Late-type stars members of young stellar kinematic groups - I. Single stars

By D. Montes, J. López-Santiago, M. Gálvez, M. J. Fernández-Figueroa, E. Castro, M. Astrofisica, Ucm, U. Madrid. 2001

330 citations recorded by the source corpus.

This is the first paper of a series aimed at studying the properties of late-type stars members of young stellar kinematic groups. We concentrate our study on classical young moving groups as: Local Association (Pleiades moving group, 20 - 150 Myr), IC 2391 supercluster (35 Myr), Ursa Major group (Sirius supercluster, 300 Myr), and Hyades supercluster (600 Myr); as well as on recently identified groups as: Castor moving group (200 Myr). In this paper we have compiled a preliminary list of single late-type stars possible members of some of these young stellar kinematic groups. Stars have been selected from previously established members of stellar kinematic groups based on photometric and kinematic properties as well as from candidates based on other criteria as their level of chromospheric activity, rotation rate, lithium abundance. Precise measurements of proper motions and parallaxes taken from Hipparcos Catalogue, as well as from Tycho-2 Catalogue, and published radial velocity measurements are used to calculate the Galactic space motions (U, V, W) and to apply the 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 sub-stellar companions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0d10f05a3e89f0dbd4a23379222395542da07cad

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In Astronomy and Astrophysics

1. Jon Fortney
2. Michael C. Liu
3. B. Bowler
4. D. Charbonneau
5. M. Marley
6. N. Madhusudhan
7. T. Dupuy
8. Eric Mamajek

In Instrumentation

1. Jon Fortney
2. Michael C. Liu
3. D. Charbonneau
4. T. Dupuy
5. M. Marley
6. A. Showman
7. N. Madhusudhan
8. E. Gaidos

Citations in the corpus

• Habitable planets around the star Gliese 581 (2007, methodology): “We have compiled a sample of K- and M-type stars with ages determined in a similar way to the solar analogs in the “Sun in Time” sample (Ribas et al. 2005), i.e., membership in clusters and moving groups (Montes et al. 2001), rotation period, membership in wide binaries, and isochrones.”
• THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “Several field L dwarfs from Seifahrt et al. (2010) were included in our sample, as they were re- ported to be candidate members of older (&100 Myr) moving groups, namely the Hyades, Pleaides, Ursa Major streams (e.g. Montes et al. 2001; Zuckerman & Song 2004).”
• HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, neutral): “…11: Jayawardhana et al. (2006), 12: Zuckerman et al. (2001), 13: Looper et al. (2010), 14: Shkolnik et al. (2012), 15: Kraus et al. (2014), 16: Montes et al. (2001), 17: Zuckerman et al. (2004), 18: Malo et al. (2013), 19: López-Santiago et al. (2006), 20: Bowler et al. (2012), 21:…”
• AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “Follow-up observations of X-ray bright M dwarfs has been successful in identifying scores of low-mass members to young moving groups (Gaidos 1998; Zuckerman et al. 2001; Montes et al. 2001; Torres et al. 2006).”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “…2007; (3) Maldonado et al. 2010; (4) Shkolnik et al. 2012; (5) Monet et al. 2003; (6) Zuckerman et al. 2011; (7) Gaia Collaboration et al. 2016a; (8) Montes et al. 2001; (9) Zickgraf et al. 2005; (10) Shkolnik et al. 2017; (11) Lépine & Simon 2009; (12) Desidera et al. 2015; (13) Egret et al.…”
• XHIP: An extended hipparcos compilation (2011, background): “Our preferred “C”-grade sources are: Montes et al., 2001; Garcia-Sanchez, 2001; Turon et al., 1993; Barbier-Brossat et al., 1994.”
• Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group (2003, methodology): “Only a third of our probable (and possible, as well) activity-based members are classified by us as final members; the results are the same (for both probable and possible activity-based members) utilizing the final membership assessments of Montes et al. (2001) as well.”
• CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS (2015, background): “Its relatively bright primary at about 9 arcsec is a young K2 V star with strong ultraviolet and X-ray emission and lithium in absorption (Pounds et al. 1993; Jeffries 1995; Montes et al. 2001; Zuckerman & Song 2004; Xing & Xing 2012).”
• The Nearest Young Moving Groups (2006, methodology): “To the initial sample of Zuckerman et al. (2004), we have added 13 stars (marked with b in Table 1) from our catalogue of Late-type Stars Possible Members of Young Stellar Kinematic Groups (Montes et al. 2001).”
• GU Bootis: A New 0.6 M☉ Detached Eclipsing Binary (2005, background): “…nor in the area covered by young population tracers (Skuljan et al. 1999); (2) the space velocities do not match those of any known moving group (Montes et al. 2001); and (3) the modulus value of theW velocity component (perpendicular to the Galactic plane) is significantly larger than expected…”
• New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets (2006, methodology): “If the star was inferred to be young due to kinematic properties (Montes et al. 2001), we adopted that age.”
• Angular Differential Imaging: A Powerful High-Contrast Imaging Technique (2005, methodology): “Mass limits corresponding to these observations, corrected for the filter use,5 are estimated using evolutionary models from Baraffe et al. (2003), assuming ages of 350, 45, and 85 Myr for Vega, HD 18803, and HD 97334B, respectively (Song et al. 2001; Montes et al. 2001).”
• Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data: Revisiting the concept of superclusters (2004, background): “The kinematic properties of all these moving groups and superclusters are listed by Montes et al. (2001) and Chereul et al. (1999).”
• ON THE ANGULAR MOMENTUM EVOLUTION OF FULLY CONVECTIVE STARS: ROTATION PERIODS FOR FIELD M-DWARFS FROM THE MEarth TRANSIT SURVEY (2010, background): “1 a See Leggett (1992). b (1) Montes et al. (2001); (2) Delfosse et al. (1998); (3) Mohanty & Basri (2003); (4) Browning et al. (2010) our sample (Mohanty & Basri 2003 state a spectral type of M8.”
• The N2K Consortium. IV. New Temperatures and Metallicities for More than 100,000 FGK Dwarfs (2005, background): “…for [Fe/H] gradients with Galactic radius (Nordstrom et al. 2004), searching for common proper motion groups with uniform abundances (e.g., Montes et al. 2001; López-Santiago et al. 2001), and sifting between star formation scenarios to best reproduce the distribution of these ‘‘moving…”
• FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, neutral): “…et al. (2001), (76) Burgasser et al. (2010c), (77) Rebolo (1998), (78) Leggett et al. (2000), (79) Gizis (2002), (80) Burgasser et al. (1999), (81)Montes et al. (2001), (82) Luhman (2013), (83) Boffin et al. (2013), (84) Giclas et al. (1959), (85) Delfosse et al. (1997), (86) Scholz et al.…”