THE TUCANA/HOROLOGIUM, COLUMBA, AB DORADUS, AND ARGUS ASSOCIATIONS: NEW MEMBERS AND DUSTY DEBRIS DISKS

By B. Zuckerman, J. H. Rhee, Inseok Song, M. Bessell. 2011

187 citations recorded by the source corpus.

We propose 35 star systems within ∼70 pc of Earth as newly identified members of nearby young stellar kinematic groups; these identifications include the first A- and late-B-type members of the AB Doradus moving group and field Argus Association. All but one of the 35 systems contain a bright solar- or earlier-type star that should make an excellent target for the next generation of adaptive optics (AO) imaging systems on large telescopes. AO imaging has revealed four massive planets in orbit around the λ Boo star HR 8799. Initially, the planets were of uncertain mass due in large part to the uncertain age of the star. We find that HR 8799 is a likely member of the ∼30 Myr old Columba Association, implying planet masses ∼6 times that of Jupiter. We consider Spitzer Space Telescope MIPS photometry of stars in the ∼30 Myr old Tucana/Horologium and Columba Associations, the ∼40 Myr old field Argus Association, and the ∼70 Myr old AB Doradus moving group. The percentage of stars in these young stellar groups that display excess emission above the stellar photosphere at 24 and 70 μm wavelengths—indicative of the presence of a dusty debris disk—is compared with corresponding percentages for members of 11 open clusters and stellar associations with ages between 8 and 750 Myr, thus elucidating the decay of debris disks with time.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/02086c4f14a1bbb6163e593a4086955106f10edf

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In Astronomy and Astrophysics

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Citations in the corpus

• CLOUDS AND CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HR8799b (2011, background): “HR8799 is, at present, a rare find among exoplanets with its four potentially massive planets (∼ 5 – 10 MJup) orbiting a ∼ 30 Myr A5 star (Zuckerman et al. 2011), and is the first and, so far, only multi-planet system to be directly imaged.”
• ORBITAL MOTION OF HR 8799 b, c, d USING HUBBLE SPACE TELESCOPE DATA FROM 1998: CONSTRAINTS ON INCLINATION, ECCENTRICITY, AND STABILITY (2011, background): “With an age estimate between 30 and 60 MYr (Marois et al. 2010b; Zuckerman et al. 2011), the HR 8799 planets are relatively bright and at relatively large angular separations (∼ 0.4 to ∼1.7 arcsec) which makes them excellent targets for direct imaging.”
• SPECTRAL AND PHOTOMETRIC DIAGNOSTICS OF GIANT PLANET FORMATION SCENARIOS (2011, background): “Furthermore, Zuckerman et al. (2011) find that HR8799’s probable association with a nearby group suggests an age of ∼30 Myr.”
• A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, background): “Most programs have only identified a small number of candidates (Kiss et al. 2011) or have concentrated on higher-mass membership (Zuckerman & Song 2004; Torres et al. 2006, 2008; Zuckerman et al. 2011).”
• The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “The nearest samples of young stars to the Sun (d < 100 pc) are found in small moving groups and associations (Zuckerman et al. 2011, Zuckerman & Song 2004).”
• OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS (2015, background): “The stars are young and belong to the TucanaHorlogium moving group (Zuckerman et al. 2011).”
• The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, unknown): “Age estimates from: 1 - this work (CMD), 2 - Zuckerman et al. (2011), 3 - Tetzlaff et al. (2010), 4 - Rhee et al. (2007), 5 - Su et al. (2006), 6 - Rieke et al. (2005), 7 - Perryman et al. (1998), 8 - Barrado yNavascués (1998), 9 - Song et al. (2001), 10 - Westin (1985),11 - Gerbaldi et al.…”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “…References References—(1) Malo et al. 2013; (2) van Leeuwen 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)…”
• A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, background): “HR 6351 and V857 Ara (HD 155915) are given as TucHor members by Zuckerman et al. (2011), and although exhibiting signs of youth (e.g. circumstellar material and Li absorption), the analysis of Malo et al. (2013) suggests that both are field objects.”
• Imaging Extrasolar Giant Planets (2016, background): “HR 8799 and possibly κ And are thought to be members of Columba (Zuckerman et al. 2011).”
• BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS (2012, background): “Zuckerman et al. (2011) proposed 8 new members to THA with spectral types between A1V and G8V.”
• MASSES, RADII, AND CLOUD PROPERTIES OF THE HR 8799 PLANETS (2012, background): “Most recently Zuckerman et al. (2011) concluded that the Galactic space motion of HR 8799 is very similar to that of the 30 Myr old Columba association and suggest that it is a member of that group.”
• BANYAN. II. VERY LOW MASS AND SUBSTELLAR CANDIDATE MEMBERS TO NEARBY, YOUNG KINEMATIC GROUPS WITH PREVIOUSLY KNOWN SIGNS OF YOUTH (2013, unknown): “…et al. 2001a), Tucana-Horologium (THA; 20 - 40 Myr; Torres et al. 2000, Zuckerman 2001), Carina (CAR; 20 - 40 Myr; Torres et al. 2008), Columba (COL; 20 - 40 Myr; Zuckerman et al. 2011), Argus (ARG; 30 - 50 Myr; Zuckerman et al. 2011) and AB Doradus (ABDMG; 70 - 120 Myr ; Zuckerman et al. 2004).”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, background): “C. J. Corbally, R. O. Gray, & R. F. Garrison, 3 Garrison, R. F., & Gray, R. O. 1994, AJ, 107, 1556 Garrison, R. F., Hiltner, W. A., & Schild, R. E. 1977, ApJS, 35, 111 Garrison, R. F., & Schild, R. E. 1979, AJ, 84, 1020 Gáspár, A., Rieke, G. H., Su, K. Y. L., Balog, Z., Trilling, D., Muzzerole, J.”
• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, background): “Over 60 stars have been identified to date in the Tucana-Horologium association (Song et al. 2003; Zuckerman & Song 2004; Torres et al. 2008; Fernández et al. 2008; da Silva et al. 2009; Kiss et al. 2011; Zuckerman et al. 2011), with a mean distance of 48 ± 7 pc (Torres et al. 2008).”