
72
23
47
18.1
62
0.3
1.0
14.0
05.0
02
42.2
01.1
02
65.3
01.1
02
3.2
01.3
92
25.5
09.1
42
5.7
32.0
726.3
328.7
22.5
Y2
11.8
N
HD
147379B
BD
+67
935B
HIP
79762
GJ
617B
M3
-16
16
45.3
367
15
22.5
22
19.4
0.8
93.1
41.3
82
477.4
02.0
091.6
02.1
02
9.8
20.2
42
29.7
20.6
52.9
90.5
631.4
432.0
32
16.4
N2
26.1
N
V2306
Oph
HIP
80824
GJ
628
M3.5
-16
30
18.0
62
12
39
45.3
82
22.0
0.1
234.5
21.8
22
89.7
01.7
02
1184.8
02.0
02
13.6
70.1
12
20.9
40.1
62
20.8
70.1
132.5
728.8
02
7.7
N2
17.7
Y
HD
160934
RE
J1738+
611
HIP
86346
GJ
4020A
K7
-17
38
39.6
361
14
16.0
12
26.7
0.1
40.7
512.1
02
21.8
03.0
043.7
03.0
02
5.0
61.5
92
23.8
80.4
52
12.2
20.6
927.3
012.2
52
1.7
Y2
11.0
N
HD
162283
BD
206
4663
HIP
87322
GJ
696
M0
-17
50
34.0
32
63
1.0
32
21.0
2.0
45.6
72.0
62
24.8
01.9
02
131.5
02.2
02
13.9
91.8
62
19.2
70.9
62
8.1
80.5
125.1
820.8
52.0
Y2
15.7
Y
BD
+18
3497
HIP
87768
GJ
698A
K5
-17
55
44.8
918
30
1.3
72
29.2
1.0
43.4
02.2
12
45.9
41.7
42
47.7
91.6
92
15.6
90.7
32
24.4
80.7
42
7.7
20.4
230.0
818.8
54.8
N2
18.1
N
HD
166348
SA
O228799
HIP
89211
GJ
707
M0
V18
12
21.3
92
43
26
41.4
32
2.0
1.3
77.1
81.2
3133.1
01.1
02
415.4
01.0
02
9.0
51.2
62
17.9
20.3
82
17.8
60.4
026.8
726.4
06.9
N2
5.2
Y
HD
171488
V889
Her
HIP
91043
G2
V18
34
20.1
018
41
24.2
32
24.3
1.5
26.8
70.8
92
20.7
10.6
62
50.9
00.6
62
8.6
71.0
22
24.0
61.1
22
5.5
20.3
426.1
621.5
42
7.0
N2
20.5
Y
HD
174429
PZ
Tel
HIP
92680
K0
V18
53
5.8
72
50
10
49.8
92
0.1
2.0
20.1
41.1
815.8
01.1
02
84.1
01.1
02
7.6
41.8
82
16.3
51.1
22
8.9
60.9
520.1
520.1
82
0.2
Y2
1.3
Y
HD
180809
tet
Lyr
HIP
94713
K0
III
19
16
22.0
938
81.4
32
29.7
0.3
4.2
40.4
92
2.0
00.7
01.4
00.8
02
10.6
10.8
62
27.6
60.4
42
3.4
70.8
929.8
37.6
81.8
N2
7.4
N
HD
181327
SA
O246056
HIP
95270
F6
V19
22
58.9
42
54
32
16.9
82
0.5
2.0
19.7
70.8
124.1
01.4
02
82.9
01.4
02
9.8
41.7
72
16.2
90.9
42
8.1
51.0
020.7
020.7
02
0.3
Y2
0.5
Y
HD
189245
HR
7631
HIP
98470
GJ
773.4
F7
V20
020.2
52
33
42
12.4
32
8.2
5.0
47.9
01.0
6130.7
01.2
02
289.5
01.1
02
13.4
94.3
72
26.1
30.8
12
13.8
02.4
032.4
832.6
12
0.6
Y2
8.7
Y
HD
196982
AT
Mic
HIP
102141
GJ
799A
dM
4.5
e-
20
41
51.1
52
32
26
6.7
32
3.7
3.0
97.8
04.6
5269.3
26.5
52
365.6
94.6
52
9.6
12.4
02
16.8
80.9
42
11.0
01.9
122.3
222.5
01.2
Y2
4.8
Y
GJ
799B
M4
-20
41
48.0
02
32
24
60.0
02
2.7
3.0
97.8
04.6
5269.3
26.5
52
365.6
94.6
52
8.8
12.4
02
16.7
20.9
32
11.6
01.9
022.1
822.5
01.2
Y2
4.8
Y
HD
197481
AU
Mic
HIP
102409
GJ
803
M0
-20
45
9.5
32
31
20
27.2
42
3.3
2.0
100.5
91.3
5278.8
01.6
02
360.0
01.6
02
9.1
51.5
72
16.2
10.4
22
11.1
71.2
221.7
121.9
61.5
Y2
4.9
Y
HD
197890
BO
Mic
HIP
102626
K0
V20
47
45.0
12
36
35
40.8
32
6.5
1.0
22.5
21.6
418.4
01.2
02
80.0
01.2
02
7.1
10.8
22
17.0
21.2
72
0.8
10.7
718.4
616.3
22
6.1
N2
2.3
Y
HD
199065A
HIP
103438
G2
V20
57
22.4
42
59
433.4
611.0
2.0
9.6
31.8
725.4
02.0
02
54.9
01.9
02
7.1
23.4
42
28.5
25.1
42
11.9
81.8
731.7
429.8
02
5.7
Y5.8
Y
HD
199065B
G5
V20
57
21.8
62
59
434.2
311.0
2.0
9.6
31.8
716.7
05.9
02
57.0
05.7
02
4.6
03.4
62
29.6
95.8
12
8.5
62.6
031.2
428.0
92
9.8
N5.5
Y
HD
202575
BD
+08
4638
HIP
105038
GJ
824
K2
-21
16
32.4
79
23
37.8
02
18.0
1.0
61.8
31.0
6143.4
01.6
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116.7
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10.6
00.4
72
19.7
70.7
92
4.6
70.5
222.9
118.0
32
0.3
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11.2
N
HD
202917
SA
O246975
HIP
105388
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-21
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49.9
62
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23.1
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1.0
2.0
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01.5
02
96.5
01.7
02
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11.4
72
20.5
31.2
52
0.6
71.4
022.0
120.5
82
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3.0
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HD
202947
BS
Ind
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105404
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535.4
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02
101.2
02.0
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3.8
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52
23.0
11.6
52
6.2
81.4
224.1
522.1
62
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106231
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206860
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207485
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107457
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207129
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207377
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107806
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02
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31.3
42
22.0
91.0
02
10.4
11.4
524.4
320.0
62
6.3
N5.2
N
HD
207575
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O255093
HIP
107947
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-21
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22
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03.0
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02
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02
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22
20.0
41.0
22
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41.4
121.6
421.0
12
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HD
208313
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108156
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209458
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108859
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11.7
62
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61.4
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90.3
42
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115.9
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10.5
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213845
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113020
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15.9
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16.0
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220140
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115147
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26.6
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72
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50.6
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221503
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116215
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222259
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12.7
N13.9
N
Late-type members of young stellar kinematic groups 51
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
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AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
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02
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12
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450.9
543.4
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11507
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22
28.9
20.4
62
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445.0
42
11.5
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HD
13382
BD
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10117
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219.4
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02
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02
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60.9
22
32.9
20.9
22
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22
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17051
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12653
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02
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12
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533.8
90.8
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02
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10.8
42
16.8
10.7
02
12.0
30.5
344.9
539.5
42
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N
HD
17922
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13528
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HD
18404
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13834
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18632
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19787
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02
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72
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21663
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22001
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22496
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17420
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02
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22
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02
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81.8
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70.9
62
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80.4
538.7
238.9
42
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25998
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02
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21.8
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16.7
80.8
12
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10.3
936.3
637.2
32
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HD
27282
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20146
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117
31
29.1
237.9
0.4
21.2
41.3
2111.1
01.1
02
27.4
01.1
02
41.6
00.5
72
18.9
01.3
32
0.9
30.9
245.7
047.6
31.0
Y40.2
Y
HD
27604
HR
1365
HIP
20109
F7
V4
18
40.0
32
52
51
36.3
420.7
2.0
13.4
90.5
247.1
01.1
074.2
01.0
02
32.0
51.2
82
17.4
51.4
52
7.0
81.4
537.1
734.0
41.3
Y14.4
N
HD
27685
BD
+16
585
HIP
20441
G4
V4
22
44.7
816
47
27.7
439.3
0.4
