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|Title:||Photometric and spectroscopic study of the intermediate-age open cluster NGC 2355||Authors:||Donati, P.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||453||Issue:||4||First Page:||4185||Abstract:||In this paper we analyse the evolutionary status and properties of the old open cluster NGC 2355, located in the Galactic anticentre direction, as a part of the long-term programme Bologna Open Clusters Chemical Evolution. NGC 2355 was observed with the Large Binocular Camera at the Large Binocular Telescope using the Bessel B, V, and I<SUB>c</SUB> filters. The cluster parameters have been obtained using the synthetic colour-magnitude diagram method, as done in other papers of this series. Additional spectroscopic observations with the Fibre-fed Echelle Spectrograph at the Nordic Optical Telescope of three giant stars were used to determine the chemical properties of the cluster. Our analysis shows that NGC 2355 has metallicity slightly less than solar, with [Fe/H]= -0.06 dex, age between 0.8 and 1 Gyr, reddening E(B - V) in the range 0.14-0.19 mag, and distance modulus (m - M)<SUB>0</SUB> of about 11 mag. We also investigate the abundances of O, Na, Al, α, iron-peak, and neutron capture elements, showing that NGC 2355 falls within the abundance distribution of similar clusters (same age and metallicity). The Galactocentric distance of NGC 2355 places it at the border between two regimes of metallicity distribution; this makes it an important cluster for the study of the chemical properties and evolution of the disc.||Acknowledgments:||We thank Paolo Montegriffo, whose software for catalogue matching we consistently use for our work and Heather Jacobson for sharing information. We thank the personnel at LBT and NOT for their help and for taking part of the data. For this paper we used the VizieR catalogue access tool (CDS, Strasbourg, France), WEBDA (originally created by J.-C. Mermilliod and now maintained by E. Paunzen), and NASA's Astrophysics Data System. This research has been partially funded by MIUR and INAF (grants ‘The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies', prot. 2010LY5N2T; grant ‘Premiale VLT 2012'). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/ . The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.||URI:||http://hdl.handle.net/20.500.12386/23291||URL:||https://academic.oup.com/mnras/article/453/4/4185/2593719||ISSN:||0035-8711||DOI:||10.1093/mnras/stv1914||Bibcode ADS:||2015MNRAS.453.4185D||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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