Identification of a Nearby Stellar Association in theHipparcos Catalog: Implications for Recent, Local Star Formation

By B. Zuckerman, R. A. Webb. 2000

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The TW Hydrae Association (~55 pc from Earth) is the nearest known region of recent star formation. Based primarily on the Hipparcos catalog, we have identified a group of nine or 10 comoving star systems at a common distance (~45 pc) from Earth that appear to comprise another, somewhat older association ("the Tucanae Association"). Together with ages and motions recently determined for some nearby field stars, the existence of the Tucanae and TW Hydrae Associations suggests that the Sun is now close to a region that was the site of substantial star formation only 10-50 Myr ago. The TW Hydrae Association represents a final chapter in the local star formation history.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

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• GEMS: Galaxy Evolution from Morphologies and SEDs (2004, background): “Recently, the COMBO-17 project (Wolf et al. 2001; Wolf et al. 2003a, W03) has af- forded a thirty-fold increase by number over the earlier redshift surveys [See also Fried et al. 2001; Im et al. 2002; Le Fevre et al. 2003; Davis et al. 2002 for other recent or ongoing surveys] .”
• Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…al. (2005) (COMBO-17, red circles, and DEEP2, black squares), Madgwick et al. (2003) (2dF, orange diamonds), Bell et al. (2003) (SDSS, blue×’s), and Im et al. (2002) (DEEP1, green stars) are shown, with 1σ errors, and at high redshifts (lower panels), observations from Giallongo et al. (2005)…”
• A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun (2010, unknown): “…Montes et al. 2001; Zuckerman et al. 2001; De Medeiros et al. 2000; Gaidos et al. 2000; Strassmeier et al. 2000; Teixeira et al. 2000; Torres et al. 2000; Zuckerman & Webb 2000; Webb et al. 1999; Gaidos 1998; Neuhäuser & Brandner 1998; Soderblom et al. 1998; Favata et al. 1997; Micela et al.…”
• The K20 survey. V. The evolution of the near-IR Luminosity Function (2003, result): “The overall density of early type galaxies atz' 0.5 is consistent with the local estimate (Kochanek et al. 2001), while at z ' 1, their number density shows at most a small decrease (<30%), consistent with recent results from Im et al. (2002).”
• Young Stars Near the Sun (2004, unknown): “Because the Tucana Association was discovered without any knowledge of its X-ray properties, Zuckerman & Webb (2000) showed that kinematics and optical spectroscopy, together, could be used to find substantial groups of coeval stars in the solar neighborhood.”
• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, unknown): “Based on this fact, Zuckerman & Webb (2000) searched the Hipparcos catalog for stars with similar space motions and within a 6 degree radius of 24 stars detected at 60 μm with IRAS.”
• The Structure and Dynamics of Luminous and Dark Matter in the Early-Type Lens Galaxy of 0047–281 at z = 0.485 (2002, background): “…galaxies changed little in the past 8 Gyr (from z 1)—as indicated, for example, by the modest evolution in their number density (Schade et al. 1999; Im et al. 2002; Cohen 2002; McCarthy et al. 2001) and by the little evolution in the scatter of the FP (T02)—with most of the evolution being driven…”
• The COMBO-17 survey: Evolution of the galaxy luminosity function from 25,000 galaxies with 0.2 < z < 1.2 (2002, background): “But samples sizes well in excess of a few thousand objects are only becoming available now or in the near future, e.g. with the 17-colour survey COMBO-17 presented here and with the large spectroscopic campaigns DEEP (Koo 2001; Im et al. 2002) and VIRMOS (LeFevre 2001).”
• The β Pictoris Moving Group (2001, unknown): “Other known kinematically related associations of nearby young stars include Tucana/Horologium at 45 pc (Zuckerman & Webb 2000; Torres et al. 2000; Stelzer & Neuha¨ ser 2000; Zuckerman, Song, & Webb 2001), TW Hydrae at 60 pc (Kastner et al. 1997; Webb et al. 1999), andh Chamaeleontis at 97 pc…”
• The Team Keck Treasury Redshift Survey of the GOODS-North Field (2004, methodology): “This effect has also been noted in the DEEP1 survey (Im et al. 2002; Weiner et al. 2004) in the Groth Survey Strip (which also used HST photometry), as well as in the Sloan Digital Sky Survey (Strateva et al. 2001; Hogg et al. 2002) and COMBO-17 survey (Bell et al. 2003).”
• Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, background): “Im et al. applied a very stringent cut to define their sample, targeting only morphologically normal, spheroid-dominated E/S0s having red colors that are consistent with passively fading stellar populations.”
• THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “INTRODUCTION With the advent of large galaxy surveys, the color bimodality of the galaxy population has become wellcharacterized (Lin et al. 1999; Strateva et al. 2001; Im et al. 2002; Blanton et al. 2003; Kauffmann et al. 2003; Bell et al. 2004b).”
• BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, unknown): “The closest and youngest moving groups include the TW Hydrae association (TWA; 5–15 Myr; de la Reza et al. 1989; Kastner et al. 1997; Zuckerman & Song 2004; Weinberger et al. 2013), β Pictoris (βPMG; 20–26 Myr; Zuckerman et al. 2001a; Malo et al. 2014b; Binks & Jeffries 2014), Tucana-Horologium (THA”
• The TW Hydrae Association: Discovery of T Tauri Star Members Near HR 4796 (2001, unknown): “During the past few years it has become clear that the southern hemisphere contains a multitude of young nearby stars that are kinematically related (Zuckerman & Webb 2000; Mamajek, Lawson, & Feigelson 2000; Torres et al. 2000; R. A. Webb et al. 2001b, in preparation).”
• BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS (2012, unknown): “Luhman et al. (2005) compared the same diagram for ABDMG and the open cluster IC 2391 (30-50Myr) to deduce an age between 75 and 150 Myr.”