26.9
61.4
0173.3
011.5
04.6
710.2
02
45.9
11.4
32
17.7
83.3
17.0
43.2
849.7
355.9
89.0
N47.8
N
HD
27989
BD
+18
636
HIP
20686
G5
V4
25
51.7
318
51
50.6
239.2
0.4
23.0
81.2
2108.2
01.0
02
34.9
01.0
02
41.9
10.4
82
17.9
11.1
02
2.2
00.7
045.6
344.9
50.6
Y38.4
Y
GJ
195A
M1-
517
23.7
345
50
22.9
731.2
0.5
72.0
04.0
058.5
05.0
02
410.0
04.8
02
37.8
40.6
62
13.7
31.3
22
9.8
20.7
641.4
339.0
22
8.0
N29.0
Y
HD
35171
111
Tau
BH
IP25220
GJ
201
K2-
523
38.3
817
19
26.8
437.1
2.0
69.7
61.5
0253.3
41.2
12
4.6
60.7
62
37.5
81.9
52
14.4
10.3
47.3
00.4
940.9
045.8
09.5
N43.5
N
HD
35296
V1119
Tau
HIP
25278
GJ
202
F8
V5
24
25.4
617
23
0.7
236.5
2.0
68.1
90.9
4250.9
00.8
02
7.2
00.8
02
36.9
41.9
52
14.6
30.3
07.6
30.4
240.4
646.7
49.6
N44.4
N
HD
37070
22
Cam
HIP
26587
F5-
539
5.4
056
21
36.1
520.0
5.0
16.6
40.7
99.9
01.0
02
132.3
01.0
02
35.1
74.5
22
21.5
62.4
72
11.2
71.3
942.7
648.1
02
6.7
N30.5
N
GJ
3379
M4-
60
4.5
02
42
23.0
030.0
0.1
186.3
06.2
0299.0
01.0
023.0
01.0
02
26.7
00.0
92
15.5
90.1
21.5
90.2
330.9
654.6
22
3.6
Y54.2
N
HD
41700
HR
2157
HIP
28764
GJ
9200
G0
V6
428.4
42
45
211.7
725.8
2.0
37.4
60.5
02
82.4
00.7
0247.1
00.7
02
37.8
10.6
92
10.4
11.7
12
14.6
40.9
141.8
638.1
713.7
N23.6
Y
HD
43931
BD
+13
1199
HIP
30051
F7
V6
19
25.4
113
26
2.1
739.0
5.0
11.6
00.9
720.4
01.4
02
10.5
01.3
02
34.9
94.7
82
19.0
21.8
04.7
50.9
240.1
145.6
77.5
N45.3
N
HD
45609
SA
O171781
HIP
30733
K0
V6
27
24.1
02
25
44
4.2
824.9
0.4
22.5
32.3
81.4
01.2
587.8
01.4
02
28.9
81.6
22
11.0
20.9
60.0
80.8
231.0
034.5
90.8
Y29.3
Y
HD
52265
BD
205
1910
HIP
33719
G0
V7
018.0
42
522
1.7
753.8
0.0
35.6
30.8
42
114.8
01.3
081.5
01.2
02
52.3
20.2
72
20.6
30.3
42
9.0
80.2
956.9
769.4
62
5.5
Y67.1
N
HD
53532
BD
+22
1569
HIP
34271
G0
V7
616.8
022
41
0.5
641.9
0.4
22.7
71.0
32
92.0
01.0
02
77.8
00.9
02
43.2
60.4
22
17.9
30.4
72
13.8
71.1
248.8
473.6
16.9
Y69.5
N
HD
58895A
SA
O235171
HIP
35910
G3
IV7
24
9.3
92
58
29
31.0
119.7
2.0
20.6
10.5
32
87.7
90.5
8137.5
20.5
12
36.8
80.9
72
16.1
91.8
92
13.1
90.6
842.3
839.4
12
10.5
N16.0
Y
HD
62576
1P
up
HIP
37648
K5
III
743
32.3
92
28
24
39.1
832.7
0.9
3.3
40.5
92
13.9
03.1
029.7
02.8
02
56.1
08.9
12
9.0
64.4
42.5
04.6
156.8
872.1
55.5
Y55.4
N
HD
65523
BD
+13
1810
HIP
39068
G5
V7
59
35.6
312
58
59.0
632.8
0.6
29.4
61.5
22
236.1
01.2
02
43.0
01.2
02
43.1
11.0
12
12.8
60.3
52
23.3
01.8
850.6
693.3
21.9
Y85.0
N
HD
70088
BD
+34
1807
HIP
40942
G5
V8
21
20.7
334
18
35.8
732.2
0.5
23.1
21.1
72
118.8
02.2
02
111.3
02.2
02
39.9
20.8
42
22.5
71.0
72
6.9
21.3
546.3
853.1
22
2.4
Y41.4
N
HD
72760
BD
200
2024
HIP
42074
GJ
3507
G5
V8
34
31.6
50
43
33.8
934.6
0.5
45.9
51.0
12
197.5
01.0
018.9
00.9
02
35.1
50.4
52
19.3
80.3
52
2.2
40.4
240.2
036.9
02
2.7
Y30.8
Y
HD
73322
BD
216
2525
HIP
42281
K1
V8
37
15.5
42
17
29
40.7
127.3
0.3
27.0
21.1
82
115.2
01.5
059.7
01.3
02
31.6
10.8
82
15.8
20.4
32
3.7
20.5
435.5
434.7
12
2.3
Y26.3
Y
HD
73171
HR
3408
HIP
42452
K1
III
839
17.6
252
42
41.8
427.3
2.0
8.2
10.8
02
29.1
00.7
02
30.7
00.7
02
34.9
02.1
22
10.3
71.6
74.0
41.8
136.6
330.2
50.1
Y17.9
N
HD
75732
rho
CncA
HIP
43587
GJ
324A
G8
V8
52
35.8
128
19
50.9
627.3
0.5
79.8
00.8
42
484.8
00.7
02
233.5
00.7
02
37.0
80.4
22
18.1
00.1
82
8.0
50.4
142.0
448.3
82
0.6
Y36.3
N
BD
+20
2233
HIP
43701
F5
V8
54
0.5
020
13
49.4
432.7
3.3
10.0
71.2
82
53.1
01.0
02
3.2
00.9
02
39.4
03.1
92
11.9
91.2
62
0.4
73.2
541.1
939.0
55.2
N30.4
Y
BD
+17
1972
HIP
43751
G5
V8
54
41.5
216
36
39.6
916.1
0.5
23.0
73.4
82
134.1
01.3
02
26.6
01.3
02
27.5
02.5
02
10.3
50.6
62
13.6
13.5
032.3
845.4
32
0.2
Y35.7
N
HIP
47620
GJ
360
M2-
942
34.8
470
22.0
26.9
0.5
85.1
43.1
82
672.2
01.9
02
268.3
02.0
02
36.1
61.2
42
13.0
80.6
72
13.9
00.7
640.8
941.1
710.4
N13.4
N
HIP
47650
GJ
362
M3-
942
51.7
270
221.9
16.1
0.5
86.6
92.2
42
667.3
02.1
02
268.5
02.2
02
34.9
10.8
72
13.1
80.4
92
13.8
60.5
739.8
140.2
210.0
N13.1
N
HD
83983
BD
+08
2257
HIP
47587
K0
V9
42
9.9
37
35
24.5
329.7
0.3
23.0
11.2
42
184.7
01.4
04.4
01.4
02
44.0
81.6
72
19.0
40.3
62
5.0
11.4
348.2
850.3
12
0.5
Y32.9
Y
HIP
47758
GJ
366.1
AB
F7/8
V9
44
12.1
02
27
46
10.0
924.0
1.0
8.4
90.7
32
51.6
00.6
036.4
00.6
02
38.6
33.1
32
17.8
11.0
33.1
10.6
942.6
540.6
74.7
N20.8
Y
HD
85301
BD
+49
1889
HIP
48423
G5
V9
52
16.7
749
11
26.8
715.1
0.7
31.0
30.9
82
213.7
01.2
02
68.9
01.3
02
34.7
60.9
42
12.0
70.5
22
7.1
30.8
237.4
838.7
95.1
N18.8
Y
HD
85488
HIP
48411
GJ
371
K5-
952
11.3
63
13
18.6
621.2
5.0
47.6
91.5
32
425.6
01.2
017.2
01.1
02
42.7
42.4
62
16.5
33.0
62
11.9
13.3
947.3
553.6
72
2.5
Y33.1
N
HD
86590
DH
Leo
HIP
49018
GJ
3580
2-
10
01.7
124
33
9.8
99.8
1.0
30.8
21.2
92
234.3
71.1
12
36.1
10.8
12
32.1
51.2
72
13.0
10.5
52
14.9
51.2
437.7
744.6
90.7
Y25.8
N
HD
86322
BD
+75
399
HIP
49163
K1
III
10
159.3
274
45
32.7
26.4
2.0
7.1
80.6
62
50.4
01.2
02
37.3
01.3
02
35.7
83.3
42
21.5
22.7
12
3.3
61.6
141.8
942.8
02
2.5
Y11.2
Y
HD
87598
BD
+69
558
HIP
49686
G5
V10
832.6
368
26
14.9
226.8
0.5
28.1
41.0
72
262.0
01.2
02
135.4
01.1
02
54.3
91.5
32
14.8
31.1
02.8
70.7
156.4
552.1
82.2
Y16.1
N
HD
87978
BD
210
2998
HIP
49674
G5
V10
826.5
82
11
654.7
728.6
0.7
25.4
71.1
32
181.0
01.5
035.2
01.2
02
37.8
71.4
82
23.6
80.5
70.6
20.9
144.6
740.1
42
2.3
Y20.9
N
HD
89376
BD
+21
2172
HIP
50524
K5
V10
19
10.6
420
33
48.2
623.1
2.0
16.8
62.1
32
163.6
00.9
02
19.9
00.9
02
46.4
24.6
72
21.7
01.9
62
7.4
03.7
551.7
754.2
82
1.5
Y28.3
Y
BD
209
3070
HIP
51007
GJ
390
M1-
10
25
10.8
42
10
13
43.3
125.0
5.0
80.0
71.8
02
693.9
01.7
0120.2
01.6
02
42.7
81.3
62
22.9
93.7
72
2.1
23.1
448.6
147.0
02
2.3
Y21.8
Y
HD
91706
BD
222
2952
HIP
51795
F6
V10
34
57.7
02
23
10
34.4
912.1
2.0
15.7
60.7
52
99.1
01.1
033.8
01.1
02
31.0
91.5
02
13.0
01.7
42
1.6
51.1
133.7
433.9
50.6
Y12.7
Y
RY
Sex
GJ
398
M3.5
10
36
1.0
05
712.0
021.0
5.0
71.0
010.0
02
634.0
00.0
095.0
00.0
02
44.6
45.6
02
16.6
02.8
52
2.2
14.6
847.6
848.0
72.9
Y22.1
Y
HD
94402
p01
Leo
HIP
53273
G8
III
10
53
43.7
12
27
45.1
515.3
2.0
10.4
50.8
12
83.3
50.8
415.0
00.7
22
38.3
12.9
52
15.4
71.4
02
1.6
41.9
041.3
541.4
41.5
Y15.6
Y
HD
98356
BD
209
3258
HIP
55235
K0
V11
18
39.7
02
10
734.2
97.5
0.3
23.6
41.2
52
271.7
01.2
081.6
01.2
02
55.5
62.9
82
13.7
70.5
72
3.9
60.6
157.3
858.3
77.1
N14.9
N
HD
99322
HR
4409
HIP
55756
K0
III
11
25
29.4
52
36
347.0
34.3
0.9
11.6
40.7
82
108.3
00.7
017.6
00.7
02
40.6
22.8
82
17.9
61.2
72
6.5
20.7
444.8
944.9
52
3.7
Y6.1
Y
BD
+23
2359
HIP
56238
GJ
430.1
M0.5
11
31
43.3
922
40
1.6
72
5.0
0.5
61.7
61.5
62
586.2
01.4
031.6
01.4
02
39.1
61.0
42
13.8
70.4
22
18.1
50.5
945.3
446.5
21.6
Y2
11.7
N
HD
101112
HR
4478
HIP
56756
K1
III
11
38
9.8
38
53
1.6
411.1
2.0
8.7
40.8
22
58.8
01.2
04.7
01.2
02
30.2
53.0
22
15.1
11.5
31.9
42.0
233.8
732.7
42
0.1
Y7.0
Y
BD
+48
1978
HIP
57859
K0
V11
51
57.8
648
519.5
02
2.1
0.3
20.1
63.0
42
216.7
02.0
047.2
01.9
02
47.6
47.3
82
12.4
82.0
02
17.2
82.3
952.1
951.4
312.5
N2
9.1
N
HD
103847
BD
+20
2661
HIP
58314
G5
V11
57
28.9
319
59
2.0
54.8
0.5
34.3
91.1
62
386.3
00.9
054.1
00.9
02
50.6
31.7
42
17.9
20.6
22
5.4
10.6
053.9
854.2
13.8
Y7.9
Y
HD
106023
BD
+23
2431
HIP
59486
K0
V12
11
59.4
123
535.4
55.8
0.4
22.7
51.1
62
247.7
00.9
02
28.6
00.9
02
42.5
52.1
62
30.2
61.5
32
2.6
00.5
852.2
851.1
42
10.3
N4.7
Y
HD
106453
SA
O180598
HIP
59707
K0+
V12
14
42.1
22
24
46
30.6
72
12.5
0.5
35.5
60.8
32
295.3
01.4
02
32.8
01.2
02
36.2
50.8
12
11.6
50.6
32
16.5
90.3
941.5
338.5
62
9.1
N2
0.4
N
HD
108147
SA
O251899
HIP
60644
F8/G
0V
12
25
46.2
72
64
119.5
22
5.1
0.0
25.9
30.6
92
181.6
00.6
52
60.8
00.5
32
30.3
40.7
52
11.3
40.4
32
14.2
40.4
135.3
832.8
72
12.5
N2
3.5
Y
HD
109200
HIP
61291
GJ
472
K1
V12
33
31.3
82
68
45
20.9
00.3
5.0
61.8
30.6
32
546.1
01.9
02
310.6
01.7
02
35.5
52.6
12
18.7
34.2
52
26.5
70.6
048.1
742.1
12
23.9
N5.1
Y
HIP
61629
GJ
479
M2-
12
37
52.2
32
52
05.2
73.0
2.5
103.5
42.1
02
1023.6
02.9
031.3
02.6
02
38.6
51.5
12
26.7
12.1
72
0.5
00.4
846.9
847.2
60.4
Y6.0
Y
52 D. Montes et al.
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Tab
le3.
–co
nti
nued
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)
DT
Vir
HIP
63510
GJ
494A
aM
2V
e13
046.5
712
22
32.5
52
10.1
5.0
87.5
01.5
12
640.1
01.5
02
25.1
01.4
02
29.7
41.0
02
18.5
41.0
32
8.8
54.8
336.1
534.4
02
6.4
N2
4.5
Y
HD
120136
tau
Boo
HIP
67275
GJ
527A
F6
IV13
47
15.7
417
27
24.8
42
16.1
0.5
64.1
20.7
02
480.8
00.4
050.4
00.4
02
33.5
10.3
52
19.0
30.2
22
7.1
80.4
939.2
037.2
22
4.3
N2
11.3
Y
HD
120780
SA
O241249
HIP
67742
GJ
531
K1
V13
52
35.8
62
50
55
18.1
82
25.0
2.0
60.8
60.9
52
596.4
01.1
02
45.9
01.0
02
51.4
11.4
42
12.0
51.5
22.8
10.4
052.8
848.6
47.3
N2
15.8
N
HD
126535
BD
218
3821
HIP
70608
K1
V14
26
34.7
02
18
49
12.2
02
19.9
0.3
22.2
91.4
62
186.7
00.9
01.8
00.9
02
40.3
91.8
02
18.3
61.7
62.1
11.0
444.4
246.2
23.0
Y2
23.8
Y
HD
131023
BD
+10
2752
HIP
72634
GJ
3868A
K0
V14
51
2.3
19
43
25.1
92
36.0
1.0
36.7
31.2
62
217.5
01.2
054.6
01.3
02
40.6
00.9
42
15.7
10.5
32
15.4
50.9
946.1
935.1
32
0.4
Y2
19.9
N
HD
134319
BD
+64
1046
HIP
73869
GJ
577
G5
-15
549.9
064
249.9
42
6.5
0.1
22.5
90.6
82
123.3
01.1
0110.1
01.2
02
32.4
51.0
52
13.5
90.3
52
2.8
20.2
035.2
935.2
41.2
Y2
6.4
Y
BD
+32
2572
HIP
75011
K0
V15
19
40.1
431
50
33.0
42
26.6
0.4
22.2
71.2
32
181.2
01.4
0141.2
01.4
02
52.6
92.4
52
17.8
90.5
32
1.3
81.2
455.6
657.2
44.4
Y2
30.1
Y
HD
149028
BD
+12
3031
HIP
80936
GV
16
31
37.0
712
25
17.5
82
32.5
0.5
20.6
21.2
12
85.5
00.8
056.4
00.9
02
36.8
60.9
32
15.8
60.3
62
0.6
81.1
740.1
342.3
90.3
Y2
35.3
Y
HD
152178
V2253
Oph
HIP
82583
G8/K
0V
p16
52
56.0
12
26
45
2.3
42
34.8
0.5
2.1
21.2
40.9
01.3
02
13.1
01.3
02
32.2
41.3
72
19.1
713.5
82
25.8
111.9
845.5
334.0
92
24.0
N2
29.6
Y
HD
152260
SA
O257449
HIP
83247
G0
V17
054.6
52
76
13
7.4
12
0.6
5.0
17.6
70.6
72
33.6
00.8
02
159.1
00.8
02
32.6
13.5
92
25.1
43.4
22
14.4
31.8
343.6
345.5
32
7.6
N2
15.1
N
V647
Her
HIP
84794
GJ
669A
M4-
17
19
54.2
126
30
3.0
32
33.6
1.0
83.0
16.0
32
217.6
02.1
0348.8
02.0
02
36.4
71.4
12
18.6
10.7
02
2.0
01.2
340.9
939.3
72
1.8
Y2
31.7
Y
HD
158972
BD
+44
2721
HIP
85639
K0
V17
30
5.3
344
31
9.9
52
29.7
0.4
25.2
80.8
12
13.2
00.9
0133.9
01.0
02
32.6
00.8
32
18.1
50.3
92
11.2
60.3
138.9
731.2
05.0
N2
19.0
N
HD
168603
BD
+33
3073
HIP
