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Exploiting kinematics and UBVIc photometry to establish high fidelity membership of the open cluster Blanco 1

Cargile, P. A. ; James, D. J. ; Platais, I. ; Mermilliod, J.-C ; Deliyannis, C. ; Steinhauer, A.

In: Proceedings of the International Astronomical Union, 2007, vol. 3, no. S248, p. 490-491

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    Titre
    • Exploiting kinematics and UBVIc photometry to establish high fidelity membership of the open cluster Blanco 1
    Auteur
    • Cargile, P. A.. Department of Physics and Astronomy, Vanderbilt University Nashville, TN 37235, USA email: p.cargile@vanderbilt.edu
    • James, D. J.. Department of Physics and Astronomy, Vanderbilt University Nashville, TN 37235, USA email: p.cargile@vanderbilt.edu
    • Platais, I.. Johns-Hopkins University, Baltimore, MD, USA
    • Mermilliod, J.-C. EPFL Lausanne, Lausanne, Switzerland
    • Deliyannis, C.. Universtiy of Indiana, Bloomington, IN, USA
    • Steinhauer, A.. SUNY-Geneseo, Geneseo, NY, USA
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Proceedings of the International Astronomical Union, 2007, vol. 3, no. S248, p. 490-491. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:294607
    Summary
    We present the results of a wide-field, high-precision UBVIc CCD photometric survey of the Galactic open cluster Blanco 1. Standardized photometry was acquired using the Y4Kcam on the SMARTS 1m telescope at CTIO. We have also determined new high-precision proper motions (σμ = 0.3 mas yr−1) over an eight square degree area down to V = 16.5. Combined with 1D kinematic data, our survey yields a complete list of cluster members down to ~ 0.5 M and new high-fidelity color-magnitude diagrams are presented for Blanco 1. Having established a bona fide membership catalog, astrophysical characteristics of solar-type cluster members such as X-ray activity and lithium abundance have been studied to gain more insights in the process of internal mixing and convection. Our new results should also help to better understand its peculiar location in the Milky Way and to unravel its dynamical history