Volume 513, April 2010
|Number of page(s)||6|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||27 April 2010|
Absolute proper motion of the Galactic open cluster M 67*
Dipartimento di Astronomia, Università di Padova, Vicolo
dell'Osservatorio 3, 35122 Padova, Italy e-mail: email@example.com
2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
3 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510-México DF, Mexico
Accepted: 23 February 2010
We derived the absolute proper motion (PM) of the old, solar-metallicity Galactic open cluster M 67 using observations collected with CFHT (1997) and with LBT (2007). About 50 galaxies with relatively sharp nuclei allow us to determine the absolute PM of the cluster. We find ( cos δ, )J2000.0 = (-9.6 ± 1.1, -3.7 ± 0.8) mas yr-1. By adopting a line-of-sight velocity of 33.78 ± 0.18 km s-1, and assuming a distance of 815 ± 50 pc, we explore the influence of the Galactic potential, with and without the bar and/or spiral arms, on the galactic orbit of the cluster.
Key words: astrometry / open cluster and associations: NGC 2682 (M 67) / Galaxy: kinematics and dynamics
Based on data acquired with the Large Binocular Telescope (LBT) at Mt. Graham, Arizona, under the Commissioning of the Large Binocular Blue Camera. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; the Ohio State University, and the Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia; and on observations obtained at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.
© ESO, 2010
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