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BANYAN. XII. NEW MEMBERS of NEARBY YOUNG ASSOCIATIONS from GAIA–TYCHO DATA Jonathan Gagne´,1, 2 Olivier Roy-Loubier,3 Jacqueline K

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BANYAN. XII. NEW MEMBERS of NEARBY YOUNG ASSOCIATIONS from GAIA–TYCHO DATA Jonathan Gagne´,1, 2 Olivier Roy-Loubier,3 Jacqueline K Draft version April 10, 2018 Typeset using LATEX twocolumn style in AASTeX62 BANYAN. XII. NEW MEMBERS OF NEARBY YOUNG ASSOCIATIONS FROM GAIA{TYCHO DATA Jonathan Gagne´,1, 2 Olivier Roy-Loubier,3 Jacqueline K. Faherty,4 Rene´ Doyon,3 and Lison Malo5 1Carnegie Institution of Washington DTM, 5241 Broad Branch Road NW, Washington, DC 20015, USA 2NASA Sagan Fellow 3Institute for Research on Exoplanets, Universit´ede Montr´eal,D´epartement de Physique, C.P. 6128 Succ. Centre-ville, Montr´eal,QC H3C 3J7, Canada 4Department of Astrophysics, American Museum of Natural History, Central Park West at 79th St., New York, NY 10024, USA 5Observatoire du Mont-M´eganticand Institute for Research on Exoplanets, Universit´ede Montr´eal,D´epartement de Physique, C.P. 6128 Succ. Centre-ville, Montr´eal,QC H3C 3J7, Canada Submitted to ApJ ABSTRACT We present a search for stellar members of young associations within 150 pc of the Sun based on TGAS and an updated version of the BANYAN Σ software to determine Bayesian membership prob- abilities that includes Gaia{2MASS color-magnitude diagrams. We identify 32 new F0{M3-type bona fide members of the 10{200 Myr-old Sco-Cen, Carina, Tucana-Horologium, Columba and Octans as- sociations and the AB Doradus, β Pictoris and Carina-Near moving groups. These new bona fide members have measurements of their full kinematics and literature data consistent with a young age. We also confirm the membership of 66 previously known candidate members using their Gaia{Tycho trigonometric distances or new literature radial velocities, and identify 219 additional new candidate members, most of which do not yet have a radial velocity measurement. This work is the first step towards a completeness-corrected survey of young association members based on Gaia{DR2 in the near future. Keywords: methods: data analysis | stars: kinematics and dynamics | proper motions 1. INTRODUCTION kinematics, consisting of the XYZ Galactic coordinates Young associations and moving groups in the Solar and UVW space velocities. These require measuring the neighborhood are valuable laboratories to study the trigonometric parallax and heliocentric radial velocities properties of age-calibrated stars in detail (Zuckerman of stars, which is challenging to perform on all stars in & Song 2004; Torres et al. 2008). Their proximity a large area of the sky. makes it possible to gather high-quality data more easily, Until recently, the discovery and kinematic character- perform high-angular resolution imaging of exoplanets ization of most young associations and moving groups and bring this characterization to the lowest-mass and in the Solar neighborhood relied on parallaxes obtained faintest substellar objects with a calibrated age (e.g., see by the Hipparcos mission (Perryman et al. 1997), allow- ing us to discover only the most massive and brightest arXiv:1804.03093v1 [astro-ph.SR] 9 Apr 2018 Marois et al. 2008; Liu et al. 2013; Delorme et al. 2013; Naud et al. 2014; Macintosh et al. 2015; Gagn´eet al. members of these young associations, in general within 2015b; Faherty et al. 2016; Gagn´eet al. 2017b). How- ∼ 100 pc. The stars bright enough to have a Hipparcos ever, the main difficulty in studying such associations parallax measurement only represent ∼ 10% of the total is also a consequence of their proximity: their members stellar population within 30 pc, and 2% within 100 pc are distributed over large areas of the sky (e.g., see Fig- (Perryman et al. 1997; Pecaut & Mamajek 2013), which ure 1 of Gagn´eet al. 2018a), making it difficult to iden- is a consequence of the initial mass function peaking at tify members without measuring their full 6-dimensional mass of ∼ 0.25 M (Bochanski et al. 2010) correspond- ing to the M spectral class. Recent studies focused on various statistical methods to obtain the full kinemat- [email protected] ics of only the most likely members of these associa- 2 Gagne´ et al. tions, based on their sky position, proper motion and photometry, as well as radial velocities and parallaxes Table 1. Young associations included in this study. when available (e.g., see Mamajek 2005; Rodriguez