Young Nearby Loose Associations

By C. Torres, G. Quast, C. Melo, M. Sterzik. 2008

144 citations recorded by the source corpus.

A significant population of stars with ages younger than the Pleiades exists in the solar neighborhood. They are grouped in loose young associations, sharing similar kinematical and physical properties, but, due to their vicinity to the Sun, they are dispersed in the sky, and hard to identify. Their strong stellar coronal activity, causing enhanced X-ray emission, allows them to be identified as counterparts of X-ray sources. The analysis presented here is based mainly on the SACY project, aimed to survey in a systematic way counterparts of ROSAT all-sky X-ray sources in the Southern Hemisphere for which proper motions are known. We give the definition, main properties, and lists of high-probability members of nine confirmed loose young associations that do not belong directly to the well-known Oph-Sco-Cen complex. The youth and vicinity of many members of these new associations make them ideal targets for follow-up studies, specifically geared towards the understanding of planetary system formation. Searches for very low-mass and brown dwarf companions are ongoing, and it will be promising to search for planetary companions with next generation instruments.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ce9c2240773728cb88a6cf4487e68361e661e926

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In Astronomy and Astrophysics

1. B. Bowler
2. Michael C. Liu
3. Eric Mamajek
4. M. Pecaut
5. C. Bell
6. E. Shkolnik
7. Motohide Tamura
8. U. Exeter

In Instrumentation

1. B. Bowler
2. Eric Mamajek
3. Michael C. Liu
4. C. Bell
5. E. Shkolnik
6. M. Pecaut
7. Motohide Tamura
8. U. Exeter

Citations in the corpus

• A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “…looking also at the distribution of distances (from the nearest to the farthest) in these two membership lists, those stars in our list cover a range of ' 65 pc, whereas those in Torres et al. (2008) cover a range of more than twice this at ' 150 pc (cf. ' 50 pc for the supposedly coeval Tuc-Hor).”
• The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, background): “The nearest of these samples are small, diffuse, nearby associations of kinematically related stars, (e.g., the β Pictoris moving group, TW Hya Association; Zuckerman & Song 2004; Torres et al. 2008).”
• PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, methodology): “I color of 1.2 mag from UCAC4, the Li depletion implies an age consistent with the Pleiades (Torres et al. 2008).”
• HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, background): “Each star has been shown to be kinematically linked (using three-dimensional space velocities) to one of these YMGs (e.g., Zuckerman & Song 2004; Torres et al. 2008; Shkolnik et al. 2011, 2012; Kraus et al. 2014), and also exhibits independent youth indicators such as elevated stellar activity…”
• On the age of the β Pictoris moving group (2014, background): “This sample is more restrictive than the larger sample assembled by Torres et al. (2006) and Torres et al. (2008), however these larger samples contain very few stars with trigonometric parallaxes, and many at larger distances (which increases the chances of interlopers polluting the sample).”
• Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, methodology): “We gathered IR data from the all-sky WISE survey (Wright et al. 2010) to study associations from the SACY sample (Torres et al. 2008), and therefore they were not affected by this problem.”
• Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager (2015, unknown): “Significant differences for the estimated age of the BPMG appear in the literature, ranging from 12 to 23 Myr ( 29 , 30 , 32 , 57 ) An age of 13 Myr for 51 Eri, independent from possible membership in the BPMG, was deduced from measurements with the CHARA optical interferometer on Mount Wilson ( 29…”