89771
K0
V18
19
8.8
233
13
52.5
52
34.0
0.5
27.2
10.8
65.9
01.4
0134.8
01.6
02
36.3
90.7
72
18.7
90.5
42
5.6
10.4
041.3
436.6
51.8
Y2
28.2
Y
HD
171759
zet
Pav
HIP
91792
K0
III
18
43
2.1
42
71
25
41.2
02
16.3
0.9
15.5
50.5
51.1
00.7
02
156.8
00.6
02
43.0
01.3
12
26.4
21.3
72
1.8
40.5
350.5
052.5
52
4.0
Y2
22.2
Y
HD
177720
SA
O245938
HIP
94051
G0
-19
851.1
22
54
217.5
22
30.0
2.0
14.6
01.2
02.5
01.3
02
65.8
01.6
02
34.4
91.9
02
10.9
01.8
06.9
91.0
236.8
427.8
82
4.7
N2
18.5
N
HD
177996
HIP
94050
GJ
4096
K1
V19
850.4
92
42
25
41.1
92
32.0
2.5
31.4
81.9
723.7
01.0
02
121.5
00.9
02
34.4
42.3
52
13.2
91.0
42.9
51.0
637.0
330.5
12
2.5
Y2
24.3
N
HD
180161
BD
+57
1961
HIP
94346
GJ
1233
G8
V19
12
11.3
657
40
19.1
32
27.9
0.4
50.0
00.5
4217.5
00.9
0408.6
00.9
02
44.0
40.4
92
22.7
40.3
82
15.7
50.1
852.0
146.8
52
11.2
N2
19.9
N
HD
179949
HR
7291
HIP
94645
GJ
749
F8
V19
15
33.2
32
24
10
45.6
62
25.5
0.5
36.9
70.8
0116.6
00.9
02
101.7
00.9
02
27.4
30.4
82
12.8
60.2
32
11.2
20.4
432.3
152.8
04.1
Y2
49.1
N
HD
181943
V4371
Sgr
HIP
95266
K1
V19
22
57.2
62
14
15
32.0
42
32.1
1.0
12.9
11.2
858.3
01.4
02
7.8
01.3
02
35.5
71.1
72
8.4
50.7
52
12.6
52.1
538.6
972.1
77.0
Y2
69.2
N
HD
183870
BD
211
5030
HIP
96085
GJ
1240
K2
V19
32
6.7
12
11
16
29.7
92
49.6
0.5
55.5
00.9
0236.7
01.1
018.6
01.2
02
51.1
90.4
62
15.0
40.2
72
4.9
80.3
253.5
963.8
66.6
N2
60.9
N
HD
187565
BD
+29
3760
HIP
97543
F8
V19
49
31.6
429
22
29.9
32
23.0
10.0
10.3
20.9
340.3
01.4
034.5
01.3
02
30.4
34.6
12
11.0
99.1
32
8.5
91.0
233.5
135.4
22
6.8
N2
26.6
Y
HD
189087
BD
+29
3820
HIP
98192
GJ
773.2
K1
V19
57
13.4
129
49
26.5
22
29.9
0.5
39.2
40.9
796.0
01.3
0242.6
01.2
02
40.3
90.7
82
15.1
60.5
65.1
20.2
343.4
445.1
57.6
N2
33.2
Y
HD
192886
HR
7749
HIP
100184
F5
V20
19
17.8
52
47
34
49.0
42
30.8
2.0
33.9
10.8
7190.6
01.1
02
182.5
01.0
02
44.3
21.7
22
17.4
70.6
42
6.2
91.3
048.0
549.4
63.9
Y2
33.2
Y
HU
Del
GJ
791.2
AM
4.5
20
29
49.0
09
41
30.0
02
29.0
0.5
113.8
01.9
0674.0
05.0
0121.0
05.0
02
35.6
00.4
62
15.7
60.4
22
11.7
80.4
240.6
847.4
92
7.8
N2
38.8
N
BD
+33
3930
HIP
101227
K0
V20
31
7.7
733
32
34.5
22
25.2
0.4
22.3
81.1
665.0
01.4
0101.8
01.4
02
31.5
41.3
52
16.8
90.5
53.0
80.3
435.9
132.7
94.6
N2
21.0
Y
HD
195818
SA
O246651
HIP
101636
G0
-20
36
2.3
52
54
56
29.0
92
22.5
2.0
15.1
61.2
049.9
01.6
02
82.7
01.8
02
32.9
32.0
22
18.1
02.0
62.5
31.5
437.6
636.2
22
5.3
N2
20.7
Y
HD
197039
BD
+15
4227
HIP
102029
F5
-20
40
35.3
115
38
35.7
02
32.5
2.0
14.3
60.8
891.4
00.8
046.9
00.9
02
43.6
62.0
22
16.0
31.8
22
6.5
91.1
646.9
752.2
02
2.1
Y2
39.7
N
HD
200560
BD
+45
3371
HIP
103859
GJ
816.1
AK
2-
21
240.7
545
53
5.1
72
14.5
0.2
51.6
50.7
2396.1
00.8
0141.0
00.8
02
34.5
00.4
82
12.9
40.2
02
18.4
80.2
841.2
239.1
52
16.4
N2
17.7
Y
HD
200968
BD
214
5936
HIP
104239
GJ
819A
K1
V21
710.3
82
13
55
22.5
02
33.2
0.4
56.6
71.1
8382.3
00.9
02
39.9
00.8
02
42.2
90.5
22
17.9
60.2
12
5.0
40.5
846.2
249.2
30.2
Y2
37.3
Y
HD
202605
BD
201
4138
HIP
105066
K0
V21
17
2.1
32
14
38.7
32
23.2
0.3
23.3
31.3
2160.5
00.8
02
23.3
00.8
02
32.9
81.2
12
19.1
60.3
52
13.0
21.4
940.3
045.8
92
9.4
N2
33.3
N
HD
203842
HR
8191
HIP
105695
F5
III
21
24
24.5
610
10
27.3
12
33.2
2.0
9.4
70.7
872.2
01.4
020.6
01.4
02
45.3
33.0
12
21.0
01.7
02
4.3
02.1
650.1
450.5
92
1.7
Y2
33.9
Y
HD
205067
HIP
106438
G2
V21
33
30.9
82
27
53
24.9
32
26.6
20.0
21.1
90.9
5200.7
01.7
02
63.5
01.6
02
47.2
713.0
42
22.8
44.7
92
12.9
914.5
754.0
861.7
82
1.0
Y2
40.0
N
BD
205
5715
HIP
109388
GJ
849
M3.5
-22
940.3
52
438
26.6
22
15.3
0.5
113.9
72.1
01136.1
01.8
02
21.8
02.1
02
43.4
00.7
32
17.4
40.3
42
16.7
50.6
349.6
856.6
12
4.8
Y2
31.5
N
HD
212754
34
Peg
HIP
110785
F7
V22
26
37.3
94
23
37.5
42
17.8
2.0
25.3
41.6
6291.5
01.1
050.7
01.1
02
54.3
03.3
32
17.1
91.4
22
11.7
12.0
958.1
562.9
60.0
Y2
30.0
N
HIP
111766
GJ
865
M3.5
-22
38
29.7
52
65
22
42.6
22
11.0
10.0
67.4
46.4
7833.2
95.0
42
160.2
06.2
82
55.3
97.2
32
19.5
44.8
52
15.1
27.5
960.6
561.1
511.2
N2
17.5
Y
HD
215274
BD
+29
4742
HIP
112219
G5
V22
43
40.4
730
533.0
72
9.8
0.4
22.2
70.9
7241.1
01.2
025.9
01.1
02
45.8
42.0
62
20.2
80.6
32
15.7
40.9
352.5
452.8
92
11.5
N2
16.3
N
HD
217382
BD
+83
640
HIP
113116
K4
III
22
54
24.9
684
20
46.2
42.9
0.9
8.3
50.4
898.0
00.3
023.8
00.4
02
52.0
72.9
62
20.7
21.5
22
12.0
60.8
757.3
256.6
72
9.2
N4.3
Y
HD
222143
BD
+45
4288
HIP
116613
GJ
4351
G3/4
V23
37
58.4
946
11
57.9
72.0
0.8
43.2
60.8
0356.9
01.2
02
12.0
01.2
02
34.4
00.7
22
13.8
20.7
92
12.6
90.3
439.1
837.9
02
10.0
N2.1
Y
HD
222422
BD
219
6489
HIP
116819
G5
V23
40
37.8
52
18
59
20.0
410.6
0.4
38.1
11.0
0303.5
01.3
02
43.6
01.1
02
28.7
20.8
42
17.1
90.5
72
21.1
30.4
839.5
838.3
32
7.2
N8.2
Y
HD
223252
20
Psc
HIP
117375
G8
III
23
47
56.5
42
245
41.7
62
6.9
2.0
11.1
90.8
596.5
00.5
05.4
00.5
02
36.9
82.8
32
18.6
51.5
32
2.9
51.8
941.5
241.4
32
2.1
Y2
6.7
Y
BD
+45
4378
HIP
118212
GJ
913
M0-
23
58
43.4
946
43
44.9
73.6
1.0
57.6
22.8
2646.7
01.3
02
4.7
01.3
02
47.7
62.3
22
20.4
01.4
62
12.1
00.6
253.3
352.4
82
8.7
N0.4
Y
Late-type members of young stellar kinematic groups 53
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Ta
ble
4.
Urs
aM
ajor
mov
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gro
up.
Nam
eS
pT
a(2
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d(2
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Vr
pma
cosd
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UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
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as/y
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m/s
)(k
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)(k
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)(k
m/s
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m/s
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m/s
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HD
745
BD
+08
13
HIP
954
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III
011
47.5
39
823.8
62
1.8
0.3
7.8
10.9
62
34.7
01.3
02
18.4
01.4
023.7
93.1
01.4
40.9
12
1.9
30.7
623.9
124.1
07.7
N2
8.5
N
HD
2410
46
Psc
HIP
2213
gG
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027
58.4
719
30
50.5
38.3
2.0
6.1
20.7
92
22.2
00.8
02
18.8
00.8
018.0
52.8
55.9
81.4
22
14.6
61.8
624.0
122.7
52.6
N4.1
Y
HD
11131
khi
Cet
BH
IP8486
GJ
9061B
G0
-1
49
23.3
42
10
42
12.7
32
4.2
0.2
43.4
74.4
82
150.0
00.9
02
91.1
00.9
019.3
11.8
62.0
70.2
92
2.5
90.7
019.5
919.7
31.9
Y2
5.1
Y
HD
11171
khi
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AH
IP8497
GJ
9061A
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149
35.1
02
10
41
11.0
92
0.9
1.5
42.3
50.8
72
148.1
00.7
02
95.7
00.7
018.7
40.6
61.9
10.1
82
5.9
51.4
019.7
520.3
91.4
Y2
5.3
Y
HD
13594
HR
647
HIP
10403
F4
V2
14
2.4
347
29
3.3
52
8.1
1.5
24.0
70.9
62
77.3
01.6
02
53.3
01.5
015.7
51.1
70.4
21.0
62
12.6
20.7
920.1
920.2
32
1.3
Y2
8.3
Y
HD
13959
BD
+05
307
HIP
10552
GJ
91.1
K4
V2
15
53.3
96
37
34.8
30.2
0.1
26.3
73.6
92
111.3
01.7
02
56.0
01.6
017.9
82.6
95.6
71.0
12
12.0
91.8
022.4
021.9
44.5
N0.3
Y
HD
14274
BD
+33
406
HIP
10820
G5
III
219
17.0
334
157.9
42
5.9
0.2
3.4
11.1
02
8.1
01.4
02.3
01.5
011.6
72.9
15.7
93.8
01.4
72.1
813.1
17.8
69.0
N2
2.4
Y
HD
24160
gE
riH
IP17874
G9
III
349
27.2
42
36
12
0.8
82.0
1.0
15.5
40.5
82
51.2
00.7
02
53.6
00.8
019.7
40.8
90.3
80.5
72
11.1
90.8
722.6
922.8
02
2.0
Y3.6
Y
HD
24916
BD
201
565
HIP
18512
GJ
157A
K4
V3
57
28.7
02
19
34.0
44.3
0.9
63.4
12.0
02
181.9
01.0
02
141.9
01.0
07.4
00.7
90.3
40.1
72
16.1
60.7
317.7
817.9
00.7
Y4.9
Y
HD
26913
V891
Tau
HIP
19855
G8
V4
15
25.7
96
11
58.7
52
7.1
0.1
47.8
61.1
52
102.6
01.0
02
112.8
01.1
013.8
90.2
22
1.3
10.1
52
9.1
70.3
416.7
016.3
32
2.3
N2
6.6
Y
HD
26923
V774
Tau
HIP
19859
G0
IV4
15
28.8
06
11
12.7
12
7.1
0.1
47.2
01.0
82
111.1
01.4
02
106.3
01.4
014.0
20.2
32
0.2
90.1
82
9.6
00.3
516.9
916.8
32
1.2
Y2
6.8
Y
HD
28495
BD
+64
458
HIP
21276
GJ
3295
G0
V4
33
54.2
664
37
59.5
12
11.0
0.3
36.3
21.0
72
80.0
01.7
040.7
01.7
014.4
40.3
52.9
90.4
32
6.3
80.3
116.0
716.1
23.8
N2
11.7
Y
HD
29697
V834
Tau
HIP
21818
GJ
174
K3
V4
41
18.8
520
54
5.4
40.4
0.3
74.1
31.2
42
233.9
00.9
02
254.3
00.8
05.7
10.3
12
3.6
00.0
92
21.0
40.3
722.0
926.9
82
5.6
N16.5
N
alf
Cae
BH
IP21770
GJ
174.1
BG
2V
440
33.7
12
41
51
49.5
12
0.6
0.9
49.6
70.5
32
141.1
80.5
32
74.9
50.4
910.0
70.3
05.9
30.6
22
9.8
20.6
115.2
614.4
25.2
N2
1.5
Y
HD
31000
BD
+36
958
HIP
22776
G5
V4
53
56.2
136
45
26.7
62
6.2
0.4
35.1
41.1
27.6
01.1
011.9
01.2
06.0
30.3
92
0.7
30.2
02.2
80.2
06.4
92.2
01.2
N2
1.6
Y
HD
33564
BD
+79
169
HIP
25110
GJ
196
F6
V5
22
33.5
379
13
52.1
32
9.9
0.9
47.6
60.5
22
78.5
00.7
0161.0
00.7
019.2
50.5
95.6
50.6
22
3.5
90.3
520.3
821.9
68.7
N2
15.5
Y
HD
38393
gam
Lep
AH
IP27072
GJ
216A
F6
V5
44
27.7
92
22
26
54.1
82
9.7
0.9
111.4
90.6
02
292.4
30.4
62
368.4
60.4
118.3
50.5
74.5
90.6
02
11.6
80.3
822.2
320.9
21.7
Y2
6.4
Y
gam
Lep
BG
J216B
K2
V5
44
26.5
42
22
25
18.7
72
9.7
0.9
111.4
90.6
02
303.7
02.6
02
358.0
02.6
018.0
00.5
75.0
70.6
02
11.9
50.3
922.1
920.8
12.3
N2
6.3
Y
HD
41593
V1386
Ori
HIP
28954
GJ
227
K0
V6
640.4
815
32
31.5
82
9.8
0.1
64.7
10.9
12
120.1
01.0
02
103.0
01.1
010.5
50.1
00.2
50.1
02
10.9
10.2
015.1
818.3
00.3
Y2
14.2
Y
HD
56168
BD
+67
483
HIP
35628
K0
V7
21
6.7
367
39
42.6
02
9.1
0.5
39.1
01.1
52
70.8
01.0
069.5
01.1
08.4
90.3
95.3
80.4
02
11.2
50.3
315.0
922.1
22
3.6
N2
18.9
N
HD
59747
BD
+37
1738
HIP
36704
G5
V7
33
0.5
837
147.4
62
16.2
0.4
50.8
01.2
92
49.6
01.4
010.0
01.4
013.0
70.3
72.7
00.1
72
10.3
30.2
416.8
821.3
21.7
Y2
20.9
Y
HD
60491
BD
206
2184
HIP
36827
K2
V7
34
26.1
72
653
48.0
42
9.7
0.7
40.3
21.2
62
80.9
01.1
02
42.5
01.1
05.9
90.5
15.9
70.5
02
11.7
50.4
014.4
810.1
17.8
N2
6.9
Y
HD
61606
BD
203
2001
HIP
37349
GJ
282A
K2
V7
39
59.3
32
335
51.0
12
18.5
0.4
70.4
40.9
471.7
01.2
02
276.1
01.3
025.5
20.3
52
2.2
30.3
42
7.4
00.1
326.6
624.2
22
9.5
N2
17.6
Y
HD
63433
BD
+27
1490
HIP
38228
G5
IV7
49
55.0
627
21
47.4
52
15.7
20.0
45.8
40.8
92
9.2
01.2
02
12.5
01.1
013.6
217.7
62.2
94.1
92
7.6
38.1
815.7
86.6
20.0
Y2
6.4
N
HD
64942
BD
209
2287
HIP
38747
G5
V7
55
58.2
32
947
49.9
42
8.1
0.8
20.6
91.1
523.4
01.3
02
24.9
01.2
011.1
