The β Pictoris Moving Group

By B. Zuckerman, Inseok Song, M. Bessell, R. Webb. 2001

358 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d97b0ef486267f183b5191e0fa40f4844875beed

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Citations in the corpus

• THE EXTREMELY RED, YOUNG L DWARF PSO J318.5338−22.8603: A FREE-FLOATING PLANETARY-MASS ANALOG TO DIRECTLY IMAGED YOUNG GAS-GIANT PLANETS (2013, methodology): “5−22, using an age of 12+8 −4 Myr (distributed uniformly) from Zuckerman et al. (2001), we find a mass of 6.5+1.3 −1.0 MJup, temperature of 1160 +30 −40 K, and log(g) of 3.86 +0.10 −0.08 dex (Figure 4).”
• The Nearest Young Moving Groups (2006, background): “In 2001, the β Pic MG (Zuckerman et al. 2001) — a group of stars with an age of ∼ 12 Myr (Zuckerman et al. 2001; Ortega et al. 2004) at a mean distance of ∼ 35 pc comoving with the well-known young star β Pic — was confirmed to be the closest kinematic group up to date.”
• WIDE COMPANIONS TO HIPPARCOS STARS WITHIN 67 pc OF THE SUN (2012, background): “At larger scales of∼1 pc we also encounter co-moving remnants of nearby clusters and associations (e.g. Zuckerman et al. 2001, 2004).”
• A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, background): “M dwarfs that are X-ray bright are often young, and this has been used to identify members of nearby young moving groups (e.g., Gaidos 1998; Zuckerman et al. 2001; Torres et al. 2006), and other young stars in the Solar Neighborhood (Riaz, Gizis, & Harvin 2005).”
• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, background): “Zuckerman et al. (2001a) cemented the existence of the β Pic moving group with the confirmation of 18 additional members on the basis of their Galactic space motions.”
• The Brown Dwarf Desert at 75-1200 AU (2004, methodology): “Recent discovery of young near clusters, (e.g., Webb et al. 1999; Zuckerman & Webb 2000; Zuckerman et al. 2001b) has confirmed this criterion to be a valuable tool for identifying young stars.”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, methodology): “…TW Hya (TWA; de La Reza et al. 1989; Kastner et al. 1997), β Pictoris (βPMG; Zuckerman et al. 2001a), Tucana-Horologium (THA; Torres et al. 2000; Zuckerman et al. 2001b), Carina (CAR; Torres et al. 2008), Columba (COL; Torres et al. 2008), Argus (ARG; Makarov & Urban 2000) and AB Doradus…”
• Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, background): “The presence of small sub-µm-sized grains inferred from our fit to the HR 7012 spectrum suggest that this system may have experienced a recent collision. η Tel is a binary member of the β Pic moving group with an estimated age of 12 Myr – 29 – (Zuckerman et al. 2001).”
• The AB Doradus Moving Group (2004, methodology): “…Sun using the double-beam grating and echelle spectrographs on the two Nasmyth foci of the Australian National University’s 2.3 m telescope (see, e.g., Zuckerman et al. 2001 for a few early results) and the Hamilton echelle spectrograph at the coude´ focus of the 3 m telescope at Lick Observatory.”
• THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “We note that this object lies beyond the ≈50-pc limiting distance of the original Zuckerman et al. (2001) search that identified the β Pic moving group, and it is also farther than 42 out of the 48 members identified by Torres et al. (2008).”
• New Members of the TW Hydrae Association, β Pictoris Moving Group, and Tucana/Horologium Association (2003, methodology): “…(TWA;Kastner et al. 1997; de la Reza et al. 1989;Webb et al. 1999; Zuckerman et al. 2001c), Pic moving group (Barrado y Navascués et al. 1999; Zuckerman et al. 2001a), and Tucana/Horologium association (Tucana/HorA; Zuckerman & Webb 2000; Torres et al. 2000; Zuckerman, Song, & Webb 2001b)…”
• A companion to AB Pic at the planet/brown dwarf boundary (2005, background): “…on the TucanaHorologium (Torres et al. 2000, Zuckerman & Webb 2000) and TW Hydrae (Kastner et al. 1997) associations, as well as theβ Pictoris (Zuckerman et al. 2001) and AB Doradus (Zuckerman et al. 2004) co-moving groups, to explore the circumstellarnvironment within semimajor axes between…”
• Imaging Extrasolar Giant Planets (2016, background): “Many of these host stars are members of young moving groups. β Pic, 51 Eri, and possibly TYC 9486-927-1 are members of the β Pic moving group (Zuckerman et al. 2001; Feigelson et al. 2006; Deacon et al. 2016).”
• A lithium depletion boundary age of 21 Myr for the Beta Pictoris moving group (2013, methodology): “The LDB age we find is at the upper end of age estimates from isochronal fits to low mass BPMG members in the HRD – 12+8 −4 Myr (Zuckerman et al. 2001).”