Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group

By J. King, Adam R. Villarreal, D. Soderblom, A. F. Gulliver, S. Adelman. 2003

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In Astronomy and Astrophysics

Citations in the corpus

Properties of planets in binary systems - The role of binary separation (2006, background): “HD 147513 HD 147413 was classified as a member of the Ursa Major moving group by Soderblom & Mayor (1983) while King et al. (2003) classified the membership as unprobable, on the basis of the discrepant kinematic parameters.”
Decay of Planetary Debris Disks (2005, background): “…1997; (21) Barrado y Navascués et al. 1999; (22) Bonatto et al. 2004; (23) U Sco, de Zeeuw et al. 1999; (24) IC 2602, Randich et al. 2001; (25) King et al. 2003; (26) Iliev & Barzova 1995; (27) Barrado y Navaqués et al. 1997. region, and (2) much of the dust in these systems is generated…”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, unknown): “Nearly all likely members of the Hyades (Perryman et al. 1998), Ursa Majoris (King et al. 2003), and TW Hydrae (Reid 2003) young nearby moving groups have proper motions that exceed 40 mas yr−1 and thus would not be selected against using the current selection method.”
Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics (2008, methodology): “An extensive study of the age, membership, and activity of the Ursa Major cluster was undertaken by King et al. (2003), and we include their “Y” or “Y?” candidate members in our census for that cluster.”
Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, background): “A comparison of the Li measurements for HN Peg A (Chen et al. 2001) to Li data for solar-type members of the Pleiades and Hyades open clusters and the Ursa Major moving group (Soderblom et al. 1990, 1993a,b) indicates that HN Peg A is probably older than the Pleiades (τ = 100- 125 Myr, Meynet et al.”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “The core membership lists of King et al. (2003) was adopted for this work, and the stream was not included in BANYAN Σ because of its heterogeneous nature.”
DISCOVERY OF A FAINT COMPANION TO ALCOR USING MMT/AO 5 μm IMAGING (2009, methodology): “…(2000), energy conversion factor from Fleming et al. (1995), and the adopted parallax, (10) combining Teff and log(L/L⊙) values with z=0.02 evolutionary tracks of Lejeune & Schaerer (2001), (11) UMa cluster age from King et al. (2003), (12) Galactic Cartesian velocity vector, calculated in §3.4.1.”
The Nearest Young Moving Groups (2006, background): “…by galactic differential rotation since they are not gravitationally bounded enough, taking into account that their nucleus consist of only a few stars as in the case of the Ursa Major MG (see King et al. 2003, for a recent review) or the recently discovered AB Doradus MG (Zuckerman et al. 2004).”
THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “King et al. (2003) and Jones et al. (2015) estimate ages for the Ursa Major core members of 500 ± 100 Myr and 414 ± 23 Myr, respectively, consistent with the spectroscopic gravity.”
PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “Shkolnik et al. (2009) assign an age range of 40–300 Myr for the primary from its high X-ray emission and lack of spectroscopic indicators of youth, while Shkolnik et al. (2012) tentatively assign it to the Ursa Major moving group (∼500 ± 100 Myr; King et al. 2003) from its kinematics.”
A NEAR-INFRARED SPECTROSCOPIC STUDY OF YOUNG FIELD ULTRACOOL DWARFS (2013, background): “– 18 – 2M 0314+16 and 2M 1705-05 are candidate members of the ∼500 Myr old (King et al. 2003) Ursa Majoris moving group (Seifahrt et al. 2010) and neither show signatures of low gravity.”
The CORALIE survey for southern extra-solar planets. XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE (2003, methodology): “Although some doubts (but no rejection) were cast on the membership (King et al. 2003), it is worth noticing that the activity level, activity-derived age and metallicity (Table 1) correspond well to the Ursa Major group.”
The Sun in Time: Activity and Environment (2007, background): “…period has been inferred from periodic X-ray modulation to be about 1 d (Güdel et al., 1995a, 1998a; Telleschi et al., 2005). π1 UMa = HD 72905 and χ1 Ori = HD 39587: These are two members of the Ursa Major stream (King et al., 2003), with an estimated age of 300Myr (Soderblom and Mayor, 1993).”