80.6
81.3
00.6
90.4
30.3
611.2
66.2
82
6.2
N2
4.1
Y
HD
71974
BD
+35
1834
HIP
41820
G5
V8
31
35.0
334
57
58.4
42
15.4
0.6
34.8
31.3
72
5.9
01.4
016.9
01.5
012.0
30.5
04.0
30.2
42
9.0
60.3
815.5
940.4
41.0
Y2
40.4
N
HD
72905
pi1
UM
aH
IP42438
GJ
311
G1.5
Vb
839
11.7
065
115.2
72
14.4
0.1
70.0
70.7
12
28.9
01.0
088.5
01.0
011.2
40.0
92
0.1
00.1
02
10.9
90.0
915.7
213.0
02.2
N2
11.6
Y
HD
75605
HR
3512
HIP
43352
G5
III
849
51.5
02
32
46
49.8
92
7.8
1.5
14.2
61.2
50.5
01.1
02
48.0
01.0
013.7
81.1
83.1
81.4
92
10.7
40.9
717.7
616.8
52
0.8
Y2
5.5
Y
HD
75935
SA
O80487
HIP
43670
G8
V8
53
49.9
426
54
47.6
92
19.0
0.6
24.6
61.3
413.4
01.1
02
5.3
01.1
016.0
80.5
03.6
80.2
72
9.8
30.4
419.2
08.8
52.1
N2
8.7
N
HD
76218
BD
+36
1888
HIP
43852
G5
V8
55
55.6
836
11
46.2
72
12.8
0.5
38.2
11.0
02
24.7
01.2
02
13.0
01.3
07.8
40.4
02
0.2
60.1
72
10.6
90.3
513.2
624.6
62
2.7
N2
24.6
N
HD
80388
BD
+79
305
HIP
46298
G1
V9
26
28.7
678
26
16.0
92
12.0
5.0
19.2
00.8
829.7
01.1
026.2
01.1
014.7
02.9
12
1.7
13.0
12
4.5
52.8
115.4
812.6
62
5.2
N2
9.6
Y
HD
81659
BD
213
2855
HIP
46324
G6/G
8V
926
42.8
32
14
29
26.6
72
16.8
0.5
25.0
71.0
037.2
01.1
02
129.7
01.1
025.6
80.8
60.5
70.6
92
16.5
30.5
030.5
531.4
61.3
Y2
18.5
Y
HD
85444
39
Hya
HIP
48356
G7
III
951
28.6
92
14
50
47.8
02
13.5
1.5
11.9
20.8
117.8
00.8
02
25.3
00.7
015.0
11.0
06.3
61.3
02
8.2
40.8
118.2
714.2
13.5
N2
7.9
Y
HD
85512
SA
O221544
HIP
48331
GJ
370
K-M
V9
51
7.0
52
43
30
10.0
12
9.6
2.0
89.6
70.8
2461.6
01.1
02
469.9
01.1
034.3
60.3
410.0
01.9
82
4.9
50.2
936.1
330.6
117.0
N2
3.5
N
BD
+03
2316
HIP
49544
GJ
378.2
K7
-10
656.8
62
57
51.9
02
15.7
0.5
44.7
71.9
62
67.6
01.5
02
96.0
01.5
05.1
50.2
60.4
70.5
42
19.3
50.5
520.0
38.4
02
11.1
N2
6.3
N
HD
88355
34
Leo
HIP
49929
F6
V10
11
38.2
113
21
18.4
22
16.0
2.0
14.4
90.8
437.8
00.8
02
35.2
00.8
021.6
41.2
62
0.7
21.0
52
8.5
31.5
623.2
730.5
22.9
Y2
25.6
N
HD
88654
BD
207
2985
HIP
50061
G5
V10
13
16.4
32
826
43.9
82
7.0
0.4
10.8
00.9
623.0
00.9
02
30.0
00.9
016.9
71.4
62
1.5
10.7
62
5.8
30.4
618.0
120.5
33.6
N2
12.6
Y
HD
89025
zet
Leo
HIP
50335
F0
III
10
16
41.4
223
25
2.3
22
15.0
1.5
12.5
60.7
819.8
40.9
82
7.3
00.5
014.3
70.9
33.1
30.4
92
8.5
11.2
716.9
916.8
42.7
N2
15.1
Y
HD
91480
37
UM
aH
IP51814
F1
V10
35
9.6
957
457.4
92
10.4
0.5
37.8
00.6
165.6
50.4
537.1
10.3
812.4
00.3
03.2
50.1
82
5.7
70.4
014.0
620.4
22
0.1
Y2
18.1
N
HD
95650
DS
Leo
HIP
53985
GJ
410
dM
2e
-11
238.3
421
58
1.7
02
13.9
2.0
85.7
61.3
6141.1
01.2
02
51.5
01.2
012.4
30.6
83.5
10.5
42
9.7
61.8
116.1
913.6
82.2
N2
11.1
Y
HD
98712
SZ
Crt
HIP
55454
GJ
425A
K4/5
V11
21
26.6
72
20
27
13.6
13.7
5.0
76.0
01.7
0181.7
01.4
02
117.5
01.4
013.7
30.5
22
2.5
73.9
40.8
83.0
614.0
013.1
65.3
N4.4
Y
HD
100043
BD
212
3442
HIP
56154
F2
V11
30
38.7
72
13
30.9
62
1.8
0.0
15.5
60.8
231.4
01.1
02
52.0
01.2
015.9
30.9
72
4.6
90.4
52
8.3
60.5
018.5
920.1
62
1.9
Y2
8.2
N
HD
100310
BD
+53
1497
HIP
56337
K0
V11
32
57.0
652
31
25.3
72
9.6
0.4
22.3
31.2
260.6
00.8
02
9.6
00.9
015.7
30.7
00.6
10.2
92
3.7
40.4
516.1
822.3
72
3.5
N2
18.5
N
HD
102070
zeta
Crt
HIP
57283
G8
IIIa
11
44
45.7
82
18
21
2.4
62
2.6
1.5
9.3
10.8
129.6
00.4
02
28.4
00.5
019.4
61.8
20.2
21.1
32
8.0
21.1
821.0
521.7
13.0
N2
6.6
Y
FI
Vir
HIP
57548
GJ
447
M4
-11
47
44.4
00
48
16.4
32
13.0
5.0
299.5
92.2
0605.6
62.2
92
1219.3
21.6
817.7
10.1
42
3.9
62.5
32
17.4
34.3
125.1
624.1
72
6.5
N2
12.8
Y
HD
238087
BD
+59
1428
HIP
59496
GJ
457
K5
-12
12
5.2
158
55
35.1
22
14.2
10.0
35.2
41.2
496.4
01.7
013.8
01.8
015.7
93.6
51.9
23.9
92
10.9
68.4
319.3
220.2
40.4
Y2
15.4
Y
BD
+19
2531
HIP
59152
K2
V12
750.9
218
56
55.8
22
5.5
0.4
25.2
71.4
0119.7
01.0
02
72.8
01.1
026.6
11.4
92
0.2
50.2
42
3.6
00.4
126.8
534.1
91.4
Y2
21.9
N
HD
238090
BD
+55
1519
HIP
59514
GJ
458A
M0
-12
12
20.8
654
29
8.7
12
13.9
5.0
65.2
91.4
7233.1
01.5
091.5
01.5
016.9
51.7
08.7
31.7
12
12.6
74.4
022.8
926.4
76.4
N2
20.3
N
HD
109647
BD
+52
1638
HIP
61481
K0
-12
35
51.2
851
13
17.3
02
9.0
0.3
38.0
81.1
1108.8
01.2
02
4.8
01.2
014.1
60.4
03.6
40.2
82
7.1
40.2
816.2
719.5
31.1
Y2
14.1
Y
HD
109799
HR
4803
HIP
61621
F1
IV12
37
42.2
82
27
819.9
92
0.9
1.5
28.9
10.7
580.4
00.9
02
93.7
00.9
016.1
20.7
70.1
81.0
72
12.2
80.9
420.2
720.2
52
1.1
Y2
1.1
Y
54 D. Montes et al.
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Tab
le4.
–co
nti
nued
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)
HD
110463
BD
+56
1618
HIP
61946
GJ
3743
K3
V12
41
44.5
255
43
28.8
32
9.7
0.3
43.0
60.8
2122.5
01.4
02
5.6
01.4
014.4
50.2
92.8
70.2
32
7.7
10.2
716.6
319.3
50.2
Y2
13.9
Y
HD
111456
BD
+61
1320
HIP
62512
GJ
9417
F6
V12
48
39.4
660
19
11.6
12
12.0
1.5
41.3
93.2
0108.7
01.3
02
1.1
01.4
014.1
70.9
61.1
50.8
82
9.8
41.2
617.2
917.6
10.0
Y2
12.5
Y
HD
112196
BD
+22
2522
HIP
63008
F8
V12
54
40.0
222
628.5
52
8.0
0.0
29.1
91.6
052.1
00.9
02
33.9
00.9
09.6
10.6
10.5
90.1
72
8.5
60.0
412.8
811.9
52
0.2
Y2
6.4
Y
HD
113139
78
UM
aH
IP63503
F2
V13
043.7
056
21
58.8
22
9.8
0.5
40.0
60.6
0108.3
60.5
02.6
70.5
112.8
80.2
23.2
50.2
52
9.1
60.4
416.1
417.4
21.8
N2
11.9
Y
HD
114723
BD
+32
2327
HIP
64405
F8
-13
12
2.0
232
57.8
82
12.7
2.0
12.8
21.4
815.3
02.0
02
6.4
01.8
05.7
81.1
52
0.1
20.8
12
12.8
71.9
914.1
17.3
70.5
Y2
4.1
N
HD
115043
BD
+57
1425
HIP
64532
GJ
503.2
G2
V13
13
37.0
156
42
29.7
62
9.3
0.3
38.9
20.6
7112.8
00.9
02
19.5
01.0
014.5
20.2
62.1
90.2
12
8.0
80.2
716.7
618.6
12
0.2
Y2
12.3
Y
HD
238224
BD
+58
1441
HIP
65327
GJ
509.1
M0
V13
23
23.2
957
54
21.9
92
6.6
5.0
39.8
41.4
4118.5
01.6
02
19.5
01.7
013.9
81.2
03.7
12.3
82
6.2
14.2
715.7
418.7
60.1
Y2
12.1
Y
HIP
66077
GJ
516A
M2.5
-13
32
44.5
916
48
39.0
52
1.8
0.0
72.6
640.6
0252.9
540.9
02
221.8
323.3
020.8
212.4
82
1.4
72.6
92
7.0
33.1
022.0
223.5
32
2.4
N2
8.8
N
HD
125451
18
Boo
HIP
69989
GJ
3841
F5
IV14
19
16.2
813
015.4
72
3.0
1.5
38.3
30.8
1106.1
00.7
02
32.7
00.7
010.1
40.6
95.3
50.1
72
8.1
31.3
714.0
513.1
44.7
N2
2.4
Y
HD
128311
BD
+10
2710
HIP
71395
GJ
3860
K0
-14
36
0.5
69
44
47.4
62
9.6
0.4
60.3
50.9
9204.5
01.1
02
250.1
01.1
016.8
70.4
32
4.4
90.1
32
20.7
70.4
127.1
324.8
42
5.7
N2
2.3
N
HD
129798
DL
Dra
HIP
71876
F2
V14
42
3.2
561
15
42.8
72
6.8
1.0
23.4
70.5
776.4
01.3
02
33.2
01.5
015.7
30.5
03.0
80.6
82
8.5
10.8
118.1
519.7
82
0.3
Y2
10.4
Y
HD
131156A
ksi
BooA
GJ
566A
G8
V14
51
23.1
019
62.0
03.0
0.9
149.2
60.7
6152.8
10.6
42
71.2
80.7
05.7
50.4
02.1
40.1
70.0
70.7
96.1
45.2
81.2
N0.8
Y
CE
Boo
HIP
72944
GJ
569A
dM
2-
14
54
29.0
016
63.6
92
7.2
0.5
101.9
11.6
7277.7
01.9
02
132.7
01.9
08.1
70.3
22.9
10.1
42
13.4
80.4
516.0
314.0
53.1
N2
1.4
Y
HD
134083
oB
oo
HIP
73996
GJ
578
F5
V15
718.0
724
52
9.1
12
7.3
2.0
50.7
00.7
6184.8
10.9
02
163.5
10.5
317.7
00.8
92
1.1
70.6
12
16.4
61.7
324.2
023.3
02
1.4
Y2
3.6
Y
HD
139194
BD
+36
2621
HIP
76330
K0
V15
35
30.1
636
12
34.6
42
14.0
0.3
33.3
70.8
8118.8
01.1
02
92.5
01.3
014.4
70.5
52
3.1
80.2
42
20.8
40.3
725.5
721.7
90.6
Y2
4.2
N
HD
141003B
bet
aS
erB
dK
3-
15
46
11.2
615
25
18.5
71.4
0.3
21.3
10.8
668.5
41.4
82
41.3
10.6
813.6
30.5
74.0
60.3
02
10.8
00.5
717.8
617.5
63.2
N1.3
Y
HD
147513
SA
O207622
HIP
80337
GJ
620.1
AG
5V
16
24
1.2
92
39
11
34.7
313.0
0.1
77.6
90.8
672.3
00.7
03.3
00.7
013.6
10.1
02
1.1
30.0
72
1.3
70.0
713.7
35.5
41.7
N3.7
N
HIP
80459
GJ
625
M1.5
-16
25
24.6
354
18
14.7
92
12.8
0.5
151.9
31.1
1434.4
02.6
02
174.0
02.6
08.1
10.1
22
2.2
20.3
72
17.5
00.3
519.4
214.1
45.4
N2
4.0
N
HD
150706
BD
+80
519
HIP
80902
GJ
632
G3
V16
31
17.5
879
47
23.1
82
16.8
0.3
36.7
30.5
695.1
00.8
02
89.2
00.8
019.3
40.2
72
4.3
20.2
82
13.1
50.2
023.7
819.8
02
2.2
N2
10.7
N
HD
152863
56
Her
HIP
82780
G5
III
16
55
2.1
625
43
50.4
51.1
0.9
7.1
40.6
719.3
01.0
02
19.1
01.0
013.3
01.4
51.3
70.7
72
12.1
41.4
418.0
618.1
51.6
Y2.6
Y
HD
155674A
BD
+54
1861
HIP
83988
GJ
659A
K0
-17
10
10.5
154
29
39.7
83.0
0.1
47.1
41.8
882.5
01.4
02
111.6
81.5
012.5
00.5
25.3
20.1
72
4.3
90.2
914.2
814.2
82
0.5
Y3.0
Y
HD
155674B
BD
+54
1862
HIP
83996
GJ
659B
K8
-17
10
12.3
654
29
24.4
82.5
0.1
47.8
63.1
186.9
01.4
02
106.1
01.5
011.7
80.7
85.2
20.2
52
4.9
70.4
513.8
113.9
00.2
Y3.0
Y
HD
165185
SA
O209710
HIP
88694
GJ
702.1
G5
V18
623.7
22
36
111.2
515.2
0.2
57.5
80.7
7106.8
01.2
07.4
01.2
014.4
20.2
03.7
30.1
42
9.3
30.1
717.5
817.1
02.9
N14.9
Y
HD
167389
SA
O47313
HIP
89282
F8:
-18
13
7.2
341
28
31.3
12
3.0
2.6
29.9
10.5
951.4
00.8
02
128.1
00.8
017.2
00.9
42
3.7
52.2
12
13.3
31.1
122.0
821.8
52
1.9
Y2
1.6
Y
HD
171746
HR
6981
HIP
91159
G2
V18
35
53.2
416
58
31.8
48.4
0.0
29.2
31.5
449.9
01.7
02
67.2
01.6
011.9
00.4
13.2
30.2
62
10.1
40.7
315.9
615.1
72.5
N7.2
Y
HD
173950
BD
+38
3292
HIP
92122
G5
V18
46
34.6
338
21
3.3
08.2
0.8
27.0
10.9
316.2
01.6
02
84.1
01.6
015.6
50.6
24.6
20.7
32
5.1
90.4
617.1
215.0
22
2.6
N2.5
Y
HD
184960
HR
7451
HIP
96258
GJ
4116
F7
V19
34
19.7
951
14
11.8
42
0.1
0.2
39.0
80.4
732.1
01.0
02
187.5
01.1
019.1
30.2
81.0
70.2
02
12.8
60.2
123.0
823.0
62
0.7
Y2
0.1
Y
HD
194943
rho
Cap
HIP
101027
GJ
791.1
AF
3V
20
28
51.6
22
17
48
49.4
118.4
2.0
33.0
40.8
62
2.7
04.4
02
16.5
04.2
015.1
61.6
25.0
30.9
82
9.4
41.1
418.5
56.7
72
0.5
Y6.3
N
HD
199951
gam
Mic
HIP
103738
G6
III
21
117.4
62
32
15
27.9
417.6
0.9
14.5
90.7
92
3.3
00.7
02.0
00.7
013.7
50.6
93.4
70.2
72
10.5
00.6
217.6
51.7
51.2
N1.7
N
BD
205
5480
HIP
104383
M1
-21
845.4
72
425
36.9
56.6
0.5
37.9
12.2
82
75.3
63.4
62
33.0
91.3
712.1
00.7
20.6
10.4
01.6
70.5
912.2
310.6
78.3
N8.8
Y
HD
205435
rho
Cyg
HIP
106481
G5
III
21
33
58.8
545
35
30.6
16.9
0.9
26.2
00.5
12
25.2
00.8
02
95.0
00.8
014.9
20.3
66.3
10.9
02
10.0
70.2
719.0
717.8
30.9
Y1.6
Y
HD
211575
BD
200
4333
HIP
110091
F3
V22
18
4.2
70
14
15.5
614.8
0.0
24.1
10.9
22
40.5
00.9
02
54.9
00.9
016.5
30.5
52.8
00.3
12
10.8
50.1
519.9
718.8
61.6
Y13.4
Y
EV
Lac
HIP
112460
GJ
873
M3.5
-22
46
49.7
344
20
2.4
00.5
2.0
198.0
72.0
52
705.6
01.5
02
460.3
01.3
019.7
30.4
23.7
91.9
22
1.7
90.4
520.1
717.2
710.4
N0.7
Y
HD
217813
MT
Peg
HIP
113829
GJ
2153
G1
V23
34.9
820
55
6.8
82
2.5
1.3
41.1
90.8
72
116.7
00.9
02
27.5
00.9
013.2
20.3
10.5
81.0
64.6
40.7
614.0
210.3
29.9
N2
3.7
Y
Late-type members of young stellar kinematic groups 55
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Ta
ble
5.
