BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS

By L. Malo, R. Doyon, D. Lafrèniere, É. Artigau, J. Gagné, F. Baron, A. Riedel. 2012

260 citations recorded by the source corpus.

We present a new method based on a Bayesian analysis to identify new members of nearby young kinematic groups. The analysis minimally takes into account the position, proper motion, magnitude, and color of a star, but other observables can be readily added (e.g., radial velocity, distance). We use this method to find new young low-mass stars in the β Pictoris and AB Doradus moving groups and in the TW Hydrae, Tucana-Horologium, Columba, Carina, and Argus associations. Starting from a sample of 758 mid-K to mid-M (K5V–M5V) stars showing youth indicators such as Hα and X-ray emission, our analysis yields 214 new highly probable low-mass members of the kinematic groups analyzed. One is in TW Hydrae, 37 in β Pictoris, 17 in Tucana-Horologium, 20 in Columba, 6 in Carina, 50 in Argus, 32 in AB Doradus, and the remaining 51 candidates are likely young but have an ambiguous membership to more than one association. The false alarm rate for new candidates is estimated to be 5% for β Pictoris and TW Hydrae, 10% for Tucana-Horologium, Columba, Carina, and Argus, and 14% for AB Doradus. Our analysis confirms the membership of 58 stars proposed in the literature. Firm membership confirmation of our new candidates will require measurement of their radial velocity (predicted by our analysis), parallax, and lithium 6708 Å equivalent width. We have initiated these follow-up observations for a number of candidates, and we have identified two stars (2MASSJ01112542+1526214, 2MASSJ05241914-1601153) as very strong candidate members of the β Pictoris moving group and one strong candidate member (2MASSJ05332558-5117131) of the Tucana-Horologium association; these three stars have radial velocity measurements confirming their membership and lithium detections consistent with young age.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/7a7ee331e698052ffd321b48264c957b9d9e44ac

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Citations in the corpus

AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, background): “However, Malo et al. (2013) assign a dynamical membership probability of 99%.”
Imaging Extrasolar Giant Planets (2016, background): “…& Simon 2009; Schlieder et al. 2010; Kiss et al. 2010; Rodriguez et al. 2011a; Schlieder et al. 2012a; Schlieder et al. 2012b; Shkolnik et al. 2012; Malo et al. 2013; Moor et al. 2013; Rodriguez et al. 2013; Malo et al. 2014; Gagné et al. 2014; Riedel et al. 2014; Kraus et al. 2014b; Gagné et…”
A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “GJ 9303 (HIP 47133) was proposed as a BPMG member by Schlieder et al. (2012a), however the Bayesian analysis of Malo et al. (2013) suggests that it is more likely associated with the field (Pv+π = 99 per cent).”
PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “For example, Vigan et al. (2012) targeted 38 A stars and 4 F stars and arrived at a frequency of 4.3+9.1 −1.3% when β Pic b is excluded (a priori knowledge of its existence can strongly bias the way the observations are conducted).”
The Hipparcos–Gaia Catalog of Accelerations (2018, background): “…and mapping of Galactic streams (Koppelman et al. 2018), of stellar moving groups with ever-expanding membership lists (Zuckerman et al. 2001, 2004; Malo et al. 2013; Gagné & Faherty 2018), measurements of the proper motions of globular clusters and dwarf galaxies (Simon 2018; Gaia Collaboration…”
BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, methodology): “Using the 2MASS J magnitude of the unresolved system with the young absolute magnitude-spectral type sequences of Malo et al. (2013), we estimate a distance of ∼ 450 pc.”
BANYAN. II. VERY LOW MASS AND SUBSTELLAR CANDIDATE MEMBERS TO NEARBY, YOUNG KINEMATIC GROUPS WITH PREVIOUSLY KNOWN SIGNS OF YOUTH (2013, methodology): “By performing a simpler Bayesian analysis similar to that presented in Malo et al. (2013) but including the CAS hypothesis, we find that the CAS hypothesis has PHk = 99.7% whereas ARG has a negligible probability (remember those probabilities are strongly biased).”
On the age of the β Pictoris moving group (2014, methodology): “The one-dimensional velocity dispersions are somewhat similar to those calculated by Malo et al. (2013) (σintU , σ int V , σ int W = 2.06, 1.30, and 1.54 km s −1) and Malo et al. (2014a) (σintU , σ int V , σ int W = 2.06, 1.32, and 1.35 km s −1), which used larger samples.”
A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 (2015, methodology): “To provide a quantitative estimate, we used the BANYAN II web tool (Malo et al. 2013; Gagné et al. 2014).”
HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, unknown): “…(2001), 13: Looper et al. (2010), 14: Shkolnik et al. (2012), 15: Kraus et al. (2014), 16: Montes et al. (2001), 17: Zuckerman et al. (2004), 18: Malo et al. (2013), 19: López-Santiago et al. (2006), 20: Bowler et al. (2012), 21: Ammler-von Eiff & Guenther (2009), 22: Perryman et al. (1998),…”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, methodology): “This is similar to the functioning of BANYAN I (Malo et al. 2013) and BANYAN II (Gagné et al. 2014).”
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): “Finally, we computed the YMGmembership probability using the online calculator of Malo et al. (2013).”
A lithium depletion boundary age of 21 Myr for the Beta Pictoris moving group (2013, methodology): “2006; Mentuch et al. 2008; Yee & Jensen 2010; Malo et al. 2013), all of which also satisfy the RV criterion discussed above.”
THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, methodology): “Kinematic BANYAN II analysis: We used the BANYAN II online tool (Malo et al. 2013; Gagné et al. 2014b), which relies on a model of the kinematic and spatial distribution of the solar neighborhood, assumed to be composed of seven YMGs (Argus [ARG], Columba [COL], β Pic [BPMG], AB Dor [ABDMG],…”