Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Gagné, Jonathan; Faherty, Jacqueline K.; Mamajek, Eric E.

doi:10.3847/1538-4357/aadaed

Cited by 44 publications

(32 citation statements)

References 76 publications

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“…To address the problem of the origin of this discrepancy, which has been observed by different authors using several theoretical models and which is already discussed in the literature (see e.g. Gagné, Faherty & Mamajek 2018) is out of the purposes of this paper. It is common opinion that part of the disagreement is caused by the atmosphere models used to obtain the synthetic spectra, which still have problems in correctly predicting the flux in the optical/blue part of the spectra (e.g.…”

Section: The Synthetic and Hyades Data Samplementioning

confidence: 96%

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Tognelli

Dell’Omodarme

Valle

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We tested the capability of a Bayesian procedure to calibrate both the helium abundance and the mixing length parameter (αML), using precise photometric data for main sequence (MS) stars in a cluster with negligible reddening and well determined distance. The method has been applied first to a mock dataset generated to mimic Hyades MS stars and then to the real Hyades cluster. We tested the impact on the results of varying the number of stars in the sample, the photometric errors, and the estimated [Fe/H]. The analysis of the synthetic dataset shows that αML is recovered with a very good precision in all the analysed cases (with an error of few percent), while [Fe/H] and the helium-to-metal enrichment ratio ΔY/ΔZ are more problematic. If spectroscopic determinations of [Fe/H] are not available and thus [Fe/H] has to be recovered alongside with ΔY/ΔZ and αML, the well known degeneracy between [Fe/H]-ΔY/ΔZ-αML could result in a large uncertainty on the recovered parameters, depending on the portion of the MS used for the analysis. On the other hand, the prior knowledge of an accurate [Fe/H] value puts a strong constraint on the models, leading to a more precise parameters recovery. Using the current set of PISA models, the most recent [Fe/H] value and the Gaia photometry and parallaxes for the Hyades cluster, we obtained the average values <αML>=2.01 ± 0.05 and <ΔY/ΔZ>=2.03 ± 0.33, sensitively reducing the uncertainty in these important parameters.

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Section: The Synthetic and Hyades Data Samplementioning

confidence: 96%

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Tognelli

Dell’Omodarme

Valle

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Volans-Carina group (VCA) Oh et al (2017) discovered a group of comoving 19 stars with Gaia DR1. The mean distance and the age of the group are 85 pc and 90 Myr, respectively (Gagné et al 2018d). Gagné et al (2018d) suggested ∼45 additional members with Gaia DR2.…”

Section: Appendix A: Additional Nymgs Included In This Studymentioning

confidence: 99%

“…The mean distance and the age of the group are 85 pc and 90 Myr, respectively (Gagné et al 2018d). Gagné et al (2018d) suggested ∼45 additional members with Gaia DR2. Figure B1.…”

Section: Appendix A: Additional Nymgs Included In This Studymentioning

confidence: 99%

Development of models for nearby young stellar moving groups: creation, revision, and finalisation of the models

Lee

Song

2019

Monthly Notices of the Royal Astronomical Society

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Lee & Song (2018, Paper 1) developed a tool for calculating Bayesian membership probability for nearby young stellar moving groups (BAMG: Bayesian Analysis of Moving Groups). The study presented the importance of careful construction of models in moving group membership assessment, using β Pictoris moving group as a test case. In this study, we build models for all major nearby young stellar moving groups (NYMGs hereafter) through 4 stages. A set of prototype models is created using members listed in the discovery paper of each group. For each group, suggested members after the discovery of the group are used for revising these prototype models. As these additional members being incorporated, group properties of a NYMG changes, thus membership probabilities change as well. A subset of stars show consistently large membership probabilities regardless of the details of a chosen method for ingesting additional members. Utilising these members, the NYMG models are finalised. The finalised models are applied for evaluating memberships of all claimed candidate members, resulting in a list of bona fide members. The mass function of bona fide members for the entire set of NYMG members indicates that more late-M type members should be identified. In addition, some objects showing a large difference in membership probability between BAMG and BANYAN Σ Gagné et al. (2018b) are presented and discussed. Memberships of some planet host stars are changed, and it can have a significant influence on the estimated planetary masses. Development of models for NYMGs 3process of building up NYMG models. Throughout this paper, D indicates a kinematic data set of stars, and subscripts describe classes of the data (e.g., D I , D 0 , and D final indicate initial, good initial, and finalised members, respectively). M represents a NYMG model (i.e., a set of 18 parameters), and subscripts indicate which set of stars are used to build the model (e.g., M 0 is generated using D 0 ). Each stage is performed iteratively. Details of each stage are described in Section 2.2−2.5.

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“…The arguably first paper to provide some order to this new field involved this group of ∼10 Myr old stars − the TW Hya Association − located about 60 pc from Earth (Kastner et al 1997). Since then perhaps as many as 10 other associations of stars with ages 200 Myr or less and within ∼100 pc of Earth have been identified (e.g., Zuckerman & Song 2004;Torres et al 2008;Mamajek 2016;Gagné et al 2018). Akin to star clusters, members of a given nearby, young stellar association or moving group have similar ages and space motions through the Milky Way (they are coeval and comoving).…”

Section: Introductionmentioning

confidence: 99%

The Nearby, Young, χ¹ Fornacis Cluster: Membership, Age, and an Extraordinary Ensemble of Dusty Debris Disks

Zuckerman

Klein

Kastner

2019

ApJ

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Only four star clusters are known within ∼100 pc of Earth. Of these, the χ 1 For cluster has barely been studied. We use the Gaia DR2 catalog and other published data to establish the cluster membership, structure, and age. The age of and distance to the cluster are ∼40 Myr and 104 pc, respectively. A remarkable, unprecedented, aspect of the cluster is the large percentage of M-type stars with warm excess infrared emission due to orbiting dust grains − these stars lie in an annulus that straddles the tidal radius of the cluster. The χ 1 For cluster appears to be closely related to two extensive, previously known, groups of comoving, coeval stars (the Tucana-Horologium and Columba Associations) that are spread over much of the southern sky. While Tuc-Hor and χ 1 For are comoving and coeval, the difference in the frequency of their warm dusty debris disks at M-type stars could hardly be more dramatic.

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Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Cited by 44 publications

References 76 publications

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Development of models for nearby young stellar moving groups: creation, revision, and finalisation of the models

The Nearby, Young, χ¹ Fornacis Cluster: Membership, Age, and an Extraordinary Ensemble of Dusty Debris Disks

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Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Cited by 44 publications

References 76 publications

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Bayesian calibration of the mixing length parameter αML and of the helium-to-metal enrichment ratio ΔY/ΔZ with open clusters: the Hyades test-bed

Development of models for nearby young stellar moving groups: creation, revision, and finalisation of the models

The Nearby, Young, χ1 Fornacis Cluster: Membership, Age, and an Extraordinary Ensemble of Dusty Debris Disks

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The Nearby, Young, χ¹ Fornacis Cluster: Membership, Age, and an Extraordinary Ensemble of Dusty Debris Disks