IC2
39
1su
per
clu
ster
.
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
WV
Tota
lV
TP
Vr
c
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)(k
m/s
)
HD
6288A
26
Cet
AH
IP4979
F1
V1
349.0
31
22
0.6
45.6
2.0
17.6
60.7
2122.5
00.6
02
40.7
00.6
02
23.6
11.1
02
24.5
21.3
32
8.5
51.7
635.1
036.2
82
2.9
Y11.1
Y
HD
8941
BD
+16
154
HIP
6869
2-
128
24.3
617
445.3
28.5
2.0
19.9
90.7
9117.5
40.7
82
34.3
20.4
82
23.4
21.2
82
17.5
61.3
42
7.6
61.4
230.2
630.6
72.0
Y10.1
Y
HD
13357
BD
+13
343
HIP
10175
G5
IV2
10
52.0
813
40
59.7
925.7
0.5
20.4
11.7
5111.7
11.8
12
73.2
41.4
62
28.2
71.1
92
19.3
62.5
22
21.1
90.5
340.2
935.2
62
5.3
N17.6
N
HD
14802
kap
For
HIP
11072
GJ
97
G2
V2
22
32.5
52
23
48
58.7
718.4
2.0
45.6
00.8
2197.3
40.7
72
4.3
90.5
12
19.3
30.6
82
16.8
10.4
42
10.1
71.8
727.5
626.6
42
1.7
Y17.1
Y
HD
16699
1E
S0237-5
3.1
AH
IP12326
2-
238
44.2
92
52
57
3.0
616.1
1.1
16.3
11.4
781.3
02.2
048.6
02.1
02
25.5
42.4
92
16.7
71.1
32
9.1
51.0
831.8
933.4
41.0
Y19.0
Y
HD
17190
BD
+25
449
HIP
12926
GJ
112
K2
IV2
46
15.2
125
38
59.6
614.2
1.0
38.9
51.1
3238.7
01.0
02
148.5
01.0
02
25.8
20.8
92
25.2
31.0
02
8.3
10.5
237.0
440.0
31.8
Y20.9
N
HD
17382
BD
+26
465
HIP
13081
GJ
113
K1
V2
48
9.1
527
47.1
18.9
0.3
44.7
11.1
5274.5
01.2
02
122.6
01.2
02
22.8
30.4
92
23.9
10.7
52
1.5
60.2
033.1
036.3
56.6
N18.7
N
HD
18803
51
Ari
HIP
14150
GJ
120.2
G8
V3
226.0
326
36
33.2
710.0
1.0
47.2
50.8
9232.8
01.0
02
167.9
01.0
02
19.1
60.8
42
22.9
60.6
32
5.9
20.4
830.4
834.5
91.4
Y19.2
N
HD
19994
94
Cet
HIP
14954
GJ
128
F8
V3
12
46.4
42
111
45.9
818.3
0.9
44.6
90.7
5194.1
00.7
02
69.9
00.7
02
19.8
50.6
32
19.5
50.3
42
6.1
30.6
828.5
333.7
82
0.7
Y25.7
N
HD
20115
BD
+00
542
HIP
15058
F8
-3
14
2.9
10
44
21.2
723.8
2.0
16.2
72.3
374.7
32.7
12
13.9
22.1
32
26.3
62.1
02
17.4
22.7
22
7.6
62.0
932.5
133.4
93.7
N25.4
Y
HD
30652
1O
riH
IP22449
GJ
178
F6
V4
49
50.4
16
57
40.6
024.6
0.9
124.6
00.9
5462.9
00.5
011.8
00.5
02
26.0
70.8
12
14.8
00.1
84.1
10.3
730.2
625.0
014.3
N22.8
Y
V1005
Ori
HIP
23200
GJ
182
M1
Ve
459
34.8
31
47
0.6
832.4
1.0
37.5
02.5
638.1
01.5
02
94.4
01.6
02
23.6
50.9
52
20.8
60.9
52
14.8
60.4
834.8
637.8
12
4.1
N35.8
Y
HD
35112
BD
+02
934
HIP
25119
G5
V5
22
37.5
02
36
11.3
535.5
0.4
50.2
41.5
269.7
01.3
02
152.1
01.3
02
25.8
70.4
02
26.1
40.4
92
12.5
30.1
938.8
555.8
10.3
Y53.5
N
HD
42499
AD
S4775A
BH
IP29241
G5
V6
956.1
52
25
37
32.6
527.6
2.0
19.8
21.3
22
28.3
01.4
038.8
01.3
02
24.0
51.3
12
12.9
21.5
92
12.1
90.7
829.9
045.7
02
2.9
Y44.3
N
HD
53143
SA
O249700
HIP
33690
GJ
260
K1
V6
59
59.6
62
61
20
10.2
421.3
2.0
54.3
30.5
42
161.1
80.5
4264.5
40.6
12
25.5
10.2
82
17.5
91.8
52
14.9
70.7
734.4
134.5
92
4.1
N22.0
Y
BD
+01
2063
HIP
40774
G5
V8
19
19.0
51
20
19.9
027.6
0.6
42.8
91.3
22
163.2
01.1
02
53.1
01.0
02
26.3
00.4
92
19.1
20.3
92
8.0
40.6
133.4
929.6
31.1
Y22.8
Y
BD
+23
1978
HIP
42253
K5
V8
36
55.7
823
14
49.1
320.1
0.3
24.0
42.9
72
108.7
01.7
02
106.7
01.7
02
24.4
21.1
42
23.9
32.2
42
11.7
02.8
336.1
436.6
02
4.1
N21.3
Y
HD
81817
HR
3751
HIP
47193
K3
IIIa
937
5.2
981
19
34.9
82
5.1
2.0
3.0
30.5
42
15.9
00.3
02
16.1
00.3
02
25.3
95.1
92
24.3
64.0
32
6.4
31.3
535.7
735.0
52
6.8
N2
4.7
Y
HD
89388
V337
Car
HIP
50371
K3
IIa
10
17
4.9
82
61
19
56.3
18.2
0.9
4.4
30.4
92
24.2
00.9
05.6
00.9
02
21.9
32.9
42
13.9
21.1
52
9.9
51.5
527.8
228.6
32
0.7
Y10.7
Y
BD
+33
1976
HIP
50660
K0
V10
20
45.9
332
23
54.3
42.7
0.6
21.0
61.3
92
153.2
01.1
02
56.7
01.1
02
26.5
11.7
32
19.5
41.3
12
16.5
91.3
736.8
837.4
51.5
Y7.3
Y
HD
91901
BD
213
3170
HIP
51931
K2
V10
36
30.7
92
13
50
35.8
218.9
0.3
31.6
31.1
62
163.6
01.2
022.2
01.1
02
24.8
40.8
62
18.7
10.3
01.4
70.4
531.1
325.3
56.9
N8.8
N
HD
93070
wC
arH
IP52468
K4
III
10
43
32.2
92
60
33
59.8
29.3
2.0
3.0
60.5
02
10.0
01.3
014.3
01.4
02
20.0
04.4
22
16.5
42.4
011.9
93.1
028.5
919.5
319.7
N6.3
Y
HD
101906
BD
+24
2386
HIP
57198
G2
V11
43
47.0
424
037.1
94.5
0.7
4.2
30.9
32
22.3
01.0
02
7.6
00.9
02
19.0
54.3
62
18.6
34.3
72
2.7
31.7
726.7
826.2
72
3.2
N1.7
Y
HD
105631
BD
+41
2276
HIP
59280
GJ
3706
K0
V12
937.2
640
15
7.4
02
3.1
2.0
41.0
70.9
82
314.0
20.5
72
51.3
40.7
62
28.2
60.8
62
22.4
30.6
12
7.5
51.9
336.8
637.4
72
1.9
Y2
7.7
Y
HD
108574
BD
+45
2038
HIP
60831
G5
V12
28
4.4
544
47
39.5
02
1.5
0.5
25.5
12.0
72
180.2
01.0
02
6.7
01.1
02
27.9
02.3
22
18.1
71.4
92
4.0
80.5
333.5
434.7
90.0
Y2
9.3
N
HD
108575
BD
+45
2038B
HIP
60832
KV
12
28
4.8
044
47
30.5
02
1.3
0.5
23.6
13.7
12
178.2
00.9
03.5
01.1
02
30.8
04.9
12
17.6
52.7
72
4.6
90.7
335.8
137.0
92.1
Y2
10.0
N
BD
+21
2462
HIP
62686
K5
-12
50
41.8
620
32
5.2
72
9.3
5.0
27.5
83.3
92
125.0
00.9
02
33.3
00.9
02
15.5
21.9
12
15.5
22.1
42
9.9
64.9
724.1
023.2
12
3.2
N2
7.4
Y
HD
111813
BD
+26
2397
HIP
62758
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V12
51
38.4
125
30
31.7
82
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0.6
26.5
41.4
52
141.9
01.3
02
37.8
01.2
02
17.6
71.0
52
19.3
41.1
62
4.9
70.6
026.6
627.3
62
4.5
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9.0
Y
HD
118100
EQ
Vir
HIP
66252
GJ
517
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13
34
43.2
02
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40.9
92
288.7
01.6
02
87.4
01.6
02
28.2
21.0
12
13.5
30.9
02
18.3
51.6
036.2
830.8
40.3
Y2
12.3
N
HD
120352
BD
200
2743
HIP
67412
K0
V13
48
58.1
92
135
34.6
42
13.5
0.4
25.0
81.3
22
136.4
00.8
02
45.2
00.8
02
21.5
80.8
72
18.8
91.2
32
9.8
60.3
730.3
330.9
32
1.5
Y2
14.9
Y
HD
121979
BD
+67
812
HIP
68076
K0
V13
56
17.7
666
56
41.0
42
15.5
0.5
22.5
20.7
32
140.9
01.0
056.8
01.1
02
25.2
81.0
12
22.1
30.5
62
11.5
90.4
135.5
434.8
32
1.8
Y2
13.9
Y
HD
125161B
GJ
9474B
K1
-14
16
13.0
051
22
30.0
02
18.7
2.0
33.5
40.5
62
147.8
06.1
084.1
04.8
02
22.2
00.8
72
15.4
91.1
92
13.9
51.7
930.4
528.1
83.0
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15.0
Y
HD
135363
RE
J1507+
76
HIP
74045
G5
V15
756.2
676
12
2.6
42
17.7
0.5
33.9
70.6
92
131.8
70.6
2169.3
20.7
92
23.0
00.6
22
20.5
40.4
02
16.1
00.3
434.7
932.3
32.8
Y2
12.5
Y
HD
140913
BD
+28
2469
HIP
77152
G0
V15
45
7.4
528
28
11.7
22
14.5
2.0
20.8
51.0
42
88.3
01.4
037.2
01.2
02
21.7
71.2
32
14.4
21.0
31.6
71.7
326.1
739.9
60.1
Y2
33.5
N
HD
142072
BD
201
3109
HIP
77749
G5
V15
52
33.7
52
154
22.8
12
24.6
0.5
24.0
70.9
92
114.8
00.9
08.7
00.9
02
29.5
00.6
02
15.7
80.6
30.0
90.7
433.4
636.1
811.8
N2
30.6
Y
HD
155875
HR
6400
HIP
84827
GJ
665
G0.5
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20
12.6
82
70
243.3
12
5.0
0.9
25.7
80.8
22
47.2
01.4
02
196.4
01.2
02
28.1
61.0
52
23.1
61.0
12
8.6
60.5
037.4
737.2
24.1
N2
4.8
Y
HD
157750
SA
O208819
HIP
85360
G2
V17
26
34.8
62
32
58
10.8
02
18.6
2.0
22.6
71.4
82
29.1
01.4
02
118.5
01.3
02
20.6
52.0
02
22.0
51.6
32
9.1
80.6
831.5
735.4
32.7
Y2
24.7
N
HD
167605
BD
+69
968
HIP
89005
K2
V18
955.5
069
40
49.7
92
8.2
2.0
32.3
00.7
22
26.6
01.2
0192.7
01.2
02
26.2
30.7
42
13.9
41.7
42
0.3
20.9
829.7
132.9
26.8
N2
17.8
N
HD
168746
BD
211
4606
HIP
90004
G5
-18
21
49.7
82
11
55
21.6
42
25.6
0.0
23.1
90.9
62
21.9
01.0
02
66.2
01.0
02
19.6
00.2
12
21.5
90.6
02
2.8
70.2
529.3
026.2
92
8.6
N2
23.7
Y
HD
175531
HIP
93096
G9
V:
18
57
56.6
82
44
58
6.8
12
13.5
2.0
15.5
12.1
826.8
01.2
02
80.1
01.4
02
20.8
02.2
02
17.6
92.8
32
10.1
62.2
329.1
329.9
62
0.5
Y2
15.2
Y
HD
191869A
SA
O246498
HIP
99803
2-
20
14
56.1
72
56
58
35.2
62
16.0
2.0
15.3
22.2
038.7
01.7
02
87.1
01.7
02
27.5
32.7
12
19.1
73.5
02
0.6
11.8
433.5
529.6
82
6.5
N2
7.3
N
HD
191869B
2-
20
14
56.1
72
56
58
35.2
62
18.0
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15.3
22.2
034.4
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02
99.4
02.1
02
29.6
12.7
52
22.4
44.0
21.6
81.7
337.1
932.0
02
9.9
N2
7.9
N
BD
+33
3936
HIP
101262
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791.3
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-20
31
32.0
733
46
33.1
22
27.1
1.0
38.1
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01.6
013.4
01.5
02
18.9
70.5
02
23.5
10.9
62
11.6
20.4
832.3
725.2
82
4.5
N2
18.6
N
HD
201651
BD
+69
1148
HIP
104225
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-21
656.3
969
40
28.5
42
13.7
2.0
30.4
50.7
2109.1
01.1
065.0
01.2
02
14.8
90.7
12
16.1
91.8
72
9.7
40.5
624.0
621.7
52
1.5
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Y
HD
203030
BD
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4507
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105232
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V21
18
58.2
226
13
49.9
52
17.3
0.4
24.4
81.0
5131.3
01.4
08.9
01.3
02
23.4
10.9
22
15.8
90.3
82
12.1
90.8
430.8
132.7
82
0.6
Y2
20.6
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HD
209779
BD
206
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109110
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V22
65.3
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29.0
22
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0.5
28.1
61.0
1160.4
00.9
02
59.3
00.9
02
20.9
30.6
82
17.7
30.5
52
12.9
90.8
230.3
531.3
62
2.1
Y2
12.6
Y
HD
210507
SA
O247351
HIP
109612
K3
-22
12
16.9
42
54
58
40.7
12
10.5
2.0
20.3
91.5
6111.4
51.3
72
65.0
21.0
22
27.1
62.0
32
16.3
51.6
12
2.2
11.7
531.7
829.9
92
1.8
Y2
1.6
N
GT
Peg
HIP
112909
GJ
875.1
M3
-22
51
53.5
431
45
15.1
42
1.8
0.5
70.3
02.7
1522.6
02.5
02
52.5
02.4
02
28.0
11.1
12
12.6
50.6
32
17.6
90.7
635.4
637.3
32
1.5
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11.9
N
HD
217352
BD
+04
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HIP
113556
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59
59.3
95
934.4
92
16.5
0.7
5.1
11.0
039.1
00.9
02
6.9
01.0
02
30.0
65.7
32
26.2
13.2
02
6.1
93.8
040.3
637.8
01.0
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8.6
N
HD
218340
SA
O255410
HIP
114236
G3
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812.3
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63
37
41.3
74.0
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17.6
11.0
8103.8
01.3
02
62.7
01.3
02
20.6
71.7
42
25.0
51.7
22
5.1
91.5
532.8
931.5
12
9.3
N3.6
Y
HD
220091
SA
O108560
HIP
115288
F0
IV23
20
57.6
217
15
9.5
42
19.0
5.0
15.1
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082.9
01.1
028.3
01.0
02
25.9
61.7
52
18.7
83.8
19.4
63.2
633.4
124.4
713.2
N2
4.4
N
BD
+00
5017
HIP
116384
GJ
900
K7
-23
35
0.2
81
36
19.5
32
10.2
1.0
51.8
01.7
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033.7
01.2
02
29.1
81.0
32
15.6
40.6
80.7
90.8
833.1
230.0
39.7
N2
2.0
N
BD
213
6464
HIP
117410
GJ
907.1
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-23
48
25.6
92
12
59
14.9
12
8.2
2.0
36.9
62.2
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02.1
017.6
02.1
02
29.1
01.8
72
13.8
91.0
50.7
31.9
332.2
529.9
78.8
N2
1.4
N
56 D. Montes et al.
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
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HD
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5938
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02
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02
15.1
70.4
82
9.1
40.3
92
6.4
20.5
818.8
421.5
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HD
12786
BD
216
365
HIP
9716
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V2
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01.2
02
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70.2
42
6.0
60.2
52
10.7
40.4
712.6
25.8
92
4.8
N4.6
N
HD
13507
BD
+39
496
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10321
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V2
12
55.0
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05.0
0.6
38.1
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956.9
01.3
02
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01.3
02
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10.4
62
7.1
00.4
82
10.4
60.3
615.0
715.0
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2.2
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HD
13531
BD
+39
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10339
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V2
13
13.3
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27.3
26.2
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39.1
00.9
157.6
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96.4
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00.4
52
6.0
40.4
62
10.3
10.3
314.9
614.4
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1.9
N5.3
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Tri
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11437
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27
29.2
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24.6
26.7
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02.2
02
71.8
02.3
02
14.3
71.2
72
15.9
31.9
32
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50.9
423.1
325.2
44.2
N12.8
N
HD
37216
BD
+52
982
HIP
26653
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V5
39
52.3
552
53
50.9
610.1
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35.9
11.1
22
10.0
01.3
02
141.4
01.4
02
16.7
80.4
52
10.0
80.5
22
8.3
20.4
021.2
719.3
62
3.1
N5.9
Y
HIP
29067
GJ
226.2
K8
V6
755.2
567
58
36.5
71.6
5.0
40.1
21.7
82
48.8
01.8
02
113.8
01.9
02
10.1
53.9
02
5.9
32.6
32
8.8
61.8
614.7
214.6
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Y
HD
41842
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O171235
HIP
28921
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V6
616.6
22
27
54
21.0
012.4
0.4
31.3
81.1
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16.4
01.5
034.4
01.4
02
11.2
80.3
52
5.8
50.3
72
5.0
50.2
613.6
712.0
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HD
47787
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O172095
HIP
31821
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V6
39
11.6
02
26
34
19.6
319.1
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20.5
62.0
72
38.0
02.6
024.6
02.4
02
16.8
00.8
82
9.2
40.8
82
10.3
00.8
621.7
620.9
83.9
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Y
HD
51825
SA
O197402
HIP
33451
GJ
255A
F8
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657
17.5
92
35
30
25.7
410.1
5.0
23.1
50.5
62
40.3
80.5
019.5
80.5
32
9.7
51.9
92
4.7
34.4
22
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01.2
513.6
516.4
60.7
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Lyn
HIP
36627
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277B
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57.3
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13
47.4
10.4
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87.1
54.8
52
251.9
03.3
02
257.1
03.1
02
6.7
41.0
02
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70.6
22
15.7
01.0
519.5
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00.4
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N
DX
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1111
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48.0
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46
42.0
09.0
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275.8
03.0
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1141.0
05.0
02
602.0
05.0
02
17.1
40.4
22
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80.1
72
13.5
30.3
423.9
323.3
62.2
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HD
77825
BD
215
2685
HIP
44526
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V9
420.6
92
15
54
51.2
73.9
0.4
35.6
31.0
32
108.9
01.2
02
28.2
01.1
02
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50.3
22
4.9
80.3
52
11.5
90.4
415.4
716.9
92
0.5
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Y
HD
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psi
Vel
HIP
46651
GJ
351A
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IV9
30
41.9
72
40
28
0.2
78.8
2.0
53.8
90.7
02
147.1
40.5
848.6
50.7
82
12.8
40.2
12
8.8
11.9
82
4.5
70.2
916.2
314.1
24.9
N6.1
Y
HD
94765
BD
+08
2434
HIP
53486
GJ
3633
K0
V10
56
30.8
07
23
18.5
05.4
0.4
56.9
81.0
32
256.8
01.3
02
77.3
01.3
02
16.6
70.3
52
14.1
90.3
22
6.9
10.4
122.9
622.3
90.5
Y2.0
Y
HIP
53767
GJ
408
M2.5
-11
04.2
622
49
58.6
83.2
0.5
150.9
51.5
92
427.0
01.5
02
280.8
01.5
02
9.2
70.2
02
12.9
70.2
02
3.7
00.4
616.3
715.5
52
4.8
N2.8
Y
HD
103720
BD
201
2594
HIP
58237
K3
V11
56
41.1
82
246
44.2
32
8.1
0.3
22.1
81.4
12
64.1
01.1
02
42.8
01.1
02
8.1
10.5
92
8.2
60.8
82
14.2
50.5
718.3
616.6
52
3.9
N2
4.6
Y
HD
119124
BD
+51
1859
HIP
66704
GJ
521.2
AF
7.7
V13
40
23.2
350
31
9.9
02
10.0
2.0
39.6
40.7
12
124.8
01.0
058.9
01.1
02
14.8
50.3
92
8.5
10.8
42
8.9
21.8
119.3
022.0
10.3
Y2
14.6
Y
BD
+24
2700
HIP
69410
K0
V14
12
41.5
623
48
51.3
62
12.2
0.4
30.6
21.1
62
41.9
01.0
02
15.3
01.0
02
6.4
60.2
52
7.7
30.3
22
9.7
50.3
914.0
211.0
02
2.5
N2
8.9
Y
HD
130819
8L
ibH
IP72603
GJ
563.4
F3
V14
50
41.1
82
15
59
50.0
52
23.0
5.0
42.2
61.0
42
135.9
30.9
42
59.4
70.6
22
24.3
33.7
12
8.6
71.3
92
11.7
83.0
928.3
921.3
57.3
N2
15.2
N
HIP
85523
GJ
674
M2.5
-17
28
39.9
52
46
53
42.6
92
10.5
1.3
220.4
31.6
3573.7
01.4
02
878.1
01.3
02
14.9
61.2
42
4.9
50.3
82
19.2
50.2
224.8
822.9
18.4
N2
9.3
Y
HD
161284
BD
+65
1203
HIP
86456
K0
V17
39
55.6
965
05.9
12
7.3
0.5
37.8
30.7
12
21.6
01.0
0109.2
01.1
02
13.2
00.3
02
8.2
50.4
32
2.3
20.2
915.7
416.5
66.8
N2
11.2
Y
HD
230017
V1436
Aql
HIP
92836
GJ
734
M0:
-18
54
54.0
018
58
60.0
02
17.0
10.0
52.0
011.0
019.0
82.9
1118.0
62.1
32
19.0
66.5
72
6.6
37.7
40.8
31.5
320.2
01.8
010.9
N2
1.5
N
HD
181321
HIP
95149
GJ
755
G5
V19
21
29.7
62
34
59
0.3
72
10.2
1.3
47.9
51.2
887.6
01.2
02
86.4
01.3
02
13.1
21.2
22
6.0
00.2
52
6.6
20.5
715.8
713.3
80.9
Y2
5.6
Y
HD
186922
BD
+76
750
HIP
96656
GJ
765.2
K0
-19
39
6.3
676
25
19.2
72
8.7
2.0
33.2
80.6
9151.0
00.9
0139.2
01.0
02
23.5
20.8
12
10.2
21.7
42
16.5
50.8
630.5
233.1
20.2
Y2
15.5
N
HD
191285
BD
214
5652
HIP
99322
GJ
781.2
K3/4
V20
936.4
72
14
17
12.8
52
12.3
5.0
31.4
91.5
879.5
01.4
02
90.6
01.4
02
12.0
54.0
32
15.2
52.2
52
10.1
32.1
821.9
219.9
92
5.4
N2
10.0
Y
HIP
108467
GJ
842.2
M0.5
-21
58
24.5
175
35
20.6
32
11.0
2.0
47.9
51.0
8231.3
02.1
024.9
02.2
02
15.0
30.8
92
13.8
91.7
82
15.2
10.6
625.5
024.5
92
0.2
Y2
8.7
Y
2R
EJ2
201+
2H
IP108706
GJ
4247
M4
-22
113.1
228
18
24.8
62
3.0
1.0
111.5
73.1
9372.1
12.7
636.4
83.3
82
13.7
00.4
32
4.4
80.9
32
7.3
30.4
616.1
715.9
44.7
N2
4.9
Y
HD
211472
BD
+53
2831
HIP
109926
GJ
4268A
K1
V22
15
54.1
454
40
22.4
02
8.6
0.5
46.6
20.6
7212.3
01.1
069.7
01.2
02
19.6
40.3
62
13.0
00.4
92
5.9
40.1
724.2
922.0
89.0
N2
7.2
Y
HD
216803
TW
PsA
HIP
113283
GJ
879
K4
V22
56
24.0
62
31
33
56.0
26.0
5.0
130.9
40.9
2334.0
01.5
02
157.1
01.3
02
6.0
82.0
62
8.2
30.5
92
10.4
94.5
214.6
513.4
22
2.5
N2.8
Y
HD
217107
BD
203
5539
HIP
113421
G8
IV22
58
15.5
42
223
43.3
82
13.6
0.5
50.7
10.7
52
5.8
00.7
02
15.1
00.8
02
1.5
80.1
22
8.5
80.2
910.5
40.4
013.6
80.0
72
1.5
N0.0
N
HK
Aqr
HIP
114252
GJ
890
M2
V23
819.5
52
15
24
35.8
13.4
1.0
45.7
52.6
0107.3
03.1
02
19.4
03.1
02
7.8
40.7
12
4.1
20.6
32
7.8
00.9
611.8
011.4
11.2
N2.0
Y
HD
218738
BD
+47
4058
HIP
114379
GJ
4315
G5
Ve
23
957.3
647
57
29.9
92
6.4
0.6
39.5
67.6
7149.7
01.5
02
4.2
01.6
02
13.5
82.9
92
11.9
41.2
82
6.0
21.4
419.0
617.5
44.8
N2
2.9
Y
HD
220476
BD
208
6103
HIP
115527
G5
V23
24
6.3
42
733
2.7
44.5
0.5
33.1
00.9
1146.2
00.9
02
5.0
00.9
02
17.2
60.5
52
6.1
20.3
62
11.1
30.4
921.4
320.6
25.6
N4.1
Y
Late-type members of young stellar kinematic groups 57
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Ta
ble
7.
Oth
ery
ou
ng
dis
cst
ars.