et al. a b c d 2011; Malo et al. 2013, 2014; Kraus et al. 2014; Gagn´e Group h$i hνi Sspa Skin Age Ref. et al. 2014; Murphy & Lawson 2015; Gagn´eet al. 2015a; Name (pc) (km s−1) (pc) (km s−1) (Myr) Riedel et al. 2017; Shkolnik et al. 2017), and have started 118TAU 100 ± 10 14 ± 2 3.4 2.1 ∼ 10 1 to uncover and confirm the kinematics of a fraction of +20 +10 +51 ABDMG 30−10 10−20 19.0 1.4 149−19 2 their low-mass stars and substellar objects. The Gaia +20 βPMG 30−10 10 ± 10 14.8 1.4 24 ± 3 2 mission (Gaia Collaboration et al. 2016b) has already +11 CAR 60 ± 20 20 ± 2 11.8 0.8 45−7 2 started to benefit this field of research with the Data +7 CARN 30 ± 20 15−10 14.0 2.1 ∼ 200 3 Release 1 (Gaia{DR1; Gaia Collaboration et al. 2016a), +4 +98 CBER 85−5 −0:1 ± 0:8 3.6 0.5 562−84 4 which provided 2 million parallaxes for the Tycho cat- +3 +6 COL 50 ± 20 21−8 15.8 0.9 42−4 2 1 alog (Høg et al. 2000) . This will be even more true CRA 139 ± 4 −1 ± 1 1.5 1.7 4{5 5 +4:6 of Gaia{DR2, which will provide a billion parallaxes EPSC 102 ± 4 14 ± 3 2.8 1.8 3:7−1:4 6 that will allow to complete the population of all young ETAC 95 ± 1 20 ± 3 0.6 2.0 11 ± 3 2 HYA 42 ± 7 39+3 4.5 1.2 750 ± 100 7 associations within 150 pc down to ∼ 0.12 M (Smart −4 et al. 2017). This completion of the stellar population of IC2391 149 ± 6 15 ± 3 2.2 1.4 50 ± 5 8 IC2602 146 ± 5 17 ± 3 1.8 1.1 46+6 9 young associations in the Solar neighborhood will have −5 LCC 110 ± 10 14 ± 5 11.6 2.2 15 ± 3 10 many direct applications, such as comparing their ini- +30 +8 OCT 130−20 8−9 22.4 1.3 35 ± 5 11 tial mass functions (e.g., see Chabrier 2005; Luhman PL8 130 ± 10 22 ± 2 5.0 1.1 ∼ 60 12 2007; Bochanski et al. 2011; Jeffries 2012; Gagn´eet al. PLE 134 ± 9 6 ± 2 4.1 1.4 112 ± 5 13 2017a), providing strategic targets for the direct imag- ROPH 131 ± 1 −6:3 ± 0:2 0.7 1.6 < 2 14 ing of exoplanets, understanding the stellar formation TAU 120 ± 10 16 ± 3 10.7 3.6 1{2 15 THA 46+8 9+5 9.1 0.8 45 ± 4 2 history of the Solar neighborhood, and will provide im- −6 −6 THOR 96 ± 2 19 ± 3 3.9 2.1 22+4 2 portant benchmark populations to characterize the fun- −3 damental properties and chemical abundances of coeval TWA 60 ± 10 10 ± 3 6.6 1.5 10 ± 3 2 UCL 130 ± 20 5 ± 5 17.4 2.5 16 ± 2 10 stars (e.g., see King et al. 2000; Schuler et al. 2006). UCRA 147 ± 7 −1 ± 3 4.5 1.8 ∼ 10 16 The latest membership classification tool, BANYAN Σ +0:8 UMA 25:4−0:7 −12 ± 3 1.2 1.3 414 ± 23 17 (Gagn´eet al. 2018a), benefitted from Gaia{DR1 data to USCO 130 ± 20 −5 ± 4 9.9 2.8 10 ± 3 10 refine its kinematic models of the 27 well-characterized XFOR 100 ± 6 19 ± 2 2.6 1.3 ∼ 500 18 young associations within 150 pc of the Sun. The ages a Peak of distance distribution and ±1σ range. of these associations are in the range ∼ 1{850 Myr, and b their general characteristics are listed in Table1, which Peak of radial velocity distribution and ±1σ range. is a summarized version of Table 1 from Gagn´eet al. c Characteristic spatial scale in XYZ space. (2018a). The BANYAN Σ tool uses Bayesian inference d Characteristic kinematic scale in UVW space. to determine the membership probability that a star Note|The full names of young associations are: 118 Tau (118TAU), AB Do- belongs to any of these 27 associations, based on its sky radus (ABDMG), β Pictoris (βPMG), Carina (CAR), Carina-Near (CARN), Coma position, proper motion, and optionally its radial veloc- Berenices (CBER), Columba (COL), Corona Australis (CRA), Chamaeleontis (EPSC), η Chamaeleontis (ETAC), the Hyades cluster (HYA), Lower Centaurus ity and distance. When radial velocity and/or distance Crux (LCC), Octans (OCT), Platais 8 (PL8), the Pleiades cluster (PLE), ρ Ophiuci are not known, these observables are marginalized and a (ROPH), the Tucana-Horologium association (THA), 32 Orionis (THOR), TW Hya (TWA), Upper Centaurus Lupus (UCL), Upper CrA (UCRA), the core of the membership probability is still calculated. BANYAN Σ Ursa Major cluster (UMA), Upper Scorpius (USCO), Taurus (TAU) and χ1 For includes more associations and generates less contami- (XFOR). nants at a fixed recovery rate compared to all previous References|(1) Mamajek 2016; (2) Bell et al. 2015; (3) Zuckerman et al. 2006; tools available in the literature (e.g., Malo et al. 2014; (4) Silaj & Landstreet 2014; (5) Gennaro et al. 2012; (6) Murphy et al. 2013; (7) Brandt & Huang 2015; (8) Barrado y Navascu´eset al. 2004; (9) Dobbie et al. Gagn´eet al. 2014; Riedel et al.
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