Search for associations containing young stars (SACY). I. Sample and searching method

By C. Torres, G. Quast, L. da Silva, R. Reza, C. Melo, M. Sterzik. 2006

492 citations recorded by the source corpus.

We report results from a high-resolution optical spectroscopic survey aimed to search for nearby young associations and young stars among optical counterparts of ROSAT All-Sky Survey X-ray sources in the Southern Hemisphere. We selected 1953 late-type ($B-V~\geq~0.6$), potentially young, optical counterparts out of a total of 9574 1RXS sources for follow-up observations. At least one high-resolution spectrum was obtained for each of 1511 targets. This paper is the first in a series presenting the results of the SACY survey. Here we describe our sample and our observations. We describe a convergence method in the ( UVW ) velocity space to find associations. As an example, we discuss the validity of this method in the framework of the β  Pic Association.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/844a88f64ab45d575f828fecfb2ed6bc5ea583d5

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In Astronomy and Astrophysics

1. Michael C. Liu
2. B. Bowler
3. Eric Mamajek
4. T. Dupuy
5. K. Allers
6. A. Kraus
7. A. Mann
8. E. Gaidos

Citations in the corpus

• IDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 PC. I. SPECTROSCOPIC OBSERVATIONS (2009, methodology): “1) sets a limit on their ages of 20–30 Myr, consistent with their known membership of the AB Dor (López-Santiago et al. 2006) and β Pic (Torres et al. 2006) YMGs, respectively.”
• SPECTROSCOPIC ORBITS FOR 15 LATE-TYPE STARS (2016, background): “Torres et al. (2006) give vsini values of 8 and 9 km s−1 for HD 212698 and HD 212697, respectively.”
• AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “Follow-up observations of X-ray bright M dwarfs has been successful in identifying scores of low-mass members to young moving groups (Gaidos 1998; Zuckerman et al. 2001; Montes et al. 2001; Torres et al. 2006).”
• The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au (2019, unknown): “…5 2.14 20150703 59.6×1 40.8 19.1 Note. a System mass. References(1) Houk & Swift (1999), (2) Gaia Collaboration et al. (2018), (3) This study (SED fitting), (4) Torres et al. (2006), (5) Bell et al. (2015), (6) Nielsen et al. (2016), (7) Zuckerman et al. (2006), (8) Keenan & McNeil (1989), (9)…”
• The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc (2015, unknown): “– a Gray et al. (2006); b Browning et al. (2010); c Torres et al. (2006); d Poveda et al. (2009); e Koen et al. (2010); f Houk & Cowley (1975) c© 2015 RAS, MNRAS 000, 1–34”
• 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).”
• A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, background): “The SACY search of Tuc-Hor (Torres et al. 2006, 2008) found 17 members with spectral types of K3-M0, of which we recovered 15 as candidates.”
• On the age of the β Pictoris moving group (2014, methodology): “Our new isochronal age estimate is also in line with other recent estimates based on Li depletion (21± 9 Myr; Mentuch et al. 2008) and more recent kinematic estimates (Torres et al. 2006; Makarov 2007).”
• A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, background): “…Lawson, & Feigelson (1999), Luhman & Steeghs (2004), Lyo et al. (2004), Zuckerman & Song (2004), Mamajek (2005), López-Santiago et al. (2006), Torres et al. (2006), Mamajek (2007), Lépine & Simon (2009), Schlieder, Lépine, & Simon (2010), Kiss et al. (2011), Rodriguez et al. (2011),…”
• HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, unknown): “…1: de la Reza et al. (1989), 2: Brandeker et al. (2003), 3: Zuckerman & Song (2004), 4: Sterzik et al. (1999), 5: Gregorio-Hetem et al. (1992), 6: Torres et al. (2006), 7: Webb et al. (1999), 8: Shkolnik et al. (2011), 9: Song et al. (2003), 10: Reid (2003), 11: Jayawardhana et al. (2006), 12:…”
• A CATALOG OF ROTATION AND ACTIVITY IN EARLY-M STARS (2012, methodology): “Virtually all active early-M stars are members of young associations, several examples can be found in Torres et al. (2006).”
• XHIP: An extended hipparcos compilation (2011, background): “Our “B”-grade sources, in order of preference are: Lopez-Santiago et al., 2010; Massarotti et al., 2008; Guillout et al., 2009; Soubiran et al., 2003; Holmberg et al., 2007; Gizis et al., 2002; White et al., 2007; Torres et al., 2006; Kharchenko et al., 2007.”
• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, background): “Over 60 members of the β Pic moving group have been identified to date (Song et al. 2003; Zuckerman & Song 2004; Torres et al. 2006, 2008; Fernández et al. 2008; da Silva et al. 2009; Lépine & Simon 2009; Rice et al. 2010; Schlieder et al. 2010; Kiss et al. 2011; Schlieder et al. (A color version…”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, methodology): “…the literature membership lists were cross-matched with various catalogs that provide radial velocities (Upgren & Harlow 1996; Hawley et al. 1997; Torres et al. 2006; Bobylev et al. 2006; Kharchenko et al. 2007; White et al. 2007; Fernández et al. 2008; Shkolnik et al. 2011; Chubak et al. 2012;…”
• The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, methodology): “2MASS J16100321-5026121 is a Li-rich K0III (Torres et al. 2006) which lies well above the 1 Myr isochrone (log(Teff)=3.70±0.01, log(L/L )=1.16±0.08), calculated using the kinematic parallax of πkin = 4.19±0.38 mas, so we consider a UCL interloper.”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “TWA 9A exhibits very high Li (EW(Li 6708Å)=470mÅ; Torres et al. 2006), lies in the direction of other TWA members, has proper motion consistent with membership in TWA, and, adopting the kinematic distance of 70.0±3.8 pc, has a space motion and isochronal age consistent with membership in TWA.”