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
W
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)
HD
224983
BD
+10
5022
HIP
184
K0
V0
221.5
411
022.4
52
16.2
0.5
29.7
51.2
12
5.0
00.9
02
43.5
00.9
06.4
10.2
62
14.1
70.3
98.3
20.4
4
HD
691
V344
And
HIP
919
K0
V0
11
22.4
430
26
58.4
72
2.8
0.5
29.3
50.9
5210.6
01.1
035.2
01.1
02
30.7
51.0
82
15.8
40.6
20.9
60.3
1
HIP
1399
2-
017
30.4
52
59
57
4.1
92
4.5
2.0
22.5
42.3
3113.2
02.3
02
40.2
52.1
42
19.3
02.0
72
16.1
12.1
35.1
51.7
0
HD
1326
GX
And
HIP
1475
GJ
15A
M1.5
V0
18
22.8
944
122.6
212.0
1.0
280.2
61.0
52887.5
01.1
0408.9
01.1
02
49.2
30.4
62
11.9
00.8
52
3.5
40.3
2
SA
O11215
HIP
2232
G0:
-0
28
17.1
063
44
5.9
39.6
1.5
9.0
43.0
662.6
02.1
02.6
02.0
02
33.1
89.7
32
8.2
95.8
22
1.4
21.3
4
HD
4128
bet
Cet
HIP
3419
GJ
31
K0
III
043
35.3
72
17
59
11.7
812.8
0.9
34.0
40.8
2232.7
90.8
332.7
10.5
42
30.6
30.7
52
11.4
60.3
82
12.8
90.8
9
HD
4614
eta
Cas
HIP
3821
GJ
34A
G3
V0
49
6.2
957
48
54.6
710.0
0.1
167.9
90.6
21087.0
70.4
42
559.7
30.4
42
30.3
20.1
12
9.2
60.1
12
16.8
90.0
6
LP
467-1
6G
J3076
M5
-1
11
25.0
015
26
24.0
04.0
0.1
118.0
021.0
0176.0
01.0
02
123.0
01.0
02
5.6
20.6
92
5.1
01.2
82
5.7
20.5
0
Wolf
44
GJ
47
M2
-1
19
6.0
061
22
15.0
08.9
0.5
78.0
08.0
0389.0
01.0
02
835.0
01.0
02
27.9
52.3
52
10.8
31.8
92
48.1
14.9
1
YZ
Cet
HIP
5643
GJ
54.1
M4.5
-1
12
30.6
42
16
59
56.2
828.2
5.0
269.0
37.5
71209.9
25.2
1646.8
83.9
12
28.4
31.1
12
0.2
70.5
22
23.9
04.9
1
HD
9770
BB
Scl
HIP
7372
GJ
60
K3
V1
35
1.0
12
29
54
37.2
031.5
1.0
42.2
91.4
773.4
01.4
033.2
01.4
02
12.0
80.4
22
6.3
50.2
72
29.7
90.9
9
HD
14374
BD
201
316
HIP
10818
G0
V2
19
16.0
40
46
47.4
124.6
0.3
25.5
11.1
161.3
00.8
02
31.9
00.9
02
18.1
10.3
22
8.3
30.5
72
19.3
00.2
8
GJ
102
M4
-2
33
37.0
024
55
24.0
02
0.3
10.0
129.0
012.0
037.0
01.0
02
689.0
01.0
04.2
07.3
62
16.9
84.4
42
18.3
65.6
3
HD
18445
SA
O168180
HIP
13769
GJ
120.1
CK
2V
257
13.1
92
24
58
30.3
949.6
0.5
38.8
71.5
015.0
01.2
02
32.6
01.3
02
17.3
00.2
72
17.6
90.2
92
43.2
10.4
5
1E
0307.5
+14
24
310
14.2
014
35
47.0
018.6
1.0
9.0
05.0
02
5.4
02.6
02
24.5
01.7
02
9.1
53.1
92
3.8
34.2
82
20.5
55.3
9
BD
+60
637
HIP
14864
GJ
3206
K7
-3
11
56.8
561
31
12.9
32
8.3
10.0
27.1
33.4
16.2
03.1
0104.3
03.3
012.4
37.5
80.3
26.6
315.7
32.2
6
HD
20630
kap
Cet
HIP
15457
GJ
137
G5
Vvar
319
21.7
03
22
12.7
119.9
0.9
109.1
80.7
8268.8
70.7
793.5
30.6
82
22.4
10.6
62
4.2
70.0
62
5.3
20.6
2
HD
26756
SA
O93829
HIP
19781
G5
V4
14
25.6
514
37
30.1
238.5
0.4
21.9
11.2
7108.4
01.2
02
20.8
01.2
02
41.5
20.5
52
17.8
71.1
32
3.0
10.8
6
HD
26900
BD
+36
860
HIP
19930
K2
V4
16
32.6
636
30
6.6
020.8
0.3
39.0
81.1
62
22.8
01.2
02
225.6
01.3
02
21.1
50.2
92
11.5
20.5
82
24.6
80.6
7
HD
27466
BD
204
799
HIP
20218
G5
V4
19
57.0
82
426
19.5
418.0
0.5
27.8
80.9
62
58.6
01.2
02
37.0
01.2
02
7.3
30.4
82
2.7
80.2
82
20.0
30.4
9
HD
28100
73
Tau
HIP
20732
G7
IIIa
426
36.3
714
42
49.6
331.8
0.9
7.1
70.8
12
6.7
00.8
02
30.3
00.8
02
22.7
51.1
52
13.2
71.6
42
27.1
81.8
5
HIP
22627
GJ
179
M3.5
-4
52
5.7
36
28
35.5
42
9.1
0.5
82.5
23.9
9146.0
94.1
52
310.1
42.4
913.3
50.5
32
17.0
70.9
71.0
50.3
2
LH
S1723
GJ
3323
M4
-5
157.0
02
656
48.0
042.0
0.1
163.0
026.0
02
546.0
01.0
02
546.0
01.0
02
21.4
61.9
02
18.4
10.2
92
38.3
33.0
2
V371
Ori
HIP
26081
GJ
207.1
M2.5
-5
33
44.7
91
56
43.4
322.1
1.0
59.4
53.8
82
241.3
44.7
12
156.6
11.6
92
13.1
31.0
02
7.0
10.4
42
28.1
61.6
0
HD
245409
BD
+11
878
HIP
26335
GJ
208
K7-M
0V
536
30.9
911
19
40.3
122.7
5.0
87.9
01.2
92
0.7
01.2
02
57.5
01.2
02
20.6
84.7
62
7.8
81.1
92
5.9
20.9
6
HD
38529
BD
+01
1126
HIP
27253
G4
V5
46
34.9
11
10
5.5
028.9
2.0
23.5
70.9
22
79.3
00.9
02
140.6
01.0
02
12.4
61.8
52
24.6
30.9
82
33.5
81.1
8
HD
40647
BD
+69
361
HIP
28902
G5
V6
65.7
069
28
34.0
82
14.5
0.5
31.3
00.9
72
135.1
01.0
02
56.2
01.1
03.9
00.4
62
3.8
30.3
42
25.9
10.6
9
HD
42807
V1357
Ori
HIP
29525
GJ
230
G2
V6
13
12.5
010
37
37.7
16.0
1.0
55.2
00.9
677.3
01.3
02
297.3
01.2
03.0
90.9
62
26.0
30.5
82
6.6
80.2
1
HD
43162
SA
O171428
HIP
29568
GJ
3389
G5
V6
13
45.3
02
23
51
42.9
622.0
1.0
59.9
00.7
52
45.4
01.1
0113.2
01.2
02
20.6
70.6
12
10.1
00.7
42
6.9
40.3
3
G104-3
7G
J232
M4.5
624
40.0
023
26
18.0
02
12.0
0.1
112.0
07.0
0390.0
01.0
02
300.0
01.0
015.5
40.2
52
16.6
41.1
67.7
20.5
5
HD
258857
BD
+05
1273
HIP
31069
K2
V6
31
11.0
85
52
36.9
729.4
0.4
32.0
92.0
62
154.3
01.6
02
61.9
01.6
02
26.8
90.3
82
10.0
90.3
62
25.3
51.6
7
HD
46375
BD
+05
1295
HIP
31246
K1
IV6
33
12.6
35
27
46.5
31.0
5.0
29.9
31.0
7114.2
40.9
22
96.7
90.7
38.5
04.5
12
20.2
72.3
18.9
60.3
9
HD
46524
SA
O171921
HIP
31187
K0
V6
32
37.0
82
29
34
56.7
319.0
0.4
23.5
21.0
32
68.0
01.5
067.7
01.4
02
23.5
70.7
32
4.1
80.6
42
12.7
20.4
8
HD
265866
HIP
33226
GJ
251
M3
-6
54
48.9
633
16
5.4
022.0
0.1
181.3
11.8
72
727.6
02.5
02
401.8
02.4
02
26.7
20.1
12
3.6
90.0
82
15.1
10.2
3
LH
S1885
GJ
3417
M4.5
-6
57
58.0
062
19
12.0
016.0
0.1
129.0
020.0
0332.0
01.0
02
395.0
01.0
02
17.1
60.6
42
10.1
82.5
814.7
51.2
6
HD
54359
BD
209
1858
HIP
34423
GJ
267
K0
V7
89.3
12
958
7.3
425.3
0.4
34.8
41.3
72
200.6
01.2
029.3
01.2
02
29.1
70.5
42
5.6
00.5
72
22.7
70.9
1
G089-0
32
GJ
3454
M0
-7
36
25.0
07
436.0
024.0
0.1
162.0
026.0
0265.0
01.0
0351.0
01.0
02
20.6
80.1
52
5.9
71.0
116.6
81.8
0
BD
221
2221
HIP
39222
G0
III
81
21.4
82
22
19
58.5
838.3
0.3
6.5
81.2
42
10.5
01.3
021.1
01.3
02
33.3
83.0
82
24.9
41.7
64.3
71.0
8
HD
69247
BD
210
2443
HIP
40465
K5
V8
15
45.1
22
10
26
54.4
02
3.7
0.4
23.0
71.5
92
59.6
01.3
02
46.3
01.3
01.4
00.3
32
1.0
50.4
52
15.8
51.0
8
HD
69433
BD
+65
626
HIP
40918
G0
V8
21
3.7
865
26
33.7
62
1.6
0.6
27.3
30.9
812.2
01.4
022.0
01.4
03.9
20.4
92.4
70.3
60.4
00.4
0
HD
74576
SA
O199544
HIP
42808
GJ
320
K1
V8
43
18.0
32
38
52
56.5
414.3
2.0
89.7
80.5
62
301.0
10.4
2340.7
60.4
42
26.1
90.4
02
9.7
21.9
62
0.8
40.0
8
HD
75289
HR
3497
HIP
43177
G0
-8
47
40.3
92
41
44
12.4
69.3
0.0
34.5
50.5
62
19.5
00.8
02
227.7
00.8
021.1
00.4
12
12.6
90.0
62
21.5
30.4
0
BD
+12
1944
HIP
43948
GJ
330
M1
-8
57
4.6
911
38
49.0
22
12.0
0.5
60.9
93.4
52
29.2
01.4
02
324.2
01.4
015.5
50.5
52
15.7
21.2
72
17.1
70.6
7
HD
81040
BD
+20
2314
HIP
46076
G0
V9
23
47.0
920
21
52.0
448.9
0.6
30.7
11.2
42
151.9
00.7
036.3
00.7
02
49.7
70.8
72
13.3
10.3
117.8
30.7
7
BD
212
2918A
GJ
352A
M3
-9
31
22.0
02
13
29
15.6
07.3
1.3
94.9
54.3
1722.9
35.2
653.5
25.9
922.1
51.2
42
2.4
21.0
929.4
41.3
5
HD
82558
LQ
Hya
HIP
46816
GJ
355
K0
V9
32
25.5
72
11
11
4.6
77.6
0.2
54.5
20.9
92
247.5
01.1
035.5
01.1
02
20.3
60.3
52
5.4
50.1
72
9.2
80.2
8
HD
82943
BD
211
2670
HIP
47007
G0
934
50.7
42
12
746.3
58.1
0.0
36.4
20.8
42.2
01.2
02
172.7
01.3
010.1
60.3
62
19.7
80.3
32
8.7
40.3
5
BD
+28
1779
HIP
47176
G5
V9
36
50.0
027
58
22.4
12
11.5
0.4
24.2
31.3
52
170.2
01.3
02
95.8
01.2
02
13.4
11.2
52
17.8
81.1
92
33.0
61.4
6
HD
83588
BD
+58
1208
HIP
47547
K2
V9
41
36.0
657
29
46.5
822.1
0.4
31.0
21.2
72
87.5
01.4
02
43.9
01.4
02
25.2
10.5
62
1.4
70.4
28.6
40.4
5
HIP
47513
GJ
361
M1.5
-9
41
10.3
613
12
34.4
311.5
0.5
88.0
61.9
82
658.7
02.0
02
144.7
01.9
02
30.0
40.6
42
15.2
50.3
52
17.7
60.7
0
BD
+63
869
HIP
48714
GJ
373
M0
-9
56
8.6
762
47
18.4
513.3
0.5
95.4
01.2
02
303.8
01.7
02
584.0
01.8
02
23.8
60.3
82
23.8
10.4
210.5
20.3
6
HD
87000
BD
+68
587
HIP
49387
G5
V10
457.0
567
25
21.8
22.0
0.3
24.6
91.2
22
16.5
01.3
02
79.4
01.3
02
6.1
00.3
92
13.0
80.7
66.1
80.3
9
HD
87884
BD
+12
2147
GJ
9316
K2
V10
812.8
311
59
48.4
06.3
4.0
44.2
08.8
02
233.3
04.2
01.0
03.9
02
22.8
54.3
92
6.9
42.0
92
9.7
74.1
9
HD
87883
BD
+34
2089
HIP
49699
K0
V10
843.1
434
14
32.1
29.1
0.4
55.3
70.9
42
65.1
01.2
02
60.7
01.3
02
8.6
00.2
62
7.0
30.1
64.1
90.3
4
HD
88230
BD
+50
1725
HIP
49908
GJ
380
K7
-10
11
22.1
449
27
15.2
42
26.0
0.1
205.2
30.8
12
1359.8
01.0
02
505.7
01.0
02
9.1
60.1
22
20.6
20.0
72
35.9
20.1
0
BD
203
2870
HIP
49986
GJ
382
M1.5
-10
12
17.6
72
344
44.4
27.7
0.5
127.9
91.5
32
150.7
01.4
02
245.2
01.5
02
2.3
10.1
72
12.6
60.3
62
2.6
90.3
5
AD
Leo
GJ
388
M4.5
Ve
10
19
36.2
719
52
11.9
012.4
1.0
213.0
04.0
02
500.8
02.0
02
46.0
01.9
02
14.5
00.5
02
7.3
60.3
53.8
10.8
2
HD
93811
BD
+52
1514
HIP
53008
GJ
3627
G5
V10
50
40.3
151
47
58.8
22
0.6
0.5
34.7
72.6
72
195.4
01.3
07.4
01.3
02
22.4
81.7
82
6.5
70.5
42
12.7
51.0
3
DE
N1048-3
9M
9V
10
48
14.6
839
56
6.1
02
10.1
0.5
244.0
099.0
02
1147.0
08.0
02
992.0
09.0
02
9.6
15.8
62
24.7
39.9
82
16.3
13.0
5
HD
95128
47
UM
aH
IP53721
GJ
407
G1
V10
59
27.9
740
25
48.9
411.3
0.5
71.0
40.6
62
317.2
00.7
056.6
00.7
02
24.1
60.2
92
2.3
90.0
60.6
50.4
6
HD
95743
BD
208
3068
HIP
54002
K3
V11
250.1
22
919
49.2
92
10.0
0.3
32.7
31.2
32
201.7
01.3
02
61.3
01.4
02
19.8
30.8
32
7.7
10.6
32
24.0
70.7
1
HD
96612
BD
+39
2424
HIP
54426
K0
V11
814.0
138
25
35.9
02
36.1
0.5
43.9
11.0
32
214.3
01.5
041.3
01.6
02
6.4
00.6
12
3.5
70.2
22
42.4
80.5
2
HD
97584
BD
+74
456
HIP
54952
GJ
420A
K5
-11
15
11.9
073
28
30.7
38.4
1.0
68.1
31.1
82
401.7
00.9
0110.4
00.9
02
28.6
20.6
60.9
80.5
62
9.5
20.7
2
RE
J1147+
12
K5
Ve
11
46
60.0
012
00.0
02
12.1
1.0
22.0
05.0
02
9.8
02.2
02
10.2
01.9
00.3
50.5
01.5
40.8
12
12.3
80.9
8
HD
102696
BD
+01
2617
HIP
57658
2-
11
49
28.0
70
36
32.9
121.7
0.4
23.2
91.6
52
133.5
51.5
92
13.6
61.0
52
22.2
31.7
92
24.5
41.1
211.0
10.7
1
HD
108984
BD
+21
2426
HIP
61099
K0
V12
31
18.2
920
13
4.1
52
7.9
0.3
39.6
20.9
52
17.0
01.0
02
169.0
00.9
08.6
80.2
62
17.0
60.4
72
10.4
30.3
0
HD
110514
BD
+03
2681
HIP
62016
K0
V12
42
38.9
32
34
36.0
66.1
0.4
32.7
11.0
92
10.5
01.0
02
48.7
01.1
03.3
70.2
12
8.4
50.3
32.5
60.3
9
HD
110833
BD
+52
1650
HIP
62145
GJ
483
K3
V12
44
14.5
451
45
33.5
49.9
0.4
66.4
00.7
82
389.8
01.1
02
176.9
01.2
02
19.9
90.2
62
21.2
30.3
513.4
80.3
7
HD
111631
BD
+00
2989
HIP
62687
GJ
488
K7
-12
50
43.5
70
46
5.2
63.7
0.5
92.7
50.9
62
29.8
01.0
02
396.9
01.0
09.4
00.1
72
17.3
30.2
62
6.2
30.4
5
HD
113720
BD
218
3539
HIP
63905
G5
V13
546.2
22
18
49
33.0
62
13.3
0.5
21.9
81.1
32
107.6
01.3
02
11.2
01.3
02
24.0
61.0
42
7.0
00.8
82
9.6
70.4
1
LP
378-5
41
GJ
2097
M1.5
-13
70.0
020
48
60.0
02
12.0
0.1
156.0
023.0
02
69.0
01.0
02
38.0
01.0
02
2.4
20.1
62
1.4
60.3
22
11.9
10.1
0
HD
114613
SA
O204227
HIP
64408
GJ
501.2
G3.5
-13
12
3.1
92
37
48
10.8
92
15.0
0.9
48.8
30.7
92
381.3
00.9
046.5
00.9
02
39.2
20.7
12
8.7
60.7
30.7
30.4
1
G165-0
8G
J3789
M4
-13
31
46.0
029
16
34.0
08.0
0.1
126.0
022.0
02
245.0
01.0
02
114.0
01.0
02
3.7
50.8
02
7.9
81.5
69.4
70.2
9
HD
119332
BD
+57
1459
HIP
66781
K0
V13
41
13.4
056
43
37.8
32
8.1
0.5
42.1
20.7
62
16.6
01.1
071.1
01.2
02
4.9
90.2
02
0.0
70.2
82
10.4
00.4
4
HD
119607
BD
216
3736
HIP
67055
K1
V13
44
29.6
62
16
51
15.9
42
10.9
0.4
22.1
11.2
82
137.2
01.4
031.7
01.4
02
30.7
01.4
92
8.8
30.8
93.0
80.7
2
HD
122968
BD
+38
2510
HIP
68734
K0
V14
411.3
637
22
9.4
62
22.6
0.4
20.3
41.1
414.5
01.7
02
43.7
01.7
07.1
30.7
02
11.8
60.5
22
20.8
40.4
0
HIP
70975
GJ
553.1
M3.5
-14
31
1.1
62
12
17
45.9
62
40.6
10.0
89.7
63.4
72
405.2
23.4
72
400.1
64.1
22
33.7
96.6
92
17.7
42.9
92
33.1
16.9
2
58 D. Montes et al.
q 2001 RAS, MNRAS 328, 45–63
at UN
IVE
RSID
AD
CO
MPL
UT
EN
SE D
E M
AD
RID
on September 16, 2013
http://mnras.oxfordjournals.org/
Dow
nloaded from
Tab
le7.
