Online Material

Appendix A: Tables

Results produced in the framework of this project are published in electronic format only. Table 1 is also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/vol/pg

Table 1 contains the following information: HIP number (Col. 1), HD number (Col. 2), right ascension and declination (ICRSJ2000) (Cols. 3 and 4), parallax and its uncertainty (Col. 5), proper motions in right ascension and declination with their uncertainties (Cols. 6 and 7), observing run identifier (Col. 8), radial velocity used in this work and its uncertainty (Col. 9), and radial velocities reported in KH07, NO04, NI02, and VF05 works (Cols. 10 to 13) with their uncertainties, if available. Column 14 contains important notes: spectroscopic binaries radial velocities standards, and stars in chromospherically active binary systems are identified in this column.

Tables 9 to 13 contain the properties of the potential candidates to MG members for the different MGs studied in this work. These tables give: HIP number (Col. 1), (B-V) colour (Col. 2), spatial-velocity components (U,V,W) with their uncertainties (Cols. 3-5), , , PV and as defined by Eggen (Cols. 6-9), measured Li  I EW (Col. 10), value and derived age (columns 11 and 12), and derived age (Cols. 13 and 14), rotational period and derived age (Cols. 15 and 16) and metallicity (Col. 17). For each Eggen's criteria, PV and (Cols. 8 and 9), there is label indicating if the star satisfies the criteria (label ``Y'') or not (label ``N'').

Tables 14 to 15 are similar to the previous ones, but they show the properties of the stars classified as Other young disc stars and stars not selected as possible MG members, respectively.

References in Tables 9 to 15 are indicated in parenthesis: (1) Martínez-Arnáiz et al. (2010) (2) Baliunas et al. (1996); (3) Duncan et al. (1991) calculated using equations in Noyes et al. (1984); (4) Gray et al. (2003); (5) Gray et al. (2006); (6) Hall et al. (2007); (7) Henry et al. (1996); (8) Jenkins et al. (2006); (9) Saffe et al. (2005); (10) Wright et al. (2004); (11) estimated form ROSAT-data using equation A1 in Mamajek & Hillenbrand (2008); (12) Noyes et al. (1984); (13) Saar & Osten (1997); (14) Messina et al. (2001).

Appendix B: Further applications of MGs members

Lists of nearby MGs members constitute promising targets for a wide variety of further investigations. We briefly summarized some of them:

First, we investigated whether there is a connection between the so-called ``solar-analogues'' (e.g. Porto de Mello & da Silva 1997; Ramírez et al. 2009; Meléndez et al. 2009) and MGs members. Taking as a reference the list of analogues published by Gaidos et al. (2000), we have found 25 matchesbetween their list and our sample, where 22 out of these 25 stars, have been classified as bona fide MG members. Another three stars, HIP 29525, HIP 80337, and HIP 116613, also candidates for MGs, satisfy Gaidos' criteria for being considered as solar analogues. These stars are listed in Table B.1. These ``young-suns'' are essential to study the history and formation of our own Solar System, indeed three of them, namely HIP 15457, HIP 42438, and HIP 64394, are included in the ambitious project The Sun in Time aimed at reconstructing the spectral irradiance evolution of the Sun (e.g Ribas et al. 2005).

As we have shown in Sect. 5.3.1, debris discs are linked to stars in MGs. It is therefore natural to check if there is a similar relation between stars with known planets and MGs. Nineteen stars of our sample have detected planets, and seven of them are MGs candidates: HIP 21482 (Hyades MG, but it is doubtful member and in addition the planet is not confirmed); HIP 43587 (Hyades MG, but it is a doubtful member), HIP 71395 (Ursa Major MG, probable member); HIP 80337 (Ursa Major, doubtful member); HIP 95319 (IC 2391 MG, but doubtful member and the planet is not confirmed); HIP 49669 and HIP 53721 (young disc stars according to their kinematics, but their calcium ages suggest that they are old stars).

Other applications are related to activity studies, i.e., flux-flux and rotation-activity-age relationships (e.g Martínez-Arnáiz et al. 2010), or search programmes to detect stellar and substellar companions (e.g Hormuth et al. 2007). Finally, we point out that an important fraction of the stars analysed in this paper will be observed in the framework of the DUNES (DUst around NEarby Stars) programme, an approved Herschel Open Time Key Project with the aim of detecting cool faint dusty discs, at flux levels as low as the Solar EKB (Maldonado et al. 2010; Eiroa et al. 2010).

Table B.1:   Solar analogues and their ascription to MGs. Label ``Y'' indicates probable members, ``?'' doubtful members, and ``N'' probable non-members, respectively.

Table 1:   Positions, proper motions and radial velocities for the observed stars.

Table 5:   Stars with known debris discs.

Table 6:   Comparison between our final membership for the Local Association and previous studies.

Table 7:   Comparison between our final memberships for the Hyades MG and those given by López-Santiago et al. (2010).

Table 8:   Comparison between our final memberships for the Ursa Major MG and those previously reported in the literature.

Table 9:   Membership criteria for the Local Association candidate stars. (Convergence Point: 5.98 h, -35.15 degrees; U =-11.6 km s^-1, V = -21.0 km s^-, W = -11.4 km s^-1; Age: 20-150 Myr).

Table 10:   Membership criteria for the Hyades candidate stars. (Convergence Point: 6.40 h, 6.50 degrees; U =-39.7 km s^-1, V = -17.7 km s^-1, W = -2.4 km s^-1; Age: 600 Myr).

Table 11:   Membership criteria for the Ursa Major MG candidate stars. (Convergence Point: 20.55 h, -38.10 degrees; U =14.9 km s^-1, V = 1.0 km s^-1, W = -10.7 km s^-1; Age: 300 Myr).

Table 12:   Membership criteria for the IC 2391 MG candidate stars. (Convergence Point: 5.82 h, -12.44 degrees; U =-20.6 km s^-1, V = -15.7 km s^-1, W = -9.1 km s^-1; Age: 35-55 Myr).

Table 13:   Membership criteria for the Castor MG candidate stars. (Convergence Point: 4.57 h, -18.44 degrees; U =-10.7 km s^-1, V = -8.0 km s^-1, W = -9.7 km s^-1; Age: 200 Myr).

Table 14:   Properties of the stars classified as Other young discs stars.

Table 15:   Properties of the stars non-members of moving groups.