2001
DOI: 10.1086/337968
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The β Pictoris Moving Group

Abstract: Following the 1983 IRAS detection and subsequent imaging of its extensive dusty circumstellar disk, b Pictoris became the prototypical and most studied example of a potential forming planetary system. Here we report the identification of 17 star systems, each with one or more characteristics indicative of extreme youth, that are moving through space together with b Pic. This diverse set of ∼12 million yr old star systems, which includes a ∼35 Jupiter mass brown dwarf, and a wide assortment of dusty circumstell… Show more

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Cited by 423 publications
(502 citation statements)
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“…However, there are significant uncertainties within these determinations (as shown in Table 1), which are derived using a convergence method represented by third degree polynomials of (V − I) C . There is an abundance of papers on the age determination of young associations, including the well-known β-Pic: 12 +8 −4 Myr (Zuckerman et al 2001), 20 ± 10 Myr (Barrado y Navascués et al 1999), TW Hydrae: 10 +10 −7 Myr (Barrado Y Navascués 2006). This is often a controversial subject; however, the relative ages between the associations are less affected and, therefore, are more robust quantities.…”
Section: Multiplicity Fraction As a Function Of Agementioning
confidence: 99%
“…However, there are significant uncertainties within these determinations (as shown in Table 1), which are derived using a convergence method represented by third degree polynomials of (V − I) C . There is an abundance of papers on the age determination of young associations, including the well-known β-Pic: 12 +8 −4 Myr (Zuckerman et al 2001), 20 ± 10 Myr (Barrado y Navascués et al 1999), TW Hydrae: 10 +10 −7 Myr (Barrado Y Navascués 2006). This is often a controversial subject; however, the relative ages between the associations are less affected and, therefore, are more robust quantities.…”
Section: Multiplicity Fraction As a Function Of Agementioning
confidence: 99%
“…The young sample was constructed by selecting K-to mid-M-type young stars in the solar neighborhood, mainly from known members of young moving groups, such as βPictoris (24±3 Myr; Zuckerman et al 2001;Bell et al 2015a), ABDoradus ( -+ 149 19 51 Myr; Zuckerman et al 2004;Bell et al 2015a), and the Octans-Near association (≈30-100 Myr; Zuckerman et al 2013), with Two Micron All Sky Survey (2MASS) K S -band magnitudes brighter than 7.1 (the brightest target, εEridani, has K S =1.8) so that an S/N of ∼80 could be achieved within approximately an hour. The young age of all stars in this sample is strongly constrained by kinematic membership in these young associations, typically in addition to lithium abundance measurements or comparison to isochrones (e.g., Torres et al 2008), except for the starεEridani, which is not a member of any known young moving group.…”
Section: The Young Samplementioning
confidence: 99%
“…initial conditions intermediate between cold and hot-start cases. But these predictions relied 1) on a system age of 12 +8 −4 Myr (Zuckerman et al 2001) and 2) on the hypothesis of a non-eccentric orbit for the planet. Since then, Binks & Jeffries (2014) reported a lithium depletion age of 21 ± 4 Myr for the β Pictoris moving group.…”
Section: Introductionmentioning
confidence: 99%