Volume 513, April 2010
|Number of page(s)||11|
|Section||Stellar structure and evolution|
|Published online||27 April 2010|
The end of the white dwarf cooling sequence in M 67*
Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, 35122 Padova, Italy
2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: firstname.lastname@example.org
3 Astrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Birkenhead, 41 1LD, UK
4 INAF – Osservatorio Astronomico di Teramo, via M. Maggini snc, 64100 Teramo, Italy
5 INAF – Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy
6 Institute of Astronomy and Astrophysics, NOA, I. Metaxa and Vas. Pavlou Street, Palaia Penteli 15236, Greece
7 Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
8 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
9 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy
10 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA
11 Center for Cosmology and Astroparticle Physics, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA
12 ESO, Alonso de Cordova 3107, Vitacura, Santiago de Chile, Chile
13 Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263129, India
Accepted: 20 January 2010
In this paper, we present for the first time a proper-motion-selected white dwarf (WD) sample of the old Galactic open cluster M 67, down to the bottom of the WD cooling sequence (CS). The color-magnitude diagram is based on data collected with the LBC-Blue camera at the prime-focus of LBT. As first epoch data, we used CFHT-archive images collected 10 years before LBC data. We measured proper motions of all the identified sources. Proper motions are then used to separate foreground and background objects from the cluster stars, including WDs. Finally, the field-object cleaned WD CS in the V vs. B–I color-magnitude diagram is compared with the models. We confirm that the age derived from the location of the bottom of the WD CS is consistent with the turn off age.
Key words: white dwarfs / open clusters and associations: individual: NGC 2682 / Hertzsprung-Russell (HR) and C-M diagrams
Based on data acquired using 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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.