–co
nti
nued
Nam
eS
pT
a(2
000)
d(2
000)
Vr
pma
cosd
md
UV
W
(hm
s)(o000)
(km
/s)
(mas
)(m
as/y
r)(m
as/y
r)(k
m/s
)(k
m/s
)(k
m/s
)
HD
128620
alf
Cen
AH
IP71683
GJ
559A
G2
V14
39
36.5
02
60
50
2.3
12
21.6
0.5
742.2
41.4
02
3679.2
61.5
1483.0
31.2
42
29.4
90.3
60.4
80.3
512.5
90.0
3
alf
Cen
BH
IP71681
GJ
559B
K0
V14
39
35.0
82
60
50
13.7
62
18.1
0.5
742.2
21.4
02
3601.0
826.1
0953.3
619.7
02
25.8
00.3
82
0.7
90.3
715.0
90.1
6
HD
129920
BD
+52
1825
HIP
71989
G2
V14
43
22.3
351
55
5.1
92
13.0
9.0
20.7
90.7
02
60.7
01.2
0120.1
01.3
02
29.9
91.0
62
1.7
14.8
42
14.4
37.6
0
HD
130215
BD
+28
2365
HIP
72200
K2
V14
46
3.0
727
30
44.4
52
20.8
0.4
37.9
31.1
018.4
01.0
02
40.2
01.0
02
1.7
70.2
52
7.7
70.1
92
19.9
90.3
7
HD
130307
BD
+03
2938
HIP
72312
GJ
3867
G8
V14
47
16.1
02
42
11.6
213.0
0.5
50.8
41.0
42
288.0
01.2
02
78.0
01.2
02
4.9
70.4
12
23.6
70.5
018.9
20.4
4
HIP
72896
GJ
568A
M3.5
-14
53
51.4
723
33
20.9
02
35.6
0.5
97.8
35.9
92
715.8
03.8
0106.4
03.7
02
38.3
11.5
52
28.2
61.2
52
15.1
91.1
1
HO
Lib
HIP
74995
GJ
581
M3
-15
19
26.8
22
743
20.2
12
9.5
0.5
159.5
22.2
72
1224.5
53.0
72
99.5
11.7
22
25.0
60.4
72
25.6
30.4
111.7
60.4
3
HD
139837
BD
+28
2454
HIP
76674
G5
V15
39
25.2
027
37
34.7
32
21.5
0.5
20.6
51.3
02
52.5
01.1
053.3
01.1
02
24.3
81.0
12
9.2
70.3
22
8.7
80.6
9
HD
144087
BD
211
4057
HIP
78738
GJ
9541A
G8
V16
425.9
22
11
26
57.7
92
32.0
0.5
35.2
52.5
62
61.2
01.4
02
22.8
01.4
02
29.9
90.4
72
7.6
50.6
02
11.9
60.4
1
HD
144088
BD
211
4058
HIP
78739
GJ
9541B
K2
V16
426.7
22
11
26
59.5
62
32.5
0.5
30.8
96.8
62
57.2
01.9
02
19.4
01.7
02
30.6
60.7
02
7.9
41.8
02
11.7
90.9
9
HD
145675
14
Her
HIP
79248
K0
V16
10
24.3
143
49
3.5
42
13.9
0.0
55.1
10.5
9132.6
01.0
02
297.0
01.1
023.7
40.3
22
12.3
40.0
92
16.1
40.1
0
HD
149661
V2133
Oph
HIP
81300
GJ
631
K2
V16
36
21.4
52
219
28.5
02
13.1
0.1
102.2
70.8
5455.0
00.7
02
308.1
00.7
00.7
20.1
32
0.4
50.0
52
28.6
30.2
0
HD
150748
BD
+49
2535
HIP
81633
KV
16
40
35.0
949
959.2
32
12.2
0.4
31.3
40.7
72.0
01.3
02
16.3
01.4
00.1
90.2
42
9.4
40.3
22
8.1
10.3
0
HD
153557
BD
+47
2415
HIP
83020
GJ
649.1
AK
0V
16
57
53.1
747
22
0.0
32
6.7
0.6
55.7
11.2
12
153.9
01.2
0267.8
01.4
02
25.6
90.5
62
6.2
60.4
66.0
30.4
5
BD
+05
3409
HIP
85665
GJ
678.1
AM
0-
17
30
22.7
35
32
54.6
62
3.2
1.3
100.1
71.3
028.4
01.6
02
250.2
01.5
04.1
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767B
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187458
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HIP
101844
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102401
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103441
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213.0
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02
34.2
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62
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6
HD
200676
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O246873
HIP
104256
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112.9
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22
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8
HD
203136
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105208
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105885
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02
53.5
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HD
209154
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216
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HIP
108732
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108752
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32
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4
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215555
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112415
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022.3
01.2
02
44.0
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32
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HD
223154
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4685
HIP
117294
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11
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81.0
62
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02
46.6
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32
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1
HD
223460
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And
HIP
117503
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02
48.7
01.5
011.0
21.4
82
8.9
21.3
22
27.7
62.8
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parameter he called Peculiar Velocity (PV ) that is defined as Vtan
but takes into account only the proper motion component
perpendicular to the C.P. (t ):
PV ¼ 4:74tp21:
The criterion compares this peculiar velocity with another
parameter he called total velocity (VT) obtained as a real VTotal
but takes into account only the proper motion component in the
direction of the C.P. (y ):
VT ¼ 4:74yp21sin21l:
The criterion considers a star as a possible member of an MG when
its peculiar velocity (PV ) is less than about 10 per cent of its total
velocity (VT):
PV , 0:1VT:
Taking into account the definition of PV and VT, this condition can
also be written in terms of components t and y as
t/y , 0:1sin21l:
This criterion takes into account the information provided by the
proper motion of the star but not the radial velocity.
(2) RADIAL VELOCITY CRITERION
For the moving cluster method we can obtain a predicted radial
velocity (called rc by Eggen) as:
rc ¼ VT cos l:
The criterion is based in the comparison of this predicted radial
velocity with the observed radial velocity of the star. Eggen
considered a star as a possible member of an MG when these two
velocities differ by less than 4–8 km s21, depending on the quality
of the observed radial velocity.
We have applied both criteria (PV and rc) to our candidate stars
(for the five MGs), in addition to the information provided by the
Galactic velocity components (U, V, W; see previous section), in
order to apply more strict requirements for SC membership and to
better discern their membership to the different MGs. For the
peculiar velocity criterion we have used the 10 per cent of VT for all
the MGs except for the Local Association, where we have used 20
per cent of VT to take into account the large dispersion observed in
this MG. For the radial velocity criterion we have taken into
account the uncertainties of the adopted radial velocity of each star.
In Tables 2 to 6 we list the total velocity (VTotal) and the parameters
needed to apply the criteria (PV, VT, and rc). The results of applying
the PV and rc criteria are indicated in the column beside each
parameter with the labels ‘Y’ (if possible member) and ‘N’ (if the
star does not satisfy that criterion). Errors in VT, PV and rc are
taking into account inside criteria. In the (U, V ) and (W, V )
diagrams (Fig. 2) we have plotted with filled symbols the stars that
satisfied both criteria.
5 D I S C U S S I O N A N D C O N C L U S I O N S
Making use of a great quantity of data from the literature (previous
general kinematic studies of moving groups, many works on late-
type stars, new results from X-ray surveys, etc.), the accurate
astrometric data recently released by the Hipparcos and Tycho-2
catalogues, and additional data obtained for our own spectroscopic
observations, we were able to identify a considerable population of
single late-type stars (for binaries see Paper II) that are members of
young ð20–600 MyrÞ stellar kinematic groups. We have used as
membership criteria the position of the stars in velocity space (U, V,
W ), Eggen’s kinematic criteria of deviation of the space motion of
the star from the convergent point, and comparison between the
observed and calculated radial velocities. Additional criteria using
age-dating methods for late-type stars (Li I l6708-A absorption
line, location on the colour–magnitude diagram, and level of
chromospheric and coronal activity) will be applied in the more
detailed study of each SKG we have undertaken, and will be
addressed in forthcoming papers.
In this paper we give the list of possible members of groups (see
Tables 2 to 7); for each star we list the stellar parameters we have
compiled, as well as the computed galactic space motions and the
results of applying the kinematic criteria. These data are also
available in tabular format and in searchable catalogue format in
the web page http://www.ucm.es/info/Astrof/skg.html that we
maintain about stellar kinematic groups.
For our extensive initial sample of single late-type stars we have
found a total of 535 stars that can be considered, for their position
in the velocity space (U, V, W ) as young disc stars. We have
Figure 3. Spacial position (RA, Dec.) for the possible stars members of the Hyades MG. The convergent point of the MG at RA ¼ 6:4h, Dec: ¼ 68: 5 is marked
with a circle. The dotted lines represent great circles defined by the proper motions and position of each star.
60 D. Montes et al.
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classified 120 stars as possible members of the Local Association,
118 of the Hyades supercluster, 84 of the Ursa Major moving
group, 53 of the IC 2391 supercluster, 34 of the Castor moving
group, and 126 as other young disc stars (classification is not clear
but it is inside or near the boundaries that determine the young disc
population in the velocity space).
When we take into account the Eggen’s kinematic criteria, in the
four MGs where the convergent point is available, the number of
possible members in each MG is reduced. Eliminating only the
stars that do not satisfy one of the two criteria (peculiar velocity
and radial velocity), we found 104 possible members of the Local
Association, 96 of the Hyades supercluster, 69 of the Ursa Major
MG, 43 of the IC 2391 supercluster, and 29 of the Castor MG.
Considering only the stars that satisfied the peculiar velocity
criterion we found 77 in the Local Association, 67 in the Hyades
supercluster, 37 in the Ursa Major MG, 28 in the IC 2391
supercluster, and 10 of the Castor MG. Finally, imposing both
criteria the number of possible members is reduced to 45 in the
Local Association, 38 in the Hyades supercluster, 28 in the Ursa
Major MG, 15 in the IC 2391 supercluster, and eight in the Castor
MG.
Analysing these results with the help of the great circles defined
by the proper motions (see Fig. 3), we can see that almost all stars
which do not satisfied the PV criterion move clearly away from the
convergent point of the MG, especially those which do not satisfy
radial velocity criteria either. In the velocity space (U, V, W ) the
stars which satisfied both criteria tend to have a lower dispersion
with respect to the expected (U, V, W ) position of the MG (see Fig.
2), but there are some cases where this is not true. The latter are
normally stars with large errors in U, Vand W (due to large errors in
radial velocity or in parallax).
Our results confirm the membership of several previously
established members of SKGs, but in other cases the new
calculated Galactic space motions indicate the membership to a
different SKG or that the star should be considered only as a young
disc star with no clear membership to any SKG (e.g., LQ Hya). In
some cases, the new calculations even located the star outside the
boundaries of the young disc population in the Boettlinger
diagram.
For the late-type stars with planetary companions included in
our sample we have found that some stars known to be young [GJ
3021 (Naef et al. 2000), i Hor (Kurster et al. 2000), t Boo (Henry
et al. 2000), 55 Cnc (Fuhrmann et al. 1998) and HD 108147
(Mayor et al. 2000)] could be possible members of the Hyades
supercluster. Some of these have been also identified by Suchkov &
Schultz (2001) as stars with planetary systems with ages similar to
the Hyades.
The groups of nearby late-type stars with different ages we have
identified in this work will be very useful for chromospheric
activity studies. High-resolution optical spectroscopic observations
of these stars will provide a simultaneous analysis of the different
optical chromospheric activity indicators, as well as yielding
rotation speed, binarity, variability and kinematics. With all this
information it will be possible to study in detail the chromosphere,
discriminating between the different structures: plages, promi-
nences, flares and microflares (see Montes et al. 2000b; 2001b,d),
and to analyse the flux–flux and rotation–activity relationships
and their age evolution.
A further study of the list of stars compiled here, as well as
detailed analysis of the origin of these young SKG and their
relation with nearby young open clusters, OB associations, T
associations and other recently identified associations of young
stars, could lead to a better understanding of the star formation
history in the solar neighbourhood.
Another important use of the list of late-type stars we give
here is that the youngest ones (the possible members of the
Local Association) can be taken as search targets for direct
imaging detection of substellar companions (brown dwarfs and
extrasolar giant planets). These young and nearby cool dwarfs
favour the optimization of the dynamical range, and the
substellar companions can be detected directly because they are
considerably more luminous when undergoing the initial phases
of gravitational contraction than at later stages. Until now only
five brown dwarfs have been detected directly (and confirmed by
both spectroscopy and proper motion) as companions to nearby
stars: the T dwarf Gl 229 B (Nakajima et al. 1995), the young L
dwarf G 196-3 B (Rebolo et al. 1998), the T dwarf Gl 570 D
(Burgasser et al. 2000), the M9 dwarf CoD 2 338 7795 B
(Neuhauser et al. 2000b) which is a member of the TW Hya
association, and the M8 dwarf HR 7329 B (Guenther et al. 2001)
which is a member of the Tucanae association. The B component
of the Ursa Major group member Gl 569 seems to be a triple brown
dwarf system (Martın et al. 2000; Kenworthy et al. 2001). In
addition, Neuhauser et al. (2000a) have shown that direct imaging
detection of extrasolar giant planets is already possible with current
technology.
Radial velocity is an important parameter in the determination of
the space-velocity components, and in some cases only poor-
quality measurements are available in the literature, resulting in
large errors in U, V and W. Good-quality spectroscopic
observations are needed to confirm the membership of these stars
to a SKG. We have already started a programme of high-resolution
echelle spectroscopic observations (using 2-m class telescopes) of
these candidate stars in order to obtain a better determination of
their radial velocity, as well as other stellar parameters. We will
use these new data to better establish the membership of these
stars (for preliminary results see Montes 2001b and Montes et al.
2001b,d).
However, a considerable number of stars in our initial sample are
too faint, and no radial velocities or accurate astrometric
parameters are available in the literature. High-resolution spectro-
scopic observations using 4- or 8-m class telescopes will be needed
to obtain the spectroscopic parameters of these stars. Accurate
astrometric parameters for a huge number of stars will be available,
in the future, with the space-astrometry missions DIVA (Double
Interferometer for Visual Astrometry) and FAME (Full-sky
Astrometric Mapping Explorer). The space mission GAIA (Global
Astrometric Interferometer for Astrophysics) will reach a much
larger distance (magnitude limit 20), and will provide both
astrometric data and radial velocities.
AC K N OW L E D G M E N T S
This research has made use the of the SIMBAD data base, operated
at CDS, Strasbourg, France, and the ARI Database for Nearby
Stars, Astronomisches Rechen-Institut, Heidelberg. We thank Dr
D. Barrado y Navascues for providing us with some additional
candidates to our initial sample of late-type stars. We also thank the
anonymous referee for suggesting several improvements and
helpful comments. This work was supported by the Universidad
Complutense de Madrid and the Spanish Direccion General de
Ensenanza Superior e Investigacion Cientıfica (DGESIC) under
grant PB97-0259.
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